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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 overviewK. 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

(A!liations 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 !Doradus (!Dor), " Scuti ("Sct), 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 di!erent frequency analysis methods. We construct two newobservables, “energy” and “e!ciency”, related to the driving energy of the pulsation mode and the convective e"ciency of the outer convectivezone, respectively.Results. We propose three main groups to describe the observed variety in pulsating A-F type stars: !Dor, "Sct, 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 di!erent 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 !Dorand "Sct range, also between 5 and 10 d"1, which is a challenge for the current models. We find indications for the existence of "Sct and !Dorstars beyond the edges of the current observational instability strips. The hybrid stars occupy the entire region within the "Sct and !Dor instabilitystrips and beyond. Non-variable stars seem to exist within the instability strips. The location of !Dor and "Sct classes in the (Te! , log g)-diagramhas been extended. We investigate two newly constructed variables, “e!ciency” and “energy”, as a means to explore the relation between !Dorand " Sct stars.Conclusions. Our results suggest a revision of the current observational instability strips of "Sct and !Dor stars and imply an investigation ofpulsation mechanisms to supplement the # mechanism and convective blocking e!ect 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: " 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 !Doradus (!Dor) and " Scuti("Sct) pulsators. The !Dor 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 !Dor peri-ods are between 8 h and 3 d. From the ground, about 70 bona fideand 88 candidate !Dor 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 "Sct 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 #-mechanism (see reviews by Breger 2000; Handler 2009a).

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Several hundreds of " 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 bydi!erent 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 di!erentcase-studies. So far, a systematic study of a su"ciently 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 !Dor-"Sct 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 "Sct stars HD 50844 (Poretti et al. 2009) andHD 174936 (García Hernández et al. 2009), and the !Dor 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 " Sct and !Dor 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 !Dor and " 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 o!ers 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 di!erent 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 !Dor, " 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 !Doror " 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 e!ectivetemperature Te! and gravity log g suggested that they lie in orclose to the instability strips of !Dor and "Sct 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 "Sct or !Dor 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 e!ect towardscooler stars. We also included stars initially assigned to otherpulsation types that showed periodicities typical for "Sct and/or!Dor stars. We are aware that many more " Sct and !Dor 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 (#T ) expressed in d, the longesttime gap in the Kepler light curves ("T ) 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 Ski! (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 di!erent 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 Pr!a 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 "Sct star by Henry et al. (2001). Our samplealso includes a candidate %2 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, Te! , metallicity [M/H], and projected rotationalvelocity v sin i. We compiled an overview of all Te! , log g, andv sin i values available for the sample stars in Table 2 in theon-line version of the paper. The di!erent sources include lit-erature and KIC, along with values derived from new ground-based data. A description of the di!erent sources is given be-low. The columns of Table 2 are (1) KIC identifier (KIC ID);(2) Te! value from KIC; (3)"(5) Te! values taken from theliterature or derived from new ground-based data (Literature);(6) adopted Te! 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 (Te! , log g)-diagram. The cross at the lefttop corner represents the typical error bars on the values: 290 K for Te!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 Te! 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 Te!(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 Te! and log g, respectively,is available. Figure 1 shows the sample of 750 stars in the(Te!, 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 di!erence was290 K for Te! 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 Te!, log g, and v sin i.Also, photometric indices by Hauck & Mermilliod (1998) wereused to estimate values of Te! and log g. We took care not toinclude Te! values that are derived from the spectral type ratherthan directly from data. The literature values of Te! and log g canbe found in Cols. 3"5 and 8, 9 of Table 2, respectively (“lit”).We note that the given errors on Te! 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 Te! 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 Te! value is available, which aregenerally faint stars (Kp > 11 mag), are not considered in anyanalysis related to temperature, unless values of Te! 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 Te! 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 " & 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 Te! 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 e"cient spectral synthesis based on a least-squares opti-misation algorithm. The resulting values of Te!, 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 Te!, 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 di!erent 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 Te! , log g and v sin i are presented in Table 2, underlabel “g”. Errors are determined from '2 statistics and representa 1-( 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 Te!(top left), log g (top right), Kepler magnitude Kp (bottom left),and total length of the Kepler light curve #T , expressed in d(bottom right). For the analysis we used Te! and log g valuesgiven in boldface in Table 2. Note that seven stars in our sampleare hotter than Te! = 9000 K, and fall o! the diagram.

The following typical global parameters have been observedfor "Sct and !Dor stars (e.g. Rodríguez & Breger 2001; Handler& Shobbrook 2002): log g = 3.2"4.3 and Te! = 6300"8600 Kfor " Sct stars, and log g = 3.9"4.3 and Te! = 6900"7500 K for!Dor stars. While !Dor stars are generally MS stars, severalmore evolved "Sct stars have been observed.

The distributions in Fig. 2 show that about 70% of thetotal sample does indeed have Te! 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 di"cult to monitor spectroscopically from

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Fig. 2. Distribution in Te! (top left), log g (top right), Kepler magni-tude Kp (bottom left), and total time span #T 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 Te! 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 " Sct and!Dor 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 su!er 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 e!ectsare 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 !Dor and"Sct stars are introduced by the correction, we also correcteda subsample of stars by a di!erent procedure that takes threetypes of e!ects 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 di!erent 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/#T d"1, with #T 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 di!erent 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 di!erent methods were consistent.

6. Classification

6.1. "Sct, !Dor, 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 " Sct, !Dor,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 the2 As obvious combination frequencies and harmonics we consid-ered n fi or k fi ± l f j, with fi and f j di!erent 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 e!ect were omitted from classification. Weused information on Te! (Table 2) to distinguish between "Sctand !Dor stars versus &Cep 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 e!ects(see Sect. 5.1), and the separation of the di!erent 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 "Sct stars,pure !Dor stars, "Sct/!Dor hybrids and !Dor/"Sct hybrids,using the fact that frequencies are only detected in the "Sct(i.e. >5 d"1, or >58 µHz) or !Dor (i.e. <5 d"1 or <58 µHz)domain, or in both domains with dominant frequencies in ei-ther the "Sct star or !Dor star region, respectively. Among the750 sample stars we see di!erent 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 !Dor ("Sct) domain and low amplitude frequenciesin the "Sct (!Dor) domain. The light curves show diversity aswell. Balona et al. (2011d) already commented on the di!erentshapes of light curves of pure !Dor stars.

In this work, we focus on stars that show at least threeindependent frequencies. We classified the stars in threegroups: "Sct stars, !Dor stars, and hybrid stars. Because theunderlying physics that causes the di!erent types of hybridbehaviour is currently not clear, all types of hybridity (both"Sct/!Dor hybrids and !Dor/"Sct 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 " Sct (i.e. >5 d"1 or >58 µHz)and !Dor domain (i.e. <5 d"1 or <58 µHz);

– the amplitudes in the two domains are either comparable,or the amplitudes do not di!er 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” "Sct stars that show a prominent long-term variability signal caused by rotation. We also tried to takecare of more evolved "Sct stars that are expected to pulsate withfrequencies lower than 5 d"1. Stars that exhibited only or mainlyfrequencies in the "Sct domain (i.e. >5 d"1) and did not sat-isfy all of the above given criteria were assigned to the pure"Sct group. Likewise, the group of pure !Dor 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 !Dor 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 !Dor stars, but are aware that nonethe-less, and most likely, our selection is contaminated with a fewnon-bona fide !Dor 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 !Dor 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 ("Sct stars) or 5 d (!Dor 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 "Sctand !Dor 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 "Sct 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 "Sct 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 for!Dor-like frequencies. Because there are no other longer-termperiodicities, there is no evidence for the possible hybrid statusof this star.

The light curves of !Dor 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 "Sct and !Dor regimes. The stars KIC 3119604 andKIC 2853280 (panels a and b, respectively) are clearly dom-inated by "Sct frequencies, while the !Dor 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 the!Dor 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 by!Dor 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 !Dor and " Sct regime (N!Dor and N"Sct, 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 "Sct 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 " Sct and !Dor regime. Note the di!erent 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 !Dor and"Sct regimes ((Freq Range)!Dor and (Freq Range)"Sct, 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 !Dor or " 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 !Dor star onlyLC data are available. This may create a selection e!ect, be-cause short-term " Sct periods are more di"cult 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 !Dor stars because the typical !Dor 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 "Sct and &Cep stars, and between !Dorand SPB stars. In general, there is good agreement (>87%, clas-sified in terms of " Sct or &Cep stars) with the classification byDebosscher et al. (2011) for stars that we classified as " Sct stars.The !Dor 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 !Dor stars. Note the di!erent 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-recognized!Dor 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 " Sct, !Dor, &Cep, 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 " Sct, !Dor, 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 "Sct and !Dor 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 Te! 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 !Dor 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 !Dor and "Sct 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 &Cep 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 "Sct frequency-dominated stars, and the two bottom panels d)"e) are !Dor 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 "Sctand SPB component (see also Balona et al. 2011b). For threestars reported in the literature as EBs (Pr!a 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 !Dor 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 possible!Dor 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 di!erent 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 !Dor, "Sct or hybrid stars: 27% are classified as"Sct stars (206 stars), 23% as hybrid stars (171 stars; of which115 stars are "Sct-dominated and 56 stars are !Dor-dominated),and 13% as !Dor 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 candidate!Dor-"Sct 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 !Dor and "Sct 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 " Sct, !Dor 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 "Sct component; d) KIC 3230227, EB with a!Dor component; e) KIC 9851142, EB with most likely a !Dor 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 "Sct stars in particular is estimatedto be at least 30% (Breger & Rodríguez 2000; Lampens & Bo"n2000). 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.Pr!a 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 the"Sct, !Dor or hybrid star groups in a (Te!, log g)-diagram. Thesolid thick black and light grey lines mark the blue and red edgeof the observed instability strip of " Sct and !Dor 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 insu"ciently constrained and omitted them. Thesame holds for the B-type stars, which are much hotter than theTe! region shown here. The stars that show no clear periodicvariability on timescales typical for "Sct and !Dor 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 (Te!, 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 !Dor and "Sct range of frequen-cies to understand why no oscillations are detected. Figure 9presents the distribution in Te! (top left), log g (top right),Kp (bottom left), and total time span #T , expressed in d, of theKepler light curves (bottom right).

The cool boundary of the observational instability strip for!Dor stars is located around Te! = 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 candidate4 For 11% of the 121 stars we have no information on Te! 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 "Sct, !Dor 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 of!Dor or "Sct 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 di"cult 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 e!ect 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 "Sct, !Dor, and hybrid stars

7.2.1. The (Teff, log g)-diagram

The current ground-based (GB) view on the positions of the"Sct and !Dor classes in the (Te!, 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. (Te! , log g)-diagram with stars that show no clear periodic vari-ability on timescales typical for "Sct and !Dor 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 Te!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 " Sct and!Dor 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 Te! (top left), log g (top right), Kepler magni-tude Kp (bottom left), and total time span #T 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 di!erence 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 "Sct and!Dor stars occupy distinct locations in the (Te!, log g)-diagram,with a small overlap region.

Panel (b) of Fig. 10 shows a di!erent picture. Here the "Sct,!Dor, and hybrid stars from the Kepler sample are plotted. Weused the adopted values of Te! 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 (Te!, log g)-diagram: the"Sct and !Dor 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 "Sct stars exist beyond the red edge of the insta-bility strip, while Kepler !Dor 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 "Sct instability strip and the red edge of the !Dor in-stability strip, and beyond. The position of the Kepler " Sct and!Dor 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 Te! and log g for all stars to confirm this finding.

Because for most stars in our sample only KIC-based es-timates of Te! 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 (Te!, log g)-diagramconfirms the general findings described for the full sample.However, the scatter across the diagram of !Dor stars is lesspresent, but almost all !Dor candidates lie outside the obser-vational instability strip for !Dor stars. Ground-based observa-tions for the derivation of more precise values of Te! 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 Te! for the three groups of A-F type stars. The his-tograms related to " Sct, hybrid, and !Dor stars are colouredin dark grey, middle grey, and light grey respectively. The dis-tribution in Te! peaks around 7400 K, 7200 K, and 7000 Kfor "Sct, hybrid, and !Dor 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(Te!, log g)-diagram. It will be interesting to investigate whystars with similar values of Te! and log g in some cases pulsateas a " Sct star, and in others as a !Dor star, or as both. Anotherinteresting and puzzling result is that !Dor and "Sct 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 !Dor and"Sct stars. It illustrates that the cut-o! magnitude for the detec-tion of !Dor and "Sct 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 "Sct, !Dor and hybrid stars (see Table 2).Of the five !Dor 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 " Sct stars,

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Fig. 10. a) (Te! , log g)-diagram of the "Sct, !Dor, and hybrid stars detected from the ground (parameters taken from the literature).b) (Te! , log g)-diagram of the Kepler stars we classified as " Sct, !Dor, and hybrid stars in this paper. Open squares represent "Sct stars, as-terisks indicate !Dor stars, and hybrid stars are marked by bullets. The black cross in the right top corner shows typical errors on the values.c) (Te! , log g)-diagram of the subsample of 69 Kepler stars for which accurate Te! and log g values are available. The colour-codes are the sameas for panel b). d) (Te! , 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 %MLT = 1.8, %ov = 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 "Sct and !Dor stars, as described by Rodríguez & Breger (2001) andHandler & Shobbrook (2002), respectively. In the on-line version of the paper the symbols representing the " Sct, !Dor, 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 "Sct star FG Vir(e.g. Breger et al. 2005) and up to 10 frequencies in the !Dor 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 "Sct (top, dark grey), hybrid (middle, middlegrey), and !Dor (bottom, light grey) stars. The highest numberof frequencies are found for hybrid stars. It is worth mentioningthat the number of detected frequencies versus Te! follows a dis-tribution that peaks near 7700 K, 7500 K, and 7000 K for "Sct,hybrid, and !Dor stars, respectively. More modes are excited

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Fig. 11. Distribution in Te! (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: " Sct stars (top; dark grey), hybrid stars (middle; middle grey), and !Dor stars(bottom; light grey). The number of stars belonging to each bin (N) is indicated on the Y-axis.

near the centre of the "Sct instability strip. For the hybrid and!Dor 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 di!erent 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 "Sct pulsators than in !Dor stars. We pointout that the origin of high peaks detected in !Dor 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 Te! = 6600"7100 K, which is the cool part of theinstability strips.

We detected "Sct 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 " 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 "Sct

and hybrid stars have frequencies up to 80 d"1, and 9% onlyshow variations with frequencies lower than 20 d"1. We note that!Dor-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 !Dor and "Sct range(see Cols. 6 and 7 in Table 3 which give the frequency range ofthe detected frequencies in the !Dor and "Sct 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 !Sct, "Dor, 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 "Sct, !Dor, 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 (Te!, log g)-diagram (Fig. 10). Driven by the ideato find observables based on physical concepts that allow insightin the di!erent 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 di!erent inherent prop-erties of the three groups in one way or another. For instance,"Sct stars pulsate with shorter periods, and are generally hot-ter than !Dor stars. A combination of these parameters willlead to a di!erentiation of the groups, such as for instancea (Te!, 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 "Sct 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 e"ciency. Therefore, we expect a relation betweenthe energy of the observed modes and the convective e"ciencyof the outer convective zone. We searched for this relation andconstructed two observables, energy and e!ciency, that are es-timates of the energy and the convective e"ciency, using theavailable observational data.

8.1. Energy

The kinetic energy of a wave is given by

Ekin =12

f ()))(A*)2, (2)

where f is a function of the stellar density )), A is the ampli-tude of the oscillation, and * 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 * (Amax*max)2, (3)

where Amax and *max 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):

#R/R = " #mln(5 + 10dT )

, (4)

where #RR is the relative pulsational amplitude, #m the observed

magnitude variation of the mode, and dT is given by

dT ="Te!

Te!/+rr, (r = R), (5)

with +r 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 di!erence between

Fig. 12. Distribution in log(energy) (right), and log(e!ciency) (left) forthe "Sct (top, dark grey), hybrid (middle, middle grey), and !Dor (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 (!Dor stars) andlow-order p-modes ("Sct stars) is around one order of magni-tude or less, where the "Sct 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 di!erences 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 "Sct (top, dark grey), hybrid (middle, middlegrey), and !Dor (bottom, light grey) stars. Clearly, the weight ofthe distribution is located in the region log(energy) > 8 for starsdominated by frequencies in the " Sct domain, and in the regionlog(energy) < 8 for stars with dominant !Dor pulsations.

8.2. Efficiency

In the introduction of this section we pointed out that a relationbetween the convective e"ciency and mode excitation can exist.Recent studies on convective e"ciency of the outer convectivezone of F-G-K stars using 3D models show that the convectivee"ciency is related to the position of the star in the Hertzsprung-Russell (HR-) diagram (Trampedach & Stein 2011). To constructan observable related to the convective e"ciency 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 % that is usually calledmixing-length parameter.

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Fig. 13. Observable log(energy) plotted versus log(e!ciency) for "Sct (open squares) and !Dor (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 Te! and log g are available. In the on-line version of the paper the symbols representing the "Sct, !Dor 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(e!ciency), respectively.

(Böhm-Vitense 1958). There, the convective e"ciency,$, isdefined as

$ =

#A2

a0(+rad " +)

$1/3, (6)

with a0 a constant, +rad and + the radiative and real temperaturegradient, respectively, and

A $ cp#p)cs%2

9(T 3g,

2$1(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 #, the pressure p, the stellar density ), thesound velocity cs, the mixing length parameter %, the Stephan-Boltzmann constant (, the temperature T , the gravity g, and thefirst adiabatic coe"cient $1. 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 between!Dor and "Sct stars (see statistical test below), and define theobservable e!ciency as

e!ciency * (T 3e! log g)"2/3 $ $. (8)

Because the e"ciency of the convective zone is expected to behigher for !Dor stars than for "Sct stars, the observable e!-ciency should have a higher value for !Dor stars than "Sct stars.This behaviour is indeed observed, as illustrated in the left panelof Fig. 12, where the distribution in log(e!ciency) is given. Themajority of "Sct stars have values log(e!ciency) < "8.1 dex,while the histograms for !Dor pulsators peak in the regionlog(e!ciency) > "8.1 dex.

8.3. Efficiency versus energy

When we plot the two new observables, log(energy) versuslog(e!ciency), the groups of "Sct and !Dor stars are fairlywell separated (see top panels Fig. 13). A log(energy) value

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of 8 leaves 90% of the " Sct and !Dor 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(e!ciency), respectively. Thehybrid stars are placed in the intermediate region. We observedthat "Sct (!Dor) dominated hybrids fall in the same region asthe " Sct (!Dor) 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(e!ciency) isdi!erent for the three di!erent groups. The test shows that thedi!erence in the mean of the distributions in both log(energy)and log(e!ciency) is statistically significant for all groups.However, the apparent separation in log(e!ciency) becomes lessevident when we take the considerable error bars into account.We also performed a '2 test (as described by Press et al. 1992) todetermine if the distributions themselves were di!erent. All dis-tributions are statistically significant, save for the !Dor versushybrid star e!ciencies, where they are marginally similar. Thisconclusion holds even if we vary the Te! and log g values withinthe error ranges and recompute the e!ciencies or vary the inputsinto the energies. We point out once again that the definitionof e!ciency is only a rough estimate of the theoretical expres-sion for the convective e"ciency, and might – at this stage – notbe refined enough to display the separating power between thegroups we expect the convective e"ciency to have. In a follow-up investigation we will assess the goodness of approximationof our definition of e!ciency by comparison with values of theconvective e"ciency as given by Eq. (6), calculated for severalmodel stars, and finetune its definition.

The two new approximate observables energy and e!ciencyreflect the di!erent internal physics of oscillators with dominant"Sct pulsations and oscillators dominated by !Dor 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 e!ciency are promising starting points to ex-plore the relation between "Sct, !Dor 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 "Sct, !Dor, 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: !Dor, " Sct, and hybrid stars. The lattergroup includes both "Sct-dominated and !Dor-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 !Dor and "Sct 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 di!erent 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 detected" Sct periods are about 18 min. We find that hybrid starsshow all kinds of periodicities within the !Dor and "Sctrange. 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 e!ects of convection can explain part of theunexpected observed modes.

– The location of !Dor and " Sct classes in the (Te!, log g)-diagram has been extended (Fig. 10). We find indications thatKepler " Sct stars exist beyond the red edge of the observa-tional instability strip, while Kepler !Dor 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 " Sct instability strip and the red edge ofthe !Dor 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 " Sct and !Dor stars. From a theoretical pointof view, the overall presence of hybrid stars implies an in-vestigation of other pulsation mechanisms to supplement the# mechanism and convective blocking e!ect to drive hybridpulsations.

– Two new “observables” that reflect the di!erent internalphysics of " Sct and !Dor pulsators are introduced to in-vestigate the relation between the two types of pulsations(Fig. 13): (1) e!ciency, related to the convective e"ciencyof the outer convective zone, and a function of Te! 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(e!ciency), 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 " Sct, !Dor and hybrid stars.

– Our study indicates that Kp = 14 mag is a cut-o!magnitudefor 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 " Sct and!Dor 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 " Sct, !Dor, and hybrid stars.

Clearly, space missions are changing the landscape of !Dor and"Sct 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 the"Sct, !Dor, and hybrid groups, understand their relationship,clarify the driving mechanism(s) for each group, and elaborateon the variables energy and e!ciency. 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 (Te!, 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 the"Sct, !Dor, 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 e"ciently 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 "Sct 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 e!ect 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 # mechanism-related e!ect presented by Gautschy& Lö%er (1996) and Lö%er (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 !Dor 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 Te! = 10 000 K (Landstreet et al.2009).

Also the theoretical instability strips of the !Dor and"Sct pulsators need revision. As shown in Fig. 1, stars exhibitingpurely !Dor or "Sct pulsations seem to exist beyond the currentblue and red edge of the respective instability strips. Moreover, itis worth investigating if the evolutionary phase of !Dor 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 !Dor 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 Te! andlog g is needed to confirm this.

Furthermore, candidate !Dor 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 di!erentiation between pulsations and rotational variabilityproves to be very di"cult (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 e!ect of tidal interactions on pulsation frequencies(e.g. Uytterhoeven et al. 2004; Derekas et al. 2011).

Four of the EBs with a candidate !Dor, "Sct, 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 "Sct stars (out of 67 stars),and one candidate !Dor 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 "Sct starsdo not di!er much. With the current small number statistics, it isnot clear whether Ap/Am stars are indeed rare among !Dor 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) " Sct, !Dor, and hybrid stars are ex-pected to be among the stars observed by Kepler. Debosscheret al. (2011) reported the discovery of many additional "Sctand !Dor 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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1 Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot;CEA, IRFU, SAp, Centre de Saclay, 91191, Gif-sur-Yvette, France

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, Sta!ordshire, ST5 5BG, UK11 Institut für Astronomie, Türkenschanzstraße 17, 1180 Wien, Austria12 Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716

Warsaw, Poland

A125, page 20 of 70


13 South African Astronomical Observatory, PO Box 9, Observatory7935, South Africa

14 Instytut Astronomiczny, Uniwersytet Wroc%awski, Kopernika 11,51-622 Wroc%aw, 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

Nice Cedex 2, France19 Instituut voor Sterrenkunde, K.U.Leuven, Celestijnenlaan 200D,

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,

CNRS, 57 avenue d’Azereix, 65000 Tarbes, France23 Thüringer Landessternwarte Tautenburg, 07778 Tautenburg,

Germany24 Department of Astronomy, New Mexico State University, Las

Cruces, NM 88001, USA25 Astronomical Institute “Anton Pannekoek”, University of

Amsterdam, Science Park 904, 1098 XH Amsterdam, TheNetherlands

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,

USA34 Sydney Institute for Astronomy, School of Physics, A28, The

University of Sydney, NSW, 2006, Australia35 Bay Area Environmental Research Inst./NASA Ames Research

Center, Mo!ett Field, CA 94035, USA36 SETI Institute/NASA Ames Research Center, Mo!ett Field, CA

94035, USA

A125, page 21 of 70

A&A 534, A125 (2011)

Tabl

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35.8

9.5

F035

BD+

3734

90..

.39

459

137.

766

.5Q

0–Q

1Q

2.3

0216

8333

1932

44.5

9+

3735

36.2

10.1

...

TY

C31

35-2

03-1

...

1585

744

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2Q

1Q

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59.5

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C31

34-1

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1.2

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4394

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1928

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462

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0.0

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0230

6716

1929

03.7

9+

3741

19.2

12.0

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461

9.5

0.0

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0479

1932

24.5

8+

3740

21.6

10.8

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460

9.5

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0231

1130

1933

00.0

7+

3739

41.6

11.9

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461

9.5

0.0

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0242

3932

1905

59.6

9+

3746

42.6

13.0

...

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462

9.5

0.0

Q0–

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0243

9660

1922

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0244

3055

1925

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1926

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0255

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38.9

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...

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3846

429

2.5

219.

4Q

0–Q

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4.2

0256

8519

1920

03.9

4+

3752

27.4

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BD+

3734

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...

5980

432

1.4

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102

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302

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02.9

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207

344

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2Q

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.02

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25.2

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nary

199

944

.22.

7Q

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54.1

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202

144

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0–Q

1..

.02

5836

5819

3234

.58+

3751

32.0

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463

9.5

0.0

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0258

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1933

03.1

9+

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544

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3750

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bina

ry38

3809

829

2.5

219.

3Q

0–Q

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4.2

0269

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1905

08.6

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34.8

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TY

C31

20-1

608-

1..

.40

233

137.

766

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0–Q

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1920

33.1

0+

3759

54.0

11.2

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C31

34-8

33-1

...

4392

179

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0–Q

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8596

1930

35.7

8+

3755

51.5

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464

9.5

0.0

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0582

1932

21.1

9+

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4418

332

1.5

248.

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4.3

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4796

1906

47.6

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3804

32.4

12.5

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461

9.5

0.0

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5795

1908

06.5

3+

3800

26.4

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207

044

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8532

8019

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C31

34-9

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4440

032

1.5

248.

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4.3

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1928

31.2

0+

3801

40.7

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C31

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1932

16.4

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36.6

13.7

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463

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9151

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A125, page 22 of 70


Tabl

e1.

cont

inue

d.

KIC

IDR

AD

ecK

pSp

ectr

alty

peN

ame

Var

iabl

eN

Dat

apoi

nts

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ers

LC

Qua

rter

sSC

(J20

00)

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0297

0244

1903

42.3

4+

3808

14.2

12.5

...

...

...

463

9.5

0.0

Q0

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0297

2401

1906

35.8

6+

3808

59.3

13.5

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...

...

460

9.5

0.0

Q0

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0297

5832

1911

01.9

9+

3808

56.6

12.6

...

...

...

209

044

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2Q

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.02

9876

6019

2357

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3806

51.7

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1826

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4519

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9.8

95.2

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102

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3809

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207

844

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2Q

0–Q

1..

.02

9955

2519

3050

.23+

3811

41.6

13.2

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...

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464

9.5

0.0

Q0

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0299

7802

1932

48.1

4+

3808

35.9

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206

244

.21.

2Q

0–Q

1..

.03

0979

1219

0336

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3812

08.2

9.4

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BD+

3733

24bi

nary

4537

810

9.5

35.3

Q0–

Q1

Q2.

203

1114

5119

2037

.54+

3815

08.2

13.5

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463

9.5

0.0

Q0

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0311

9604

1928

30.5

0+

3816

09.4

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TY

C31

34-7

0-1

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4754

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2.8

187.

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1928

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044

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3821

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9.6

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BD+

3834

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nary%

4042

613

7.7

66.3

Q0–

Q1

Q2.

303

2186

3719

0531

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3820

07.4

10.6

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TY

C31

20-5

64-1

...

4007

222

8.8

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5Q

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1818

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466

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C31

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410

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TY

C31

35-3

96-1

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4013

522

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3.3

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1938

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3821

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C31

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1920

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1841

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1932

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137.

766

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1937

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5066

1938

29.6

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3825

24.9

13.6

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464

9.5

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Q0

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0342

4493

1900

37.5

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3830

20.2

9.6

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BD+

3833

91..

.40

427

137.

766

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2.3

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1902

50.2

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3834

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...

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C31

20-1

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4419

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3835

24.4

13.4

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9.5

0.0

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0342

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1905

12.8

6+

3832

46.6

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462

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631

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1939

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A125, page 23 of 70

A&A 534, A125 (2011)

Tabl

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cont

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d.

KIC

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Var

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1911

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44.4

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1926

47.5

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16.7

9.8

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1943

07.5

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49.9

10.4

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2255

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909

169.

895

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0–Q

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1938

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...

4519

610

9.5

35.3

Q0–

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203

9707

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3900

46.8

11.5

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C31

36-1

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175

169.

895

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1584

244

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2Q

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1100

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3910

15.3

9.8

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3834

65..

.15

856

44.4

1.2

Q1

Q0

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1916

32.7

8+

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...

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2.3

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3835

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nary

4546

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35.3

Q0–

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204

0694

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3908

25.2

11.2

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TY

C31

35-4

85-1

...

4411

832

1.5

248.

3Q

0–Q

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4.3

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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

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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

...

...

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207

544

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2Q

0–Q

1..

.04

1506

1119

1858

.20+

3916

01.4

7.9

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17,A

235H

D18

1469

bina

ry38

4316

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9.4

35.3

Q0–

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204

1608

7619

2929

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3913

17.6

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TY

C31

34-8

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4523

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9.5

35.4

Q0–

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204

1643

6319

3250

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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–

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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

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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

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TY

C31

21-1

037-

1..

.38

629

292.

521

9.3

Q0–

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204

2693

3719

3312

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3922

23.8

10.9

A8I

I35..

.bi

nary

3969

212

6.8

66.3

Q1

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304

2815

8119

4357

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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–

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4803

2119

4238

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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–

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304

5509

6219

1405

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3936

56.9

10.5

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TY

C31

25-3

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228.

815

8.5

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C31

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A125, page 24 of 70


Tabl

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cont

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37.5

10.9

A018

HD

2261

96..

.43

254

310.

524

8.4

Q1

Q4.

304

6477

6319

1841

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3942

26.7

10.8

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TY

C31

25-3

07-1

...

4519

610

9.5

35.4

Q0–

Q1

Q2.

204

6494

7619

2035

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3947

01.5

9.4

A235

BD+

3937

32..

.45

459

109.

535

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0–Q

1Q

2.2

0467

1225

1943

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8+

3945

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A718

HD

2255

44..

.54

194

137.

966

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1Q

0,Q

2.3

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1948

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32.5

10.2

A018

HD

2259

50..

.40

407

137.

766

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0–Q

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2.3

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1939

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C31

39-1

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7.3

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C31

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228.

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3958

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4031

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420

321.

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8630

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48.3

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44.2

1.2

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0490

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1908

48.0

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.49

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1940

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533

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0..

.Q

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0244

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0..

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1955

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1941

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NG

C68

1997

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2258

08..

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206

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A125, page 25 of 70

A&A 534, A125 (2011)

Tabl

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40.5

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4131

85..

.40

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815

8.5

Q0–

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305

9542

6419

1927

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4113

25.6

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1816

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535

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1934

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4037

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1948

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2259

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1955

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1887

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332

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593

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4118

26.4

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1803

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6.4

Q0–

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0678

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4123

33.4

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2264

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79.6

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Q0–

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1233

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2701

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1832

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1871

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Q0–

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4320

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15.3

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1798

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6.4

Q0–

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4409

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8.3

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A125, page 26 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.

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A125, page 27 of 70

A&A 534, A125 (2011)

Tabl

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A125, page 28 of 70


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A125, page 29 of 70

A&A 534, A125 (2011)

Tabl

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913

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308

8713

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TY

C35

41-1

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616

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534

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1697

1921

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...

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1585

444

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2Q

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008

9153

3520

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4510

02.9

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HD

1905

66..

.45

192

169.

895

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0893

3391

1852

06.4

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39.4

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1752

01..

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159

44.2

1.2

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33.8

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12.8

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...

...

4519

516

9.8

95.2

Q0–

Q1

Q3.

108

9729

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5132

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4515

51.8

11.5

...

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4519

416

9.8

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Q0–

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108

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1885

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206

137.

766

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C35

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A125, page 30 of 70


Tabl

e1.

cont

inue

d.

KIC

IDR

AD

ecK

pSp

ectr

alty

peN

ame

Var

iabl

eN

Dat

apoi

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uart

ers

LC

Qua

rter

sSC

(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

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109

1110

5619

5407

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4524

06.7

10.5

F035

BD+

4530

06..

.38

573

292.

521

9.3

Q0–

Q1

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209

1178

7520

0146

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4528

35.9

7.5

kA2m

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844

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5547

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4531

27.5

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C35

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79.6

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Q0–

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109

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4533

12.6

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1930

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4533

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11.3

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TY

C35

56-1

431-

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nary$

4546

410

9.5

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2016

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4536

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712

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4528

12..

.14

392

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422

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842

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1934

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5+

4541

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TY

C35

56-9

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...

4503

916

9.8

95.2

Q0–

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2293

1819

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BD+

4529

62..

.40

433

137.

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1905

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1914

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...

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1324

331

0.5

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135

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8.5

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4553

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C35

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4552

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137.

766

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0940

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A125, page 31 of 70

A&A 534, A125 (2011)

Tabl

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cont

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d.

KIC

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1937

26.4

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535

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1938

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1899

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1936

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1936

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1938

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C35

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1950

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C35

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C35

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A125, page 33 of 70

A&A 534, A125 (2011)Ta

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A125, page 34 of 70


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.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

pSp

ectr

alty

peN

ame

Var

iabl

eN

Dat

apoi

nts

#T

"TQ

uart

ers

LC

Qua

rter

sSC

(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,

eclip

sing

bina

ry(H

artm

anet

al.2

004)

;(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

ili19

76);

(10)

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)

;(13)

P=

4.56

427

d,ec

lipsi

ngbi

nary

(Mal

kov

etal

.200

6);

(14)

Abt

(198

4);(1

5)G

riga

hcèn

eet

al.(

2010

);(1

6)H

enry

etal

.(20

01);

(17)

Sato

&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&

Lyna

s-G

ray

(197

7);(2

2)G

uette

r(1

968)

;(23)

Abt

&C

ardo

na(1

984)

;(24)

Perr

yman

etal

.(19

97);

(25)

Mac

rae

(195

2);(2

6)Fl

oque

t(19

75);

(27)

Floq

uet

(197

0);(2

8)L

indo!

(197

2);(2

9)M

oore

&Pa

ddoc

k(1

950)

;(30)

Bid

elm

anet

al.

(198

8);(3

1)St

ephe

nson

(198

6);(3

2)V

ysso

tsky

(195

8);(3

3)H

ill&

Schi

lt(1

952)

;(34)

Can

non

(192

5);(3

5)K

harc

henk

o&

Roe

ser(

2009

);(3

6)E

clip

sing

bina

ry(P

r!a

etal

.201

1);(3

7)B

alon

aet

al.(

2011

c);

(38)

Ecl

ipsi

ngbi

nary

(Sla

wso

net

al.2

011)

;(39)

Wri

ghte

tal.

(200

3);(4

0)H

o%ei

t(19

51);

(41)

Mol

enda

-Zak

owic

zet

al.(

2008

).($

)B

inar

ityis

susp

ecte

dby

insp

ectio

nof

Dig

itize

dSk

ySu

rvey

and

2MA

SSim

ages

;(%)

spec

tros

copi

cbi

nary

.

A125, page 38 of 70


ble

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(in

dex)

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kms"

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the

750

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ple

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s"1 )

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Lite

ratu

reA

dopt

ed$

Spec

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Spec

tra

0116

2150

6870

...

...

...

6870±

290a

3.47

...

...

3.5±

0.3a

...

...

0129

4756

8410

...

...

...

8410±

290a

3.92

...

...

3.9±

0.3a

...

...

0143

2149

7270

...

...

...

7270±

290a

3.99

...

...

4.0±

0.3a

...

...

0157

1152%

7050

6500±

130b

7000±

75g

...

7000±

75g

3.16

4.49±

0.21

b4.

15±

0.26g

4.2±

0.26g

91±

13g

...

0157

1717

8110

...

...

...

8110±

290a

3.98

...

...

4.0±

0.3a

...

...

0157

3064

4639

...

...

...

4639±

290a

2.54

...

...

2.5±

0.3a

...

...

0171

8594

7500

...

...

...

7500±

290a

3.95

...

...

4.0±

0.3a

...

...

0199

5489

...

6410±

120b

...

...

6410±

120b

...

4.43±

0.21

b..

.4.

43±

0.21

b..

...

.02

0209

66..

.65

60±

130b

...

...

6560±

130b

...

3.50±

0.23

b..

.3.

50±

0.23

b..

...

.02

1622

8366

80..

...

...

.66

80±

290a

4.07

...

...

4.1±

0.3a

...

...

0216

3434

4590

...

...

...

4590±

290a

2.67

...

...

2.7±

0.3a

...

...

0216

6218

7150

7070±

80g

...

...

7070±

80g

3.35

3.84±

0.21

b2.

69±

0.19g

2.69±

0.19g

100±

3g..

.02

1683

3381

40..

...

...

.81

40±

290a

3.83

...

...

3.8±

0.3a

...

...

0230

0165

7140

...

...

...

7140±

290a

3.58

...

...

3.6±

0.3a

...

...

0230

3365

7280

...

...

...

7280±

290a

3.65

...

...

3.7±

0.3a

...

...

0230

6469

4600

...

...

...

4600±

290a

2.42

...

...

2.4±

0.3a

...

...

0230

6716

4670

...

...

...

4670±

290a

2.32

...

...

2.3±

0.3a

...

...

0231

0479

4440

...

...

...

4440±

290a

2.02

...

...

2.0±

0.3a

...

...

0231

1130

4640

...

...

...

4640±

290a

2.31

...

...

2.3±

0.3a

...

...

0242

3932

...

...

...

...

...

...

...

...

...

...

...

0243

9660

7990

...

...

...

7990±

290a

3.95

...

...

4.0±

0.3a

...

...

0244

3055

4590

...

...

...

4590±

290a

2.52

...

...

2.5±

0.3a

...

...

0244

4598

...

...

...

...

...

...

...

...

...

...

...

0255

6297

4590

...

...

...

4590±

290a

2.48

...

...

2.5±

0.3a

...

...

0255

6387

...

...

...

...

...

...

...

...

...

...

...

0255

7115

4340

...

...

...

4340±

290a

2.22

...

...

2.2±

0.3a

...

...

0255

7430

6250

...

...

...

6250±

290a

4.10

...

...

4.1±

0.3a

...

...

0255

8273

6440

...

...

...

6440±

290a

4.19

...

...

4.2±

0.3a

...

...

0256

8519

6170

...

...

...

6170±

290a

4.46

...

...

4.5±

0.3a

...

...

0256

9639

8020

...

...

...

8020±

290a

4.12

...

...

4.1±

0.3a

...

...

0257

1868

7930

...

...

...

7930±

290a

3.56

...

...

3.6±

0.3a

...

...

0257

2386

...

...

...

...

...

...

...

...

...

...

...

0257

5161

...

6940±

150b

...

...

6940±

150b

...

4.00±

0.21

b..

.4.

00±

0.21

b..

...

.02

5782

51..

.66

10±

130b

...

...

6610±

130b

...

4.23±

0.21

b..

.4.

23±

0.21

b..

...

.02

5836

5846

20..

...

...

.46

20±

290a

2.44

...

...

2.4±

0.3a

...

...

0258

4202

...

...

...

...

...

...

...

...

...

...

...

0258

4908

8180

...

...

...

8180±

290a

3.70

...

...

3.7±

0.3a

...

...

0269

4337

7290

...

...

...

7290±

290a

3.99

...

...

4.0±

0.3a

...

...

0270

7479

7280

...

...

...

7280±

290a

4.10

...

...

4.1±

0.3a

...

...

0271

8596

4850

...

...

...

4850±

290a

2.63

...

...

2.6±

0.3a

...

...

0272

0582

7060

...

...

...

7060±

290a

4.17

...

...

4.2±

0.3a

...

...

0283

4796

4570

...

...

...

4570±

290a

2.34

...

...

2.3±

0.3a

...

...

0283

5795

...

6690±

130b

...

...

6690±

130b

...

3.74±

0.22

b..

.3.

74±

0.22

b..

...

.

A125, page 39 of 70

A&A 534, A125 (2011)Ta

ble

2.co

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(dex

)v

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tra

Spec

tra

0285

3280

7320

...

...

...

7320±

290a

3.59

...

...

3.6±

0.3a

...

...

0285

5687

4770

...

...

...

4770±

290a

2.52

...

...

2.5±

0.3a

...

...

0286

0123

4620

...

...

...

4620±

290a

2.53

...

...

2.5±

0.3a

...

...

0296

9151

4700

...

...

...

4700±

290a

2.37

...

...

2.4±

0.3a

...

...

0297

0244

4720

...

...

...

4720±

290a

2.24

...

...

2.2±

0.3a

...

...

0297

2401

4660

...

...

...

4660±

290a

2.59

...

...

2.6±

0.3a

...

...

0297

5832

...

...

...

...

...

...

...

...

...

...

...

0298

7660

7310

...

...

...

7310±

290a

3.59

...

...

3.6±

0.3a

...

...

0298

9746

...

...

...

...

...

...

....

....

...

...

.02

9955

2548

50..

...

...

.48

50±

290a

2.64

...

...

2.6±

0.3a

...

...

0299

7802

...

...

...

...

...

...

...

...

...

...

...

0309

7912

7880

...

...

...

7880±

290a

3.56

...

...

3.6±

0.3a

...

...

0311

1451

...

...

...

...

...

...

...

...

...

...

...

0311

9604

8210

...

...

...

8210±

290a

4.04

...

...

4.0±

0.3a

...

...

0311

9825

...

...

...

...

...

...

...

...

...

...

...

0321

5800

...

...

...

...

...

...

...

...

...

...

...

0321

7554%

7800

7830±

120g

...

...

7830±

120g

3.50

3.69±

0.09g

...

3.69±

0.09g

228±

18g

...

0321

8637

7190

...

...

...

7190±

290a

3.89

...

...

3.9±

0.3a

...

...

0321

9256

7290

7500±

150i

...

...

7500±

150i

3.56

3.6±

0.1i

...

3.6±

0.1i

90±

5i..

.03

2207

8345

90..

...

...

.45

90±

290a

2.58

...

...

2.6±

0.3a

...

...

0322

2364

...

6750±

130b

...

...

6750±

130b

...

3.82±

0.21

b..

.3.

82±

0.21

b..

...

.03

2302

2779

70..

...

...

.79

70±

290a

3.89

...

...

3.9±

0.3a

...

...

0323

1406

7800

...

...

...

7800±

290a

3.76

...

...

3.8±

0.3a

...

...

0324

0556

8420

...

...

...

8420±

290a

3.85

...

...

3.9±

0.3a

...

...

0324

5420

7870

...

...

...

7870±

290a

3.66

...

...

3.7±

0.3a

...

...

0324

8627

4660

...

...

...

4660±

290a

2.32

...

...

2.3±

0.3a

...

...

0332

7681

6500

...

...

...

6500±

290a

3.68

...

...

3.7±

0.3a

...

...

0333

1147

7020

...

...

...

7020±

290a

3.55

...

...

3.6±

0.3a

...

...

0333

7002

7200

...

...

...

7200±

290a

3.60

...

...

3.6±

0.3a

...

...

0334

7643

6780

...

...

...

6780±

290a

4.07

...

...

4.1±

0.3a

...

...

0334

8390

7140

6850±

150b

...

...

6850±

150b

4.02

4.10±

0.21

b..

.4.

10±

0.21

b..

...

.03

3540

2248

10..

...

...

.48

10±

290a

2.26

...

...

2.3±

0.3a

...

...

0335

5066

4900

...

...

...

4900±

290a

2.74

...

...

2.7±

0.3a

...

...

0342

4493

7230

...

...

...

7230±

290a

3.44

...

...

3.4±

0.3a

...

...

0342

5802

8050

...

...

...

8050±

290a

4.06

...

...

4.1±

0.3a

...

...

0342

7144

4790

...

...

...

4790±

290a

2.55

...

...

2.5±

0.3a

...

...

0342

7365

4900

...

...

...

4900±

290a

2.48

...

...

2.5±

0.3a

...

...

0342

9637

6960

7200±

150i

...

...

7200±

150i

3.42

4.0±

0.1i

...

4.0±

0.1i

50±

5i..

.03

4379

4074

3073

42±

162e

7700±

120i

...

7700±

120i

3.86

3.3±

0.2e

4.1±

0.2i

4.1±

0.2i

120±

5i..

.03

4404

9574

10..

...

...

.74

10±

290a

3.93

...

...

3.9±

0.3a

...

...

0344

9373

...

...

...

...

...

...

...

...

...

...

...

0344

9625

...

...

...

...

...

...

...

...

...

...

...

0345

3494

7810

7750±

70g

...

...

7750±

70g

3.84

3.6±

0.3g

...

3.6±

0.3g

210±

15g

...

A125, page 40 of 70


ble

2.co

ntin

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Te!

(K)

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(dex

)v

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i(km

s"1 )

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...

...

...

4570±

290a

2.39

...

...

2.4±

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...

...

0345

8097

...

...

...

...

...

...

...

...

...

...

...

0345

8318

...

...

...

...

...

...

...

...

...

...

...

0352

5951

4570

...

...

...

4570±

290a

2.47

...

...

2.5±

0.3a

...

...

0352

8578

5020

...

...

...

5020±

290a

2.78

...

...

2.8±

0.3a

...

...

0353

9153

7310

6790±

140b

...

...

6790±

140b

3.81

3.73±

0.21

b..

.3.

73±

0.21

b..

...

.03

5460

6147

70..

...

...

.47

70±

290a

2.34

...

...

2.3±

0.3a

...

...

0355

8145

7340

...

...

...

7340±

290a

4.11

...

...

4.1±

0.3a

...

...

0362

9080

4830

...

...

...

4830±

290a

2.74

...

...

2.7±

0.3a

...

...

0363

3693

4530

...

...

...

4530±

290a

2.38

...

...

2.4±

0.3a

...

...

0363

4384

7480

...

...

...

7480±

290a

3.86

...

...

3.9±

0.3a

...

...

0364

3717

4410

...

...

...

4410±

290a

2.02

...

...

2.0±

0.3a

...

...

0364

4116

7500

...

...

...

7500±

290a

4.11

...

...

4.1±

0.3a

...

...

0365

5513

...

...

...

...

...

...

...

...

...

...

...

0365

5608

6600

...

...

...

6600±

290a

4.33

...

...

4.3±

0.3a

...

...

0366

3141

...

...

...

...

...

...

...

...

...

...

...

0373

3735

6440

6671±

76c

6760±

0d65

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0o66

71±

76c

4.03

4.31±

0.10

d..

.4.

3±

0.1d

...

...

0375

8717

...

...

...

...

...

...

...

...

...

...

...

0375

9814

4890

...

...

...

4890±

290a

3.51

...

...

3.5±

0.3a

...

...

0376

0002

7030

...

...

...

7030±

290a

4.04

...

...

4.0±

0.3a

...

...

0376

0826

8640

...

...

...

8640±

290a

3.42

...

...

3.4±

0.3a

...

...

0376

1641

8150

...

...

...

8150±

290a

4.10

...

...

4.1±

0.3a

...

...

0383

6911

...

...

...

...

...

...

...

...

...

...

...

0385

0810

7300

...

...

...

7300±

290a

3.56

...

...

3.6±

0.3a

...

...

0385

1151

8190

...

...

...

8190±

290a

4.10

...

...

4.1±

0.3a

...

...

0386

8032

8340

...

...

...

8340±

290a

4.04

...

...

4.0±

0.3a

...

...

0394

1283

7800

...

...

...

7800±

290a

3.87

...

...

3.9±

0.3a

...

...

0394

2911

7310

...

...

...

7310±

290a

3.99

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...

4.0±

0.3a

...

...

0396

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7460±

290a

3.59

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3.6±

0.3a

...

...

0397

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...

...

7160±

290a

4.14

...

...

4.1±

0.3a

...

...

0403

5667

7960

...

...

...

7960±

290a

3.87

...

...

3.9±

0.3a

...

...

0404

4353

8300

...

...

...

8300±

290a

3.56

...

...

3.6±

0.3a

...

...

0404

8488

5900

...

...

...

5900±

290a

4.21

...

...

4.2±

0.3a

...

...

0404

8494

7620

...

...

...

7620±

290a

3.95

...

...

4.0±

0.3a

...

...

0406

9477

7190

...

...

...

7190±

290a

3.80

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...

3.8±

0.3a

...

...

0407

5519

...

...

...

...

...

...

...

...

...

...

...

0407

7032

6790

...

...

...

6790±

290a

4.05

...

...

4.1±

0.3a

...

...

0414

4300

...

...

...

...

...

...

...

...

...

...

...

0415

0611

6620

...

...

...

6620±

290a

4.05

...

...

4.1±

0.3a

...

...

0416

0876

8290

...

...

...

8290±

290a

3.65

...

...

3.7±

0.3a

...

...

0416

4363

7480

6470±

120b

...

...

6470±

120b

3.83

3.84±

0.22

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0.22

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...

...

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290a

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...

...

3.5±

0.3a

...

...

0417

0631

7500

...

...

...

7500±

290a

3.47

...

...

3.5±

0.3a

...

...

A125, page 41 of 70

A&A 534, A125 (2011)Ta

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...

...

7220±

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...

3.9±

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...

...

0425

2757

7650

...

...

...

7650±

290a

3.72

...

...

3.7±

0.3a

...

...

0426

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...

...

...

8000±

290a

3.58

...

...

3.6±

0.3a

...

...

0428

1581

8140

...

...

...

8140±

290a

3.84

...

...

3.8±

0.3a

...

...

0438

3117

8250

...

...

...

8250±

290a

3.63

...

...

3.6±

0.3a

...

...

0447

6836

6760

...

...

...

6760±

290a

3.88

...

...

3.9±

0.3a

...

...

0448

0321

7150

...

...

...

7150±

290a

3.87

...

...

3.9±

0.3a

...

...

0448

8840

7130

...

...

...

7130±

290a

3.54

...

...

3.5±

0.3a

...

...

0455

0962

7290

...

...

...

7290±

290a

3.54

...

...

3.5±

0.3a

...

...

0455

6345

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...

...

...

7290±

290a

3.87

...

...

3.9±

0.3a

...

...

0457

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7000±

150i

...

...

7000±

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4.0±

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4.0±

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80±

20i

...

0458

8487

7860

...

...

...

7860±

290a

3.98

...

...

4.0±

0.3a

...

...

0464

7763

6890

6850±

140b

...

...

6850±

140b

4.05

3.56±

0.22

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.3.

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0.22

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...

.04

6494

7683

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...

...

.83

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290a

3.87

...

...

3.9±

0.3a

...

...

0467

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...

...

...

8230±

290a

3.27

...

...

3.3±

0.3a

...

...

0467

7684

7860

...

...

...

7860±

290a

3.32

...

...

3.3±

0.3a

...

...

0475

8316

6980

...

...

...

6980±

290a

4.07

...

...

4.1±

0.3a

...

...

0476

8677

8360

...

...

...

8360±

290a

3.97

...

...

4.0±

0.3a

...

...

0484

0675

7110

...

...

...

7110±

290a

3.55

...

...

3.6±

0.3a

...

...

0485

0899

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7132±

163e

7244±

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4.2±

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...

...

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290a

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...

3.9±

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...

...

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290o

...

...

...

...

...

...

0486

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7520

...

...

...

7520±

290a

3.90

...

...

3.9±

0.3a

...

...

0490

9697

7820

...

...

...

7820±

290a

3.92

...

...

3.9±

0.3a

...

...

0491

9818

7320

...

...

...

7320±

290a

3.97

...

...

4.0±

0.3a

...

...

0492

0125

7630

...

...

...

7630±

290a

3.62

...

...

3.6±

0.3a

...

...

0493

6524

7470

...

...

...

7470±

290a

3.79

...

...

3.8±

0.3a

...

...

0493

7257

...

...

...

...

...

...

...

...

...

...

...

0498

9900

7900

...

...

...

7900±

290a

3.51

...

...

3.5±

0.3a

...

...

0502

4150

5250

...

...

...

5250±

290a

...

...

...

...

...

...

0502

4454

6210

...

...

...

6210±

290a

4.11

...

...

4.1±

0.3a

...

...

0502

4455

6760

...

...

...

6760±

290a

4.44

...

...

4.4±

0.3a

...

...

0502

4456

4300

...

...

...

4300±

290a

...

...

...

...

...

...

0502

4750

...

...

...

...

...

...

...

...

...

...

...

0503

8228

6740

...

...

...

6740±

290a

4.13

...

...

4.1±

0.3a

...

...

0508

0290

5140

...

...

...

5140±

290a

3.58

...

...

3.6±

0.3a

...

...

0508

8308

6570

6740±

50g

...

...

6740±

50g

4.04

2.70±

0.13g

...

2.70±

0.13g

41±

1g..

.05

1057

5470

90..

...

...

.70

90±

290a

4.13

...

...

4.1±

0.3a

...

...

0511

2786

...

...

...

...

...

...

...

...

...

...

...

0511

2932

...

...

...

...

...

...

...

...

...

...

...

0511

3797

8140

...

...

...

8140±

290a

3.83

...

...

3.8±

0.3a

...

...

0516

4767

...

6576±

121e

6960±

80g

6982±

0o69

60±

80g

...

3.11±

0.19

e4.

01±

0.37g

3.11±

0.19

e16

2±

9g..

.05

1807

9674

50..

...

...

.74

50±

290a

3.89

...

...

3.9±

0.3a

...

...

A125, page 42 of 70


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Spec

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0519

7256

7610

...

...

...

7610±

290a

3.88

...

...

3.9±

0.3a

...

...

0519

9464

6080

...

...

...

6080±

290a

4.53

...

...

4.5±

0.3a

...

...

0520

0084

7470

...

...

...

7470±

290a

3.84

...

...

3.8±

0.3a

...

...

0520

1088

5450

...

...

...

5450±

290a

...

...

...

...

...

...

0520

9712

8360

...

...

...

8360±

290a

3.95

...

...

4.0±

0.3a

...

...

0521

7733

9120

...

...

...

9120±

290a

4.22

...

...

4.2±

0.3a

...

...

0521

9533

7410

...

...

...

7410±

290a

3.94

...

...

3.9±

0.3a

115n

...

0527

2673

7120

...

...

...

7120±

290a

3.76

...

...

3.8±

0.3a

...

...

0529

4571

6580

...

...

...

6580±

290a

4.07

...

...

4.1±

0.3a

...

...

0529

6877

6660

6500±

200i

...

...

6500±

200i

4.11

3.8±

0.3i

...

3.8±

0.3i

200±

20i

...

0535

6349

8290

...

...

...

8290±

290a

3.91

...

...

3.9±

0.3a

...

...

0537

1747

7070

...

...

...

7070±

290a

4.03

...

...

4.0±

0.3a

...

...

0539

1416

8060

...

...

...

8060±

290a

3.89

...

...

3.9±

0.3a

...

...

0542

8254

7390

...

...

...

7390±

290a

3.93

...

...

3.9±

0.3a

...

...

0543

6432

8330

...

...

...

8330±

290a

3.90

...

...

3.9±

0.3a

...

...

0543

7206

7710

...

...

...

7710±

290a

3.67

...

...

3.7±

0.3a

...

...

0544

6068%

5340

5980±

120g

...

...

5980±

120g

4.48

3.58±

0.28g

...

3.58±

0.28g

11±

1g..

.05

4731

7174

50..

...

...

.74

50±

290a

3.63

...

...

3.6±

0.3a

...

...

0547

4427

6880

...

...

...

6880±

290a

4.14

...

...

4.1±

0.3a

...

...

0547

6495

7360

...

...

...

7360±

290a

3.92

...

...

3.9±

0.3a

...

...

0547

6864

6580

6550±

120b

...

...

6550±

120b

4.11

3.72±

0.22

b..

.3.

72±

0.22

b..

...

.05

5138

6161

7066

10±

140b

...

...

6610±

140b

4.43

4.48±

0.21

b..

.4.

48±

0.21

b..

...

.05

6030

4980

00..

...

...

.80

00±

290a

3.71

...

...

3.7±

0.3a

...

...

0563

0362

7360

...

...

...

7360±

290a

3.53

...

...

3.5±

0.3a

...

...

0563

2093

8090

...

...

...

8090±

290a

4.07

...

...

4.1±

0.3a

...

...

0564

1711

7160

...

...

...

7160±

290a

3.97

...

...

4.0±

0.3a

...

...

0570

9664

7200

...

...

...

7200±

290a

4.04

...

...

4.0±

0.3a

...

...

0572

2346

6670

...

...

...

6670±

290a

4.21

...

...

4.2±

0.3a

...

...

0572

4048

6520

...

...

...

6520±

290a

4.08

...

...

4.1±

0.3a

...

...

0572

4440

7290

7699±

81c

7537±

186e

7350±

120i

7350±

120i

3.57

3.98±

0.21

e3.

6±

0.3i

3.6±

0.3i

220±

5i..

.05

7248

1073

30..

...

...

.73

30±

290a

3.88

...

...

3.9±

0.3a

...

...

0576

8203

6450

...

...

...

6450±

290a

3.95

...

...

3.9±

0.3a

...

...

0577

2411

6760

...

...

...

6760±

290a

4.18

...

...

4.2±

0.3a

...

...

0577

4557

7050

...

...

...

7050±

290a

3.99

...

...

4.0±

0.3a

...

...

0578

5707

8010

7940±

80g

...

...

7940±

80g

3.62

3.44±

0.26g

...

3.44±

0.26g

170±

11g

...

0581

0113

6360

6480±

120b

...

...

6480±

120b

4.22

3.60±

0.23

b..

.3.

60±

0.23

b..

...

.05

8577

1467

10..

...

...

.67

10±

290a

3.80

...

...

3.8±

0.3a

...

...

0588

0360

7690

...

...

...

7690±

290a

3.64

...

...

3.6±

0.3a

...

...

0594

0273

8010

...

...

...

8010±

290a

3.59

...

...

3.6±

0.3a

...

...

0595

4264

6720

6900±

146e

...

...

6900±

146e

4.15

3.86±

0.21

e..

.3.

86±

0.21

e..

...

.05

9658

3765

2069

75±

200i

...

...

6975±

200i

4.15

4.0±

0.4i

...

4.0±

0.3i

20±

10i

...

0598

0337

7680

...

...

...

7680±

290a

3.76

...

...

3.8±

0.3a

...

...

0598

8140

7450

7267±

163e

7400±

150i

...

7400±

150i

3.54

3.32±

0.23

e3.

7±

0.3i

3.32±

0.23

e70±

20i

...

A125, page 43 of 70

A&A 534, A125 (2011)Ta

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...

...

7110±

290a

3.79

...

...

3.8±

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...

...

0606

7817

7840

...

...

...

7840±

290a

3.86

...

...

3.9±

0.3a

...

...

0612

3324

6670

6700±

130b

6641±

123e

...

6700±

130b

3.40

3.09±

0.23

b3.

06±

0.21

e3.

1±

0.3b

...

...

0614

1372

7080

...

...

...

7080±

290a

4.21

...

...

4.2±

0.3a

...

...

0614

2919

7000

...

...

...

7000±

290a

4.02

...

...

4.0±

0.3a

...

...

0618

7665

6880

6025±

60c

6025±

0d..

.60

25±

60c

4.01

4.27±

0.11

d..

.4.

27±

0.11

d..

...

.06

1997

3178

50..

...

...

.78

50±

290a

3.55

...

...

3.6±

0.3a

...

...

0626

8890

7280

...

...

...

7280±

290a

3.49

...

...

3.5±

0.3a

...

...

0627

9848

...

6826±

140e

...

...

6826±

140e

...

3.8±

0.2e

...

3.8±

0.2e

...

...

0628

9468

8270

8150±

100g

...

...

8150±

100g

3.74

3.29±

0.09g

...

3.29±

0.09g

148±

7g..

.06

3017

4567

9067

40±

130b

...

...

6740±

130b

4.13

4.01±

0.21

b..

.4.

01±

0.21

b..

...

.06

3813

0680

60..

...

...

.80

60±

290a

3.63

...

...

3.6±

0.3a

...

...

0643

2054

7090

7287±

167e

7400±

150l

...

7400±

150l

3.85

3.81±

0.19

e3.

9±

0.2l

3.81±

0.19

e..

...

.06

4409

3083

20..

...

...

.83

20±

290a

4.09

...

...

4.1±

0.3a

...

...

0644

3122

7480

...

...

...

7480±

290a

3.54

...

...

3.5±

0.3a

...

...

0644

6951

7380

...

...

...

7380±

290a

4.06

...

...

4.1±

0.3a

...

...

0644

8112

8150

...

...

...

8150±

290a

4.01

...

...

4.0±

0.3a

...

...

0646

2033

8390

...

...

...

8390±

290a

4.32

...

...

4.3±

0.3a

...

...

0650

0578

7840

...

...

...

7840±

290a

3.64

...

...

3.6±

0.3a

...

...

0650

9175

7300

7520±

60g

...

...

7520±

60g

3.52

3.29±

0.3g

...

3.3±

0.3g

132±

8g..

.06

5198

6971

50..

...

...

.71

50±

290a

3.80

...

...

3.8±

0.3a

...

...

0658

6052

7520

...

...

...

7520±

290a

4.05

...

...

4.1±

0.3a

...

...

0658

7551

8380

8870±

190g

...

...

8870±

190g

3.93

3.78±

0.09g

...

3.78±

0.09g

138±

9g..

.06

5904

0370

30..

...

...

.70

30±

290a

3.93

...

...

3.9±

0.3a

...

...

0660

6229

6750

...

...

...

6750±

290a

4.09

...

...

4.1±

0.3a

...

...

0661

4168

7270

...

...

...

7270±

290a

4.14

...

...

4.1±

0.3a

...

...

0662

9106

7070

...

...

...

7070±

290a

3.95

...

...

4.0±

0.3a

...

...

0666

8729

7770

...

...

...

7770±

290a

3.48

...

...

3.5±

0.3a

...

...

0667

0742

7450

6386±

62c

...

...

6386±

62c

3.61

...

...

3.6±

0.3a

...

...

0667

8614

7410

...

...

...

7410±

290a

3.85

...

...

3.9±

0.3a

...

...

0669

4649

7750

...

...

...

7750±

290a

3.66

...

...

3.7±

0.3a

...

...

0675

6386

7990

7900±

70g

...

...

7900±

70g

3.51

3.17±

0.10g

...

3.2±

0.1g

190±

12g

...

0675

6481

7310

...

...

...

7310±

290a

3.52

...

...

3.5±

0.3a

...

...

0676

1539

7240

...

...

...

7240±

290a

4.04

...

...

4.0±

0.3a

...

...

0677

6331

7650

...

...

...

7650±

290a

3.72

...

...

3.7±

0.3a

...

...

0679

0335

7690

...

...

...

7690±

290a

3.52

...

...

3.5±

0.3a

...

...

0680

4821

7480

...

...

...

7480±

290a

3.65

...

...

3.7±

0.3a

...

...

0686

5077

7770

...

...

...

7770±

290a

3.62

...

...

3.6±

0.3a

...

...

0692

2690

7320

...

...

...

7320±

290a

3.61

...

...

3.6±

0.3a

...

...

0692

3424

7060

...

...

...

7060±

290a

4.16

...

...

4.2±

0.3a

...

...

0693

7758

7840

...

...

...

7840±

290a

3.47

...

...

3.5±

0.3a

...

...

0693

9291

7140

...

...

...

7140±

290a

3.52

...

...

3.5±

0.3a

...

...

0694

7064

8170

...

...

...

8170±

290a

3.91

...

...

3.9±

0.3a

...

...

A125, page 44 of 70


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...

...

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...

...

0696

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...

...

...

7650±

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3.39

...

...

3.4±

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...

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...

...

...

6910±

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4.06

...

...

4.1±

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...

...

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6205

6970

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140b

...

...

6900±

140b

4.05

3.73±

0.21

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0.21

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...

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...

...

.70

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290a

4.11

...

...

4.1±

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...

...

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...

...

...

7270±

290a

4.08

...

...

4.1±

0.3a

...

...

0711

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7780

7608±

190e

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200i

...

7500±

200i

3.49

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3.26±

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...

0712

2746

8340

7740±

200b

...

...

7740±

200b

3.84

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0.18

b..

...

.07

2042

3780

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...

...

.80

70±

290a

4.05

...

...

4.1±

0.3a

...

...

0721

1759

8220

...

...

...

8220±

290a

3.77

...

...

3.8±

0.3a

...

...

0721

2040

7500

...

...

...

7500±

290a

3.97

...

...

4.0±

0.3a

...

...

0721

5607

6530

...

...

...

6530±

290a

4.06

...

...

4.1±

0.3a

...

...

0721

7483

6940

...

...

...

6940±

290a

3.89

...

...

3.9±

0.3a

...

...

0722

0356

6340

...

...

...

6340±

290a

4.26

...

...

4.3±

0.3a

...

...

0726

5427

7560

...

...

...

7560±

290a

4.13

...

...

4.1±

0.3a

...

...

0728

7118

7850

...

...

...

7850±

290a

3.76

...

...

3.8±

0.3a

...

...

0730

0387

7000

...

...

...

7000±

290a

3.60

...

...

3.6±

0.3a

...

...

0730

4385

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...

...

...

6890±

290a

3.60

...

...

3.6±

0.3a

...

...

0733

8125

7860

...

...

...

7860±

290a

3.96

...

...

4.0±

0.3a

...

...

0735

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7290

...

...

...

7290±

290a

3.65

...

...

3.7±

0.3a

...

...

0735

2425

6890

...

...

...

6890±

290a

4.07

...

...

4.1±

0.3a

...

...

0735

2776

7460

...

...

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7460±

290a

3.99

...

...

4.0±

0.3a

...

...

0738

5478

6480

...

...

...

6480±

290a

3.87

...

...

3.9±

0.3a

...

...

0743

6266

7020

...

...

...

7020±

290a

4.05

...

...

4.1±

0.3a

...

...

0745

0284

7930

...

...

...

7930±

290a

3.74

...

...

3.7±

0.3a

...

...

0750

2559

7470

...

...

...

7470±

290a

3.89

...

...

3.9±

0.3a

...

...

0753

3694

7860

...

...

...

7860±

290a

3.80

...

...

3.8±

0.3a

...

...

0754

8061

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5370±

120q

...

...

5370±

120q

2.42

1.50±

0.35

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.2.

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0.3a

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2q..

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250r

...

...

7500±

250l

3.84

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0.25

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90±

0.25

l10±

2l..

.07

5532

3769

30..

...

...

.69

30±

290a

4.12

...

...

4.1±

0.3a

...

...

0758

3939

8310

...

...

...

8310±

290a

3.95

...

...

3.9±

0.3a

...

...

0759

6250

6870

...

...

...

6870±

290a

3.90

...

...

3.9±

0.3a

...

...

0766

2076

7050

...

...

...

7050±

290a

4.01

...

...

4.0±

0.3a

...

...

0766

8791

8150

...

...

...

8150±

290a

3.89

...

...

3.9±

0.3a

...

...

0766

9848

...

...

...

...

...

...

...

...

...

19o

19.4±

2.0n

0769

4191

7850

...

...

...

7850±

290a

3.54

...

...

3.5±

0.3a

...

...

0769

7795

7480

...

...

...

7480±

290a

3.56

...

...

3.6±

0.3a

...

...

0769

9056

7410

...

...

...

7410±

290a

3.67

...

...

3.7±

0.3a

...

...

0770

2705

7310

6710±

130b

...

...

6710±

130b

4.00

2.88±

0.23

b..

.2.

88±

0.23

b..

...

.07

7324

5875

50..

...

...

.75

50±

290a

3.64

...

...

3.6±

0.3a

...

...

0774

2739

7170

...

...

...

7170±

290a

3.89

...

...

3.9±

0.3a

...

...

0774

8238

7230

7260±

64g

...

...

7260±

64g

3.47

4.06±

0.28g

...

4.06±

0.28g

119±

6g..

.07

7568

5380

60..

...

...

.80

60±

290a

3.94

...

...

3.9±

0.3a

...

...

A125, page 45 of 70

A&A 534, A125 (2011)Ta

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...

...

...

...

...

...

...

...

...

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...

...

...

7450±

290a

3.50

...

...

3.5±

0.3a

...

...

0777

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...

...

...

7300±

290a

3.53

...

...

3.5±

0.3a

...

...

0777

3133

6640

...

...

...

6640±

290a

3.52

...

...

3.5±

0.3a

...

...

0777

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8120

...

...

...

8120±

290a

3.75

...

...

3.8±

0.3a

...

...

0779

8339

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6880±

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6700±

200i

6745±

0o68

80±

144e

3.40

3.90±

0.21

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7±

0.3i

3.90±

0.21

e15

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2.0n

15±

5g,i

0782

7131

8290

...

...

...

8290±

290a

3.49

...

...

3.5±

0.3a

...

...

0783

1302

8160

...

...

...

8160±

290a

3.86

...

...

3.9±

0.3a

...

...

0783

4612

7450

...

...

...

7450±

290a

3.67

...

...

3.7±

0.3a

...

...

0784

2286

7660

...

...

...

7660±

290a

3.77

...

...

3.8±

0.3a

...

...

0784

2621

7620

...

...

...

7620±

290a

3.54

...

...

3.5±

0.3a

...

...

0784

8288

7380

...

...

...

7380±

290a

3.52

...

...

3.5±

0.3a

...

...

0789

0526

7080

...

...

...

7080±

290a

4.07

...

...

4.1±

0.3a

...

...

0790

0367

6970

...

...

...

6970±

290a

4.14

...

...

4.1±

0.3a

...

...

0790

8633

7840

...

...

...

7840±

290a

3.73

...

...

3.7±

0.3a

...

...

0795

9867

8480

...

...

...

8480±

290a

3.90

...

...

3.9±

0.3a

...

...

0797

7996

7120

...

...

...

7120±

290a

3.77

...

...

3.8±

0.3a

...

...

0798

5370

5610

...

...

...

5610±

290a

4.60

...

...

4.6±

0.3a

...

...

0802

9546

7120

...

...

...

7120±

290a

3.89

...

...

3.9±

0.3a

...

...

0804

3961

6350

...

...

...

6350±

290a

3.62

...

...

3.6±

0.3a

...

...

0805

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6770±

150b

...

...

6770±

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3.67

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b..

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...

...

0810

3917

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...

...

...

7130±

290a

4.16

...

...

4.2±

0.3a

...

...

0810

4589

6510

...

...

...

6510±

290a

4.29

...

...

4.3±

0.3a

...

...

0812

3127

7160

...

...

...

7160±

290a

3.69

...

...

3.7±

0.3a

...

...

0814

3903

3680

...

...

...

3680±

290a

4.22

...

...

4.2±

0.3a

...

...

0814

4674

7290

...

...

...

7290±

290a

3.85

...

...

3.9±

0.3a

...

...

0814

5477

6800

...

...

...

6800±

290a

4.06

...

...

4.1±

0.3a

...

...

0814

9341

7540

...

...

...

7540±

290a

4.00

...

...

4.0±

0.3a

...

...

0815

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5020

...

...

...

5020±

290a

4.14

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...

4.1±

0.3a

...

...

0819

7761

7070

...

...

...

7070±

290a

4.09

...

...

4.1±

0.3a

...

...

0819

7788

8010

7500±

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...

...

7500±

150i

3.98

4.0±

0.3i

...

4.0±

0.3i

230±

20i

...

0821

1500

7400

...

...

...

7400±

290a

3.91

...

...

3.9±

0.3a

...

...

0821

8419

4550

...

...

...

4550±

290a

2.20

...

...

2.2±

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...

...

0822

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...

...

...

...

...

...

...

...

...

...

...

0822

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140b

...

...

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...

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...

...

4.5±

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...

...

0823

0025

7280

...

...

...

7280±

290a

3.48

...

...

3.5±

0.3a

...

...

0824

5366

...

...

...

...

...

...

...

...

...

...

...

0824

8630

7310

...

...

...

7310±

290a

3.74

...

...

3.7±

0.3a

...

...

0826

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...

...

...

7230±

290a

4.10

...

...

4.1±

0.3a

...

...

0826

4075

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...

...

...

7650±

290a

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...

...

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0.3a

...

...

0826

4274

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...

...

7640±

290a

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...

3.7±

0.3a

...

...

0826

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200i

...

...

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200i

3.73

3.7±

0.3i

...

3.7±

0.3i

250±

20i

...

A125, page 46 of 70


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...

...

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...

...

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...

...

...

...

...

...

...

...

...

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...

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...

...

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...

3.7±

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...

...

0826

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...

...

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...

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...

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...

...

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...

...

4.1±

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...

...

0829

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...

...

6450±

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...

4.2±

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...

...

0832

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...

...

...

7590±

290a

3.92

...

...

3.9±

0.3a

...

...

0833

0056

7240

...

...

...

7240±

290a

4.10

...

...

4.1±

0.3a

...

...

0833

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6900

...

...

...

6900±

290a

4.12

...

...

4.1±

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...

...

0833

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6020

...

...

...

6020±

290a

4.86

...

...

4.9±

0.3a

...

...

0833

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...

...

...

7620±

290a

4.03

...

...

4.0±

0.3a

...

...

0835

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...

...

...

6560±

290a

4.30

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...

4.3±

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...

...

0835

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...

...

7040±

290a

4.11

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4.1±

0.3a

...

...

0835

5837

5860

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...

...

5860±

290a

4.30

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...

4.3±

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...

...

0839

7426

7030

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...

...

7030±

290a

3.55

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...

3.6±

0.3a

...

...

0841

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7780

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...

...

7780±

290a

4.00

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...

4.0±

0.3a

...

...

0842

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7360

...

...

...

7360±

290a

3.67

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...

3.7±

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...

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...

...

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3.9±

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0845

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...

...

5050±

290a

4.52

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...

0848

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6360±

290a

4.33

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4.3±

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0848

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6190±

290a

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0848

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290a

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290a

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290a

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0851

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8320±

290a

3.60

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...

8240±

290a

4.02

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0.3a

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...

0852

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7350±

290a

4.19

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4.2±

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7860±

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...

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200i

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...

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...

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...

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...

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...

...

7380±

290a

3.45

...

...

3.4±

0.3a

...

...

A125, page 47 of 70

A&A 534, A125 (2011)Ta

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...

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...

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...

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6800±

290a

4.15

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...

4.2±

0.3a

...

...

0875

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...

7340±

60g

...

...

7340±

60g

...

3.72±

0.3g

...

3.7±

0.3g

165±

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...

...

6570±

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3.81

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...

3.7±

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...

0883

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...

...

6200±

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3.85

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...

3.9±

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...

0886

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...

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...

...

...

...

...

...

...

...

...

...

0887

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...

...

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290a

3.43

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...

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7730±

290a

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...

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...

0891

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...

...

7770±

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3.48

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3.5±

0.3a

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0893

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193e

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...

...

7180±

290a

3.90

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...

3.9±

0.3a

...

...

0902

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...

6880±

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.09

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290a

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...

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0.3a

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...

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...

...

7610±

290a

3.74

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...

3.7±

0.3a

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...

0907

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...

...

...

...

...

...

...

...

...

...

...

0907

3007

...

...

...

...

...

...

...

...

...

...

...

0907

3985

5990

...

...

...

5990±

290a

4.37

...

...

4.4±

0.3a

...

...

0907

7192

4750

...

...

...

4750±

290a

4.40

...

...

4.4±

0.3a

...

...

0910

8615

6710

...

...

...

6710±

290a

3.81

...

...

3.8±

0.3a

...

...

0911

1056

6800

...

...

...

6800±

290a

3.65

...

...

3.7±

0.3a

...

...

0911

7875

...

...

...

...

...

...

...

...

...

...

...

0913

8872

7500

...

...

...

7500±

290a

4.03

...

...

4.0±

0.3a

...

...

0914

3785

7600

...

...

...

7600±

290a

4.25

...

...

4.3±

0.3a

...

...

0914

7229

7300

...

...

...

7300±

290a

3.57

...

...

3.6±

0.3a

...

...

0915

6808

7070

...

...

...

7070±

290a

3.94

...

...

3.9±

0.3a

...

...

0920

1644

...

...

...

...

...

...

...

...

...

...

...

0920

4672

4030

...

...

...

4030±

290a

1.82

...

...

1.8±

0.3a

...

...

0920

4718

7150

...

...

...

7150±

290a

3.93

...

...

3.9±

0.3a

...

...

0921

0037

...

...

...

...

...

...

...

...

...

...

...

0921

6367

7840

...

...

...

7840±

290a

3.65

...

...

3.7±

0.3a

...

...

0922

2942

7000

...

...

...

7000±

290a

3.99

...

...

4.0±

0.3a

...

...

0922

9318

7140

...

...

...

7140±

290a

3.65

...

...

3.7±

0.3a

...

...

A125, page 48 of 70


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...

...

8050±

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3.79

...

...

3.8±

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...

...

0926

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5060

...

...

...

5060±

290a

4.46

...

...

4.5±

0.3a

...

...

0926

4462

4870

...

...

...

4870±

290a

3.31

...

...

3.3±

0.3a

...

...

0926

7042

8130

...

...

...

8130±

290a

3.81

...

...

3.8±

0.3a

...

...

0926

8087

...

...

...

...

...

...

...

...

...

...

...

0927

2082

...

...

...

...

...

...

...

...

...

...

...

0927

4000

5660

...

...

...

5660±

290a

4.46

...

...

4.5±

0.3a

...

...

0929

1618

7610

...

...

...

7610±

290a

3.61

...

...

3.6±

0.3a

...

...

0930

6095

6340

...

...

...

6340±

290a

4.63

...

...

4.6±

0.3a

...

...

0932

4334

7250

...

...

...

7250±

290a

4.06

...

...

4.1±

0.3a

...

...

0932

7993

4600

...

...

...

4600±

290a

2.37

...

...

2.4±

0.3a

...

...

0933

6219

6520

...

...

...

6520±

290a

4.26

...

...

4.3±

0.3a

...

...

0935

1622

7450

...

...

...

7450±

290a

3.53

...

...

3.5±

0.3a

...

...

0935

3572

7190

...

...

...

7190±

290a

3.99

...

...

4.0±

0.3a

...

...

0936

8220

6660

...

...

...

6660±

290a

4.10

...

...

4.1±

0.3a

...

...

0938

6259

5810

...

...

...

5810±

290a

4.30

...

...

4.3±

0.3a

...

...

0939

1395

7310

...

...

...

7310±

290a

3.96

...

...

4.0±

0.3a

...

...

0939

5246

...

...

...

...

...

...

...

...

...

...

...

0940

8694

7480

6810±

130b

...

...

6810±

130b

3.62

3.80±

0.19

b..

.3.

80±

0.19

b..

...

.09

4130

5784

7086

30±

140g

...

...

8630±

140g

3.87

3.62±

0.07g

...

3.62±

0.07g

165±

8g..

.09

4509

4082

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...

...

.82

10±

290a

4.21

...

...

4.2±

0.3a

...

...

0945

1598

6060

...

...

...

6060±

290a

4.56

...

...

4.6±

0.3a

...

...

0945

3075

8060

...

...

...

8060±

290a

4.00

...

...

4.0±

0.3a

...

...

0945

8750

5070

...

...

...

5070±

290a

3.69

...

...

3.7±

0.3a

...

...

0947

3000

7130

...

...

...

7130±

290a

3.88

...

...

3.9±

0.3a

...

...

0948

9590

7160

...

...

...

7160±

290a

4.09

...

...

4.1±

0.3a

...

...

0949

0042

7060

...

...

...

7060±

290a

3.98

...

...

4.0±

0.3a

...

...

0949

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...

...

...

6880±

290a

4.07

...

...

4.1±

0.3a

...

...

0950

9296

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...

...

...

7400±

290a

3.61

...

...

3.6±

0.3a

...

...

0951

4879

5880

...

...

...

5880±

290a

4.10

...

...

4.1±

0.3a

...

...

0952

0434

...

...

...

...

...

...

...

...

...

...

...

0952

0864

...

...

...

...

...

...

...

...

...

...

...

0953

2644

7300

...

...

...

7300±

290a

3.56

...

...

3.6±

0.3a

...

...

0953

3449

...

...

...

...

...

...

...

...

...

...

...

0953

3489

...

...

...

...

...

...

...

...

...

...

...

0955

0886

7490

...

...

...

7490±

290a

3.89

...

...

3.9±

0.3a

...

...

0955

1281

7450

...

...

...

7450±

290a

3.65

...

...

3.7±

0.3a

...

...

0958

0794

7300

...

...

...

7300±

290a

4.05

...

...

4.1±

0.3a

...

...

0958

2720

5620

...

...

...

5620±

290a

4.49

...

...

4.5±

0.3a

...

...

0959

3997

7620

...

...

...

7620±

290a

3.62

...

...

3.6±

0.3a

...

...

0959

4100

6520

...

...

...

6520±

290a

4.51

...

...

4.5±

0.3a

...

...

0960

4762

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...

...

...

7290±

290a

3.77

...

...

3.8±

0.3a

...

...

0963

0640

6530

...

...

...

6530±

290a

4.10

...

...

4.1±

0.3a

...

...

A125, page 49 of 70

A&A 534, A125 (2011)Ta

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...

...

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...

...

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...

...

0964

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...

...

...

6440±

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...

...

4.3±

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...

...

0964

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...

...

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...

...

4.1±

0.3a

...

...

0964

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...

...

...

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290a

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...

...

4.2±

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...

...

0965

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...

...

...

8390±

290a

3.68

...

...

3.7±

0.3a

...

...

0965

1065

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7010±

150b

...

...

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150b

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...

...

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290a

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...

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...

...

0965

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...

...

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290a

3.48

...

...

3.5±

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...

...

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...

...

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3.9±

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...

3.9±

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20i

...

0965

5151

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...

...

...

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290a

4.18

...

...

4.2±

0.3a

...

...

0965

5177

6900

...

...

...

6900±

290a

3.87

...

...

3.9±

0.3a

...

...

0965

5393

7570

...

...

...

7570±

290a

4.06

...

...

4.1±

0.3a

...

...

0965

5422

7600

...

...

...

7600±

290a

3.38

...

...

3.4±

0.3a

...

...

0965

5433

8300

...

...

...

8300±

290a

...

...

...

...

...

...

0965

5438

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...

...

...

6970±

290a

4.09

...

...

4.1±

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...

...

0965

5487

...

...

...

...

...

...

...

...

...

...

...

0965

5501

7740

...

...

...

7740±

290a

3.88

...

...

3.9±

0.3a

...

...

0965

5514

7440

...

...

...

7440±

290a

3.61

...

...

3.6±

0.3a

...

...

0965

5800

6780

...

...

...

6780±

290a

4.16

...

...

4.2±

0.3a

...

...

0965

6348

7670

7190±

160b

...

...

7190±

160b

3.52

3.9±

0.2b

...

3.9±

0.2b

...

...

0966

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...

...

...

7190±

290a

3.99

...

...

4.0±

0.3a

...

...

0967

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...

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8230±

290a

3.87

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...

3.9±

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...

0969

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...

...

...

...

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0969

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...

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4.14

...

...

4.1±

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...

...

0969

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...

...

...

...

...

...

...

...

...

...

...

0970

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...

...

...

7590±

290a

4.03

...

...

4.0±

0.3a

...

...

0970

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6700±

100m

...

...

6700±

100m

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3.7±

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...

3.7±

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...

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...

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0971

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3.65

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...

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...

...

0971

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...

...

...

...

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...

...

...

...

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0971

6947

7300

...

...

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7300±

290a

4.04

...

...

4.0±

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...

...

0976

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...

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4.03

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...

...

0976

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...

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290a

4.68

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...

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...

0976

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...

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...

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...

3.7±

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...

...

0977

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...

...

...

7450±

290a

4.05

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...

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0977

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...

0981

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87g

...

...

7847±

87g

3.47

3.15±

0.23g

...

3.15±

0.23g

56±

4g..

.

A125, page 50 of 70


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...

...

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...

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...

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...

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...

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...

...

0988

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...

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5090±

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...

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...

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...

...

7410±

290a

3.53

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...

3.5±

0.3a

...

...

0994

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...

...

7040±

290a

4.29

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...

4.3±

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...

0994

4730

5920

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...

...

5920±

290a

4.18

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...

4.2±

0.3a

...

...

0997

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...

...

...

7790±

290a

3.64

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...

3.6±

0.3a

...

...

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...

...

5270±

290a

4.35

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...

4.4±

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...

...

0999

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...

...

6050±

290a

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...

4.3±

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...

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...

...

5290±

290a

3.85

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...

3.9±

0.3a

...

...

0999

5464

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...

...

4850±

290a

2.64

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...

2.6±

0.3a

...

...

1000

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...

...

8200±

290a

3.96

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...

4.0±

0.3a

...

...

1000

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7490

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...

...

7490±

290a

3.74

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...

3.7±

0.3a

...

...

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...

...

4340±

290a

4.60

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...

4.6±

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...

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...

...

4680±

290a

2.39

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...

2.4±

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...

...

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...

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7160±

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3.92

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...

3.9±

0.3a

...

...

1003

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...

...

...

6700±

290a

4.30

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...

4.3±

0.3a

...

...

1003

5772

7290

...

...

...

7290±

290a

3.48

...

...

3.5±

0.3a

...

...

1005

6217

6000

...

...

...

6000±

290a

4.28

...

...

4.3±

0.3a

...

...

1005

6297

7160

...

...

...

7160±

290a

4.03

...

...

4.0±

0.3a

...

...

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7129

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...

...

4860±

290a

3.17

...

...

3.2±

0.3a

...

...

1006

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...

...

5270±

290a

4.93

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...

4.9±

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...

...

1006

4111

7220

...

...

...

7220±

290a

4.05

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...

4.1±

0.3a

...

...

1006

5244

7260

...

...

...

7260±

290a

3.98

...

...

4.0±

0.3a

...

...

1006

8892

4610

...

...

...

4610±

290a

2.29

...

...

2.3±

0.3a

...

...

1006

9934

7060

...

...

...

7060±

290a

4.01

...

...

4.0±

0.3a

...

...

1007

3601

7100

6680±

130b

...

...

6680±

130b

4.09

3.47±

0.22

b..

.3.

47±

0.22

b..

...

.10

0903

4571

90..

...

...

.71

90±

290a

3.94

...

...

3.9±

0.3a

...

...

1009

6499

7780

8021±

218e

...

...

8012±

218e

4.13

3.91±

0.16

e..

.3.

91±

0.16

e..

...

.10

1195

1762

3064

50±

80g

...

...

6450±

80g

4.38

4.3±

0.2g

...

4.3±

0.2g

78±

4g..

.10

1307

7780

20..

...

...

.80

20±

290a

3.71

...

...

3.7±

0.3a

...

...

1013

4600

5010

...

...

...

5010±

290a

3.06

...

...

3.1±

0.3a

...

...

1013

4800

7910

...

...

...

7910±

290a

3.71

...

...

3.7±

0.3a

...

...

1014

0513

5880

6030±

100b

...

...

6030±

100b

3.96

4.30±

0.22

b..

.4.

30±

0.22

b..

...

.10

1406

6566

20..

...

...

.66

20±

290a

4.37

...

...

4.4±

0.3a

...

...

1016

4569

7720

7130±

150b

...

...

7130±

150b

3.66

2.90±

0.22

b..

.2.

90±

0.22

b..

...

.10

2063

4052

1057

60±

80b

...

...

5760±

80b

4.46

4.48±

0.22

b..

.4.

48±

0.22

b..

...

.

A125, page 51 of 70

A&A 534, A125 (2011)Ta

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...

...

6310±

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...

.10

2083

4571

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...

...

.71

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4.01

...

...

4.0±

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...

...

1021

3987

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...

...

...

7830±

290a

3.94

...

...

3.9±

0.3a

...

...

1025

3943

7740

...

...

...

7740±

290a

3.70

...

...

3.7±

0.3a

...

...

1025

4547

5880

...

...

...

5880±

290a

4.84

...

...

4.8±

0.3a

...

...

1026

4728

7790

...

...

...

7790±

290a

3.85

...

...

3.9±

0.3a

...

...

1026

6959

5050

...

...

...

5050±

290a

4.40

...

...

4.4±

0.3a

...

...

1027

3246

6070

6300±

120b

...

...

6300±

120b

4.15

4.54±

0.21

b..

.4.

54±

0.21

b..

...

.10

2733

8469

7062

20±

110b

...

...

6220±

110b

3.96

3.79±

0.25

b..

.3.

79±

0.25

b..

...

.10

2739

6066

6064

60±

130b

...

...

6460±

130b

4.44

4.13±

0.22

b..

.4.

13±

0.22

b..

...

.10

2742

4452

10..

...

...

.52

10±

290a

4.53

...

...

4.5±

0.3a

...

...

1028

1360

7530

...

...

...

7530±

290a

4.05

...

...

4.1±

0.3a

...

...

1028

9211

7900

...

...

...

7900±

290a

3.73

...

...

3.7±

0.3a

...

...

1033

8279

5400

...

...

...

5400±

290a

4.47

...

...

4.5±

0.3a

...

...

1033

9342

5950

...

...

...

5950±

290a

4.19

...

...

4.2±

0.3a

...

...

1034

0511

5850

...

...

...

5850±

290a

4.40

...

...

4.4±

0.3a

...

...

1034

1072

6300

...

...

...

6300±

290a

4.18

...

...

4.2±

0.3a

...

...

1035

5055

8110

...

...

...

8110±

290a

3.74

...

...

3.7±

0.3a

...

...

1036

1229

6980

...

...

...

6980±

290a

4.03

...

...

4.0±

0.3a

...

...

1038

3933

5100

...

...

...

5100±

290a

4.27

...

...

4.3±

0.3a

...

...

1038

5459

6920

...

...

...

6920±

290a

4.23

...

...

4.2±

0.3a

...

...

1038

9037

4710

...

...

...

4710±

290a

2.19

...

...

2.2±

0.3a

...

...

1039

4332

4920

...

...

...

4920±

290a

4.47

...

...

4.5±

0.3a

...

...

1044

8764

7400

...

...

...

7400±

290a

4.00

...

...

4.0±

0.3a

...

...

1045

0550

4970

...

...

...

4970±

290a

3.63

...

...

3.6±

0.3a

...

...

1045

0675

6420

...

...

...

6420±

290a

4.12

...

...

4.1±

0.3a

...

...

1045

1090

7580

7640±

60g

...

...

7640±

60g

4.13

3.74±

0.19g

...

3.74±

0.19g

44±

2g..

.10

4512

5056

50..

...

...

.56

50±

290a

4.06

...

...

4.1±

0.3a

...

...

1045

3475

5200

...

...

...

5200±

290a

4.47

...

...

4.5±

0.3a

...

...

1046

7969

8850

...

...

...

8850±

290a

4.09

...

...

4.1±

0.3a

...

...

1047

1914

7290

...

...

...

7290±

290a

3.95

...

...

4.0±

0.3a

...

...

1048

4808

8140

...

...

...

8140±

290a

3.99

...

...

4.0±

0.3a

...

...

1052

6137

3180

...

...

...

3180±

290a

...

...

...

...

...

...

1052

6615

6080

...

...

...

6080±

290a

4.62

...

...

4.6±

0.3a

...

...

1053

3506

6510

...

...

...

6510±

290a

4.18

...

...

4.2±

0.3a

...

...

1053

3616

8320

...

...

...

8320±

290a

3.77

...

...

3.8±

0.3a

...

...

1053

4629

6070

...

...

...

6070±

290a

3.94

...

...

3.9±

0.3a

...

...

1053

6147

1249

020

800±

0f..

...

.20

800±

290f

5.89

3.8f

...

3.8±

0.3f

195±

10f

...

1053

7907

7500

...

...

...

7500±

290a

3.45

...

...

3.4±

0.3a

...

...

1054

9292

7740

...

...

...

7740±

290a

3.94

...

...

3.9±

0.3a

...

...

1054

9371

6970

...

...

...

6970±

290a

3.95

...

...

4.0±

0.3a

...

...

1058

6837

7020

...

...

...

7020±

290a

4.23

...

...

4.2±

0.3a

...

...

1059

0857

7560

...

...

...

7560±

290a

3.76

...

...

3.8±

0.3a

...

...

A125, page 52 of 70


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...

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...

1061

5125

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...

...

...

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3.59

...

...

3.6±

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...

...

1064

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...

...

...

...

...

...

...

...

...

...

...

1064

7611

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...

...

...

7130±

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...

...

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...

...

1064

7860

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...

...

...

5460±

290a

4.61

...

...

4.6±

0.3a

...

...

1064

8728

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...

...

...

6600±

290a

4.08

...

...

4.1±

0.3a

...

...

1065

2134

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...

...

...

6880±

290a

4.17

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...

4.2±

0.3a

...

...

1065

8302

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...

3.9±

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...

...

1065

8802

7480

...

...

...

7480±

290a

4.11

...

...

4.1±

0.3a

...

...

1066

3892

5960

6020±

100b

...

...

6020±

100b

4.32

4.9±

0.2b

...

4.9±

0.2b

...

...

1066

4703

7630

...

...

...

7630±

290a

3.65

...

...

3.7±

0.3a

...

...

1066

4975

7950

6641±

123e

...

...

6641±

123e

3.58

...

...

3.6±

0.3a

...

...

1067

5762

7220

...

...

...

7220±

290a

3.59

...

...

3.6±

0.3a

...

...

1068

4587

7290

...

...

...

7290±

290a

3.83

...

...

3.8±

0.3a

...

...

1068

4673

7110

...

...

...

7110±

290a

3.91

...

...

3.9±

0.3a

...

...

1068

5653

7970

...

...

...

7970±

290a

3.90

...

...

3.9±

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...

...

1068

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7270

...

...

...

7270±

290a

3.95

...

...

4.0±

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...

...

1070

9716

6050

...

...

...

6050±

290a

4.35

...

...

4.4±

0.3a

...

...

1071

3398

...

...

...

...

...

...

...

...

...

...

...

1071

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...

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7290±

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3.50

...

...

3.5±

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...

...

1072

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...

...

5370±

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4.18

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...

4.2±

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...

...

1073

0618

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...

...

...

6200±

290a

4.22

...

...

4.2±

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...

...

1077

5968

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...

...

7490±

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3.84

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...

3.8±

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...

...

1077

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...

...

...

...

...

...

...

...

...

...

1077

7903

7320

...

...

...

7320±

290a

3.53

...

...

3.5±

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...

...

1077

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...

...

...

6390±

290a

4.16

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...

4.2±

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...

...

1078

3150

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...

...

...

7340±

290a

3.93

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...

3.9±

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...

...

1078

8451

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...

...

...

8790±

290a

4.02

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...

4.0±

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...

1079

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3.2±

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...

1079

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...

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6020±

290a

4.20

...

...

4.2±

0.3a

...

...

1081

3970

7420

...

...

...

7420±

290a

3.61

...

...

3.6±

0.3a

...

...

1081

5466

8310

...

...

...

8310±

290a

3.86

...

...

3.9±

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...

...

1085

3783

7830

...

...

...

7830±

290a

3.88

...

...

3.9±

0.3a

...

...

1086

1649

5900

...

...

...

5900±

290a

4.18

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...

4.2±

0.3a

...

...

1090

2738

4640

...

...

...

4640±

290a

2.47

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...

2.5±

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...

...

1092

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...

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5930±

290a

4.24

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...

4.2±

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...

...

1092

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5570±

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4.09

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...

4.1±

0.3a

...

...

1092

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...

...

...

7900±

290a

3.98

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...

4.0±

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...

...

1097

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...

...

...

5530±

290a

4.31

...

...

4.3±

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...

...

1097

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...

...

...

7780±

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...

...

...

3.9±

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...

...

1097

7859

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70g

...

...

8190±

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3.94

3.61±

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...

3.61±

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4.00

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...

4.0±

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...

...

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7780

7200±

200p

...

...

7200±

200p

3.82

3.5±

0.2p

...

3.5±

0.2p

100p

...

A125, page 53 of 70

A&A 534, A125 (2011)Ta

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4.3±

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1102

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...

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7320±

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4.15

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...

4.2±

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...

1102

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...

6850±

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...

3.9±

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...

...

1106

7972

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...

...

...

5990±

290a

4.46

...

...

4.5±

0.3a

...

...

1106

9435

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...

...

...

5590±

290a

4.55

...

...

4.6±

0.3a

...

...

1108

2830

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...

...

...

7020±

290a

3.96

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...

4.0±

0.3a

...

...

1109

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7710

...

...

...

7710±

290a

3.71

...

...

3.7±

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...

...

1112

2763

6530

...

...

...

6530±

290a

4.28

...

...

4.3±

0.3a

...

...

1112

5764

7980

...

...

...

7980±

290a

3.85

...

...

3.9±

0.3a

...

...

1112

7190

7630

...

...

...

7630±

290a

3.72

...

...

3.7±

0.3a

...

...

1112

8041

5670

...

...

...

5670±

290a

4.47

...

...

4.5±

0.3a

...

...

1112

8126

5940

...

...

...

5940±

290a

4.32

...

...

4.3±

0.3a

...

...

1112

9289

5990

...

...

...

5990±

290a

4.31

...

...

4.3±

0.3a

...

...

1118

0361

8330

...

...

...

8330±

290a

3.55

...

...

3.6±

0.3a

...

...

1118

2716

5390

...

...

...

5390±

290a

4.22

...

...

4.2±

0.3a

...

...

1118

3399

7260

...

...

...

7260±

290a

4.03

...

...

4.0±

0.3a

...

...

1118

3539

7470

...

...

...

7470±

290a

3.51

...

...

3.5±

0.3a

...

...

1119

3046

8170

...

...

...

8170±

290a

3.70

...

...

3.7±

0.3a

...

...

1119

7934

7860

...

...

...

7860±

290a

3.68

...

...

3.7±

0.3a

...

...

1119

9412

7470

...

...

...

7470±

290a

3.70

...

...

3.7±

0.3a

...

...

1123

0518

6140

...

...

...

6140±

290a

4.38

...

...

4.4±

0.3a

...

...

1123

2922

...

...

...

...

...

...

...

...

...

...

...

1123

3189

...

...

...

...

...

...

...

...

...

...

...

1123

4888

5940

...

...

...

5940±

290a

4.33

...

...

4.3±

0.3a

...

...

1123

5721

5740

...

...

...

5740±

290a

4.33

...

...

4.3±

0.3a

...

...

1123

6253

5430

...

...

...

5430±

290a

4.45

...

...

4.5±

0.3a

...

...

1124

0653

6460

...

...

...

6460±

290a

4.12

...

...

4.1±

0.3a

...

...

1125

3226

6470

6736±

75c

6800±

400h

6622±

0o67

36±

75c

4.18

4.2±

0.1h

...

4.2±

0.1h

19±

1h..

.11

2857

6774

60..

...

...

.74

60±

290a

3.65

...

...

3.7±

0.3a

...

...

1128

8686

...

...

...

...

...

...

...

...

...

...

...

1129

0197

6340

...

...

...

6340±

290a

4.30

...

...

4.3±

0.3a

...

...

1130

9335

7280

...

...

...

7280±

290a

3.86

...

...

3.9±

0.3a

...

...

1134

0063

4900

...

...

...

4900±

290a

3.10

...

...

3.1±

0.3a

...

...

1134

0713

...

...

...

...

...

...

...

...

...

...

...

1134

2032

...

...

...

...

...

...

...

...

...

...

...

1139

3580

3850

...

...

...

3850±

290a

4.45

...

...

4.5±

0.3a

...

...

1139

4216

5140

...

...

...

5140±

290a

4.19

...

...

4.2±

0.3a

...

...

1139

5018

5420

5740±

80b

...

...

5740±

80b

4.47

3.65±

0.24

b..

.3.

65±

0.24

b..

...

.11

3950

2853

2057

20±

80b

...

...

5320±

290a

4.42

4.26±

0.23

b..

.4.

26±

0.23

b..

...

.11

3953

92..

...

...

...

...

...

...

...

...

...

...

.11

4029

51..

.71

50±

120i

7250±

100k

...

7250±

100k

...

3.5±

0.1i

3.5±

0.1k

3.5±

0.1k

100±

2i..

.11

4457

7461

1062

10±

110b

...

...

6210±

290b

4.33

4.64±

0.20

b..

.4.

6±

0.2b

...

...

A125, page 54 of 70


ble

2.co

ntin

ued.

Te!

(K)

logg

(dex

)v

sin

i(km

s"1 )

KIC

IDK

ICa

Lite

ratu

reL

itera

ture

Lite

ratu

reA

dopt

ed$

KIC

aL

itera

ture

Lite

ratu

reA

dopt

ed$

Spec

tra

Spec

tra

1144

5913

6950

7200±

120i

7250±

100k

...

7250±

100k

3.89

3.5±

0.2i

3.5±

0.2k

3.5±

0.2k

51±

1k..

.11

4461

4343

00..

...

...

.43

00±

290a

4.47

...

...

4.5±

0.3a

...

...

1144

6181

5770

...

...

...

5770±

290a

4.38

...

...

4.4±

0.3a

...

...

1144

7883

6690

6800±

400h

...

...

6690±

290a

4.07

4.2±

0.1h

...

4.2±

0.1h

105±

3h..

.11

4479

5364

10..

...

...

.64

10±

290a

4.43

...

...

4.4±

0.3a

...

...

1144

8266

5980

6110±

110b

...

...

6110±

110b

4.27

4.69±

0.20

b..

.4.

7±

0.2b

...

...

1144

9931

5940

6130±

110b

...

...

6130±

110b

4.52

4.84±

0.20

b..

.4.

8±

0.2b

...

...

1145

4008

6870

...

...

...

6870±

290a

3.79

...

...

3.8±

0.3a

...

...

1149

4765

7050

...

...

...

7050±

290a

3.99

...

...

4.0±

0.3a

...

...

1149

7012

7660

...

...

...

7660±

290a

3.87

...

...

3.9±

0.3a

...

...

1149

8538

6290

6410±

70c

6450±

80g

6441±

0o64

10±

70c

4.04

3.30±

0.41g

...

3.3±

0.3g

40±

1g45

o

1149

9354

5780

6020±

100b

...

...

6020±

100b

4.47

4.39±

0.22

b..

.4.

39±

0.22

b..

...

.11

4994

5358

10..

...

...

.58

10±

290a

4.38

...

...

4.4±

0.3a

...

...

1150

2075

3980

...

...

...

3980±

290a

4.57

...

...

4.6±

0.3a

...

...

1150

8397

7460

...

...

...

7460±

290a

3.52

...

...

3.5±

0.3a

...

...

1150

9728

7790

...

...

...

7790±

290a

3.73

...

...

3.7±

0.3a

...

...

1151

5690

6460

...

...

...

6460±

290a

4.11

...

...

4.1±

0.3a

...

...

1154

9609

5580

...

...

...

5580±

290a

4.56

...

...

4.6±

0.3a

...

...

1155

1622

5690

...

...

...

5690±

290a

4.50

...

...

4.5±

0.3a

...

...

1157

2666

7040

...

...

...

7040±

290a

3.49

...

...

3.5±

0.3a

...

...

1160

2449

7390

...

...

...

7390±

290a

3.83

...

...

3.8±

0.3a

...

...

1160

7193

7210

...

...

...

7210±

290a

4.14

...

...

4.1±

0.3a

...

...

1161

2274

7470

...

...

...

7470±

290a

3.62

...

...

3.6±

0.3a

...

...

1162

2328

...

...

...

...

...

...

...

...

...

...

...

1165

1083

...

...

...

...

...

...

...

...

...

...

...

1165

1147

6030

...

...

...

6030±

290a

4.48

...

...

4.5±

0.3a

...

...

1165

3958

6620

6450±

120b

...

...

6450±

120b

4.25

4.20±

0.21

b..

.4.

20±

0.21

b..

...

.11

6542

1060

6062

00±

110b

...

...

6200±

110b

4.46

4.63±

0.21

b..

.4.

63±

0.21

b..

...

.11

6578

4061

20..

...

...

.61

20±

290a

4.66

...

...

4.7±

0.3a

...

...

1166

1993

7200

...

...

...

7200±

290a

3.93

...

...

3.9±

0.3a

...

...

1167

1429

7360

...

...

...

7360±

290a

3.58

...

...

3.6±

0.3a

...

...

1170

0370

8290

...

...

...

8290±

290a

3.99

...

...

4.0±

0.3a

...

...

1170

0604

7630

...

...

...

7630±

290a

3.85

...

...

3.9±

0.3a

...

...

1170

6449

...

...

...

...

...

...

...

...

...

...

...

1170

6564

4550

...

...

...

4550±

290a

2.35

...

...

2.4±

0.3a

...

...

1170

7341

4210

...

...

...

4210±

290a

4.58

...

...

4.6±

0.3a

...

...

1170

8170

6640

6776±

79c

6918±

0d67

14±

0o67

76±

79c

4.15

4.21±

0.07

d..

.4.

21±

0.07

d..

...

.11

7141

5082

70..

...

...

.82

70±

290a

3.87

...

...

3.9±

0.3a

...

...

1171

8839

8260

...

...

...

8260±

290a

3.78

...

...

3.8±

0.3a

...

...

1175

3169

7210

...

...

...

7210±

290a

3.94

...

...

3.9±

0.3a

...

...

1175

4974

...

...

...

...

...

...

...

...

...

...

...

1182

1140

8050

...

...

...

8050±

290a

3.85

...

...

3.9±

0.3a

...

...

1182

2666

8440

...

...

...

8440±

290a

3.87

...

...

3.9±

0.3a

...

...

A125, page 55 of 70

A&A 534, A125 (2011)

Tabl

e2.

cont

inue

d.

Te!

(K)

logg

(dex

)v

sin

i(km

s"1 )

KIC

IDK

ICa

Lite

ratu

reL

itera

ture

Lite

ratu

reA

dopt

ed$

KIC

aL

itera

ture

Lite

ratu

reA

dopt

ed$

Spec

tra

Spec

tra

1182

4964

7190

...

...

...

7190±

290a

3.97

...

...

4.0±

0.3a

...

...

1187

4676

8220

...

...

...

8220±

290a

4.00

...

...

4.0±

0.3a

...

...

1187

4898

7010

6650±

130b

...

...

6650±

130b

3.96

3.72±

0.22

b..

.3.

72±

0.22

b..

...

.11

9102

5671

30..

...

...

.71

30±

290a

3.53

...

...

3.5±

0.3a

...

...

1191

0642

7660

...

...

...

7660±

290a

3.59

...

...

3.6±

0.3a

...

...

1197

3705%

7400

1189

8±

0f73

00±

300i

1115

0±

0j11

150±

290j

4.04

4.2±

0.3i

3.96

j4.

0±

0.3j

120±

20i

103±

10j

1201

8834

7270

...

...

...

7270±

290a

4.00

...

...

4.0±

0.3a

...

...

1202

0590

8020

...

...

...

8020±

290a

3.67

...

...

3.7±

0.3a

...

...

1205

8428

7110

...

...

...

7110±

290a

3.99

...

...

4.0±

0.3a

...

...

1206

2443

7380

...

...

...

7380±

290a

3.97

...

...

4.0±

0.3a

...

...

1206

8180

7460

...

...

...

7460±

290a

3.78

...

...

3.8±

0.3a

...

...

1210

2187

7030

...

...

...

7030±

290a

4.13

...

...

4.1±

0.3a

...

...

1211

7689

6910

...

...

...

6910±

290a

4.09

...

...

4.1±

0.3a

...

...

1212

2075

7120

...

...

...

7120±

290a

3.89

...

...

3.9±

0.3a

...

...

1221

6817

6680

...

...

...

6680±

290a

3.81

...

...

3.8±

0.3a

...

...

1221

7281

7130

...

...

...

7130±

290a

3.71

...

...

3.7±

0.3a

...

...

1235

3648

7410

7190±

45g

...

...

7190±

45g

3.47

3.60±

0.26g

...

3.60±

0.26g

189±

12g

...

1264

7070

7280

...

...

...

7280±

290a

3.87

...

...

3.9±

0.3a

...

...

1278

4394

7850

...

...

...

7850±

290a

3.61

...

...

3.6±

0.3a

...

...

Not

es.(%

)Sp

ectr

osco

pic

bina

ry;

valu

esde

rived

from

phot

omet

ry:

(a)

KIC

Cat

alog

ue,L

atha

met

al.(

2005

);(b

)SP

Mph

otom

etry

,thi

spa

per;

(c)

Mas

ana

etal

.(20

06);

(d)

Alle

nde

Prie

to&

Lam

bert

(199

9);(e

)H

auck

&M

erm

illio

d(1

998)

;val

ues

deriv

edfr

omph

otom

etry

orsp

ectr

osco

py:(f

)B

alon

aet

al.(

2011

b);v

alue

sde

rived

from

spec

tros

copy

:(g)

TL

Ssp

ectr

a,th

ispa

per;

(h)

SOPH

IEsp

ectr

a,th

ispa

per;

(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

reta

l.(2

011)

;(n)

Gle

bock

i&St

awik

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

estim

ated

erro

rson

the

KIC

valu

esar

e29

0K

forT

e!an

d0.

3de

xfo

rlogg

(see

text

).

A125, page 56 of 70


ble

3.C

lass

ifica

tion

and

char

acte

riza

tion

of"

Sct,!

Dor

,and

hybr

idst

ars.

KIC

IDC

lass

NN!

Dor

N"S

ctN

tota

l(F

req

Ran

ge) !

Dor

(Fre

qR

ange

) "Sc

tA

mpl

itude

high

Freq

high

Flag

(d"1

)(d"1

)(p

pm)

(d"1

)"

Scts

tars

0116

2150

"Sc

t13

60

136

204

...

[4.0

,35.

5]18

5716

.408

...

0157

1717

"Sc

t98

098

126

...

[5.4

,56.

5]76

741

.235

•01

7185

94"

Sct

530

5313

9..

.[5

.4,7

6.1]

1674

18.3

28..

.02

3033

65"

Sct

370

3716

2..

.[5

.0,3

4.8]

7340

14.8

06..

.02

4396

60"

Sct

360

3651

...

[15.

9,79

.5]

829

42.9

67..

.02

5718

68"

Sct

189

018

934

5..

.[4

.0,5

2.7]

1766

20.5

50..

.02

5723

86"

Sct

120

1259

...

[9.1

,12.

1]10

919.

481

•02

9876

60"

Sct

186

018

653

7..

.[4

.3,6

4.0]

3610

15.0

49..

.03

2175

54"

Sct

138

013

844

6..

.[4

.0,5

6.1]

2407

5.60

4..

.03

2192

56"

Sct

355

035

553

2..

.[4

.0,7

9.7]

1431

17.8

57..

.03

3476

43"

Sct

930

9316

4..

.[4

.2,6

8.2]

654

29.6

95..

.03

4258

02"

Sct

160

1630

...

[24.

3,44

.4]

643

31.6

93..

.03

4296

37"

Sct

180

1829

...

[9.3

,19.

4]16

4010

.338

...

0344

0495

"Sc

t8

08

9..

.[4

.1,2

1.7]

332

15.9

73..

.03

4583

18"

Sct

160

1647

...

[7.0

,23.

0]11

4713

.490

...

0355

8145

"Sc

t81

081

140

...

[4.0

,44.

2]28

9122

.122

...

0363

4384

"Sc

t20

80

208

573

...

[4.4

,68.

7]15

8411

.648

...

0364

4116

"Sc

t75

075

95..

.[6

.5,4

2.6]

1325

30.0

22..

.03

6555

13"

Sct

120

1246

...

[5.2

,12.

6]28

488.

333

...

0376

0002

"Sc

t86

086

159

...

[7.3

,33.

1]22

4616

.260

...

0376

1641

"Sc

t62

062

149

...

[11.

6,74

.6]

506

37.3

07..

.03

8508

10"

Sct

104

010

442

2..

.[4

.5,5

1.1]

1936

14.4

62..

.03

9412

83"

Sct

114

011

417

3..

.[9

.4,6

9.1]

1067

33.2

70..

.03

9429

11"

Sct

190

019

029

5..

.[4

.3,5

2.9]

1220

29.4

90..

.04

0356

67"

Sct

310

3178

...

[4.8

,79.

0]55

246

.399

...

0404

8494

"Sc

t87

087

254

...

[9.9

,42.

0]47

0114

.364

...

0407

7032

"Sc

t27

40

274

869

...

[4.6

,75.

8]37

0714

.482

...

0416

8574

"Sc

t43

042

139

...

[4.4

,18.

9]14

957.

989

...

0425

2757

"Sc

t13

50

135

332

...

[5.0

,36.

5]39

6121

.480

...

0426

9337

"Sc

t10

60

106

297

...

[5.0

,69.

1]15

5235

.215

•04

3831

17"

Sct

110

1112

...

[22.

8,45

.1]

399

26.2

59..

.04

6477

63"

Sct

142

014

249

4..

.[4

.1,7

4.2]

3973

23.7

17..

.04

6494

76"

Sct

880

8819

5..

.[4

.3,4

6.7]

1544

20.6

99..

.04

8406

75"

Sct

490

4963

...

[4.5

,47.

4]11

6822

.069

...

0485

6630

"Sc

t12

40

124

373

...

[4.4

,48.

7]26

8019

.582

...

0486

3077

"Sc

t16

00

160

631

...

[4.1

,40.

9]23

9920

.992

...

0490

9697

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.

A125, page 57 of 70

A&A 534, A125 (2011)Ta

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A125, page 58 of 70


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A125, page 59 of 70

A&A 534, A125 (2011)Ta

ble

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ntin

ued.

KIC

IDC

lass

NN!

Dor

N"S

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A125, page 60 of 70


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A125, page 61 of 70

A&A 534, A125 (2011)Ta

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A125, page 62 of 70


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.

A125, page 63 of 70

A&A 534, A125 (2011)Ta

ble

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ntin

ued.

KIC

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lass

NN!

Dor

N"S

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A125, page 64 of 70


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A125, page 65 of 70

A&A 534, A125 (2011)Ta

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A125, page 66 of 70


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A125, page 70 of 70

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