J/MNRAS/490/2241 Spectroscopy of Pristine EMP star candidates (Aguado+, 2019)
The Pristine survey - VI.
The first three years of medium-resolution follow-up spectroscopy of Pristine
EMP star candidates.
Aguado D.S., Youakim K., Gonzalez Hernandez J.I., Allende Prieto C.,
Starkenburg E., Martin N., Bonifacio P., Arentsen A., Caffau E.,
Peralta de Arriba L., Sestito F., Garcia-Dias R., Fantin N., Hill V.,
Jablonca P., Jahandar F., Kielty C., Longeard N., Lucchesi R.,
Sanchez-Janssen R., Osorio Y., Palicio P.A., Tolstoy E., Wilson T.G.,
Cote P., Kordopatis G., Lardo C., Navarro J.F., Thomas G.F., Venn K.
<Mon. Not. R. Astron. Soc., 490, 2241-2253 (2019)>
=2019MNRAS.490.2241A 2019MNRAS.490.2241A (SIMBAD/NED BibCode)
ADC_Keywords: Abundances, [Fe/H] ; Photometry ; Spectroscopy ;
Effective temperatures ; Optical
Keywords: stars: abundances - Galaxy: evolution - Galaxy: formation -
Local Group - dark ages, reionization, first stars - early Universe
Abstract:
We present the results of a 3-yr long, medium-resolution spectroscopic
campaign aimed at identifying very metal-poor stars from candidates
selected with the CaHK, metallicity-sensitive Pristine survey. The
catalogue consists of a total of 1007 stars, and includes 146
rediscoveries of metal-poor stars already presented in previous
surveys, 707 new very metal-poor stars with [Fe/H]←2.0, and 95 new
extremely metal-poor stars with [Fe/H]←3.0. We provide a
spectroscopic [Fe/H] for every star in the catalogue, and [C/Fe]
measurements for a subset of the stars (10 per cent with [Fe/H]←3 and
24 per cent with -3<[Fe/H]←2) for which a carbon determination is
possible, contingent mainly on the carbon abundance, effective
temperature and signal-to-noise ratio of the stellar spectra. We find
an average carbon enhancement fraction ([C/Fe]≥+0.7) of 41±4 per
cent for stars with -3<[Fe/H]←2 and 58±14 per cent for stars with
[Fe/H]←3, and report updated success rates for the Pristine survey of
56 per cent and 23 per cent to recover stars with [Fe/H]←2.5 and ←3,
respectively. Finally, we discuss the current status of the survey and
its preparation for providing targets to upcoming multi-object
spectroscopic surveys such as William Herschel Telescope Enhanced Area
Velocity Explorer.
Description:
The spectroscopic data presented here were collected over a period of
six semesters, from 2016 March to 2019 February. Due to the wide range
in target brightness, three different facilities were used to conduct
follow-up observations of EMP candidates selected from the Pristine
survey: the Intermediate Dispersion Spectrograph (IDS) on the 2.5-m
Isaac Newton Telescope (INT), the Intermediate-dispersion Spectrograph
and Imaging System (ISIS, Jorden 1990SPIE.1235..790J 1990SPIE.1235..790J) on the 4.2-m
William Herschel Telescope (WHT), and the ESO Faint Object
Spectrograph and Camera (EFOSC2, Buzzoni et al. 1984Msngr..38....9B 1984Msngr..38....9B)
on the 3.6-m New Technology Telescope (NTT).
The minimum desired signal-to-noise (S/N) ratio per pixel for the
observations was ∼15-25 in the calcium H & K spectral region
(∼3950Å), depending on the effective temperature of the specific
star. Therefore, the average exposure time for a single integration
was 1500, 900, and 1500s, for the INT, ISIS, and EFOSC observations,
respectively.
Table 4 is a catalogue of 1007 stars from three years of follow-up
spectroscopy of Pristine candidates.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 130 1007 Efective temperatures, surface gravities,
metallicities and carbon abundances of the
Pristine spectroscopic sample
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See also:
J/AN/338/686 : Pristine survey II. Bright stars abundances (Caffau+, 2017)
J/MNRAS/472/2963 : Metallicities of Pristine stars (Youakim+, 2017)
J/MNRAS/487/3797 : A bright star sample observed with SOPHIE
(Bonifacio+, 2019)
J/MNRAS/519/5554 : Pristine survey. XX. (Arentsen+, 2023)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Pristine stat name (PDDD.dddd+DD.dddd)
19 A1 --- f_Name [*] Flag on Name (1)
21- 32 F12.8 deg RAdeg Right ascension (J2000)
34- 44 F11.8 deg DEdeg Declination (J2000)
46- 51 F6.3 mag Vmag SDSS V magnitude derived using g and r (2)
53- 58 F6.3 mag CaHKmag Magnitude obtained from the Pristine
narrow-band filter
60- 64 F5.3 mag e_CaHKmag Error on CaHKmag
66- 71 F6.2 [-] [Fe/H]P Photometric metallicity determined using
the (g-i)0 SDSS colours and Pristine
photometry
73- 77 F5.2 [-] [Fe/H]F Spectroscopic metallicity derived from FERRE
79- 83 F5.2 [-] e_[Fe/H]F Error on [Fe/H]F
85- 88 I4 K Teff Effective temperature derived from FERRE
90- 92 I3 K e_Teff Error on Teff
94- 96 F3.1 [cm/s2] logg Surface gravity derived from FERRE
98-100 F3.1 [cm/s2] e_logg Error on logg
102-106 F5.2 [-] [C/Fe] C/Fe abundance ratio derived from FERRE
108-112 F5.2 [-] e_[C/Fe] Error on [C/Fe]
114 A1 --- q_[Fe/H]F [TX] Quality flag on [Fe/H]F (3)
116-117 I2 --- q_[C/Fe] [-1/1] Quality flag on [C/Fe] (4)
119-130 A12 --- prevobs Other survey(s) with spectroscopic
observations of the source
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Note (1): Flag as follows:
* = Coordinates of select stars have been removed as they are the subject
of an ongoing high-resolution follow-up study (Kietly et al.,
in preparation)
Note (2): Magnitude derived using SDSS g and r according to
https://www.sdss3.org/dr8/algorithms/sdssUBVRITransform.php
Note (3): Quality flag as follows:
T = Stars for which the S/N is too low for a robust determination of stellar
parameters, but that still has some information in the observed
spectrum, and are good candidates to be re-observed with higher S/N and
at higher resolution facilities (6 per cent of the sample) (66/1007)
X = Synthetic spectral fit was reliable and that the given [Fe/H]F value
can be trusted to within the provided uncertainties (93 per cent of the
sample have this flag) (941/1007)
Note (4): Quality flag as follows:
-1 = The carbon determination is not reliable (173/1007)
1 = The carbon determination is reliable (834/1007)
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History:
From electronic version of the journal
References:
Starkenburg et al., Paper I 2017MNRAS.471.2587S 2017MNRAS.471.2587S
Caffau et al., Paper II 2017AN....338..686C 2017AN....338..686C, Cat. J/AN/338/686
Youakim et al., Paper III 2017MNRAS.472.2963Y 2017MNRAS.472.2963Y, Cat. J/MNRAS/472/2963
Starkenburg et al., Paper IV 2018MNRAS.481.3838S 2018MNRAS.481.3838S
Bonifacio et al., Paper V 2019MNRAS.487.3797B 2019MNRAS.487.3797B, Cat. J/MNRAS/487/3797
Starkenburg et al., Paper VII 2019MNRAS.490.5757S 2019MNRAS.490.5757S
Youakim et al., Paper VIII 2020MNRAS.492.4986Y 2020MNRAS.492.4986Y
Venn et al., Paper IX 2020MNRAS.492.3241V 2020MNRAS.492.3241V
Sestito et al., Paper X 2020MNRAS.497L...7S 2020MNRAS.497L...7S
Caffau et al., Paper XI 2020MNRAS.493.4677C 2020MNRAS.493.4677C
Kielty et al., Paper XII 2021MNRAS.506.1438K 2021MNRAS.506.1438K
Fernandez-Alvar et al., Paper XIII 2021MNRAS.508.1509F 2021MNRAS.508.1509F
Lardo et al., Paper XIV 2021MNRAS.508.3068L 2021MNRAS.508.3068L
Lucchesi et al., Paper XV 2022MNRAS.511.1004L 2022MNRAS.511.1004L
Martin et al., Paper XVI 2022MNRAS.516.5331M 2022MNRAS.516.5331M
Yuan et al. Paper XVII 2022MNRAS.514.1664Y 2022MNRAS.514.1664Y
Errani et al., Paper XVIII 2022MNRAS.514.3532E 2022MNRAS.514.3532E
Caffau et al., Paper XIX 2023MNRAS.518.3796C 2023MNRAS.518.3796C
Arentsen et al., Paper XX 2023MNRAS.519.5554A 2023MNRAS.519.5554A, Cat. J/MNRAS/519/5554
(End) Ana Fiallos [CDS] 30-Jan-2023