J/A+A/667/A76 64 Virgo galaxies radial surface brightness (Junais+, 2022)
A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE). XIII.
The role of ram-pressure stripping in transforming the diffuse and ultra-diffuse
galaxies in the Virgo cluster .
Junais S., Boissier S., Boselli A., Ferrarese L., Cote P., Gwyn S.,
Roediger J., Lim S., Peng E.W., Cuillandre J.-C., Longobardi A., Fossati M.,
Hensler G., Koda J., Bautista J., Boquien M., Malek K., Amram P., Roehlly Y.
<Astron. Astrophys. 667, A76 (2022)>
=2022A&A...667A..76J 2022A&A...667A..76J (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, photometry ; Photometry, SDSS ;
Photometry, H-alpha ; Photometry, ultraviolet
Keywords: galaxies: clusters: general - galaxies: clusters: individual: Virgo -
galaxies: evolution - galaxies: interactions -
galaxies: star formation
Abstract:
Low-surface-brightness galaxies (LSBs) contribute to a significant
fraction of all the galaxies in the Universe. Ultra-diffuse galaxies
(UDGs) form a subclass of LSBs that has attracted a lot of attention
in recent years (although its definition may vary between studies).
Although UDGs are found in large numbers in galaxy clusters, groups,
and in the field, their formation and evolution are still very much
debated. Using a comprehensive set of multiwavelength data from the
NGVS (optical), VESTIGE (Halpha narrowband), and GUViCS (UV) surveys,
we studied a sample of 64 diffuse galaxies and UDGs in the Virgo
cluster to investigate their formation history. We analyzed the
photometric colors and surface-brightness profiles of these galaxies
and then compared them to models of galaxy evolution, including
ram-pressure stripping (RPS) events to infer any possible strong
interactions with the hot cluster gas in the past. While our sample
consists mainly of red LSBs, which is typical in cluster environments,
we found evidence of a color variation with the cluster-centric
distance. Blue, HI-bearing, star-forming diffuse galaxies are found at
larger distances from the cluster center than the rest of the sample.
The comparison of our models with multifrequency observations suggests
that most of the galaxies of the sample might have undergone a strong
RPS event in their lifetime, on average 1.6Gyr ago (with a large
dispersion, and RPS still ongoing for some of them). This process
resulted in the transformation of initially gas-rich diffuse blue
galaxies into gas-poor and red ones that form the dominant population
now, the more extreme UDGs having undergone the process in a more
distant past on average. The RPS in dense environments could be one of
the major mechanisms for the formation of the large number of
quiescent UDGs we observe in galaxy clusters.
Description:
Multi-wavelength images and radial surface brightness profiles in
eight photometric bands for a sample of 64 diffuse and ultra-diffuse
galaxies in the Virgo cluster are provided. The original data are
taken from the GUViCS, NGVS and VESTIGE surveys. Units and calibration
are kept as in the standard products from these survey (i.e. GALEX FUV
and NUV, CFHT MegaCam u, g, i, z and VESTIGE r, narrowband Halpha).
All the images have the same pixel scale of 0.187 arcsec/pixel.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tabled1.dat 104 64 *Properties of the selected sample of galaxies
appen.dat 201 1270 Radial surface brightness profiles
list.dat 96 507 List of fits images
fits/* . 507 Individual fits images
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Note on tabled1.dat: All the geometrical parameters given in this table are
taken from the NGVS catalog.
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Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- ID Source ID based on the position in the
NGVS catalog
6- 32 A27 --- NGVS Name of the source in NGVS
(NGVSJHH:MM:SS.ss+DD:MM:SS.s)
34- 41 A8 --- VCC VCC name
43- 49 F7.3 deg RAdeg Right ascension (J2000)
51- 56 F6.3 deg DEdeg Declination (J2000)
58- 61 F4.2 Mpc DM87 Projected distance of the galaxy from M87
63- 67 F5.2 mag gmag g-band magnitude
69- 73 F5.2 10+7Msun M* Stellar mass of the galaxies
(see Sect. 2.1)
75- 78 F4.2 kpc Reg Effective radius of the source
80- 84 F5.2 mag/arcsec+2 mu0g g-band central surface brightness
86- 89 F4.2 --- q Axis ratio
91- 96 F6.2 deg PA [] Position angle
98-102 F5.3 mag E(B-V) Foreground galactic extinction from
Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S)
104 I1 --- Flag [1/2] Flag for the galaxy type (1)
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Note (1): Flag for the galaxy type as follows:
1 = UDGs from Lim et al. (2020ApJ...899...69L 2020ApJ...899...69L)
2 = Diffuse galaxies
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Byte-by-byte Description of file: appen.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- ID ID of the galaxy
6- 14 F9.5 deg RAdeg Right Ascension of center (J2000)
16- 23 F8.5 deg DEdeg Declination of center (J2000)
25- 30 F6.2 arcsec Rarcsec Radius in angular units
32- 36 F5.2 kpc Rkpc Radius in physical units
38 A1 --- l_SuBru Limit flag on SuBru
39- 43 F5.2 mag/arcsec2 SuBru Observed u band surface brightness (1)
45- 48 F4.2 mag/arcsec2 E_SuBru Upper limit uncertainty in SuBru
50- 53 F4.2 mag/arcsec2 e_SuBru Lower limit uncertainty in SuBru
55 A1 --- l_SuBrg Limit flag on SuBrg (3)
56- 60 F5.2 mag/arcsec2 SuBrg Observed g band surface brightness (1)
62- 65 F4.2 mag/arcsec2 E_SuBrg Upper limit uncertainty in SuBrg
67- 70 F4.2 mag/arcsec2 e_SuBrg Lower limit uncertainty in SuBrg
72 A1 --- l_SuBrr Limit flag on SuBrr (3)
73- 77 F5.2 mag/arcsec2 SuBrr Observed r band surface brightness (1)
79- 82 F4.2 mag/arcsec2 E_SuBrr Upper limit uncertainty in SuBrr
84- 87 F4.2 mag/arcsec2 e_SuBrr Lower limit uncertainty in SuBrr
89 A1 --- l_SuBri Limit flag on SuBri (3)
90- 94 F5.2 mag/arcsec2 SuBri Observed i band surface brightness (1)
96- 99 F4.2 mag/arcsec2 E_SuBri Upper limit uncertainty in SuBri
101-104 F4.2 mag/arcsec2 e_SuBri Lower limit uncertainty in SuBri
106 A1 --- l_SuBrz Limit flag on SuBrz (3)
107-111 F5.2 mag/arcsec2 SuBrz Observed z band surface brightness (1)
113-116 F4.2 mag/arcsec2 E_SuBrz Upper limit uncertainty in SuBrz
118-121 F4.2 mag/arcsec2 e_SuBrz Lower limit uncertainty in SuBrz
123 A1 --- l_SigmaHa Limit flag on SigmaHa (3)
124-131 E8.4 mW/m2/arcsec2 SigmaHa Observed Hα narrow-band surface
brightness (erg/cm2/s/arcsec2)
134-141 E8.4 mW/m2/arcsec2 E_SigmaHa Upper limit uncertainty in SigmaHa
(erg/cm2/s/arcsec2)
144-151 E8.4 mW/m2/arcsec2 e_SigmaHa Lower limit uncertainty in SigmaHa
(erg/cm2/s/arcsec2)
153 A1 --- l_SuBrFUV Limit flag on SuBrFUV (3)
154-160 F7.2 mag/arcsec2 SuBrFUV ?=-100 Observed FUV band surface
brightness (1) (4)
162-168 F7.2 mag/arcsec2 E_SuBrFUV ?=-100 Upper limit uncertainty in
SuBrFUV (4)
170-176 F7.2 mag/arcsec2 e_SuBrFUV ?=-100 Lower limit uncertainty in
SuBrFUV (4)
178 A1 --- l_SuBrNUV Limit flag on SuBrnuv
179-185 F7.2 mag/arcsec2 SuBrNUV ?=-100 Observed NUV band surface
brightness (1) (4)
187-193 F7.2 mag/arcsec2 E_SuBrNUV ?=-100 Upper limit uncertainty in
SuBrnuv (4)
195-201 F7.2 mag/arcsec2 e_SuBrNUV ?=-100 Lower limit uncertainty in
SuBrnuv (4)
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Note (1): Corrected for Galactic extinction and inclination.
All the magnitudes are in AB units.
Note (3): Three sigma upper limits in surface brightness are marked with > or <.
Note (4): Unavailable data-points are marked as -100.
FUV and NUV data is not available for galaxy ID 892 and ID 935.
For ID 1164, FUV data is not available.
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- ID ID of the galaxy
6- 14 F9.5 deg RAdeg Right Ascension of center (J2000)
15- 23 F9.5 deg DEdeg Declination of center (J2000)
25- 29 F5.3 arcsec/pix scale Scale of the image
31- 34 I4 --- Nx Number of pixels along X-axis
36- 39 I4 --- Ny Number of pixels along Y-axis
41- 46 I6 Kibyte size Size of FITS file
48- 66 A19 --- FileName Name of FITS file, in subdirectory fits
68- 96 A29 --- Title Title of the FITS file
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Acknowledgements:
Junais Madathodika, junais.madathodika(at)lam.fr
References:
Boselli et al., Paper I 2018A&A...614A..56B 2018A&A...614A..56B
Fossati et al., Paper II 2018A&A...614A..57F 2018A&A...614A..57F
Boselli et al., Paper III 2018A&A...615A.114B 2018A&A...615A.114B
Boselli et al., Paper IV 2018A&A...620A.164B 2018A&A...620A.164B
Boselli et al., Paper V 2019A&A...623A..52B 2019A&A...623A..52B
Boselli et al., Paper VI 2020A&A...634L...1B 2020A&A...634L...1B
Boselli et al., Paper VII 2020A&A...644A.161L 2020A&A...644A.161L
Volmer et al., Paper VIII 2021A&A...645A.121V 2021A&A...645A.121V
Boselli et al., Paper IX 2021A&A...646A.139B 2021A&A...646A.139B, Cat. J/A+A/646/A139
Junais et al., Paper X 2021A&A...650A..99J 2021A&A...650A..99J, Cat. J/A+A/650/A99
Sardaneta et al., Paper XI 2022A&A...659A..45S 2022A&A...659A..45S, Cat. J/A+A/659/A45
Boselli et al., Paper XII 2022A&A...659A..46B 2022A&A...659A..46B. Cat. J/A+A/659/A46
(End) Patricia Vannier [CDS] 09-Aug-2022