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
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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
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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
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?
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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
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Vol. 73, No. 8/August 1983/J. Opt. Soc. Am. 1005Table 2. Continued
(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
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Vol. 73, No. 8/August 1983/J. Opt. Soc. Am. 1007Table 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 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
A. Rajaratnam and K. T. Lua
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1008 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
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
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1010 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 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.
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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).
A. Rajaratnam and K. T. Lua