J/ApJS/247/46 Opt. photometry of SMUDGes ultra-diffuse galaxies (Barbosa+, 2020)
One hundred SMUDGes in S-PLUS: ultra-diffuse galaxies flourish in the field.
Barbosa C.E., Zaritsky D., Donnerstein R., Zhang H., Dey A.,
Mendes de Oliveira C., Sampedro L., Molino A., Costa-Duarte M.V., Coelho P.,
Cortesi A., Herpich F.R., Hernandez-Jimenez J.A., Santos-Silva T.,
Pereira E., Werle A., Overzier R.A., Cid Fernandes R., Smith Castelli A.V.,
Ribeiro T., Schoenell W., Kanaan A.
<Astrophys. J. Suppl. Ser., 247, 46 (2020)>
=2020ApJS..247...46B 2020ApJS..247...46B
ADC_Keywords: Galaxies, photometry; Redshifts; Extinction; Abundances, [Fe/H];
Optical; Stars, masses; Stars, ages
Keywords: Low surface brightness galaxies ; Stellar populations ; Stellar ages ;
Metallicity ; Stellar masses
Abstract:
We present the first systematic study of the stellar populations of
ultra-diffuse galaxies (UDGs) in the field, integrating the large area
search and characterization of UDGs by the SMUDGes survey with the
twelve-band optical photometry of the S-PLUS survey. Based on Bayesian
modeling of the optical colors of UDGs, we determine the ages,
metallicities, and stellar masses of 100 UDGs distributed in an area
of ∼330deg2 in the Stripe 82 region. We find that the stellar masses
and metallicities of field UDGs are similar to those observed in
clusters and follow the trends previously defined in studies of dwarf
and giant galaxies. However, field UDGs have younger luminosity-
weighted ages than do UDGs in clusters. We interpret this result to
mean that field UDGs have more extended star formation histories,
including some that continue to form stars at low levels to the
present time. Finally, we examine stellar population scaling relations
that show that UDGs are, as a population, similar to other low surface
brightness galaxies.
Description:
Zaritsky+ (2019, J/ApJS/240/1) presented the initial results from the
Systematically Measuring Ultra-diffuse Galaxies (SMUDGes) survey, a
systematic study to detect and characterize the photometric properties
of ultra-diffuse galaxies (UDGs) over a large area of the sky
(∼14000°2) using data from the Legacy survey
(Dey+ 2019AJ....157..168D 2019AJ....157..168D), a deep three-band observational campaign
that supports the Dark Energy Spectroscopic Instrument (DESI) project.
We use data from the Southern Photometric Local Universe Survey
(S-PLUS, Mendes de Oliveira+ 2019MNRAS.489..241M 2019MNRAS.489..241M) first data release
(DR1), which covers an area of 336deg2 in the Stripe 82 equatorial
field, observed with the T80S, a 0.8m robotic telescope with a wide
FoV of ∼1.8°2, located in Cerro Tololo, Chile.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
udgs.dat 106 100 Stellar population parameters for SMUDGes
ultra-diffuse galaxies (UDGs) obtained from
SED fitting of the S-PLUS optical data
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See also:
J/ApJS/137/117 : Las Campanas Distant Cluster Survey (Gonzales+, 2001)
J/ApJ/621/673 : Line indices for 124 early-type galaxies (Thomas+, 2005)
J/MNRAS/404/1639 : MILES base models & new line index system (Vazdekis+, 2010)
J/MNRAS/413/971 : Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)
J/AJ/144/4 : Dwarf galaxies in the Local Group (McConnachie+, 2012)
J/ApJ/779/102 : Metallicities of RGB stars in dwarf galaxies (Kirby+, 2013)
J/ApJ/794/120 : Sloan Digital Sky Survey coadd. Stripe 82 (Annis+, 2014)
J/ApJS/225/11 : Subaru-UDGs in the Coma cluster (Yagi+, 2016)
J/MNRAS/456/1359 : IAC Stripe 82 Legacy Project: Photometry (Fliri J.+, 2016)
J/ApJ/842/133 : HI-bearing ultra-diffuse ALFALFA galaxies (Leisman+, 2017)
J/A+A/608/A142 : Fornax Deep Survey with VST. III. LSB gal. (Venhola+, 2017)
J/ApJS/240/1 : SMUDGes. I. First results in Coma Cluster (Zaritsky+, 2019)
Byte-by-byte Description of file: udgs.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SMDG]
5- 18 A14 --- SMDG Galaxy name (HHMMSSs+DDMMSS) (Galaxy)
20- 24 F5.3 mag Av [0.04/0.2] Total extinction in the V-band
26- 30 F5.3 mag e_Av [0.03/0.2] Lower uncertainty on Av (Av_lowerr)
32- 36 F5.3 mag E_Av [0.07/0.3] Upper uncertainty on Av (Av_uperr)
38- 43 F6.3 [-] [Fe/H] [-1.5/-0.1] Metallicity (Z)
45- 49 F5.3 [-] e_[Fe/H] [0.2/1] Lower uncertainty on [Fe/H] (Z_lowerr)
51- 55 F5.3 [-] E_[Fe/H] [0.3/1.1] Upper uncertainty on [Fe/H] (Z_uperr)
57- 60 F4.2 Gyr Age [0.5/8.6] Age (T)
62- 65 F4.2 Gyr e_Age [0.09/5] Lower uncertainty on Age (T_lowerr)
67- 70 F4.2 Gyr E_Age [0.1/8] Upper uncertainty on Age (T_uperr)
72- 77 F6.4 --- zphot [0.008/0.03] Photometric redshift (photz)
79- 84 F6.4 --- e_zphot [0.006/0.02] Lower uncertainty on zphot
(photz_lowerr)
86- 91 F6.4 --- E_zphot [0.01/0.03] Upper uncertainty on zphot
(photz_uperr)
93- 96 F4.2 [Msun] logM* [6.8/8.6] Log of stellar mass (logMstar)
98-101 F4.2 [Msun] e_logM* [0.8/1.3] Lower uncertainty on logM*
(logMstar_lowerr)
103-106 F4.2 [Msun] E_logM* [0.4/0.9] Upper uncertainty on logM*
(logMstar_uperr)
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History:
From electronic version of the journal (original FITS file available
in the FTP section)
(End) Emmanuelle Perret [CDS] 10-Jun-2020