J/A+A/654/A105 MATLAS ultra diffuse galaxies (Marleau+, 2021)
Ultra diffuse galaxies in the MATLAS low-to-moderate density fields.
Marleau F.R., Habas R., Poulain M., Duc. P.A., Mueller O., Lim S.,
Durrell P.R., Sanchez-Janssen R., Paudel S., Ahad S.L., Chougule A.,
Bilek M., Fensch J.
<Astron. Astrophys. 654, A105 (2021)>
=2021A&A...654A.105M 2021A&A...654A.105M (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Galaxies, nearby ; Galaxies, optical ;
Galaxies, photometry ; Magnitudes
Keywords: Galaxy: general - galaxies: formation - galaxies: dwarf -
galaxies: fundamental parameters - galaxies: nuclei -
galaxies: star clusters: general
Abstract:
Recent advances in deep dedicated imaging surveys over the past decade
have uncovered a surprisingly large number of extremely faint low
surface brightness galaxies with large physical sizes called ultra
diffuse galaxies (UDGs) in clusters and, more recently, in lower
density environments. As part of the Mass Assembly of early-Type
GaLAxies with their fine Structures (MATLAS) survey, a deep imaging
large program at the Canada-France-Hawaii Telescope (CFHT), our team
has identified 2210 dwarf galaxies, 59 (∼3%) of which qualify as UDGs.
Averaging over the survey area, we find ∼0.4 UDG per square degree.
They are found in a range of low to moderate density environments,
although 61% of the sample fall within the virial radii of groups.
Based on a detailed analysis of their photometric and structural
properties, we find that the MATLAS UDGs do not show significant
differences from the traditional dwarfs, except from the predefined
size and surface brightness cut. Their median color is as red as the
one measured in galaxy clusters, albeit with a narrower color range.
The majority of the UDGs are visually classified as dwarf ellipticals
with log stellar masses of 6.5-8.7. The fraction of nucleated UDGs
(∼34%) is roughly the same as the nucleated fraction of the
traditional dwarfs. Only five (∼8%) UDGs show signs of tidal
disruption and only two are tidal dwarf galaxy candidates. A study of
globular cluster (GC) candidates selected in the CFHT images finds no
evidence of a higher GC specific frequency S_N for UDGs than for
classical dwarfs, contrary to what is found in most clusters. The UDG
halo-to-stellar mass ratio distribution, as estimated from the GC
counts, peaks at roughly the same value as for the traditional dwarfs,
but spans the smaller range of ∼10-2000. We interpret these results to
mean that the large majority of the field-to-group UDGs do not have a
different formation scenario than traditional dwarfs.
Description:
This work is based on data in the g, r and i-band from the MATLAS
survey (Duc et al., 2015, Cat. J/MNRAS/446/120) performed with the
Canada-France-Hawaii Telescope. This catalogue presents the properties
of the 59 MATLAS ultra diffuse galaxies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 96 59 Photometric properties of the MATLAS UDGs
table2.dat 93 59 Additional properties of the MATLAS UDGs
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See also:
J/MNRAS/446/120 : ATLAS3D project. XXIX (Duc+, 2015)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name UDG ID, MATLAS-NNNN
13- 20 F8.4 deg RAdeg Right ascension (J2000)
22- 28 F7.4 deg DEdeg Declination (J2000)
30- 33 A4 --- Morph Morphology
35- 38 F4.1 --- Dist1 Assumed host ETG distance
40- 43 F4.1 --- Dist2 ?=- Dwarf distance
45- 50 F6.3 mag gmag Apparent magnitude in the g-band
52- 56 F5.3 mag e_gmag Apparent magnitude in the g-band erro
58- 63 F6.3 mag g-r ?=- g-r color corrected for Galactic extinction
65- 69 F5.3 mag e_g-r ?=- g-r color corrected for Galactic
extinction error
71- 76 F6.3 mag g-i ?=- g-i color corrected for Galactic extinction
78- 82 F5.3 mag e_g-i ?=- g-i color corrected for Galactic
extinction error
84- 90 F7.3 mag gMAG Absolute magnitude in the g-band (1)
92- 96 F5.3 mag e_gMAG Absolute magnitude in the g-band (1)
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Note (1): computed using the UDG distance when available, otherwise the assumed
host ETG distance is used.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name UDG ID, MATLAS-NNNN
13- 18 F6.3 mag/arcsec2 mu0 Central surface brightness in the g-band
20- 24 F5.3 mag/arcsec2 e_mu0 Central surface brightness in
the g-band error
26- 31 F6.3 mag/arcsec2 mueavg Average surface brightness within one
effective radius in the g-band
33- 37 F5.3 mag/arcsec2 e_mueavg Average surface brightness within one
effective radius in the g-band
39- 44 F6.3 arcsec Re Effective radius in arcsec in the g-band
46- 50 F5.3 arcsec e_Re Effective radius in arcsec in the g-band
52- 56 F5.3 kpc Rekpc Effective radius in kpc
in the g-band (1)
58- 62 F5.3 kpc e_Rekpc Effective radius in kpc
in the g-band error (1)
64- 67 F4.2 [Msun] log(M*) ?=- Stellar mass computed based on the
stellar mass-to-light ratios (2)
69- 72 F4.2 [Msun] e_log(M*) ? Stellar mass computed based on the
stellar mass-to-light ratios error (2)
74- 79 F6.1 --- Mhalo/M* ?=- Halo-to-stellar mass ratio (3)
81- 86 F6.1 --- e_Mhalo/M* ? Error on halo-to-stellar mass ratio,
lower value
88- 93 F6.1 --- E_Mhalo/M* ? Error on halo-to-stellar mass ratio,
upper value
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Note (1): Effective radius in kpc computed using the UDG distance when
available, otherwise the assumed host distance is used.
Note (2): from Bell et al. (2003ApJS..149..289B 2003ApJS..149..289B) and the derived g-r color.
Note (3): computed based on the mass ratio from Harris et al.
(2017) and the derived GC count.
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Acknowledgements:
Francine Marleau, francine.marleau(at)uibk.ac.at
(End) Patricia Vannier [CDS] 24-Sep-2021