J/ApJS/221/24 SDSS-III APOGEE H-band spectral line lists (Shetrone+, 2015)
The SDSS-III APOGEE spectral line list for H-band spectroscopy.
Shetrone M., Bizyaev D., Lawler J.E., Allende Prieto C., Johnson J.A.,
Smith V.V., Cunha K., Holtzman J., Garcia Perez A.E., Meszaros SZ.,
Sobeck J., Zamora O., Garcia-Hernandez D.A., Souto D., Chojnowski D.,
Koesterke L., Majewski S., Zasowski G.
<Astrophys. J. Suppl. Ser., 221, 24 (2015)>
=2015ApJS..221...24S 2015ApJS..221...24S (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics ; Spectra, infrared ; Equivalent widths
Keywords: atomic data; line: identification; methods: laboratory: atomic;
molecular data
Abstract:
We present the H-band spectral line lists adopted by the Apache Point
Observatory Galactic Evolution Experiment (APOGEE). The APOGEE line
lists comprise astrophysical, theoretical, and laboratory sources from
the literature, as well as newly evaluated astrophysical oscillator
strengths and damping parameters. We discuss the construction of the
APOGEE line list, which is one of the critical inputs for the APOGEE
Stellar Parameters and Chemical Abundances Pipeline, and present three
different versions that have been used at various stages of the
project. The methodology for the newly calculated astrophysical line
lists is reviewed. The largest of these three line lists contains
134457 molecular and atomic transitions. In addition to the format
adopted to store the data, the line lists are available in MOOG,
Synspec, and Turbospectrum formats. The limitations of the line lists
along with guidance for its use on different spectral types are
discussed. We also present a list of H-band spectral features that are
either poorly represented or completely missing in our line list. This
list is based on the average of a large number of spectral fit
residuals for APOGEE observations spanning a wide range of stellar
parameters.
Description:
The Apache Point Observatory Galactic Evolution Experiment (APOGEE)
obtained high-resolution (R∼22500) and high signal-to-noise ratio
(S/N>100) spectra in the H band (1.51-1.70um), using the Sloan
Foundation 2.5-m Telescope, for more than 100000 cool giant stars (see
Zasowski et al. 2013AJ....146...81Z 2013AJ....146...81Z, for more information about
targeting) spanning all components of the Milky Way. Stellar
parameters and individual chemical abundances are derived from the
combined APOGEE spectra (Nidever et al. 2015AJ....150..173N 2015AJ....150..173N) with the
APOGEE Stellar Parameters and Chemical Abundances Pipeline (ASPCAP),
which is described in detail in Garcia Perez et al. (2015arXiv151007635G 2015arXiv151007635G).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table6.dat 23 445 Missing lines
table7.dat 186 134457 *ASPCAP DR12 (20131216) line list
table8.dat 186 134230 *ASPCAP INT (20120216) line list
table9.dat 186 134052 *ASPCAP DR10 (20110510) line list
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Note on table7.dat and table9.dat: In order to run APOGEE Stellar Parameters
and Chemical Abundances Pipeline (ASPCAP) on the first year of
APOGEE results (DR10; Ahn et al. 2014ApJS..211...17A 2014ApJS..211...17A), an initial line list
was generated and adopted. In subsequent years, improvements were made and
different methodologies were adopted in the line list used for the release of
the full three year data set of APOGEE (DR12; Alam et al.
2015ApJS..219...12A 2015ApJS..219...12A). The APOGEE internal naming scheme for the DR10 and DR12
line lists are 20110510 and 20131216, respectively.
Note on table8.dat: In the years between DR10 and DR12, Garcria Perez et al.
(2013ApJ...767L...9G 2013ApJ...767L...9G), Smith et al. (2013ApJ...765...16S 2013ApJ...765...16S) and Cunha et al.
(2015ApJ...798L..41C 2015ApJ...798L..41C) made use of an intermediate line list, 20120216.
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Description of file: In addition the same DR data is available on the FTP,
in MOOG (Sneden 1974PhDT.......316S 1974PhDT.......316S), Turbospectrum (Alvarez & Plez
1998A&A...330.1109A 1998A&A...330.1109A; Plez 2012, http://ascl.net/1205.004), and
AAS{espsilon}T (Koesterke 2009AIPC.1171...73K 2009AIPC.1171...73K) formats in the included
tar.gz package (apjs521087_table7.tar.gz, apjs521087_table8.tar.gz and
apjs521087_table9.tar.gz files for table7.dat (DR12), table8.dat (INT)
and table9.dat (DR10), respectively).
See also:
J/AJ/149/7 : SDSS-III/APOGEE. I. Be stars (Chojnowski+, 2015)
J/ApJS/214/26 : Line lists for CN isotopes transitions (Sneden+, 2014)
J/ApJS/214/18 : VII log(gf) values, and V abundance in HD 84937 (Wood+ 2014)
J/ApJ/794/125 : IN-SYNC. I. APOGEE stellar parameters (Cottaar+, 2014)
J/AJ/146/133 : Stellar parameters from SDSS-III APOGEE DR10 (Meszaros+, 2013)
J/ApJS/208/27 : Sun and HD 84937 TiII log(gf) and abundances (Wood+, 2013)
J/A+A/548/A55 : C and O isotopic ratios in Arcturus and Aldebaran (Abia+ 2012)
J/A+A/468/1115 : Thorium and argon lines in the visible (Lovis+, 2007)
J/A+A/363/1081 : Non-linear limb-darkening law for LTE models (Claret, 2000)
J/ApJS/124/527 : Oscillator strengths for lines in J+H bands (Melendez+, 1999)
J/ApJS/95/535 : Infrared CO line list for X 1Σ+ state (Goorvitch, 1994)
Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 7 F7.1 0.1nm lambda [15174.1/16945.8] Vacuum wavelength in Angstroms
9- 11 I3 10-13m EW [10/219]? Equivalent width in milli-Angstroms
12 A1 --- f_EW Flag on EqWid (e=emission or N=N/A)
14- 23 A10 --- Notes [ ,a-k] Additional notes (1)
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Note (1): Note as follows:
a = Seen in the cool APOGEE giant spectra residual;
b = Seen in the hot APOGEE spectra residual;
c = Between APOGEE detectors;
d = all FTS stars;
e = only M FTS stars;
f = found only in HD199799;
g = see Hasselquist et al. 2016 in prep.;
h = Seen in cool APOGEE dwarf spectra residuals
i = Seen in APOGEE Be spectra, see Chojnowski et al. (2015, J/AJ/149/7)
j = This may be a DIB feature, see Zasowski et al. (2015ApJ...798...35Z 2015ApJ...798...35Z)
k = This may be a DIB feature, see Geballe et al. (2011Natur.479..200G 2011Natur.479..200G).
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Byte-by-byte Description of file: table[789].dat
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Bytes Format Units Label Explanations
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1- 9 F9.4 nm lambda [1500.4/1700.5] Vacuum wavelength
11- 17 F7.3 [-] orggf [-16.8/1.2]? Original log(gf) value
19- 25 F7.3 [-] newgf [-9.5/1.1]? Improved literature or
laboratory log(gf)
27- 30 F4.2 [-] e_newgf [0.01/1]? Error in newgf, when available
32- 34 A3 --- r_newgf Source for newgf
35- 41 F7.3 [-] astgf [-14.7/1.3]? Astrophysical log(gf)
43- 45 A3 --- r_astgf Source for astrogf
47- 54 F8.2 --- specid [1/608.18] Species identifier
55- 66 F12.3 cm-1 EP1 [0/771723.1] Lower Energy Level
67- 71 F5.1 --- J1 [0/159] J value for EP1
72- 82 A11 --- EP1id EP1 level identification
83- 94 F12.3 cm-2 EP2 [6200.7/778194.1] Upper Energy Level
95- 99 F5.1 --- J2 [0/160] J value for EP2
100-110 A11 --- EP2id EP2 level identification
111-116 F6.2 --- Rad [0/11.1]? Damping Rad
117-122 F6.2 --- Sta [-8/0]? Damping Stark
123-128 F6.2 --- vdW [-8.4/0]? Damping vdW
130-131 I2 --- unlte [0/99]? NLTE level number upper
132-133 I2 --- lnlte [0/99]? NLTE level number lower
134-136 I3 --- iso1 [0/65]? First isotope number
137-142 F6.3 [-] hyp [-9.999/0]? Hyperfine component log fractional
strength
143-145 I3 --- iso2 [0/65]? Second isotope number
146-151 F6.3 [-] isof [-4/0]? Log isotopic abundance fraction
152-156 I5 mK hE1 [-520/425]? Hyperfine shift for 1st level to be
added to E1
157-161 I5 mK hE2 [-603/469]? Hyperfine shift for 1st level to be
added to E2
162-162 A1 --- F0 [F] Hyperfine F symbol
163-163 I1 --- F1 [0/9]? Hyperfine F for the first level
164-164 A1 --- Note1 [?z] Note on character of hyperfine data
for first level (z=none; ?=guessed)
165-165 A1 --- S [-] The symbol "-" for legibility
166-166 I1 --- F2 [0/9]? Hyperfine F' for the second level
167-167 A1 --- note2 [?z] Note on character of hyperfine data for
second level (z=none; ?=guessed)
168-172 I5 --- g1 [-720/3934]? Lande g for first level times 1000
173-177 I5 --- g2 [-689/4006]? Lande g for second level times 1000
178-180 A3 --- vdWorg Source for the original vdW damping
181-186 F6.2 --- vdWast [-8.1/-5.2]? Astrophysical vdW damping
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 28-Jan-2016