J/MNRAS/515/1841 M37 ugi observations and memberships study (Griggio+, 2022)
Astro-photometric study of M37 with Gaia and wide-field ugi-imaging.
Griggio M., Bedin L.R., Raddi R., Reindl N., Tomasella L., Scalco M.,
Salaris M., Cassisi S., Ochner P., Ciroi S., Rosati P., Nardiello D.,
Anderson J., Libralato M., Bellini A., Vallenari A., Spina L., Pedani M.
<Mon. Not. R. Astron. Soc. 515, 1841 (2022)>
=2022MNRAS.515.1841G 2022MNRAS.515.1841G (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Photometry ; Ultraviolet ; Optical ; Infrared ;
Positional data ; Parallaxes, trigonometric ; Proper motions
Keywords: catalogues - white dwarfs -
open clusters and associations: individual: M37 (NGC 2099)
Abstract:
We present an astrometric and photometric wide-field study of the
Galactic open star cluster M37 (NGC 2099). The studied field was
observed with ground-based images covering a region of about four
square degrees in the Sloan-like filters ugi. We exploited the Gaia
catalogue to calibrate the geometric distortion of the large field
mosaics, developing software routines that can be also applied to
other wide-field instruments. The data are used to identify the
hottest white dwarf (WD) member candidates of M37. Thanks to the Gaia
EDR3 exquisite astrometry we identified seven such WD candidates, one
of which, besides being a high-probability astrometric member, is the
putative central star of a planetary nebula. To our knowledge, this is
a unique object in an open cluster, and we have obtained follow-up
low-resolution spectra that are used for a qualitative
characterization of this young WD. Finally, we publicly release a
three-colour atlas and a catalogue of the sources in the field of
view, which represents a complement of existing material.
Description:
In scope of WD member candidates study, we firstly use membership
probabilities, astrometric parameters and CMD diagrams in ugi sloan
filters to select cluster members. As presented in the section 2 Data
set, we collect data with the Schmidt 67/92 cm telescope in Asiago
use for photometry centered on M37 FOV (i.e section 2 and 3 to see all
photometry procedures and calibrations). Next, we use membership
probabilities derived from Griggio & Bedin (2022MNRAS.511.4702G 2022MNRAS.511.4702G, Cat.
J/MNRAS/511/4702) and selection tests for highly reliable cluster
members with GaiaEDR3 astrometric and phometric data as illustrated in
figure 5 of the section 4. The results and informations are available
in table.dat for 210907 stars in the M37 FOV in which 1868 stars are
considered as M37 star members.
Objects:
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RA (2000) DE Designation(s)
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05 52 17.76 +32 32 42.0 M37 = C 0549+325
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table.dat 318 210907 Final photometric, astrometric and membership
for the M37 field of view
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See also:
J/MNRAS/511/4702 : Membership probabilities of M 37 stars (Griggio+, 2022)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
J/MNRAS/399/323 : Simulated UVEX colors with reddening (Groot+, 2009)
V/165 : IGAPS. merged IPHAS and UVEX of northern Galactic plane
(Monguio+, 2020)
J/ApJ/842/6 : Astro-photometric catalog of the core of NGC 5139
(Bellini+, 2017)
J/ApJ/912/165 : Massive white dwarfs in young star clusters (Richer+, 2021)
J/MNRAS/490/1821 : Abundances for stars in 18 open clusters (Casamiquela+,2019)
J/A+A/585/A150 : On the metallicity of open clusters. III. (Netopil+, 2016)
J/A+A/561/A93 : On the metallicity of open clusters. II. (Heiter+, 2014)
J/A+A/511/A56 : Abundances of five open clusters (Pancino+, 2010)
J/A+A/438/1163 : Catalogue of Open Cluster Data (COCD) (Kharchenko+, 2005)
J/A+A/477/165 : Nearby open clusters tidal radii and masses (Piskunov+,2008)
Byte-by-byte Description of file: table.dat
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Bytes Format Units Label Explanations
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1- 19 I19 --- GaiaEDR3 ?=0 Gaia EDR3 id of the source (gid)
21- 30 F10.6 deg RAdeg ?=999 Right ascension from Gaia EDR3 (ICRS)
at Ep=2016.0 (ra)
32- 41 F10.6 deg DEdeg ?=999 Declination from Gaia EDR3 (ICRS)
at Ep=2016.0 (dec)
43- 51 F9.4 pix xpos Calculated mean position bin pixel in x ccd
direction (x) (1)
53- 61 F9.4 pix ypos Calculated mean position bin pixel in y ccd
direction (y) (1)
63- 73 F11.6 mag imag Apparent magnitude in i Sloan filter (i)
75- 87 E13.7 mag e_imag []? Mean error of imag (ei)
89 A1 --- n_imag Note takes i for suspicious imag and e_imag
values (n_imag)
91-101 F11.6 mag gmag Apparent magnitude in g Sloan filter (g)
103-115 E13.7 mag e_gmag []? Mean error of gmag (eg)
117 A1 --- n_gmag Note takes i for suspicious gmag and e_gmag
values (n_gmag)
119-129 F11.6 mag umag Apparent magnitude in u Sloan filter (u)
131-143 E13.7 mag e_umag []? Mean error of umag (eu)
145 A1 --- n_umag Note takes i for suspicious umag and e_umag
values (n_umag)
147-153 F7.5 --- q_imag Quality of the PSF fit for i Sloan filter
done by KS2 software as exposed in section
3.4 Second-pass photometry (qi) (2)
155-161 F7.5 --- q_gmag Quality of the PSF fit for g Sloan filter
done by KS2 software as exposed in section
3.4 Second-pass photometry (qg) (2)
163-169 F7.5 --- q_umag Quality of the PSF fit for u Sloan filter
done by KS2 software as exposed in section
3.4 Second-pass photometry (qu) (2)
171-178 F8.5 --- Fraci Positive or negative fraction of flux within
the PSF aperture in i Sloan filter due to
neighbours stars (oi)
180-187 F8.5 --- Fracg Positive or negative fraction of flux within
the PSF aperture in g Sloan filter due to
neighbours stars (og)
189-196 F8.5 --- Fracu Positive or negative fraction of flux within
the PSF aperture in u Sloan filter due to
neighbours stars (ou)
198 I1 --- Flagtot [0/1] Final photometric which takes 1 passed
photometric cuts in all filters (pho_sel) (3)
200 I1 --- f_imag [0/1] Photometric flag in i Sloan filter
takes 1 if the source is above 3σ
(phoseli) (3)
202 I1 --- f_gmag [0/1] Photometric flag in g Sloan filter
takes 1 if the source is above 3σ
(phoselg) (3)
204 I1 --- f_umag [0/1] Photometric flag in u Sloan filter
takes 1 if the source is above 3σ
(phoselu) (3)
206-212 F7.3 mag Gmag ?=999 G-band mean magnitude (Vega) from
Gaia EDR3 (G)
214-222 F9.5 mag e_Gmag ?=999 Standard error of Gmag (eG)
224-230 F7.3 mag BPmag ?=999 Integrated BP mean magnitude (Vega)
from Gaia EDR3 (Gbp)
232-240 F9.5 mag e_BPmag ?=999 Standard error of BPmag (eGbp)
242-248 F7.3 mag RPmag ?=999 Integrated RP mean magnitude (Vega)
from Gaia EDR3 (Grp)
250-258 F9.5 mag e_RPmag ?=999 Standard error of RPmag (eGrp)
260-266 F7.3 mas Plx ?=999 Absolute stellar parallax of the
source at the Ep=2016.0 from Gaia EDR3 (PI)
268-274 F7.3 mas e_Plx ?=999 Standard error of Plx (ePI)
276-282 F7.3 mas/yr pmRA ?=999 Proper motion in right ascension
pmRA*cosDE of the source in ICRS at
Ep=2016.0 from Gaia EDR3 (muRa)
284-290 F7.3 mas/yr e_pmRA ?=999 Standard error of pmRA (emuRa)
292-299 F8.3 mas/yr pmDE ?=999 Proper motion in declination direction
from Gaia EDR3 (muDec)
301-307 F7.3 mas/yr e_pmDE ?=999 Standard error of pmDE (emuDec)
309-316 F8.3 --- Pmemb ?=-999 Computed membership probability
including the parallax distribution proposed
by Griggio et al. (2022MNRAS.511.4702G 2022MNRAS.511.4702G,
Cat. J/MNRAS/511/4702) (P)
318 I1 --- f_Pmemb [0/1] Flag takes 1 for 1868 cases when stars
passed selction criteria as illustrated by
figure 5 of the section 4 (member)
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Note (1): As explained in section 3.3 The master frame, on the plane tangent
to the celestial sphere at the central point of the FOV, we
computed for each star the transformed positions x and y.
Note (2): The qfit measures how well a source is fitted by the PSF. It
ranges to 0 (bad fit) from 1 (indicates a perfect fit) (i.e section 5
Sloan colour-magnitude diagrams).
Note (3): As explicited in figure 6 of the section 5, we combined PSF quality
flag a selection for sources that are at least 3σ above the sky
background for each filter. Then if all flags are respected, Flagtot
takes 1.
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 17-Jun-2025