J/AN/338/686 Pristine survey II. Bright stars abundances (Caffau+, 2017)
The Pristine survey. II. A sample of bright stars observed with FEROS.
Caffau E., Bonifacio P., Starkenburg E., Martin N., Youakim K., Henden A.A.,
Gonzalez Hernandez J.I., Aguado D.S., Allende Prieto C., Venn K.,
Jablonka P.
<Astron. Nachrichten 338, 686-695 (2017)>
=2017AN....338..686C 2017AN....338..686C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, metal-deficient ; Radial velocities ; Abundances
Keywords: star: abundances - stars: atmospheres - galaxy: abundances -
galaxy: evolution
Abstract:
Extremely metal-poor (EMP) stars are old objects formed in the first
Gyr of the Universe. They are rare and, to select them the most
successful strategy has been to build on large and low-resolution
spectroscopic surveys. The combination of narrow- and broad-band
photometry provides a powerful and cheaper alternative to select
metal-poor stars. The ongoing Pristine Survey is adopting this
strategy, conducting photometry with the Canada France Hawaii
Telescope MegaCam wide-field imager and a narrow-band filter centered
at 395.2nm on the Ca II-H and -K lines. In this paper, we present the
results of the spectroscopic follow-up conducted on a sample of 26
stars at the bright end of the magnitude range of the Survey (g≤15),
using FEROS at the MPG/ESO 2.2-m telescope (manufactured by Zeiss,
Oberkochen, Germany). From our chemical investigation on the sample,
we conclude that this magnitude range is too bright to use the Sloan
Digital Sky Survey (SDSS) gri bands, which are typically saturated.
Instead, the Pristine photometry can be usefully combined with the
AAVSO Photometric All Sky Survey (APASS) gri photometry to provide
reliable metallicity estimates. Data from FEROS.
Description:
Atmospheric parameters and radial velocities for 27 stars and detailed
abundances for 23 stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
atmpar.dat 113 27 Coordinates, atmospheric parameters and
radial velocities (table 2)
abund.dat 279 23 Chemical abundances (tables 3-5)
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Byte-by-byte Description of file: atmpar.dat
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Bytes Format Units Label Explanations
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1- 25 A25 --- Name Name (Pristine DDD.dddd+DD.dddd)
27- 37 F11.7 deg RAdeg Right Ascension (J2000.0)
39- 50 F12.8 deg DEdeg Declination (J2000.0)
52- 55 F4.1 mag g0mag Dereddened SDSS g magnitude
57- 62 F6.1 km/s BRV Barycentric radial velocities
64- 67 I4 K Teff ? Effective temperature
69- 72 F4.2 [cm/s2] logg ? logarithmic surface gravity
74- 77 F4.2 km/s Vturb ? microturbulent velocity
79- 83 F5.2 [Sun] [Fe/H] ? logarithmic iron abundance with respect
to the Sun
85-113 A29 --- Com Comments (1)
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Note (1): (Y) indicates stars that passed the selection criterion of the
Pristine calibration.
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Byte-by-byte Description of file: abund.dat
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Bytes Format Units Label Explanations
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1- 25 A25 -- Name Star name (Pristine DDD.dddd+DD.dddd)
27- 31 F5.2 [-] A(NaI) ? NaI abundance, log[N(X)/N(H)]+12
33- 36 F4.2 [-] e_A(NaI) ? Error on A(NaI)
39- 43 F5.2 [-] A(AlI) ? AlI abundance, log[N(X)/N(H)]+12
45- 48 F4.2 [-] e_A(AlI) ? Error on A(AlI)
51- 55 F5.2 [-] A(MgI) ? MgI abundance, log[N(X)/N(H)]+12
57- 60 F4.2 [-] e_A(MgI) ? Error on A(MgI)
63- 67 F5.2 [-] A(SiI) ? SiI abundance, log[N(X)/N(H)]+12
69- 72 F4.2 [-] e_A(SiI) ? Error on A(SiI)
75- 79 F5.2 [-] A(SiII) ? SiII abundance, log[N(X)/N(H)]+12
81- 84 F4.2 [-] e_A(SiII) ? Error on A(SiII)
88- 92 F5.2 [-] A(SI) ? SI abundance, log[N(X)/N(H)]+12
94- 97 F4.2 [-] e_A(SI) ? Error on A(SI)
99-103 F5.2 [-] A(CaI) ? CaI abundance, log[N(X)/N(H)]+12
105-108 F4.2 [-] e_A(CaI) ? Error on A(CaI)
111-115 F5.2 [-] A(ScII) ? ScII abundance, log[N(X)/N(H)]+12
117-120 F4.2 [-] e_A(ScII) ? Error on A(ScII)
124-128 F5.2 [-] A(TiI) ? TiI abundance, log[N(X)/N(H)]+12
130-133 F4.2 [-] e_A(TiI) ? Error on A(TiI)
136-140 F5.2 [-] A(TiII) ? TiII abundance, log[N(X)/N(H)]+12
142-145 F4.2 [-] e_A(TiII) ? Error on A(TiII)
149-153 F5.2 [-] A(VI) ? VI abundance, log[N(X)/N(H)]+12
155-158 F4.2 [-] e_A(VI) ? Error on A(VI)
160-164 F5.2 [-] A(CrI) ? CrI abundance, log[N(X)/N(H)]+12
166-169 F4.2 [-] e_A(CrI) ? Error on A(CrI)
172-176 F5.2 [-] A(MnI) ? MnI abundance, log[N(X)/N(H)]+12
178-181 F4.2 [-] e_A(MnI) ? Error on A(MnI)
184-188 F5.2 [-] A(FeI) ? FeI abundance, log[N(X)/N(H)]+12
190-193 F4.2 [-] e_A(FeI) ? Error on A(FeI)
196-200 F5.2 [-] A(FeII) ? FeII abundance, log[N(X)/N(H)]+12
202-205 F4.2 [-] e_A(FeII) ? Error on A(FeII)
209-213 F5.2 [-] A(CoI) ? CoI abundance, log[N(X)/N(H)]+12
215-218 F4.2 [-] e_A(CoI) ? Error on A(CoI)
221-225 F5.2 [-] A(NiI) ? NiI abundance, log[N(X)/N(H)]+12
227-230 F4.2 [-] e_A(NiI) ? Error on A(NiI)
233-237 F5.2 [-] A(CuI) ? CuI abundance, log[N(X)/N(H)]+12
239-242 F4.2 [-] e_A(CuI) ? Error on A(CuI)
245-249 F5.2 [-] A(ZnI) ? ZnI abundance, log[N(X)/N(H)]+12
251-254 F4.2 [-] e_A(ZnI) ? Error on A(ZnI)
257-261 F5.2 [-] A(YII) ? YII abundance, log[N(X)/N(H)]+12
263-266 F4.2 [-] e_A(YII) ? Error on A(YII)
269-273 F5.2 [-] A(BaII) ? BaII abundance, log[N(X)/N(H)]+12
276-279 F4.2 [-] e_A(BaII) ? Error on A(BaII)
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Acknowledgements:
Piercarlo Bonifacio, Piercarlo.Bonifacio(at)obspm.fr
References:
Starkenburg et al., Paper I 2017MNRAS.471.2587S 2017MNRAS.471.2587S
Youakim et al., Paper III 2017MNRAS.472.2963Y 2017MNRAS.472.2963Y
Starkenburg et al., Paper IV 2018MNRAS.481.3838S 2018MNRAS.481.3838S
(End) Piercarlo Bonifacio [GEPI, France]. Patricia Vannier [CDS] 02-May-2019