J/MNRAS/510/4308 Local main-sequence stars with phot. metallicities (Kim+, 2022)
Stars in the local Galactic thick disk and halo in Gaia EDR3: A catalogue of
half a million local main-sequence stars with photometric metallicities.
Kim B., Lepine S.
<Mon. Not. R. Astron. Soc. 510, 4308-4329 (2022)>
=2022MNRAS.510.4308K 2022MNRAS.510.4308K (SIMBAD/NED BibCode)
ADC_Keywords: Stars, nearby ; Stars, dwarfs ; Stars, late-type ;
Abundances, [Fe/H] ; Optical
Keywords: catalogues - stars: abundances - stars: kinematics and dynamics -
Galaxy: halo - Galaxy: solar neighbourhood
Abstract:
We present a catalogue of 551214 main-sequence stars in the local
(d<2kpc) Galactic thick disk and halo, based on a search of stars with
large proper motions (>40.0mas/yr) in the Gaia Early Data Release 3.
We derive photometric metallicity calibrated from the
colour-luminosity-metallicity distribution of 20047 stars with
spectroscopic metallicities, collected from various spectroscopic
surveys, including SDSS SEGUE/APOGEE, GALAH DR3, and LAMOST DR6. We
combine these results to construct an empirical colour-
magnitude-metallicity grid, which can be used to estimate photometric
metallicities for low-mass metal-poor stars of K and M subtypes from
their absolute G magnitude and colour values. We find that low-mass,
high-velocity stars in our catalogue share similar kinematics as
reported in recent studies of more luminous Galactic halo stars. The
pseudo-kinematic analysis of our sample recovers the main local halo
structures, including the Gaia-Enceladus Stream and the Helmi stream;
aside from these the local halo stars appear to show a remarkably
smooth distribution in velocity space. Since the future Gaia data
release will provide radial velocity measurements for only a small
number of our sample, our catalogue provides targets of high interest
for the future spectroscopic observation programs.
Description:
We have collected high-proper-motion stars with precise
astrometric and photometric measurements in Gaia EDR3 in order to
identify the local halo population out to 2kpc.
Our catalogue contains 551214 main-sequence stars in d<2kpc,
including 321879 late-type dwarfs (MG>7.5).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table6.dat 118 551214 Catalogue of candidates in the Galactic thick
disk and halo in Gaia EDR3
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See also:
I/350 : Gaia Early Data Release 3 (Gaia Collaboration 2020)
III/284 : APOGEE-2 data from DR16 (Johnsson+, 2020)
J/MNRAS/506/150 : The GALAH+ Survey DR3 (Buder+, 2021)
J/AJ/159/30 : High proper-motion M-type stars spectroscopic obs.
(Hejazi+, 2020)
J/AJ/137/4377 : List of SEGUE plate pairs (Yanny+, 2009)
http://argonaut.skymaps.info : Interactive 3D dust map
Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 19 I19 --- GaiaEDR3 Gaia EDR3 unique source identifier
21- 31 F11.7 deg RAdeg Right ascension (ICRS) at Ep=2016
33- 43 F11.7 deg DEdeg Declination (ICRS) at Ep=2016
45- 52 F8.4 mas plx Parallax
54- 59 F6.4 mas e_plx Standard error of parallax
61- 69 F9.3 mas/yr pmRA Proper motion in right ascension direction,
pmRA*cosDE
71- 79 F9.3 mas/yr pmDE Proper motion in declination direction
81- 86 F6.3 mag Gmag G-band mean magnitude
88- 92 F5.3 mag G-RP G-RP colour index
94- 98 F5.3 mag E(G-RP) G-RP colour excess (1)
100-104 F5.3 mag AG G-band extinction (2)
106-111 F6.3 [-] [Fe/H]KNN Metallicity estimate from
the KNN regressor
113-118 F6.3 [-] [Fe/H]grid Metallicity estimate from
the photometric metallicity grid
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Note (1): We adapt the 3D dust map from Green et al. (2019ApJ...887...93G 2019ApJ...887...93G) to
obtain B-V colour excess for each of our stars. We then convert E(B-V) to
E(G-RP) based on the colour excess ratio and extinction coefficient for
Gaia passbands from Table 3 in Wang & Chen (2019ApJ...877..116W 2019ApJ...877..116W).
A(V)=3.16*E(B-V)=2.394*E(BP-RP)
E(BP-RP)=1.320*E(B-V)
Note (2): According to Wang & Chen (2019ApJ...877..116W 2019ApJ...877..116W),
A(G)=1.890*E(BP-RP), A(RP)=1.429*E(BP-RP)
E(G-RP)=A(G)-A(RP)=0.461*E(BP-RP)
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History:
From Bokyoung Kim, bokyoung.kim(at)ed.ac.uk
Acknowledgements:
We appreciate the Gaia DPAC, SDSS APOGEE/SEGUE groups, the LAMOST
team, and the GALAH survey team for their efforts in producing the
data sets we have used to calibrate our photometric metallicity grid.
This work has made use of data from the European Space Agency (ESA)
mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia
Data Processing and Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/ consortium). Funding for the
DPAC has been provided by national institutions, in particular the
institutions participating in the Gaia Multilateral Agreement.
Funding for SDSS-III and SDSS-IV has been provided by the Alfred P.
Sloan Foundation, the Participating Institutions, the National Science
Foundation, and the U.S. Department of Energy Office of Science.
SDSS-IV acknowledges support and resources from the centre for High
Performance Computing at the University of Utah. The SDSS website is
http://www.sdss.org.
Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber
Spectroscopic Telescope LAMOST) is a National Major Scientific Project
built by the Chinese Academy of Sciences. Funding for the project has
been provided by the National Development and Reform Commission.
LAMOST is operated and managed by the National Astronomical
Observatories, Chinese Academy of Sciences.
This work made use of the Third Data Release of the GALAH Survey
(Buder et al., 2021MNRAS.506..150B 2021MNRAS.506..150B, Cat. J/MNRAS/506/150). The GALAH
Survey is based on data acquired through the Australian Astronomical
Observatory, under programs: A/2013B/13 (The GALAH pilot survey);
A/2014A/25, A/2015A/19, A2017A/18 (The GALAH survey phase 1);
A2018A/18 (Open clusters with HERMES); A2019A/1 (Hierarchical star
formation in Ori OB1); A2019A/15 (The GALAH survey phase 2);
A/2015B/19, A/2016A/22, A/2016B/10, A/2017B/16, A/2018B/15 (The
HERMES-TESS program); and A/2015A/3, A/2015B/1, A/2015B/19,
A/2016A/22, A/2016B/12, A/2017A/14 (The HERMES K2-follow-up program).
We acknowledge the traditional owners of the land on which the AAT
stands, the Gamilaraay people, and pay our respects to elders past and
present. This paper includes data that has been provided by AAO Data
Central (datacentral.org.au).
References:
Ahumada et al., 2020ApJS..249....3A 2020ApJS..249....3A
Buder et al., 2021MNRAS.506..150B 2021MNRAS.506..150B, Cat. J/MNRAS/506/150
Cui et al., 2012RAA....12.1197C 2012RAA....12.1197C
De Silva et al., 2015MNRAS.449.2604D 2015MNRAS.449.2604D
Gaia Collaboration, Gaia DR1 2016A&A...595A...1G 2016A&A...595A...1G, Cat. I/337
Gaia Collaboration, Gaia DR2 2018A&A...616A...1G 2018A&A...616A...1G, Cat. I/345
Gaia Collaboration, Gaia DR3 2021A&A...649A...1G 2021A&A...649A...1G, Cat. I/350
Green et al.,, 2019ApJ...887...93G 2019ApJ...887...93G
Hejazi et al., 2020AJ....159...30H 2020AJ....159...30H, Cat. J/AJ/159/30
Majewski et al., 2017AJ....154...94M 2017AJ....154...94M, Cat. III/284
Wang & Chen 2019ApJ...877..116W 2019ApJ...877..116W
Yanny et al., 2009AJ....137.4377Y 2009AJ....137.4377Y, Cat. J/AJ/137/4377
(End) Patricia Vannier [CDS] 07-Jan-2022