J/MNRAS/460/1131 Selection function of Milky Way field stars (Stonkute+, 2016)
The Gaia-ESO Survey: the selection function of the Milky Way field stars.
Stonkute E., Koposov S.E., Howes L.M., Feltzing S., Worley C.C.,
Gilmore G., Ruchti G.R., Kordopatis G., Randich S., Zwitter T., Bensby T.,
Bragaglia A., Smiljanic R., Costado M.T., Tautvaisiene G., Casey A.R.,
Korn A.J., Lanzafame A.C., Pancino E., Franciosini E., Hourihane A.,
Jofre P., Lardo C., Lewis J., Magrini L., Monaco L., Morbidelli L.,
Sacco G.G., Sbordone L.
<Mon. Not. R. Astron. Soc., 460, 1131-1146 (2016)>
=2016MNRAS.460.1131S 2016MNRAS.460.1131S (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Surveys ; Populations, stellar
Keywords: techniques: spectroscopic - surveys - stars: general -
Galaxy: evolution
Abstract:
The Gaia-ESO Survey was designed to target all major Galactic
components (i.e. bulge, thin and thick discs, halo and clusters), with
the goal of constraining the chemical and dynamical evolution of the
Milky Way. This paper presents the methodology and considerations that
drive the selection of the targeted, allocated and successfully
observed Milky Way field stars. The detailed understanding of the
survey construction, specifically the influence of target selection
criteria on observed Milky Way field stars is required in order to
analyse and interpret the survey data correctly. We present the target
selection process for the Milky Way field stars observed with Very
Large Telescope/Fibre Large Array Multi Element Spectrograph and
provide the weights that characterize the survey target selection. The
weights can be used to account for the selection effects in the
Gaia-ESO Survey data for scientific studies. We provide a couple of
simple examples to highlight the necessity of including such
information in studies of the stellar populations in the Milky Way.
Description:
The observations are conducted with the FLAMES (Pasquini et al.,
2002Msngr.110....1P 2002Msngr.110....1P) at the Very Large Telescope (VLT) array operated
by the European Southern Observatory on Cerro Paranal, Chile. FLAMES
is a fibre facility of the VLT and is mounted at the Nasmyth A
platform of the second Unit Telescope of VLT.
In this paper, we present the Gaia-ESO Survey selection function only
for the Milky Way field stars observed with the GIRAFFE and UVES
spectrographs at VLT, not including the bulge. All targets were
selected according to their colours and magnitudes, using photometry
from the VISTA Hemisphere Survey (VHS; McMahon et al.
2013Msngr.154...35M 2013Msngr.154...35M) and the Two Micron All-Sky Survey (2MASS;
Skrutskie et al., 2006, Cat. VII/233). Selected potential target lists
were generated at the Cambridge Astronomy Survey Unit (CASU) centre.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 226 330 Main parameters and weights of the targeted and
allocated Milky Way fields
table5.dat 84 7888 CMD weights of successfully observed stars with
GIRAFFE in iDR4
table6.dat 71 1367 CMD weights of successfully observed stars with
UVES in iDR4
--------------------------------------------------------------------------------
See also:
J/A+A/598/A5 : Gaia-ESO Survey iDR4 calibrators (Pancino+, 2017)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 20 A20 --- Field GES Milky Way field name from CASU (GES_FLD)
22- 23 I2 h RAh Right ascension of GES Milky Way field
centre (J2000)
25- 26 I2 min RAm Right ascension of GES Milky Way field
centre (J2000)
28- 33 F6.3 s RAs Right ascension of GES Milky Way field
centre (J2000)
35 A1 --- DE- Declination sign of GES Milky Way field
centre (J2000)
36- 37 I2 deg DEd Declination of GES Milky Way field
centre (J2000)
39- 40 I2 arcmin DEm Declination of GES Milky Way field
centre (J2000)
42- 46 F5.2 arcsec DEs Declination of GES Milky Way field
centre (J2000)
48- 52 F5.3 mag E(B-V) Galactic dust extinction median value measured
from the Schlegel, Finkbeiner & Davis
(1998ApJ...500..525S 1998ApJ...500..525S) maps
54- 58 F5.3 --- DG ?=- Right-edge limit of second priority
targets for GIRAFFE (ΔG)
60- 64 F5.3 --- DU ?=- Right-edge limit of second priority
targets for UVES (ΔU)
66- 70 F5.3 --- WTFbG ?=- Weight of blue box for GIRAFFE (1)
72- 76 F5.3 --- WTFb1G ?=- Weight of blue box with J1 for GIRAFFE (1)
78- 82 F5.3 --- WTFb2G ?=- Weight of blue box with J2 for GIRAFFE (1)
84- 88 F5.3 --- WTFb3G ?=- Weight of blue box with J3 for GIRAFFE (1)
90- 94 F5.3 --- WTFb4G ?=- Weight of blue box with J4 for GIRAFFE (1)
96-100 F5.3 --- WTFrG ?=- Weight of red box for GIRAFFE (1)
102-106 F5.3 --- WTFeG ?=- Weight of extra red box for GIRAFFE (1)
108-112 F5.3 --- WATbG ?=- Weight of blue box for GIRAFFE (2)
114-118 F5.3 --- WATb1G ?=- Weight of blue box with J1 for GIRAFFE (2)
120-124 F5.3 --- WATb2G ?=- Weight of blue box with J2 for GIRAFFE (2)
126-130 F5.3 --- WATb3G ?=- Weight of blue box with J3 for GIRAFFE (2)
132-136 F5.3 --- WATb4G ?=- Weight of blue box with J4 for GIRAFFE (2)
138-142 F5.3 --- WATrG ?=- Weight of red box for GIRAFFE (2)
144-148 F5.3 --- WATeG ?=- Weight of extra box for GIRAFFE (2)
150-154 F5.3 --- WTFbU ?=- Weight of blue box for UVES (1)
156-160 F5.3 --- WTFb1U ?=- Weight of blue box with J1 for UVES (1)
162-166 F5.3 --- WTFb2U ?=- Weight of blue box with J2 for UVES (1)
168-172 F5.3 --- WTFb3U ?=- Weight of blue box with J3 for UVES (1)
174-178 F5.3 --- WTFb4U ?=- Weight of blue box with J4 for UVES (1)
180-184 F5.3 --- WTFeU ?=- Weight of extra box for UVES (1)
186-190 F5.3 --- WATbU ?=- Weight of blue box for UVES (2)
192-196 F5.3 --- WATb1U ?=- Weight of blue box with J1 for UVES (2)
198-202 F5.3 --- WATb2U ?=- Weight of blue box with J2 for UVES (2)
204-208 F5.3 --- WATb3U ?=- Weight of blue box with J3 for UVES (2)
210-214 F5.3 --- WATb4U ?=- Weight of blue box with J4 for UVES (2)
216-220 F5.3 --- WATeU ?=- Weight of extra box for UVES (2)
222-226 F5.3 % BlueFract Approximate fraction of targets in the blue
versus the red box
--------------------------------------------------------------------------------
Note (1): where targeted star counts are versus star counts in 1°FoV.
Note (2): where allocated star counts are versus targeted star counts.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- CName CNAME (HHMMSSss+DDMMSSs, J2000)
18- 37 A20 --- Field GES field (GES_FLD)
39- 46 F8.4 deg RAdeg Right ascension (J2000)
48- 55 F8.4 deg DEdeg Declination (J2000)
57- 65 F9.7 --- WOFG Weight of a successfully observed target
in each CMD bin
67- 75 F9.7 --- WTotG Total Weight
77- 84 A8 --- Box Box (Blue or Red/Blue)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- CName CNAME (HHMMSSss+DDMMSSs, J2000)
18- 37 A20 --- Field GES field (GES_FLD)
39- 46 F8.4 deg RAdeg Right ascension (J2000)
48- 55 F8.4 deg DEdeg Declination (J2000)
57- 63 F7.5 --- WOFU Weight of a successfully observed target
in each CMD bin
65- 71 F7.5 --- WTotU Total Weight
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 06-Oct-2017