J/A+A/692/A115 Pristine survey DR1 (Martin+, 2024)
The Pristine survey. XXIII. Data Release 1 and an all-sky metallicity catalogue
based on Gaia DR3 BP/RP spectro-photometry.
Martin N.F., Starkenburg E., Yuan Z., Fouesneau M., Ardern-Arentsen A.,
De Angeli F., Gran F., Montelius M., Rusterucci S., Andrae R.,
Bellazzini M., Montegriffo P., Esselink A.F., Zhang H., Venn K.A.,
Viswanathan A., Aguado D.S., Battaglia G., Bayer M., Bonifacio P.,
Caffau E., Cote P., Carlberg R., Fabbro S., Fernandez-Alvar E.,
Gonzalez Hernandez J.I., Gonzalez Rivera de La Vernhe I., Hill V.,
Ibata R.A., Jablonka P., Kordopatis G., Lardo C., McConnachie A.W.,
Navarrete C., Navarro J., Recio-Blanco A., Sanchez Janssen R., Sestito F.,
Thomas G.F., Vitali S., Youakim K.
<Astron. Astrophys. 692, A115 (2024)>
=2024A&A...692A.115M 2024A&A...692A.115M (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Milky Way ; Abundances ; Optical
Keywords: catalogs - surveys - stars: abundances - Galaxy: abundances
Abstract:
We used the spectro-photometric information of ∼219 million stars
from Gaia's Data Release 3 (DR3) to calculate synthetic, narrowband,
metallicity-sensitive CaHK magnitudes that mimic the observations of
the Pristine survey, a survey of photometric metallicities of Milky
Way stars that has been mapping more than 6500 deg2of the northern
sky with the Canada-France-Hawaii Telescope since 2015. These
synthetic magnitudes were used for an absolute recalibration of the
deeper Pristine photometry and, combined with broadband Gaia
information, synthetic and Pristine CaHK magnitudes were used to
estimate photometric metallicities over the whole sky. The resulting
metallicity catalogue is accurate down to [Fe/H]~-3.5 and is
particularly suited for the exploration of the metalpoor Milky Way
([Fe/H]←1.0). We make available here the catalogue of synthetic
CaHKsyn magnitudes for all stars with BP/RP information in Gaia DR3,
as well as an associated catalogue of more than ∼30 million
photometric metallicities for high signal-to-noise FGK stars. This
paper further provides the first public data release of the Pristine
catalogue in the form of higher quality recalibrated Pristine CaHK
magnitudes and photometric metallicities for all stars in common with
the BP/RP spectro-photometric information in Gaia DR3. We demonstrate
that, when available, the much deeper Pristine data greatly enhance
the quality of the derived metallicities, in particular at the faint
end of the catalogue (GBP~>16). Combined, both photometric
metallicity catalogues include more than two million metal-poor star
candidates ([Fe/H]phot←1.0) as well as more than 200000 and ∼8000
very and extremely metal-poor candidates ([Fe/H]phot←2.0 and ←3.0,
respectively). Finally, we show that these metallicity catalogues can
be used efficiently, among other applications, for Galactic
archaeology, to hunt for the most metal-poor stars, and to study how
the structure of the Milky Way varies with metallicity, from the flat
distribution of disk stars to the spheroid-shaped metal-poor halo.
Description:
We have taken advantage of the recently released Gaia DR3 (Cat. I/355)
spectrophotometric BP/RP information to build a catalogue of synthetic
CaHKsyn magnitudes mimicking the narrowband photometry of the Pristine
survey that, centered on the calcium H & K lines, is sensitive to the
metallicity of a star. We seize this opportunity to reprocess the full
∼11500 images of the Pristine survey gathered since 2015 and
present the current state of the survey that now covers more than
6500 deg2. In particular, we use the Gaia-based synthetic
observations to refine the calibration of the Pristine photometry with
a neural-net based algorithm, PhotCalib.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
pristine_ca.sam 130 1000 Photometry catalogue that includes both the
synthetic CaHKsyn and the Pristine CaHK
photometric information (table 1)
(219194028 sources)
pristine_gaia.sam 231 1000 Pristine-Gaia synthetic metallicity catalogue
(table 2) (52297046 sources)
pristine_dr1.sam 228 1000 Pristine DR1 metallicity catalogue
(table 3) (6380652 sources)
--------------------------------------------------------------------------------
See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: pristine_ca.sam
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaDR3 Gaia DR3 source_id (source_id)
21- 30 F10.6 deg RAdeg Gaia DR3 right ascension ICRS (J2016) (RA)
32- 41 F10.6 deg DEdeg Gaia DR3 declination ICRS (J2016) float (DE)
43- 55 E13.6 e-/s FCaHK CaHK mean flux (CaHK_flux)
57- 68 E12.6 e-/s e_FCaHK Uncertainty on the CaHK mean flux
(dCaHKflux)
70- 75 F6.3 mag CaHKsynmag CaHKsyn, synthetic Pristine-like CaHK
magnitude (CaHK_syn)
77- 86 E10.3 mag e_CaHKsynmag [] δ CaHKsyn, uncertainty on CaHKsyn
(dCaHKsyn)
88- 92 F5.3 --- Pvar Probability for the source to be variable,
as defined in section 5 (Pvar)
94-103 F10.6 deg RAPdeg ? Pristine right ascension ICRS (J2015.5)
(RA_Pr)
105-114 F10.6 deg DEPdeg ? Pristine declination ICRS (J2015.5)
(Dec_Pr)
116-121 F6.3 mag CaHKPrmag ? CaHK Pristine magnitude (CaHK_Pr)
123-127 F5.3 mag e_CaHKPrmag ? Uncertainty on the CaHK Pristine magnitude
(dCaHKPr)
129-130 I2 --- Flag Morphology and quality flag
(mergedCASUflag) (G1)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: pristine_gaia.sam
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaDR3 Gaia DR3 source_id (source_id)
21- 30 F10.6 deg RAdeg Gaia DR3 right ascension ICRS (J2016) (RA)
32- 41 F10.6 deg DEdeg Gaia DR3 declination ICRS (J2016) (Dec)
43- 48 F6.4 mag E(B-V) Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S)
extinction value (E(B-V))
50- 55 F6.3 mag Gmag0 ? De-reddened Gaia G magnitude (G_0)
57- 61 F5.3 mag e_Gmag0 δG, uncertainty on the Gaia G
magnitude (d_G)
63- 68 F6.3 mag Bpmag0 ? De-reddened Gaia GBP magnitude (BP_0)
70- 74 F5.3 mag e_Bpmag0 δGBP, uncertainty on the Gaia GBP
magnitude (d_BP)
76- 81 F6.3 mag Rpmag0 ? De-reddened Gaia GRP magnitude (RP_0)
83- 87 F5.3 mag e_Rpmag0 δGRP, uncertainty on the Gaia GRP
magnitude (d_RP)
89- 94 F6.3 mag CaHKmag0 ? De-reddened Pristine-like CaHKsyn
magnitude (CaHK_0)
96-101 F6.3 mag e_CaHKmag0 δCaHKsyn, uncertainty on the
Pristine-like CaHKsyn magnitude
(dCaHKsyn)
103-108 F6.3 [-] [Fe/H]phsyn ? Photometric metallicity [Fe/H]phot based
on the CaHKsyn magnitude and using the
(favored) giant model (FeH_CaHKsyn)
110-115 F6.3 [-] b_[Fe/H]ph ? Lower bound of the 68% confidence
interval on FeH_CaHKsyn based on the
Monte Carlo
sampling of the magnitude uncertainties
(FeHCaHKsyn16th)
117-122 F6.3 [-] [Fe/H]ph ? Median value of FeH_CaHKsyn based on the
Monte Carlo sampling of the magnitude
uncertainties (FeHCaHKsyn50th)
124-129 F6.3 [-] B_[Fe/H]ph ? Upper bound of the 68% confidence
interval on FeH_CaHKsyn based on the
Monte Carlo sampling of the magnitude
uncertainties (FeHCaHKsyn84th)
131-134 F4.2 --- MCfCaHKsyn Fraction of the Monte Carlo samples of the
magnitude uncertainties that fall outside
the model color-color space
(mcfrac_CaHKsyn)
136-141 F6.3 mag Gmag0dw ? De-reddened Gaia G magnitude for the
dwarf model (G0dw)
143-148 F6.3 mag Bpmag0dw ? De-reddened Gaia GBP magnitude for the
dwarf model (BP0dw)
150-155 F6.3 mag Rpmag0dw ? De-reddened Gaia GRP magnitude for the
dwarf model (RP0dw)
157-162 F6.3 mag CaHKmag0dw ? De-reddened Pristine-like CaHKsyn
magnitude (CaHK0dw)
164-169 F6.3 [-] [Fe/H]phsyndw ? Photometric metallicity [Fe/H]phot based
on the CaHKsyn magnitude and using the
(favored) giant model for the dwarf model
(FeHCaHKsyndw)
171-176 F6.3 [-] b_[Fe/H]phdw ? Lower bound of the 68% confidence
interval on FeH_CaHKsyn based on the
Monte Carlo sampling of the magnitude
uncertainties for the dwarf model
(FeHCaHKsyndw_16th)
178-183 F6.3 [-] [Fe/H]phdw ? Median value of FeH_CaHKsyn based on the
Monte Carlo sampling of the magnitude
uncertainties for the dwarf model
(FeHCaHKsyndw_50th)
185-190 F6.3 [-] B_[Fe/H]phdw ? Upper bound of the 68% confidence
interval on FeH_CaHKsyn based on the
Monte Carlo sampling of the magnitude
uncertainties for the dwarf model
(FeHCaHKsyndw_84th)
192-195 F4.2 --- MCfCaHKsyndw Fraction of the Monte Carlo samples of the
magnitude uncertainties that fall outside
the model color-color space
for the dwarf model (mcfracCaHKsyndw)
197-204 F8.6 --- Pvar Probability for the source to be variable,
as defined in Section 5 (Pvar)
206-212 F7.3 --- RUWE ? Gaia DR3 Renormalised Unit Weight Error
(RUWE)
214-222 F9.6 mag Cstar Gaia DR3 corrected flux excess, C*,
as defined in equation 6 of Riello et al.
(2021A&A...649A...3R 2021A&A...649A...3R) (Cstar)
224-231 F8.6 mag s_Cstar Normalized standard deviation of C* for
the G magnitude of this source, as
defined in equation 18 of Riello et al.
(2021A&A...649A...3R 2021A&A...649A...3R) (Cstar_1sigma)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: pristine_dr1.sam
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaDR3 Gaia DR3 source_id (source_id)
21- 30 F10.6 deg RAdeg Gaia DR3 right ascension ICRS (J2016) (RA)
32- 41 F10.6 deg DEdeg Gaia DR3 declination ICRS (J2016) (Dec)
43- 47 F5.3 mag E(B-V) Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S)
extinction value (E(B-V))
49- 50 I2 --- Flag Morphology and quality flag10
(mergedCASUflag) (G1)
52- 57 F6.3 mag Gmag0 De-reddened Gaia G magnitude (G_0)
59- 63 F5.3 mag e_Gmag0 δG, uncertainty on the Gaia G
magnitude (d_G)
65- 70 F6.3 mag Bpmag0 De-reddened Gaia GBP magnitude (BP_0)
72- 76 F5.3 mag e_Bpmag0 δGBP, uncertainty on the Gaia GBP
magnitude (d_BP)
78- 83 F6.3 mag Rpmag0 De-reddened Gaia GRP magnitude (RP_0)
85- 89 F5.3 mag e_Rpmag0 δGRP, uncertainty on the Gaia GRP
magnitude (d_RP)
91- 96 F6.3 mag CaHKmag0 De-reddened Pristine CaHK magnitude
(CaHK_0)
98-102 F5.3 mag e_CaHKmag0 δCaHK, uncertainty on the Pristine
CaHK magnitude (d_CaHK)
104-109 F6.3 [-] [Fe/H]phPgm ? Photometric metallicity [Fe/H]phot based
on the Pristine CaHK magnitudes and using
the (favored) giant model (FeH_Pristine)
111-116 F6.3 [-] b_[Fe/H]phP ? Lower bound of the 68% confidence
interval on FeH_Pristine based on the
Monte Carlo sampling of the magnitude
uncertainties (FeHPristine16th)
118-123 F6.3 [-] [Fe/H]phP ? Median value of FeH_Pristine based on
the Monte Carlo sampling of the magnitude
uncertainties (FeHPristine50th)
125-130 F6.3 [-] B_[Fe/H]phP ? Upper bound of the 68% confidence
interval on FeH_Pristine based on the
Monte Carlo sampling of the magnitude
uncertainties (FeHPristine84th)
132-135 F4.2 --- MCfCaHKP Fraction of the Monte Carlo samples of the
magnitude uncertainties that fall outside
the model color-color space
(mcfrac_Pristine)
137-142 F6.3 mag Gmag0dw De-reddened Gaia G magnitude for the
dwarf model (G0dw)
144-149 F6.3 mag Bpmag0dw De-reddened Gaia GBP magnitude for the
dwarf model (BP0dw)
151-156 F6.3 mag Rpmag0dw De-reddened Gaia GRP magnitude for the
dwarf model (RP0dw)
158-163 F6.3 mag CaHKmag0dw De-reddened Pristine-like CaHKsyn
magnitude (CaHK0dw)
165-170 F6.3 [-] [Fe/H]phPgmdw ? Photometric metallicity [Fe/H]phot based
on the Pristine CaHK magnitudes and using
the (favored) giant model for the dwarf
model (FeHPristinedw)
172-177 F6.3 [-] b_[Fe/H]phPdw ? Lower bound of the 68% confidence
interval on FeH_Pristine based on the
Monte Carlo sampling of the magnitude
uncertainties for the dwarf model
(FeHPristinedw_16th)
179-184 F6.3 [-] [Fe/H]phPdw ? Median value of FeH_Pristine based on
the Monte Carlo sampling of the magnitude
uncertainties for the dwarf model
(FeHPristinedw_50th)
186-191 F6.3 [-] B_[Fe/H]phPdw ? Upper bound of the 68% confidence
interval on FeH_Pristine based on the
Monte Carlo sampling of the magnitude
uncertainties for the dwarf model
(FeHPristinedw_84th)
193-196 F4.2 --- MCfCaHKPdw Fraction of the Monte Carlo samples of the
magnitude uncertainties that fall outside
the model color-color space for the dwarf
model (mcfracPristinedw)
198-203 F6.3 --- RUWE ? Gaia DR3 Renormalised Unit Weight Error
(RUWE)
205-209 F5.3 --- Pvar Probability for the source to be variable,
as defined in Section 5 (Pvar)
211-219 F9.6 mag Cstar Gaia DR3 corrected flux excess, C*, as
defined in equation 6 of Riello et al.
(2021A&A...649A...3R 2021A&A...649A...3R) (Cstar)
221-228 F8.6 mag s_Cstar Normalized standard deviation of C* for
the G magnitude of this source, as
defined in equation 18 of Riello et al.
(2021A&A...649A...3R 2021A&A...649A...3R) (Cstar_1sigma)
--------------------------------------------------------------------------------
Note (G1): Merged flag based on the CASU_flag of individual detections, as
mentioned in sub-section 3.3.1. The flag discriminates between saturated
stars (-9), likely point sources (-2), very likely point sources (-1),
extended sources (+1), discrepant flags from individual detections (+2),
merged source from individual detections with inconsistent photometry (+3).
--------------------------------------------------------------------------------
Acknowledgements:
Nicolas Martin, nicolas.martin(at)astro.unistra.fr
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/472/2953
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
Aguado et al., Paper VI 2019MNRAS.490.2241A 2019MNRAS.490.2241A, Cat. J/MNRAS/490/2241
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, cat. J/MNRAS/492/5757
Sestito et al., Paper X 2020MNRAS.497L...7S 2020MNRAS.497L...7S, Cat. J/MNRAS/497/L7
Caffau et al., Paper XI 2020MNRAS.493.4677C 2020MNRAS.493.4677C, Cat. J/MNRAS/493/4677
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
Lombardo et al., Paper XXI 2023MNRAS.522.4815L 2023MNRAS.522.4815L
Sitnova et al., Paper XXII 2023MNRAS.526.5976S 2023MNRAS.526.5976S
(End) Francois-Xavier Pineau, Patricia Vannier [CDS] 27-Nov-2024