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III/114 Spectra of Late-Type Standards, 2.0-2.5 Microns (Kleinmann+ 1986)
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Spectra of Late-Type Standard Stars in the Region 2.0-2.5 Microns
Kleinmann S.G., Hall D.N.B.
<Astrophys. Journ. Suppl. 62, 501 (1986)>
=1986ApJS...62..501K
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ADC_Keywords: Stars, late-type; Stars, standard;
Spectrophotometry; Spectra, infrared
Description:
This catalog contains a collection of K-band spectra for 26 stars with
near-solar abundances, ranging in spectral class from F8 to M7 and in
luminosity from dwarfs to supergiants. The spectra cover the wavelength
region from 4150 to 4950 /cm and generally exhibit a signal to noise
ratio above 400. Five stars here are supergiants, 15 are giants, and six
are dwarfs. Data included: observation date, starting wavenumber,
wavenumber increment, scale factor of relative intensity, and offset of
relative intensity.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
BS_8752.fit 2880 15 Spectrum of BS 8752
BS_8752n.fit 2880 15 Noise Spectrum of BS 8752
RW_CEP.fit 2880 15 Spectrum of RW CEP
RW_CEPn.fit 2880 15 Noise Spectrum of RW CEP
BS_8726.fit 2880 15 Spectrum of BS 8726
BS_8726n.fit 2880 15 Noise Spectrum of BS 8726
MU_CEP.fit 2880 15 Spectrum of MU CEP
MU_CEPn.fit 2880 15 Noise Spectrum of MU CEP
SU_PER.fit 2880 15 Spectrum of SU PER
SU_PERn.fit 2880 15 Noise Spectrum of SU PER
UPS_PEG.fit 2880 15 Spectrum of UPS PEG
UPS_PEGn.fit 2880 15 Noise Spectrum of UPS PEG
31_COM.fit 2880 15 Spectrum of 31 COM
31_COMn.fit 2880 15 Noise Spectrum of 31 COM
84_HER.fit 2880 15 Spectrum of 84 HER
84_HERn.fit 2880 15 Noise Spectrum of 84 HER
OMI_UMA.fit 2880 15 Spectrum of OMIC UMA
OMI_UMAn.fit 2880 15 Noise Spectrum of OMIC UMA
EPS_VIR.fit 2880 15 Spectrum of EPS VIR
EPS_VIRn.fit 2880 15 Noise Spectrum of EPS VIR
IOT_CEP.fit 2880 15 Spectrum of IOTA CEP
IOT_CEPn.fit 2880 15 Noise Spectrum of IOTA CEP
KAP_OPH.fit 2880 15 Spectrum of KAP OPH
KAP_OPHn.fit 2880 15 Noise Spectrum of KAP OPH
39_CYG.fit 2880 15 Spectrum of 39 CYG
39_CYGn.fit 2880 15 Noise Spectrum of 39 CYG
GAM_DRA.fit 2880 15 Spectrum of GAM DRA
GAM_DRAn.fit 2880 15 Noise Spectrum of GAM DRA
GAM_SGE.fit 2880 15 Spectrum of GAM SGE
GAM_SGEn.fit 2880 15 Noise Spectrum of GAM SGE
75_CYG.fit 2880 15 Spectrum of 75 CYG
75_CYGn.fit 2880 15 Noise Spectrum of 75 CYG
XI_PEG.fit 2880 15 Spectrum of XI PEG
XI_PEGn.fit 2880 15 Noise Spectrum of XI PEG
R_LYRAE.fit 2880 15 Spectrum of R LYRAE
R_LYRAEn.fit 2880 15 Noise Spectrum of R LYRAE
BK_VIR.fit 2880 15 Spectrum of BK VIR
BK_VIRn.fit 2880 15 Noise Spectrum of BK VIR
SW_VIR.fit 2880 15 Spectrum of SW VIR
SW_VIRn.fit 2880 15 Noise Spectrum of SW VIR
16CYG_A.fit 2880 15 Spectrum of 16 CYG A
16CYG_An.fit 2880 15 Noise Spectrum of 16 CYG A
16CYG_B.fit 2880 15 Spectrum of 16 CYG B
16CYG_Bn.fit 2880 15 Noise Spectrum of 16 CYG B
SIG_DRA.fit 2880 15 Spectrum of SIG DRA
SIG_DRAn.fit 2880 15 Noise Spectrum of SIG DRA
61CYG_A.fit 2880 15 Spectrum of 61 CYG A
61CYG_An.fit 2880 15 Noise Spectrum of 61 CYG A
GL_411.fit 2880 15 Spectrum of GL 411
GL_411n.fit 2880 15 Noise Spectrum of GL 411
WOLF359.fit 2880 15 Spectrum of WOLF 359
WOLF359n.fit 2880 15 Noise Spectrum of WOLF 359
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Remarks and Modifications:
A magnetic tape containing the atlas Spectra of Late-Type Standard Stars in
the Region 2.0-2.5 Microns was received from Dr. Susan G. Kleinmann on April
28, 1987. The tape contained 52 files one file for each signal and noise
spectrum, in VAX/VMS SAVESET format. As received, each spectrum consisted
of three parts: (I) the first 412 logical records contained a "big
information block" (BIB) consisting of what might be termed engineering
data from the Fourier transform spectrometer. This is largely redundant
information from spectrum to spectrum and most of the records were actually
unused; (2) a "small information block" (SIB) of two records containing in-
formation pertinent to each observation, and; (3) the array of data points.
Following discussions with Dr. Kleinmann, it was mutually agreed that the
BIBs could be removed from the spectra, the SIBs modified slightly for
easier processing, and all the spectra combined into a single file. The
merging of the data simplifies the structure and is not a hindrance to
processing because each spectrum contains the same number of records and can
be read with a DO statement. The elimination of the redundant information
also decreased the size of the catalog by a factor of 2, a definite
advantage for storage requirements and dissemination. After the above
modifications were made, the data were archived for distribution. The
spectra are in the same order as in Table I of the source reference.
Acknowledgments:
The original ADC documentation by Kang, Y.W. and Warren, W.H. Jr. (1988)
was used to create this ReadMe file.
References:
Keenan, P. C. and McNeil, R. C. 1976, An Atlas of Spectra of The Cooler
Stars (Columbus: The Ohio State University Press).
Keenan, P. C. and Pitts, R. E. 1980, Astrophys. J. Suppl. 42, 541.
Kleinmann, S. G. and Hall, D. N. B. 1986, Astrophys. J. Suppl. 62, 501.
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(End) C.-H. Joseph Lyu [Hughes STX/NASA] 13-Jul-1995