the kepler characterization of the variability among a
TRANSCRIPT
A&A 534, A125 (2011)DOI: 10.1051/0004-6361/201117368c© ESO 2011
Astronomy&
Astrophysics
The Kepler characterization of the variability amongA- and F-type stars
I. General overview
K. Uytterhoeven1,2,3, A. Moya4, A. Grigahcène5, J. A. Guzik6, J. Gutiérrez-Soto7,8,9, B. Smalley10, G. Handler11,12,L. A. Balona13, E. Niemczura14, L. Fox Machado15, S. Benatti16,17, E. Chapellier18, A. Tkachenko19, R. Szabó20,
J. C. Suárez7, V. Ripepi21, J. Pascual7, P. Mathias22, S. Martín-Ruíz7, H. Lehmann23, J. Jackiewicz24, S. Hekker25,26,M. Gruberbauer27,11, R. A. García1, X. Dumusque5,28, D. Díaz-Fraile7, P. Bradley29, V. Antoci11, M. Roth2, B. Leroy8,
S. J. Murphy30, P. De Cat31, J. Cuypers31, H. Kjeldsen32, J. Christensen-Dalsgaard32 , M. Breger11,33, A. Pigulski14,L. L. Kiss20,34, M. Still35, S. E. Thompson36, and J. Van Cleve36
(Affiliations can be found after the references)
Received 30 May 2011 / Accepted 29 June 2011
ABSTRACT
Context. The Kepler spacecraft is providing time series of photometric data with micromagnitude precision for hundreds of A-F type stars.Aims. We present a first general characterization of the pulsational behaviour of A-F type stars as observed in the Kepler light curves of a sampleof 750 candidate A-F type stars, and observationally investigate the relation between γDoradus (γDor), δ Scuti (δSct), and hybrid stars.Methods. We compile a database of physical parameters for the sample stars from the literature and new ground-based observations. We analysethe Kepler light curve of each star and extract the pulsational frequencies using different frequency analysis methods. We construct two newobservables, “energy” and “efficiency”, related to the driving energy of the pulsation mode and the convective efficiency of the outer convectivezone, respectively.Results. We propose three main groups to describe the observed variety in pulsating A-F type stars: γDor, δSct, and hybrid stars. We assign 63%of our sample to one of the three groups, and identify the remaining part as rotationally modulated/active stars, binaries, stars of different spectraltype, or stars that show no clear periodic variability. 23% of the stars (171 stars) are hybrid stars, which is a much higher fraction than what hasbeen observed before. We characterize for the first time a large number of A-F type stars (475 stars) in terms of number of detected frequencies,frequency range, and typical pulsation amplitudes. The majority of hybrid stars show frequencies with all kinds of periodicities within the γDorand δSct range, also between 5 and 10 d−1, which is a challenge for the current models. We find indications for the existence of δSct and γDorstars beyond the edges of the current observational instability strips. The hybrid stars occupy the entire region within the δSct and γDor instabilitystrips and beyond. Non-variable stars seem to exist within the instability strips. The location of γDor and δSct classes in the (Teff , log g)-diagramhas been extended. We investigate two newly constructed variables, “efficiency” and “energy”, as a means to explore the relation between γDorand δ Sct stars.Conclusions. Our results suggest a revision of the current observational instability strips of δSct and γDor stars and imply an investigation ofpulsation mechanisms to supplement the κ mechanism and convective blocking effect to drive hybrid pulsations. Accurate physical parameters forall stars are needed to confirm these findings.
Key words. stars: oscillations – stars: fundamental parameters – binaries: general – asteroseismology – stars: variables: δ Scuti – stars: statistics
1. Introduction
With the advent of the asteroseismic space missions MOST(Walker et al. 2003), CoRoT (Baglin et al. 2006), and Kepler(Borucki et al. 2010), a new window is opening towards the un-derstanding of the seismic behaviour of A- and F-type pulsators.The main advantages of these space missions are (1) the long-term continuous monitoring of thousands of stars, which enablesboth the determination of long-period oscillations and the re-solving of beat frequencies; and (2) the photometric precisionat the level of milli- to micro-magnitudes, which will providea more complete frequency spectrum and also allow the detec-tion of low-amplitude variations that are unobservable from theground and providing a more complete frequency spectrum. Theavailability of these long-term, very precise light curves makespossible the first comprehensive analysis of the variability of asample of several hundred candidate A-F type stars that is pre-sented here.
The region of variable A- and F-type, including main se-quence (MS), pre-MS, and post-MS stars, with masses be-tween 1.2 and 2.5 M� hosts the γDoradus (γDor) and δ Scuti(δSct) pulsators. The γDor stars were recognized as a new classof pulsating stars less than 20 years ago (Balona et al. 1994).Our current understanding is that they pulsate in high-order grav-ity (g) modes (Kaye et al. 1999a), excited by a flux modulationmechanism induced by the upper convective layer (Guzik et al.2000; Dupret et al. 2004; Grigahcène 2005). Typical γDor peri-ods are between 8 h and 3 d. From the ground, about 70 bona fideand 88 candidate γDor pulsators have been detected (Balonaet al. 1994; Handler 1999; Henry et al. 2005; De Cat et al. 2006;Henry et al. 2011, among other papers).
The δSct variables, on the other hand, have been known fordecades. They show low-order g and pressure (p) modes withperiods between 15 min and 5 h that are self-excited throughthe κ-mechanism (see reviews by Breger 2000; Handler 2009a).
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Several hundreds of δ Sct stars have been observed from theground (e.g. catalogue by Rodríguez & Breger 2001).
Because the instability strips of both classes overlap, the ex-istence of hybrid stars, i.e. stars showing pulsations excited bydifferent excitation mechanisms, is expected, and a few candi-date hybrid stars have indeed been detected from the ground(Henry & Fekel 2005; Uytterhoeven et al. 2008; Handler 2009b).
The main open question in seismic studies of A- and F-typestars concerns the excitation and mode selection mechanism of pand g modes. The only way to understand and find out sys-tematics in the mode-selection mechanism is a determinationof pulsation frequencies and pulsation mode parameters for alarge number of individual class members for each of the pulsa-tion classes, and a comparison of the properties of the differentcase-studies. So far, a systematic study of a sufficiently substan-tial sample was hampered by two factors. First, the number ofdetected well-defined pulsation modes is too small to constructunique seismic models, which is caused by ground-based obser-vational constraints, such as bad time-sampling and a high noise-level. Second, only a small number of well-studied cases ex-ist, because a proper seismic study requires a long-term project,involving ground-based multi-site campaigns spanning severalseasons, or a dedicated space mission.
First demonstrations of the strength and innovative characterof space data with respect to seismic studies of A-F type stars arethe detection of two hybrid γDor-δSct stars by the MOST satel-lite (HD 114839, King et al. 2006; BD+18-4914, Rowe et al.2006), and the detection of an impressive number of frequenciesat low amplitudes, including high-degree modes as confirmedby ground-based spectroscopy, in the precise space CoRoT pho-tometry of the δSct stars HD 50844 (Poretti et al. 2009) andHD 174936 (García Hernández et al. 2009), and the γDor starHD 49434 (Chapellier et al. 2011). The first indications that hy-brid behaviour might be common in A-F type stars were foundfrom a pilot study of a larger sample of Kepler and CoRoT stars(Grigahcène et al. 2010; Hareter et al. 2010). Recently, Balonaet al. (2011a) announced the detection of δ Sct and γDor typepulsations in the Kepler light curves of Ap stars. Hence, a break-through is expected in a currently poorly-understood field ofseismic studies of A-F type pulsators through a systematic andcareful investigation of the pulsational behaviour in a large sam-ple of stars.
The goals of the current paper are (1) to present a first generalcharacterization of the pulsational behaviour of main-sequenceA-F type stars as observed in the Kepler light curves of a largesample; and (2) to observationally investigate the relation be-tween γDor and δ Sct stars and the role of hybrids. In forthcom-ing papers, detailed seismic studies and modelling of selectedstars will be presented.
2. The Kepler sample of A-F type stars
2.1. The Kepler data
The NASA space mission Kepler was launched in March 2009and is designed to search for Earth-size planets in the extendedsolar neighbourhood (Borucki et al. 2010; Koch et al. 2010).To this end, the spacecraft continuously monitors the brightnessof ∼150 000 stars in a fixed area of 105 deg2 in the constellationsCygnus, Lyra, and Draco, at Galactic latitudes from 6 to 20 deg.The nearly uninterrupted time series with micromagnitude preci-sion also opens up opportunities for detailed and in-depth aster-oseismic studies with unprecedented precision (Gilliland et al.2010a). Of all Kepler targets, more than 5000 stars have been
selected as potential targets for seismic studies by the KeplerAsteroseismic Science Consortium, KASC1.
The Kepler Mission offers two observing modes: long ca-dence (LC) and short cadence (SC). The former monitors se-lected stars with a time resolution of ∼30 min (Jenkins et al.2010a), the latter provides a 1-min sampling (Gilliland et al.2010b). The LC data are well-suited to search for long-periodg-mode variations in A-F type stars (periods from a few hours toa few days), while the SC data are needed to unravel the p-modeoscillations (periods of the order of minutes to hours).
The Kepler asteroseismic data are made available tothe KASC quarterly. In this paper we consider data fromthe first year of Kepler operations: the 9.7 d Q0 com-missioning period (1−11 May 2009), the 33.5 d Q1 phasedata (12 May−14 June 2009), the 88.9 d Q2 phase data(19 June−15 September 2009), the 89.3 d time string of Q3(18 September−16 December 2009), and 89.8 d of Q4 data(19 December 2009−19 March 2010). The SC data are subdi-vided into three-monthly cycles, labelled, for example, Q3.1,Q3.2 and Q3.3.
Not all quarters Q0–Q4 are available for all stars. The firstyear of Kepler operations was dedicated to the survey phase ofthe mission. During this phase as many different stars as possiblewere monitored with the aim to identify the best potential can-didates for seismic studies. From the survey sample, the KASCworking groups selected subsamples of the best seismic candi-dates for long-term follow-up with Kepler. From quarter Q5 on-wards, only a limited number of selected KASC stars are beingobserved with Kepler. The results of the selection process of themost promising γDor, δ Sct, and hybrid candidates are presentedin this work.
2.2. Selection of the A-F type star sample
We selected all stars in the Kepler Asteroseismic ScienceOperations Center (KASOC) database initially labelled as γDoror δ Sct candidates. The stars were sorted into these KASOCcatagories either because the Kepler Input Catalogue (KIC;Latham et al. 2005; Brown et al. 2011) value of their effectivetemperature Teff and gravity log g suggested that they lie in orclose to the instability strips of γDor and δSct stars, or be-cause they where proposed as potential variable A-F type can-didates in pre-launch asteroseismic Kepler observing propos-als. To avoid sampling bias and to aim at completeness of thesample, we analysed all stars listed in the KASOC catalogueas δSct or γDor candidates. Our analysis results provide feed-back on the initial guess on variable class assigment by KASOC.As will be seen (Sect. 6.2), several of these stars actually be-long to other pulsation classes, many of which are cool stars.Because there are much fewer B-type stars in the Kepler field ofview than cooler stars, there is a natural selection effect towardscooler stars. We also included stars initially assigned to otherpulsation types that showed periodicities typical for δSct and/orγDor stars. We are aware that many more δ Sct and γDor candi-date stars are being discovered among the KASC targets, but wecannot include all in this study.
The total sample we considered consists of 750 stars.For 517 stars both LC and SC data are available, while 65and 168 stars were only observed in SC and LC mode, respec-tively. An overview of the A-F type star sample is given inTable 1, available in the on-line version of the paper. The firstthree columns indicate the KIC identifier of the star (KIC ID),
1 http://astro.phys.au.dk/KASC
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right ascension (RA), declination (Dec), and Kepler magni-tude (Kp). The Kepler bandpass is wider than the typicalbroad-band filters that are commonly used in optical astronomy(e.g. Johnson UBVRI), and can be described as “white” light.The next three columns provide information on the spectral type(Spectral Type), alternative name of the target (Name), and acomment on its variability (Variable). Information on binaritycomes from the Washington Double Star Catalog (Worley &Douglass 1997; Mason et al. 2001), unless mentioned otherwise.For binary stars labelled with “�”, the double star was suspectedby inspecting Digitized Sky Survey and 2MASS images by eye.The next set of columns provides information on the Kepler timeseries. For each star, the number of datapoints (N datapoints), thetotal time span of the dataset (ΔT ) expressed in d, the longesttime gap in the Kepler light curves (δT ) expressed in d, andthe available (range of) quarters in LC (Quarters LC) and SC(Quarters SC) mode are given.
2.3. Sample stars in the literature
Most of the 750 sample stars were previously unstudied. Wesearched the catalogue by Skiff (2007) and found informationon spectral types for only 212 stars. Besides 198 confirmed A-or F-type stars, among which are fourteen chemically peculiarstars, we discovered that stars with a different spectral type alsoended up in the sample. There are six known B stars, one M star,three K stars, and six G-type stars in the sample. The G starKIC 7548061 (V1154 Cyg) is a known and well-studied Cepheid(e.g. Pigulski et al. 2009) and is the subject of a dedicated paperbased on Kepler data by Szabó et al. (2011). Sixty-two stars areknown to belong to multiple systems, including at least four-teen eclipsing binaries (EB; KIC 1432149, Hartman et al. 2004;KIC 10206340, Malkov et al. 2006; catalogues by Prša et al.2011; and Slawson et al. 2011). Seven stars are only known as“(pulsating) variable stars”. The star KIC 2987660 (HD 182634)is reported as a δSct star by Henry et al. (2001). Our samplealso includes a candidate α2 Canum Venaticorum star, namelyKIC 9851142 or V2094 Cyg (Carrier et al. 2002; Otero 2007).The Kepler field hosts four open clusters. In our sample at leastsix known members of NGC 6819 are included. Also one, eight,and nine members of NGC 6791, NGC 6811, and NGC 6866,respectively, are in our sample. All 750 stars are included inthe analysis.
3. Physical parameters of the sample stars
Seismic models require accurate values of physical parameterssuch as log g, Teff , metallicity [M/H], and projected rotationalvelocity v sin i. We compiled an overview of all Teff , log g, andv sin i values available for the sample stars in Table 2 in theon-line version of the paper. The different sources include lit-erature and KIC, along with values derived from new ground-based data. A description of the different sources is given be-low. The columns of Table 2 are (1) KIC identifier (KIC ID);(2) Teff value from KIC; (3)−(5) Teff values taken from theliterature or derived from new ground-based data (Literature);(6) adopted Teff value (Adopted); (7) log g value from KIC;(8)−(9) log g values taken from the literature or derived fromnew ground-based data (Literature); (10) adopted log g value(Adopted); (11)−(12) v sin i values derived from spectroscopicdata (Spectra). Stars that are known to be spectroscopic binariesare flagged ◦ behind its KIC identifier (KIC ID). The derivedphysical parameters of the binary stars have to be considered
Fig. 1. 750 sample stars in the (Teff , log g)-diagram. The cross at the lefttop corner represents the typical error bars on the values: 290 K for Teff
and 0.3 dex for log g.
with caution because the contribution of the binary componentsmight not have been correctly separated.
KIC-independent values of log g and Teff are only avail-able for 110 stars. The values used for the subsequent analy-sis are (in order of priority, depending on availability and ac-curacy) the spectroscopically derived values, or the most recentphotometrically derived values. For all other stars we use theonly source: the KIC values. The corresponding adopted Teff(in K), and log g (in dex) values are given in boldface in the sixthand tenth column of Table 2, respectively (column “Adopted”).For 65 and 71 stars no value of Teff and log g, respectively,is available. Figure 1 shows the sample of 750 stars in the(Teff, log g)-diagram. We estimated the error bars on the KIC val-ues by comparing them with the adopted values taken fromthe literature or ground-based data. The average difference was290 K for Teff and 0.3 dex for log g. v sin i values are only avail-able for 52 of the sample stars.
3.1. Literature
Besides papers dedicated to specific targets of our sample,the on-line catalogues by Soubiran et al. (2010), Lafrasseet al. (2010), Kharchenko et al. (2009), Masana et al. (2006),Nordström et al. (2004), Glebocki & Stawikowski (2000),Allende Prieto & Lambert (1999), and Wright et al. (2003) werevery helpful in the search for values of Teff, log g, and v sin i.Also, photometric indices by Hauck & Mermilliod (1998) wereused to estimate values of Teff and log g. We took care not toinclude Teff values that are derived from the spectral type ratherthan directly from data. The literature values of Teff and log g canbe found in Cols. 3−5 and 8, 9 of Table 2, respectively (“lit”).We note that the given errors on Teff and log g, which sometimesseem unrealistic small, are taken from the quoted paper and arenot rounded to the number of significant digits. Values of v sin i,expressed in km s−1, are given in the last two columns of Table 2.The source of each value is indicated by the label.
3.2. Kepler Input Catalogue
The KIC provides an estimate of Teff and log g for most Keplertargets derived from Sloan photometry (see the second and
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seventh column, “KIC”, of Table 2, respectively). Unfortunately,the KIC values of log g are known to have large errorbars (Molenda-Zakowicz et al. 2011; Lehmann et al. 2011).Moreover, a comparison between KIC estimates of the stellarradius and the radius derived from evolutionary models indicatethat the KIC values of log g might be shifted towards lower val-ues by about 0.1 dex. The temperature values, on the other hand,are fairly good for A-F type stars, and become less reliable formore massive or peculiar stars, because for higher temperaturesthe interstellar reddening is apparently not properly taken intoaccount. The stars in our sample are reddened up to 0.3 magin (B − V), with an average reddening of E(B − V) = 0.04 mag.The 85 stars for which no KIC Teff value is available, which aregenerally faint stars (Kp > 11 mag), are not considered in anyanalysis related to temperature, unless values of Teff exist in theliterature or are available from the analysis of new ground-basedobservations (see below).
3.3. New ground-based observations of sample stars
In the framework of the ground-based observational project forthe characterization of KASC targets (see Uytterhoeven et al.2010a,b, for an overview), targets of the A-F type sample arebeing observed using multi-colour photometry and/or high-to-mid-resolution spectroscopy. The goal is to obtain precise valuesof physical parameters that are needed for the seismic modellingof the stars. A detailed analysis of a first subsample of A-F typestars has been presented by Catanzaro et al. (2011). Several otherpapers are in preparation. We include the available results to datein this paper, because the precise values of Teff and log g areneeded for the interpretations in Sects. 7 and 8.
3.3.1. Strömgren photometry from the ObservatorioSan Pedro Mártir
Multi-colour observations were obtained for 48 sample starsover the period 2010 June 13−17 with the six-channeluvby − β Strömgren spectrophotometer attached to the 1.5-mtelescope at the Observatorio Astrónomico Nacional-San PedroMártir (OAN-SPM), Baja California, Mexico. Each night, a setof standard stars was observed to transform instrumental obser-vations into the standard system using the well known trans-formation relations given by Strömgren (1966), and to correctfor atmospheric extinction. Next, the photometric data were de-reddeded using Moon’s UVBYBETA programme (Moon 1985),and Teff and log g values were obtained using the uvby grid pre-sented by Smalley & Kupka (1997). A detailed description ofthe data will be given by Fox Machado et al. (in prep.). The re-sulting stellar atmospheric parameters are presented in Table 2under label “b”.
3.3.2. SOPHIE spectra from the Observatoirede Haute Provence
We also analysed spectra of two sample stars, KIC 11253226and KIC 11447883, obtained during the nights of 2009 July 31,August 1, and August 5 with the high-resolution (R ∼ 70 000)spectrograph SOPHIE, which is attached to the 1.93-m telescopeat the Observatoire de Haute Provence (OHP), France. The spec-tra were reduced using a software package directly adapted fromHARPS, subsequently corrected to the heliocentric frame, andmanually normalized by fitting a cubic spline.
To derive stellar atmospheric parameters, the observed spec-tra, which covers the wavelength range 3870−6940 Å, werecompared with synthetic spectra. The synthetic spectra werecomputed with the SYNTHE code (Kurucz 1993), using atmo-spheric models computed with the line-blanketed LTE ATLAS9code (Kurucz 1993). The parameters were derived using themethodology presented in Niemczura et al. (2009) which relieson an efficient spectral synthesis based on a least-squares opti-misation algorithm. The resulting values of Teff, log g and v sin iare presented in Table 2, under label “h”. The detailed analysisresults, including element abundances and microturbulence, willbe presented in a dedicated paper (Niemczura et al., in prep.),including several other Kepler stars.
3.3.3. Spectra from the Tautenburg Observatory
Spectra of 26 sample stars were obtained from May toAugust 2010 with the Coude-Échelle spectrograph attached tothe 2-m telescope of the Thüringer Landessternwarte Tautenburg(TLS), Germany. The spectra cover 4700 to 7400 Å in wave-length range, with a resolution of R = 32 000. The spectra werereduced using standard ESO-MIDAS packages. We obtained be-tween two and seven spectra per star, which were radial velocitycorrected and co-added. The resulting signal-to-noise in the con-tinua is between 150 and 250.
Stellar parameters such as Teff, log g, [M/H], and v sin i havebeen determined by a comparison of the observed spectra withsynthetic ones, where we used the spectral range 4740 to 5800 Å,which is almost free of telluric contributions. The synthetic spec-tra have been computed with the SynthV programme (Tsymbal1996) based on atmosphere models computed with LLmodels(Shulyak et al. 2004). Scaled solar abundances have been usedfor different values of [M/H]. A detailed description of the ap-plied method can be found in Lehmann et al. (2011). The result-ing values of Teff , log g and v sin i are presented in Table 2, underlabel “g”. Errors are determined from χ2 statistics and representa 1-σ confidence level. Detailed analysis results, including alsovalues of [M/H] and microturbulent velocity, will be publishedin a dedicated paper (Tkachenko et al., in prep.).
4. Characterization of the sample
Figure 2 shows the distribution of the 750 sample stars in Teff(top left), log g (top right), Kepler magnitude Kp (bottom left),and total length of the Kepler light curve ΔT , expressed in d(bottom right). For the analysis we used Teff and log g valuesgiven in boldface in Table 2. Note that seven stars in our sampleare hotter than Teff = 9000 K, and fall off the diagram.
The following typical global parameters have been observedfor δSct and γDor stars (e.g. Rodríguez & Breger 2001; Handler& Shobbrook 2002): log g = 3.2−4.3 and Teff = 6300−8600 Kfor δ Sct stars, and log g = 3.9−4.3 and Teff = 6900−7500 K forγDor stars. While γDor stars are generally MS stars, severalmore evolved δSct stars have been observed.
The distributions in Fig. 2 show that about 70% of thetotal sample does indeed have Teff values between 6300 Kand 8600 K. However, a significant number (about 20%) arecooler stars. The log g values of our sample are concentratedon 3.5−4.5, which represents about 76% of the total sample.
The sample consists of stars with magnitudes in the range6 < Kp < 15 mag. The majority (about 55%) is located in theinterval Kp = [10, 12] mag. Given that stars with magnitudesfainter than V = 9 are difficult to monitor spectroscopically from
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Fig. 2. Distribution in Teff (top left), log g (top right), Kepler magni-tude Kp (bottom left), and total time span ΔT of the Kepler light curves,expressed in d (bottom right) of the 750 sample stars. The number ofstars belonging to each bin (N) is indicated on the Y-axis. We used theadopted values of Teff and log g, as given in boldface in Table 2.
the ground with 2 m-class telescopes, the fact that about 92% ofthe stars are fainter than V = 9 has implications for the feasibilityof possible spectroscopic ground-based follow-up observations(see Uytterhoeven et al. 2010a,b).
Finally, the total length of the Kepler dataset (not takinginto account possible gaps of several tens of days) is spread be-tween 9.5 and 322 d. For a considerable fraction (19%) of thesample only Q0 and Q1 data are available, with a total lengthof 44 d, implying a frequency resolution slightly worse than0.02 d−1. On the other hand, 351 stars, or 47% of the total sam-ple, have a time span of more than 200 d (resulting in a frequencyresolution better than 0.005 d−1). Of these 351 stars, 46% have amaximum time gap in the light curve of less than 10 d, and 23%have a gap of over 200 d and up to 325 d.
In the following sections we will describe the variabilityanalysis results of all 750 stars. At this stage we did not excludeany of the stars from the sample on grounds of non-compatibilityof physical parameters with the current expectations for A- andF-type pulsators, to present a homogenous analysis and to inves-tigate if Kepler confirms the current understanding of δ Sct andγDor stars.
5. Frequency analysis
5.1. Treatment of the Kepler light curves
In this paper we used the “non-corrected” light curves avail-able to KASC for asteroseismic investigations through theKASOC database. A description of the Kepler data reductionpipeline is given by Jenkins et al. (2010a,b). However, these rawtime series suffer from some instrumental perturbations that needto be corrected for, e.g. perturbations caused by the heating andcooling down of the Kepler CCDs, variations caused by changesin the aperture size of the source mask, etc. Some of the effectsare well known, and the corresponding non-stellar frequenciesare tabulated by the Kepler team (e.g. frequencies near 32, 400,430, and 690 d−1). Other perturbations are not documented, andare harder to evaluate and correct for.
We subjected the light curves of all sample stars to an auto-mated procedure that involves fitting a cubic spline to the timeseries, and correcting the residuals for discontinuities and out-liers. To investigate if and to what extent artificial periodicities
at the same timescale as the expected pulsations in γDor andδSct stars are introduced by the correction, we also correcteda subsample of stars by a different procedure that takes threetypes of effects into account, namely outliers, jumps, and drifts(see García et al. 2011). Both correction methods gave the samefrequency analysis results within the accuracy of the dataset.
Next, the Kepler flux (FKp(t)) was converted to parts-per-million (ppm) (Fppm(t)), using the following formula:
Fppm(t) = 106 ×(
FKp(t)
f(t)− 1
), (1)
with f (t) a polynomial fit to the light curve. A test on the ef-fect of the use of different polynomial orders (2 to 10) on thedetected frequencies in the time series showed that, in general,a third or fourth order polynomial fits the overall curvature bet-ter than a linear fit. The choice of the polynomial did not changeperiodicities with frequencies higher than 0.2 d−1. The obtainederror for frequencies between 0.01 and 0.2 d−1 was of the or-der of 1/ΔT d−1, with ΔT the total time span of the light curveexpressed in d.
5.2. Frequency analysis
The Kepler time series of the 750 sample stars were analysedin a homogenous way, using a programme based on the Lomb-Scargle analysis method (Scargle 1982). Frequencies were ex-tracted in an iterative way until the Scargle false alarm proba-bility (fap; Scargle 1982), a measure for the significance of apeak with respect to the underlying noise level, reached 0.001.In view of the almost uninterrupted and equidistant sampling ofthe Kepler data, this estimate of the fap is a fast and reliable ap-proximation of the true fap, because the number of independentfrequencies can be estimated precisely (see also the discussionin Sect. 4 of Balona et al. 2011b). Frequencies were calculatedwith an oversampling factor of 10. Time series consisting of onlyLC data were not searched for periods shorter than 1 h, becausethe corresponding Nyquist frequency is 24 d−1. For SC data, witha time sampling of about 1 min, frequencies up to 720 d−1 couldbe detected.
As a comparison, subsamples of the stars were analysedusing different analysis methods, such as SigSpec (Reegen2007, 2011), Period04 (Lenz & Breger 2005), the general-ized Lomb-Scargle periodogram (Zechmeister & Kürster 2009),and the non-interactive code, freqfind (Leroy & Gutiérrez-Soto,in prep.). The latter code is based on the non-uniform fast Fouriertransform by Keiner et al. (2009), and significantly decreases thecomputation time for unevenly spaced data. The results obtainedwith the different methods were consistent.
6. Classification
6.1. δSct, γDor, and hybrid stars
We performed a careful inspection (one-by-one, and by eye) ofthe 750 light curves, the extracted frequency spectra, and list ofdetected frequencies, and tried to identify candidate δ Sct, γDor,and hybrid stars. We used a conservative approach and omittedfrequencies with amplitudes lower than 20 ppm for the classi-fication. We also filtered out obvious combination frequenciesand harmonics2 in an automatic way, and only considered appar-ent independent frequencies for the analysis. We suspect that the
2 As obvious combination frequencies and harmonics we consid-ered n fi or k fi ± l f j, with fi and f j different frequencies, n ∈ [2, 3, 4, 5],and k, l ∈ [1, 2, 3, 4, 5].
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variable signal of a few stars is contaminated by the light varia-tions of a brighter neighbouring star on the CCD. We flagged allstars with a high contamination factor (>0.15), as given by theKIC. If the light curves of the neighbouring stars on the CCDwere available through KASOC3, we carefully checked the lightcurves of these stars with their neighbours. Stars that show an ob-vious contamination effect were omitted from classification. Weused information on Teff (Table 2) to distinguish between δSctand γDor stars versus βCep and SPB stars. To be conservative,low frequencies (<0.5 d−1) (see, for instance, the frequency spec-tra in Fig. 4) are currently not taken into account in the analysis,because in this frequency range real stellar frequencies are con-taminated with frequencies resulting from instrumental effects(see Sect. 5.1), and the separation of the different origins requiresa dedicated study, which is beyond the scope of this paper.
We encountered a variety of light curve behaviour. Basedon a small number of stars and using only the first quarterof Kepler data, Grigahcène et al. (2010) already proposed asubdivision of the A-F type pulsators into pure δSct stars,pure γDor stars, δSct/γDor hybrids and γDor/δSct hybrids,using the fact that frequencies are only detected in the δSct(i.e. >5 d−1, or >58 μHz) or γDor (i.e. <5 d−1 or <58 μHz)domain, or in both domains with dominant frequencies in ei-ther the δSct star or γDor star region, respectively. Among the750 sample stars we see different manifestations of hybrid vari-ability. There are stars that show frequencies with amplitudes ofsimilar height in both regimes, and stars with dominant frequen-cies in the γDor (δSct) domain and low amplitude frequenciesin the δSct (γDor) domain. The light curves show diversity aswell. Balona et al. (2011d) already commented on the differentshapes of light curves of pure γDor stars.
In this work, we focus on stars that show at least threeindependent frequencies. We classified the stars in threegroups: δSct stars, γDor stars, and hybrid stars. Because theunderlying physics that causes the different types of hybridbehaviour is currently not clear, all types of hybridity (bothδSct/γDor hybrids and γDor/δSct hybrids) are included in thegroup of hybrids. A star was classified as a hybrid star only if itsatisfied all of the following criteria:
– frequencies are detected in the δ Sct (i.e. >5 d−1 or >58 μHz)and γDor domain (i.e. <5 d−1 or <58 μHz);
– the amplitudes in the two domains are either comparable,or the amplitudes do not differ more than a factor of 5−7(case-to-case judgement);
– at least two independent frequencies are detected in bothregimes with amplitudes higher than 100 ppm.
By using these criteria, we should reduce the number of falsepositive detections. In particular, we tried to avoid a hybrid starclassification of “pure” δSct stars that show a prominent long-term variability signal caused by rotation. We also tried to takecare of more evolved δSct stars that are expected to pulsate withfrequencies lower than 5 d−1. Stars that exhibited only or mainlyfrequencies in the δSct domain (i.e. >5 d−1) and did not sat-isfy all of the above given criteria were assigned to the pureδSct group. Likewise, the group of pure γDor stars consists ofstars that do not comply with the hybrid star criteria, and that
3 Unfortunately, only 40 stars of the sample could be checked in thisway. We saw a clear contamination for the stars KIC 4048488 andKIC 4048494, KIC 5724810 and KIC 5724811, and KIC 3457431 andKIC 3457434. Less clear contamination is seen for KIC 4937255 andKIC 4937257, and KIC 10035772 and KIC 10035775, which are starsthat show no obvious periodic variable signals.
have only or mainly frequencies lower than 5 d−1. However, theclassification of pure γDor stars is not as straightforward, be-cause several other physical processes and phenomena can giverise to variability on similar timescales, such as binarity androtational modulation caused by migrating star spots. We triedour best to select only γDor stars, but are aware that nonethe-less, and most likely, our selection is contaminated with a fewnon-bona fide γDor stars. For stars that were observed in non-consecutive Kepler quarters, we tried to beware of frequenciesintroduced by the spectral window. For instance, frequently apeak near 48 d−1 (555 μHz) is detected (e.g. KIC 2166218 andKIC 7798339), which for a γDor pulsator can result in an incor-rect classification as hybrid star.
In Figs. 3−5 a portion of the light curve with a time spanof 2 d (δSct stars) or 5 d (γDor and hybrid stars) and a schematicoverview of the detected independent frequencies (i.e. combina-tion frequencies are filtered out in an automated way, see above)are given for a few representative stars of each group. The am-plitudes and Kepler flux are expressed in ppm, and the frequen-cies are given in both d−1 (bottom X-axis) and μHz (top X-axis).The dotted grey line in the amplitude spectra separates the δSctand γDor regime. The dates are in the Heliocentric Julian Date(HJD) format HJD0 = 2 454 950.0. The figures illustrate the va-riety of pulsational behaviour within the groups. The δSct stars(Fig. 3) display an impressive variety of amplitude heights. Thevariability of the stars in panels (d) and (e), KIC 9845907 andKIC 9306095, respectively, is dominated by one high-amplitudefrequency. Several lower amplitude variations are also present.The chance of confusing a high amplitude δSct star (HADS)and binarity is high for KIC 9306095. The stars in panels (a)−(c)show multiperiodic variations with frequency amplitudes of sim-ilar size. The rotational frequency near 1.2 d−1 and its first har-monic of the star KIC 10717871 (panel c) could be mistaken forγDor-like frequencies. Because there are no other longer-termperiodicities, there is no evidence for the possible hybrid statusof this star.
The light curves of γDor stars (Fig. 4) vary from obvi-ous beat patterns to less recognizable variable signals. Balonaet al. (2011d) already pointed out that there are symmetric(e.g. panel d) and asymmetric (e.g. panel e) light curves amongthe stars that show obvious beating, and that most likely in thesecases the pulsation frequencies are comparable to the rotationfrequency. Balona et al. (2011d) also suggested that the moreirregular light curves likely stem from slowly rotating stars.
Examples of hybrid stars are given in Fig. 5. The greydotted line in the right panels guide the eye to separatethe δSct and γDor regimes. The stars KIC 3119604 andKIC 2853280 (panels a and b, respectively) are clearly dom-inated by δSct frequencies, while the γDor frequencies havelower amplitudes. The star KIC 9664869 (panel c) is an ex-ample of a star that exhibits frequencies with amplitudes ofcomparable height in the two regimes. The highest peak in theγDor region is most likely related to the stellar rotation pe-riod, however, because several harmonics are also observed. Thebottom two panels are examples of hybrid stars dominated byγDor periodicities.
Table 3, available in the on-line version of the paper, presentsan overview of the stars assigned to the three groups. For eachstar (KIC ID) we provide the classification (Class), the to-tal number of independent frequencies (N) detected above thesignificance level (fap = 0.001) and with amplitudes higherthan 20 ppm, and the number of independent frequencies de-tected in the γDor and δ Sct regime (NγDor and NδSct, respec-tively). The next column gives as a reference the total number
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Fig. 3. Light curve and frequency spectrum of five stars assigned to the δSct group, illustrating the variety of pulsational behaviour within thegroup. The left panel shows a portion of the Kepler light curves. The Kepler flux is expressed in ppm, HJD is given in d with respect to HJD0 =2 454 950.0. The right panel gives a schematic representation of the detected independent frequencies, expressed in d−1 (bottom X-axis) or μHz(top X-axis). Amplitudes are given in ppm. The dotted grey line separates the δ Sct and γDor regime. Note the different Y-axis scales for each star.a) KIC 8415752; b) KIC 8103917; c) KIC10717871; d) KIC 9845907; e) KIC 9306095.
of frequencies detected above the significance level, includingcombination frequencies and harmonics (Ntotal). The next fourcolumns denote the frequency range of peaks in the γDor andδSct regimes ((Freq Range)γDor and (Freq Range)δSct, expressedin d−1), the highest amplitude (Amplitudehigh, expressed in ppm)and associated frequency (Freqhigh, in d−1). In the last column aflag (•) indicates if the risk on light contamination with a neigh-bouring star on the CCD is high (contamination factor >0.15).A typical error on the frequency associated with the highest am-plitude is 0.0001 d−1. The error on the amplitude ranges froma few ppm up to about 30 ppm. We note that for stars identi-fied as γDor or δ Sct stars we report on frequencies up to 6 d−1
or from 4 d−1, respectively, to account for, for instance, the fre-quency spectrum of more evolved stars.
We note that for several stars classified as γDor star onlyLC data are available. This may create a selection effect, be-cause short-term δ Sct periods are more difficult to detect in theshort timestring of LC data owing to sampling restrictions. Also,as mentioned above, even though we carefully checked the starsone by one, we expect to have a few false positive detections ofhybrid and γDor stars because the typical γDor frequencies canbe easily confused with variations of the order of a day caused
by rotation or binarity. A more careful analysis and interpreta-tion of the full frequency spectrum of all individual stars of thesample will clarify this matter, but this is beyond the scope ofthis paper.
We compared our classification with the automated super-vised classification results presented by Debosscher et al. (2011).Because these authors studied public Kepler Q1 data, only479 objects of our sample appear in their catalogue. We point outthat the classifier by Debosscher et al. (2009) only takes three in-dependent frequencies with the highest amplitudes into account.Hence, the recognition and classification of hybrid behaviouris currently not implemented. Moreover, because the classifierdoes not take external information into account that can distin-guish between B-type stars and A-F type stars (e.g. colour infor-mation, spectral classification based on spectra), there is oftena confusion between δSct and βCep stars, and between γDorand SPB stars. In general, there is good agreement (>87%, clas-sified in terms of δ Sct or βCep stars) with the classification byDebosscher et al. (2011) for stars that we classified as δ Sct stars.The γDor stars, as we classified them, are in general less eas-ily recognized by the automated classifier. Often they appearas “miscellaneous” in their list. This is not surprising, because
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Fig. 4. Similar figure as Fig. 3, but for five candidate γDor stars. Note the different X-axis scale with respect to Fig. 3. a) KIC 1432149;b) KIC 5180796; c) KIC 7106648; d) KIC 8330056; e) KIC 7304385.
so far only a few high-quality light curves of well-recognizedγDor stars were available that could be used as a template tofeed the classifier. Stars that we identified as hybrid stars appearin the catalogue by Debosscher et al. (2011) as “miscellaneous”or as δ Sct, γDor, βCep, or SPB stars. The work presented in thispaper will provide valuable feedback and information to refinethe automated supervised classification procedure developed byDebosscher et al. (2009).
6.2. Other classes
About 63% of our sample is recognized as δ Sct, γDor, or hy-brid star. Table 4, in the on-line version of the paper, gives anoverview of the “classification” of the remaining 37% of thestars. For each star (KIC ID) the associated classification (Class)and a flag (Flag) indicating a high risk on light contamination bya neighbouring star (• if there is a contamination factor >0.15),are given. Table 4 includes stars that show no clear periodic vari-ability on timescales typical for δSct and γDor pulsators (“. . . ”,or “solar-like”), stars that exhibit stellar activity and show a ro-tationally modulated signal (“rotation/activity”), binaries (“bi-nary” or eclipsing binary “EB”), B-type stars (“Bstar”), can-didate red giant stars (“red giant”), Cepheids (“Cepheid”), andstars whose light is contaminated by another star (“contami-nated”). Although the observed ranges in Teff and log g includetypical values for RR Lyr stars (see Fig. 2), we did not find any
in our sample, but there are ∼40 such stars observed by Kepler,which are studied separately (Kolenberg et al. 2010; Benko et al.2010). Unclear cases mostly show a behaviour that might be re-lated to rotation and are hence also labelled “rotation/activity”.We also assigned the candidate γDor stars for which less thanthree significant peaks were detected to this category. The lightcurve and frequency spectra of a few examples of these otherclassifications are given in Figs. 6 and 7.
One hundred and twenty-one stars do not show an obvi-ous periodicity in the expected range for γDor and δSct stars,or have an unresolved frequency spectrum within the availabledataset. The star KIC 9386259 (Fig. 6, panel a) is an example ofa star showing no clear periodicity. Furthermore, we used the la-bel “. . . ” for some stars for which less than three significant fre-quencies were detected (e.g. KIC 11509728 and KIC 11910256).We investigated the stars for signatures of solar-like oscillationsand identified 75 candidate solar-like oscillators (“solar-like”,see Table 4).
We identified seven B-type stars and 44 red giant stars in thesample. The giant stars show an envelope of frequencies withamplitudes up to 100−200 ppm in the region 0.5−5 d−1, as il-lustrated by KIC 2584202 (Fig. 6, panel b). Among the B-typestars, we recognized five SPB stars and one candidate βCep star.
Within the sample we identified at least 39 binaries, includ-ing 28 EBs. In Table 4 the binary stars are labelled “binary”,or “EB” for an EB. If the variability of one of the components
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Fig. 5. Similar figure as Fig. 3, but for five candidate hybrid stars. a) KIC 3119604; b) KIC 2853280; c) KIC 9664869; d) KIC 9970568;e) KIC 3337002. The two top panel a)−b) are δSct frequency-dominated stars, and the two bottom panels d)−e) are γDor frequency-dominatedstars.
is identified as typical for one of the three groups outlinedin Sect. 6.1, we also indicated this in Table 4. Panels (c)−(e)of Fig. 6 show examples of EBs. An interesting target isKIC 11973705, because it most likely is a binary with a δSctand SPB component (see also Balona et al. 2011b). For threestars reported in the literature as EBs (Prša et al. 2011; Slawsonet al. 2011; Hartman et al. 2004), KIC 2557115, KIC 5810113,and KIC 1432149, we find no clear evidence of their eclipsingnature in the Kepler lightcurves. In case of KIC 1432149, pre-sented by Hartman et al. (2004) as an EB with period 9.3562 d,we cannot confirm its eclipsing nature or its orbital period, andwe suspect that this target has been misidentified as an EB.
Several stars show an irregular light curve typical of stellaractivity, or a clearly rotationally modified signal (panels (a)−(c)of Fig. 7). It is also not impossible that low-amplitude pulsat-ing γDor star candidates are hidden among the stars labelledas “rotation/activity” in Table 4. Namely, when only one or twoof their pulsation frequencies reach the current detection thresh-old, they are not yet assigned to a pulsation group. A possibleγDor candidate is given in panel (d) of Fig. 7.
In some cases the light curves look very peculiar, andthe origin of the variability is not clear. This is the casefor KIC 3348390 (panel (e) of Fig. 7) and KIC 4857678,for instance.
We discovered several interesting targets among the 750 starsof the sample. Dedicated studies of groups of individual starswill be presented in forthcoming papers. Below, we will sort thestars into different classes.
7. Characterization of the different classes
The classification described in the previous section results inthe following distribution. A total of 63% of the sample can beidentified as γDor, δSct or hybrid stars: 27% are classified asδSct stars (206 stars), 23% as hybrid stars (171 stars; of which115 stars are δSct-dominated and 56 stars are γDor-dominated),and 13% as γDor stars (100 stars). A striking result is that al-most a quarter of the sample, i.e. 171 stars, shows hybrid be-haviour. This is in sharp contrast with the results obtained fromground-based observations, where so far only three candidateγDor-δSct hybrid stars have been discovered. The far superiorprecision of the space data opens a new window in detectinglow amplitude variations. This result was already hinted at byGrigahcène et al. (2010) and Hareter et al. (2010), but the quan-tification by means of this sample is remarkable.
Of the remaining 37% of the sample, a considerable number(121 stars, 16%) do not show clear variability with periods in theexpected range for γDor and δSct stars. Among this group are
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Fig. 6. Similar figure as Fig. 3, but for stars that were not assigned to the groups of δ Sct, γDor or hybrid stars. a) KIC 9386259, no clear periodicsignal detected; b) KIC 2584202, red giant star; c) KIC 5197256, EB or ellipsoidal variable with a δSct component; d) KIC 3230227, EB with aγDor component; e) KIC 9851142, EB with most likely a γDor component.
75 candidate solar-like oscillators. Our sample has seven B-typestars (1%) and 44 stars (6%) are identified as red giant stars.One Cepheid turned out to be among the sample. About 8% ofthe sample shows stellar activity, often manifesting itself by arotationally modulated signal.
At least 5% of the sample stars are identified through theanalysis of their light curve as binary or multiple systems, ofwhich 3.5% show eclipses. When we also consider the knownbinaries from the literature (Table 1), we arrive at a binary rateof 12% within the sample. The number of binary detectionsis only a fraction of what is expected. The binary rate amongA-F type stars in general and δSct stars in particular is estimatedto be at least 30% (Breger & Rodríguez 2000; Lampens & Boffin2000). Several additional stars are expected to be part of multi-ple systems with possibly much longer periods than the availableKepler time span. The percentage of EBs in our sample is high.Prša et al. (2011) reported a 1.2% occurence rate of EBs amongthe Kepler targets.
Figure 8 shows the stars that are not assigned to one of theδSct, γDor or hybrid star groups in a (Teff, log g)-diagram. Thesolid thick black and light grey lines mark the blue and red edgeof the observed instability strip of δ Sct and γDor stars, respec-tively (Rodríguez & Breger 2001; Handler & Shobbrook 2002).Owing to the possibly incorrect separation of the binary com-ponent’s contribution, we considered the physical parameters of
the binaries as insufficiently constrained and omitted them. Thesame holds for the B-type stars, which are much hotter than theTeff region shown here. The stars that show no clear periodicvariability on timescales typical for δSct and γDor pulsators(open triangles) and stars that exhibit stellar activity (bullets)are found along the MS and in more evolved stars. The loca-tion of the only Cepheid in our sample is marked by a cross.The candidate red giants (open squares) are all but one found inthe expected region of the (Teff, log g)-diagram. This implies thatthe KIC photometry separates giant from MS stars well.
7.1. Characterization of stars that show no clear periodicvariability
We now focus on the properties of the 121 stars that show noclear periodic variability in the γDor and δSct range of frequen-cies to understand why no oscillations are detected. Figure 9presents the distribution in Teff (top left), log g (top right),Kp (bottom left), and total time span ΔT , expressed in d, of theKepler light curves (bottom right).
The cool boundary of the observational instability strip forγDor stars is located around Teff = 6900 K. At least4 78% ofthe 121 stars have cooler temperatures, and hence no A-F typevariability is expected. About 75 stars are identified as candidate
4 For 11% of the 121 stars we have no information on Teff or log g.
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Fig. 7. Similar figure as Fig. 3, but for stars that were not assigned to the groups of δSct, γDor or hybrid stars. Stellar activity/rotational modula-tion: a) KIC 8748251; b) KIC 8703413 and c) KIC 11498538; no clear classification: d) KIC 12062443; and e) KIC 3348390.
solar-like oscillators. However, 10% of the 121 stars that showno clear periodicity are located inside the instability strip ofγDor or δSct stars5 (see also Fig. 8). Additional investigation isneeded to confirm that these stars do not show variability, whichwould imply that non-variable stars exist in the instability strip.
Sixty percent (71 stars) of our non-variable stars are fainterthan Kp = 12 mag, and 18% are fainter than Kp = 14 mag.The faintness of the star most likely has an impact on the(non-)detection of periodicities. To quantify this, we countedthe fraction of apparently non-periodic stars per magnitude binfor the full sample of 750 stars. The number of stars thatshow no clear peridodicity increases dramatically towards faintstars: the fraction is only 2% for magnitude Kp = 9 mag, 5% forKp = 10 mag, 12% for Kp = 11 mag, 15% for Kp = 12 mag,41% for Kp = 13 mag, and 68% for Kp > 14 mag. The fainterthe star, the more difficult it becomes to detect periodicities. Ouranalysis results, which were obtained by only considering am-plitudes above 20 ppm, lead us to suspect that the Kepler detec-tion limit of A-F type low-amplitude oscillations (≤20 ppm) liesaround Kp = 14 mag (see also Sect. 7.2).
We find no evidence for a selection effect towards stars witha short time span in the available Kepler time series. The rightpanel of Fig. 9 shows that also several time series with long time
5 As demonstrated in Sect. 7.2, a revision of the current instability stripis required.
spans do not show clear variability. Also, the observing modehas no obvious influence on the (non-)detection of oscillations.Fifty-four percent of the 121 stars have only LC data, while 46%have only SC data.
To summarize, stars that show no clear periodic variationsare generally the cooler and fainter stars of the sample. We donot find evidence for a bias towards the total time span of theavailable light curve or towards the observing mode (LC ver-sus SC).
7.2. Characterization of δSct, γDor, and hybrid stars
7.2.1. The (Teff, log g)-diagram
The current ground-based (GB) view on the positions of theδSct and γDor classes in the (Teff, log g)-diagram (parame-ters are taken from the literature6) is presented in panel (a) ofFig. 10. A comparison of log g values derived from Geneva pho-tometry and from other sources (photometry and spectroscopy)
6 Rodríguez & Breger (2001); Rodríguez et al. (2000); Henry & Fekel(2005); Poretti et al. (1997); Breger et al. (1997); Zerbi et al. (1997,1999); Aerts et al. (1998); Kaye et al. (1999b); Gray & Kaye (1999);Eyer & Aerts (2000); Guinan et al. (2001); Aerts (2001); Martín et al.(2003); Mathias et al. (2004); Rowe et al. (2006); Bruntt et al. (2008);Cuypers et al. (2009); Uytterhoeven et al. (2008); Catanzaro et al.(2010, 2011).
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Fig. 8. (Teff , log g)-diagram with stars that show no clear periodic vari-ability on timescales typical for δSct and γDor pulsators (open trian-gles), stars identified as red giants (open squares), stars that exhibit stel-lar activity (bullet), and a Cepheid (cross). The cross at the right topcorner represents the typical error bars on the values: 290 K for Teff
and 0.3 dex for log g. The solid thick black and light grey lines markthe blue and red edge of the observed instability strips of δ Sct andγDor stars, as described by Rodríguez & Breger (2001) and Handler &Shobbrook (2002), respectively. In the on-line version of the paper theopen squares, open triangles, bullets, and crosses, are red, blue, black,and black, respectively.
Fig. 9. Distribution in Teff (top left), log g (top right), Kepler magni-tude Kp (bottom left), and total time span ΔT of the Kepler light curves(bottom right) of the 121 stars that show no clear periodic varibility. Thenumber of stars belonging to each bin is given on the Y-axis.
indicates a systematic difference of about 0.4 dex for log g val-ues above 4.35 dex as calculated from the Geneva photometry(Cuypers & Hendrix, priv. comm.). Therefore we have correctedthe values based on Geneva photometry. Evidently, the δSct andγDor stars occupy distinct locations in the (Teff, log g)-diagram,with a small overlap region.
Panel (b) of Fig. 10 shows a different picture. Here the δSct,γDor, and hybrid stars from the Kepler sample are plotted. Weused the adopted values of Teff and log g, as given in Table 2. Thecross in the top right corner of the figure shows typical errors onthe values. The stars are scattered in the (Teff, log g)-diagram: theδSct and γDor stars are not confined anymore to the two re-gions that were clearly seen for the ground-based stars. Evenwhen considering the large error bars on the values, the scatter is
present. Kepler δSct stars exist beyond the red edge of the insta-bility strip, while Kepler γDor pulsations appear in both hotterand cooler stars than previously observed from the ground. TheKepler hybrid stars occupy the entire region between the blueedge of the δSct instability strip and the red edge of the γDor in-stability strip, and beyond. The position of the Kepler δ Sct andγDor stars suggests that the edges of the so far accepted observa-tional instability strips need to be revised. However, we need ac-curate values of Teff and log g for all stars to confirm this finding.
Because for most stars in our sample only KIC-based es-timates of Teff and log g are available, we selected the stars thathave reliable estimates of these parameters derived from ground-based spectra or multi-colour photometry (see Sect. 3). Fromthis selection, 69 are classified as belonging to one of the threegroups. The subsample of 69 stars is plotted in panel (c) ofFig. 10. The position of the stars in the (Teff, log g)-diagramconfirms the general findings described for the full sample.However, the scatter across the diagram of γDor stars is lesspresent, but almost all γDor candidates lie outside the obser-vational instability strip for γDor stars. Ground-based observa-tions for the derivation of more precise values of Teff and log gare needed for all other stars to confirm the exact locations ofthe stars.
Panel (d) of Fig. 10 shows the Kepler stars assigned tothe three groups that have amplitudes higher than 1000 ppm(see Table 3), which approximately corresponds to amplitudeshigher than 1 mmag and hence might be observable from theground. We notice that the Kepler stars with ground-based ob-servable amplitudes also do not fit within the observational in-stability strips.
The left column of Fig. 11 presents an overview of the dis-tribution in Teff for the three groups of A-F type stars. The his-tograms related to δ Sct, hybrid, and γDor stars are colouredin dark grey, middle grey, and light grey respectively. The dis-tribution in Teff peaks around 7400 K, 7200 K, and 7000 Kfor δSct, hybrid, and γDor pulsators, respectively. Comparingthese values with the center of the observed instability strips byRodríguez & Breger (2001) and Handler & Shobbrook (2002),we find that a large part of the Kepler stars are concentrated nearthe overlap of the two instability strips, and that many mem-bers of the three groups coincide in the same region in the(Teff, log g)-diagram. It will be interesting to investigate whystars with similar values of Teff and log g in some cases pulsateas a δ Sct star, and in others as a γDor star, or as both. Anotherinteresting and puzzling result is that γDor and δSct pulsationsseem to be excited in a far wider range of temperatures then pre-viously expected.
The distribution in log g is similar for all classes. Most starshave log g values between 3.5 dex and 4.3 dex, with a peakaround log g = 3.9 dex. We point out that the log g values de-rived from the KIC for A-F type stars are known to have largeuncertainties, and only few stars have measurements from othersources. Without more stars with accurate values derived fromground-based observations we cannot draw any conclusions.
The distribution in Kepler magnitude Kp (bottom left,Fig. 2) is representative for the distribution in Kp for γDor andδSct stars. It illustrates that the cut-off magnitude for the detec-tion of γDor and δSct type of variations with Kepler lies aroundKp = 14 mag. The majority of the sample stars have magnitudesin the range Kp = 10−12 mag.v sin i values are available for 41 stars of the subsam-
ple consisting of δSct, γDor and hybrid stars (see Table 2).Of the five γDor stars, four have v sin i values above 90 km s−1,and one has v sin i = 15 km s−1. Of the sixteen δ Sct stars,
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Fig. 10. a) (Teff , log g)-diagram of the δSct, γDor, and hybrid stars detected from the ground (parameters taken from the literature).b) (Teff , log g)-diagram of the Kepler stars we classified as δ Sct, γDor, and hybrid stars in this paper. Open squares represent δSct stars, as-terisks indicate γDor stars, and hybrid stars are marked by bullets. The black cross in the right top corner shows typical errors on the values.c) (Teff , log g)-diagram of the subsample of 69 Kepler stars for which accurate Teff and log g values are available. The colour-codes are the sameas for panel b). d) (Teff , log g)-diagram of the subsample of Kepler stars that show pulsations with amplitudes higher than 1000 ppm (>1 mmag).Evolutionary tracks for MS stars with masses 1.4 M�, 1.7 M�, and 2.0 M� are plotted with grey dotted lines. The evolutionary tracks have beencomputed using the Code Liégeois d’Évolution Stellaire (CLES, Scuflaire et al. 2008). The input physics included is similar to the one used inDupret et al. (2005) with the following values for the modelling parameters αMLT = 1.8, αov = 0.2 and Z = 0.02. The solid thick black and lightgrey lines mark the blue and red edge of the observed instability strips of δSct and γDor stars, as described by Rodríguez & Breger (2001) andHandler & Shobbrook (2002), respectively. In the on-line version of the paper the symbols representing the δ Sct, γDor, and hybrid stars are red,blue, and black, respectively.
eight stars have high v sin i values, six have moderate val-ues (40 < v sin i < 90 km s−1), and two low values(v sin i < 40 km s−1). Of the 20 hybrid stars almost allhave high v sin i values, with six stars having v sin i valuesabove 200 km s−1. Extrapolating these numbers to the full sam-ple, we expect that many stars in the sample are moderate-to-fastrotators.
7.2.2. Frequencies and amplitudes
Up to 500 non-combination frequencies are detected in theKepler time series of a single star (see Table 3). These largenumbers of frequencies are in sharp contrast with the small num-ber of frequencies observed from the ground, e.g. up to 79 pul-sation and combination frequencies for the δSct star FG Vir(e.g. Breger et al. 2005) and up to 10 frequencies in the γDor hy-brid candidate HD 49434 (Uytterhoeven et al. 2008), but are
commonly seen in space observations because of their higherprecision and sensitivity to low-amplitude variations (e.g. Porettiet al. 2009; García Hernández et al. 2009; Chapellier et al. 2011).However, it needs to be carefully checked whether all of the ap-parent individual frequencies are of pulsational origin.
For the majority of stars (66%), less than 100 frequencieswere found, and 10% of the stars show variations with more than200 frequencies. If we look at the extreme cases we find that for29 stars (6%) fewer than 10 frequencies were detected, while for5 stars (1%) more than 400 frequencies were found. The middlepanel of Fig. 11 shows the distribution of the number of detectedfrequencies for the δSct (top, dark grey), hybrid (middle, middlegrey), and γDor (bottom, light grey) stars. The highest numberof frequencies are found for hybrid stars. It is worth mentioningthat the number of detected frequencies versus Teff follows a dis-tribution that peaks near 7700 K, 7500 K, and 7000 K for δSct,hybrid, and γDor stars, respectively. More modes are excited
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Fig. 11. Distribution in Teff (left column), number of detected (independent) frequencies (middle column) and highest amplitude (ppm, in logarith-mic scale) (right column), for the three groups of A-F type stars: δ Sct stars (top; dark grey), hybrid stars (middle; middle grey), and γDor stars(bottom; light grey). The number of stars belonging to each bin (N) is indicated on the Y-axis.
near the centre of the δSct instability strip. For the hybrid andγDor stars most detected frequencies are found towards the rededge of the (overlap in the) instability strip.
The right panel of Fig. 11 shows the distribution ofthe highest measured amplitude in ppm logarithmic scale(log(Amplitude)) for the different groups using the same colour-code as before. The range in highest amplitude measured is 40 to155 000 ppm. For about 59% of the stars the highest amplitudeis lower than 2000 ppm. Only 16 stars (3.5%) show variabilitywith highest amplitudes below 100 ppm, while 26 stars (5%)have amplitudes above 10 000 ppm. In general, higher ampli-tudes are detected in δSct pulsators than in γDor stars. We pointout that the origin of high peaks detected in γDor stars, e.g. theamplitude of 23 000 ppm in the star KIC 7304385, is most likelyrelated to the rotation of the star. It is worth mentioning thatamplitudes above 10 000 ppm are also detected in faint targets.The highest amplitudes are found for stars within the tempera-ture range Teff = 6600−7100 K, which is the cool part of theinstability strips.
We detected δSct frequencies between 4 and 80 d−1. Wefound indications that a handful of stars vary with even shorterperiods. However, these short periods need to be confirmed bymeans of a careful investigation of the specific frequency spec-tra, which is beyond the scope of this paper.
When considering the δ Sct stars and hybrid classes, whichamount to atotal of 375 stars, we find that 56% shows an upperfrequency limit between 40 and 70 d−1. Only 10% of the δSct
and hybrid stars have frequencies up to 80 d−1, and 9% onlyshow variations with frequencies lower than 20 d−1. We note thatγDor-dominated hybrids that show variations with frequencieshigher than 60 d−1 are rare (three stars in our sample).
The majority of the hybrid stars detected in the Kepler datashow all kinds of periodicities within the γDor and δSct range(see Cols. 6 and 7 in Table 3 which give the frequency range ofthe detected frequencies in the γDor and δSct domains). Thisobservational fact is interesting because from a theoretical pointof view no excited modes are expected between about 5 and10 d−1, i.e. the so-called “frequency gap” (see, e.g. Grigahcèneet al. 2010). Only for five hybrid stars a “frequency gap” is ob-served7. Possible explanations for the absence of gaps, within thepresent non-adiabatic theories, are that the frequencies withinthe gap are high-degree and/or rotationally split modes (Bouabidet al. 2009).
8. A first step towards understanding the relationbetween δSct, γDor, and hybrid stars
As presented in the previous section, it is not trivial to distin-guish between the three groups of variable A-F type stars de-fined in Sect. 6.1. The relation between the three groups is cur-rently unclear as well because δSct, γDor, and hybrid stars
7 The six hybrid stars that show a “frequency gap” are: KIC 3851151,KIC 4556345, KIC 7770282, KIC 9052363, and KIC 9775454.
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coincide in the (Teff, log g)-diagram (Fig. 10). Driven by the ideato find observables based on physical concepts that allow insightin the different internal physics of the three types of stars, weconstructed two new observables that can provide an alterna-tive way to improve our understanding of the relation betweenthe three groups. We point out that several observational pa-rameters can be found that reflect the different inherent prop-erties of the three groups in one way or another. For instance,δSct stars pulsate with shorter periods, and are generally hot-ter than γDor stars. A combination of these parameters willlead to a differentiation of the groups, such as for instancea (Teff, fmax)-diagram, with fmax the frequency associated to thehighest amplitude mode. However, we emphasize that our aimis to find observables that can be directly related to the internalphysics of the stars.
According to the current instability theories, which need tobe revised following the results presented in this work, the maindriving process of the oscillations in δSct stars is related to theopacity variations in the ionization zones (Unno et al. 1989).These zones are located in the region where the main energytransport mechanism is convection and where a small quantity ofenergy is transported by radiation. The total amount of drivingenergy going into the mode is directly related to the radiative lu-minosity in this zone, and this latter quantity is a function of theconvective efficiency. Therefore, we expect a relation betweenthe energy of the observed modes and the convective efficiencyof the outer convective zone. We searched for this relation andconstructed two observables, energy and efficiency, that are es-timates of the energy and the convective efficiency, using theavailable observational data.
8.1. Energy
The kinetic energy of a wave is given by
Ekin =12
f (ρ∗)(Aζ)2, (2)
where f is a function of the stellar density ρ∗, A is the ampli-tude of the oscillation, and ζ is the pulsation frequency. Usingthe available observational data, we construct the following ob-servable that we call energy, which is a first approximation andestimate of the kinetic energy of the wave:
energy ≡ (Amaxζmax)2, (3)
where Amax and ζmax refer to the highest amplitude mode of thestar (in ppm), and associated frequency (in d−1). The pulsationamplitude is a function of the observed amplitude and the rela-tive variation of the flux, and is given by the expression (Moya& Rodríguez-López 2010):
ΔR/R = − Δmln(5 + 10dT )
, (4)
where ΔRR is the relative pulsational amplitude, Δm the observed
magnitude variation of the mode, and dT is given by
dT =δTeff
Teff/ξrr, (r = R), (5)
with ξr the variation in radius of the mode, and dT is evaluatedat the surface of the star (r = R).
Non-adiabatic calculations of a representative model of a hy-brid pulsating A-F type star including time dependent convec-tion (Grigahcène et al. 2005) show that the difference between
Fig. 12. Distribution in log(energy) (right), and log(efficiency) (left) forthe δSct (top, dark grey), hybrid (middle, middle grey), and γDor (bot-tom, light grey) stars. The number of stars belonging to each bin (N) isindicated on the Y-axis.
the predicted dT value of asymptotic g-modes (γDor stars) andlow-order p-modes (δSct stars) is around one order of magni-tude or less, where the δSct stars have higher values. Therefore,we can directly use the observed magnitude variation as a mea-surement of the radial amplitude variation. That we are using anapproximation does not change the conclusions of the presentstudy, because the observed differences are larger than two or-ders of magnitude (see Figs. 12 and 13).
The right column of Fig. 12 shows the distribution inlog(energy) for the δSct (top, dark grey), hybrid (middle, middlegrey), and γDor (bottom, light grey) stars. Clearly, the weight ofthe distribution is located in the region log(energy) > 8 for starsdominated by frequencies in the δ Sct domain, and in the regionlog(energy) < 8 for stars with dominant γDor pulsations.
8.2. Efficiency
In the introduction of this section we pointed out that a relationbetween the convective efficiency and mode excitation can exist.Recent studies on convective efficiency of the outer convectivezone of F-G-K stars using 3D models show that the convectiveefficiency is related to the position of the star in the Hertzsprung-Russell (HR-) diagram (Trampedach & Stein 2011). To constructan observable related to the convective efficiency that can bedescribed with only variables related with the position in theHR-diagram, we found inspiration in the analytic descriptionof the convective energy given by the mixing length theory8
8 In analogy to the mean free parameter in gas kinetic theory, the mix-ing length is defined as the mean distance over which a fluid bulb con-serves its properties. Generally, the mixing-length is assumed to be pro-portional to the pressure-scale height by a factor α that is usually calledmixing-length parameter.
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Fig. 13. Observable log(energy) plotted versus log(efficiency) for δSct (open squares) and γDor (asterisks) stars only (top), and for hybrid starsas well (bullets) (bottom). The left panels include all 480 Kepler stars that are assigned to one of the three groups. The right panels show the49 stars for which reliable values of Teff and log g are available. In the on-line version of the paper the symbols representing the δSct, γDor andhybrid stars are red, blue, and black, respectively. The cross in the right bottom corner of the top left panel represents the typical error bars on thevalues: 0.04 dex and 0.12 dex for log(energy) and log(efficiency), respectively.
(Böhm-Vitense 1958). There, the convective efficiency,Γ, isdefined as
Γ =
[A2
a0(rad − )
]1/3
, (6)
with a0 a constant, rad and the radiative and real temperaturegradient, respectively, and
A ∼ cpκpρcsα2
9σT 3g√
2Γ1(7)
(see Cox & Giuli 1968).This quantity, which measures the ratio between the convec-
tive and radiative conductivity, depends on a large number ofphysical variables: the specific heat capacity at constant pres-sure cp, the opacity κ, the pressure p, the stellar density ρ, thesound velocity cs, the mixing length parameter α, the Stephan-Boltzmann constant σ, the temperature T , the gravity g, and thefirst adiabatic coefficient Γ1. Because we only have informationon a limited number of observational variables, our estimate of
the quantity is only an approximation. Inspired by these equa-tions, we searched for the combination of temperature and grav-ity that empirically provided the best means to separate betweenγDor and δSct stars (see statistical test below), and define theobservable efficiency as
efficiency ≡ (T 3eff log g)−2/3 ∼ Γ. (8)
Because the efficiency of the convective zone is expected to behigher for γDor stars than for δSct stars, the observable effi-ciency should have a higher value for γDor stars than δSct stars.This behaviour is indeed observed, as illustrated in the left panelof Fig. 12, where the distribution in log(efficiency) is given. Themajority of δSct stars have values log(efficiency) < −8.1 dex,while the histograms for γDor pulsators peak in the regionlog(efficiency) > −8.1 dex.
8.3. Efficiency versus energy
When we plot the two new observables, log(energy) versuslog(efficiency), the groups of δSct and γDor stars are fairlywell separated (see top panels Fig. 13). A log(energy) value
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of 8 leaves 90% of the δ Sct and γDor stars separated. Thebottom panel of Fig. 13 shows the same diagram with valuesfor the hybrid stars included, using the same colours and sym-bols as before. Typical errors on the values are 0.04 dex and0.12 dex for log(energy) and log(efficiency), respectively. Thehybrid stars are placed in the intermediate region. We observedthat δSct (γDor) dominated hybrids fall in the same region asthe δ Sct (γDor) stars.
We performed a Mann-Whitney U test with an adaptedp-value (p = 0.0166) according to the closed-test principle de-scribed in Horn & Vollandt (1995), to statistically investigate ifthe mean of the distribution in log(energy) and log(efficiency) isdifferent for the three different groups. The test shows that thedifference in the mean of the distributions in both log(energy)and log(efficiency) is statistically significant for all groups.However, the apparent separation in log(efficiency) becomes lessevident when we take the considerable error bars into account.We also performed a χ2 test (as described by Press et al. 1992) todetermine if the distributions themselves were different. All dis-tributions are statistically significant, save for the γDor versushybrid star efficiencies, where they are marginally similar. Thisconclusion holds even if we vary the Teff and log g values withinthe error ranges and recompute the efficiencies or vary the inputsinto the energies. We point out once again that the definitionof efficiency is only a rough estimate of the theoretical expres-sion for the convective efficiency, and might – at this stage – notbe refined enough to display the separating power between thegroups we expect the convective efficiency to have. In a follow-up investigation we will assess the goodness of approximationof our definition of efficiency by comparison with values of theconvective efficiency as given by Eq. (6), calculated for severalmodel stars, and finetune its definition.
The two new approximate observables energy and efficiencyreflect the different internal physics of oscillators with dominantδSct pulsations and oscillators dominated by γDor pulsations,and seem to allow us to distinguish between them. However,it needs to be further investigated if the two observables canbe considered as independent parameters. This, together with anexploration of the physical mechanisms behind the instabilityof these stars, is the topic of a forthcoming paper. The observ-ables energy and efficiency are promising starting points to ex-plore the relation between δSct, γDor and hybrid stars, but needto be refined.
9. Summary, discussion, and future prospects
We analysed the Kepler light curves based on survey phasedata with time spans between 9 d and 322 d available throughKASOC and associated frequency spectra of 750 candidateA-F type stars in search for δSct, γDor, and hybrid pulsators.The main results are:
– The Kepler light curves of the sample of 750 candidateA-F type stars show a variety in variability behaviour.
– Observationally, we propose three main groups to describethe observed variety: γDor, δ Sct, and hybrid stars. The lattergroup includes both δSct-dominated and γDor-dominatedhybrid stars. About 63% of the sample are unambiguouslyassigned to one of the three groups.
– About 23% of the sample are hybrid candidates (171 stars,or 36% of the stars assigned to the three groups). Thisis in strong contrast with the number of hybrid candi-dates so far observed from the ground, but compatiblewith the first Kepler study of γDor and δSct variables by
Grigahcène et al. (2010). The far superior precision of theKepler space data opens a new window in detecting low-amplitude variations. Kepler will be ideal to study hybrid be-haviour in different types of stars, such as roAp stars (Balonaet al. 2011a), sdB stars (Østensen et al. 2010), and B stars(Balona et al. 2011b).
– We presented a characterization of the stars in terms of num-ber of detected frequencies, frequency range, and typicalpulsation amplitudes, which provides valuable feedback formodels and instability studies. This is the first time that thiskind of information is available for a substantial sample ofstars. Up to 500 non-combination frequencies are detected inthe Kepler time series of a single star. The highest pulsationamplitude measured is 58 000 ppm. The shortest detectedδ Sct periods are about 18 min. We find that hybrid starsshow all kinds of periodicities within the γDor and δSctrange. In particular, the majority of hybrid stars shows fre-quencies between 5 and 10 d−1. From a theoretical point ofview, this result presents a number of challenges, because thecurrently accepted over-stability mechanisms cannot explainthe presence of pulsational modes in the wide frequencyranges observed with Kepler. It needs to be investigated ifand to what extent the presence of stochastic modes, high-degree, and/or rotationally split modes with high amplitudes,granulation and effects of convection can explain part of theunexpected observed modes.
– The location of γDor and δ Sct classes in the (Teff, log g)-diagram has been extended (Fig. 10). We find indications thatKepler δ Sct stars exist beyond the red edge of the observa-tional instability strip, while Kepler γDor pulsations seem toappear in both hotter and cooler stars than observed so far.The Kepler hybrid stars occupy the entire region betweenthe blue edge of the δ Sct instability strip and the red edge ofthe γDor instability strip and beyond. These results, if con-firmed by verification of the temperature and log g valuesin a more comprehensive sample, imply that the observa-tional instability strips need to be extended to accommodatethe Kepler δ Sct and γDor stars. From a theoretical pointof view, the overall presence of hybrid stars implies an in-vestigation of other pulsation mechanisms to supplement theκ mechanism and convective blocking effect to drive hybridpulsations.
– Two new “observables” that reflect the different internalphysics of δ Sct and γDor pulsators are introduced to in-vestigate the relation between the two types of pulsations(Fig. 13): (1) efficiency, related to the convective efficiencyof the outer convective zone, and a function of Teff and log g;and (2) energy, the driving energy of a mode, and a functionof the highest observed frequency amplitude and the associ-ated frequency. Both observables are empirical and are con-structed using only available measured variables. The im-pact and physical significance of the group separation in the(log(efficiency), log(energy))-diagram needs to be investi-gated in more detail. The two new observables are a promis-ing starting point for further investigations of the relation be-tween δ Sct, γDor and hybrid stars.
– Our study indicates that Kp = 14 mag is a cut-offmagnitudefor detection of variations with amplitudes below 20 ppm inA-F type stars with Kepler.
– Sixteen percent of the sample stars show no clear variabil-ity within the expected range of frequencies for δ Sct andγDor stars. Faint and cool stars predominate this sample.Among the stars, we identified 75 candidate solar-like stars.No correlation between non-variability and the length of the
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available dataset or the available cadence mode is found. Wefind indications for the presence of constant stars inside theinstability strips of A-F type pulsators.
– The remaining 21% of sample stars are identified as aCepheid, B-type stars, red giant stars, stars that show stellaractivity, or binaries. At least 12% of the sample are identi-fied as a binary or multiple system, based on investigationof the Kepler light curve or on input from the literature.Many long-period binaries are expected to be among the re-maining stars of the sample. 3.5% of the sample stars showseclipses. Several of the EBs have variable components, in-cluding δ Sct, γDor, and hybrid stars.
Clearly, space missions are changing the landscape of γDor andδSct pulsators. We aimed at a global analysis of the samplestars. A careful seismic analysis of individual stars is neededto confirm their classification, clarify the observed variety inpulsational behaviour, fully characterize the properties of theδSct, γDor, and hybrid groups, understand their relationship,clarify the driving mechanism(s) for each group, and elaborateon the variables energy and efficiency. The observational re-sults with Kepler presented here open up several new questionsand theoretical challenges for the current models related to pul-sational instability, thermodynamics, and stellar structure. Wemention here some topics for further investigation.
To be able to place the stars confidently in the (Teff, log g)-diagram, estimate the projected rotational velocity, and deriveaccurate abundances, at least one high-resolution spectrum isneeded for each star. To this end, an observational campaignis ongoing (Uytterhoeven et al. 2010a,b). Most stars of theδSct, γDor, and hybrid stars in our sample with magnitudeKp ≤ 10.5 mag have recently been observed or are scheduled tobe observed in the coming months. However, 70% of the stars inTable 3 are fainter than magnitude Kp = 10.5 mag, for which itis time-consuming and less practical to observe them with theavailable 2-m class telescopes that are equipped with a high-resolution spectrograph.
Because the oscillation modes in A-F type stars do not pro-duce evident frequency patterns in their mode spectra, as is thecase for solar-like oscillators, the identification of pulsationmodes benefits from high-resolution spectral or multi-colourtime series. Here we encounter limitations owing to the relativefaintness of the Kepler sample too. For instance, it is only fea-sible to efficiently spectroscopically monitor the few brightest(Kp ≤ 9 mag) stars from the ground, while multi-colour pho-tometry can go a few magnitudes fainter. Moreover, it will beimpossible with the current instrumentation to detect the pulsa-tion amplitudes of the order of a few μmag from the ground.Therefore, only for a limited selection of the stars in Table 3,i.e. bright stars exhibiting high-amplitude variations, will it befeasible to organize ground-based follow-up campaigns.
For all other stars, we will have to rely on extractinginformation on the pulsation modes directly from frequencypatterns observed in the Kepler data. Quasi-periodic patternshave been observed before in δSct stars (Handler et al. 1997;García Hernández et al. 2009). But in fast rotating stars therotation destroys regular frequency and period patterns ofp- and g-modes, which complicates the mode identification(e.g. Lignières et al. 2006; Ballot et al. 2010). For slowly rotat-ing g-mode pulsators (Vrot < 70 km s−1), a mode-identificationtechnique has been developed that relies only on accurate valuesof at least three frequencies (Frequency Ratio Method, Moyaet al. 2005; Suárez et al. 2005), which is ideal to apply tothe information extracted from the Kepler white light, without
colour or spectral information. Unfortunately, many of our starsare moderate-to-fast rotators (see Sect. 7.2). Hence, the modeidentification will be very challenging and will require moreinvestigation.
An individual analysis of the candidate hybrid stars is neededto confirm their hybrid status and to firmly characterize their pul-sation properties. The current theoretical instability models forhybrid stars need to be revised to be able to accommodate allstars that have been proposed as hybrid candidates in this pa-per. This includes a revision of the mechanisms that allow driv-ing of p- and g-modes in A-F type stars with a broad range oftemperatures. Additional processes that can be investigated withpossible effect on the driving are stochastic excitation (Houdeket al. 1999; Samadi et al. 2002), a convective driving mecha-nism similar to g-mode pulsations in white dwarfs (Goldreich &Wu 1999), a κ mechanism-related effect presented by Gautschy& Löffler (1996) and Löffler (2000), and radiative levitation(Turcotte et al. 2000). Asteroseismic diagnostics have been stud-ied to find signatures of stochastic mechanisms at the origin ofthe instability of γDor oscillators (Pereira et al. 2007). In thatwork, this possibility was not discarded, but continuous and pre-cise space data were not yet available. The Kepler time series ofthe sample of stars studied here will be an ideal new testbed forthis method.
The long, continuous time series that Kepler will deliver dur-ing its lifetime will unveil a large number of amplitudes at μmaglevel. This precision will open up opportunities to search forsignatures of granulation in the variable star light (Kallinger &Matthews 2010). Spectroscopically, convective signatures havebeen detected in the microturbulence and line broadening ofA-F type stars cooler than Teff = 10 000 K (Landstreet et al.2009).
Also the theoretical instability strips of the γDor andδSct pulsators need revision. As shown in Fig. 1, stars exhibitingpurely γDor or δSct pulsations seem to exist beyond the currentblue and red edge of the respective instability strips. Moreover, itis worth investigating if the evolutionary phase of γDor stars canbe derived from properties in their frequency spectra, as is re-cently suggested by Bouabid et al. (2011), based on a theoreticalstudy of seismic properties of MS and pre-MS γDor pulsators.
Another open question is the existence of non-variableA-F type stars inside the instability strips. So far, it is suggested(Poretti et al. 2003; Breger 2004) that all seemingly constantstars in the instability strip are low-amplitude pulsators. In thisstudy we find indications that non-variability exists within the in-stability strip, but a more in-depth investigation based on a morecomprehensive sample of stars with precise values of Teff andlog g is needed to confirm this.
Furthermore, candidate γDor stars with only a few exciteddominant modes deserve to be looked at in more detail. The re-lation between rotation and pulsations is not yet clear. Moreover,the differentiation between pulsations and rotational variabilityproves to be very difficult (Breger 2011; Monnier et al. 2010).In the pilot study by Balona et al. (2011d) it was suggestedthat pulsation and rotation periods might be very closely related.It needs to be investigated to which extent the rotation influencesthe excitation of the observed modes. To help this investigation,v sin i values are needed.
Constraints on important physical parameters that are cru-cial for seismic modelling, such as stellar radius and mass, canbe derived directly for pulsators in binary systems (e.g. Tangoet al. 2006; Desmet et al. 2010). Our sample consists of sev-eral binaries and eclipsing systems with (a) pulsating compo-nent(s) (see Table 4). Hence, these targets in particular are very
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promising for dedicated ground-based follow-up observations,and a seismic analysis. Moreover, it will be interesting to in-vestigate the effect of tidal interactions on pulsation frequencies(e.g. Uytterhoeven et al. 2004; Derekas et al. 2011).
Four of the EBs with a candidate γDor, δSct, or hybrid com-ponent in our sample are known as chemically peculiar stars(see Table 1). Three candidate hybrid stars (out of 61 stars withknown spectral type), four candidate δSct stars (out of 67 stars),and one candidate γDor star (out of 25 stars) are also Ap orAm stars. So far, we detected both p- and g-mode pulsatorsamong the chemically peculiar stars. Balona et al. (2011c) statedthat the instability strip of pulsating Am type stars and δSct starsdo not differ much. With the current small number statistics, it isnot clear whether Ap/Am stars are indeed rare among γDor stars(Handler & Shobbrook 2002). One of the open questions is ifchemical peculiarity is related to hybridity. The first discoveredhybrid HD 8801 (Henry & Fekel 2005) intruigingly turned outto be an Am star. In a recent abundance study by Hareter et al.(2011) one of the two studied hybrid stars is also confirmed asbeing a chemically peculiar star. Together with the results of thisstudy, this brings the total of known chemically peculiar hybridstars to five. There is currently no evidence for a direct link be-tween chemical peculiarity and hybrid behaviour, but a carefulabundance analysis of a representative sample of hybrid stars isneeded to confirm this.
Many more (candidate) δ Sct, γDor, and hybrid stars are ex-pected to be among the stars observed by Kepler. Debosscheret al. (2011) reported the discovery of many additional δSctand γDor candidates in the public Kepler Q1 data. Also, a con-siderable fraction of the host stars of the recently published1235 Kepler planet candidates (Borucki et al. 2011) turn outto be A-F type stars. Hence, we have promising prospects instudying and understanding the A-F type star variable behaviourin detail through a much larger and more complete sample ofA-F stars in the Kepler field when longer timestrings of Keplerdata will become publicly available. Kepler is definitely openingthe window towards the accurate characterization of pulsatingA-F stars.
Acknowledgements. We are grateful to Joanna Molenda-Zakowicz, JamesNemec and the anonymous referee for their suggestions and comments toimprove this paper. Funding for the Kepler mission is provided by NASA’sScience Mission Directorate. We thank the entire Kepler team for the devel-opment and operations of this outstanding mission. K.U. acknowledges finan-cial support by the Deutsche Forschungsgemeinschaft (DFG) in the frame-work of project UY 52/1-1, and by the Spanish National Plan of R&D for2010, project AYA2010-17803. A.M. acknowledges the funding of AstroMadrid(CAM S2009/ESP-1496). E.N. and A.P. acknowledge the financial supportof the NN 203 405139 and NN 203 302635 grant, respectively, from theMNiSW. The work by G.H. and V.A. was supported by the Austrian Fonds zurFörderung der wissenschaftlichen Forschung under grant P20526-N16. L.F.M.acknowledge financial support from the UNAM under grant PAPIIT IN114309.R.Sz. and L.L.K. have been supported by the “Lendület” program of theHungarian Academy of Sciences and the Hungarian OTKA grants K83790 andMB08C 81013. RSz was supported by the János Bolyai Research Scholarship ofthe Hungarian Academy of Sciences. SH acknowledges financial support fromthe Netherlands Organisation for Scientific Research (NWO). This research hasbeen funded by the Spanish grants ESP2007-65475-C02-02, AYA 2010-21161-C02-02 and CSD2006-00070. The research leading to these results has receivedfunding from the European Community’s Seventh Framework Programme(FP7/2007-2013) under grant agreement No. 269194. This research has madeuse of the SIMBAD database, operated at CDS, Strasbourg, France, and is partlybased on observations obtained at the Observatorio Astrónomico Nacional-SanPedro Mártir (OAN-SPM), Baja California, Mexico, at the Observatoire deHaute Provence, France, and at the Thüringer Landessternwarte Tautenburg,Germany. We acknowledge with thanks the variable star observations from theAAVSO International Database contributed by observers worldwide and used inthis research.
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2 Kiepenheuer-Institut für Sonnenphysik, Schöneckstraße 6, 79104Freiburg im Breisgau, Germany
3 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife,Spain; Departamento de Astrofísica, Universidad de La Laguna,38205 La Laguna, Tenerife, Spaine-mail: [email protected]
4 Laboratorio de Astrofísica Estelar y Exoplanetas, LAEX-CAB(INTA-CSIC), PO BOX 78, 28691 Villanueva de la Cañada, Madrid,Spain
5 Centro de Astrofísica, Faculdade de Ciências, Universidade doPorto, Rua das Estrelas, 4150-762 Porto, Portugal
6 Los Alamos National Laboratory, XTD-2, Los Alamos, NM 87545-2345, USA
7 Instituto de Astrofísica de Andalucía (CSIC), Apartado 3004, 18080Granada, Spain
8 LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris-Diderot, 92195 Meudon, France
9 Valentian International University, Prolongación C/ José PradasGallen, s/n 12006 Castellón de la Plana, Spain
10 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK11 Institut für Astronomie, Türkenschanzstraße 17, 1180 Wien, Austria12 Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716
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14 Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11,51-622 Wrocław, Poland
15 Observatorio Astronómico Nacional, Instituto de Astronomía,UNAM, Ensenada B.C., Apdo. Postal 877, Mexico
16 CISAS, Padova University, via Venezia 15, 35131 Padova, Italy17 INAF - Astronomical Observatory of Padova, Vicolo Osservatorio
5, 35122 Padova, Italy18 UMR 6525 H. Fizeau, UNS, CNRS, OCA, Campus Valrose, 06108
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3001 Leuven, Belgium20 Konkoly Observatory of the Hungarian Academy of Sciences, 1525
Budapest PO Box 67, Hungary21 INAF - Osservatorio Astronomico di Capodimonte, via Moiariello
16, 80131 Napoli, Italy22 Lab. d’Astrophysique de Toulouse-Tarbes, Université de Toulouse,
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26 University of Birmingham, School of Physics and Astronomy,Edgbaston, Birmingham B15 2TT, UK
27 Department of Astronomy and Physics, Saint Marys University,Halifax, NS B3H 3C3, Canada
28 Observatoire de Genève, Université de Genève, 51 Ch. desMaillettes, 1290 Sauverny, Switzerland
29 Los Alamos National Laboratory, XCP-6, MS T-087, Los Alamos,NM 87545-2345, USA
30 Jeremiah Horrocks Institute of Astrophysics, University of CentralLancashire, Preston PR1 2HE, UK
31 Royal Observatory of Belgium, Ringlaan 3, 1180 Brussel, Belgium32 Department of Physics and Astronomy, University of Aarhus, bygn.
1520, Ny Munkegade, 8000 Aarhus C., Denmark33 Department of Astronomy, University of Texas, Austin, TX 78712,
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A125, page 21 of 70
A&A 534, A125 (2011)
Tabl
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2Q
0–Q
1..
.02
5571
1519
0659
.52+
3749
16.3
12.6
...
...
bina
ry38
460
9.5
0.0
Q0
...
0255
7430
1907
22.8
7+
3748
57.2
11.5
...
...
bina
ry36
3857
379
.64.
5Q
0–Q
1Q
2.1
0255
8273
1908
24.8
4+
3753
38.9
11.3
...
...
...
3846
429
2.5
219.
4Q
0–Q
1Q
4.2
0256
8519
1920
03.9
4+
3752
27.4
11.3
...
BD+
3734
18a
...
5980
432
1.4
4.9
Q0–
Q4
Q4.
102
5696
3919
2046
.80+
3750
13.8
10.6
...
Cl*
NG
C67
91S
BG
5986
NG
C67
9139
847
228.
815
8.6
Q0–
Q1
Q3.
302
5718
6819
2217
.62+
3753
08.4
8.7
A035
HD
1822
71..
.40
134
228.
815
8.5
Q0–
Q1
Q3.
302
5723
8619
2245
.89+
3753
02.9
13.3
...
...
...
207
344
.21.
2Q
0–Q
1..
.02
5751
6119
2517
.66+
3749
25.2
10.9
F035
BD+
3734
52bi
nary
199
944
.22.
7Q
0–Q
1..
.02
5782
5119
2751
.65+
3749
54.1
11.7
...
...
...
202
144
.22.
3Q
0–Q
1..
.02
5836
5819
3234
.58+
3751
32.0
12.6
...
...
...
463
9.5
0.0
Q0
...
0258
4202
1933
03.1
9+
3748
57.9
11.8
...
...
...
206
544
.21.
2Q
0–Q
1..
.02
5849
0819
3341
.47+
3750
41.7
10.8
...
...
bina
ry38
3809
829
2.5
219.
3Q
0–Q
1Q
4.2
0269
4337
1905
08.6
2+
3754
34.8
10.4
...
TY
C31
20-1
608-
1..
.40
233
137.
766
.4Q
0–Q
1Q
2.3
0270
7479
1920
33.1
0+
3759
54.0
11.2
...
TY
C31
34-8
33-1
...
4392
179
.64.
5Q
0–Q
1Q
2.1
0271
8596
1930
35.7
8+
3755
51.5
13.4
...
...
...
464
9.5
0.0
Q0
...
0272
0582
1932
21.1
9+
3759
09.0
11.4
...
...
...
4418
332
1.5
248.
4Q
0–Q
1Q
4.3
0283
4796
1906
47.6
2+
3804
32.4
12.5
...
...
...
461
9.5
0.0
Q0
...
0283
5795
1908
06.5
3+
3800
26.4
12.6
...
...
...
207
044
.21.
4Q
0–Q
1..
.02
8532
8019
2627
.98+
3802
05.2
11.0
...
TY
C31
34-9
2-1
...
4440
032
1.5
248.
3Q
0–Q
1Q
4.3
0285
5687
1928
31.2
0+
3801
40.7
10.3
...
TY
C31
34-1
0-1
...
462
9.5
0.0
Q0
...
0286
0123
1932
16.4
2+
3803
36.6
13.7
...
...
...
463
9.5
0.0
Q0
...
0296
9151
1902
17.7
6+
3811
27.8
11.9
...
...
...
460
9.5
0.0
Q0
...
A125, page 22 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0297
0244
1903
42.3
4+
3808
14.2
12.5
...
...
...
463
9.5
0.0
Q0
...
0297
2401
1906
35.8
6+
3808
59.3
13.5
...
...
...
460
9.5
0.0
Q0
...
0297
5832
1911
01.9
9+
3808
56.6
12.6
...
...
...
209
044
.21.
2Q
0–Q
1..
.02
9876
6019
2357
.46+
3806
51.7
8.0
F216
,A335
HD
1826
34δ
Sct
245
196
169.
895
.2Q
0–Q
1Q
3.1
0298
9746
1925
49.3
4+
3809
13.6
13.2
...
...
...
207
844
.21.
2Q
0–Q
1..
.02
9955
2519
3050
.23+
3811
41.6
13.2
...
...
...
464
9.5
0.0
Q0
...
0299
7802
1932
48.1
4+
3808
35.9
13.2
...
...
...
206
244
.21.
2Q
0–Q
1..
.03
0979
1219
0336
.72+
3812
08.2
9.4
A535
BD+
3733
24bi
nary
4537
810
9.5
35.3
Q0–
Q1
Q2.
203
1114
5119
2037
.54+
3815
08.2
13.5
...
...
...
463
9.5
0.0
Q0
...
0311
9604
1928
30.5
0+
3816
09.4
10.7
...
TY
C31
34-7
0-1
...
4754
726
2.8
187.
3Q
0–Q
1Q
4.1
0311
9825
1928
42.1
9+
3816
47.1
11.0
...
...
...
209
044
.21.
2Q
0–Q
1..
.03
2158
0019
0103
.65+
3818
24.3
13.2
...
...
...
207
044
.21.
6Q
0–Q
1..
.03
2175
5419
0351
.02+
3821
28.8
9.6
A535
BD+
3834
15bi
nary◦
4042
613
7.7
66.3
Q0–
Q1
Q2.
303
2186
3719
0531
.68+
3820
07.4
10.6
...
TY
C31
20-5
64-1
...
4007
222
8.8
158.
5Q
0–Q
1Q
3.3
0321
9256
1906
27.5
3+
3821
13.9
8.3
A335
HD
1783
06..
.58
430
321.
432
.9Q
0–Q
4Q
3.2
0322
0783
1908
43.4
9+
3819
32.8
13.6
...
...
...
460
9.5
0.0
Q0
...
0322
2364
1910
59.5
4+
3821
19.9
11.1
...
TY
C31
21-1
831-
1..
.2
063
44.2
1.2
Q0–
Q1
...
0323
0227
1920
27.0
2+
3823
59.5
9.0
A535
HD
1818
50bi
nary
3848
466
44.2
1.2
Q0
Q1
0323
1406
1921
43.7
3+
3818
53.3
10.5
...
TY
C31
34-1
188-
1..
.45
158
169.
895
.2Q
0–Q
1Q
3.1
0324
0556
1931
15.9
8+
3818
46.4
10.3
...
TY
C31
35-6
07-1
...
4539
410
9.5
35.3
Q0–
Q1
Q2.
203
2454
2019
3558
.61+
3818
21.2
10.6
...
TY
C31
35-3
96-1
...
4013
522
8.8
158.
5Q
0–Q
1Q
3.3
0324
8627
1938
54.2
9+
3821
04.1
12.3
...
...
...
463
9.5
0.0
Q0
...
0332
7681
1908
12.4
8+
3829
02.3
11.3
...
TY
C31
20-1
051-
1bi
nary�
4439
932
1.5
248.
3Q
0–Q
1Q
4.3
0333
1147
1913
07.7
5+
3827
34.3
10.1
...
TY
C31
21-1
178-
1..
.15
791
44.4
1.2
Q1
Q0
0333
7002
1920
04.2
5+
3824
41.0
10.8
...
TY
C31
34-2
162-
1bi
nary
3868
129
2.5
219.
3Q
0–Q
1Q
4.2
0334
7643
1931
16.2
2+
3824
02.9
8.0
A235
HD
1841
05..
.45
121
109.
035
.4Q
0–Q
1Q
2.2
0334
8390
1932
00.6
2+
3824
18.0
11.4
...
TY
C31
35-1
35-1
puls
atin
g340
286
137.
766
.3Q
0–Q
1Q
2.3
0335
4022
1937
33.1
0+
3827
51.8
12.1
...
...
...
461
9.5
0.0
Q0
...
0335
5066
1938
29.6
6+
3825
24.9
13.6
...
...
...
464
9.5
0.0
Q0
...
0342
4493
1900
37.5
4+
3830
20.2
9.6
A535
BD+
3833
91..
.40
427
137.
766
.3Q
0–Q
1Q
2.3
0342
5802
1902
50.2
6+
3834
04.0
11.2
...
TY
C31
20-1
011-
1..
.43
321
79.6
4.5
Q0–
Q1
Q2.
103
4271
4419
0453
.21+
3835
24.4
13.4
...
...
...
460
9.5
0.0
Q0
...
0342
7365
1905
12.8
6+
3832
46.6
13.6
...
...
...
462
9.5
0.0
Q0
...
0342
9637
1908
38.0
4+
3830
31.8
7.7
kF2h
A9m
F318
HD
1788
75bi
nary
,Am
star
1400
631
0.5
4.5
Q1–
Q4
...
0343
7940
1919
22.0
1+
3831
49.4
8.5
F035
HD
1815
69..
.58
013
321.
432
.9Q
0–Q
4Q
3.2
0344
0495
1922
12.3
6+
3830
32.6
10.5
...
TY
C31
34-6
32-1
...
4514
016
9.8
95.2
Q0–
Q1
Q3.
103
4493
7319
3135
.98+
3830
34.6
12.7
...
...
...
206
244
.21.
2Q
0–Q
1..
.03
4496
2519
3149
.30+
3834
50.6
13.4
...
...
...
203
444
.21.
9Q
0–Q
1..
.03
4534
9419
3531
.73+
3834
54.4
9.6
A535
BD+
3836
66..
.40
408
137.
766
.3Q
0–Q
1Q
2.3
0345
7434
1939
18.8
6+
3832
18.4
12.4
...
...
...
462
9.5
0.0
Q0
...
0345
8097
1939
53.3
3+
3833
25.9
11.7
...
...
...
208
644
.21.
2Q
0–Q
1..
.03
4583
1819
4003
.91+
3835
51.6
12.8
...
...
...
209
044
.21.
2Q
0–Q
1..
.03
5259
5119
0034
.73+
3840
26.4
12.9
...
...
...
462
9.5
0.0
Q0
...
0352
8578
1904
56.7
8+
3838
56.5
13.5
...
...
...
461
9.5
0.0
Q0
...
0353
9153
1919
32.7
1+
3839
04.9
11.4
...
TY
C31
21-3
79-1
...
3988
913
7.7
66.3
Q0–
Q1
Q2.
303
5460
6119
2713
.94+
3838
19.2
10.9
...
...
...
462
9.5
0.0
Q0
...
0355
8145
1939
13.0
6+
3838
05.1
11.3
...
TY
C31
35-1
89-1
...
4395
831
0.5
248.
3Q
1Q
4.3
A125, page 23 of 70
A&A 534, A125 (2011)
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0362
9080
1904
07.2
2+
3842
20.2
13.5
...
...
...
459
9.5
0.0
Q0
...
0363
3693
1911
21.6
5+
3843
48.4
12.6
...
...
...
463
9.5
0.0
Q0
...
0363
4384
1912
20.2
8+
3843
34.1
11.2
...
...
...
4385
479
.64.
5Q
0–Q
1Q
2.1
0364
3717
1923
43.7
5+
3847
30.2
12.9
...
...
...
463
9.5
0.0
Q0
...
0364
4116
1924
10.7
3+
3843
01.1
10.9
...
TY
C31
34-1
328-
1..
.38
681
292.
521
9.3
Q0–
Q1
Q4.
203
6555
1319
3553
.30+
3847
03.7
10.5
...
TY
C31
35-1
42-1
...
209
044
.21.
2Q
0–Q
1..
.03
6556
0819
3559
.16+
3844
45.3
11.4
...
...
...
4380
732
1.5
248.
3Q
0–Q
1Q
4.3
0366
3141
1942
39.1
7+
3843
05.7
13.2
...
...
bina
ry�
206
744
.21.
6Q
0–Q
1..
.03
7337
3519
0901
.92+
3853
59.6
8.4
F535
HD
1789
71..
.57
376
321.
435
.3Q
0–Q
4Q
2.2
0375
8717
1937
42.1
4+
3851
20.4
11.8
...
TY
C31
35-3
60-1
...
206
144
.21.
6Q
0–Q
1..
.03
7598
1419
3846
.25+
3851
32.5
10.7
G035
TY
C31
35-7
7-1
...
4538
210
9.5
35.3
Q0–
Q1
Q2.
203
7600
0219
3858
.01+
3852
43.6
10.6
...
TY
C31
35-7
08-1
...
4606
820
0.7
126.
4Q
0–Q
1Q
3.2
0376
0826
1939
48.2
2+
3853
47.9
8.8
A1V
17H
D18
5894
...
464
9.5
0.0
Q0
...
0376
1641
1940
30.2
4+
3851
59.9
11.0
A018
HD
2253
41..
.15
851
44.4
1.2
Q1
Q0
0383
6911
1908
30.0
5+
3854
42.7
12.5
...
...
...
208
944
.21.
2Q
0–Q
1..
.03
8508
1019
2624
.72+
3858
32.7
10.0
...
TY
C31
34-3
-1..
.15
860
44.4
1.2
Q1
Q0
0385
1151
1926
47.5
4+
3856
16.7
9.8
A235
BD+
3835
94..
.15
771
44.4
1.4
Q1
Q0
0386
8032
1943
07.5
8+
3856
49.9
10.4
A018
HD
2255
04..
.44
909
169.
895
.3Q
0–Q
1Q
3.1
0394
1283
1909
43.6
8+
3902
45.6
10.3
...
TY
C31
20-8
67-1
...
4544
910
9.5
35.3
Q0–
Q1
Q2.
203
9429
1119
1216
.27+
3904
16.9
10.8
...
TY
C31
21-7
19-1
...
3865
829
2.5
219.
3Q
0–Q
1Q
4.2
0396
6357
1938
24.1
0+
3904
58.9
11.2
...
...
...
4519
610
9.5
35.3
Q0–
Q1
Q2.
203
9707
2919
4218
.60+
3900
46.8
11.5
...
TY
C31
36-1
008-
1..
.45
175
169.
895
.2Q
0–Q
1Q
3.1
0403
5667
1858
29.5
7+
3910
56.7
10.0
...
TY
C31
19-3
47-1
...
1584
244
.41.
2Q
1Q
004
0443
5319
1100
.82+
3910
15.3
9.8
A235
BD+
3834
65..
.15
856
44.4
1.2
Q1
Q0
0404
8488
1916
32.7
8+
3910
30.1
11.6
A535
...
bina
ry39
583
126.
866
.5Q
1Q
2.3
0404
8494
1916
33.0
7+
3910
28.7
9.5
A535
BD+
3835
12bi
nary
4546
510
9.5
35.3
Q0–
Q1
Q2.
204
0694
7719
3838
.52+
3908
25.2
11.2
...
TY
C31
35-4
85-1
...
4411
832
1.5
248.
3Q
0–Q
1Q
4.3
0407
5519
1943
50.0
2+
3908
48.5
12.5
F018
HD
2256
44..
.2
070
44.2
1.6
Q0–
Q1
...
0407
7032
1945
03.1
7+
3911
26.0
9.7
F035
...
...
4390
579
.64.
5Q
0–Q
1Q
2.1
0414
4300
1911
26.1
1+
3912
18.0
12.3
...
...
...
207
544
.21.
2Q
0–Q
1..
.04
1506
1119
1858
.20+
3916
01.4
7.9
A5V
17,A
235H
D18
1469
bina
ry38
4316
010
9.4
35.3
Q0–
Q1
Q2.
204
1608
7619
2929
.16+
3913
17.6
10.2
...
TY
C31
34-8
1-1
...
4523
510
9.5
35.4
Q0–
Q1
Q2.
204
1643
6319
3250
.54+
3914
26.5
11.4
...
...
...
4028
513
7.7
66.3
Q0–
Q1
Q2.
304
1685
7419
3641
.02+
3915
17.9
10.3
...
TY
C31
35-4
37-1
...
4032
113
7.7
66.3
Q0–
Q1
Q2.
304
1706
3119
3833
.07+
3914
18.7
10.8
...
TY
C31
35-6
41-1
...
3862
829
2.5
219.
3Q
0–Q
1Q
4.2
0418
0199
1946
02.3
5+
3912
19.7
10.1
A718
HD
2257
18..
.15
829
44.4
1.2
Q1
Q0
0425
2757
1915
35.2
8+
3920
07.2
10.9
...
TY
C31
21-1
037-
1..
.38
629
292.
521
9.3
Q0–
Q1
Q4.
204
2693
3719
3312
.96+
3922
23.8
10.9
A8I
I35..
.bi
nary
3969
212
6.8
66.3
Q1
Q2.
304
2815
8119
4357
.00+
3920
47.4
9.4
A218
HD
2255
69..
.45
460
109.
535
.3Q
0–Q
1Q
2.2
0438
3117
1943
34.1
0+
3924
24.0
11.0
A318
HD
2255
35..
.49
453
44.2
1.2
Q0
Q1
0447
6836
1939
31.4
2+
3934
57.8
11.5
...
...
...
4543
410
9.5
35.3
Q0–
Q1
Q2.
204
4803
2119
4238
.38+
3933
40.4
10.3
A318
HD
2254
79..
.45
390
109.
535
.3Q
0–Q
1Q
2.2
0448
8840
1949
27.5
8+
3932
15.3
11.4
...
TY
C31
40-5
68-1
...
4033
813
7.7
66.3
Q0–
Q1
Q2.
304
5509
6219
1405
.11+
3936
56.9
10.5
...
TY
C31
25-3
570-
1..
.40
112
228.
815
8.5
Q0–
Q1
Q3.
304
5563
4519
2028
.85+
3936
36.4
10.8
...
TY
C31
38-1
615-
1..
.47
527
262.
818
7.3
Q0–
Q1
Q4.
104
5703
2619
3609
.02+
3937
43.0
9.8
...
BD+
3938
58va
riab
le4,
3814
474
321.
54.
5Q
0–Q
4..
.
A125, page 24 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0458
8487
1951
21.8
2+
3941
37.5
10.9
A018
HD
2261
96..
.43
254
310.
524
8.4
Q1
Q4.
304
6477
6319
1841
.14+
3942
26.7
10.8
...
TY
C31
25-3
07-1
...
4519
610
9.5
35.4
Q0–
Q1
Q2.
204
6494
7619
2035
.90+
3947
01.5
9.4
A235
BD+
3937
32..
.45
459
109.
535
.3Q
0–Q
1Q
2.2
0467
1225
1943
40.0
8+
3945
33.1
10.0
A718
HD
2255
44..
.54
194
137.
966
.3Q
1Q
0,Q
2.3
0467
7684
1948
44.7
1+
3947
32.5
10.2
A018
HD
2259
50..
.40
407
137.
766
.3Q
0–Q
1Q
2.3
0475
8316
1939
41.6
9+
3948
04.6
11.1
...
TY
C31
39-1
185-
1..
.47
354
262.
818
7.3
Q0–
Q1
Q4.
104
7686
7719
4823
.95+
3952
58.0
11.2
A18
HD
2259
06..
.40
676
79.6
5.1
Q0–
Q1
Q2.
104
8406
7519
3257
.94+
3958
45.3
9.6
...
TY
C31
39-1
403-
1..
.40
137
228.
815
8.5
Q0–
Q1
Q3.
304
8508
9919
4304
.49+
3959
49.6
7.0
F0I
V19
,A535
HD
1865
05..
.45
19.
50.
0Q
0..
.04
8566
3019
4746
.58+
3958
56.3
11.4
...
...
...
4031
713
7.7
66.3
Q0–
Q1
Q2.
304
8576
7819
4844
.06+
3954
60.0
7.0
F035
HD
1875
23..
.14
420
321.
54.
7Q
0–Q
4..
.04
8630
7719
5313
.85+
3956
48.3
11.1
A018
HD
2263
81..
.49
510
44.2
1.2
Q0
Q1
0490
9697
1908
48.0
0+
4004
06.0
10.7
...
TY
C31
24-2
306-
1bi
nary
4757
926
2.8
187.
3Q
0–Q
1Q
4.1
0491
9818
1922
10.6
6+
4003
17.1
10.7
...
TY
C31
38-3
6-1
...
4737
026
2.8
187.
3Q
0–Q
1Q
4.1
0492
0125
1922
35.0
4+
4003
47.2
11.1
F035
BD+
3937
45..
.49
479
44.2
1.2
Q0
Q1
0493
6524
1940
48.3
1+
4002
28.9
13.1
...
...
...
4950
444
.21.
2Q
0Q
104
9372
5719
4127
.31+
4004
54.8
13.5
...
...
...
1018
822
8.7
4.9
Q0–
Q3
...
0498
9900
1855
25.6
6+
4010
37.7
6.9
A235
HD
1758
41..
.37
933
25.9
0.0
...
Q3.
305
0241
5019
4106
.58+
4010
19.6
13.2
...
...
...
4893
533
.40.
0..
.Q
105
0244
5419
4117
.02+
4010
34.8
13.7
...
NG
C68
1960
9N
GC
6819
4897
033
.40.
0..
.Q
105
0244
5519
4117
.02+
4006
04.0
14.8
...
NG
C68
1996
0N
GC
6819
4895
533
.40.
0..
.Q
105
0244
5619
4117
.04+
4010
51.9
11.1
...
NG
C68
1955
0N
GC
6819
1383
530
9.7
4.9
Q1–
Q4
...
0502
4750
1941
26.5
9+
4011
41.8
11.2
...
NG
C68
1997
5N
GC
6819
1032
722
8.7
4.5
Q0–
Q3
...
0503
8228
1952
43.8
5+
4010
56.0
11.4
...
...
...
4440
732
1.5
248.
3Q
0–Q
1Q
4.3
0508
0290
1859
19.1
0+
4012
54.8
9.5
F835
BD+
4035
47..
.41
935
79.6
5.0
Q0–
Q1
Q2.
105
0883
0819
1327
.19+
4014
32.1
8.7
F535
HD
1800
99bi
nary
3840
304
137.
766
.3Q
0–Q
1Q
2.3
0510
5754
1934
31.1
5+
4017
36.6
11.4
...
TY
C31
39-2
577-
1..
.40
240
137.
766
.3Q
0–Q
1Q
2.3
0511
2786
1941
23.6
9+
4012
35.5
11.5
...
NG
C68
1997
2N
GC
6819
1446
132
1.5
4.5
Q0–
Q4
...
0511
2932
1941
28.9
9+
4013
15.5
13.2
...
NG
C68
1999
5N
GC
6819
4892
533
.40.
0..
.Q
105
1137
9719
4212
.62+
4017
46.0
9.1
A318
HD
2254
47..
.43
613
79.6
4.5
Q0–
Q1
Q2.
105
1647
6718
5354
.19+
4019
25.6
7.8
F2I
V20
HD
1755
37..
.14
422
321.
54.
6Q
0–Q
4..
.05
1807
9619
1949
.58+
4019
18.7
10.2
...
TY
C31
25-2
69-1
...
4485
510
9.5
35.4
Q0–
Q1
Q2.
205
1972
5619
3833
.82+
4019
25.7
11.0
...
TY
C31
39-1
882-
1bi
nary
4443
032
1.5
248.
3Q
0–Q
1Q
4.3
0519
9464
1940
45.4
8+
4022
03.1
14.8
...
...
...
4892
733
.40.
0..
.Q
105
2000
8419
4120
.66+
4023
31.7
9.2
A039
HD
2254
10bi
nary�
4130
279
.65.
1Q
0–Q
1Q
2.1
0520
1088
1942
12.0
5+
4018
02.8
13.6
A335
...
...
4895
033
.40.
0..
.Q
105
2097
1219
4921
.98+
4021
13.2
11.3
A239
HD
2260
09..
.45
346
109.
535
.3Q
0–Q
1Q
2.2
0521
7733
1955
44.7
6+
4023
30.3
7.4
B1V
22,B
2II21
HD
1888
91bi
nary
4226
128
.90.
0..
.Q
4.3
0521
9533
1957
09.9
1+
4022
50.5
9.2
A239
,kA
2hA
8mA
823H
D22
6766
bina
ry49
385
44.2
1.2
Q0
Q1
0527
2673
1924
19.8
7+
4024
27.6
10.4
...
TY
C31
38-9
94-1
...
4517
516
9.8
95.2
Q0–
Q1
Q3.
105
2945
7119
4712
.53+
4028
02.4
10.5
F239
HD
2258
08..
.47
206
262.
818
7.3
Q0–
Q1
Q4.
105
2968
7719
4904
.75+
4024
36.6
12.3
...
HA
T19
9-27
597
vari
able
5,38
2872
232
1.9
75.3
Q0–
Q4
Q0
0535
6349
1919
36.1
0+
4035
07.3
8.1
A035
HD
1816
80bi
nary
4529
218
9.7
126.
4Q
1Q
3.2
0537
1747
1937
43.4
9+
4035
38.4
10.5
F35
BD+
4038
11..
.45
893
200.
712
6.4
Q0–
Q1
Q3.
205
3914
1619
5514
.78+
4033
12.8
10.2
A739
HD
2265
70..
.45
456
109.
535
.3Q
0–Q
1Q
2.2
0542
8254
1856
52.8
0+
4037
47.4
10.5
...
TY
C31
23-1
722-
1..
.46
080
200.
712
6.4
Q0–
Q1
Q3.
2
A125, page 25 of 70
A&A 534, A125 (2011)
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0543
6432
1911
27.9
1+
4041
26.6
9.0
A235
HD
1796
18..
.49
499
44.2
1.2
Q0
Q1
0543
7206
1912
43.5
6+
4037
57.1
8.4
A235
HD
1799
36..
.46
078
200.
712
6.4
Q0–
Q1
Q3.
205
4460
6819
2418
.10+
4038
58.8
9.7
...
BD+
4037
04bi
nary
4393
779
.64.
5Q
0–Q
1Q
2.1
0547
3171
1952
17.8
8+
4041
10.1
9.0
A239
HD
2262
84..
.15
859
44.4
1.2
Q1
Q0
0547
4427
1953
21.1
4+
4039
12.9
11.4
...
TY
C31
41-2
904-
1..
.44
428
321.
524
8.3
Q0–
Q1
Q4.
305
4764
9519
5453
.11+
4036
55.2
10.2
A339
HD
2265
28..
.42
944
79.6
4.6
Q0–
Q1
Q2.
105
4768
6419
5509
.22+
4039
20.7
11.5
...
...
...
4168
268
.65.
1Q
1Q
2.1
0551
3861
1857
24.5
3+
4042
53.0
11.6
...
TY
C31
23-2
012-
1bi
nary
3845
178
109.
511
3.0
Q0–
Q1
Q2.
205
6030
4919
0343
.90+
4048
17.2
11.2
...
TY
C31
24-1
423-
1..
.44
428
321.
524
8.3
Q0–
Q1
Q4.
305
6303
6219
3919
.25+
4053
58.9
10.5
...
TY
C31
39-1
246-
1..
.40
134
228.
815
8.5
Q0–
Q1
Q3.
305
6320
9319
4104
.78+
4053
17.4
10.9
A39
HD
2253
91..
.15
846
44.4
1.2
Q1
Q0
0564
1711
1949
38.3
8+
4053
49.8
10.4
F039
HD
2260
29..
.40
404
137.
766
.3Q
0–Q
1Q
2.3
0570
9664
1932
25.5
8+
4054
03.0
11.3
...
TY
C31
39-8
26-1
...
4545
610
9.5
35.3
Q0–
Q1
Q2.
205
7223
4619
4532
.76+
4056
41.9
11.2
...
TY
C31
40-9
25-1
...
4757
526
2.8
187.
3Q
0–Q
1Q
4.1
0572
4048
1947
00.4
6+
4056
10.0
11.4
...
...
...
4406
732
1.5
248.
4Q
0–Q
1Q
4.3
0572
4440
1947
19.7
8+
4059
39.6
7.9
A535
HD
1872
34..
.57
568
321.
54.
5Q
0–Q
4Q
3.1
0572
4810
1947
39.2
4+
4054
41.5
10.9
A739
HD
2258
42bi
nary�
1585
644
.41.
2Q
1Q
005
7682
0318
5136
.46+
4105
27.7
10.8
...
TY
C31
23-1
9-1
...
4544
810
9.5
35.3
Q0–
Q1
Q2.
205
7724
1118
5959
.59+
4100
54.3
10.6
...
...
bina
ry37
713
292.
521
9.9
Q0–
Q1
Q4.
205
7745
5719
0401
.78+
4101
49.6
11.0
...
TY
C31
24-2
058-
1..
.44
425
321.
524
8.3
Q0–
Q1
Q4.
305
7857
0719
2031
.70+
4104
48.4
9.0
A235
HD
1819
02..
.43
397
79.6
4.5
Q0–
Q1
Q2.
105
8101
1319
4739
.34+
4101
32.5
11.6
...
...
bina
ry38
4538
310
9.5
35.3
Q0–
Q1
Q2.
205
8577
1418
5846
.37+
4109
56.0
11.2
...
TY
C31
23-7
42-1
...
3865
629
2.5
219.
3Q
0–Q
1Q
4.2
0588
0360
1932
23.2
6+
4108
09.2
8.8
A035
HD
1843
80..
.49
507
44.2
1.2
Q0
Q1
0594
0273
1855
48.1
7+
4115
40.5
10.5
F035
BD+
4131
85..
.40
102
228.
815
8.5
Q0–
Q1
Q3.
305
9542
6419
1927
.19+
4113
25.6
8.2
F035
HD
1816
54..
.57
187
321.
535
.3Q
0–Q
4Q
2.2
0596
5837
1934
06.5
0+
4115
03.3
9.2
F235
BD+
4037
86va
riab
le6
2407
922
8.5
4.5
Q0–
Q3
Q0
0598
0337
1948
24.2
9+
4116
51.3
10.1
F039
HD
2259
12bi
nary
4379
679
.05.
0Q
0–Q
1Q
2.1
0598
8140
1955
10.0
3+
4117
10.1
8.9
F037
HD
1887
74..
.10
332
321.
593
.4Q
0–Q
4..
.06
0327
3019
1422
.30+
4118
26.4
8.7
A237
HD
1803
49..
.46
077
200.
712
6.4
Q0–
Q1
Q3.
206
0678
1719
5354
.89+
4123
33.4
10.2
A339
HD
2264
43..
.43
924
79.6
4.5
Q0–
Q1
Q2.
106
1233
2419
2701
.51+
4129
09.1
8.7
F035
HD
1832
81bi
nary
4043
113
7.7
66.3
Q0–
Q1
Q2.
306
1413
7219
4637
.94+
4128
33.6
11.1
...
HA
T19
9-04
866
vari
able
4440
832
1.5
248.
3Q
0–Q
1Q
4.3
0614
2919
1947
55.8
5+
4126
58.9
10.6
...
TY
C31
44-6
08-1
bina
ry�
4002
122
8.8
158.
5Q
0–Q
1Q
3.3
0618
7665
1901
38.0
6+
4130
26.9
11.5
...
TY
C31
28-1
790-
1..
.45
465
109.
535
.3Q
0–Q
1Q
2.2
0619
9731
1920
31.9
4+
4135
19.5
10.9
...
TY
C31
42-1
75-1
...
1582
044
.41.
2Q
1Q
006
2688
9019
0228
.39+
4136
11.4
11.2
...
TY
C31
28-2
125-
1..
.45
464
109.
535
.3Q
0–Q
1Q
2.2
0627
9848
1920
19.4
4+
4139
39.9
8.9
F035
HD
1818
77..
.2
087
44.2
1.2
Q0–
Q1
...
0628
9468
1933
00.6
0+
4139
13.4
9.4
A235
BD+
4133
89..
.45
438
109.
535
.3Q
0–Q
1Q
2.2
0630
1745
1945
51.3
6+
4137
54.0
10.9
...
TY
C31
44-7
87-1
...
4524
810
9.5
35.4
Q0–
Q1
Q2.
206
3813
0619
4636
.34+
4144
16.9
8.7
A035
HD
1871
41..
.39
980
228.
815
8.5
Q0–
Q1
Q3.
306
4320
5419
1209
.53+
4150
15.3
8.2
F035
HD
1798
37..
.46
058
200.
712
6.4
Q0–
Q1
Q3.
206
4409
3019
2433
.79+
4153
24.0
10.6
...
TY
C31
42-1
367-
1..
.45
857
200.
712
6.4
Q0–
Q1
Q3.
206
4431
2219
2736
.34+
4149
39.9
11.2
...
TY
C31
42-1
661-
1..
.45
463
109.
535
.3Q
0–Q
1Q
2.2
0644
6951
1932
35.9
3+
4153
32.3
11.3
...
TY
C31
43-1
362-
1..
.44
431
321.
524
8.3
Q0–
Q1
Q4.
306
4481
1219
3402
.57+
4153
03.1
10.0
A235
BD+
4133
95..
.15
813
44.4
1.2
Q1
Q0
A125, page 26 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0646
2033
1948
33.7
2+
4149
49.3
10.7
...
TY
C31
44-6
46-1
...
4006
622
8.8
158.
5Q
0–Q
1Q
3.3
0650
0578
1853
24.9
4+
4159
16.9
10.8
...
TY
C31
27-1
666-
1..
.38
671
292.
521
9.3
Q0–
Q1
Q4.
206
5091
7519
0908
.64+
4156
59.8
10.0
A235
BD+
4132
48..
.15
859
44.4
1.2
Q1
Q0
0651
9869
1924
03.2
6+
4156
54.4
10.5
...
TY
C31
42-7
33-1
...
4487
916
9.8
95.2
Q0–
Q1
Q3.
106
5860
5218
5802
.14+
4201
05.7
11.3
...
...
...
4546
510
9.5
35.3
Q0–
Q1
Q2.
206
5875
5119
0054
.70+
4202
23.9
9.8
A035
BD+
4132
07..
.15
844
44.4
1.2
Q1
Q0
0659
0403
1905
53.3
5+
4202
14.5
10.6
...
TY
C31
28-2
036-
1..
.40
133
228.
815
8.5
Q0–
Q1
Q3.
306
6062
2919
2725
.34+
4200
31.0
11.1
...
TY
C31
42-7
17-1
...
4756
926
2.7
187.
3Q
0–Q
1Q
4.1
0661
4168
1936
27.5
0+
4204
26.8
11.4
...
...
...
4040
513
7.7
66.3
Q0–
Q1
Q2.
306
6291
0619
5038
.40+
4201
23.2
10.1
F039
HD
2261
35..
.15
861
44.4
1.2
Q1
Q0
0666
8729
1853
50.6
2+
4210
15.8
8.6
A235
HD
1755
36..
.46
078
200.
712
6.4
Q0–
Q1
Q3.
206
6707
4218
5719
.82+
4207
37.5
9.3
A535
BD+
4131
95..
.43
924
79.6
4.5
Q0–
Q1
Q2.
106
6786
1419
1046
.30+
4206
40.7
10.8
...
TY
C31
29-8
00-1
...
3791
829
2.5
219.
4Q
0–Q
1Q
4.2
0669
4649
1931
01.2
0+
4210
11.2
10.4
...
...
bina
ry45
188
169.
895
.2Q
0–Q
1Q
3.1
0675
6386
1855
54.2
4+
4212
37.9
8.7
A235
HD
1759
39..
.15
860
44.4
1.2
Q1
Q0
0675
6481
1856
01.8
7+
4213
34.7
9.3
F035
BD+
4231
97..
.43
844
79.6
4.5
Q0–
Q1
Q2.
106
7615
3919
0503
.58+
4213
18.7
10.3
...
TY
C31
28-1
341-
1..
.45
451
109.
535
.3Q
0–Q
1Q
2.2
0677
6331
1925
59.4
7+
4216
45.3
10.9
...
TY
C31
42-5
11-1
...
4441
132
1.5
248.
3Q
0–Q
1Q
4.3
0679
0335
1941
30.7
4+
4212
11.1
10.5
...
TY
C31
44-1
756-
1..
.46
068
200.
712
6.4
Q0–
Q1
Q3.
206
8048
2119
5404
.99+
4217
29.9
10.6
A35
HD
2264
54va
riab
le7
4012
122
8.8
158.
5Q
0–Q
1Q
3.3
0686
5077
1929
39.3
8+
4223
25.4
9.8
...
TY
C31
42-1
206-
1..
.15
858
44.4
1.2
Q1
Q0
0692
2690
1846
11.0
6+
4224
02.5
10.4
...
TY
C31
26-7
80-1
...
4516
716
9.8
95.2
Q0–
Q1
Q3.
106
9234
2418
4749
.73+
4226
27.6
11.3
...
TY
C31
26-1
059-
1..
.44
223
321.
524
8.4
Q0–
Q1
Q4.
306
9377
5819
1301
.18+
4229
58.4
9.8
A235
BD+
4232
78..
.15
860
44.4
1.2
Q1
Q0
0693
9291
1915
18.7
9+
4226
19.2
10.1
...
TY
C31
29-2
577-
1..
.42
750
79.6
4.5
Q0–
Q1
Q2.
106
9470
6419
2517
.66+
4225
13.3
11.3
...
TY
C31
42-1
168-
1..
.45
456
109.
535
.3Q
0–Q
1Q
2.2
0695
1642
1931
05.9
3+
4229
53.2
9.7
A535
BD+
4233
70..
.15
807
44.4
1.2
Q1
Q0
0696
5789
1945
41.3
0+
4229
34.4
10.1
A535
BD+
4234
46bi
nary
4392
679
.64.
5Q
0–Q
1Q
2.1
0700
7103
1843
57.1
9+
4231
05.7
11.2
...
TY
C31
26-2
522-
1..
.38
311
292.
521
9.3
Q0–
Q1
Q4.
207
1062
0519
1157
.48+
4240
22.6
11.4
...
TY
C31
29-8
79-1
bina
ry�
4394
579
.64.
5Q
0–Q
1Q
2.1
0710
6648
1912
39.7
9+
4238
40.5
10.5
...
TY
C31
29-2
589-
1..
.44
969
169.
895
.3Q
0–Q
1Q
3.1
0710
9598
1916
56.8
1+
4238
11.7
10.6
...
TY
C31
29-2
517-
1..
.46
064
200.
712
6.4
Q0–
Q1
Q3.
207
1195
3019
2919
.03+
4238
29.1
8.5
A335
HD
1837
87..
.14
473
321.
54.
5Q
0–Q
4..
.07
1227
4619
3310
.10+
4238
26.9
10.9
...
TY
C31
43-1
631-
1..
.15
833
44.4
1.2
Q1
Q0
0720
4237
1932
01.3
4+
4242
21.5
10.8
...
TY
C31
43-2
61-1
...
4758
426
2.8
187.
3Q
0–Q
1Q
4.1
0721
1759
1940
30.7
7+
4247
02.9
11.0
...
TY
C31
44-1
426-
1..
.49
467
44.2
1.2
Q0
Q1
0721
2040
1940
49.0
3+
4247
05.6
10.9
...
TY
C31
44-2
042-
1..
.38
635
292.
521
9.3
Q0–
Q1
Q4.
207
2156
0719
4411
.64+
4245
09.5
10.5
...
TY
C31
44-1
656-
1..
.47
487
262.
818
7.3
Q0–
Q1
Q4.
107
2174
8319
4557
.86+
4245
23.1
10.6
...
TY
C31
44-8
56-1
...
4951
144
.21.
2Q
0Q
107
2203
5619
4828
.15+
4244
36.9
11.5
...
...
...
4419
432
1.5
248.
4Q
0–Q
1Q
4.3
0726
5427
1903
27.8
9+
4249
54.6
11.5
...
...
...
4041
313
7.7
66.3
Q0–
Q1
Q2.
307
2871
1819
3331
.34+
4250
11.3
10.7
...
TY
C31
43-1
359-
1..
.47
575
262.
818
7.3
Q0–
Q1
Q4.
107
3003
8719
4719
.51+
4252
02.0
10.5
...
TY
C31
44-1
600-
1..
.46
064
200.
712
6.4
Q0–
Q1
Q3.
207
3043
8519
5051
.55+
4248
06.0
10.0
...
TY
C31
45-9
01-1
...
1028
922
8.7
4.5
Q0–
Q3
...
0733
8125
1848
49.7
5+
4255
05.4
11.1
...
TY
C31
26-3
094-
1..
.48
494
44.2
1.8
Q0
Q1
0735
0486
1910
48.2
2+
4254
38.6
11.3
...
...
...
4527
910
9.5
35.3
Q0–
Q1
Q2.
2
A125, page 27 of 70
A&A 534, A125 (2011)
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0735
2425
1913
48.7
0+
4257
28.8
10.6
...
TY
C31
29-1
319-
1..
.38
650
292.
521
9.3
Q0–
Q1
Q4.
207
3527
7619
1423
.02+
4255
27.7
11.1
...
TY
C31
29-2
485-
1..
.49
484
44.2
1.2
Q0
Q1
0738
5478
1950
57.8
6+
4259
45.9
11.5
...
TY
C31
45-1
71-1
bina
ry38
4244
210
9.5
35.3
Q0–
Q1
Q2.
207
4362
6619
1634
.20+
4301
26.7
11.4
...
...
...
4040
213
7.7
66.3
Q0–
Q1
Q2.
307
4502
8419
3337
.68+
4305
49.2
10.4
A535
BD+
4233
80..
.45
192
169.
895
.2Q
0–Q
1Q
3.1
0750
2559
1848
17.6
9+
4307
06.6
11.3
...
TY
C31
26-2
023-
1..
.44
216
321.
524
8.3
Q0–
Q1
Q4.
307
5336
9419
3412
.91+
4307
03.5
10.4
...
TY
C31
43-1
179-
1..
.40
429
137.
766
.3Q
0–Q
1Q
2.3
0754
8061
1948
15.4
6+
4307
36.8
8.8
G224
,G2I
b41V
1154
Cyg
Cep
heid
863
501
321.
531
9.7
Q0–
Q4
Q1
0754
8479
1948
36.5
0+
4306
32.0
8.4
A335
HD
1875
47..
.46
077
200.
712
6.4
Q0–
Q1
Q3.
207
5532
3719
5243
.10+
4306
00.1
11.3
...
...
...
4442
832
1.5
248.
3Q
0–Q
1Q
4.3
0758
3939
1847
32.0
6+
4317
04.7
9.7
A035
BD+
4330
78..
.40
086
228.
815
8.5
Q0–
Q1
Q3.
307
5962
5019
1103
.60+
4313
07.8
11.3
...
...
...
4441
932
1.5
248.
3Q
0–Q
1Q
4.3
0766
2076
1850
56.9
3+
4318
13.6
10.0
F035
BD+
4330
97..
.15
812
44.4
1.2
Q1
Q0
0766
8791
1905
23.6
4+
4320
05.6
9.3
A235
HD
1781
20..
.43
532
79.6
4.5
Q0–
Q1
Q2.
107
6698
4819
0719
.99+
4318
55.2
7.4
F2I
II20
HD
1786
15..
.10
175
228.
74.
7Q
0–Q
3..
.07
6941
9119
4209
.29+
4323
37.4
10.8
...
TY
C31
48-1
126-
1..
.38
456
292.
521
9.4
Q0–
Q1
Q4.
207
6977
9519
4620
.83+
4322
36.0
11.0
...
TY
C31
48-1
808-
1..
.49
510
44.2
1.2
Q0
Q1
0769
9056
1947
39.4
3+
4320
19.4
10.5
...
TY
C31
48-4
31-1
...
4011
322
8.8
158.
5Q
0–Q
1Q
3.3
0770
2705
1950
55.4
2+
4319
03.0
11.4
...
...
...
4036
813
7.7
66.3
Q0–
Q1
Q2.
307
7324
5818
4927
.38+
4328
12.1
10.8
...
TY
C31
30-1
50-1
...
3845
229
2.5
219.
4Q
0–Q
1Q
4.2
0774
2739
1911
16.9
2+
4324
24.8
11.3
...
TY
C31
33-2
367-
1..
.44
582
109.
535
.3Q
0–Q
1Q
2.2
0774
8238
1920
38.2
1+
4329
03.7
9.5
A535
HD
1819
85..
.40
114
137.
766
.5Q
0–Q
1Q
2.3
0775
6853
1932
39.1
2+
4326
11.2
9.0
A035
HD
1844
49..
.49
461
44.2
1.2
Q0
Q1
0776
7565
1945
39.0
0+
4329
43.0
9.3
A535
HD
1869
95bi
nary
206
944
.21.
2Q
0–Q
1..
.07
7702
8219
4833
.12+
4327
04.2
9.7
F035
BD+
4333
70..
.15
796
44.4
1.2
Q1
Q0
0777
1991
1950
06.5
5+
4329
05.9
11.1
...
TY
C31
49-1
784-
1..
.49
327
44.2
1.2
Q0
Q1
0777
3133
1951
13.7
5+
4327
43.0
10.9
...
TY
C31
49-1
852-
1..
.46
078
200.
712
6.4
Q0–
Q1
Q3.
207
7774
3519
5524
.38+
4329
47.9
10.7
...
...
...
4758
326
2.8
187.
3Q
0–Q
1Q
4.1
0779
8339
1841
34.9
9+
4332
58.9
7.9
F035
HD
1731
09..
.57
256
321.
535
.3Q
0–Q
4Q
2.2
0782
7131
1933
47.1
4+
4331
02.2
8.0
A235
HD
1846
95va
riab
le9
4308
830
.30.
7..
.Q
3.1
0783
1302
1939
00.8
6+
4335
03.4
11.3
...
TY
C31
47-9
82-1
...
4456
298
.635
.3Q
1Q
2.2
0783
4612
1943
04.8
7+
4335
32.8
10.3
...
TY
C31
48-2
091-
1..
.40
432
137.
766
.3Q
0–Q
1Q
2.3
0784
2286
1951
14.4
5+
4330
41.8
9.9
A235
BD+
4333
84..
.15
840
44.4
1.2
Q1
Q0
0784
2621
1951
35.6
9+
4331
10.1
11.1
...
TY
C31
49-1
211-
1..
.43
215
79.6
4.9
Q0–
Q1
Q2.
107
8482
8819
5652
.27+
4330
14.8
10.8
...
TY
C31
49-2
143-
1bi
nary�
3803
428
1.5
219.
3Q
1Q
4.2
0789
0526
1926
27.5
3+
4340
53.8
11.3
...
TY
C31
46-1
192-
1..
.45
435
109.
535
.3Q
0–Q
1Q
2.2
0790
0367
1939
44.9
5+
4341
45.3
11.3
...
TY
C31
47-1
2-1
...
3868
129
2.5
219.
3Q
0–Q
1Q
4.2
0790
8633
1949
06.8
9+
4341
22.8
11.2
...
TY
C31
48-6
60-1
...
4516
310
9.5
35.4
Q0–
Q1
Q2.
207
9598
6719
2658
.34+
4344
40.1
9.8
A235
BD+
4332
45..
.15
836
44.4
1.2
Q1
Q0
0797
7996
1949
50.5
0+
4346
28.6
11.5
...
TY
C31
48-5
97-1
...
4607
420
0.7
126.
4Q
0–Q
1Q
3.2
0798
5370
1956
59.7
4+
4345
08.3
9.8
G535
HD
1892
10..
.55
936
321.
54.
5Q
0–Q
4Q
2.1
0802
9546
1928
22.4
6+
4352
16.0
11.0
...
TY
C31
46-1
256-
1..
.49
145
44.2
1.2
Q0
Q1
0804
3961
1946
55.4
9+
4350
27.8
10.7
...
TY
C31
48-1
402-
1..
.45
467
109.
511
2.9
Q0–
Q1
Q2.
208
0541
4619
5653
.35+
4349
27.0
11.3
...
...
...
3928
413
7.7
66.5
Q0–
Q1
Q2.
308
1039
1719
3607
.25+
4355
08.0
11.5
...
...
...
4519
216
9.8
95.2
Q0–
Q1
Q3.
108
1045
8919
3700
.82+
4355
56.5
11.5
...
...
...
4421
732
1.5
248.
3Q
0–Q
1Q
4.3
A125, page 28 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
1.co
ntin
ued.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0812
3127
1957
04.1
3+
4355
31.7
11.0
...
TY
C31
49-5
34-1
...
8690
232
1.5
248.
3Q
0–Q
1Q
4.3
0814
3903
1846
15.7
4+
4400
13.4
13.8
...
...
...
1337
331
0.5
6.0
Q1–
Q4
...
0814
4674
1848
20.4
2+
4400
12.4
11.6
...
TY
C31
30-1
700-
1..
.39
858
228.
815
8.6
Q0–
Q1
Q3.
308
1454
7718
5015
.98+
4403
16.7
14.8
...
...
...
1400
731
0.5
325.
1Q
1–Q
4..
.08
1493
4118
5828
.85+
4402
41.5
10.9
...
TY
C31
31-1
906-
1..
.46
057
200.
712
6.4
Q0–
Q1
Q3.
208
1591
3519
1759
.83+
4401
12.6
13.8
...
...
...
1223
831
0.5
7.3
Q1–
Q4
...
0819
7761
2004
09.3
1+
4404
16.0
10.7
F235
BD+
4334
73s
NG
C68
6610
4902
344
.21.
2Q
0Q
108
1977
8820
0411
.18+
4405
33.3
13.0
...
...
...
4524
610
9.5
35.3
Q0–
Q1
Q2.
208
2115
0018
4612
.19+
4408
08.3
8.1
A535
HD
1739
78bi
nary
5686
831
0.5
4.9
Q1–
Q4
Q3.
108
2184
1919
0034
.61+
4408
29.0
11.9
...
...
...
1443
632
1.5
4.5
Q0–
Q4
...
0822
2685
1910
07.4
9+
4408
18.5
8.9
F0V
25,F
235H
D17
9336
...
208
044
.21.
2Q
0–Q
1..
.08
2235
6819
1156
.54+
4408
49.9
11.5
F225
...
...
5227
432
1.5
4.5
Q0–
Q4
Q2.
308
2239
8719
1246
.30+
4406
18.9
14.2
...
...
...
567
831
0.5
187.
5Q
1,Q
4..
.08
2300
2519
2229
.45+
4406
16.2
10.9
F025
TY
C31
46-1
037-
1..
.15
850
44.4
1.2
Q1
Q0
0824
5366
1943
33.9
1+
4406
19.5
11.2
...
TY
C31
48-1
360-
1..
.40
134
228.
815
8.5
Q0–
Q1
Q3.
308
2486
3019
4723
.30+
4407
59.0
11.2
...
TY
C31
48-4
84-1
...
4440
732
1.5
248.
3Q
0–Q
1Q
4.3
0826
4061
2003
27.9
4+
4409
19.2
13.5
...
...
NG
C68
6644
106
98.6
35.3
Q1
Q2.
208
2640
7520
0328
.34+
4407
55.2
13.7
...
...
NG
C68
6639
585
126.
866
.3Q
1Q
2.3
0826
4274
2003
39.6
7+
4409
23.3
13.8
...
...
NG
C68
6639
285
126.
866
.5Q
1Q
2.3
0826
4404
2003
47.1
4+
4409
25.7
12.2
...
...
NG
C68
6645
464
109.
535
.3Q
0–Q
1Q
2.2
0826
4546
2003
54.8
4+
4409
50.3
13.4
...
NG
C68
6617
NG
C68
6649
495
44.2
1.2
Q0
Q1
0826
4583
2003
57.3
6+
4409
33.6
11.3
...
HIP
9879
7N
GC
6866
4527
210
9.5
35.3
Q0–
Q1
Q2.
208
2645
8820
0357
.62+
4408
37.5
10.7
...
...
NG
C68
6649
512
44.2
1.2
Q0
Q1
0826
4617
2003
59.3
5+
4410
25.8
13.9
...
...
NG
C68
6644
828
98.1
35.3
Q1
Q2.
208
2646
7420
0402
.86+
4411
55.4
11.2
...
...
...
4212
079
.65.
1Q
0–Q
1Q
2.1
0826
4698
2004
03.9
6+
4410
20.5
12.4
...
...
...
4493
798
.635
.3Q
1Q
2.2
0828
3796
1858
53.0
9+
4416
40.3
14.5
...
...
...
1396
531
0.5
69.8
Q1–
Q4
...
0829
3302
1918
03.6
7+
4414
36.1
13.4
...
...
...
1372
132
1.3
6.9
Q0–
Q4
...
0832
3104
1955
37.8
2+
4414
32.9
9.7
kA2m
F026
...
...
3914
779
.66.
0Q
0–Q
1Q
2.1
0833
0056
2003
33.0
5+
4412
06.5
13.8
...
...
...
3975
512
6.8
66.3
Q1
Q2.
308
3300
9220
0334
.92+
4414
50.1
13.5
...
...
...
4347
568
.64.
5Q
1Q
2.1
0833
0463
2003
58.6
3+
4414
09.7
14.9
...
...
...
3768
728
1.5
219.
3Q
1Q
4.2
0833
0778
2004
16.1
8+
4412
04.6
13.4
...
...
...
4189
079
.64.
5Q
0–Q
1Q
2.1
0835
2420
1904
11.4
0+
4421
44.7
12.6
...
...
...
4043
313
7.7
66.3
Q0–
Q1
Q2.
308
3551
3019
1001
.61+
4422
29.9
10.3
F0I
II25
BD+
4430
72bi
nary
5739
532
1.5
35.3
Q0–
Q4
Q2.
208
3558
3719
1127
.07+
4422
46.7
13.3
...
...
...
1333
231
0.5
6.2
Q1–
Q4
...
0839
7426
2005
34.3
0+
4420
09.8
11.1
...
...
...
4950
544
.21.
2Q
0Q
108
4157
5219
0000
.02+
4427
48.5
10.7
...
TY
C31
32-1
272-
1..
.46
040
200.
712
6.4
Q0–
Q1
Q3.
208
4297
5619
2543
.13+
4426
26.3
10.5
...
TY
C31
46-1
441-
1..
.46
052
200.
712
6.4
Q0–
Q1
Q3.
208
4467
3819
4849
.37+
4424
12.6
11.1
...
TY
C31
48-6
65-1
...
4950
244
.21.
2Q
0Q
108
4545
5319
5637
.15+
4425
54.7
11.5
...
TY
C31
49-2
13-1
...
4029
813
7.7
66.3
Q0–
Q1
Q2.
308
4593
5420
0137
.63+
4424
51.1
11.1
...
TY
C31
62-1
077-
1..
.43
947
79.6
4.5
Q0–
Q1
Q2.
108
4600
2520
0222
.08+
4429
31.3
13.7
...
...
...
4396
898
.635
.9Q
1Q
2.2
0846
0993
2003
41.3
0+
4424
54.1
11.2
...
...
...
3828
229
2.5
219.
3Q
0–Q
1Q
4.2
0847
9107
1856
30.1
4+
4433
02.1
14.9
...
...
...
1357
031
0.5
324.
9Q
1–Q
4..
.08
4825
4019
0431
.01+
4435
20.1
14.1
...
...
...
1346
731
0.5
5.4
Q1–
Q4
...
A125, page 29 of 70
A&A 534, A125 (2011)
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0848
8065
1916
14.8
3+
4433
57.3
14.2
...
...
...
1316
131
0.5
5.9
Q1–
Q4
...
0848
9712
1918
59.5
0+
4433
43.7
8.6
A225
HD
1815
98..
.46
063
200.
712
6.4
Q0–
Q1
Q3.
208
4996
3919
3414
.23+
4430
13.4
10.5
...
TY
C31
47-8
49-1
...
4754
826
2.7
187.
3Q
0–Q
1Q
4.1
0850
7325
1944
27.1
0+
4433
21.1
10.5
...
TY
C31
48-1
229-
1..
.46
058
200.
712
6.4
Q0–
Q1
Q3.
208
5160
0819
5342
.72+
4435
42.6
10.6
A35
...
bina
ry�
4710
925
1.8
187.
3Q
1Q
4.1
0851
6686
1954
22.5
6+
4434
20.0
10.9
...
TY
C31
49-8
63-1
...
3857
229
2.5
219.
3Q
0–Q
1Q
4.2
0852
5286
2003
36.3
6+
4435
50.4
13.4
...
...
...
4177
768
.65.
1Q
1Q
2.1
0854
5456
1900
22.7
3+
4439
58.5
11.7
...
...
...
1585
944
.41.
2Q
1Q
008
5609
9619
2846
.42+
4440
08.5
10.6
...
TY
C31
46-8
02-1
...
4013
022
8.8
158.
5Q
0–Q
1Q
3.3
0856
5229
1935
28.3
2+
4440
09.6
11.1
...
TY
C31
47-5
09-1
...
4950
944
.21.
2Q
0Q
108
5796
1519
5244
.14+
4436
58.0
11.2
...
TY
C31
49-5
71-1
...
4440
232
1.5
248.
3Q
0–Q
1Q
4.3
0858
3770
1956
58.5
1+
4440
59.2
10.1
B9I
II35
HD
1891
77bi
nary
5530
632
1.5
4.5
Q0–
Q4
Q2.
108
5905
5320
0413
.46+
4440
18.9
11.2
...
...
...
4439
832
1.5
248.
3Q
0–Q
1Q
4.3
0860
8260
1856
07.4
2+
4447
24.9
10.9
...
TY
C31
31-1
633-
1..
.38
676
292.
521
9.3
Q0–
Q1
Q4.
208
6239
5319
2559
.76+
4444
45.3
9.4
A535
BD+
4431
34..
.45
466
109.
535
.3Q
0–Q
1Q
2.2
0865
1452
1959
54.1
9+
4442
18.6
10.8
...
TY
C31
49-3
07-1
...
4527
510
9.5
35.3
Q0–
Q1
Q2.
208
6557
1220
0450
.98+
4444
57.7
11.0
...
...
...
4440
132
1.5
248.
3Q
0–Q
1Q
4.3
0869
5156
1936
27.7
4+
4450
14.8
10.9
...
TY
C31
47-3
95-1
...
1585
744
.41.
2Q
1Q
008
7034
1319
4711
.45+
4450
53.6
8.7
kA2m
F026
HD
1872
54..
.39
574
228.
815
8.6
Q0–
Q1
Q3.
308
7148
8619
5910
.18+
4451
44.9
10.9
F35
HD
1896
37..
.14
442
321.
54.
5Q
0–Q
4..
.08
7170
6520
0140
.54+
4452
47.4
10.9
...
TY
C31
62-7
1-1
...
1585
044
.41.
2Q
1Q
008
7382
4418
5758
.94+
4459
17.2
8.2
A3V
20H
D17
6390
...
4603
520
0.7
126.
4Q
0–Q
1Q
3.2
0874
2449
1907
33.1
7+
4457
56.3
14.0
...
...
...
1386
231
0.5
4.5
Q1–
Q4
...
0874
6834
1916
37.0
6+
4456
01.4
13.0
...
...
...
1404
332
1.4
6.3
Q0–
Q4
...
0874
7415
1917
39.5
0+
4458
05.0
11.8
...
...
...
1409
332
1.4
5.9
Q0–
Q4
...
0874
8251
1919
07.7
3+
4457
54.0
11.2
F025
...
...
9504
626
2.7
187.
3Q
0–Q
1Q
4.1
0875
0029
1921
54.9
1+
4459
42.0
9.7
A5p
?25B
D+
4431
13..
.15
834
44.4
1.2
Q1
Q0
0876
6619
1946
09.1
9+
4459
09.8
10.8
...
...
bina
ry44
792
98.6
35.3
Q1
Q2.
208
8278
2119
4041
.38+
4505
58.7
11.1
...
TY
C35
56-3
407-
1..
.43
942
79.6
4.5
Q0–
Q1
Q2.
108
8384
5719
5309
.36+
4505
53.6
11.2
...
TY
C35
58-2
497-
1..
.77
120
292.
521
9.3
Q0–
Q1
Q4.
208
8693
0218
5845
.58+
4510
42.0
14.1
...
...
...
1380
331
0.5
4.5
Q1–
Q4
...
0886
9892
1900
00.7
4+
4508
03.5
12.6
...
...
...
4042
913
7.7
66.3
Q0–
Q1
Q2.
308
8713
0419
0256
.93+
4511
42.2
10.8
...
TY
C35
41-1
172-
1..
.50
616
321.
534
.8Q
0–Q
4Q
4.2
0888
1697
1921
36.0
2+
4507
06.9
10.6
A525
...
...
1585
444
.41.
2Q
1Q
008
9153
3520
0345
.55+
4510
02.9
9.6
A235
HD
1905
66..
.45
192
169.
895
.2Q
0–Q
1Q
3.1
0893
3391
1852
06.4
1+
4513
39.4
8.9
F035
HD
1752
01..
.49
159
44.2
1.2
Q0
Q1
0894
0640
1906
33.8
9+
4514
24.9
12.8
A525
...
...
4519
516
9.8
95.2
Q0–
Q1
Q3.
108
9729
6619
5132
.42+
4515
51.8
11.5
...
...
...
4519
416
9.8
95.2
Q0–
Q1
Q3.
108
9755
1519
5345
.58+
4513
09.3
9.5
A235
HD
1885
38..
.40
206
137.
766
.5Q
0–Q
1Q
2.3
0902
0157
1924
43.6
6+
4521
01.2
10.8
F2I
II25
BD+
4528
92..
.45
344
109.
135
.3Q
0–Q
1Q
2.2
0902
0199
1924
48.4
8+
4520
48.9
8.9
F2C
rEu?
35,F
0V37
HD
1828
95A
pva
riab
le11
1584
544
.41.
2Q
1Q
009
0523
6320
0207
.70+
4522
07.6
10.7
A235
HD
1902
26..
.47
457
262.
818
7.3
Q0–
Q1
Q4.
109
0720
1118
5355
.80+
4528
35.9
10.7
...
TY
C35
40-2
380-
1..
.45
179
169.
895
.2Q
0–Q
1Q
3.1
0907
3007
1856
09.0
7+
4526
59.2
10.6
...
TY
C35
40-2
491-
1..
.40
433
137.
766
.3Q
0–Q
1Q
2.3
0907
3985
1858
15.2
9+
4529
45.6
13.4
...
...
...
1411
232
1.5
5.7
Q0–
Q4
...
0907
7192
1905
34.8
5+
4526
47.0
14.5
...
...
...
1397
531
0.5
4.5
Q1–
Q4
...
A125, page 30 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0910
8615
1951
37.6
1+
4527
04.4
11.4
...
TY
C35
57-2
024-
1..
.42
088
79.6
4.5
Q0–
Q1
Q2.
109
1110
5619
5407
.15+
4524
06.7
10.5
F035
BD+
4530
06..
.38
573
292.
521
9.3
Q0–
Q1
Q4.
209
1178
7520
0146
.73+
4528
35.9
7.5
kA2m
F237
...
...
1582
844
.41.
2Q
1Q
009
1388
7218
5547
.57+
4531
27.5
10.1
...
TY
C35
40-1
966-
1..
.43
944
79.6
4.5
Q0–
Q1
Q2.
109
1437
8519
0642
.17+
4533
12.6
12.1
A525
...
...
1584
744
.41.
2Q
1Q
009
1472
2919
1411
.59+
4534
59.1
10.7
F0V
25T
YC
3542
-122
3-1
...
9434
426
2.8
187.
3Q
0–Q
1Q
4.1
0915
6808
1930
53.1
8+
4533
12.7
11.3
...
TY
C35
56-1
431-
1bi
nary�
4546
410
9.5
35.3
Q0–
Q1
Q2.
209
2016
4418
5258
.58+
4536
43.7
11.0
...
TY
C35
40-3
014-
1..
.46
072
200.
712
6.4
Q0–
Q1
Q3.
209
2046
7218
5958
.82+
4540
35.7
9.8
G35
BD+
4528
12..
.14
392
321.
54.
5Q
0–Q
4..
.09
2047
1819
0003
.36+
4536
27.5
8.8
kA3m
F037
HD
1768
43A
mst
ar40
057
228.
515
8.5
Q0–
Q1
Q3.
309
2100
3719
1207
.37+
4538
11.9
13.5
...
...
...
4013
422
8.8
158.
5Q
0–Q
1Q
3.3
0921
6367
1924
20.8
6+
4539
16.7
12.1
A2p
:25..
...
.15
842
44.4
1.2
Q1
Q0
0922
2942
1934
45.6
5+
4541
22.1
10.5
...
TY
C35
56-9
29-1
...
4503
916
9.8
95.2
Q0–
Q1
Q3.
109
2293
1819
4351
.82+
4541
09.0
9.6
F035
BD+
4529
62..
.40
433
137.
766
.3Q
0–Q
1Q
2.3
0924
6481
2003
33.7
0+
4537
13.7
9.0
A035
HD
1905
48..
.15
840
44.4
1.2
Q1
Q0
0926
4399
1853
05.9
8+
4544
20.3
14.3
...
...
...
1339
331
0.3
7.6
Q1–
Q4
...
0926
4462
1853
13.3
2+
4545
08.3
13.0
...
...
...
1399
232
0.9
5.0
Q0–
Q4
...
0926
7042
1858
52.0
6+
4544
58.2
13.4
...
...
...
4013
222
8.8
158.
5Q
0–Q
1Q
3.3
0926
8087
1901
09.0
7+
4547
36.5
12.1
...
...
...
2865
432
2.0
4.6
Q0–
Q4
Q0
0927
2082
1910
33.7
9+
4545
04.0
9.0
A727
HD
1794
58..
.44
436
109.
535
.4Q
0–Q
1Q
2.2
0927
4000
1914
57.7
9+
4542
32.2
14.2
...
...
...
1324
331
0.5
7.0
Q1–
Q4
...
0929
1618
1943
36.7
4+
4543
57.1
9.7
A535
BD+
4529
61..
.40
135
228.
815
8.5
Q0–
Q1
Q3.
309
3060
9520
0041
.90+
4547
59.3
12.4
...
...
...
4546
710
9.5
35.3
Q0–
Q1
Q2.
209
3243
3418
4926
.86+
4553
38.4
13.7
...
...
...
4711
325
1.8
187.
3Q
1Q
4.1
0932
7993
1857
59.7
6+
4553
29.7
9.8
K035
BD+
4528
05..
.14
398
321.
54.
6Q
0–Q
4..
.09
3362
1919
1636
.91+
4552
16.5
13.3
...
...
...
1391
132
0.7
5.7
Q0–
Q4
...
0935
1622
1941
26.8
6+
4553
53.1
9.1
F035
BD+
4529
55..
.43
586
79.6
4.5
Q0–
Q1
Q2.
109
3535
7219
4358
.61+
4553
54.7
10.6
...
TY
C35
57-1
126-
1..
.40
133
228.
815
8.5
Q0–
Q1
Q3.
309
3682
2020
0118
.62+
4552
05.7
11.3
...
...
...
3868
029
2.5
219.
3Q
0–Q
1Q
4.2
0938
6259
1849
12.5
5+
4554
26.8
13.3
...
J184
9125
5+45
5426
8..
.13
252
320.
47.
7Q
0–Q
4..
.09
3913
9519
0129
.78+
4555
14.4
11.4
...
TY
C35
41-2
014-
1..
.40
405
137.
766
.3Q
0–Q
1Q
2.3
0939
5246
1910
06.4
1+
4558
27.0
11.8
F225
...
...
1585
944
.41.
2Q
1Q
009
4086
9419
3445
.60+
4554
16.3
11.5
...
...
...
1586
044
.447
.9Q
1Q
009
4130
5719
4119
.15+
4557
45.8
9.6
A235
BD+
4529
54..
.40
419
137.
766
.3Q
0–Q
1Q
2.3
0945
0940
1858
53.4
2+
4600
17.7
12.7
...
...
...
4519
416
9.8
95.2
Q0–
Q1
Q3.
109
4515
9819
0028
.58+
4603
02.2
13.6
...
...
...
3966
421
7.8
158.
5Q
1Q
3.3
0945
3075
1903
44.0
9+
4603
46.0
12.4
...
...
...
4391
279
.64.
5Q
0–Q
1Q
2.1
0945
8750
1916
37.4
9+
4602
11.4
13.8
...
...
...
1342
931
0.5
6.5
Q1–
Q4
...
0947
3000
1939
48.6
7+
4601
38.5
10.1
...
TY
C35
56-3
291-
1..
.15
859
44.4
1.2
Q1
Q0
0948
9590
1959
40.4
2+
4601
56.3
10.9
...
TY
C35
58-1
6-1
...
3868
229
2.5
219.
3Q
0–Q
1Q
4.2
0949
0042
2000
11.6
9+
4605
43.3
10.5
...
TY
C35
58-1
852-
1..
.44
756
169.
895
.2Q
0–Q
1Q
3.1
0949
0067
2000
12.8
6+
4603
33.0
10.6
...
TY
C35
58-1
208-
1..
.77
094
292.
521
9.3
Q0–
Q1
Q4.
209
5092
9618
5055
.32+
4606
48.5
9.9
...
TY
C35
40-1
568-
1..
.15
841
44.4
1.2
Q1
Q0
0951
4879
1903
49.5
8+
4606
58.1
10.7
...
TY
C35
41-3
0-1
...
6345
432
1.5
4.9
Q0–
Q4
Q1
0952
0434
1916
48.2
2+
4609
49.7
14.5
...
...
...
1329
031
0.5
6.0
Q1–
Q4
...
0952
0864
1917
41.6
2+
4610
17.4
11.1
...
...
...
1442
832
1.5
4.5
Q0–
Q4
...
A125, page 31 of 70
A&A 534, A125 (2011)
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0953
2644
1937
26.4
7+
4610
07.4
12.7
...
...
...
4944
944
.21.
2Q
0Q
109
5334
4919
3837
.37+
4611
16.9
11.3
...
TY
C35
56-3
494-
1..
.45
449
109.
535
.3Q
0–Q
1Q
2.2
0953
3489
1938
41.7
1+
4607
21.6
13.0
...
...
...
4896
133
.40.
0..
.Q
109
5508
8620
0006
.74+
4607
30.5
11.0
...
TY
C35
58-1
238-
1..
.44
429
321.
524
8.3
Q0–
Q1
Q4.
309
5512
8120
0033
.60+
4611
55.4
10.4
A335
HD
1899
16..
.45
192
169.
895
.2Q
0–Q
1Q
3.1
0958
0794
1914
08.0
2+
4616
00.1
11.3
F0V
25..
...
.15
859
44.4
1.2
Q1
Q0
0958
2720
1918
17.1
8+
4612
46.6
12.7
...
...
bina
ry�
1444
032
1.5
4.6
Q0–
Q4
...
0959
3997
1936
47.7
6+
4617
34.0
12.6
...
...
...
3853
229
2.5
219.
3Q
0–Q
1Q
4.2
0959
4100
1936
55.9
9+
4615
18.5
13.0
...
...
...
4945
444
.21.
2Q
0Q
109
6047
6219
5059
.64+
4616
03.3
10.6
A535
TY
C35
57-1
418-
1..
.39
877
228.
815
8.6
Q0–
Q1
Q3.
309
6306
4018
4631
.25+
4619
16.1
13.7
...
...
...
1393
931
0.5
4.5
Q1–
Q4
...
0963
2537
1852
00.2
4+
4621
51.6
12.0
...
...
...
1586
144
.41.
2Q
1Q
009
6402
0419
1014
.09+
4620
42.6
11.5
F525
...
...
6348
132
1.5
4.5
Q0–
Q4
Q1
0964
2894
1916
18.0
7+
4621
16.1
11.1
F025
TY
C35
42-1
780-
1..
.46
081
200.
712
6.4
Q0–
Q1
Q3.
209
6439
8219
1838
.69+
4621
27.9
12.9
...
...
...
1396
932
0.7
6.5
Q0–
Q4
...
0965
0390
1929
17.8
1+
4621
26.1
9.4
A035
HD
1838
29..
.45
231
109.
535
.3Q
0–Q
1Q
2.2
0965
1065
1930
25.6
3+
4622
52.2
11.1
...
TY
C35
56-7
68-1
...
4951
044
.21.
2Q
0Q
109
6547
8919
3628
.80+
4618
39.2
13.3
...
...
...
4022
713
7.7
66.3
Q0–
Q1
Q2.
309
6550
5519
3651
.91+
4623
20.4
11.4
A428
NG
C68
1126
NG
C68
1140
429
137.
766
.3Q
0–Q
1Q
2.3
0965
5114
1936
58.1
8+
4620
22.6
12.1
A428
NG
C68
1118
NG
C68
1152
782
321.
54.
5Q
0–Q
4Q
2.3
0965
5151
1937
01.1
8+
4622
59.4
13.2
...
NG
C68
1116
NG
C68
1148
853
33.4
0.0
...
Q1
0965
5177
1937
03.2
4+
4619
25.7
10.9
A428
NG
C68
1170
NG
C68
1143
883
79.6
4.5
Q0–
Q1
Q2.
109
6553
9319
3721
.38+
4619
53.3
12.6
...
...
...
4757
426
2.8
187.
3Q
0–Q
1Q
4.1
0965
5422
1937
24.1
0+
4623
52.1
11.5
...
NG
C68
1139
NG
C68
1145
605
189.
712
6.4
Q1
Q3.
209
6554
3319
3724
.86+
4618
39.0
11.9
B728
NG
C68
1111
4N
GC
6811
,bin
ary�
1299
431
0.5
6.8
Q1–
Q4
...
0965
5438
1937
25.2
2+
4619
35.7
12.3
...
...
...
4750
526
2.8
187.
3Q
0–Q
1Q
4.1
0965
5487
1937
29.2
1+
4622
39.1
13.1
...
...
...
4895
633
.40.
0..
.Q
109
6555
0119
3731
.22+
4621
31.9
12.4
A528
NG
C68
1149
NG
C68
1147
543
262.
818
7.3
Q0–
Q1
Q4.
109
6555
1419
3732
.11+
4619
15.0
11.5
A428
NG
C68
1111
3N
GC
6811
,bin
ary
6352
332
1.5
4.5
Q0–
Q4
Q1
0965
5800
1937
53.1
6+
4618
28.8
12.7
...
...
...
7724
229
2.5
219.
3Q
0–Q
1Q
4.2
0965
6348
1938
45.2
9+
4618
23.6
10.3
...
TY
C35
56-3
198-
1..
.49
500
44.2
1.2
Q0
Q1
0966
4869
1950
12.1
0+
4618
52.3
11.2
...
TY
C35
57-3
68-1
...
4951
044
.21.
2Q
0Q
109
6732
9320
0011
.23+
4619
17.0
10.6
A035
HD
1898
61..
.39
895
228.
815
8.6
Q0–
Q1
Q3.
309
6932
8218
5114
.90+
4626
56.1
10.4
...
TY
C35
40-1
359-
1..
.45
385
109.
535
.3Q
0–Q
1Q
2.2
0969
6853
1859
33.4
3+
4624
11.3
11.3
...
TY
C35
41-9
67-1
...
4186
979
.65.
1Q
0–Q
1Q
2.1
0969
9950
1906
55.3
2+
4625
08.0
13.4
...
...
...
4013
322
8.8
158.
5Q
0–Q
1Q
3.3
0970
0145
1907
23.5
7+
4628
21.7
12.7
...
...
...
4042
613
7.7
66.3
Q0–
Q1
Q2.
309
7003
2219
0750
.71+
4629
11.9
12.7
...
AS
AS
J190
751+
4629
.2..
.45
194
169.
895
.2Q
0–Q
1Q
3.1
0970
0679
1908
42.5
3+
4624
14.8
9.9
G2I
II25
BD+
4626
33..
.40
416
137.
766
.3Q
0–Q
1Q
2.3
0970
3601
1915
25.0
3+
4628
10.6
14.3
...
...
...
1349
531
0.5
5.7
Q1–
Q4
...
0971
6107
1936
56.7
6+
4626
58.0
13.1
...
...
...
4844
633
.40.
1..
.Q
109
7163
5019
3717
.98+
4627
45.3
12.5
...
...
bina
ry�
4940
144
.21.
2Q
0Q
109
7169
4719
3811
.95+
4628
02.5
12.9
...
...
...
4930
244
.21.
2Q
0Q
109
7605
3119
0659
.78+
4632
20.4
9.5
F035
BD+
4626
21..
.43
946
79.6
4.5
Q0–
Q1
Q2.
109
7627
1319
1212
.26+
4630
50.3
11.1
F025
...
...
4013
422
8.8
158.
5Q
0–Q
1Q
3.3
0976
4712
1916
49.5
8+
4632
01.7
13.9
...
...
...
1315
831
0.5
6.3
Q1–
Q4
...
A125, page 32 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
0976
4965
1917
24.9
1+
4635
35.2
8.9
A5m
p25H
D18
1206
Ap
orA
mst
ar49
507
44.2
1.2
Q0
Q1
0977
3512
1932
21.7
7+
4635
29.8
10.0
A235
BD+
4627
14..
.15
860
44.4
1.2
Q1
Q0
0977
5385
1935
24.7
0+
4635
26.9
11.1
...
TY
C35
56-1
982-
1..
.43
914
79.6
4.5
Q0–
Q1
Q2.
109
7754
5419
3532
.02+
4635
22.3
8.2
F1I
V29
HD
1851
15hy
brid
1510
327
228.
74.
5Q
0–Q
3..
.09
7764
7419
3700
.19+
4631
14.2
13.0
...
...
...
6342
632
1.5
4.5
Q0–
Q4
Q1
0977
7532
1938
31.0
6+
4631
34.1
10.9
...
TY
C35
56-3
228-
1..
.57
342
321.
54.
5Q
0–Q
4Q
3.1
0979
0479
1955
05.5
7+
4635
05.1
9.9
A235
HD
1888
33..
.15
822
44.4
1.2
Q1
Q0
0981
2351
1846
10.3
2+
4637
51.0
7.9
A035
HD
1740
19..
.45
192
169.
895
.2Q
0–Q
1Q
3.1
0981
3078
1848
21.5
5+
4641
43.7
11.9
...
...
...
1585
944
.41.
2Q
1Q
009
8182
6919
0040
.73+
4639
58.7
11.4
...
...
...
1585
144
.41.
2Q
1Q
009
8360
2019
3543
.10+
4640
03.0
12.8
...
...
...
1446
332
1.5
4.5
Q0–
Q4
...
0984
5907
1949
30.4
6+
4640
01.7
11.6
...
...
...
1586
044
.41.
2Q
1Q
009
8511
4219
5512
.05+
4639
55.9
7.6
kA5h
A7m
F320
,V
2094
Cyg
Am
star
,or
4778
731
0.5
4.5
Q1–
Q4
Q2.
3A
7pC
rEu40
α2
CV
n12
0987
4181
1851
26.5
7+
4646
48.0
10.8
...
...
...
3867
029
2.5
219.
3Q
0–Q
1Q
4.2
0988
1909
1910
03.5
8+
4642
16.1
11.4
F225
...
...
4384
579
.64.
5Q
0–Q
1Q
2.1
0988
5882
1918
45.0
5+
4644
27.8
14.1
...
...
...
1380
931
0.5
5.0
Q1–
Q4
...
0990
9300
1953
27.1
7+
4645
39.5
11.5
...
...
...
8877
832
1.5
248.
3Q
0–Q
1Q
4.3
0991
3481
1958
20.7
6+
4645
55.9
10.9
...
TY
C35
58-6
37-1
...
1375
944
.14.
6Q
1Q
009
9442
0819
1358
.44+
4650
00.2
14.2
...
...
...
1398
031
0.5
4.5
Q1–
Q4
...
0994
4730
1915
11.5
4+
4648
52.2
14.1
...
...
...
1398
031
0.5
4.6
Q1–
Q4
...
0997
0568
1955
01.1
5+
4652
29.2
9.6
A235
HD
1888
32..
.40
424
137.
766
.3Q
0–Q
1Q
2.3
0999
1621
1844
43.2
5+
4655
47.6
13.9
...
...
...
1327
631
0.5
6.1
Q1–
Q4
...
0999
1766
1845
08.0
2+
4658
02.0
14.2
...
...
...
1349
531
0.5
5.7
Q1–
Q4
...
0999
4789
1852
50.4
5+
4659
48.0
13.8
...
...
...
1332
231
0.5
6.4
Q1–
Q4
...
0999
5464
1854
26.0
2+
4659
11.5
13.2
...
...
...
1436
032
1.5
4.9
Q0–
Q4
...
1000
0056
1905
07.5
1+
4659
01.5
14.2
...
...
...
3658
328
.93.
9..
.Q
4.2
1000
2897
1911
41.7
1+
4655
12.7
12.2
...
...
...
1585
344
.41.
2Q
1Q
010
0045
1019
1455
.08+
4655
02.6
14.2
...
...
...
1394
131
0.5
4.5
Q1–
Q4
...
1000
6158
1918
07.3
9+
4657
26.2
9.7
K035
BD+
4626
65..
.14
431
321.
54.
5Q
0–Q
4..
.10
0145
4819
3214
.23+
4654
20.9
10.7
...
TY
C35
60-2
590-
1..
.47
550
262.
818
7.3
Q0–
Q1
Q4.
110
0309
4319
5412
.43+
4656
12.6
11.3
...
TY
C35
62-2
361-
1..
.38
677
292.
521
9.3
Q0–
Q1
Q4.
210
0357
7220
0005
.26+
4654
22.8
11.1
...
TY
C35
62-3
2-1
...
4390
379
.64.
5Q
0–Q
1Q
2.1
1005
6217
1850
47.5
2+
4700
23.3
12.9
...
...
...
1369
932
0.6
6.8
Q0–
Q4
...
1005
6297
1851
00.2
4+
4700
11.3
13.4
...
...
...
4013
722
8.8
158.
5Q
0–Q
1Q
3.3
1005
7129
1852
50.3
8+
4700
27.8
13.9
...
...
...
1393
031
0.5
4.9
Q1–
Q4
...
1006
2593
1904
12.9
1+
4703
05.0
13.3
...
...
...
1439
932
1.5
4.6
Q0–
Q4
...
1006
4111
1907
24.9
1+
4705
13.2
10.3
A535
BD+
4626
24bi
nary
4446
210
9.5
35.9
Q0–
Q1
Q2.
210
0652
4419
0947
.30+
4704
34.5
12.3
...
...
...
4394
579
.64.
5Q
0–Q
1Q
2.1
1006
8892
1917
00.3
1+
4705
38.4
11.4
...
...
...
1443
332
1.5
4.6
Q0–
Q4
...
1006
9934
1918
56.1
4+
4705
14.4
11.3
...
TY
C35
47-4
70-1
...
8832
632
1.5
248.
3Q
0–Q
1Q
4.3
1007
3601
1924
48.7
0+
4702
41.1
11.5
...
TY
C35
47-2
0-1
...
433
213
321.
64.
5..
.Q
0–Q
4.3
1009
0345
1949
00.1
2+
4705
05.2
11.3
...
TY
C35
61-2
58-1
...
4517
010
9.5
35.4
Q0–
Q1
Q2.
210
0964
9919
5554
.07+
4705
24.2
6.9
A3V
30H
D18
9013
...
3797
725
.90.
0..
.Q
3.3
1011
9517
1845
55.4
6+
4707
21.6
9.9
...
TY
C35
44-1
245-
1..
.52
795
321.
54.
5Q
0–Q
4Q
2.3
1013
0777
1910
00.3
4+
4711
12.1
12.6
...
...
...
4034
813
7.7
66.3
Q0–
Q1
Q2.
3
A125, page 33 of 70
A&A 534, A125 (2011)Ta
ble
1.co
ntin
ued.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
1013
4600
1917
02.9
3+
4708
52.0
13.6
...
...
...
1428
232
1.3
4.9
Q0–
Q4
...
1013
4800
1917
24.6
0+
4708
32.4
11.8
...
...
...
1585
844
.41.
2Q
1Q
010
1405
1319
2625
.46+
4706
05.4
11.0
...
...
...
435
810
321.
64.
5..
.Q
0–Q
4.3
1014
0665
1926
38.4
7+
4706
08.0
12.1
...
...
...
432
553
321.
64.
5..
.Q
0–Q
4.3
1016
4569
1957
20.3
5+
4709
58.8
11.4
...
TY
C35
62-1
846-
1..
.39
573
137.
766
.5Q
0–Q
1Q
2.3
1020
6340
1924
58.8
2+
4714
57.3
11.2
B1
V85
0C
ygbi
nary
1340
303
432
1.6
324.
3..
.Q
0–Q
4.3
1020
8303
1928
12.5
8+
4714
04.0
11.9
...
...
...
432
367
321.
64.
5..
.Q
0–Q
4.3
1020
8345
1928
17.0
4+
4717
14.6
11.6
...
...
...
4606
920
0.7
126.
4Q
0–Q
1Q
3.2
1021
3987
1937
05.1
6+
4717
19.5
11.4
...
TY
C35
60-2
645-
1bi
nary�
3915
512
6.8
66.7
Q1
Q2.
310
2539
4318
4724
.48+
4718
05.7
10.2
...
TY
C35
44-2
546-
1..
.43
944
79.6
4.5
Q0–
Q1
Q2.
110
2545
4718
4846
.27+
4722
26.3
13.9
...
...
...
1339
331
0.5
5.6
Q1–
Q4
...
1026
4728
1910
59.6
6+
4720
21.6
9.9
A235
BD+
4727
69..
.15
840
44.4
1.2
Q1
Q0
1026
6959
1915
19.4
2+
4722
59.2
15.0
...
...
...
1359
831
0.5
5.6
Q1–
Q4
...
1027
3246
1926
05.7
6+
4721
30.1
10.9
...
...
...
432
872
321.
64.
5..
.Q
0–Q
4.3
1027
3384
1926
19.5
4+
4723
36.7
11.5
...
...
...
436
154
321.
64.
5..
.Q
0–Q
4.3
1027
3960
1927
17.4
2+
4718
39.2
11.7
...
...
...
431
979
321.
64.
5..
.Q
0–Q
4.3
1027
4244
1927
44.7
4+
4718
34.9
11.5
...
...
...
373
959
321.
635
.3..
.Q
0–Q
4.3
1028
1360
1938
39.2
2+
4723
24.5
11.1
...
TY
C35
60-1
923-
1..
.43
712
30.0
0.0
Q1
Q3.
210
2892
1119
4858
.75+
4723
25.7
10.2
A235
BD+
4729
27..
.45
449
109.
535
.3Q
0–Q
1Q
2.2
1033
8279
1925
28.9
4+
4726
07.8
12.0
...
...
...
436
158
321.
64.
5..
.Q
0–Q
4.3
1033
9342
1927
05.3
5+
4724
08.2
12.0
...
...
...
432
133
321.
64.
5..
.Q
0–Q
4.3
1034
0511
1928
56.1
6+
4724
44.0
11.6
...
...
...
431
104
321.
64.
5..
.Q
0–Q
4.3
1034
1072
1929
46.2
0+
4724
09.4
9.0
F835
HD
1839
54..
.14
797
810
9.7
4.5
...
Q0–
Q2.
210
3550
5519
4916
.61+
4724
27.3
9.3
A235
HD
1877
09..
.45
466
109.
535
.3Q
0–Q
1Q
2.2
1036
1229
1956
08.9
3+
4728
30.5
10.9
...
TY
C35
62-1
455-
1..
.40
046
137.
766
.3Q
0–Q
1Q
2.3
1038
3933
1844
15.6
5+
4734
09.2
13.3
...
...
...
1372
932
0.9
5.8
Q0–
Q4
...
1038
5459
1848
19.3
9+
4732
07.6
10.5
...
TY
C35
44-2
086-
1..
.10
335
228.
74.
5Q
0–Q
4Q
4.1
1038
9037
1856
44.6
2+
4732
01.8
10.4
K35
BD+
4727
21..
.14
423
321.
54.
6Q
0–Q
4..
.10
3943
3219
0802
.76+
4733
08.8
13.3
...
...
...
1445
732
1.5
4.5
Q0–
Q4
...
1044
8764
1844
12.4
1+
4740
31.0
10.8
...
...
...
4519
416
9.8
95.2
Q0–
Q1
Q3.
110
4505
5018
4844
.04+
4736
50.9
13.2
...
...
...
1371
932
1.2
4.6
Q0–
Q4
...
1045
0675
1849
01.1
5+
4736
27.9
12.8
...
...
...
1380
432
1.4
6.2
Q0–
Q4
...
1045
1090
1849
55.9
2+
4738
14.4
9.2
A235
HD
1747
89..
.43
946
79.6
4.5
Q0–
Q1
Q2.
110
4512
5018
5015
.94+
4738
22.5
14.1
...
...
...
1327
431
0.5
5.7
Q1–
Q4
...
1045
3475
1855
16.6
3+
4737
33.0
14.2
...
...
...
1390
731
0.1
4.5
Q1–
Q4
...
1046
7969
1923
32.4
7+
4740
28.6
12.0
...
...
...
431
107
321.
64.
5..
.Q
0–Q
4.3
1047
1914
1930
03.0
2+
4736
18.6
10.7
...
TY
C35
60-2
319-
1..
.47
572
262.
818
7.3
Q0–
Q1
Q4.
110
4848
0819
4804
.58+
4740
45.0
10.6
...
TY
C35
61-1
801-
1..
.40
134
228.
815
8.5
Q0–
Q1
Q3.
310
5261
3719
1142
.82+
4745
27.1
10.2
M731
TY
C35
46-1
494-
1..
.13
014
320.
58.
2Q
0–Q
4..
.10
5266
1519
1239
.94+
4747
43.4
14.4
...
...
...
1345
031
0.4
6.0
Q1–
Q4
...
1053
3506
1924
50.4
2+
4743
47.5
11.5
...
...
...
433
130
321.
64.
5..
.Q
0–Q
4.3
1053
3616
1925
00.9
1+
4747
49.8
9.6
A535
BD+
4728
28..
.40
147
137.
766
.5Q
0–Q
1Q
2.3
1053
4629
1926
43.2
7+
4746
08.7
11.3
...
...
...
431
681
321.
64.
5..
.Q
0–Q
4.3
1053
6147
1929
11.9
3+
4744
43.0
11.6
...
...
...
449
999
321.
94.
5Q
0–Q
4Q
0–Q
4.3
1053
7907
1932
08.1
8+
4742
28.8
9.9
F035
BD+
4728
56..
.15
860
44.4
1.2
Q1
Q0
1054
9292
1948
10.5
6+
4745
33.3
11.0
...
...
...
4442
732
1.5
248.
3Q
0–Q
1Q
4.3
A125, page 34 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
1054
9371
1948
16.1
5+
4742
28.8
9.5
A535
BD+
4729
22..
.43
939
79.6
4.5
Q0–
Q1
Q2.
110
5868
3719
0302
.38+
4748
48.9
12.4
...
...
...
4531
610
9.5
35.3
Q0–
Q1
Q2.
210
5908
5719
1138
.54+
4753
45.3
10.0
F035
BD+
4727
73..
.15
851
44.4
1.2
Q1
Q0
1060
4429
1934
36.4
6+
4750
14.0
9.9
F035
BD+
4728
68bi
nary�
5253
813
7.9
101.
1..
.Q
0–Q
2.3
1061
5125
1948
58.9
2+
4751
56.6
10.3
...
...
...
4038
513
7.7
66.3
Q0–
Q1
Q2.
310
6474
9318
5145
.14+
4757
29.4
11.7
...
...
...
1586
044
.41.
2Q
1Q
010
6476
1118
5204
.49+
4759
54.2
12.0
...
...
...
1585
144
.41.
2Q
1Q
010
6478
6018
5237
.75+
4755
26.2
13.3
...
...
...
1366
732
1.0
7.4
Q0–
Q4
...
1064
8728
1854
35.7
6+
4756
52.3
11.4
...
...
...
4410
232
1.5
248.
4Q
0–Q
1Q
4.3
1065
2134
1902
08.2
8+
4755
45.2
11.9
...
...
...
1124
925
2.5
4.5
Q0–
Q4
...
1065
8302
1915
07.6
8+
4754
19.0
13.1
...
...
...
4359
179
.64.
5Q
0–Q
1Q
2.1
1065
8802
1916
03.0
0+
4757
27.0
11.9
...
...
...
1585
444
.41.
2Q
1Q
010
6638
9219
2445
.10+
4758
53.9
11.8
...
...
...
430
810
321.
64.
5..
.Q
0–Q
4.3
1066
4703
1926
02.4
7+
4758
53.9
10.9
...
TY
C35
47-1
575-
1..
.44
427
321.
524
8.3
Q0–
Q1
Q4.
310
6649
7519
2628
.49+
4758
11.7
7.6
A235
HD
1832
80..
.38
016
25.9
0.0
...
Q3.
310
6757
6219
4305
.02+
4757
32.6
10.9
...
TY
C35
61-3
71-1
...
1584
244
.41.
2Q
1Q
010
6845
8719
5336
.67+
4759
53.1
11.0
...
TY
C35
62-4
61-1
...
4443
032
1.5
248.
3Q
0–Q
1Q
4.3
1068
4673
1953
42.4
1+
4758
27.2
11.1
...
TY
C35
62-8
05-1
...
4951
144
.21.
2Q
0Q
110
6856
5319
5450
.30+
4755
43.1
11.1
...
TY
C35
62-3
01-1
...
4946
544
.21.
2Q
0Q
110
6867
5219
5603
.43+
4758
55.8
11.3
...
TY
C35
62-7
07-1
...
4545
510
9.5
35.3
Q0–
Q1
Q2.
210
7097
1618
4529
.64+
4805
33.0
13.9
...
...
...
1350
131
0.5
6.1
Q1–
Q4
...
1071
3398
1853
42.4
3+
4802
25.8
11.2
...
TY
C35
44-1
186-
1..
.15
860
44.4
1.2
Q1
Q0
1071
7871
1903
14.8
8+
4802
56.6
10.5
...
TY
C35
45-2
523-
1..
.40
421
137.
766
.3Q
0–Q
1Q
2.3
1072
3718
1915
05.9
3+
4800
40.9
14.2
...
...
...
1365
031
0.5
5.9
Q1–
Q4
...
1073
0618
1926
30.4
8+
4805
34.8
10.5
...
TY
C35
47-1
205-
1..
.41
166
532
1.6
7.3
...
Q0–
Q4.
310
7759
6818
4515
.58+
4806
56.6
10.6
...
TY
C35
44-7
33-1
...
3991
022
8.8
158.
6Q
0–Q
1Q
3.3
1077
7541
1848
50.1
4+
4806
45.9
14.1
...
...
...
1265
231
0.5
7.3
Q1–
Q4
...
1077
7903
1849
40.4
2+
4807
13.9
10.2
...
BD+
4727
05..
.43
945
79.6
4.5
Q0–
Q1
Q2.
110
7786
4018
5117
.76+
4806
19.5
13.8
...
...
...
1319
031
0.5
7.4
Q1–
Q4
...
1078
3150
1901
20.7
6+
4808
30.9
13.1
...
...
...
1129
925
2.5
4.5
Q0–
Q4
...
1078
8451
1912
37.8
0+
4808
15.5
11.1
...
TY
C35
46-1
364-
1..
.40
136
228.
815
8.5
Q0–
Q1
Q3.
310
7975
2619
2749
.37+
4810
36.3
8.3
B532
HD
1835
58..
.14
772
710
9.7
4.5
...
Q0–
Q2.
210
7978
4919
2820
.69+
4810
57.2
10.8
...
TY
C35
47-1
020-
1bi
nary
435
432
321.
65.
1..
.Q
0–Q
4.3
1081
3970
1950
47.2
1+
4810
17.3
11.3
...
TY
C35
61-1
538-
1..
.40
408
137.
766
.3Q
0–Q
1Q
2.3
1081
5466
1952
28.6
3+
4810
28.0
11.2
...
TY
C35
61-4
34-1
bina
ry�
4394
679
.64.
5Q
0–Q
1Q
2.1
1085
3783
1913
30.6
0+
4812
21.2
11.0
...
TY
C35
46-3
74-1
...
4442
832
1.5
248.
3Q
0–Q
1Q
4.3
1086
1649
1927
58.3
7+
4817
37.9
12.1
...
...
...
431
057
321.
64.
5..
.Q
0–Q
4.3
1090
2738
1845
46.9
9+
4823
01.6
12.5
...
...
...
970
621
7.8
5.4
Q1–
Q3
...
1092
0182
1927
36.1
7+
4819
09.9
11.8
...
...
...
430
256
321.
64.
5..
.Q
0–Q
4.3
1092
0273
1927
45.7
7+
4819
45.4
11.9
...
...
...
430
371
321.
64.
5..
.Q
0–Q
4.3
1092
0447
1928
04.9
7+
4818
27.6
11.2
...
TY
C35
47-1
099-
1..
.44
429
321.
524
8.3
Q0–
Q1
Q4.
310
9716
7419
1909
.79+
4826
53.3
13.8
...
...
...
1273
431
0.5
5.7
Q1–
Q4
...
1097
5247
1926
34.3
7+
4829
14.9
11.1
...
...
...
4855
644
.21.
3Q
0Q
110
9778
5919
3137
.99+
4826
33.1
8.8
A235
HD
1843
33..
.49
510
44.2
1.2
Q0
Q1
1098
8009
1948
08.2
3+
4827
37.8
10.2
...
TY
C35
61-6
22-1
...
4394
779
.64.
5Q
0–Q
1Q
2.1
1101
3201
1848
00.0
7+
4832
32.0
9.3
A235
BD+
4827
68..
.43
656
79.6
4.5
Q0–
Q1
Q2.
1
A125, page 35 of 70
A&A 534, A125 (2011)Ta
ble
1.co
ntin
ued.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
1101
7401
1859
53.8
1+
4833
17.0
14.6
...
...
...
1087
324
1.5
150.
6Q
1–Q
4..
.11
0205
2119
0739
.65+
4834
19.4
11.4
...
...
...
338
509
252.
75.
1..
.Q
0–Q
4.1
1102
1188
1909
15.5
8+
4833
38.9
11.3
...
...
...
342
509
252.
74.
5..
.Q
0–Q
4.1
1102
7270
1922
35.1
4+
4835
49.5
11.3
...
TY
C35
47-1
058-
1..
.88
810
321.
524
8.3
Q0–
Q1
Q4.
311
0679
7218
4826
.30+
4836
16.9
14.3
...
...
...
1255
031
0.5
7.2
Q1–
Q4
...
1106
9435
1852
28.2
5+
4840
08.7
14.5
...
...
...
1330
031
0.5
5.9
Q1–
Q4
...
1108
2830
1924
46.8
7+
4838
19.8
10.9
...
TY
C35
47-7
59-1
bina
ry38
597
292.
521
9.3
Q0–
Q1
Q4.
211
0904
0519
3912
.38+
4836
24.2
9.6
A535
BD+
4829
25..
.40
423
137.
766
.3Q
0–Q
1Q
2.3
1112
2763
1852
27.2
4+
4847
55.6
13.9
...
...
...
1329
731
0.5
5.8
Q1–
Q4
...
1112
5764
1901
09.6
7+
4842
57.5
11.1
...
TY
C35
45-6
9-1
...
4904
133
.40.
0..
.Q
111
1271
9019
0437
.85+
4846
32.4
11.4
...
...
...
1585
644
.41.
2Q
1Q
011
1280
4119
0659
.26+
4843
27.7
10.8
...
...
...
339
574
252.
74.
6..
.Q
0–Q
4.1
1112
8126
1907
12.1
9+
4847
45.1
11.3
...
...
...
338
231
252.
75.
1..
.Q
0–Q
4.1
1112
9289
1910
15.1
9+
4844
32.1
11.7
...
...
...
336
245
252.
75.
1..
.Q
0–Q
4.1
1118
0361
1904
04.6
1+
4852
00.3
7.7
A2/
3V20
HD
1778
76..
.39
548
217.
815
8.5
Q1
Q3.
311
1827
1619
1024
.26+
4850
41.5
12.0
...
...
...
337
715
252.
75.
1..
.Q
0–Q
4.1
1118
3399
1912
06.2
9+
4852
21.4
12.8
...
...
...
1132
425
2.5
4.6
Q0–
Q4
...
1118
3539
1912
25.8
0+
4850
21.2
10.8
...
TY
C35
50-4
56-1
...
4518
016
9.8
95.2
Q0–
Q1
Q3.
111
1930
4619
3245
.31+
4852
07.6
9.6
A235
BD+
4829
12..
.40
255
137.
766
.3Q
0–Q
1Q
2.3
1119
7934
1941
29.0
6+
4848
22.0
11.0
...
TY
C35
65-5
14-1
...
4432
432
1.5
248.
3Q
0–Q
1Q
4.3
1119
9412
1943
51.5
8+
4848
07.5
10.9
...
TY
C35
65-6
74-1
...
5816
032
1.6
248.
3Q
1Q
0–Q
4.3
1123
0518
1855
50.5
0+
4855
32.1
13.6
...
...
...
1045
424
1.5
5.7
Q1–
Q4
...
1123
2922
1902
17.3
3+
4854
33.0
14.1
...
...
...
1029
024
1.5
6.2
Q1–
Q4
...
1123
3189
1902
52.4
2+
4856
31.6
13.5
...
...
...
1054
525
1.5
5.6
Q0–
Q4
...
1123
4888
1907
00.2
2+
4856
07.0
11.9
...
...
...
337
220
252.
75.
1..
.Q
0–Q
4.1
1123
5721
1909
10.6
1+
4855
39.1
11.9
...
...
...
338
373
252.
75.
1..
.Q
0–Q
4.1
1123
6253
1910
39.3
4+
4856
39.3
12.0
...
...
...
328
959
252.
75.
1..
.Q
0–Q
4.1
1124
0653
1919
53.1
8+
4854
03.6
10.6
...
TY
C35
51-5
23-1
...
7727
229
2.5
219.
3Q
0–Q
1Q
4.2
1125
3226
1943
39.6
2+
4855
44.2
8.4
F535
HD
1867
00..
.56
546
321.
535
.3Q
0–Q
4Q
2.2
1128
5767
1901
12.1
9+
4902
05.6
10.3
F235
BD+
4828
15..
.45
466
109.
535
.3Q
0–Q
1Q
2.2
1128
8686
1908
39.3
1+
4903
12.5
11.8
...
TY
C35
50-8
92-1
...
1586
144
.41.
2Q
1Q
011
2901
9719
1240
.70+
4902
36.3
11.4
...
TY
C35
50-4
2-1
...
337
111
252.
75.
1..
.Q
0–Q
4.1
1130
9335
1948
47.2
1+
4905
50.0
10.5
...
TY
C35
65-1
318-
1..
.45
182
169.
895
.2Q
0–Q
1Q
3.1
1134
0063
1904
11.6
6+
4910
52.6
14.4
...
...
...
1061
724
1.5
4.9
Q1–
Q4
...
1134
0713
1905
42.7
9+
4908
47.4
13.0
...
...
...
4607
620
0.7
126.
4Q
0–Q
1Q
3.2
1134
2032
1909
19.6
3+
4911
48.3
12.8
...
...
...
1133
225
2.5
4.5
Q0–
Q4
...
1139
3580
1906
05.3
5+
4917
49.7
11.5
...
...
...
340
340
252.
74.
5..
.Q
0–Q
4.1
1139
4216
1907
48.4
3+
4914
02.1
12.0
...
...
...
338
263
252.
75.
1..
.Q
0–Q
4.1
1139
5018
1909
55.4
9+
4915
04.5
10.8
...
TY
C35
50-3
00-1
...
335
442
252.
75.
1..
.Q
0–Q
4.1
1139
5028
1909
57.8
6+
4916
44.4
11.7
...
...
...
336
659
252.
74.
5..
.Q
0–Q
4.1
1139
5392
1910
54.3
4+
4917
04.6
12.6
...
...
...
4546
110
9.5
35.3
Q0–
Q1
Q2.
211
4029
5119
2732
.81+
4915
23.5
8.1
kF3h
A9m
F514
HD
1834
89A
mst
ar14
2872
132
2.0
4.5
Q0–
Q4
Q0
1144
5774
1905
21.0
0+
4918
01.6
11.9
...
...
...
341
474
252.
75.
1..
.Q
0–Q
4.1
1144
5913
1905
40.6
3+
4918
20.8
8.5
kA7h
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HD
1783
27A
m,h
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524
170
228.
54.
5Q
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4461
4319
0619
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4920
52.2
11.8
...
...
...
334
372
252.
75.
1..
.Q
0–Q
4.1
1144
6181
1906
24.3
6+
4922
19.3
11.9
...
...
...
338
310
252.
74.
8..
.Q
0–Q
4.1
A125, page 36 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
1.co
ntin
ued.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
1144
7883
1911
04.9
2+
4919
22.3
9.8
F035
BD+
4929
51..
.35
151
725
3.0
4.5
Q0–
Q4
Q0–
Q4.
111
4479
5319
1113
.92+
4922
41.1
11.3
...
...
...
342
439
252.
74.
5..
.Q
0–Q
4.1
1144
8266
1912
02.9
3+
4918
46.2
11.5
...
...
...
339
553
252.
74.
5..
.Q
0–Q
4.1
1144
9931
1915
46.0
8+
4919
42.5
12.1
...
...
...
1278
032
0.0
7.8
Q0–
Q4
...
1145
4008
1924
45.9
4+
4923
03.2
11.1
...
TY
C35
51-2
195-
1..
.94
458
262.
818
7.5
Q0–
Q1
Q4.
111
4947
6518
5757
.77+
4924
56.4
11.1
...
TY
C35
49-1
627-
1..
.49
461
44.2
1.2
Q0
Q1
1149
7012
1903
53.0
4+
4925
39.1
9.7
F035
BD+
4929
27..
.49
507
44.2
1.2
Q0
Q1
1149
8538
1907
46.8
5+
4929
07.3
7.3
F535
HD
1788
74..
.10
495
879
.74.
5..
.Q
0–Q
2.1
1149
9354
1909
50.9
3+
4925
10.5
12.0
...
...
...
298
877
252.
730
.9..
.Q
0–Q
4.1
1149
9453
1910
05.3
5+
4925
47.5
10.7
...
TY
C35
50-1
330-
1..
.34
256
225
2.7
4.5
...
Q0–
Q4.
111
5020
7519
1607
.75+
4928
46.6
14.2
...
...
...
1378
830
9.6
4.6
Q1–
Q4
...
1150
8397
1929
38.3
0+
4929
48.4
10.7
...
...
...
3864
329
2.5
219.
3Q
0–Q
1Q
4.2
1150
9728
1932
21.2
4+
4927
49.4
9.7
A232
BD+
4930
39..
.15
835
44.4
1.6
Q1
Q0
1151
5690
1942
55.3
0+
4925
27.0
10.6
...
TY
C35
65-5
80-1
...
3811
429
2.5
219.
4Q
0–Q
1Q
4.2
1154
9609
1904
23.6
4+
4932
58.2
13.2
...
...
...
1089
825
2.1
4.8
Q0–
Q4
...
1155
1622
1910
12.6
7+
4933
08.0
13.9
...
...
...
1036
924
1.5
5.7
Q1–
Q4
...
1157
2666
1951
22.8
0+
4935
28.8
9.9
...
TY
C35
65-1
155-
1..
.15
857
44.4
1.2
Q1
Q0
1160
2449
1908
13.7
8+
4939
07.6
9.9
...
TY
C35
50-1
718-
1..
.15
855
44.4
1.2
Q1
Q0
1160
7193
1919
29.7
8+
4941
07.8
12.6
...
...
...
1439
332
1.5
4.6
Q0–
Q4
...
1161
2274
1930
41.5
4+
4939
10.7
10.6
...
TY
C35
64-1
819-
1..
.40
115
228.
815
8.5
Q0–
Q1
Q3.
311
6223
2819
4756
.14+
4939
14.1
9.5
A233
BD+
4931
09..
.2
089
44.2
1.2
Q0–
Q1
...
1165
1083
1901
15.6
5+
4946
57.8
11.3
...
...
...
1105
725
2.5
4.6
Q0–
Q4
...
1165
1147
1901
26.5
7+
4945
14.1
13.8
...
...
...
1042
324
1.3
5.5
Q1–
Q4
...
1165
3958
1908
57.1
9+
4944
22.2
11.9
...
...
...
335
138
252.
74.
5..
.Q
0–Q
4.1
1165
4210
1909
41.7
6+
4947
37.4
11.9
...
...
...
334
440
252.
74.
5..
.Q
0–Q
4.1
1165
7840
1918
15.2
6+
4945
33.7
15.0
...
...
...
1304
331
0.5
6.1
Q1–
Q4
...
1166
1993
1927
55.7
8+
4945
43.5
9.4
F233
BD+
4930
18..
.45
466
109.
535
.3Q
0–Q
1Q
2.2
1167
1429
1945
48.8
2+
4947
11.6
11.0
...
TY
C35
65-1
003-
1..
.41
580
321.
524
8.3
Q0–
Q1
Q4.
311
7003
7018
5738
.28+
4951
03.6
10.6
...
TY
C35
49-6
77-1
...
3978
622
8.7
158.
6Q
0–Q
1Q
3.3
1170
0604
1858
21.7
4+
4953
55.7
11.1
...
TY
C35
49-9
14-1
...
4910
044
.21.
3Q
0Q
111
7064
4919
1334
.66+
4951
01.2
11.0
...
...
...
1438
432
1.5
4.9
Q0–
Q4
...
1170
6564
1913
51.1
7+
4951
34.5
12.4
...
...
...
1438
032
1.5
4.8
Q0–
Q4
...
1170
7341
1915
32.3
8+
4951
13.6
13.8
...
...
...
1391
531
0.5
4.8
Q1–
Q4
...
1170
8170
1917
18.5
0+
4951
00.8
7.2
F235
HD
1812
52..
.57
638
321.
535
.3Q
0–Q
4Q
2.2
1171
4150
1930
25.7
8+
4953
09.0
10.3
...
TY
C35
64-2
31-1
...
3981
413
7.7
66.4
Q0–
Q1
Q2.
311
7188
3919
3917
.64+
4948
06.1
10.9
...
TY
C35
64-8
91-1
...
4437
232
1.5
248.
3Q
0–Q
1Q
4.3
1175
3169
1903
04.3
7+
4954
06.3
14.7
...
...
...
1056
324
1.5
5.7
Q1–
Q4
...
1175
4974
1908
15.9
4+
4957
15.4
12.7
...
...
...
4519
516
9.8
156.
1Q
0–Q
1Q
3.1
1182
1140
1941
26.9
8+
5003
11.0
10.0
F033
BD+
4930
81..
.15
800
44.4
1.2
Q1
Q0
1182
2666
1943
57.5
3+
5004
31.8
10.7
...
...
...
4751
526
2.8
187.
3Q
0–Q
1Q
4.1
1182
4964
1947
43.1
0+
5005
14.2
10.6
...
TY
C35
65-2
47-1
...
3982
422
8.8
158.
6Q
0–Q
1Q
3.3
1187
4676
1947
15.3
1+
5011
20.1
10.1
A535
BD+
4931
06..
.15
861
44.4
1.2
Q1
Q0
1187
4898
1947
35.9
5+
5006
09.4
11.0
...
TY
C35
65-1
373-
1..
.15
858
44.4
1.2
Q1
Q0
1191
0256
1917
46.5
6+
5016
17.4
10.6
...
...
bina
ry�
4686
325
1.8
187.
5Q
1Q
4.1
1191
0642
1918
33.7
7+
5017
00.6
10.2
...
TY
C35
50-1
782-
1..
.45
401
109.
535
.3Q
0–Q
1Q
2.2
A125, page 37 of 70
A&A 534, A125 (2011)
Tabl
e1.
cont
inue
d.
KIC
IDR
AD
ecK
pS
pect
ralt
ype
Nam
eV
aria
ble
ND
atap
oint
sΔ
TδT
Qua
rter
sL
CQ
uart
ers
SC
(J20
00)
(J20
00)
(d)
(d)
1197
3705
1946
42.5
8+
5021
01.3
9.1
B934
HD
2349
99..
.28
668
322.
04.
6Q
0–Q
4Q
012
0188
3419
3848
.29+
5024
13.8
10.8
...
TY
C35
64-2
74-1
...
9514
626
2.8
187.
3Q
0–Q
1Q
4.1
1202
0590
1942
20.3
5+
5027
38.8
10.0
...
TY
C35
65-8
59-1
...
1583
044
.41.
4Q
1Q
012
0584
2819
1805
.66+
5033
35.9
11.1
...
TY
C35
50-8
95-1
...
4905
544
.21.
2Q
0Q
112
0624
4319
2748
.05+
5031
10.2
10.9
...
TY
C35
51-4
50-1
...
1582
644
.41.
6Q
1Q
012
0681
8019
3922
.42+
5032
03.4
10.4
...
TY
C35
64-1
358-
1..
.40
428
137.
766
.3Q
0–Q
1Q
2.3
1210
2187
1904
01.9
7+
5037
26.3
11.1
...
TY
C35
49-8
8-1
...
4930
844
.21.
2Q
0Q
112
1176
8919
4037
.25+
5038
31.5
10.8
...
TY
C35
68-9
96-1
...
4544
110
9.5
35.3
Q0–
Q1
Q2.
212
1220
7519
4815
.07+
5039
11.8
10.7
...
TY
C35
69-3
91-1
bina
ry�
4756
826
2.8
187.
3Q
0–Q
1Q
4.1
1221
6817
1943
11.1
4+
5053
45.6
10.7
...
TY
C35
69-3
68-1
...
4043
313
7.7
66.3
Q0–
Q1
Q2.
312
2172
8119
4400
.38+
5053
13.2
9.9
F234
HD
2349
84..
.15
841
44.4
1.2
Q1
Q0
1235
3648
1918
07.9
7+
5110
47.5
9.6
A234
HD
2348
59..
.40
397
137.
766
.3Q
0–Q
1Q
2.3
1264
7070
1921
51.1
4+
5142
20.1
10.7
...
TY
C35
55-1
407-
1..
.47
581
262.
818
7.3
Q0–
Q1
Q4.
112
7843
9419
1951
.41+
5205
39.6
9.8
A534
HD
2348
69..
.15
729
44.4
1.6
Q1
Q0
Not
es.(1
)P=
9.35
62d,
ecli
psin
gbi
nary
(Har
tman
etal
.200
4);(2
)P=
0.06
65d
(Hen
ryet
al.2
001)
;(3)
P=
4.03
03d,
puls
atin
gst
ar(H
artm
anet
al.2
004)
;(4
)P=
0.56
07d
(Har
tman
etal
.200
4);
(5)
P=
0.18
86d
(Har
tman
etal
.200
4);(6
)P=
0.29
48d
(Har
tman
etal
.200
4);(7
)P=
35.9
d(W
atso
n20
06);
(8)
P=
4.92
4d
(Pig
ulsk
ieta
l.20
09);
(9)
P=
2.18
d(M
agal
ashv
ili&
Kum
ishv
ili1
976)
;(1
0)P=
0.06
6677
d(W
atso
n20
06);
(11)
P=
0.38
414
d(W
atso
n20
06);
(12)
P=
8.48
03d
(Ote
ro20
07);
8.48
0322
d(C
arri
eret
al.2
002)
;(1
3)P=
4.56
427
d,ec
lips
ing
bina
ry(M
alko
vet
al.2
006)
;(1
4)A
bt(1
984)
;(15)
Gri
gahc
ène
etal
.(20
10);
(16)
Hen
ryet
al.(
2001
);(1
7)S
ato
&K
uji(
1990
);(1
8)C
anno
n(1
925)
;(19)
Abt
(200
4);(2
0)G
reni
eret
al.(
1999
);(2
1)H
ill&
Lyn
as-G
ray
(197
7);(2
2)G
uett
er(1
968)
;(2
3)A
bt&
Car
dona
(198
4);
(24)
Perr
yman
etal
.(1
997)
;(2
5)M
acra
e(1
952)
;(2
6)F
loqu
et(1
975)
;(2
7)F
loqu
et(1
970)
;(2
8)L
indoff
(197
2);
(29)
Moo
re&
Padd
ock
(195
0);
(30)
Bid
elm
anet
al.
(198
8);(3
1)S
teph
enso
n(1
986)
;(32)
Vys
sots
ky(1
958)
;(33)
Hil
l&S
chil
t(19
52);
(34)
Can
non
(192
5);(3
5)K
harc
henk
o&
Roe
ser
(200
9);(3
6)E
clip
sing
bina
ry(P
rša
etal
.201
1);(3
7)B
alon
aet
al.(
2011
c);
(38)
Ecl
ipsi
ngbi
nary
(Sla
wso
net
al.
2011
);(3
9)W
righ
tet
al.
(200
3);
(40)
Hoffl
eit
(195
1);
(41)
Mol
enda
-Zak
owic
zet
al.
(200
8).
(�)
Bin
arit
yis
susp
ecte
dby
insp
ecti
onof
Dig
itiz
edS
kyS
urve
yan
d2M
AS
Sim
ages
;(◦)sp
ectr
osco
pic
bina
ry.
A125, page 38 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
2.Eff
ectiv
ete
mpe
ratu
re(i
nK
),lo
gg
(in
dex)
,andv
sin
ival
ues
(in
kms−
1)
for
the
750
sam
ple
star
s.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0116
2150
6870
...
...
...
6870±2
90a
3.47
...
...
3.5±0
.3a
...
...
0129
4756
8410
...
...
...
8410±2
90a
3.92
...
...
3.9±0
.3a
...
...
0143
2149
7270
...
...
...
7270±2
90a
3.99
...
...
4.0±0
.3a
...
...
0157
1152◦
7050
6500±1
30b
7000±7
5g..
.70
00±7
5g3.
164.
49±0
.21b
4.15±0
.26g
4.2±0
.26g
91±1
3g..
.01
5717
1781
10..
...
...
.81
10±2
90a
3.98
...
...
4.0±0
.3a
...
...
0157
3064
4639
...
...
...
4639±2
90a
2.54
...
...
2.5±0
.3a
...
...
0171
8594
7500
...
...
...
7500±2
90a
3.95
...
...
4.0±0
.3a
...
...
0199
5489
...
6410±1
20b
...
...
6410±1
20b
...
4.43±0
.21b
...
4.43±0
.21b
...
...
0202
0966
...
6560±1
30b
...
...
6560±1
30b
...
3.50±0
.23b
...
3.50±0
.23b
...
...
0216
2283
6680
...
...
...
6680±2
90a
4.07
...
...
4.1±0
.3a
...
...
0216
3434
4590
...
...
...
4590±2
90a
2.67
...
...
2.7±0
.3a
...
...
0216
6218
7150
7070±8
0g..
...
.70
70±8
0g3.
353.
84±0
.21b
2.69±0
.19g
2.69±0
.19g
100±3
g..
.02
1683
3381
40..
...
...
.81
40±2
90a
3.83
...
...
3.8±0
.3a
...
...
0230
0165
7140
...
...
...
7140±2
90a
3.58
...
...
3.6±0
.3a
...
...
0230
3365
7280
...
...
...
7280±2
90a
3.65
...
...
3.7±0
.3a
...
...
0230
6469
4600
...
...
...
4600±2
90a
2.42
...
...
2.4±0
.3a
...
...
0230
6716
4670
...
...
...
4670±2
90a
2.32
...
...
2.3±0
.3a
...
...
0231
0479
4440
...
...
...
4440±2
90a
2.02
...
...
2.0±0
.3a
...
...
0231
1130
4640
...
...
...
4640±2
90a
2.31
...
...
2.3±0
.3a
...
...
0242
3932
...
...
...
...
...
...
...
...
...
...
...
0243
9660
7990
...
...
...
7990±2
90a
3.95
...
...
4.0±0
.3a
...
...
0244
3055
4590
...
...
...
4590±2
90a
2.52
...
...
2.5±0
.3a
...
...
0244
4598
...
...
...
...
...
...
...
...
...
...
...
0255
6297
4590
...
...
...
4590±2
90a
2.48
...
...
2.5±0
.3a
...
...
0255
6387
...
...
...
...
...
...
...
...
...
...
...
0255
7115
4340
...
...
...
4340±2
90a
2.22
...
...
2.2±0
.3a
...
...
0255
7430
6250
...
...
...
6250±2
90a
4.10
...
...
4.1±0
.3a
...
...
0255
8273
6440
...
...
...
6440±2
90a
4.19
...
...
4.2±0
.3a
...
...
0256
8519
6170
...
...
...
6170±2
90a
4.46
...
...
4.5±0
.3a
...
...
0256
9639
8020
...
...
...
8020±2
90a
4.12
...
...
4.1±0
.3a
...
...
0257
1868
7930
...
...
...
7930±2
90a
3.56
...
...
3.6±0
.3a
...
...
0257
2386
...
...
...
...
...
...
...
...
...
...
...
0257
5161
...
6940±1
50b
...
...
6940±1
50b
...
4.00±0
.21b
...
4.00±0
.21b
...
...
0257
8251
...
6610±1
30b
...
...
6610±1
30b
...
4.23±0
.21b
...
4.23±0
.21b
...
...
0258
3658
4620
...
...
...
4620±2
90a
2.44
...
...
2.4±0
.3a
...
...
0258
4202
...
...
...
...
...
...
...
...
...
...
...
0258
4908
8180
...
...
...
8180±2
90a
3.70
...
...
3.7±0
.3a
...
...
0269
4337
7290
...
...
...
7290±2
90a
3.99
...
...
4.0±0
.3a
...
...
0270
7479
7280
...
...
...
7280±2
90a
4.10
...
...
4.1±0
.3a
...
...
0271
8596
4850
...
...
...
4850±2
90a
2.63
...
...
2.6±0
.3a
...
...
0272
0582
7060
...
...
...
7060±2
90a
4.17
...
...
4.2±0
.3a
...
...
0283
4796
4570
...
...
...
4570±2
90a
2.34
...
...
2.3±0
.3a
...
...
0283
5795
...
6690±1
30b
...
...
6690±1
30b
...
3.74±0
.22b
...
3.74±0
.22b
...
...
A125, page 39 of 70
A&A 534, A125 (2011)Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0285
3280
7320
...
...
...
7320±2
90a
3.59
...
...
3.6±0
.3a
...
...
0285
5687
4770
...
...
...
4770±2
90a
2.52
...
...
2.5±0
.3a
...
...
0286
0123
4620
...
...
...
4620±2
90a
2.53
...
...
2.5±0
.3a
...
...
0296
9151
4700
...
...
...
4700±2
90a
2.37
...
...
2.4±0
.3a
...
...
0297
0244
4720
...
...
...
4720±2
90a
2.24
...
...
2.2±0
.3a
...
...
0297
2401
4660
...
...
...
4660±2
90a
2.59
...
...
2.6±0
.3a
...
...
0297
5832
...
...
...
...
...
...
...
...
...
...
...
0298
7660
7310
...
...
...
7310±2
90a
3.59
...
...
3.6±0
.3a
...
...
0298
9746
...
...
...
...
...
...
....
....
...
...
.02
9955
2548
50..
...
...
.48
50±2
90a
2.64
...
...
2.6±0
.3a
...
...
0299
7802
...
...
...
...
...
...
...
...
...
...
...
0309
7912
7880
...
...
...
7880±2
90a
3.56
...
...
3.6±0
.3a
...
...
0311
1451
...
...
...
...
...
...
...
...
...
...
...
0311
9604
8210
...
...
...
8210±2
90a
4.04
...
...
4.0±0
.3a
...
...
0311
9825
...
...
...
...
...
...
...
...
...
...
...
0321
5800
...
...
...
...
...
...
...
...
...
...
...
0321
7554◦
7800
7830±1
20g
...
...
7830±1
20g
3.50
3.69±0
.09g
...
3.69±0
.09g
228±1
8g..
.03
2186
3771
90..
...
...
.71
90±2
90a
3.89
...
...
3.9±0
.3a
...
...
0321
9256
7290
7500±1
50i
...
...
7500±1
50i
3.56
3.6±0
.1i
...
3.6±0
.1i
90±5
i..
.03
2207
8345
90..
...
...
.45
90±2
90a
2.58
...
...
2.6±0
.3a
...
...
0322
2364
...
6750±1
30b
...
...
6750±1
30b
...
3.82±0
.21b
...
3.82±0
.21b
...
...
0323
0227
7970
...
...
...
7970±2
90a
3.89
...
...
3.9±0
.3a
...
...
0323
1406
7800
...
...
...
7800±2
90a
3.76
...
...
3.8±0
.3a
...
...
0324
0556
8420
...
...
...
8420±2
90a
3.85
...
...
3.9±0
.3a
...
...
0324
5420
7870
...
...
...
7870±2
90a
3.66
...
...
3.7±0
.3a
...
...
0324
8627
4660
...
...
...
4660±2
90a
2.32
...
...
2.3±0
.3a
...
...
0332
7681
6500
...
...
...
6500±2
90a
3.68
...
...
3.7±0
.3a
...
...
0333
1147
7020
...
...
...
7020±2
90a
3.55
...
...
3.6±0
.3a
...
...
0333
7002
7200
...
...
...
7200±2
90a
3.60
...
...
3.6±0
.3a
...
...
0334
7643
6780
...
...
...
6780±2
90a
4.07
...
...
4.1±0
.3a
...
...
0334
8390
7140
6850±1
50b
...
...
6850±1
50b
4.02
4.10±0
.21b
...
4.10±0
.21b
...
...
0335
4022
4810
...
...
...
4810±2
90a
2.26
...
...
2.3±0
.3a
...
...
0335
5066
4900
...
...
...
4900±2
90a
2.74
...
...
2.7±0
.3a
...
...
0342
4493
7230
...
...
...
7230±2
90a
3.44
...
...
3.4±0
.3a
...
...
0342
5802
8050
...
...
...
8050±2
90a
4.06
...
...
4.1±0
.3a
...
...
0342
7144
4790
...
...
...
4790±2
90a
2.55
...
...
2.5±0
.3a
...
...
0342
7365
4900
...
...
...
4900±2
90a
2.48
...
...
2.5±0
.3a
...
...
0342
9637
6960
7200±1
50i
...
...
7200±1
50i
3.42
4.0±0
.1i
...
4.0±0
.1i
50±5
i..
.03
4379
4074
3073
42±1
62e
7700±1
20i
...
7700±1
20i
3.86
3.3±0
.2e
4.1±0
.2i
4.1±0
.2i
120±5
i..
.03
4404
9574
10..
...
...
.74
10±2
90a
3.93
...
...
3.9±0
.3a
...
...
0344
9373
...
...
...
...
...
...
...
...
...
...
...
0344
9625
...
...
...
...
...
...
...
...
...
...
...
0345
3494
7810
7750±7
0g..
...
.77
50±7
0g3.
843.
6±0
.3g
...
3.6±0
.3g
210±1
5g..
.
A125, page 40 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0345
7434
4570
...
...
...
4570±2
90a
2.39
...
...
2.4±0
.3a
...
...
0345
8097
...
...
...
...
...
...
...
...
...
...
...
0345
8318
...
...
...
...
...
...
...
...
...
...
...
0352
5951
4570
...
...
...
4570±2
90a
2.47
...
...
2.5±0
.3a
...
...
0352
8578
5020
...
...
...
5020±2
90a
2.78
...
...
2.8±0
.3a
...
...
0353
9153
7310
6790±1
40b
...
...
6790±1
40b
3.81
3.73±0
.21b
...
3.73±0
.21b
...
...
0354
6061
4770
...
...
...
4770±2
90a
2.34
...
...
2.3±0
.3a
...
...
0355
8145
7340
...
...
...
7340±2
90a
4.11
...
...
4.1±0
.3a
...
...
0362
9080
4830
...
...
...
4830±2
90a
2.74
...
...
2.7±0
.3a
...
...
0363
3693
4530
...
...
...
4530±2
90a
2.38
...
...
2.4±0
.3a
...
...
0363
4384
7480
...
...
...
7480±2
90a
3.86
...
...
3.9±0
.3a
...
...
0364
3717
4410
...
...
...
4410±2
90a
2.02
...
...
2.0±0
.3a
...
...
0364
4116
7500
...
...
...
7500±2
90a
4.11
...
...
4.1±0
.3a
...
...
0365
5513
...
...
...
...
...
...
...
...
...
...
...
0365
5608
6600
...
...
...
6600±2
90a
4.33
...
...
4.3±0
.3a
...
...
0366
3141
...
...
...
...
...
...
...
...
...
...
...
0373
3735
6440
6671±7
6c67
60±0
d65
46±0
o66
71±7
6c4.
034.
31±0
.10d
...
4.3±0
.1d
...
...
0375
8717
...
...
...
...
...
...
...
...
...
...
...
0375
9814
4890
...
...
...
4890±2
90a
3.51
...
...
3.5±0
.3a
...
...
0376
0002
7030
...
...
...
7030±2
90a
4.04
...
...
4.0±0
.3a
...
...
0376
0826
8640
...
...
...
8640±2
90a
3.42
...
...
3.4±0
.3a
...
...
0376
1641
8150
...
...
...
8150±2
90a
4.10
...
...
4.1±0
.3a
...
...
0383
6911
...
...
...
...
...
...
...
...
...
...
...
0385
0810
7300
...
...
...
7300±2
90a
3.56
...
...
3.6±0
.3a
...
...
0385
1151
8190
...
...
...
8190±2
90a
4.10
...
...
4.1±0
.3a
...
...
0386
8032
8340
...
...
...
8340±2
90a
4.04
...
...
4.0±0
.3a
...
...
0394
1283
7800
...
...
...
7800±2
90a
3.87
...
...
3.9±0
.3a
...
...
0394
2911
7310
...
...
...
7310±2
90a
3.99
...
...
4.0±0
.3a
...
...
0396
6357
7460
...
...
...
7460±2
90a
3.59
...
...
3.6±0
.3a
...
...
0397
0729
7160
...
...
...
7160±2
90a
4.14
...
...
4.1±0
.3a
...
...
0403
5667
7960
...
...
...
7960±2
90a
3.87
...
...
3.9±0
.3a
...
...
0404
4353
8300
...
...
...
8300±2
90a
3.56
...
...
3.6±0
.3a
...
...
0404
8488
5900
...
...
...
5900±2
90a
4.21
...
...
4.2±0
.3a
...
...
0404
8494
7620
...
...
...
7620±2
90a
3.95
...
...
4.0±0
.3a
...
...
0406
9477
7190
...
...
...
7190±2
90a
3.80
...
...
3.8±0
.3a
...
...
0407
5519
...
...
...
...
...
...
...
...
...
...
...
0407
7032
6790
...
...
...
6790±2
90a
4.05
...
...
4.1±0
.3a
...
...
0414
4300
...
...
...
...
...
...
...
...
...
...
...
0415
0611
6620
...
...
...
6620±2
90a
4.05
...
...
4.1±0
.3a
...
...
0416
0876
8290
...
...
...
8290±2
90a
3.65
...
...
3.7±0
.3a
...
...
0416
4363
7480
6470±1
20b
...
...
6470±1
20b
3.83
3.84±0
.22b
...
3.84±0
.22b
...
...
0416
8574
7710
...
...
...
7710±2
90a
3.50
...
...
3.5±0
.3a
...
...
0417
0631
7500
...
...
...
7500±2
90a
3.47
...
...
3.5±0
.3a
...
...
A125, page 41 of 70
A&A 534, A125 (2011)Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0418
0199
7220
...
...
...
7220±2
90a
3.91
...
...
3.9±0
.3a
...
...
0425
2757
7650
...
...
...
7650±2
90a
3.72
...
...
3.7±0
.3a
...
...
0426
9337
8000
...
...
...
8000±2
90a
3.58
...
...
3.6±0
.3a
...
...
0428
1581
8140
...
...
...
8140±2
90a
3.84
...
...
3.8±0
.3a
...
...
0438
3117
8250
...
...
...
8250±2
90a
3.63
...
...
3.6±0
.3a
...
...
0447
6836
6760
...
...
...
6760±2
90a
3.88
...
...
3.9±0
.3a
...
...
0448
0321
7150
...
...
...
7150±2
90a
3.87
...
...
3.9±0
.3a
...
...
0448
8840
7130
...
...
...
7130±2
90a
3.54
...
...
3.5±0
.3a
...
...
0455
0962
7290
...
...
...
7290±2
90a
3.54
...
...
3.5±0
.3a
...
...
0455
6345
7290
...
...
...
7290±2
90a
3.87
...
...
3.9±0
.3a
...
...
0457
0326
...
7000±1
50i
...
...
7000±1
50i
...
4.0±0
.3i
...
4.0±0
.3i
80±2
0i..
.04
5884
8778
60..
...
...
.78
60±2
90a
3.98
...
...
4.0±0
.3a
...
...
0464
7763
6890
6850±1
40b
...
...
6850±1
40b
4.05
3.56±0
.22b
...
3.56±0
.22b
...
...
0464
9476
8330
...
...
...
8330±2
90a
3.87
...
...
3.9±0
.3a
...
...
0467
1225
8230
...
...
...
8230±2
90a
3.27
...
...
3.3±0
.3a
...
...
0467
7684
7860
...
...
...
7860±2
90a
3.32
...
...
3.3±0
.3a
...
...
0475
8316
6980
...
...
...
6980±2
90a
4.07
...
...
4.1±0
.3a
...
...
0476
8677
8360
...
...
...
8360±2
90a
3.97
...
...
4.0±0
.3a
...
...
0484
0675
7110
...
...
...
7110±2
90a
3.55
...
...
3.6±0
.3a
...
...
0485
0899
...
7132±1
63e
7244±0
d..
.71
32±1
63e
...
4.2±0
.2e
4.26±0
.05d
4.26±0
.05d
...
...
0485
6630
7350
...
...
...
7350±2
90a
3.89
...
...
3.9±0
.3a
...
...
0485
7678
...
6668±0
o..
...
.66
80±2
90o
...
...
...
...
...
...
0486
3077
7520
...
...
...
7520±2
90a
3.90
...
...
3.9±0
.3a
...
...
0490
9697
7820
...
...
...
7820±2
90a
3.92
...
...
3.9±0
.3a
...
...
0491
9818
7320
...
...
...
7320±2
90a
3.97
...
...
4.0±0
.3a
...
...
0492
0125
7630
...
...
...
7630±2
90a
3.62
...
...
3.6±0
.3a
...
...
0493
6524
7470
...
...
...
7470±2
90a
3.79
...
...
3.8±0
.3a
...
...
0493
7257
...
...
...
...
...
...
...
...
...
...
...
0498
9900
7900
...
...
...
7900±2
90a
3.51
...
...
3.5±0
.3a
...
...
0502
4150
5250
...
...
...
5250±2
90a
...
...
...
...
...
...
0502
4454
6210
...
...
...
6210±2
90a
4.11
...
...
4.1±0
.3a
...
...
0502
4455
6760
...
...
...
6760±2
90a
4.44
...
...
4.4±0
.3a
...
...
0502
4456
4300
...
...
...
4300±2
90a
...
...
...
...
...
...
0502
4750
...
...
...
...
...
...
...
...
...
...
...
0503
8228
6740
...
...
...
6740±2
90a
4.13
...
...
4.1±0
.3a
...
...
0508
0290
5140
...
...
...
5140±2
90a
3.58
...
...
3.6±0
.3a
...
...
0508
8308
6570
6740±5
0g..
...
.67
40±5
0g4.
042.
70±0
.13g
...
2.70±0
.13g
41±1
g..
.05
1057
5470
90..
...
...
.70
90±2
90a
4.13
...
...
4.1±0
.3a
...
...
0511
2786
...
...
...
...
...
...
...
...
...
...
...
0511
2932
...
...
...
...
...
...
...
...
...
...
...
0511
3797
8140
...
...
...
8140±2
90a
3.83
...
...
3.8±0
.3a
...
...
0516
4767
...
6576±1
21e
6960±8
0g69
82±0
o69
60±8
0g..
.3.
11±0
.19e
4.01±0
.37g
3.11±0
.19e
162±9
g..
.05
1807
9674
50..
...
...
.74
50±2
90a
3.89
...
...
3.9±0
.3a
...
...
A125, page 42 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0519
7256
7610
...
...
...
7610±2
90a
3.88
...
...
3.9±0
.3a
...
...
0519
9464
6080
...
...
...
6080±2
90a
4.53
...
...
4.5±0
.3a
...
...
0520
0084
7470
...
...
...
7470±2
90a
3.84
...
...
3.8±0
.3a
...
...
0520
1088
5450
...
...
...
5450±2
90a
...
...
...
...
...
...
0520
9712
8360
...
...
...
8360±2
90a
3.95
...
...
4.0±0
.3a
...
...
0521
7733
9120
...
...
...
9120±2
90a
4.22
...
...
4.2±0
.3a
...
...
0521
9533
7410
...
...
...
7410±2
90a
3.94
...
...
3.9±0
.3a
115n
...
0527
2673
7120
...
...
...
7120±2
90a
3.76
...
...
3.8±0
.3a
...
...
0529
4571
6580
...
...
...
6580±2
90a
4.07
...
...
4.1±0
.3a
...
...
0529
6877
6660
6500±2
00i
...
...
6500±2
00i
4.11
3.8±0
.3i
...
3.8±0
.3i
200±2
0i..
.05
3563
4982
90..
...
...
.82
90±2
90a
3.91
...
...
3.9±0
.3a
...
...
0537
1747
7070
...
...
...
7070±2
90a
4.03
...
...
4.0±0
.3a
...
...
0539
1416
8060
...
...
...
8060±2
90a
3.89
...
...
3.9±0
.3a
...
...
0542
8254
7390
...
...
...
7390±2
90a
3.93
...
...
3.9±0
.3a
...
...
0543
6432
8330
...
...
...
8330±2
90a
3.90
...
...
3.9±0
.3a
...
...
0543
7206
7710
...
...
...
7710±2
90a
3.67
...
...
3.7±0
.3a
...
...
0544
6068◦
5340
5980±1
20g
...
...
5980±1
20g
4.48
3.58±0
.28g
...
3.58±0
.28g
11±1
g..
.05
4731
7174
50..
...
...
.74
50±2
90a
3.63
...
...
3.6±0
.3a
...
...
0547
4427
6880
...
...
...
6880±2
90a
4.14
...
...
4.1±0
.3a
...
...
0547
6495
7360
...
...
...
7360±2
90a
3.92
...
...
3.9±0
.3a
...
...
0547
6864
6580
6550±1
20b
...
...
6550±1
20b
4.11
3.72±0
.22b
...
3.72±0
.22b
...
...
0551
3861
6170
6610±1
40b
...
...
6610±1
40b
4.43
4.48±0
.21b
...
4.48±0
.21b
...
...
0560
3049
8000
...
...
...
8000±2
90a
3.71
...
...
3.7±0
.3a
...
...
0563
0362
7360
...
...
...
7360±2
90a
3.53
...
...
3.5±0
.3a
...
...
0563
2093
8090
...
...
...
8090±2
90a
4.07
...
...
4.1±0
.3a
...
...
0564
1711
7160
...
...
...
7160±2
90a
3.97
...
...
4.0±0
.3a
...
...
0570
9664
7200
...
...
...
7200±2
90a
4.04
...
...
4.0±0
.3a
...
...
0572
2346
6670
...
...
...
6670±2
90a
4.21
...
...
4.2±0
.3a
...
...
0572
4048
6520
...
...
...
6520±2
90a
4.08
...
...
4.1±0
.3a
...
...
0572
4440
7290
7699±8
1c75
37±1
86e
7350±1
20i
7350±1
20i
3.57
3.98±0
.21e
3.6±0
.3i
3.6±0
.3i
220±5
i..
.05
7248
1073
30..
...
...
.73
30±2
90a
3.88
...
...
3.9±0
.3a
...
...
0576
8203
6450
...
...
...
6450±2
90a
3.95
...
...
3.9±0
.3a
...
...
0577
2411
6760
...
...
...
6760±2
90a
4.18
...
...
4.2±0
.3a
...
...
0577
4557
7050
...
...
...
7050±2
90a
3.99
...
...
4.0±0
.3a
...
...
0578
5707
8010
7940±8
0g..
...
.79
40±8
0g3.
623.
44±0
.26g
...
3.44±0
.26g
170±1
1g..
.05
8101
1363
6064
80±1
20b
...
...
6480±1
20b
4.22
3.60±0
.23b
...
3.60±0
.23b
...
...
0585
7714
6710
...
...
...
6710±2
90a
3.80
...
...
3.8±0
.3a
...
...
0588
0360
7690
...
...
...
7690±2
90a
3.64
...
...
3.6±0
.3a
...
...
0594
0273
8010
...
...
...
8010±2
90a
3.59
...
...
3.6±0
.3a
...
...
0595
4264
6720
6900±1
46e
...
...
6900±1
46e
4.15
3.86±0
.21e
...
3.86±0
.21e
...
...
0596
5837
6520
6975±2
00i
...
...
6975±2
00i
4.15
4.0±0
.4i
...
4.0±0
.3i
20±1
0i..
.05
9803
3776
80..
...
...
.76
80±2
90a
3.76
...
...
3.8±0
.3a
...
...
0598
8140
7450
7267±1
63e
7400±1
50i
...
7400±1
50i
3.54
3.32±0
.23e
3.7±0
.3i
3.32±0
.23e
70±2
0i..
.
A125, page 43 of 70
A&A 534, A125 (2011)Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0603
2730
7110
...
...
...
7110±2
90a
3.79
...
...
3.8±0
.3a
...
...
0606
7817
7840
...
...
...
7840±2
90a
3.86
...
...
3.9±0
.3a
...
...
0612
3324
6670
6700±1
30b
6641±1
23e
...
6700±1
30b
3.40
3.09±0
.23b
3.06±0
.21e
3.1±0
.3b
...
...
0614
1372
7080
...
...
...
7080±2
90a
4.21
...
...
4.2±0
.3a
...
...
0614
2919
7000
...
...
...
7000±2
90a
4.02
...
...
4.0±0
.3a
...
...
0618
7665
6880
6025±6
0c60
25±0
d..
.60
25±6
0c4.
014.
27±0
.11d
...
4.27±0
.11d
...
...
0619
9731
7850
...
...
...
7850±2
90a
3.55
...
...
3.6±0
.3a
...
...
0626
8890
7280
...
...
...
7280±2
90a
3.49
...
...
3.5±0
.3a
...
...
0627
9848
...
6826±1
40e
...
...
6826±1
40e
...
3.8±0
.2e
...
3.8±0
.2e
...
...
0628
9468
8270
8150±1
00g
...
...
8150±1
00g
3.74
3.29±0
.09g
...
3.29±0
.09g
148±7
g..
.06
3017
4567
9067
40±1
30b
...
...
6740±1
30b
4.13
4.01±0
.21b
...
4.01±0
.21b
...
...
0638
1306
8060
...
...
...
8060±2
90a
3.63
...
...
3.6±0
.3a
...
...
0643
2054
7090
7287±1
67e
7400±1
50l
...
7400±1
50l
3.85
3.81±0
.19e
3.9±0
.2l
3.81±0
.19e
...
...
0644
0930
8320
...
...
...
8320±2
90a
4.09
...
...
4.1±0
.3a
...
...
0644
3122
7480
...
...
...
7480±2
90a
3.54
...
...
3.5±0
.3a
...
...
0644
6951
7380
...
...
...
7380±2
90a
4.06
...
...
4.1±0
.3a
...
...
0644
8112
8150
...
...
...
8150±2
90a
4.01
...
...
4.0±0
.3a
...
...
0646
2033
8390
...
...
...
8390±2
90a
4.32
...
...
4.3±0
.3a
...
...
0650
0578
7840
...
...
...
7840±2
90a
3.64
...
...
3.6±0
.3a
...
...
0650
9175
7300
7520±6
0g..
...
.75
20±6
0g3.
523.
29±0
.3g
...
3.3±0
.3g
132±8
g..
.06
5198
6971
50..
...
...
.71
50±2
90a
3.80
...
...
3.8±0
.3a
...
...
0658
6052
7520
...
...
...
7520±2
90a
4.05
...
...
4.1±0
.3a
...
...
0658
7551
8380
8870±1
90g
...
...
8870±1
90g
3.93
3.78±0
.09g
...
3.78±0
.09g
138±9
g..
.06
5904
0370
30..
...
...
.70
30±2
90a
3.93
...
...
3.9±0
.3a
...
...
0660
6229
6750
...
...
...
6750±2
90a
4.09
...
...
4.1±0
.3a
...
...
0661
4168
7270
...
...
...
7270±2
90a
4.14
...
...
4.1±0
.3a
...
...
0662
9106
7070
...
...
...
7070±2
90a
3.95
...
...
4.0±0
.3a
...
...
0666
8729
7770
...
...
...
7770±2
90a
3.48
...
...
3.5±0
.3a
...
...
0667
0742
7450
6386±6
2c..
...
.63
86±6
2c3.
61..
...
.3.
6±0
.3a
...
...
0667
8614
7410
...
...
...
7410±2
90a
3.85
...
...
3.9±0
.3a
...
...
0669
4649
7750
...
...
...
7750±2
90a
3.66
...
...
3.7±0
.3a
...
...
0675
6386
7990
7900±7
0g..
...
.79
00±7
0g3.
513.
17±0
.10g
...
3.2±0
.1g
190±1
2g..
.06
7564
8173
10..
...
...
.73
10±2
90a
3.52
...
...
3.5±0
.3a
...
...
0676
1539
7240
...
...
...
7240±2
90a
4.04
...
...
4.0±0
.3a
...
...
0677
6331
7650
...
...
...
7650±2
90a
3.72
...
...
3.7±0
.3a
...
...
0679
0335
7690
...
...
...
7690±2
90a
3.52
...
...
3.5±0
.3a
...
...
0680
4821
7480
...
...
...
7480±2
90a
3.65
...
...
3.7±0
.3a
...
...
0686
5077
7770
...
...
...
7770±2
90a
3.62
...
...
3.6±0
.3a
...
...
0692
2690
7320
...
...
...
7320±2
90a
3.61
...
...
3.6±0
.3a
...
...
0692
3424
7060
...
...
...
7060±2
90a
4.16
...
...
4.2±0
.3a
...
...
0693
7758
7840
...
...
...
7840±2
90a
3.47
...
...
3.5±0
.3a
...
...
0693
9291
7140
...
...
...
7140±2
90a
3.52
...
...
3.5±0
.3a
...
...
0694
7064
8170
...
...
...
8170±2
90a
3.91
...
...
3.9±0
.3a
...
...
A125, page 44 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0695
1642
7180
...
...
...
7180±2
90a
3.37
...
...
3.4±0
.3a
...
...
0696
5789
7650
...
...
...
7650±2
90a
3.39
...
...
3.4±0
.3a
...
...
0700
7103
6910
...
...
...
6910±2
90a
4.06
...
...
4.1±0
.3a
...
...
0710
6205
6970
6900±1
40b
...
...
6900±1
40b
4.05
3.73±0
.21b
...
3.73±0
.21b
...
...
0710
6648
7010
...
...
...
7010±2
90a
4.11
...
...
4.1±0
.3a
...
...
0710
9598
7270
...
...
...
7270±2
90a
4.08
...
...
4.1±0
.3a
...
...
0711
9530
7780
7608±1
90e
7500±2
00i
...
7500±2
00i
3.49
3.26±0
.21e
3.6±0
.3i
3.26±0
.21e
200±2
0i..
.07
1227
4683
4077
40±2
00b
...
...
7740±2
00b
3.84
4.00±0
.18b
...
4.00±0
.18b
...
...
0720
4237
8070
...
...
...
8070±2
90a
4.05
...
...
4.1±0
.3a
...
...
0721
1759
8220
...
...
...
8220±2
90a
3.77
...
...
3.8±0
.3a
...
...
0721
2040
7500
...
...
...
7500±2
90a
3.97
...
...
4.0±0
.3a
...
...
0721
5607
6530
...
...
...
6530±2
90a
4.06
...
...
4.1±0
.3a
...
...
0721
7483
6940
...
...
...
6940±2
90a
3.89
...
...
3.9±0
.3a
...
...
0722
0356
6340
...
...
...
6340±2
90a
4.26
...
...
4.3±0
.3a
...
...
0726
5427
7560
...
...
...
7560±2
90a
4.13
...
...
4.1±0
.3a
...
...
0728
7118
7850
...
...
...
7850±2
90a
3.76
...
...
3.8±0
.3a
...
...
0730
0387
7000
...
...
...
7000±2
90a
3.60
...
...
3.6±0
.3a
...
...
0730
4385
6890
...
...
...
6890±2
90a
3.60
...
...
3.6±0
.3a
...
...
0733
8125
7860
...
...
...
7860±2
90a
3.96
...
...
4.0±0
.3a
...
...
0735
0486
7290
...
...
...
7290±2
90a
3.65
...
...
3.7±0
.3a
...
...
0735
2425
6890
...
...
...
6890±2
90a
4.07
...
...
4.1±0
.3a
...
...
0735
2776
7460
...
...
...
7460±2
90a
3.99
...
...
4.0±0
.3a
...
...
0738
5478
6480
...
...
...
6480±2
90a
3.87
...
...
3.9±0
.3a
...
...
0743
6266
7020
...
...
...
7020±2
90a
4.05
...
...
4.1±0
.3a
...
...
0745
0284
7930
...
...
...
7930±2
90a
3.74
...
...
3.7±0
.3a
...
...
0750
2559
7470
...
...
...
7470±2
90a
3.89
...
...
3.9±0
.3a
...
...
0753
3694
7860
...
...
...
7860±2
90a
3.80
...
...
3.8±0
.3a
...
...
0754
8061
5000
5370±1
20q
...
...
5370±1
20q
2.42
1.50±0
.35q
...
2.4±0
.3a
12±2
q..
.07
5484
7973
4075
00±2
50r
...
...
7500±2
50l
3.84
3.90±0
.25l
...
3.90±0
.25l
10±2
l..
.07
5532
3769
30..
...
...
.69
30±2
90a
4.12
...
...
4.1±0
.3a
...
...
0758
3939
8310
...
...
...
8310±2
90a
3.95
...
...
3.9±0
.3a
...
...
0759
6250
6870
...
...
...
6870±2
90a
3.90
...
...
3.9±0
.3a
...
...
0766
2076
7050
...
...
...
7050±2
90a
4.01
...
...
4.0±0
.3a
...
...
0766
8791
8150
...
...
...
8150±2
90a
3.89
...
...
3.9±0
.3a
...
...
0766
9848
...
...
...
...
...
...
...
...
...
19o
19.4±2
.0n
0769
4191
7850
...
...
...
7850±2
90a
3.54
...
...
3.5±0
.3a
...
...
0769
7795
7480
...
...
...
7480±2
90a
3.56
...
...
3.6±0
.3a
...
...
0769
9056
7410
...
...
...
7410±2
90a
3.67
...
...
3.7±0
.3a
...
...
0770
2705
7310
6710±1
30b
...
...
6710±1
30b
4.00
2.88±0
.23b
...
2.88±0
.23b
...
...
0773
2458
7550
...
...
...
7550±2
90a
3.64
...
...
3.6±0
.3a
...
...
0774
2739
7170
...
...
...
7170±2
90a
3.89
...
...
3.9±0
.3a
...
...
0774
8238
7230
7260±6
4g..
...
.72
60±6
4g3.
474.
06±0
.28g
...
4.06±0
.28g
119±6
g..
.07
7568
5380
60..
...
...
.80
60±2
90a
3.94
...
...
3.9±0
.3a
...
...
A125, page 45 of 70
A&A 534, A125 (2011)Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0776
7565
...
...
...
...
...
...
...
...
...
...
...
0777
0282
7450
...
...
...
7450±2
90a
3.50
...
...
3.5±0
.3a
...
...
0777
1991
7300
...
...
...
7300±2
90a
3.53
...
...
3.5±0
.3a
...
...
0777
3133
6640
...
...
...
6640±2
90a
3.52
...
...
3.5±0
.3a
...
...
0777
7435
8120
...
...
...
8120±2
90a
3.75
...
...
3.8±0
.3a
...
...
0779
8339
6680
6880±1
44e
6700±2
00i
6745±0
o68
80±1
44e
3.40
3.90±0
.21e
3.7±0
.3i
3.90±0
.21e
15.4±2
.0n
15±5
g,i
0782
7131
8290
...
...
...
8290±2
90a
3.49
...
...
3.5±0
.3a
...
...
0783
1302
8160
...
...
...
8160±2
90a
3.86
...
...
3.9±0
.3a
...
...
0783
4612
7450
...
...
...
7450±2
90a
3.67
...
...
3.7±0
.3a
...
...
0784
2286
7660
...
...
...
7660±2
90a
3.77
...
...
3.8±0
.3a
...
...
0784
2621
7620
...
...
...
7620±2
90a
3.54
...
...
3.5±0
.3a
...
...
0784
8288
7380
...
...
...
7380±2
90a
3.52
...
...
3.5±0
.3a
...
...
0789
0526
7080
...
...
...
7080±2
90a
4.07
...
...
4.1±0
.3a
...
...
0790
0367
6970
...
...
...
6970±2
90a
4.14
...
...
4.1±0
.3a
...
...
0790
8633
7840
...
...
...
7840±2
90a
3.73
...
...
3.7±0
.3a
...
...
0795
9867
8480
...
...
...
8480±2
90a
3.90
...
...
3.9±0
.3a
...
...
0797
7996
7120
...
...
...
7120±2
90a
3.77
...
...
3.8±0
.3a
...
...
0798
5370
5610
...
...
...
5610±2
90a
4.60
...
...
4.6±0
.3a
...
...
0802
9546
7120
...
...
...
7120±2
90a
3.89
...
...
3.9±0
.3a
...
...
0804
3961
6350
...
...
...
6350±2
90a
3.62
...
...
3.6±0
.3a
...
...
0805
4146
8150
6770±1
50b
...
...
6770±1
50b
3.67
3.08±0
.27b
...
3.7±0
.3a
...
...
0810
3917
7130
...
...
...
7130±2
90a
4.16
...
...
4.2±0
.3a
...
...
0810
4589
6510
...
...
...
6510±2
90a
4.29
...
...
4.3±0
.3a
...
...
0812
3127
7160
...
...
...
7160±2
90a
3.69
...
...
3.7±0
.3a
...
...
0814
3903
3680
...
...
...
3680±2
90a
4.22
...
...
4.2±0
.3a
...
...
0814
4674
7290
...
...
...
7290±2
90a
3.85
...
...
3.9±0
.3a
...
...
0814
5477
6800
...
...
...
6800±2
90a
4.06
...
...
4.1±0
.3a
...
...
0814
9341
7540
...
...
...
7540±2
90a
4.00
...
...
4.0±0
.3a
...
...
0815
9135
5020
...
...
...
5020±2
90a
4.14
...
...
4.1±0
.3a
...
...
0819
7761
7070
...
...
...
7070±2
90a
4.09
...
...
4.1±0
.3a
...
...
0819
7788
8010
7500±1
50i
...
...
7500±1
50i
3.98
4.0±0
.3i
...
4.0±0
.3i
230±2
0i..
.08
2115
0074
00..
...
...
.74
00±2
90a
3.91
...
...
3.9±0
.3a
...
...
0821
8419
4550
...
...
...
4550±2
90a
2.20
...
...
2.2±0
.3a
...
...
0822
2685
...
...
...
...
...
...
...
...
...
...
...
0822
3568
6790
6740±1
40b
...
...
6740±1
40b
3.88
4.38±0
.21b
...
4.38±0
.21b
...
...
0822
3987
5550
...
...
...
5550±2
90a
4.45
...
...
4.5±0
.3a
...
...
0823
0025
7280
...
...
...
7280±2
90a
3.48
...
...
3.5±0
.3a
...
...
0824
5366
...
...
...
...
...
...
...
...
...
...
...
0824
8630
7310
...
...
...
7310±2
90a
3.74
...
...
3.7±0
.3a
...
...
0826
4061
7230
...
...
...
7230±2
90a
4.10
...
...
4.1±0
.3a
...
...
0826
4075
7650
...
...
...
7650±2
90a
4.06
...
...
4.1±0
.3a
...
...
0826
4274
7640
...
...
...
7640±2
90a
3.74
...
...
3.7±0
.3a
...
...
0826
4404
7890
7500±2
00i
...
...
7500±2
00i
3.73
3.7±0
.3i
...
3.7±0
.3i
250±2
0i..
.
A125, page 46 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0826
4546
7630
...
...
...
7630±2
90a
3.96
...
...
4.0±0
.3a
...
...
0826
4583
8360
7240±1
60b
...
...
7240±1
60b
3.64
2.97±0
.22b
...
3.97±0
.22b
...
...
0826
4588
...
...
...
...
...
...
...
...
...
...
...
0826
4617
7310
...
...
...
7310±2
90a
4.12
...
...
4.1±0
.3a
...
...
0826
4674
8030
...
...
...
8030±2
90a
3.69
...
...
3.7±0
.3a
...
...
0826
4698
8010
7500±2
00i
...
...
7500±2
00i
3.79
3.9±0
.2i
...
3.9±0
.2i
210±2
0i..
.08
2837
9655
00..
...
...
.55
00±2
90a
4.05
...
...
4.1±0
.3a
...
...
0829
3302
6450
...
...
...
6450±2
90a
4.22
...
...
4.2±0
.3a
...
...
0832
3104
7590
...
...
...
7590±2
90a
3.92
...
...
3.9±0
.3a
...
...
0833
0056
7240
...
...
...
7240±2
90a
4.10
...
...
4.1±0
.3a
...
...
0833
0092
6900
...
...
...
6900±2
90a
4.12
...
...
4.1±0
.3a
...
...
0833
0463
6020
...
...
...
6020±2
90a
4.86
...
...
4.9±0
.3a
...
...
0833
0778
7620
...
...
...
7620±2
90a
4.03
...
...
4.0±0
.3a
...
...
0835
2420
6560
...
...
...
6560±2
90a
4.30
...
...
4.3±0
.3a
...
...
0835
5130
7040
...
...
...
7040±2
90a
4.11
...
...
4.1±0
.3a
...
...
0835
5837
5860
...
...
...
5860±2
90a
4.30
...
...
4.3±0
.3a
...
...
0839
7426
7030
...
...
...
7030±2
90a
3.55
...
...
3.6±0
.3a
...
...
0841
5752
7780
...
...
...
7780±2
90a
4.00
...
...
4.0±0
.3a
...
...
0842
9756
7360
...
...
...
7360±2
90a
3.67
...
...
3.7±0
.3a
...
...
0844
6738
7150
...
...
...
7150±2
90a
3.93
...
...
3.9±0
.3a
...
...
0845
4553
6670
...
...
...
6670±2
90a
3.58
...
...
3.6±0
.3a
...
...
0845
9354
7430
...
...
...
7430±2
90a
3.62
...
...
3.6±0
.3a
...
...
0846
0025
...
...
...
...
...
...
...
...
...
...
...
0846
0993
6710
...
...
...
6710±2
90a
3.98
...
...
4.0±0
.3a
...
...
0847
9107
5050
...
...
...
5050±2
90a
4.52
...
...
4.5±0
.3a
...
...
0848
2540
6360
...
...
...
6360±2
90a
4.33
...
...
4.3±0
.3a
...
...
0848
8065
6190
...
...
...
6190±2
90a
4.20
...
...
4.2±0
.3a
...
...
0848
9712
8350
...
...
...
8350±2
90a
3.52
...
...
3.5±0
.3a
...
...
0849
9639
6580
...
...
...
6580±2
90a
4.12
...
...
4.1±0
.3a
...
...
0850
7325
7140
...
...
...
7140±2
90a
3.43
...
...
3.4±0
.3a
...
...
0851
6008
8320
...
...
...
8320±2
90a
3.60
...
...
3.6±0
.3a
...
...
0851
6686
8240
...
...
...
8240±2
90a
4.02
...
...
4.0±0
.3a
...
...
0852
5286
7350
...
...
...
7350±2
90a
4.19
...
...
4.2±0
.3a
...
...
0854
5456
7860
...
...
...
7860±2
90a
3.87
...
...
3.9±0
.3a
...
...
0856
0996
7870
...
...
...
7870±2
90a
3.61
...
...
3.6±0
.3a
...
...
0856
5229
7740
...
...
...
7740±2
90a
3.88
...
...
3.9±0
.3a
...
...
0857
9615
8260
...
...
...
8260±2
90a
3.98
...
...
4.0±0
.3a
...
...
0858
3770
7660
9000±2
00i
...
...
9000±2
00i
3.47
3.0±0
.2i
...
3.0±0
.2i
130±1
0i..
.08
5905
5373
00..
...
...
.73
00±2
90a
3.98
...
...
4.0±0
.3a
...
...
0860
8260
7890
...
...
...
7890±2
90a
3.91
...
...
3.9±0
.3a
...
...
0862
3953
7730
7720±5
0g..
...
.77
20±5
0g3.
743.
47±0
.08g
...
3.47±0
.08g
84±4
g..
.08
6514
5269
40..
...
...
.69
40±2
90a
4.07
...
...
4.1±0
.3a
...
...
0865
5712
7380
...
...
...
7380±2
90a
3.45
...
...
3.4±0
.3a
...
...
A125, page 47 of 70
A&A 534, A125 (2011)Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0869
5156
7640
...
...
...
7640±2
90a
3.37
...
...
3.4±0
.3a
...
...
0870
3413
7710
...
...
...
7710±2
90a
3.77
...
...
3.8±0
.3a
...
...
0871
4886
9140
1900
0±0
f..
...
.19
000±2
90f
4.09
4.3
f..
.4.
3±0
.3f
...
...
0871
7065
7440
...
...
...
7440±2
90a
3.76
...
...
3.8±0
.3a
...
...
0873
8244
8170
8260±1
60g
...
...
8260±1
60g
4.15
3.25±0
.12g
...
3.25±0
.12g
133±8
g..
.08
7424
4955
80..
...
...
.55
80±2
90a
4.38
...
...
4.4±0
.3a
...
...
0874
6834
4690
...
...
...
4690±2
90a
3.28
...
...
3.3±0
.3a
...
...
0874
7415
5030
...
...
...
5030±2
90a
3.51
...
...
3.5±0
.3a
...
...
0874
8251
6800
...
...
...
6800±2
90a
4.15
...
...
4.2±0
.3a
...
...
0875
0029
...
7340±6
0g..
...
.73
40±6
0g..
.3.
72±0
.3g
...
3.7±0
.3g
165±8
g..
.08
7666
1969
9065
70±1
20b
...
...
6570±1
20b
3.81
3.59±0
.22b
...
3.59±0
.22b
...
...
0882
7821
7390
...
...
...
7390±2
90a
3.69
...
...
3.7±0
.3a
...
...
0883
8457
6200
...
...
...
6200±2
90a
3.85
...
...
3.9±0
.3a
...
...
0886
9302
7280
...
...
...
7280±2
90a
4.18
...
...
4.2±0
.3a
...
...
0886
9892
...
...
...
...
...
...
...
...
...
...
...
0887
1304
7150
...
...
...
7150±2
90a
3.43
...
...
3.4±0
.3a
...
...
0888
1697
7730
...
...
...
7730±2
90a
3.86
...
...
3.9±0
.3a
...
...
0891
5335
7770
...
...
...
7770±2
90a
3.48
...
...
3.5±0
.3a
...
...
0893
3391
7630
7616±1
93e
...
...
7616±1
93e
3.69
3.71±0
.19e
...
3.71±0
.19e
...
...
0894
0640
...
...
...
...
...
...
...
...
...
...
...
0897
2966
7660
...
...
...
7660±2
90a
3.80
...
...
3.8±0
.3a
...
...
0897
5515
7180
...
...
...
7180±2
90a
3.90
...
...
3.9±0
.3a
...
...
0902
0157
6960
6880±1
50b
...
...
6880±1
50b
3.97
4.12±0
.21b
...
4.12±0
.21b
...
...
0902
0199
6540
...
...
...
6540±2
90a
3.98
...
...
4.0±0
.3a
...
...
0905
2363
7610
...
...
...
7610±2
90a
3.74
...
...
3.7±0
.3a
...
...
0907
2011
...
...
...
...
...
...
...
...
...
...
...
0907
3007
...
...
...
...
...
...
...
...
...
...
...
0907
3985
5990
...
...
...
5990±2
90a
4.37
...
...
4.4±0
.3a
...
...
0907
7192
4750
...
...
...
4750±2
90a
4.40
...
...
4.4±0
.3a
...
...
0910
8615
6710
...
...
...
6710±2
90a
3.81
...
...
3.8±0
.3a
...
...
0911
1056
6800
...
...
...
6800±2
90a
3.65
...
...
3.7±0
.3a
...
...
0911
7875
...
...
...
...
...
...
...
...
...
...
...
0913
8872
7500
...
...
...
7500±2
90a
4.03
...
...
4.0±0
.3a
...
...
0914
3785
7600
...
...
...
7600±2
90a
4.25
...
...
4.3±0
.3a
...
...
0914
7229
7300
...
...
...
7300±2
90a
3.57
...
...
3.6±0
.3a
...
...
0915
6808
7070
...
...
...
7070±2
90a
3.94
...
...
3.9±0
.3a
...
...
0920
1644
...
...
...
...
...
...
...
...
...
...
...
0920
4672
4030
...
...
...
4030±2
90a
1.82
...
...
1.8±0
.3a
...
...
0920
4718
7150
...
...
...
7150±2
90a
3.93
...
...
3.9±0
.3a
...
...
0921
0037
...
...
...
...
...
...
...
...
...
...
...
0921
6367
7840
...
...
...
7840±2
90a
3.65
...
...
3.7±0
.3a
...
...
0922
2942
7000
...
...
...
7000±2
90a
3.99
...
...
4.0±0
.3a
...
...
0922
9318
7140
...
...
...
7140±2
90a
3.65
...
...
3.7±0
.3a
...
...
A125, page 48 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0924
6481
8050
...
...
...
8050±2
90a
3.79
...
...
3.8±0
.3a
...
...
0926
4399
5060
...
...
...
5060±2
90a
4.46
...
...
4.5±0
.3a
...
...
0926
4462
4870
...
...
...
4870±2
90a
3.31
...
...
3.3±0
.3a
...
...
0926
7042
8130
...
...
...
8130±2
90a
3.81
...
...
3.8±0
.3a
...
...
0926
8087
...
...
...
...
...
...
...
...
...
...
...
0927
2082
...
...
...
...
...
...
...
...
...
...
...
0927
4000
5660
...
...
...
5660±2
90a
4.46
...
...
4.5±0
.3a
...
...
0929
1618
7610
...
...
...
7610±2
90a
3.61
...
...
3.6±0
.3a
...
...
0930
6095
6340
...
...
...
6340±2
90a
4.63
...
...
4.6±0
.3a
...
...
0932
4334
7250
...
...
...
7250±2
90a
4.06
...
...
4.1±0
.3a
...
...
0932
7993
4600
...
...
...
4600±2
90a
2.37
...
...
2.4±0
.3a
...
...
0933
6219
6520
...
...
...
6520±2
90a
4.26
...
...
4.3±0
.3a
...
...
0935
1622
7450
...
...
...
7450±2
90a
3.53
...
...
3.5±0
.3a
...
...
0935
3572
7190
...
...
...
7190±2
90a
3.99
...
...
4.0±0
.3a
...
...
0936
8220
6660
...
...
...
6660±2
90a
4.10
...
...
4.1±0
.3a
...
...
0938
6259
5810
...
...
...
5810±2
90a
4.30
...
...
4.3±0
.3a
...
...
0939
1395
7310
...
...
...
7310±2
90a
3.96
...
...
4.0±0
.3a
...
...
0939
5246
...
...
...
...
...
...
...
...
...
...
...
0940
8694
7480
6810±1
30b
...
...
6810±1
30b
3.62
3.80±0
.19b
...
3.80±0
.19b
...
...
0941
3057
8470
8630±1
40g
...
...
8630±1
40g
3.87
3.62±0
.07g
...
3.62±0
.07g
165±8
g..
.09
4509
4082
10..
...
...
.82
10±2
90a
4.21
...
...
4.2±0
.3a
...
...
0945
1598
6060
...
...
...
6060±2
90a
4.56
...
...
4.6±0
.3a
...
...
0945
3075
8060
...
...
...
8060±2
90a
4.00
...
...
4.0±0
.3a
...
...
0945
8750
5070
...
...
...
5070±2
90a
3.69
...
...
3.7±0
.3a
...
...
0947
3000
7130
...
...
...
7130±2
90a
3.88
...
...
3.9±0
.3a
...
...
0948
9590
7160
...
...
...
7160±2
90a
4.09
...
...
4.1±0
.3a
...
...
0949
0042
7060
...
...
...
7060±2
90a
3.98
...
...
4.0±0
.3a
...
...
0949
0067
6880
...
...
...
6880±2
90a
4.07
...
...
4.1±0
.3a
...
...
0950
9296
7400
...
...
...
7400±2
90a
3.61
...
...
3.6±0
.3a
...
...
0951
4879
5880
...
...
...
5880±2
90a
4.10
...
...
4.1±0
.3a
...
...
0952
0434
...
...
...
...
...
...
...
...
...
...
...
0952
0864
...
...
...
...
...
...
...
...
...
...
...
0953
2644
7300
...
...
...
7300±2
90a
3.56
...
...
3.6±0
.3a
...
...
0953
3449
...
...
...
...
...
...
...
...
...
...
...
0953
3489
...
...
...
...
...
...
...
...
...
...
...
0955
0886
7490
...
...
...
7490±2
90a
3.89
...
...
3.9±0
.3a
...
...
0955
1281
7450
...
...
...
7450±2
90a
3.65
...
...
3.7±0
.3a
...
...
0958
0794
7300
...
...
...
7300±2
90a
4.05
...
...
4.1±0
.3a
...
...
0958
2720
5620
...
...
...
5620±2
90a
4.49
...
...
4.5±0
.3a
...
...
0959
3997
7620
...
...
...
7620±2
90a
3.62
...
...
3.6±0
.3a
...
...
0959
4100
6520
...
...
...
6520±2
90a
4.51
...
...
4.5±0
.3a
...
...
0960
4762
7290
...
...
...
7290±2
90a
3.77
...
...
3.8±0
.3a
...
...
0963
0640
6530
...
...
...
6530±2
90a
4.10
...
...
4.1±0
.3a
...
...
A125, page 49 of 70
A&A 534, A125 (2011)Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0963
2537
7820
...
...
...
7820±2
90a
3.83
...
...
3.8±0
.3a
...
...
0964
0204
6440
...
...
...
6440±2
90a
4.25
...
...
4.3±0
.3a
...
...
0964
2894
7050
...
...
...
7050±2
90a
4.09
...
...
4.1±0
.3a
...
...
0964
3982
6580
...
...
...
6580±2
90a
4.20
...
...
4.2±0
.3a
...
...
0965
0390
8390
...
...
...
8390±2
90a
3.68
...
...
3.7±0
.3a
...
...
0965
1065
7390
7010±1
50b
...
...
7010±1
50b
3.67
3.82±0
.21b
...
3.82±0
.21b
...
...
0965
4789
6990
...
...
...
6990±2
90a
4.09
...
...
4.1±0
.3a
...
...
0965
5055
7620
...
...
...
7620±2
90a
3.48
...
...
3.5±0
.3a
...
...
0965
5114
7750
7400±2
00i
...
...
7400±2
00i
3.78
3.9±0
.3i
...
3.9±0
.3i
150±2
0i..
.09
6551
5170
60..
...
...
.70
60±2
90a
4.18
...
...
4.2±0
.3a
...
...
0965
5177
6900
...
...
...
6900±2
90a
3.87
...
...
3.9±0
.3a
...
...
0965
5393
7570
...
...
...
7570±2
90a
4.06
...
...
4.1±0
.3a
...
...
0965
5422
7600
...
...
...
7600±2
90a
3.38
...
...
3.4±0
.3a
...
...
0965
5433
8300
...
...
...
8300±2
90a
...
...
...
...
...
...
0965
5438
6970
...
...
...
6970±2
90a
4.09
...
...
4.1±0
.3a
...
...
0965
5487
...
...
...
...
...
...
...
...
...
...
...
0965
5501
7740
...
...
...
7740±2
90a
3.88
...
...
3.9±0
.3a
...
...
0965
5514
7440
...
...
...
7440±2
90a
3.61
...
...
3.6±0
.3a
...
...
0965
5800
6780
...
...
...
6780±2
90a
4.16
...
...
4.2±0
.3a
...
...
0965
6348
7670
7190±1
60b
...
...
7190±1
60b
3.52
3.9±0
.2b
...
3.9±0
.2b
...
...
0966
4869
7190
...
...
...
7190±2
90a
3.99
...
...
4.0±0
.3a
...
...
0967
3293
8230
...
...
...
8230±2
90a
3.87
...
...
3.9±0
.3a
...
...
0969
3282
...
...
...
...
...
...
...
...
...
...
...
0969
6853
7130
...
...
...
7130±2
90a
4.14
...
...
4.1±0
.3a
...
...
0969
9950
...
...
...
...
...
...
...
...
...
...
...
0970
0145
7590
...
...
...
7590±2
90a
4.03
...
...
4.0±0
.3a
...
...
0970
0322
...
6700±1
00m
...
...
6700±1
00m
...
3.7±0
.1m
...
3.7±0
.1m
19±1
m..
.09
7006
7950
70..
...
...
.50
70±2
90a
4.45
...
...
4.5±0
.3a
...
...
0970
3601
5720
...
...
...
5720±2
90a
4.89
...
...
4.9±0
.3a
...
...
0971
6107
7460
...
...
...
7460±2
90a
3.65
...
...
3.7±0
.3a
...
...
0971
6350
...
...
...
...
...
...
...
...
...
...
...
0971
6947
7300
...
...
...
7300±2
90a
4.04
...
...
4.0±0
.3a
...
...
0976
0531
6740
...
...
...
6740±2
90a
4.03
...
...
4.0±0
.3a
...
...
0976
2713
6960
...
...
...
6960±2
90a
4.09
...
...
4.1±0
.3a
...
...
0976
4712
6020
...
...
...
6020±2
90a
4.68
...
...
4.7±0
.3a
...
...
0976
4965
7460
7470±4
5g..
...
.74
70±4
5g4.
093.
78±0
.19g
...
3.78±0
.19g
85±3
g..
.09
7735
1279
60..
...
...
.79
60±2
90a
3.70
...
...
3.7±0
.3a
...
...
0977
5385
7450
...
...
...
7450±2
90a
4.05
...
...
4.5±0
.3a
...
...
0977
5454
...
7109±1
59e
7050±1
50i
...
7050±1
50i
...
3.91±0
.21e
4.0±0
.3i
3.91±0
.21i
70±5
i..
.09
7764
74..
...
...
...
...
...
...
...
...
...
...
.09
7775
32..
...
...
...
...
...
...
...
...
...
...
.09
7904
7978
40..
...
...
.78
40±2
90a
4.04
...
...
4.0±0
.3a
...
...
0981
2351
7790
7847±8
7g..
...
.78
47±8
7g3.
473.
15±0
.23g
...
3.15±0
.23g
56±4
g..
.
A125, page 50 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
0981
3078
...
6811±1
38b
...
...
6811±1
38b
...
3.67±0
.21b
...
3.67±0
.21b
...
...
0981
8269
...
...
...
...
...
...
...
...
...
...
...
0983
6020
7480
...
...
...
7480±2
90a
4.09
...
...
4.1±0
.3a
...
...
0984
5907
7940
...
...
...
7940±2
90a
4.03
...
...
4.0±0
.3a
...
...
0985
1142
6800
7047±1
56e
...
...
7047±1
56e
3.95
3.97±0
.21e
...
3.97±0
.21e
...
...
0987
4181
7180
...
...
...
7180±2
90a
4.08
...
...
4.1±0
.3a
...
...
0988
1909
6810
...
...
...
6810±2
90a
3.86
...
...
3.9±0
.3a
...
...
0988
5882
5090
...
...
...
5090±2
90a
2.63
...
...
2.6±0
.3a
...
...
0990
9300
6670
...
...
...
6670±2
90a
4.19
...
...
4.2±0
.3a
...
...
0991
3481
7410
...
...
...
7410±2
90a
3.53
...
...
3.5±0
.3a
...
...
0994
4208
7040
...
...
...
7040±2
90a
4.29
...
...
4.3±0
.3a
...
...
0994
4730
5920
...
...
...
5920±2
90a
4.18
...
...
4.2±0
.3a
...
...
0997
0568
7790
...
...
...
7790±2
90a
3.64
...
...
3.6±0
.3a
...
...
0999
1621
5270
...
...
...
5270±2
90a
4.35
...
...
4.4±0
.3a
...
...
0999
1766
6050
...
...
...
6050±2
90a
4.25
...
...
4.3±0
.3a
...
...
0999
4789
5290
...
...
...
5290±2
90a
3.85
...
...
3.9±0
.3a
...
...
0999
5464
4850
...
...
...
4850±2
90a
2.64
...
...
2.6±0
.3a
...
...
1000
0056
8200
...
...
...
8200±2
90a
3.96
...
...
4.0±0
.3a
...
...
1000
2897
7490
...
...
...
7490±2
90a
3.74
...
...
3.7±0
.3a
...
...
1000
4510
4340
...
...
...
4340±2
90a
4.60
...
...
4.6±0
.3a
...
...
1000
6158
4680
...
...
...
4680±2
90a
2.39
...
...
2.4±0
.3a
...
...
1001
4548
7160
...
...
...
7160±2
90a
3.92
...
...
3.9±0
.3a
...
...
1003
0943
6700
...
...
...
6700±2
90a
4.30
...
...
4.3±0
.3a
...
...
1003
5772
7290
...
...
...
7290±2
90a
3.48
...
...
3.5±0
.3a
...
...
1005
6217
6000
...
...
...
6000±2
90a
4.28
...
...
4.3±0
.3a
...
...
1005
6297
7160
...
...
...
7160±2
90a
4.03
...
...
4.0±0
.3a
...
...
1005
7129
4860
...
...
...
4860±2
90a
3.17
...
...
3.2±0
.3a
...
...
1006
2593
5270
...
...
...
5270±2
90a
4.93
...
...
4.9±0
.3a
...
...
1006
4111
7220
...
...
...
7220±2
90a
4.05
...
...
4.1±0
.3a
...
...
1006
5244
7260
...
...
...
7260±2
90a
3.98
...
...
4.0±0
.3a
...
...
1006
8892
4610
...
...
...
4610±2
90a
2.29
...
...
2.3±0
.3a
...
...
1006
9934
7060
...
...
...
7060±2
90a
4.01
...
...
4.0±0
.3a
...
...
1007
3601
7100
6680±1
30b
...
...
6680±1
30b
4.09
3.47±0
.22b
...
3.47±0
.22b
...
...
1009
0345
7190
...
...
...
7190±2
90a
3.94
...
...
3.9±0
.3a
...
...
1009
6499
7780
8021±2
18e
...
...
8012±2
18e
4.13
3.91±0
.16e
...
3.91±0
.16e
...
...
1011
9517
6230
6450±8
0g..
...
.64
50±8
0g4.
384.
3±0
.2g
...
4.3±0
.2g
78±4
g..
.10
1307
7780
20..
...
...
.80
20±2
90a
3.71
...
...
3.7±0
.3a
...
...
1013
4600
5010
...
...
...
5010±2
90a
3.06
...
...
3.1±0
.3a
...
...
1013
4800
7910
...
...
...
7910±2
90a
3.71
...
...
3.7±0
.3a
...
...
1014
0513
5880
6030±1
00b
...
...
6030±1
00b
3.96
4.30±0
.22b
...
4.30±0
.22b
...
...
1014
0665
6620
...
...
...
6620±2
90a
4.37
...
...
4.4±0
.3a
...
...
1016
4569
7720
7130±1
50b
...
...
7130±1
50b
3.66
2.90±0
.22b
...
2.90±0
.22b
...
...
1020
6340
5210
5760±8
0b..
...
.57
60±8
0b4.
464.
48±0
.22b
...
4.48±0
.22b
...
...
A125, page 51 of 70
A&A 534, A125 (2011)Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
1020
8303
6380
6310±1
20b
...
...
6310±1
20b
4.17
4.05±0
.22b
...
4.05±0
.22b
...
...
1020
8345
7150
...
...
...
7150±2
90a
4.01
...
...
4.0±0
.3a
...
...
1021
3987
7830
...
...
...
7830±2
90a
3.94
...
...
3.9±0
.3a
...
...
1025
3943
7740
...
...
...
7740±2
90a
3.70
...
...
3.7±0
.3a
...
...
1025
4547
5880
...
...
...
5880±2
90a
4.84
...
...
4.8±0
.3a
...
...
1026
4728
7790
...
...
...
7790±2
90a
3.85
...
...
3.9±0
.3a
...
...
1026
6959
5050
...
...
...
5050±2
90a
4.40
...
...
4.4±0
.3a
...
...
1027
3246
6070
6300±1
20b
...
...
6300±1
20b
4.15
4.54±0
.21b
...
4.54±0
.21b
...
...
1027
3384
6970
6220±1
10b
...
...
6220±1
10b
3.96
3.79±0
.25b
...
3.79±0
.25b
...
...
1027
3960
6660
6460±1
30b
...
...
6460±1
30b
4.44
4.13±0
.22b
...
4.13±0
.22b
...
...
1027
4244
5210
...
...
...
5210±2
90a
4.53
...
...
4.5±0
.3a
...
...
1028
1360
7530
...
...
...
7530±2
90a
4.05
...
...
4.1±0
.3a
...
...
1028
9211
7900
...
...
...
7900±2
90a
3.73
...
...
3.7±0
.3a
...
...
1033
8279
5400
...
...
...
5400±2
90a
4.47
...
...
4.5±0
.3a
...
...
1033
9342
5950
...
...
...
5950±2
90a
4.19
...
...
4.2±0
.3a
...
...
1034
0511
5850
...
...
...
5850±2
90a
4.40
...
...
4.4±0
.3a
...
...
1034
1072
6300
...
...
...
6300±2
90a
4.18
...
...
4.2±0
.3a
...
...
1035
5055
8110
...
...
...
8110±2
90a
3.74
...
...
3.7±0
.3a
...
...
1036
1229
6980
...
...
...
6980±2
90a
4.03
...
...
4.0±0
.3a
...
...
1038
3933
5100
...
...
...
5100±2
90a
4.27
...
...
4.3±0
.3a
...
...
1038
5459
6920
...
...
...
6920±2
90a
4.23
...
...
4.2±0
.3a
...
...
1038
9037
4710
...
...
...
4710±2
90a
2.19
...
...
2.2±0
.3a
...
...
1039
4332
4920
...
...
...
4920±2
90a
4.47
...
...
4.5±0
.3a
...
...
1044
8764
7400
...
...
...
7400±2
90a
4.00
...
...
4.0±0
.3a
...
...
1045
0550
4970
...
...
...
4970±2
90a
3.63
...
...
3.6±0
.3a
...
...
1045
0675
6420
...
...
...
6420±2
90a
4.12
...
...
4.1±0
.3a
...
...
1045
1090
7580
7640±6
0g..
...
.76
40±6
0g4.
133.
74±0
.19g
...
3.74±0
.19g
44±2
g..
.10
4512
5056
50..
...
...
.56
50±2
90a
4.06
...
...
4.1±0
.3a
...
...
1045
3475
5200
...
...
...
5200±2
90a
4.47
...
...
4.5±0
.3a
...
...
1046
7969
8850
...
...
...
8850±2
90a
4.09
...
...
4.1±0
.3a
...
...
1047
1914
7290
...
...
...
7290±2
90a
3.95
...
...
4.0±0
.3a
...
...
1048
4808
8140
...
...
...
8140±2
90a
3.99
...
...
4.0±0
.3a
...
...
1052
6137
3180
...
...
...
3180±2
90a
...
...
...
...
...
...
1052
6615
6080
...
...
...
6080±2
90a
4.62
...
...
4.6±0
.3a
...
...
1053
3506
6510
...
...
...
6510±2
90a
4.18
...
...
4.2±0
.3a
...
...
1053
3616
8320
...
...
...
8320±2
90a
3.77
...
...
3.8±0
.3a
...
...
1053
4629
6070
...
...
...
6070±2
90a
3.94
...
...
3.9±0
.3a
...
...
1053
6147
1249
020
800±0
f..
...
.20
800±2
90f
5.89
3.8
f..
.3.
8±0
.3f
195±1
0f
...
1053
7907
7500
...
...
...
7500±2
90a
3.45
...
...
3.4±0
.3a
...
...
1054
9292
7740
...
...
...
7740±2
90a
3.94
...
...
3.9±0
.3a
...
...
1054
9371
6970
...
...
...
6970±2
90a
3.95
...
...
4.0±0
.3a
...
...
1058
6837
7020
...
...
...
7020±2
90a
4.23
...
...
4.2±0
.3a
...
...
1059
0857
7560
...
...
...
7560±2
90a
3.76
...
...
3.8±0
.3a
...
...
A125, page 52 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
1060
4429
7620
7200±2
00p
...
...
7200±2
00p
3.53
3.5±0
.5p
...
3.5±0
.3a
60p
...
1061
5125
7160
...
...
...
7160±2
90a
3.59
...
...
3.6±0
.3a
...
...
1064
7493
...
...
...
...
...
...
...
...
...
...
...
1064
7611
7130
...
...
...
7130±2
90a
3.97
...
...
4.0±0
.3a
...
...
1064
7860
5460
...
...
...
5460±2
90a
4.61
...
...
4.6±0
.3a
...
...
1064
8728
6600
...
...
...
6600±2
90a
4.08
...
...
4.1±0
.3a
...
...
1065
2134
6880
...
...
...
6880±2
90a
4.17
...
...
4.2±0
.3a
...
...
1065
8302
1481
015
900±0
f..
...
.15
900±2
90f
6.08
3.9
f..
.3.
9±0
.3f
...
...
1065
8802
7480
...
...
...
7480±2
90a
4.11
...
...
4.1±0
.3a
...
...
1066
3892
5960
6020±1
00b
...
...
6020±1
00b
4.32
4.9±0
.2b
...
4.9±0
.2b
...
...
1066
4703
7630
...
...
...
7630±2
90a
3.65
...
...
3.7±0
.3a
...
...
1066
4975
7950
6641±1
23e
...
...
6641±1
23e
3.58
...
...
3.6±0
.3a
...
...
1067
5762
7220
...
...
...
7220±2
90a
3.59
...
...
3.6±0
.3a
...
...
1068
4587
7290
...
...
...
7290±2
90a
3.83
...
...
3.8±0
.3a
...
...
1068
4673
7110
...
...
...
7110±2
90a
3.91
...
...
3.9±0
.3a
...
...
1068
5653
7970
...
...
...
7970±2
90a
3.90
...
...
3.9±0
.3a
...
...
1068
6752
7270
...
...
...
7270±2
90a
3.95
...
...
4.0±0
.3a
...
...
1070
9716
6050
...
...
...
6050±2
90a
4.35
...
...
4.4±0
.3a
...
...
1071
3398
...
...
...
...
...
...
...
...
...
...
...
1071
7871
7290
...
...
...
7290±2
90a
3.50
...
...
3.5±0
.3a
...
...
1072
3718
5370
...
...
...
5370±2
90a
4.18
...
...
4.2±0
.3a
...
...
1073
0618
6200
...
...
...
6200±2
90a
4.22
...
...
4.2±0
.3a
...
...
1077
5968
7490
...
...
...
7490±2
90a
3.84
...
...
3.8±0
.3a
...
...
1077
7541
...
...
...
...
...
...
...
...
...
...
...
1077
7903
7320
...
...
...
7320±2
90a
3.53
...
...
3.5±0
.3a
...
...
1077
8640
6390
...
...
...
6390±2
90a
4.16
...
...
4.2±0
.3a
...
...
1078
3150
7340
...
...
...
7340±2
90a
3.93
...
...
3.9±0
.3a
...
...
1078
8451
8790
...
...
...
8790±2
90a
4.02
...
...
4.0±0
.3a
...
...
1079
7526
1171
023
600±5
600
f20
870±0
f..
.20
870±5
600
f4.
413.
2±0
.0f
...
3.2±0
.3f
...
...
1079
7849
6020
...
...
...
6020±2
90a
4.20
...
...
4.2±0
.3a
...
...
1081
3970
7420
...
...
...
7420±2
90a
3.61
...
...
3.6±0
.3a
...
...
1081
5466
8310
...
...
...
8310±2
90a
3.86
...
...
3.9±0
.3a
...
...
1085
3783
7830
...
...
...
7830±2
90a
3.88
...
...
3.9±0
.3a
...
...
1086
1649
5900
...
...
...
5900±2
90a
4.18
...
...
4.2±0
.3a
...
...
1090
2738
4640
...
...
...
4640±2
90a
2.47
...
...
2.5±0
.3a
...
...
1092
0182
5930
...
...
...
5930±2
90a
4.24
...
...
4.2±0
.3a
...
...
1092
0273
5570
...
...
...
5570±2
90a
4.09
...
...
4.1±0
.3a
...
...
1092
0447
7900
...
...
...
7900±2
90a
3.98
...
...
4.0±0
.3a
...
...
1097
1674
5530
...
...
...
5530±2
90a
4.31
...
...
4.3±0
.3a
...
...
1097
5247
7780
...
...
...
7780±2
90a
...
...
...
3.9±0
.3a
...
...
1097
7859
8050
8190±7
0g..
...
.81
90±7
0g3.
943.
61±0
.07g
...
3.61±0
.07g
63±3
g..
.10
9880
0973
20..
...
...
.73
20±2
90a
4.00
...
...
4.0±0
.3a
...
...
1101
3201
7780
7200±2
00p
...
...
7200±2
00p
3.82
3.5±0
.2p
...
3.5±0
.2p
100p
...
A125, page 53 of 70
A&A 534, A125 (2011)Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
1101
7401
5410
...
...
...
5410±2
90a
4.39
...
...
4.4±0
.3a
...
...
1102
0521
6670
...
...
...
6670±2
90a
4.31
...
...
4.3±0
.3a
...
...
1102
1188
7320
...
...
...
7320±2
90a
4.15
...
...
4.2±0
.3a
...
...
1102
7270
6850
...
...
...
6850±2
90a
3.91
...
...
3.9±0
.3a
...
...
1106
7972
5990
...
...
...
5990±2
90a
4.46
...
...
4.5±0
.3a
...
...
1106
9435
5590
...
...
...
5590±2
90a
4.55
...
...
4.6±0
.3a
...
...
1108
2830
7020
...
...
...
7020±2
90a
3.96
...
...
4.0±0
.3a
...
...
1109
0405
7710
...
...
...
7710±2
90a
3.71
...
...
3.7±0
.3a
...
...
1112
2763
6530
...
...
...
6530±2
90a
4.28
...
...
4.3±0
.3a
...
...
1112
5764
7980
...
...
...
7980±2
90a
3.85
...
...
3.9±0
.3a
...
...
1112
7190
7630
...
...
...
7630±2
90a
3.72
...
...
3.7±0
.3a
...
...
1112
8041
5670
...
...
...
5670±2
90a
4.47
...
...
4.5±0
.3a
...
...
1112
8126
5940
...
...
...
5940±2
90a
4.32
...
...
4.3±0
.3a
...
...
1112
9289
5990
...
...
...
5990±2
90a
4.31
...
...
4.3±0
.3a
...
...
1118
0361
8330
...
...
...
8330±2
90a
3.55
...
...
3.6±0
.3a
...
...
1118
2716
5390
...
...
...
5390±2
90a
4.22
...
...
4.2±0
.3a
...
...
1118
3399
7260
...
...
...
7260±2
90a
4.03
...
...
4.0±0
.3a
...
...
1118
3539
7470
...
...
...
7470±2
90a
3.51
...
...
3.5±0
.3a
...
...
1119
3046
8170
...
...
...
8170±2
90a
3.70
...
...
3.7±0
.3a
...
...
1119
7934
7860
...
...
...
7860±2
90a
3.68
...
...
3.7±0
.3a
...
...
1119
9412
7470
...
...
...
7470±2
90a
3.70
...
...
3.7±0
.3a
...
...
1123
0518
6140
...
...
...
6140±2
90a
4.38
...
...
4.4±0
.3a
...
...
1123
2922
...
...
...
...
...
...
...
...
...
...
...
1123
3189
...
...
...
...
...
...
...
...
...
...
...
1123
4888
5940
...
...
...
5940±2
90a
4.33
...
...
4.3±0
.3a
...
...
1123
5721
5740
...
...
...
5740±2
90a
4.33
...
...
4.3±0
.3a
...
...
1123
6253
5430
...
...
...
5430±2
90a
4.45
...
...
4.5±0
.3a
...
...
1124
0653
6460
...
...
...
6460±2
90a
4.12
...
...
4.1±0
.3a
...
...
1125
3226
6470
6736±7
5c68
00±4
00h
6622±0
o67
36±7
5c4.
184.
2±0
.1h
...
4.2±0
.1h
19±1
h..
.11
2857
6774
60..
...
...
.74
60±2
90a
3.65
...
...
3.7±0
.3a
...
...
1128
8686
...
...
...
...
...
...
...
...
...
...
...
1129
0197
6340
...
...
...
6340±2
90a
4.30
...
...
4.3±0
.3a
...
...
1130
9335
7280
...
...
...
7280±2
90a
3.86
...
...
3.9±0
.3a
...
...
1134
0063
4900
...
...
...
4900±2
90a
3.10
...
...
3.1±0
.3a
...
...
1134
0713
...
...
...
...
...
...
...
...
...
...
...
1134
2032
...
...
...
...
...
...
...
...
...
...
...
1139
3580
3850
...
...
...
3850±2
90a
4.45
...
...
4.5±0
.3a
...
...
1139
4216
5140
...
...
...
5140±2
90a
4.19
...
...
4.2±0
.3a
...
...
1139
5018
5420
5740±8
0b..
...
.57
40±8
0b4.
473.
65±0
.24b
...
3.65±0
.24b
...
...
1139
5028
5320
5720±8
0b..
...
.53
20±2
90a
4.42
4.26±0
.23b
...
4.26±0
.23b
...
...
1139
5392
...
...
...
...
...
...
...
...
...
...
...
1140
2951
...
7150±1
20i
7250±1
00k
...
7250±1
00k
...
3.5±0
.1i
3.5±0
.1k
3.5±0
.1k
100±2
i..
.11
4457
7461
1062
10±1
10b
...
...
6210±2
90b
4.33
4.64±0
.20b
...
4.6±0
.2b
...
...
A125, page 54 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
2.co
ntin
ued.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
1144
5913
6950
7200±1
20i
7250±1
00k
...
7250±1
00k
3.89
3.5±0
.2i
3.5±0
.2k
3.5±0
.2k
51±1
k..
.11
4461
4343
00..
...
...
.43
00±2
90a
4.47
...
...
4.5±0
.3a
...
...
1144
6181
5770
...
...
...
5770±2
90a
4.38
...
...
4.4±0
.3a
...
...
1144
7883
6690
6800±4
00h
...
...
6690±2
90a
4.07
4.2±0
.1h
...
4.2±0
.1h
105±3
h..
.11
4479
5364
10..
...
...
.64
10±2
90a
4.43
...
...
4.4±0
.3a
...
...
1144
8266
5980
6110±1
10b
...
...
6110±1
10b
4.27
4.69±0
.20b
...
4.7±0
.2b
...
...
1144
9931
5940
6130±1
10b
...
...
6130±1
10b
4.52
4.84±0
.20b
...
4.8±0
.2b
...
...
1145
4008
6870
...
...
...
6870±2
90a
3.79
...
...
3.8±0
.3a
...
...
1149
4765
7050
...
...
...
7050±2
90a
3.99
...
...
4.0±0
.3a
...
...
1149
7012
7660
...
...
...
7660±2
90a
3.87
...
...
3.9±0
.3a
...
...
1149
8538
6290
6410±7
0c64
50±8
0g64
41±0
o64
10±7
0c4.
043.
30±0
.41g
...
3.3±0
.3g
40±1
g45
o
1149
9354
5780
6020±1
00b
...
...
6020±1
00b
4.47
4.39±0
.22b
...
4.39±0
.22b
...
...
1149
9453
5810
...
...
...
5810±2
90a
4.38
...
...
4.4±0
.3a
...
...
1150
2075
3980
...
...
...
3980±2
90a
4.57
...
...
4.6±0
.3a
...
...
1150
8397
7460
...
...
...
7460±2
90a
3.52
...
...
3.5±0
.3a
...
...
1150
9728
7790
...
...
...
7790±2
90a
3.73
...
...
3.7±0
.3a
...
...
1151
5690
6460
...
...
...
6460±2
90a
4.11
...
...
4.1±0
.3a
...
...
1154
9609
5580
...
...
...
5580±2
90a
4.56
...
...
4.6±0
.3a
...
...
1155
1622
5690
...
...
...
5690±2
90a
4.50
...
...
4.5±0
.3a
...
...
1157
2666
7040
...
...
...
7040±2
90a
3.49
...
...
3.5±0
.3a
...
...
1160
2449
7390
...
...
...
7390±2
90a
3.83
...
...
3.8±0
.3a
...
...
1160
7193
7210
...
...
...
7210±2
90a
4.14
...
...
4.1±0
.3a
...
...
1161
2274
7470
...
...
...
7470±2
90a
3.62
...
...
3.6±0
.3a
...
...
1162
2328
...
...
...
...
...
...
...
...
...
...
...
1165
1083
...
...
...
...
...
...
...
...
...
...
...
1165
1147
6030
...
...
...
6030±2
90a
4.48
...
...
4.5±0
.3a
...
...
1165
3958
6620
6450±1
20b
...
...
6450±1
20b
4.25
4.20±0
.21b
...
4.20±0
.21b
...
...
1165
4210
6060
6200±1
10b
...
...
6200±1
10b
4.46
4.63±0
.21b
...
4.63±0
.21b
...
...
1165
7840
6120
...
...
...
6120±2
90a
4.66
...
...
4.7±0
.3a
...
...
1166
1993
7200
...
...
...
7200±2
90a
3.93
...
...
3.9±0
.3a
...
...
1167
1429
7360
...
...
...
7360±2
90a
3.58
...
...
3.6±0
.3a
...
...
1170
0370
8290
...
...
...
8290±2
90a
3.99
...
...
4.0±0
.3a
...
...
1170
0604
7630
...
...
...
7630±2
90a
3.85
...
...
3.9±0
.3a
...
...
1170
6449
...
...
...
...
...
...
...
...
...
...
...
1170
6564
4550
...
...
...
4550±2
90a
2.35
...
...
2.4±0
.3a
...
...
1170
7341
4210
...
...
...
4210±2
90a
4.58
...
...
4.6±0
.3a
...
...
1170
8170
6640
6776±7
9c69
18±0
d67
14±0
o67
76±7
9c4.
154.
21±0
.07d
...
4.21±0
.07d
...
...
1171
4150
8270
...
...
...
8270±2
90a
3.87
...
...
3.9±0
.3a
...
...
1171
8839
8260
...
...
...
8260±2
90a
3.78
...
...
3.8±0
.3a
...
...
1175
3169
7210
...
...
...
7210±2
90a
3.94
...
...
3.9±0
.3a
...
...
1175
4974
...
...
...
...
...
...
...
...
...
...
...
1182
1140
8050
...
...
...
8050±2
90a
3.85
...
...
3.9±0
.3a
...
...
1182
2666
8440
...
...
...
8440±2
90a
3.87
...
...
3.9±0
.3a
...
...
A125, page 55 of 70
A&A 534, A125 (2011)
Tabl
e2.
cont
inue
d.
Teff
(K)
logg
(dex
)v
sin
i(km
s−1)
KIC
IDK
ICa
Lit
erat
ure
Lit
erat
ure
Lit
erat
ure
Ado
pted�
KIC
aL
iter
atur
eL
iter
atur
eA
dopt
ed�
Spe
ctra
Spe
ctra
1182
4964
7190
...
...
...
7190±2
90a
3.97
...
...
4.0±0
.3a
...
...
1187
4676
8220
...
...
...
8220±2
90a
4.00
...
...
4.0±0
.3a
...
...
1187
4898
7010
6650±1
30b
...
...
6650±1
30b
3.96
3.72±0
.22b
...
3.72±0
.22b
...
...
1191
0256
7130
...
...
...
7130±2
90a
3.53
...
...
3.5±0
.3a
...
...
1191
0642
7660
...
...
...
7660±2
90a
3.59
...
...
3.6±0
.3a
...
...
1197
3705◦
7400
1189
8±0
f73
00±3
00i
1115
0±0
j11
150±2
90j
4.04
4.2±0
.3i
3.96
j4.
0±0
.3j
120±2
0i10
3±1
0j
1201
8834
7270
...
...
...
7270±2
90a
4.00
...
...
4.0±0
.3a
...
...
1202
0590
8020
...
...
...
8020±2
90a
3.67
...
...
3.7±0
.3a
...
...
1205
8428
7110
...
...
...
7110±2
90a
3.99
...
...
4.0±0
.3a
...
...
1206
2443
7380
...
...
...
7380±2
90a
3.97
...
...
4.0±0
.3a
...
...
1206
8180
7460
...
...
...
7460±2
90a
3.78
...
...
3.8±0
.3a
...
...
1210
2187
7030
...
...
...
7030±2
90a
4.13
...
...
4.1±0
.3a
...
...
1211
7689
6910
...
...
...
6910±2
90a
4.09
...
...
4.1±0
.3a
...
...
1212
2075
7120
...
...
...
7120±2
90a
3.89
...
...
3.9±0
.3a
...
...
1221
6817
6680
...
...
...
6680±2
90a
3.81
...
...
3.8±0
.3a
...
...
1221
7281
7130
...
...
...
7130±2
90a
3.71
...
...
3.7±0
.3a
...
...
1235
3648
7410
7190±4
5g..
...
.71
90±4
5g3.
473.
60±0
.26g
...
3.60±0
.26g
189±1
2g..
.12
6470
7072
80..
...
...
.72
80±2
90a
3.87
...
...
3.9±0
.3a
...
...
1278
4394
7850
...
...
...
7850±2
90a
3.61
...
...
3.6±0
.3a
...
...
Not
es.(◦)
Spe
ctro
scop
icbi
nary
;va
lues
deri
ved
from
phot
omet
ry:
(a)
KIC
Cat
alog
ue,
Lat
ham
etal
.(2
005)
;(b
)S
PM
phot
omet
ry,
this
pape
r;(c
)M
asan
aet
al.
(200
6);
(d)
All
ende
Pri
eto
&L
ambe
rt(1
999)
;(e)
Hau
ck&
Mer
mil
liod
(199
8);v
alue
sde
rive
dfr
omph
otom
etry
orsp
ectr
osco
py:(f
)B
alon
aet
al.(
2011
b);v
alue
sde
rive
dfr
omsp
ectr
osco
py:(g
)T
LS
spec
tra,
this
pape
r;(h
)S
OP
HIE
spec
tra,
this
pape
r;(i
)C
atan
zaro
etal
.(20
11);
(j)
Leh
man
net
al.(
2011
);(k
)B
alon
aet
al.(
2011
c);(l
)A
ntoc
ieta
l.,pr
iv.c
omm
.;(m
)B
rege
ret
al.(
2011
);(n
)G
lebo
cki&
Sta
wik
owsk
i(20
00);
(o)
Nor
dstr
ömet
al.
(200
4);(p
)C
atan
zaro
etal
.(20
10);
(q)
Mol
enda
-Zak
owic
zet
al.(
2008
);(r
)A
ntoc
ieta
l.(2
011)
;(�)
the
esti
mat
eder
rors
onth
eK
ICva
lues
are
290
Kfo
rT
effan
d0.
3de
xfo
rlo
gg
(see
text
).
A125, page 56 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
3.C
lass
ifica
tion
and
char
acte
riza
tion
ofδ
Sct
,γD
or,a
ndhy
brid
star
s.
KIC
IDC
lass
NNγ
Dor
NδS
ctN
tota
l(F
req
Ran
ge) γ
Dor
(Fre
qR
ange
) δS
ctA
mpl
itud
e hig
hF
req h
igh
Fla
g(d−1
)(d−1
)(p
pm)
(d−1
)δ
Sct
star
s01
1621
50δ
Sct
136
013
620
4..
.[4
.0,3
5.5]
1857
16.4
08..
.01
5717
17δ
Sct
980
9812
6..
.[5
.4,5
6.5]
767
41.2
35•
0171
8594
δS
ct53
053
139
...
[5.4
,76.
1]16
7418
.328
...
0230
3365
δS
ct37
037
162
...
[5.0
,34.
8]73
4014
.806
...
0243
9660
δS
ct36
036
51..
.[1
5.9,
79.5
]82
942
.967
...
0257
1868
δS
ct18
90
189
345
...
[4.0
,52.
7]17
6620
.550
...
0257
2386
δS
ct12
012
59..
.[9
.1,1
2.1]
1091
9.48
1•
0298
7660
δS
ct18
60
186
537
...
[4.3
,64.
0]36
1015
.049
...
0321
7554
δS
ct13
80
138
446
...
[4.0
,56.
1]24
075.
604
...
0321
9256
δS
ct35
50
355
532
...
[4.0
,79.
7]14
3117
.857
...
0334
7643
δS
ct93
093
164
...
[4.2
,68.
2]65
429
.695
...
0342
5802
δS
ct16
016
30..
.[2
4.3,
44.4
]64
331
.693
...
0342
9637
δS
ct18
018
29..
.[9
.3,1
9.4]
1640
10.3
38..
.03
4404
95δ
Sct
80
89
...
[4.1
,21.
7]33
215
.973
...
0345
8318
δS
ct16
016
47..
.[7
.0,2
3.0]
1147
13.4
90..
.03
5581
45δ
Sct
810
8114
0..
.[4
.0,4
4.2]
2891
22.1
22..
.03
6343
84δ
Sct
208
020
857
3..
.[4
.4,6
8.7]
1584
11.6
48..
.03
6441
16δ
Sct
750
7595
...
[6.5
,42.
6]13
2530
.022
...
0365
5513
δS
ct12
012
46..
.[5
.2,1
2.6]
2848
8.33
3..
.03
7600
02δ
Sct
860
8615
9..
.[7
.3,3
3.1]
2246
16.2
60..
.03
7616
41δ
Sct
620
6214
9..
.[1
1.6,
74.6
]50
637
.307
...
0385
0810
δS
ct10
40
104
422
...
[4.5
,51.
1]19
3614
.462
...
0394
1283
δS
ct11
40
114
173
...
[9.4
,69.
1]10
6733
.270
...
0394
2911
δS
ct19
00
190
295
...
[4.3
,52.
9]12
2029
.490
...
0403
5667
δS
ct31
031
78..
.[4
.8,7
9.0]
552
46.3
99..
.04
0484
94δ
Sct
870
8725
4..
.[9
.9,4
2.0]
4701
14.3
64..
.04
0770
32δ
Sct
274
027
486
9..
.[4
.6,7
5.8]
3707
14.4
82..
.04
1685
74δ
Sct
430
4213
9..
.[4
.4,1
8.9]
1495
7.98
9..
.04
2527
57δ
Sct
135
013
533
2..
.[5
.0,3
6.5]
3961
21.4
80..
.04
2693
37δ
Sct
106
010
629
7..
.[5
.0,6
9.1]
1552
35.2
15•
0438
3117
δS
ct11
011
12..
.[2
2.8,
45.1
]39
926
.259
...
0464
7763
δS
ct14
20
142
494
...
[4.1
,74.
2]39
7323
.717
...
0464
9476
δS
ct88
088
195
...
[4.3
,46.
7]15
4420
.699
...
0484
0675
δS
ct49
049
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7.4]
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A125, page 57 of 70
A&A 534, A125 (2011)Ta
ble
3.co
ntin
ued.
KIC
IDC
lass
NNγ
Dor
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A125, page 58 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
3.co
ntin
ued.
KIC
IDC
lass
NNγ
Dor
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ge) γ
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A125, page 59 of 70
A&A 534, A125 (2011)Ta
ble
3.co
ntin
ued.
KIC
IDC
lass
NNγ
Dor
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A125, page 60 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
3.co
ntin
ued.
KIC
IDC
lass
NNγ
Dor
NδS
ctN
tota
l(F
req
Ran
ge) γ
Dor
(Fre
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ange
) δS
ctA
mpl
itud
e hig
hF
req h
igh
Fla
g(d−1
)(d−1
)(p
pm)
(d−1
)10
6845
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Sct
306
030
676
0..
.[4
.0,4
8.9]
7128
12.8
37..
.10
6846
73δ
Sct
90
928
...
[5.8
,10.
4]74
3010
.387
...
1068
6752
δS
ct62
062
87..
.[1
2.7,
58.8
]62
840
.473
...
1071
3398
δS
ct80
080
383
...
[5.1
,48.
1]31
0615
.348
...
1071
7871
δS
ct23
40
234
693
...
[4.2
,39.
7]37
7812
.217
...
1077
5968
δS
ct11
011
17..
.[4
.5,2
4.7]
432
21.5
49..
.10
7779
03δ
Sct
277
027
796
6..
.[4
.1,3
8.0]
4486
16.7
91..
.10
7884
51δ
Sct
122
012
230
1..
.[4
.0,4
3.1]
3603
23.1
60..
.10
8139
70δ
Sct
183
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364
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9.8]
5261
9.60
6..
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8154
66δ
Sct
267
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9.0]
2188
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12..
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8537
83δ
Sct
102
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213
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.[4
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0.7]
1708
28.9
55..
.10
9204
47δ
Sct
890
8913
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2.9]
1622
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23..
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9778
59δ
Sct
670
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0..
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3.6]
2014
59.9
69..
.10
9880
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Sct
169
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8.8]
5483
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0132
01δ
Sct
260
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[5.5
,57.
8]52
233
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...
1102
1188
δS
ct70
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77..
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5.5]
1360
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0904
05δ
Sct
540
5489
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[4.1
,37.
5]99
214
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...
1112
5764
δS
ct35
035
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.[1
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]18
6838
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...
1112
7190
δS
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047
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...
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7,59
.3]
3559
18.7
31..
.11
1835
39δ
Sct
213
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344
0..
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8.8]
2265
22.6
64..
.11
3407
13δ
Sct
260
2611
3..
.[4
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3.6]
1133
310
.150
...
1139
5392
δS
ct90
090
413
...
[4.8
,46.
2]65
7725
.188
...
1140
2951
δS
ct97
097
161
...
[5.3
,49.
1]88
423
.846
...
1149
7012
δS
ct85
085
258
...
[4.0
,41.
1]16
6024
.105
...
1166
1993
δS
ct14
70
147
440
...
[4.3
,49.
5]34
7314
.035
...
1167
1429
δS
ct31
20
312
624
...
[4.1
,49.
4]14
2515
.970
...
1170
0370
δS
ct30
030
30..
.[5
.2,7
2.0]
101
28.6
78..
.11
7549
74δ
Sct
870
8439
6..
.[4
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9.9]
5765
816
.345
...
1182
1140
δS
ct32
032
70..
.[1
8.4,
57.4
]23
524
.877
...
1187
4676
δS
ct73
073
241
...
[4.9
,67.
5]17
9813
.577
...
1202
0590
δS
ct19
019
34..
.[1
8.8,
37.4
]39
322
.215
...
1206
8180
δS
ct29
80
298
722
...
[4.1
,49.
3]22
2620
.302
...
1235
3648
δS
ct48
044
277
...
[4.3
,24.
0]39
287.
818
...
1264
7070
δS
ct33
033
52..
.[9
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9.2]
1110
13.3
56..
.12
7843
94δ
Sct
30
311
...
[29.
4,47
.9]
107
42.6
52..
.H
ybri
dst
ars
0216
8333
hybr
id68
1353
278
[0.2
,5.0
][5
.5,4
9.1]
1452
21.7
18..
.02
6943
37hy
brid
5227
2212
3[0
.2,4
.9]
[5.4
,34.
6]50
624
.500
...
0270
7479
hybr
id18
858
124
674
[0.2
,5.0
][5
.1,5
1.1]
2267
15.1
58..
.02
8532
80hy
brid
5328
2310
2[0
.2,5
.0]
[5.0
,35.
1]98
813
.000
...
0297
5832
hybr
id15
104
128
[0.3
,3.5
][5
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6.5]
733
2.03
4•
0309
7912
hybr
id21
154
56[0
.2,4
.6]
[5.2
,20.
0]21
21.
466
•03
1196
04hy
brid
171
1215
719
6[0
.2,4
.6]
[5.0
,76.
9]55
441
.151
...
A125, page 61 of 70
A&A 534, A125 (2011)Ta
ble
3.co
ntin
ued.
KIC
IDC
lass
NNγ
Dor
NδS
ctN
tota
l(F
req
Ran
ge) γ
Dor
(Fre
qR
ange
) δS
ctA
mpl
itud
e hig
hF
req h
igh
Fla
g(d−1
)(d−1
)(p
pm)
(d−1
)03
2314
06hy
brid
362
6229
279
3[0
.2,5
.0]
[5.0
,65.
0]17
6117
.438
...
0324
0556
hybr
id19
140
151
329
[0.3
,5.0
][5
.0,6
3.6]
867
25.2
20..
.03
2454
20hy
brid
4210
3222
4[0
.8,3
.9]
[5.0
,45.
8]27
3314
.097
...
0333
7002
hybr
id16
292
6452
9[0
.2,4
.9]
[5.0
,52.
8]45
944.
558
...
0343
7940
hybr
id34
710
622
495
7[0
.2,5
.0]
[5.1
,63.
2]48
8610
.476
...
0345
3494
hybr
id17
647
129
358
[0.3
,5.0
][5
.0,6
2.9]
487
7.49
9..
.03
8511
51hy
brid
73
122
[0.2
,1.3
][2
6.5,
26.5
]42
26.4
87..
.03
9707
29hy
brid
156
4410
533
2[0
.2,5
.0]
[5.6
,28.
2]13
9418
.828
...
0404
4353
hybr
id59
1344
153
[0.6
,4.8
][5
.1,5
4.5]
553
2.39
0..
.04
1706
31hy
brid
495
7441
213
8[0
.2,5
.0]
[5.1
,59.
5]62
648.
314
...
0418
0199
hybr
id91
3061
404
[0.5
,4.9
][5
.2,5
1.2]
790
3.28
4..
.04
2815
81hy
brid
7751
2128
2[0
.2,4
.6]
[5.2
,54.
3]47
80.
882
...
0447
6836
hybr
id9
53
52[0
.5,5
.0]
[5.5
,10.
9]96
99.
859
...
0448
0321
hybr
id14
254
8650
4[0
.2,5
.0]
[5.1
,61.
2]23
230.
710
...
0448
8840
hybr
id17
842
129
517
[0.3
,5.0
][5
.0,5
1.3]
1277
15.8
03..
.04
5509
62hy
brid
179
9383
603
[0.2
,5.0
][5
.3,5
4.1]
2912
2.25
9..
.04
5563
45hy
brid
137
1911
618
6[0
.3,4
.2]
[13.
1,64
.5]
653
26.6
40..
.04
6712
25hy
brid
7439
3019
1[0
.2,5
.0]
[5.1
,46.
3]12
718.
880
...
0476
8677
hybr
id13
37
47[0
.2,4
.7]
[6.2
,52.
2]12
422
.904
...
0491
9818
hybr
id45
3410
74[0
.4,5
.0]
[5.0
,32.
4]34
22.
871
...
0492
0125
hybr
id28
208
92[0
.4,4
.8]
[5.6
,29.
3]39
023
.884
...
0498
9900
hybr
id42
2416
210
[0.2
,4.8
][5
.0,3
8.9]
718
2.18
9..
.05
0382
28hy
brid
203
7212
561
6[0
.2,5
.0]
[5.1
,49.
7]22
610.
904
...
0521
9533
hybr
id35
2211
112
[0.3
,4.6
][5
.4,2
9.9]
437
10.2
85..
.05
3563
49hy
brid
4114
2260
[0.2
,5.0
][5
.1,5
1.5]
205
9.82
6..
.05
4372
06hy
brid
120
3282
258
[0.2
,4.7
][5
.2,4
9.7]
1637
13.0
11..
.05
4460
68hy
brid
6333
2421
7[0
.3,4
.9]
[5.3
,52.
1]55
80.
287
...
0547
3171
hybr
id11
246
6439
1[0
.3,4
.8]
[5.1
,54.
5]35
787.
574
...
0547
6864
hybr
id85
2654
374
[0.2
,3.4
][5
.1,1
9.2]
1862
1.66
7•
0564
1711
hybr
id11
946
6829
4[0
.3,4
.8]
[5.0
,51.
6]75
821
.111
...
0572
2346
hybr
id17
972
9950
7[0
.2,4
.9]
[5.0
,50.
4]30
0211
.325
•05
7244
40hy
brid
425
7034
366
3[0
.2,5
.0]
[5.1
,79.
7]19
1819
.251
...
0581
0113
hybr
id41
1722
92[0
.2,3
.5]
[5.8
,20.
6]65
20.
333
...
0585
7714
hybr
id21
041
166
850
[0.2
,3.7
][5
.0,5
5.0]
2293
012
.227
...
0594
0273
hybr
id17
080
8146
3[0
.2,5
.0]
[5.0
,51.
0]15
713.
016
...
0596
5837
hybr
id93
2960
354
[0.7
,4.5
][5
.0,4
9.2]
7243
3.39
2..
.06
0327
30hy
brid
8726
5714
4[0
.2,5
.0]
[5.0
,78.
1]11
4016
.267
...
0606
7817
hybr
id13
327
103
296
[0.2
,4.9
][5
.1,7
9.7]
1374
34.4
08..
.06
1413
72hy
brid
195
1421
[0.3
,4.8
][5
.1,3
1.9]
338
18.9
91•
0614
2919
hybr
id59
3719
115
[0.3
,4.9
][5
.4,4
9.2]
986
16.3
16..
.06
1876
65hy
brid
184
6012
165
9[0
.2,5
.0]
[5.0
,35.
5]38
2611
.729
...
0619
9731
hybr
id42
1821
215
[0.4
,4.9
][5
.1,2
2.5]
2183
7.64
3..
.06
2688
90hy
brid
359
7328
415
2[0
.2,4
.8]
[5.1
,55.
1]15
399
6.86
6..
.
A125, page 62 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
3.co
ntin
ued.
KIC
IDC
lass
NNγ
Dor
NδS
ctN
tota
l(F
req
Ran
ge) γ
Dor
(Fre
qR
ange
) δS
ctA
mpl
itud
e hig
hF
req h
igh
Fla
g(d−1
)(d−1
)(p
pm)
(d−1
)06
2894
68hy
brid
6217
4010
3[0
.5,4
.9]
[5.1
,40.
4]43
213
.652
...
0638
1306
hybr
id64
4316
123
[0.2
,4.9
][5
.3,5
3.3]
234
5.81
4..
.06
4320
54hy
brid
356
6827
982
9[0
.2,5
.0]
[5.0
,74.
9]29
0110
.571
...
0644
3122
hybr
id15
463
8453
7[0
.2,5
.0]
[5.0
,55.
3]14
662.
425
...
0644
6951
hybr
id28
830
256
509
[0.4
,4.8
][5
.1,5
2.9]
1509
14.8
72..
.06
5091
75hy
brid
112
4268
449
[0.6
,5.0
][5
.1,5
3.7]
4431
3.95
4..
.06
5875
51hy
brid
444
3979
[0.2
,3.6
][5
.5,6
0.6]
192
17.4
22..
.06
6141
68hy
brid
143
4099
392
[0.2
,4.8
][5
.0,5
7.7]
2002
8.35
6..
.06
6707
42hy
brid
194
5713
453
0[0
.4,5
.0]
[5.1
,70.
3]14
1112
.789
...
0669
4649
hybr
id12
039
7824
8[0
.3,4
.9]
[5.0
,57.
7]10
2712
.771
...
0675
6386
hybr
id63
952
237
[0.3
,4.8
][5
.1,7
2.6]
1001
8.96
4..
.06
7564
81hy
brid
114
4271
256
[0.2
,5.0
][5
.1,7
4.0]
540
5.76
6..
.06
7615
39hy
brid
212
5615
462
7[0
.2,4
.9]
[5.1
,59.
1]19
7517
.826
...
0677
6331
hybr
id40
551
351
789
[0.2
,5.0
][5
.3,4
8.7]
1697
13.7
89..
.06
9226
90hy
brid
183
4612
847
8[0
.3,4
.9]
[5.0
,49.
4]14
7515
.257
...
0695
1642
hybr
id75
3440
295
[0.2
,4.6
][5
.5,5
0.8]
2838
0.72
1..
.07
1095
98hy
brid
152
3311
629
1[0
.3,4
.8]
[5.1
,54.
7]90
818
.597
...
0711
9530
hybr
id10
678
1948
1[0
.2,5
.0]
[5.0
,15.
2]24
434.
193
...
0712
2746
hybr
id54
747
191
[1.1
,4.9
][5
.1,4
8.8]
735
30.1
54..
.07
2042
37hy
brid
269
5421
453
7[0
.2,4
.9]
[5.0
,63.
4]29
2617
.993
...
0721
1759
hybr
id16
337
125
587
[0.3
,4.9
][5
.1,7
9.4]
736
7.31
8..
.07
3003
87hy
brid
329
6425
485
2[0
.2,4
.9]
[5.2
,50.
5]34
6910
.293
...
0735
0486
hybr
id22
174
58[0
.3,4
.7]
[5.3
,17.
1]13
01.
330
...
0735
2776
hybr
id10
532
6538
2[0
.2,5
.0]
[6.1
,36.
5]17
642.
374
...
0750
2559
hybr
id64
3820
145
[0.5
,4.7
][5
.2,3
1.9]
1383
4.52
2..
.07
5336
94hy
brid
146
559
[0.3
,4.9
][5
.6,4
9.5]
1621
11.2
43..
.07
5532
37hy
brid
4634
1013
2[0
.2,4
.9]
[5.4
,15.
6]21
8414
.713
...
0766
8791
hybr
id23
417
30[0
.2,4
.9]
[5.0
,31.
1]98
20.6
43..
.07
7027
05hy
brid
196
6313
057
5[0
.3,4
.9]
[5.1
,53.
3]87
82.
038
...
0773
2458
hybr
id20
104
26[0
.2,4
.9]
[5.0
,32.
1]35
913
.184
...
0774
8238
hybr
id53
3017
144
[0.4
,4.9
][5
.0,4
9.1]
552
2.29
2..
.07
7568
53hy
brid
61
56
[0.2
,3.1
][5
.0,2
7.0]
9821
.141
...
0777
0282
hybr
id70
5310
195
[0.2
,4.7
][2
8.5,
51.3
]21
361.
004
...
0777
1991
hybr
id12
64
25[0
.8,4
.1]
[5.3
,21.
4]70
2.05
5..
.07
8271
31hy
brid
3917
1917
5[0
.3,4
.7]
[5.0
,39.
4]93
910
.044
...
0783
1302
hybr
id76
2251
184
[0.2
,3.6
][5
.5,4
8.8]
1051
18.7
50•
0784
8288
hybr
id24
762
178
370
[0.2
,4.9
][5
.0,6
6.9]
840
25.2
38•
0795
9867
hybr
id73
2343
303
[0.2
,4.5
][5
.6,3
9.3]
1081
7.71
3..
.07
9779
96hy
brid
118
2784
220
[0.2
,4.9
][5
.1,5
8.2]
1224
11.0
30..
.08
0295
46hy
brid
7938
3835
9[0
.2,4
.7]
[5.7
,27.
4]99
62.
034
...
0805
4146
hybr
id38
1124
80[0
.3,3
.2]
[5.5
,76.
0]18
566
.295
...
0814
9341
hybr
id18
327
149
350
[0.2
,4.9
][5
.1,5
0.5]
1681
27.0
16..
.08
1977
88hy
brid
128
5275
410
[0.3
,4.8
][5
.1,4
7.3]
3441
14.9
98..
.
A125, page 63 of 70
A&A 534, A125 (2011)Ta
ble
3.co
ntin
ued.
KIC
IDC
lass
NNγ
Dor
NδS
ctN
tota
l(F
req
Ran
ge) γ
Dor
(Fre
qR
ange
) δS
ctA
mpl
itud
e hig
hF
req h
igh
Fla
g(d−1
)(d−1
)(p
pm)
(d−1
)08
2644
04hy
brid
9732
5741
4[0
.2,4
.8]
[5.1
,52.
3]53
809.
396
...
0826
4583
hybr
id50
3414
175
[0.3
,4.8
][5
.1,5
4.0]
519
0.96
8..
.08
2646
74hy
brid
5433
1621
5[0
.2,5
.0]
[5.2
,18.
1]40
06.
598
...
0826
4698
hybr
id14
049
8946
5[0
.3,4
.8]
[5.2
,47.
9]18
4813
.801
•08
3974
26hy
brid
4622
2419
7[0
.3,4
.9]
[5.1
,14.
1]12
415.
576
...
0845
4553
hybr
id59
2626
255
[0.2
,5.0
][5
.0,2
2.7]
2014
2.92
0..
.08
4609
93hy
brid
258
7018
663
0[0
.2,5
.0]
[5.0
,56.
6]10
8518
.067
...
0850
7325
hybr
id79
4136
146
[0.2
,4.9
][5
.1,4
9.2]
213
11.6
79..
.08
5160
08hy
brid
126
5271
229
[0.3
,5.0
][5
.0,4
9.1]
886
13.3
76..
.08
5905
53hy
brid
7022
4714
6[0
.3,4
.9]
[5.5
,53.
3]10
0224
.285
...
0873
8244
hybr
id11
639
7118
5[0
.2,5
.0]
[5.0
,49.
6]34
614
.621
...
0891
5335
hybr
id71
2742
162
[0.2
,4.2
][5
.1,3
3.5]
1429
8.82
8..
.08
9406
40hy
brid
232
6416
486
6[0
.3,4
.9]
[5.4
,52.
7]10
783
17.8
39..
.08
9729
66hy
brid
286
4723
764
1[0
.2,5
.0]
[5.1
,50.
5]29
4619
.225
...
0897
5515
hybr
id25
147
61[0
.3,4
.7]
[5.3
,25.
8]29
313
.972
...
0905
2363
hybr
id13
47
16[0
.2,1
.5]
[19.
1,48
.0]
4441
.966
...
0907
2011
hybr
id13
327
101
445
[0.2
,4.9
][5
.3,5
5.9]
6138
6.11
6..
.09
0730
07hy
brid
104
5050
347
[0.2
,5.0
][5
.0,2
9.5]
5031
11.4
71..
.09
2229
42hy
brid
9462
2425
9[0
.2,5
.0]
[5.2
,50.
3]67
12.
162
...
0935
1622
hybr
id48
2117
127
[0.2
,4.8
][5
.2,1
3.4]
1152
6.02
0..
.09
3913
95hy
brid
2824
297
[0.2
,4.5
][5
.3,1
5.4]
465
1.94
9..
.09
4130
57hy
brid
137
3510
127
7[0
.2,4
.9]
[5.1
,51.
8]49
713
.546
...
0947
3000
hybr
id11
64
43[0
.2,5
.0]
[5.6
,17.
4]99
78.
699
...
0950
9296
hybr
id96
4253
389
[0.2
,4.9
][5
.3,5
1.0]
1406
17.6
77..
.09
5326
44hy
brid
6433
2827
3[0
.4,5
.0]
[5.4
,35.
5]15
2020
.487
...
0953
3489
hybr
id17
78
37[1
.5,4
.4]
[6.4
,37.
6]33
34.
008
...
0955
0886
hybr
id10
924
8025
5[0
.4,5
.0]
[5.6
,68.
6]30
6350
.126
...
0960
4762
hybr
id10
34
12[0
.9,3
.7]
[5.2
,24.
3]12
618
.151
...
0965
0390
hybr
id12
256
5731
3[0
.4,4
.9]
[5.1
,51.
7]79
71.
071
...
0965
1065
hybr
id10
720
8434
5[0
.2,4
.8]
[5.5
,47.
6]22
5919
.478
...
0965
5438
hybr
id22
711
43[0
.2,4
.6]
[5.4
,31.
9]38
912
.992
...
0965
5501
hybr
id13
824
110
173
[0.2
,4.4
][5
.0,5
3.7]
530
27.7
23..
.09
6563
48hy
brid
2918
213
7[0
.2,4
.8]
[5.5
,21.
9]80
62.
818
...
0966
4869
hybr
id88
4933
320
[0.2
,5.0
][5
.4,4
1.5]
1389
1.62
2..
.09
7006
79hy
brid
5035
1111
4[0
.2,5
.0]
[5.1
,34.
7]95
0.26
2..
.09
7169
47hy
brid
6319
3930
2[0
.2,4
.8]
[5.4
,16.
8]83
36.
215
...
0976
4965
hybr
id24
810
72[0
.3,5
.0]
[5.1
,34.
6]96
127
.178
...
0977
5385
hybr
id22
137
58[0
.7,4
.0]
[5.1
,25.
9]18
91.
788
...
0977
5454
hybr
id18
102
73[0
.2,4
.6]
[14.
7,14
.9]
316
4.16
1..
.09
7904
79hy
brid
95
325
[1.4
,4.4
][5
.5,2
0.0]
246
1.61
8..
.09
8130
78hy
brid
7329
3735
2[0
.3,3
.9]
[7.4
,39.
5]38
7117
.588
...
0997
0568
hybr
id15
064
8339
5[0
.2,5
.0]
[5.0
,55.
5]94
53.
408
...
1001
4548
hybr
id16
242
114
314
[0.2
,5.0
][5
.0,5
7.8]
775
1.52
8..
.
A125, page 64 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
3.co
ntin
ued.
KIC
IDC
lass
NNγ
Dor
NδS
ctN
tota
l(F
req
Ran
ge) γ
Dor
(Fre
qR
ange
) δS
ctA
mpl
itud
e hig
hF
req h
igh
Fla
g(d−1
)(d−1
)(p
pm)
(d−1
)10
0357
72hy
brid
125
3883
427
[0.2
,4.9
][5
.4,6
5.8]
1947
26.8
91..
.10
0652
44hy
brid
115
4357
448
[0.2
,5.0
][5
.0,4
9.1]
1009
711
.930
...
1013
0777
hybr
id36
155
305
908
[0.4
,4.9
][5
.1,6
3.7]
2101
33.8
21..
.10
1645
69hy
brid
5325
2414
5[0
.2,4
.9]
[5.0
,53.
5]46
615
.396
...
1020
8345
hybr
id74
4127
212
[0.3
,4.9
][5
.1,2
0.5]
861
3.45
2..
.10
2647
28hy
brid
101
3761
436
[0.2
,4.6
][5
.4,5
3.5]
875
3.37
9..
.10
3612
29hy
brid
2520
513
7[0
.5,4
.9]
[5.6
,29.
3]81
32.
653
...
1047
1914
hybr
id30
846
254
534
[0.2
,4.9
][5
.2,5
7.0]
2156
15.0
70..
.10
5379
07hy
brid
110
2283
510
[0.2
,4.5
][5
.1,4
5.3]
4741
11.5
55..
.10
6474
93hy
brid
7828
4737
8[0
.2,4
.6]
[5.1
,56.
1]55
3617
.101
...
1064
7611
hybr
id69
2242
317
[0.5
,4.6
][5
.1,5
1.2]
4527
15.7
23..
.10
6649
75hy
brid
95
321
[1.3
,4.4
][6
.1,1
9.9]
383
2.57
5..
.10
6757
62hy
brid
6823
4030
0[0
.3,4
.7]
[5.0
,50.
4]31
1815
.914
...
1068
5653
hybr
id47
2421
149
[0.2
,5.0
][5
.4,4
3.9]
565
19.4
11..
.10
7831
50hy
brid
7763
661
3[0
.3,5
.0]
[5.1
,17.
0]38
961.
560
...
1097
5247
hybr
id8
53
8[0
.3,4
.8]
[7.1
,19.
5]86
13.9
43..
.11
1803
61hy
brid
3611
2572
[0.2
,5.0
][5
.0,6
0.0]
334
3.75
2..
.11
1930
46hy
brid
112
6248
303
[0.2
,4.9
][5
.0,5
4.7]
704
1.27
5..
.11
1979
34hy
brid
213
8112
139
7[0
.3,5
.0]
[5.1
,60.
4]72
01.
939
...
1128
5767
hybr
id13
340
8641
6[0
.2,5
.0]
[5.0
,59.
7]64
9621
.061
...
1128
8686
hybr
id62
2233
316
[0.2
,4.6
][5
.3,4
1.1]
4053
18.4
87..
.11
3093
35hy
brid
146
2212
227
2[0
.3,4
.8]
[5.0
,59.
7]11
9123
.435
...
1144
5913
hybr
id16
718
144
328
[0.2
,4.2
][7
.2,5
0.4]
1654
31.5
58..
.11
5083
97hy
brid
9242
4814
5[0
.2,4
.9]
[5.1
,48.
2]34
011
.367
...
1157
2666
hybr
id44
1722
164
[0.2
,4.9
][5
.0,4
8.9]
976
18.2
79..
.11
6024
49hy
brid
8436
4031
0[0
.5,4
.9]
[6.4
,49.
7]13
9210
.579
...
1160
7193
hybr
id10
273
1439
6[0
.2,4
.9]
[5.0
,16.
5]71
61.
817
...
1170
0604
hybr
id20
144
66[0
.3,5
.0]
[5.0
,27.
0]51
527
.013
...
1171
4150
hybr
id13
91
28[0
.3,4
.1]
[6.0
,11.
0]30
70.
756
...
1171
8839
hybr
id16
749
115
235
[0.3
,4.9
][5
.1,4
2.4]
696
16.4
41..
.11
8226
66hy
brid
5131
2073
[0.4
,5.0
][5
.0,3
5.7]
298
2.05
0..
.11
8249
64hy
brid
2111
538
[0.4
,4.5
][5
.0,3
4.6]
125
2.16
0..
.12
1176
89hy
brid
2316
574
[0.3
,4.6
][5
.1,2
5.0]
1229
3.21
8..
.12
1220
75hy
brid
8054
2021
5[0
.3,5
.0]
[5.0
,31.
9]12
601.
116
•12
2168
17hy
brid
143
5584
609
[0.2
,5.0
][5
.2,5
2.6]
2200
78.
121
...
γD
orst
ars
0143
2149
γD
or8
80
56[0
.6,3
.5]
...
322
3.45
1..
.01
5711
52γ
Dor
5757
018
9[0
.3,5
.8]
...
1061
0.39
4..
.02
0209
66γ
Dor
1313
031
[0.3
,3.2
]..
.79
81.
735
...
0216
6218
γD
or17
170
42[0
.3,3
.2]
...
149
1.79
8..
.02
3001
65γ
Dor
4747
021
9[0
.5,5
.5]
...
2500
1.67
9..
.02
5582
73γ
Dor
2525
065
[0.3
,3.3
]..
.33
42.
015
...
0256
8519
γD
or6
60
21[0
.2,4
.1]
...
150
0.84
8..
.
A125, page 65 of 70
A&A 534, A125 (2011)Ta
ble
3.co
ntin
ued.
KIC
IDC
lass
NNγ
Dor
NδS
ctN
tota
l(F
req
Ran
ge) γ
Dor
(Fre
qR
ange
) δS
ctA
mpl
itud
e hig
hF
req h
igh
Fla
g(d−1
)(d−1
)(p
pm)
(d−1
)02
5751
61γ
Dor
88
038
[0.6
,2.5
]..
.32
92.
245
...
0272
0582
γD
or34
340
70[0
.3,5
.6]
...
467
0.55
1..
.02
8357
95γ
Dor
88
064
[0.4
,2.4
]..
.86
50.
359
...
0321
5800
γD
or16
160
51[0
.2,3
.7]
...
1696
1.50
6..
.03
2186
37γ
Dor
8383
023
7[0
.2,6
.0]
...
4526
3.84
9..
.03
2223
64γ
Dor
2323
093
[0.4
,3.7
]..
.49
62.
482
...
0332
7681
γD
or14
140
36[0
.3,1
.5]
...
301
1.01
1..
.03
3311
47γ
Dor
2424
011
5[0
.3,5
.8]
...
4684
1.42
7..
.03
4244
93γ
Dor
5454
020
4[0
.2,5
.9]
...
7606
2.70
9..
.03
4496
25γ
Dor
1818
077
[0.3
,3.3
]..
.10
350.
942
...
0353
9153
γD
or10
910
90
373
[0.2
,6.0
]..
.45
122.
035
...
0365
5608
γD
or9
90
14[0
.5,2
.6]
...
770.
636
...
0366
3141
γD
or4
40
34[2
.3,5
.0]
...
135
2.78
8..
.03
7587
17γ
Dor
1313
063
[0.6
,3.2
]..
.25
90.
871
...
0386
8032
γD
or8
80
39[0
.3,1
.7]
...
249
0.39
8..
.03
9663
57γ
Dor
8787
034
9[0
.2,5
.3]
...
3706
1.59
5..
.04
0694
77γ
Dor
7777
025
0[0
.2,5
.7]
...
3305
1.40
8..
.04
1643
63γ
Dor
7373
030
0[0
.2,5
.9]
...
8312
1.38
1•
0467
7684
γD
or37
370
132
[0.3
,5.6
]..
.89
04.
496
...
0475
8316
γD
or12
612
60
416
[0.2
,5.9
]..
.44
890.
991
...
0502
4455
γD
or18
180
102
[0.5
,4.4
]..
.15
561.
341
•05
1057
54γ
Dor
156
156
054
4[0
.2,5
.8]
...
1051
11.
687
...
0511
3797
γD
or26
260
114
[0.2
,5.1
]..
.43
12.
836
...
0516
4767
γD
or11
110
32[0
.2,2
.1]
...
109
0.95
8..
.05
1807
96γ
Dor
2525
088
[0.3
,4.3
]..
.50
31.
890
...
0529
4571
γD
or66
660
176
[0.4
,4.9
]..
.11
381.
494
...
0537
1747
γD
or62
620
216
[0.2
,5.9
]..
.13
791.
128
...
0563
0362
γD
or69
690
210
[0.2
,5.8
]..
.68
214.
856
...
0572
4048
γD
or25
250
62[0
.2,4
.3]
...
269
2.13
1..
.05
7724
11γ
Dor
1818
027
[0.3
,3.5
]..
.83
0.84
3..
.05
8803
60γ
Dor
3636
013
9[0
.2,5
.8]
...
787
1.60
1..
.05
9542
64γ
Dor
2727
066
[1.2
,4.0
]..
.14
421.
840
...
0630
1745
γD
or17
170
74[0
.3,5
.8]
...
1023
0.39
3..
.06
4620
33γ
Dor
4646
013
7[0
.2,4
.5]
...
740
1.43
5..
.06
5005
78γ
Dor
5050
012
6[0
.2,6
.0]
...
782
1.50
0..
.06
5198
69γ
Dor
142
142
051
3[0
.2,5
.8]
...
5215
1.35
3..
.06
9234
24γ
Dor
5757
014
4[0
.3,5
.7]
...
1948
2.73
5..
.07
0071
03γ
Dor
8080
026
7[0
.2,5
.9]
...
1780
1.54
0..
.07
1066
48γ
Dor
3838
010
3[0
.2,6
.0]
...
1335
2.35
5..
.07
2156
07γ
Dor
2121
033
[0.3
,4.9
]..
.29
12.
231
...
0722
0356
γD
or23
230
42[0
.4,4
.4]
...
741.
261
...
0730
4385
γD
or14
714
70
774
[0.2
,5.4
]..
.23
271
1.26
9..
.07
4362
66γ
Dor
4545
018
2[0
.2,4
.4]
...
1703
1.71
4..
.07
6941
91γ
Dor
1616
017
[0.5
,5.3
]..
.92
2.65
8..
.07
7427
39γ
Dor
5757
028
2[0
.2,5
.9]
...
2292
2.05
7..
.07
7675
65γ
Dor
2626
012
7[0
.4,4
.9]
...
532
1.99
4..
.
A125, page 66 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.
Tabl
e3.
cont
inue
d.
KIC
IDC
lass
NNγ
Dor
NδS
ctN
tota
l(F
req
Ran
ge) γ
Dor
(Fre
qR
ange
) δS
ctA
mpl
itud
e hig
hF
req h
igh
Fla
g(d−1
)(d−1
)(p
pm)
(d−1
)07
7983
39γ
Dor
80
04
[0.2
,4.9
]..
.38
0.45
0..
.07
8905
26γ
Dor
2020
075
[0.2
,5.4
]..
.39
11.
353
...
0790
8633
γD
or11
110
18[0
.2,3
.0]
...
121
2.79
5..
.08
1045
89γ
Dor
1818
039
[0.2
,2.1
]..
.12
90.
538
...
0812
3127
γD
or14
114
10
320
[0.2
,6.0
]..
.19
910.
774
...
0814
4674
γD
or18
180
39[0
.2,5
.2]
...
520.
494
...
0819
7761
γD
or56
560
274
[0.2
,5.3
]..
.64
071.
097
...
0822
2685
γD
or35
350
104
[0.2
,4.0
]..
.43
302.
010
...
0823
0025
γD
or50
500
232
[0.2
,5.9
]..
.87
83.
659
...
0826
4061
γD
or70
700
321
[0.2
,5.9
]..
.53
501.
400
...
0826
4075
γD
or34
340
157
[0.2
,5.9
]..
.22
381.
201
...
0826
4274
γD
or34
340
135
[0.2
,5.3
]..
.21
021.
483
•08
2645
88γ
Dor
4343
018
9[0
.2,5
.9]
...
5540
5.00
2..
.08
2646
17γ
Dor
126
126
046
3[0
.3,5
.8]
...
2975
31.
242
•08
3300
56γ
Dor
3232
010
4[0
.2,5
.5]
...
974
2.53
7•
0835
5130
γD
or16
516
50
636
[0.2
,5.8
]..
.10
314
1.37
5..
.08
4897
12γ
Dor
4646
012
8[0
.2,6
.0]
...
257
0.55
5..
.08
6514
52γ
Dor
9191
035
6[0
.2,5
.8]
...
1028
52.
434
...
0876
6619
γD
or39
390
158
[0.3
,5.6
]..
.11
222.
047
•08
8384
57γ
Dor
3939
010
7[0
.2,5
.9]
...
743
2.25
6..
.08
8693
02γ
Dor
114
114
077
2[0
.2,4
.0]
...
5990
0.64
7..
.08
8713
04γ
Dor
136
136
054
6[0
.2,5
.6]
...
3742
0.97
0..
.09
0201
57γ
Dor
2929
011
8[0
.3,2
.8]
...
1323
1.23
4..
.09
1178
75γ
Dor
55
08
[0.6
,1.4
]..
.13
30.
667
...
0914
7229
γD
or98
980
311
[0.2
,5.4
]..
.41
721.
984
...
0949
0042
γD
or10
710
70
280
[0.2
,5.8
]..
.67
51.
621
...
0949
0067
γD
or68
680
150
[0.2
,5.9
]..
.68
62.
240
...
0959
4100
γD
or33
330
181
[0.2
,5.9
]..
.19
871.
052
...
0965
4789
γD
or75
750
313
[0.2
,5.7
]..
.59
130.
992
...
0965
5151
γD
or32
320
197
[0.9
,6.0
]..
.23
281.
418
•09
6558
00γ
Dor
6464
026
8[0
.2,4
.1]
...
4462
1.94
4..
.09
7161
07γ
Dor
3030
016
1[0
.7,6
.0]
...
1755
2.15
2•
0990
9300
γD
or94
940
372
[0.2
,5.8
]..
.70
731.
496
...
1006
9934
γD
or12
512
50
333
[0.2
,6.0
]..
.46
691.
082
...
1007
3601
γD
or21
210
46[0
.2,2
.2]
...
901.
220
...
1009
6499
γD
or18
180
83[0
.2,6
.0]
...
484
2.66
8..
.10
2813
60γ
Dor
2323
011
0[0
.8,5
.6]
...
490
1.96
1..
.10
3854
59γ
Dor
9494
042
8[0
.2,5
.8]
...
1142
62.
596
...
1058
6837
γD
or48
480
189
[0.2
,5.9
]..
.13
171.
569
...
1065
2134
γD
or78
780
546
[0.2
,3.5
]..
.47
570.
766
...
1119
9412
γD
or12
120
53[0
.4,5
.7]
...
2856
0.68
5..
.11
4478
83γ
Dor
6161
020
9[0
.2,3
.0]
...
1871
1.36
7..
.11
6122
74γ
Dor
2929
010
7[0
.2,5
.4]
...
2638
2.54
0..
.11
8748
98γ
Dor
1717
010
0[0
.2,5
.2]
...
1971
0.98
9..
.12
0188
34γ
Dor
103
103
030
9[0
.3,5
.7]
...
2834
1.76
2..
.12
0584
28γ
Dor
6868
026
1[0
.2,5
.9]
...
2812
1.59
8..
.12
1021
87γ
Dor
6969
024
6[0
.2,6
.0]
...
4821
0.92
9..
.
A125, page 67 of 70
A&A 534, A125 (2011)Ta
ble
4.C
lass
ifica
tion
ofth
est
ars
that
dono
tbel
ong
toth
eδ
Sct
,γD
oror
hybr
idgr
oups
.
KIC
IDC
lass
Fla
gK
ICID
Cla
ssF
lag
KIC
IDC
lass
Fla
gS
tars
wit
hno
clea
rpe
riod
icsi
gnal
inth
eδ
Sct
andγ
Dor
regi
ons
0216
3434
...
•09
3862
59..
...
.10
9201
82so
lar-
like
...
0231
1130
...
•09
4587
50..
.•
1092
0273
sola
r-li
ke..
.02
5782
51..
...
.09
5148
79..
...
.11
0679
72so
lar-
like
...
0297
0244
...
...
0952
0434
sola
r-li
ke..
.11
0694
35so
lar-
like
...
0299
7802
...
...
0959
3997
...
...
1112
2763
sola
r-li
ke..
.03
1114
51..
...
.09
7036
01so
lar-
like
...
1112
8041
...
...
0311
9825
...
...
0976
4712
sola
r-li
ke..
.11
1281
26so
lar-
like
...
0322
0783
...
...
0999
1621
sola
r-li
ke..
.11
1292
89so
lar-
like
...
0342
7365
...
...
0999
1766
sola
r-li
ke..
.11
1827
16so
lar-
like
...
0373
3735
...
...
0999
4789
sola
r-li
ke..
.11
2305
18so
lar-
like
...
0375
9814
...
...
1005
6217
sola
r-li
ke..
.11
2329
22so
lar-
like
...
0376
0826
...
...
1006
2593
...
...
1123
3189
sola
r-li
ke..
.04
5884
87..
...
.10
0903
45..
...
.11
2348
88so
lar-
like
...
0485
0899
...
...
1014
0665
sola
r-li
ke..
.11
2357
21so
lar-
like
...
0502
4150
sola
r-li
ke•
1020
8303
sola
r-li
ke..
.11
2362
53so
lar-
like
...
0502
4454
sola
r-li
ke•
1025
4547
sola
r-li
ke..
.11
2532
26..
...
.05
0244
56..
.•
1026
6959
sola
r-li
ke•
1129
0197
sola
r-li
ke..
.05
1129
32so
lar-
like
•10
2732
46so
lar-
like
...
1139
3580
sola
r-li
ke..
.05
1994
64so
lar-
like
•10
2739
60so
lar-
like
...
1139
4216
sola
r-li
ke..
.05
2010
88..
.•
1033
9342
sola
r-li
ke..
.11
3950
18so
lar-
like
...
0598
0337
...
...
1034
0511
sola
r-li
ke..
.11
3950
28so
lar-
like
...
0733
8125
...
...
1034
1072
sola
r-li
ke..
.11
4461
43so
lar-
like
...
0766
2076
...
...
1038
3933
sola
r-li
ke..
.11
4461
81so
lar-
like
...
0766
9848
sola
r-li
ke..
.10
4505
50so
lar-
like
...
1144
8266
sola
r-li
ke..
.08
1439
03so
lar-
like
...
1045
0675
sola
r-li
ke..
.11
4499
31..
...
.08
1591
35..
...
.10
4512
50so
lar-
like
•11
4540
08..
...
.08
2184
19so
lar-
like
...
1045
3475
...
...
1149
9354
sola
r-li
ke..
.08
2239
87so
lar-
like
...
1046
7969
sola
r-li
ke..
.11
5020
75so
lar-
like
...
0829
3302
...
...
1052
6137
...
...
1150
9728
...
...
0832
3104
...
...
1052
6615
sola
r-li
ke•
1154
9609
sola
r-li
ke..
.08
3558
37..
...
.10
5335
06so
lar-
like
...
1155
1622
sola
r-li
ke•
0846
0025
...
•10
5346
29so
lar-
like
...
1165
1083
sola
r-li
ke..
.08
4825
40..
...
.10
6478
60so
lar-
like
...
1165
1147
sola
r-li
ke..
.08
4880
65..
...
.10
6638
92so
lar-
like
...
1165
3958
sola
r-li
ke..
.09
0739
85so
lar-
like
...
1070
9716
sola
r-li
ke..
.11
6542
10so
lar-
like
...
0920
4672
...
...
1072
3718
sola
r-li
ke..
.11
6578
40so
lar-
like
•09
2643
99..
...
.10
7306
18so
lar-
like
...
1170
6449
sola
r-li
ke•
0926
4462
sola
r-li
ke..
.10
7775
41so
lar-
like
•11
7073
41so
lar-
like
...
0927
2082
...
...
1077
8640
sola
r-li
ke•
1191
0256
...
...
0927
4000
...
...
1086
1649
sola
r-li
ke..
.11
9106
42..
...
.09
3362
19..
...
...
...
...
...
...
...
.B
inar
ies
0129
4756
bina
ry+δ
Sct
...
0667
8614
EB+δ
Sct
...
0976
0531
bina
ry..
.
A125, page 68 of 70
K. Uytterhoeven et al.: The Kepler characterization of the variability among A- and F-type stars. I.Ta
ble
4.co
ntin
ued.
KIC
IDC
lass
Fla
gK
ICID
Cla
ssF
lag
KIC
IDC
lass
Fla
g02
1622
83E
B+δ
Sct
...
0738
5478
EB+γ
Dor
...
0985
1142
EB+γ
Dor
...
0255
7430
EB+γ
Dor
...
0759
6250
EB+γ
Dor
...
0991
3481
EB+γ
Dor
...
0258
4908
EB
...
0804
3961
EB+δ
Sct
...
0994
4730
bina
ry..
.02
7185
96bi
nary
...
0814
5477
EB
...
1011
9517
EB
...
0323
0227
EB+γ
Dor
...
0822
3568
bina
ry..
.10
2063
40E
B+γ
Dor
...
0415
0611
EB+
hybr
id..
.08
3300
92E
B+δ
Sct
...
1027
4244
EB+γ
Dor
...
0457
0326
EB+δ
Sct
...
0847
9107
EB
•10
9716
74E
B..
.05
0883
08E
B+γ
Dor
...
0854
5456
EB
...
1108
2830
bina
ry..
.05
1972
56E
B+δ
Sct
...
0920
4718
bina
ry+δ
Sct
...
1118
0361
EB
...
0529
6877
EB
...
0921
6367
EB+γ
Dor
...
1134
2032
bina
ry..
.05
5138
61E
B..
.09
4515
98E
B..
.11
4479
53E
B..
.05
9881
40bi
nary+δ
Sct
...
0963
0640
bina
ry+δ
Sct
...
1197
3705
bina
ry+
SP
B+δ
Sct
...
Ste
llar
activ
ity/
rota
tion
alm
odul
atio
n01
5730
64ro
tati
on/a
ctiv
ity
...
0828
3796
rota
tion/a
ctiv
ity
...
1014
0513
rota
tion/a
ctiv
ity
...
0199
5489
rota
tion/a
ctiv
ity
...
0833
0463
rota
tion/a
ctiv
ity
•10
3382
79ro
tati
on/a
ctiv
ity
...
0242
3932
rota
tion/a
ctiv
ity
...
0870
3413
rota
tion/a
ctiv
ity
...
1039
4332
rota
tion/a
ctiv
ity
...
0256
9639
rota
tion/a
ctiv
ity
...
0874
2449
rota
tion/a
ctiv
ity
•10
6487
28ro
tati
on/a
ctiv
ity
...
0258
3658
rota
tion/a
ctiv
ity
...
0874
8251
rota
tion/a
ctiv
ity
...
1079
7849
rota
tion/a
ctiv
ity
...
0334
8390
rota
tion/a
ctiv
ity
...
0907
7192
rota
tion/a
ctiv
ity
...
1101
7401
rota
tion/a
ctiv
ity
•03
5285
78ro
tati
on/a
ctiv
ity
...
0926
8087
rota
tion/a
ctiv
ity
...
1102
0521
rota
tion/a
ctiv
ity
...
0364
3717
rota
tion/a
ctiv
ity
...
0958
2720
rota
tion/a
ctiv
ity
...
1102
7270
rota
tion/a
ctiv
ity
...
0407
5519
rota
tion/a
ctiv
ity
...
0963
2537
rota
tion/a
ctiv
ity
...
1118
3399
rota
tion/a
ctiv
ity
...
0416
0876
rota
tion/a
ctiv
ity
...
0964
0204
rota
tion/a
ctiv
ity
...
1124
0653
rota
tion/a
ctiv
ity
...
0485
7678
rota
tion/a
ctiv
ity
...
0964
3982
rota
tion/a
ctiv
ity
...
1144
5774
rota
tion/a
ctiv
ity
...
0520
0084
rota
tion/a
ctiv
ity
•09
6554
87ro
tati
on/a
ctiv
ity
•11
4947
65ro
tati
on/a
ctiv
ity
...
0543
6432
rota
tion/a
ctiv
ity
...
0969
6853
rota
tion/a
ctiv
ity
...
1149
8538
rota
tion/a
ctiv
ity
...
0547
6495
rota
tion/a
ctiv
ity
...
0971
6350
rota
tion/a
ctiv
ity
...
1149
9453
rota
tion/a
ctiv
ity
...
0627
9848
rota
tion/a
ctiv
ity
...
0977
7532
rota
tion/a
ctiv
ity
...
1151
5690
rota
tion/a
ctiv
ity
...
0644
0930
rota
tion/a
ctiv
ity
...
0988
1909
rota
tion/a
ctiv
ity
...
1162
2328
rota
tion/a
ctiv
ity
...
0644
8112
rota
tion/a
ctiv
ity
...
0994
4208
rota
tion/a
ctiv
ity
...
1170
8170
rota
tion/a
ctiv
ity
...
0798
5370
rota
tion/a
ctiv
ity
...
1000
4510
rota
tion/a
ctiv
ity
...
1206
2443
rota
tion/a
ctiv
ity
...
0821
1500
rota
tion/a
ctiv
ity
...
1006
4111
rota
tion/a
ctiv
ity
...
1221
7281
rota
tion/a
ctiv
ity
...
Bty
pest
ars
0521
7733
Bst
arS
PB
...
1003
0943
Bst
arca
ndid
ateβ
Cep
...
1065
8302
Bst
arS
PB
...
0858
3770
Bst
ar..
.10
5361
47B
star
SP
B..
.10
7975
26B
star
SP
B..
.08
7148
86B
star
SP
B..
...
...
...
...
...
...
.C
andi
date
red
gian
ts02
3064
69re
dgi
ant
...
0299
5525
red
gian
t..
.08
7468
34re
dgi
ant
•02
3067
16re
dgi
ant
...
0324
8627
red
gian
t..
.09
3279
93re
dgi
ant
...
0231
0479
red
gian
t..
.03
3540
22re
dgi
ant
...
0952
0864
red
gian
t..
.02
4430
55re
dgi
ant
...
0335
5066
red
gian
t..
.09
8858
82re
dgi
ant
...
0244
4598
red
gian
t..
.03
4271
44re
dgi
ant
...
0999
5464
red
gian
t..
.02
5562
97re
dgi
ant
...
0344
9373
red
gian
t..
.10
0061
58re
dgi
ant
...
0255
6387
red
gian
t..
.03
4580
97re
dgi
ant
...
1005
7129
red
gian
t..
.
A125, page 69 of 70
A&A 534, A125 (2011)
Tabl
e4.
cont
inue
d.
KIC
IDC
lass
Fla
gK
ICID
Cla
ssF
lag
KIC
IDC
lass
Fla
g02
5571
15re
dgi
ant
...
0352
5951
red
gian
t..
.10
0688
92re
dgi
ant
...
0258
4202
red
gian
t..
.03
5460
61re
dgi
ant
...
1013
4600
red
gian
t..
.02
8347
96re
dgi
ant
...
0362
9080
red
gian
t..
.10
3890
37re
dgi
ant
...
0285
5687
red
gian
t..
.03
6336
93re
dgi
ant
...
1090
2738
red
gian
t..
.02
8601
23re
dgi
ant
...
0383
6911
red
gian
t..
.11
3400
63re
dgi
ant
...
0296
9151
red
gian
t..
.04
1443
00re
dgi
ant
...
1170
6564
red
gian
t..
.02
9724
01re
dgi
ant
...
0502
4750
red
gian
t..
.11
7531
69re
dgi
ant
•02
9897
46re
dgi
ant
...
0511
2786
red
gian
t..
...
...
...
.C
ephe
id07
5480
61C
ephe
id..
...
...
...
...
...
...
.C
onta
min
ated
star
s03
4574
34co
ntam
inat
ed•
0493
7257
cont
amin
ated
•09
6554
33co
ntam
inat
ed•
0404
8488
cont
amin
ated
•05
7248
10co
ntam
inat
ed•
...
...
...
A125, page 70 of 70