telluric spectra 4690a-5525a

8/4/2019 Telluric Spectra 4690a-5525a

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Vol. 73, No. 8/August 1983/J. Opt. Soc. Am. 999

Telluric spectra from 4690 o 5525A in a humid atmosphereA. Rajaratnam and K.T. Lua

Department of Physics,National University of Singapore, Kent Ridge,Singapore 0511Received August 28, 1981; revised manuscript received March 29, 1983

Solar spectra in the region 4690 to 5525 A have been taken with a 4.5-m high-resolution grating spectrograph fordifferent solar zenith angles. Three-hundred eighty-five telluric lines were measured, and their wavelengths, half-intensity widths, equivalent widths, and identifications are reported.

INTRODUCTIONA large number of telluric lines have been measured and listedin the tables of solar spectrum wavelengths of Moore et al.,'Swensson et al. ,2 and Migeotte et al.3 In the 1978edition ofthe Air Force Geophysics Laboratory's (AFGL's) atmo-spheric-absorption line parameters compilation (see Refs. 4and 5), 139,000 transitions arising from atmospheric absorp-tion covering 0.3-17 880 cm- 1 were included. A compre-hensive review of the absorption of solar radiation by atmo-spheric gases was given by Laulainen. 6However, most of the measurements on atmospheric ab-sorption was done at low or medium resolution (see, e.g., Ref.7), whereas, for those done at high resolution, the primaryobjective was to study the stellar atmospheres, and observa-tions were mostly made at high-altitude observatories to avoidatmospheric water vapor.The atmospheric-absorption parameters listed in the AFGLcompilations4 5 were derived from high-resolution measure-ments made at large solar zenith angles so as to detect moretelluric lines. However, this listing ends at 17 880 cm-'.Singapore, having one of the world's most humid atmo-spheres, has for its vertical atmospheric column on the average5-cm precipitable water vapor. During late afternoons, whenthe relative air mass increases to 30 or more, the atmosphericwater-vapor path length is more than 150 cm of H20.In view of this, Singapore provides an ideal site for studyingthe atmospheric water-vapor absorption.In this paper we report the detection of telluric lines in thespectral region of 4690 to 5525 A (21 313 to 18 095 cm-1 ).EXPERIMENTAL DETAILSThe image of the solar disk was stabilized with an equato-rial-mount coelostat system installed on top of a light towersituated at one end of our laboratory building. The collectorwas a 200-mm-diameter parabolic mirror of 3.5-m focal lengthgiving a solar image of around 30 mm. The solar spectra werephotographed with a 4.5-m plane-grating spectrograph at aresolution of 306 000 at second order. Overlapping of dif-ferent orders was avoided by using bandpass color filters.The solar spectra were taken at an instrumental dispersionof 0.68 mm/A at secondorder. An optimum slit width of 20Am was used throughout the whole experiment. The slitheight was set at 6 mm. Exposure times varied from fractionsof a second to a few minutes.

Solar spectra were taken for different solar zenith angles.The spectra for the setting sun (maximum solar zenith angle)were the most valuable as many weak telluric lines that failedto appear earlier were well developed on these spectra.Whereas most of the spectra were taken at the center of thesolar disk, a number of spectra were also taken from the eastand west limbs of the solar image.The position of the spectral lines were measured by usingan Abb6 comparator, and their intensities were evaluated fromthe densitometric tracing made from a Jarrell-Ash micro-densitometer. A portion of the microdensitometer tracingof the solar spectrum around 5018 A is shown in Fig. 1.

DEDUCTION OF WAVELENGTHThe wavelengths of solar lines listed in Ref. 1 were used asreference. For computing wavelengths, a least-squaresmethod similar to that employed by Pierce and Breckinridge8was used. Wavelengths (X) of the identified solar lines andtheir positions (x) were fitted to a third-degree polynomial,i.e.,

X=a +ax +a2x2 +a3x3, (1)where ao, a1 , a2, and a 3 were constants, and the standard de-viation of fitting o-was computed. The polynomial constantsao, a 1, a2, and a3 were used with the comparator readings (x)to compute the wavelength for every measured line.

As our solar image was only 30 mm in diameter, it was notpossible to ensure that solar spectra were taken at the exactcenter of the solar image, and telluric wavelengths obtainedfrom Eq. (1) (by using solar wavelengths as standards) wereshifted by an amount rX, which was given bybX = XA- X, (2)

where Asand Xrepresent the Doppler-shifted and -unshiftedwavelengths, respectively, for any spectral line. A quantitys is defined as

s= &/X. (3)It was noted that s was a constant for any single spectralexposure as s = v/c, where v was the average radial velocityof the solar atmosphere toward the earth and c was the ve-locity of light.As there were frequently a large number of known telluriclines on a spectral plate, several values of s were derived and

0030-3941/83/080999-13$01.00 1983 Optical Society of America

A. Rajaratnam and K. T. Lua


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1000 J. Opt. Soc. Am.IVol. 73, No. 8/August 1983

C:0UGD

a)04-'0L.UM

I itLA9l-

LAI-Co9-

ColLO

Ei ;r

0iLi-SStC)LO .-

C)CJLO

0U-co(I?

LO

Ga,tCJ

EEto.

Fig. 1. Microdensitometric tracing of solar spectrum around 5018 A. Telluric lines are marked atm.their average(s) computed. In this calculation, XAwas thewavelength of a known telluric line computed from Eq. (1) (inwhich solar wavelengths from Ref. 1 were used as standards)and X was the wavelength of the same telluric line, which wasalso obtained from Ref. 1. Wavelengths of new telluric lines[as obtained from Eq. (1)] were then corrected accordingly byusing Eqs. (2) and (3).

INTENSITY MEASUREMENTAs the response of the photographic emulsion is stronglywavelength dependent,- a calibrated seven-step neutral-den-sity filter was used in front of the spectrograph slit. Intensitycalibration was performed every 50 A throughout the entirespectral region.The half-intensity widths (HW's) of the spectral lines weremeasured with a scale placed on top of the microdensitometrictracing of the solar spectra. The widths were then convertedto wavelength units (milliangstroms) according to the lineardispersion of the spectrum. The equivalent widths (EW's)were estimated from the product of peak percentage absorp-tions (A) and the HW's, i.e.,

EW= A X HW, (4)where

Io - IA (5)IoPRECISION OF MEASUREMENTPrecision of Wavelength MeasurementAlthough the Abb6 comparator used in measuring line posi-tions was able to provide readings accurate to 0.1 Am (equiv-

-E Aalent to 0.15 mA at 5000A), the precision of the positionmeasurement was much lower because of the difficulty inascertaining the spectral line center (especially or faint lines)and also the stability of the reference solar lines. The solaratmosphere is never at rest. Direct measurements9 of themean random velocity of solar granules leads to a value of 370m/sec, which alone may cause a Doppler displacement of 6.2mA at 5000A. This would not only broaden the solar linesused as standards but may also shift the centers of the solarlines in some direction if there is an instantaneous directionalmovement of the solar atmosphere when the spectrum istaken. Fortunately, because of the smallness of the solarimage, with a slit size of 20 um X 6 mm, there was enoughaveraging to avoid this instantaneous directional movementof the solar lines. However, even if this movement did occur,the effect would have been absorbed in the Doppler-shiftcorrection, which was mentioned earlier.The Doppler-shift correction led to a further error in thewavelength measurement. The average standard deviationin s was found to be 0.67 X 10-6, which is equivalent to 3.4 mAat 5000 A.As all spectral lines were measured four to ten times, stan-dard deviations of the wavelength measurement (S) wereobtained. They had an average value of 5.3 mA for wave-lengths measured to 0.001A (394 lines) and 23 mA for thosemeasured to 0.01A (77 lines).The internal consistency of the wavelength measurementcan be deduced from the combination differences applyingto the identified water-vapor lines. The difference betweenthe calculated wave numbers (based on the derived energylevels'1 ) and the measured wave numbers has an average valueof 0.020 cm- 1 , which is equivalent to 5.8 mA at 18 390 cm' 1 .The line at 18 250.77 cm-' has not been included in this cal-culation since it consists of three unresolved water-vaporlines.



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Vol. 73, No. 8/August 1983/J. Opt. Soc. Am. 1001Table 1. Ratio of Equivalent Widths Measured inThis Work to Those Measured by Moore et aLa

Spectral Region (A) b4689-4855 0.84 + 0.084855-5231 0.93 0.085231-5410 0.93 i 0.095409-5684 0.85 0.135684-5977 0.84 i 0.095977-6015 0.88 i 0.01

Average 0.88 + 0.08a Ref.1.

Precision of Intensity MeasurementThe HW's of 118spectral lines were randomly selected andmeasured twice (fromdifferent spectra) and their deviationscalculated. The average deviation was found to be 3.9% of themeasured widths. This amounts to 5 mA on the wavelengthscale for an average HW of 136 mA.Another 103 telluric lines were again randomly selected, andthe EW's were computed twice (from different spectra).Again,it wasfound that they agreedwith eachother to within9.6%.The reliability of the intensity measurement was also testedby comparing intensities of solar lines measured in this workwith those given in Ref. 1, assuming that intensities of solarlines remain consistently unchanged.A ratio b is defined as

EW (this measurement)b = * 6)EW (Ref. 1)It was found that b has an average value of 0.88 0.08 (see

Table 1). This is not unexpected since it is well known thatthe equivalent width of a Voigt function' 0 is given by the ex-pression in Eq. (4) multiplied by aconstant that variesfrom1.06 for a pure Gaussian line to 1.57 for a pure Lorentzian line.For solar lines, a typical value of 1.12 is applied. If this factoris applied to b, it becomes 0.986, which indicates that thepresent measurements are, on the average, within 1.4% ofthose listed in Ref. 1.CLASSIFICATION OF SPECTRAL LINESA spectral line was classified as telluric, i.e., arising from theabsorption of the earth's atmosphere, provided that

(1) It did not showa Doppler shift as solar spectra fromthe east and west limbs of the solar imageswere compared.(2) It exhibited a significant intensity enhancement assolar spectra of low sun were compared with those taken atnoon.An analysis of the vibrational-rotational spectrum of thewater vapor has been carried out, and 65 spectral lines werefound to originate from the absorption of atmospheric watervapor. The details of the analysis have been reported else-where."

TABLE OF TELLURIC WAVELENGTHS FROM4690 TO 5525 AOur table of telluric wavelengths contains 471 telluric linesconverting the spectral region 4690 to 5525 A (see Table 2).The entries in the columnsof the table are explained as fol-lows:

Table 2. Telluric Wavelengths from 4690to 5525A(1) (2) (3) (4) (5) (6) (7) (8) (9)Standard WaveWavelength Deviation Number HW EWNo. (A) (mA) (cm) (mA) (mA) Origin Band Transition Remark

4690.798(3)Ti I

4696.38(4)C24696.622(4)C 2

4720.133(3.5)Fe IIp

4850.201(1.5)Cr I?

21 4851.13722 4851.885 5 20607.965 20604.79 85 3 ATM131 25 ATM

12345678910

11121314151617181920

4690.724690.8284694.5234695.544696.4274696.6414696.8014702.014710.7754711.3154720.2204721.9124832.3154833.724835.5174846.0814850.0564850.194850.3304850.711

60562447914765S9164681257

21312.7221312.2321295.4621290.8421286.8221285.8521285.1321261.5521221.9921219.5621179.5221171.9420688.2320682.2220674.5320629.4620612.5620611.9920611.3920609.77

1057419610096131105103

786510413915711913114497144

85161

12619921

131715113121316129

84775

ATMATMATMATMATMATMATMATMATMATMUIATMU'UIUIUIATMATMATMATM

(continuedverleaf)



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1002 J. Opt. Soc. Am./Vol. 73, No. 8/August 1983

Table 2. Continued(1) (2) (3) (4) (5) (6) (7) (8) (9)Standard WaveWavelength Deviation Number HW EWNo. (A) (mA) (cm) (mA) (mA) Origin Band Transition Remark

23242526272829303132333435363738394041424344454647484950515253545556575859606162636465666768697071727374757677

4852.7774853.0474853.1444854.4864856.8114861.024861.5254863.0774864.914864.974868.6704868.7424868.9424877.7884889.7394889.8874895.614900.5154904.064904.764904.9004907.494908.874915.084994.8314997.7414999.8145001.6715002.125006.9835007.5075009.0465009.7805011.6565015.9225016.6905017.0715018.0865018.6215018.7435019.1325019.2625019.4965020.2175020.3715024.3205024.5875025.8725206.1675026.6195028.4885028.7485029.2305029.3345029.481

4 19877.807 19877.22

127199937691696987

58521628

382

UIATMATMATMATMATMATMUI

4864.85(2)V I p39 10 UIUI78 2 UI100 3 UI100 13 ATM

45752

30866422

765876407

122262315354763

247657

20601.0020599.8520599.4420593.7520583.8920566.0720563.9320557.3720549.6220549.3720533.7520533.4520532.6020495.3720445.2820444.6620420.7620400.3220385.5720382.6620382.0820371.3220365.6020339.8720015.1120003.4619995.1619987.7419985.9419966.5319964.4419958.3119955.3919947.9219930.9519927.9019926.3919922.3619920.2319919.7519918.2019917.6919916.7619913.9019913.2919897.6419896.5819891.4919202.6419888.5419881.1519880.1219878.21

ATMATMUIATMUIUIUIUIUIUIUIUIATMATMATMATMUIUIUIATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMUIATMUIATM

75 5 ATM100 53 ATM

156869960224

13414211618116411617810297110110189

677192

109104

7312221550831219296

1099279969679

20910975125

5029.484(4.5)MgH

2111628456986345156

144755

1291540

1112201525

5161123232512431316

5017.047(7.5)C 2

5019.22(4)Cr I5019.478(7.5)Fe II?



5/13

Vol. 73, No. 8/August 1983/J. Opt. Soc. Am. 1003Table 2. Continued

(1) (2) (3) (4) (5) (6) (7) (8) (9)Standard WaveWavelength Deviation Number HW EWNo. (A) (mA) (cm) (mA) (mA) Origin Band Transition Remark

5034.057(2)Co I5034.356(7)C2

78798081828384858687888990919293949596979899100

101102103104105106107108109110111112113114115116 5050.481117118119120121122123124125126127128129130

5052.3805053.4785053.8205055.2155056.1655056.2935056.445056.6895056.9675057.5945058.2365059.0175059.5165061.109

131 5062.270132 5065.97

8 19794.57 141 32 ATM768669286277367

19787.1319782.8319781.4919776.0319772.3219771.8219771.2419770.2719769.1819766.7319764.2219761.1719759.2219753.00

1211251121121331331331335011213311291112

5518416

1636871338572132047

ATMATMATMUIATMATMATMATMUIATMATMATMATMATM

5056.126(12)C25056.252(11)C25056.434(12)MgH

6 19748.47 100 12 ATM11 19734.05 137 98 ATM 5065.989(19)Ti i(continuedverleaf)

5030.2905030.4165031.2705032.675033.0855033.2805034.1075034.3235034.5205034.6455034.8795034.9365035.2625035.6045035.6915036.295036.6265036.7815037.275037.705038.2825038.8475039.5205039.7015040.6395041.405041.9005042.9165043.0885043.9655045.3105045.6735045.7825046.3325046.9855047.4475047.6345050.298

478

28553253627752237

262553937

1427744127567756

19874.0219873.5319870.1519864.6219862.9919862.2219858.9519858.1019857.3319856.8319855.9119855.6819854.4019853.0519852.7119850.3519849.0219848.4119846.4819844.7919842.5019840.2719837.6219836.9119833.2219830.2319828.2619824.2719823.5919820.1419814.8619813.4319813.0119810.8519808.2819806.4719805.7419795.29

1171551349688101134

11784847596381421157150

109113117961011091172149612413411314220896

9696112133112

4293825

631506747

410503836841

86956640354140

129377891743926981223

2518

UIUIATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMATMUIATMATMATMATM

5034.991(4)Fe

5036.277(42)Fe I

5037.200(3.5)Atm5037.709(20)C2

5039.774(7)C25040.614(16)Ti

5042.921(8)MgH

5045.270(12)C2

5046.929(4.5)C25047.558(2)C 2



6/13


7/13


(1) (2) (3) (4) (5) (6) (7) (8) (9)Standard WaveWavelength Deviation Number HW EWNo. I (A) (mA) (cm) (mA) (mA) Origin Band Transition Remark188189190191192193194195196197198199200201202203204205206207208209210211212213214215216217218219220221222223224225226227228229230231232233234235236237238239240

5162.2105234.2635236.6375236.8965237.5365240.0305240.1855240.3115240.7945243.495243.5475243.9825244.7385245.1885245.8205246.9135251.125251.4975252.3085254.425254.4695254.745266.3775269.2465269.7765276.9945287.8865290.5905294.3985297.5915301.395304.6115310.3165323.545376.5165380.675382.8535385.8435387.895387.9465388.2005389.875390.2875390.7505392.8135394.1645394.3185395.4485395.7195396.4205397.8805397.955398.540

241 5399.850242 5401.107

63686428227.34446228661864476728

10472465

2242456

17453073788627815

10

19366.1519099.5719090.9119089.9619087.6319078.5519077.9819077.5219075.7619065.9619065.7519064.1719061.4219059.7819057.4919053.5219038.2519036.8919033.9519026.3019026.1219025.1418983.1018972.7618970.8618944.9118905.8818896.2218882.6318871.2518857.7318846.2818826.0318779.2718594.2318579.8818572.3418562.0318554.9818554.7918553.9118548.1618546.7318545.1318538.0418533.4018532.8718528.9918528.0618525.6518520.6418520.4018518.37

124116

74112128120124

9

87669191991579

152

9411098130102146211276140107270151111

9187871319599105106

126118106679155

91049

616141223

114284139109

101814107491793

12151534714158

1325687145

UIU'UIUIUIATMATMATMUIATMUIUIUIATMUIUIATMATMATMATMUIATMATMATMATMATMATMATMATMATMUIATMATMATMUIUIATMATMATMATMATMATMATMATMATMATMH20H20ATMATMH20ATMATM

10 18513.88 106 11 ATM8 18509.57 ? ? H2 0

5162.281(154)Fe5234.213(8)Ndi

5240.359(5)Fe p5240.878(4.5)V I

5251.487(2.5)Ti I

5254.651(7)Co I5266.309(12)Co I

5269.701(?)Fe I

5301.312(3)Fe I p5310.242(3)Co i?5323.507(1)Fe I

5382.755(1)Fe I5385.890(1.5)Nd i

411 633-532411 321-202

411 542-441

5394.200(2)Atm?

5398.519(4.5)Atm?5399.777(5)Co?

411 523-422 (continued verleaf)



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1006 J. Opt. Soc. Am./Vol. 73, No. 8/August 1983Table 2. Continued

(1) (2) (3) (4) (5) (6) (7) (8) (9)Standard WaveWavelength Deviation Number HW EWNo. (A) (mA) (cm) (mA) (mA) Origin Band Transition Remark243 5402.077

244 5402.333

8 18506.25 106 35 H 20H207 18505.37 91 16 ATMATMH20ATMATMATMATMATMATMH20H20H20ATMH20H20

411 532-431411 817-716

411 533-432

5406.337(9)Fe I p411 524-423411 431-330411 533-514411 422-321411 432-311

7 18483.11 111 27 ATM

245246247248249250251252253254255256257258259260261262263264265266267268269270271272273274275276277278279280281282283284285286287288289290291292293294

3 18442.83 114 58 H 20

5408.088(3)Co I?

5408.823(5.5)Fe II

5402.5995403.0825403.4185404.5415404.8935405.0965406.2975406.9345407.1005407.8005408.0315408.0515408.2405408.3905408.8405409.3925409.5025409.9705411.7425411.9905412.1875412.935413.1065413.9205414.1225414.3715414.475414.7625414.965415.0985415.3695415.5505415.6505416.1435416.5925416.6895416.9135417.2485417.485417.635417.9155418.1555418.3035418.4885419.325419.3935419.7245419.875420.2925420.45

411 404-303411 524-505

411 414-313

5414.367(12)H 20

5414.881(5)Fe I p

411 423-404411 322-221

411 707-606411 221-202

411 303-202

411 313-212 5419.393(5)H 2 0

5420.318(?)Mn I5420.412(?)Mn I

411 211-110 5420.622(7)H 20

48286457553459

18504.4618502.8118501.6618497.8118496.6118495.9118491.8018489.6318489.0618486.6618485.8818485.8118485.1618484.65

8783791348771154918351878787

12103227

122315205343426

ATMATMATMATMATMATMATMH20ATMATMH20H20ATMATMH20UIH20ATMH20ATMH20H20ATMUIUIH20ATMATMATMUIH20ATMU'ATMATM

411 606-505 5413.101(18)Atm5414.075(31)Fe II

6623322632532642626663675526222534293820.612

18481.2218480.8518479.2518473.2018472.3518471.6818469.1418468.5418465.7718465.0818464.2318463.8918462.9018462.2218461.7518460.8318460.2118459.8718458.1918456.6618456.3318455.5618454.4218453.6318453.1218452.1518451.3318450.8318450.2018447.3718447.1218445.9918445.5018444.0618443.52

10347831009110111583

14910911810695245

100919358

107848811094951711088941

10913099

197106

?5541810312362126269771210191

1282237

13162218163553

6063

11146

A. Rajaratnam. and K. T. Lua

295 5420.653


9/13


(1) (2) (3) (4) (5) (6) (7) (8) (9)Standard WaveWavelength Deviation Number HW EWNo. (A) (mA) (cm) (mA) (mA) Origin Band Transition Remark296297298299300301302303304305306307308

309310311312313314315316317318

5422.9585423.1005423.455423.535424.0025424.375424.5415424.8595425.7685425.945426.435426.5265426.806

5427.0515427.8775428.3835428.5895428.6355428.6665430.1405430.2635430.8795431.210

411 202-101 5422.951(6.5)H 20

411 212-111411 413-414 5424.544(10)Ni I

363415714552

305045

3659789776

319 5431.38320 5431.597321 5431.78

27 18406.413 18405.67

27 18405.05

? ? UIH2094 32 H2 0H2073 6 ATM

411411411211-212441-440440-441

5431.541(4.5)Nd I

322323324325326327328329330331332333334335336337338339340341342343344

5432.315432.455433.1445433.5985433.7305433.9285434.0405434.1805434.7205434.8435435.4055435.5995436.3405436.8605437.1075437.385438.0005438.1665438.9225439.505439.7775440.235441.144

20153795628353365

26568

173

158

18403.2618402.7818400.4318398.8918398.4518397.7818397.4018396.9218395.1018394.6818392.7818392.1218389.6118387.8518387.0218386.1018384.0018383.4418380.8818378.9318377.9918376.4618373.38

8690

61102122110

89134147931701507769

10197

110113

9

17

285322756168662471

514

543

61513

ATMUIATMATMH20H20ATMH20H20H20H20

I H 2 0H20H20ATMH20{ H 2 0

I H 2 0ATMATMH20ATMATMH20H20

92 52 H 20

5432.33(?)Ti

411 542-541411 110-111411411411411411411411

411411411

422-423330-331331-330321-322633-634220-221431-432

111-110432-431532-533

5436.302(36)Fe I5436.845(1)0 I?

5438.051(2.5)Fe I

411 322-3215439.708(2)Atm

411 533-532411 212-211411 000-101 5442.293(5)H 2 0/Nd II(continued verleaf)

18434.9918434.5118433.3218433.0518431.4418430.1918429.6118428.5318425.4418424.8618423.2018422.8718421.92

18421.0918418.2918416.5718415.8718415.7118415.6118410.6118410.1918408.1018406.98

10653106141

258719583

113110125

19214916110216717211512311557

612915

21618177

6813

281013265059262735

H20UIATMATMH20H20ATMATMATMUIATMATMH20H20ATMUIATMH20ATMH20ATMATMUIATM

411 652-651411 651-652

5427.803(5.5)Fe I411 312-313

411 101-000 5428.707(6)Fe I p


345 5442.298 3 18369.48


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Table 2. Continued(1) (2) (3) (4) (5) (6) (7) (8) (9)Standard WaveWavelength Deviation Number HW EWNo. (A) (mA) (cm) (mA) (mA) Origin Band Transition Remark

5442.420(8.5)Cr I411 423-422

5443.426(3.5)Fe I p

5444.588(14)Co I

346347348349350351352353354355356357358359360361362363364365366367368369370371372373374375376377378379380381382383384385386387388389390391392393394395396397398399

5442.3505443.0415443.1725443.295443.4735443.8165444.0635444.0735444.1985444.5035445.4105445.8505446.0755446.3795447.1105447.285448.1075448.7275448.9265449.0335449.4135449.525450.2705451.1245451.6505451.9655452.3765453.945454.4505455.1165455.2885456.1065456.1915456.3935456.7785457.1725457.4805458.2055458.5285458.7595458.9755459.2325459.4305459.5905459.7625460.0555460.2075460.615461.0165461.8505462.0015462.0445462.4335463.677

985162644457217923155331325482

3273374148343557122S512588566

18369.3118366.9718366.5318366.1318365.5218364.3618363.5318363.4918363.0718362.0418358.9818357.5018356.7418355.7218353.2518352.6818349.9018347.8118347.1418346.7818345.5018345.1418342.6118339.7418337.9718336.9118335.5318330.2718328.5618326.3218325.7418322.9918322.7118322.0318320.7418319.4118318.3818315.9518314.8618314.0918313.3618312.5018311.8418311.3018310.7218309.7418309.2318307.8818306.5218303.7218303.2218303.0718301.7718297.60

14 18296.69 289 38 ATM

10492929

96727272849

9810879

1029

13699

11982123

97899

11090114

24413894

913098126

102981108985891748919073

10110110512593

1098197

133104

9449

25812

127

4512

122436282251

91126

717112010351814908

195383361941134

1875

2621512419417

ATMATMH20ATMATMATMATMATMATMATMATMATMATMATMH20ATMH20ATMATMATMH20ATMATMH20ATMATMATMATMH20ATMATMATMATMH20ATMH20ATMH20H20ATMUIATMH20ATMATMATMUIATMUIATMATMATMH20H20

5448.933(2)Ti I411 101-202

411 110-211 5451.127(6)Nd II

5451.957(3.5)Ti5452.298(3.5)Co I411 414-413

5455.095(2)Fe I p

411 202-303 5456.366(8.5)H 2 0

411 221-322

411 303-322411 220-321

411 211-312

411 313-414411 331-432

5457.474(11)Mn I5458.58(6)Fe I

5459.201(1.5)H 20

5461.823(2.5)Fe I p

5462.501(40)Ni I

5463.972(9.5)Cr I

411 313-312411 111-212 5447.248(3)Ni i? p

A. Rajaratnarn and K. T. Lua

400 5463.95


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12/13


Table 2. Continued(1) (2) (3) (4) (5) (6) (7) (8) (9)Standard WaveWavelength Deviation Number HW EW

No. (A) (mA) (cm) (mA) (mA) Origin Band Transition Remark455 5499.756 3 18177.57 ? ? ATM456 5500.069 7 18176.54 52 1 UI457 5500.390 10 18175.48 108 6 ATM458 5500.83 14 18174.02 92 3 ATM 5500.749(3)C 2459 5503.541 6 18165.07 192 10 UI460 5503.754 6 18164.37 96 5 ATM461 5505.168 3 18159.70 72 2 ATM462 5505.633 2 18158.17 108 3 UI 5505.728(2.5)Fe I p463 5507.560 7 18151.81 80 4 ATM464 5508.492 3 18148.74 ? ? UI465 5509.92 18 18144.04 ? ? H 2O 411 313-432 5509.909(19)Y ii466 5511.321 3 18139.43 72 9 ATM467 5513.762 5 18131.40 76 5 H 2 0 411 817-918468 5515.905 2 18124.35 72 7 ATM469 5523.967 2 18097.90 175 14 UI470 5524.572 7 18095.92 79 4 ATM 5524.578(2)C 2471 5524.891 4 18094.87 146 7 ATM

Column 1: WavelengthsWavelengths of spectral lines with a precision of measurementbetter than 0.01 A are entered to three decimal places. Thosewith a measurement precision worse than 0.01 Aare enteredto two decimal places only.Column 2: Standard Deviation of MeasurementAs wavelengths under column 1 are averages of several mea-surements (four to ten times), standard deviations are derivedand entered in this column in units of milliangstroms.Column 3: Vacuum Wave NumbersThe vacuum wave numbers of the spectral lines were calcu-lated from Edlen's formula,'4 i.e.,(n - 1)108 = 6432.8+ 2,949,810(146v2)l+ 25,540(41v2)-l, (7)and

Vvac = 1/Xvac = 1/nlXair, (8)where Vvac s the vacuum wave number in inverse micrometersand n is the refractive index of the air.Column 4: Half-Intensity WidthsThe HW's are entered in units of milliangstroms in this col-umn. A question mark is entered if this quantity has not beenmeasured.Column 5: Equivalent WidthsThe equivalent widths as estimated from Eq. (4) are enteredin milliangstroms. The water-vapor path lengths duringwhich the spectra were taken were estimated from the solarzenith angles and the water-vapor contents in the verticalatmospheric column. These data are provided in Table 3.

Table 3. Water-Vapor Path LengthSpectral Region Solar Zenith Water Vapor

(A) Angle (deg) (cm H2 0)4689-5231 81.8 375231-5408 82.5 405408-5684 82.9 42

Column 6: Origins of Spectral LinesThe identified water-vapor lines are entered as H20. Spectrallines that are arising from the absorption of the Earth's at-mosphere are entered as ATM; otherwise an entry of UI in-dicates that the identification of the atmospheric origin is notcertain.

Column 7: Band Designation of Water-Vapor LinesIt was found that all identified water-vapor lines listed inthis table belong to the vibration-rotation band 411.

Column 8: Rotational TransitionsThe rotational quantum numbers for each identified transi-tion are given. The upper vibrational state is 411, and thelower state is the ground state 000. The upper rotationalstates (J'Ka'Kc') are given first, followed by the lower ones(J"Ka"Kc").

Column 9: RemarksMany spectral lines are blended by solar lines. The wave-lengths, equivalent widths (in milliangstroms), and origins arelisted under this column. These data are obtained from Ref.1.



13/13

Vol. 73, No. 8/August 1983/J. Opt. Soc. Am. 1011CONCLUSIONWe have measured 471 spectral lines in the region of 4690 to5515 A,of which 65 are identified as atmospheric water-vaporlines and 320 are from the absorption of the atmospheric gaseswhose origins are not identified. The wavelengths, wavenumbers, half-intensity widths, equivalent widths, andidentifications are arranged into a table. We believe that twogroups of atmospheric lines near 4860 and 5080 Aalso belongto atmospheric water vapor. Work has already started inthese two regions, and results will be reported later.ACKNOWLEDGMENTWe wish to express our sincere thanks to the reviewers fortheir valuable comments.REFERENCES1. C. E. Moore, M. G. J. Minnaert, and J. Houtgast, "The solar

spectrum 2935 A to 8770 A," Nat. Bur. Stand. (U.S.) Monog. 61(1966).2. J. W. Swensson, W. S. Benedict, L. Delbouille, and G. Roland,"The solar spectrum from X7498 to X12016, a table of measuresand identifications," Mem. Soc. R. Sci. Liege 5 (1970).

3. M. Migeotte, L. Neven, and J. Swensson, "The solar spectrumfrom 2.8 to 23.8 microns. Part II, measures and identifications,"Mem. Soc. R. Sci. Liege 2 (1957).4. R. A. McClatchey, W. S. Benedict, S. A. Clough, D. E. Burch, R.F. Calfee, K. Fox, L. S. Rothman, and J. S. Garing, "AFCRL at-mospheric absorption line parameters compilation," Environ-mental research papers No. 434, AFCRL-TR-73-0096 (Air ForceCambridgeResearch Laboratories, Bedford, Mass., 1973).5. L. S. Rothman, "Update of AFGL atmospheric absorption lineparameters compilation," Appl. Opt. 17, 3517-3518 (1978).6. N. Laulainen, "Minor gases in the Earth's atmosphere: a reviewand bibliography of their spectra," Project Astra Pub. No. 18(University of Washington, Seattle, Wash., 1972).7. J. A. Curcio, L. F. Drummeter, and G. L. Knestrick, "An atlas ofthe absorption spectrum of the lower atmosphere from 5400Ato 8520 A,"Appl. Opt. 3, 1401-1409 (1964).8. A. K. Pierce and J. B. Breckinridge, "The Kitt Peak table ofphotographic solar spectrum wavelengths," Kitt Peak Contrib.559 (1973).9. R. S. Richardson and M. Schwarzschild, "On the turbulent ve-locities of solar granules," Astrophys. J. 111, 351-361 (1950).10. G. D. Finn and D. Mugglestone, "Table of the line broadeningfunction H(a, v)," Mon. Not. R. Astron. Soc. 129, 221-235

(1965).11. A. Rajaratnam and K. T. Lua, "Analysis of H 20 vibration-rotationspectra in the visible region," J. Phys. B 15,3615-3638 (1982).12. B. Edlen, "The dispersion of standard air," J. Opt. Soc. Am. 43,339-344 (1953).


telluric spectra 4690a-5525a

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