J/ApJ/879/69 The Payne applied to the APOGEE DR14 data set (Ting+, 2019)
The Payne: self-consistent ab initio fitting of stellar spectra.
Ting Y.-S., Conroy C., Rix H.-W., Cargile P.
<Astrophys. J., 879, 69-69 (2019)>
=2019ApJ...879...69T 2019ApJ...879...69T (SIMBAD/NED BibCode)
ADC_Keywords: Spectra, infrared; Surveys; Abundances
Keywords: methods: data analysis; stars: abundances; techniques: spectroscopic
Abstract:
We present The Payne, a general method for the precise and
simultaneous determination of numerous stellar labels from observed
spectra, based on fitting physical spectral models. The Payne combines
a number of important methodological aspects: it exploits the
information from much of the available spectral range; it fits all
labels (stellar parameters and elemental abundances) simultaneously;
it uses spectral models, where the structure of the atmosphere and the
radiative transport are consistently calculated to reflect the stellar
labels. At its core The Payne has an approach to accurate and precise
interpolation and prediction of the spectrum in high-dimensional label
space that is flexible and robust, yet based on only a moderate number
of ab initio models (O (1000) for 25 labels). With a simple
neural-net-like functional form and a suitable choice of training
labels, this interpolation yields a spectral flux prediction good to
10-3rms across a wide range of Teff and logg (including dwarfs and
giants). We illustrate the power of this approach by applying it to
the APOGEE DR14 data set, drawing on Kurucz models with recently
improved line lists: without recalibration, we obtain physically
sensible stellar parameters as well as 15 elemental abundances that
appear to be more precise than the published APOGEE DR14 values. In
short, The Payne is an approach that for the first time combines all
these key ingredients, necessary for progress toward optimal modeling
of survey spectra; and it leads to both precise and accurate estimates
of stellar labels, based on physical models and without "recalibration".
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 213 222707 APOGEE-Payne catalog: APOGEE stellar labels
determined with The Payne
--------------------------------------------------------------------------------
See also:
V/146 : LAMOST DR1 catalogs (Luo+, 2015)
III/284 : APOGEE-2 data from DR16 (Johnsson+, 2020)
J/A+A/492/171 : VIc light curves of NGC 6791 V20 (Grundahl+, 2008)
J/A+A/497/497 : Physical parameters from JHK flux (Gonzalez-Hernandez+, 2009)
J/AZh/88/750 : Abundances in stars of gal. sub-structures (Mishenina+, 2011)
J/AJ/142/193 : RAVE stellar elemental abundances (DR1) (Boeche+, 2011)
J/A+A/545/A32 : Chemical abundances of 1111 FGK stars (Adibekyan+, 2012)
J/AJ/146/133 : Stellar parameters from SDSS-III APOGEE DR10 (Meszaros+, 2013)
J/A+A/562/A71 : Abundances of solar neighbourhood dwarfs (Bensby+, 2014)
J/A+A/568/A25 : C and O abundances in stellar populations (Nissen+, 2014)
J/AJ/148/51 : WIYN Open Cluster. LXI. NGC 6819 phot. (Anthony-Twarog+, 2014)
J/A+A/577/A9 : Sc, V, Mn, and Co in Milky Way stars (Battistini+, 2015)
J/ApJ/808/16 : The Cannon: a new approach to measure abundances (Ness+, 2015)
J/A+A/587/A2 : SP_Ace derived data from stellar spectra (Boeche+, 2016)
J/MNRAS/456/3655 : Masses and ages of red giants (Martig+, 2016)
J/AJ/151/144 : ASPCAP weights for APOGEE chemical elements (Garcia+, 2016)
J/ApJ/823/114 : The Cannon: a new approach to determine masses (Ness+, 2016)
J/ApJ/833/225 : -2.6≤[Fe/H]≤0.2 F and G dwarfs. II. Abundances (Zhao+, 2016)
J/ApJS/236/42 : Asteroseismology of ∼16000 Kepler red giants (Yu+, 2018)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- APOGEE APOGEE Identifier (2M or APHHMMSSss+DDMMSSs;
J2000 and 1 occurrence for "VESTA")
20- 28 F9.5 deg RAdeg Right Ascension, decimal degrees (J2000)
30- 38 F9.5 deg DEdeg [-33/88] Declination, decimal degrees (J2000)
40- 47 F8.3 K Teff [3050/7950] Stellar effective temperature
49- 53 F5.3 [cm/s2] logg [0/5] log of stellar surface gravity
55- 59 F5.3 km/s Vt [0/3] Microturbulent velocity dispersion
61- 66 F6.3 [-] [C/H] [-2.24/0.63] Elemental Abundance, [C/H]
68- 73 F6.3 [-] [N/H] [-2.52/1.4] Elemental Abundance, [N/H]
75- 80 F6.3 [-] [O/H] [-2.53/1.62] Elemental Abundance, [O/H]
82- 87 F6.3 [-] [Mg/H] [-2.5/1.7] Elemental Abundance, [Mg/H]
89- 94 F6.3 [-] [Al/H] [-2.52/1] Elemental Abundance, [Al/H]
96-101 F6.3 [-] [Si/H] [-2.4/1.21] Elemental Abundance, [Si/H]
103-108 F6.3 [-] [S/H] [-2.14/0.55] Elemental Abundance, [S/H]
110-115 F6.3 [-] [K/H] [-2.47/1.42] Elemental Abundance, [K/H]
117-122 F6.3 [-] [Ca/H] [-2.51/0.57] Elemental Abundance, [Ca/H]
124-129 F6.3 [-] [Ti/H] [-2.31/1.06] Elemental Abundance, [Ti/H]
131-136 F6.3 [-] [Cr/H] [-2.33/1.35] Elemental Abundance, [Cr/H]
138-143 F6.3 [-] [Mn/H] [-2.37/0.94] Elemental Abundance, [Mn/H]
145-150 F6.3 [-] [Fe/H] [-1.45/0.45] Elemental Abundance, [Fe/H]
152-157 F6.3 [-] [Ni/H] [-2.55/0.83] Elemental Abundance, [Ni/H]
159-164 F6.3 [-] [Cu/H] [-2.5/1.72] Elemental Abundance, [Cu/H]
166-171 F6.3 --- C12C13 [0.005/100] Isotope Ratio, C12/C13
173-178 F6.3 km/s Vmac [0.1/30] Macroturbulent velocity dispersion
180-192 F13.3 --- Chi2 [0.05/1.42e+08] Reduced χ2 of the fit
194-213 A20 --- Qual Quality flag (1)
--------------------------------------------------------------------------------
Note (1): Quality flag as follows:
good = 196683 occurrences
chi2_R>50 = 16526 occurrences
vmac>20kms = 8858 occurrences
vmac>20kms;chi2_R>50 = 640 occurrences
We caution that in this catalog we keep stars that have large
Χ2R in the fitting for completeness, but we recommend readers
only use stars that show "good" in the "Qual" column. This flag
excludes all stars with χR2>50, a fiducial cut we adopt in
this study. It also excludes fast rotators with vmacro>20km/s
(mostly hot stars with Teff>6000K). See Section 3.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 25-Oct-2023