J/AJ/162/125 Searching transiting planets around halo stars. I. (Kolecki+, 2021)
Searching for transiting planets around halo stars.
I. Sample selection and validation.
Kolecki J.R., Wang J., Johnson J.A., Zinn J.C., Ilyin I., Strassmeier K.G.
<Astron. J., 162, 125-125 (2021)>
=2021AJ....162..125K 2021AJ....162..125K (SIMBAD/NED BibCode)
ADC_Keywords: Stars, halo; Stars, metal-deficient; Abundances, [Fe/H];
Spectra, optical
Keywords: Halo stars; Exoplanets; Metallicity
Abstract:
By measuring the elemental abundances of a star, we can gain insight
into the composition of its initial gas cloud-the formation site of
the star and its planets. Planet formation requires metals, the
availability of which is determined by the elemental abundance. In the
case where metals are extremely deficient, planet formation can be
stifled. To investigate such a scenario requires a large sample of
metal-poor stars and a search for planets therein. This paper focuses
on the selection and validation of a halo star sample. We select
∼17000 metal-poor halo stars based on their Galactic kinematics, and
confirm their low metallicities ([Fe/H]←0.5), using spectroscopy from
the literature. Furthermore, we perform high-resolution spectroscopic
observations using LBT/PEPSI and conduct detailed metallicity ([Fe/H])
analyses on a sample of 13 previously-known halo stars that also have
hot kinematics. We can use the halo star sample presented here to
measure the frequency of planets and to test planet formation in
extremely metal-poor environments. The result of the planet search and
its implications will be presented and discussed in a companion paper
by Boley et al.
Description:
Potsdam Echelle Polarimetric and Spectroscopic Instrument (PEPSI)
spectrograph is located at the Large Binocular Telescope (LBT, 2x8.4m
on Mt. Graham, Arizona, USA). LBT PEPSI observations were made on 2019
March 25, May 15, June 23, and June 25, UT with 200µm fiber
(R=130000 and 1.75" on sky) in two spectral regions 4800-5441Å and
6278-7419Å (cross-dispersers (CD) 3 and 5) with 10-60minutes
integration time depending on the star brightness.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 341 16940 Final halo catalog
table3.dat 113 156 Table of PEPSI equivalent widths
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See also:
B/pastel : The PASTEL catalogue (Soubiran+, 2016-)
III/145 : Radial Velocities in the Cardinal Directions (Sandage+ 1987)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
V/130 : Geneva-Copenhagen Survey Solar neighbourhood III (Holmberg+, 2009)
V/146 : LAMOST DR1 catalogs (Luo+, 2015)
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
III/279 : RAVE 5th data release (Kunder+, 2017)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
III/284 : APOGEE-2 data from DR16 (Johnsson+, 2020)
J/A+A/511/L10 : Abundances and space velocities of 94 stars (Nissen+, 2010)
J/ApJ/709/447 : Chemical composition of OGLE-2007-BLG-514S (Epstein+, 2010)
J/ApJ/743/140 : Abundances (Be,α) in metal-poor stars (Boesgaard+, 2011)
J/A+A/564/A133 : Gaia FGK benchmark stars: metallicity (Jofre+, 2014)
J/MNRAS/443/L89 : Kapteyn's star spectro. measurements (Anglada-Escude+ 2014)
J/AJ/151/144 : ASPCAP weights for 15 APOGEE chemical elements (Garcia+, 2016)
J/ApJS/225/32 : Extended abundance analysis of cool stars (Brewer+, 2016)
J/AJ/155/89 : California-Kepler Survey (CKS). IV. Planets (Petigura+, 2018)
J/AJ/156/18 : APOGEE DR14:Binary comp. of evolved stars (Price-Whelan+, 2018)
J/AJ/156/102 : TESS Input Catalog and Candidate Target List (Stassun+, 2018)
J/MNRAS/473/2004 : TESS-HERMES Survey Data Release 1 catalog (Sharma+, 2018)
J/MNRAS/478/4513 : GALAH Survey DR2 (Buder+, 2018)
http://physics.nist.gov/asd : NIST database (v5.8, Kramida+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- ID TIC Identifier (1)
11- 26 A16 --- 2MASS 2MASS position-based identifier
28- 46 I19 --- GAIA Gaia DR2 identifier
48- 66 F19.15 deg RAdeg [0/360] Gaia DR2 Right Ascension ICRS (J2015.5)
68- 86 F19.15 deg DEdeg [-90/90] Gaia DR2 Declination ICRS (J2015.5)
88- 93 F6.3 mag Tmag [8.64/16] TESS magnitude
95-100 F6.3 mag Gmag [8.88/17.3] Gaia DR2 G-band magnitude
102-107 F6.3 mag Jmag [8.21/14.9] 2MASS J-band magnitude
109-114 F6.3 mag Hmag [7.93/14.5] 2MASS H-band magnitude
116-121 F6.3 mag Kmag [7.88/14.2] 2MASS K-band magnitude
123-129 F7.4 [-] [M/H] [-3.85/0.06]? Metallicity
131-134 I4 pc Dist [100/1000] Distance from
Bailer-Jones+, 2018, I/347
136-140 F5.3 mas plx [0.97/9.95] Gaia DR2 parallax
142-149 F8.3 mas/yr pmRA [-830/884] Proper motion in RA (Gaia DR2)
151-158 F8.3 mas/yr pmDE [-935/-0.08] Proper motion in Dec (Gaia DR2)
160-168 F9.7 mag E(B-V) [0.0002/1.72] Color Excess, reddening
170-177 F8.6 Lsun Lum [0.003/5.12] Luminosity
179-195 F17.15 mas e_RAdeg [0.007/0.6] Uncertainty in RAdeg
197-213 F17.15 mas e_DEdeg [0.007/0.7] Uncertainty in DEdeg
215-222 F8.6 mag e_Tmag [0.006/0.3] Uncertainty in Tmag
224-231 F8.6 mag e_Gmag [0.0001/0.02] Uncertainty in Gmag
233-237 F5.3 mag e_Jmag [0.01/10]? Uncertainty in Jmag
239-243 F5.3 mag e_Hmag [0.01/0.2]? Uncertainty in Hmag
245-249 F5.3 mag e_Kmag [0.01/0.3]? Uncertainty in Kmag
251-258 F8.6 [-] e_[M/H] [0.006/0.3]? Uncertainty in [M/H]
260-265 F6.2 pc e_Dist [0.1/310] Uncertainty in Dist
267-273 F7.5 mas e_plx [0.01/0.9] Uncertainty in plx
275-279 F5.3 mas/yr e_pmRA [0.01/2] Uncertainty in pmRA
281-285 F5.3 mas/yr e_pmDE [0.01/8] Uncertainty in pmDE
287-295 A9 mag e_E(B-V) Uncertainty in E(B-V)
297-305 F9.7 Lsun e_Lum [0.0007/5]? Uncertainty in Lstar
307-316 F10.6 deg LAT [-89/89] Ecliptic Latitude
318-327 F10.6 deg LONG [0/360] Ecliptic Longtitude
329-341 A13 --- Lists Denotes membership in TIC Special Lists
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Note (1): All columns taken directly from CTL v08.01/TIC v8.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Ion Ionization number; FeI or FeII
7- 13 F7.2 0.1nm lambda [4745/7402] Wavelength, Angstroms (1)
15- 18 F4.2 eV ExPot [0.86/4.83] Excitation potential (2)
20- 24 F5.2 [-] loggf [-3.7/0.64] Statistical weight*oscillator strength
(2)
26- 31 F6.2 0.1ppm EW01 [5/172]? Equivalent width for BD+183423 (3)
33- 38 F6.2 0.1ppm EW02 [5/171]? Equivalent width for BD+202594 (3)
40- 44 F5.2 0.1ppm EW03 [6/88]? Equivalent width for BD+203603 (3)
46- 51 F6.2 0.1ppm EW04 [6/119]? Equivalent width for BD+251981 (3)
53- 57 F5.2 0.1ppm EW05 [5/93]? Equivalent width for BD+342476 (3)
59- 64 F6.2 0.1ppm EW06 [5/129]? Equivalent width for BD+362165 (3)
66- 71 F6.2 0.1ppm EW07 [5/128]? Equivalent width for BD+422667 (3)
73- 78 F6.2 0.1ppm EW08 [5/196]? Equivalent width for BD+511696 (3)
80- 85 F6.2 0.1ppm EW09 [5/193]? Equivalent width for BD+75839 (3)
87- 92 F6.2 0.1ppm EW10 [5/211]? Equivalent width for HD64090 (3)
94- 99 F6.2 0.1ppm EW11 [5/119]? Equivalent width for HD108177 (3)
101-106 F6.2 0.1ppm EW12 [5/225]? Equivalent width for HD160693 (3)
108-113 F6.2 0.1ppm EW13 [5/145]? Equivalent width for HD194598 (3)
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Note (1): Only those lines that we were able to measure for at least one star
are listed. Lines measured as weaker than the 5mÅ cutoff are not included
in this table.
Note (2): From NIST Atomic Spectra Database (v5.8, Kramida+, 2020);
http://physics.nist.gov/asd
Note (3): In milli-Angstroms
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 09-Dec-2021