J/A+A/676/A41 Surface brightness of NEP galaxies (Junais+, 2023)
Variation of optical and infrared properties of galaxies in relation to
their surface brightness.
Junais S., Malek K., Boissier S., Pearson W.J., Pollo A., Boselli A.,
Boquien M., Donevski D., Goto T., Hamed M., Kim S.J., Koda J.,
Matsuhara H., Riccio G., Romano M.
<Astron. Astrophys. 676, A41 (2023)>
=2023A&A...676A..41J 2023A&A...676A..41J (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, optical ; Infrared ; Redshifts
Keywords: galaxies: general - galaxies: formation - galaxies: star formation -
galaxies: ISM
Abstract:
Although it is recognized now that low surface brightness galaxies
(LSBs) contribute to a large fraction of the number density of
galaxies, many of their properties are still poorly known. LSBs are
often considered as 'dust poor', with a very low amount of dust, based
on a few studies. We use, for the first time, a large sample of LSBs
and high surface brightness galaxies (HSBs) with deep observational
data to study the variation of stellar and dust properties as a
function of the surface brightness/surface mass density. Our sample
consists of 1631 galaxies that are optically selected (with ugrizy-
bands) at z<0.1 from the North Ecliptic Pole (NEP) wide field. We use
the large multi-wavelength set of ancillary data in this field,
ranging from UV to FIR. We measured the optical size and the surface
brightness of the targets, and analyzed their spectral energy
distribution using the CIGALE fitting code. Based on the measured
average r-band surface brightness (µe), our sample consists of
1003 LSBs (µe>23mag/arcsec2) and 628 HSBs
(µe≤23mag/arcsec2). We found that the specific star formation
rate and specific infrared luminosity (total infrared luminosity per
stellar mass) remain mostly flat as a function of surface brightness
for both LSBs and HSBs that are star- forming but decline steeply for
the quiescent galaxies. The majority of LSBs in our sample have
negligible dust attenuation (Av<0.1mag), except for about 4% of them
that show significant attenuation with a mean Av of 0.8mag. We found
that these LSBs with a significant attenuation also have a high r-band
mass-to-light ratio (M/Lr>3M☉/L☉), making them outliers
from the linear relation of surface brightness and stellar mass
surface density. These outlier LSBs also show similarity to the
extreme giant LSBs from the literature, indicating a possibly higher
dust attenuation in giant LSBs as well. This work provides a large
catalog of LSBs and HSBs with detailed measurements of their several
optical and infrared physical properties. Our results suggest that the
dust content of LSBs is more varied than previously thought, with some
of them having significant attenuation making them fainter than their
intrinsic value. With these results, we will be able to make
predictions on the dust content of the population of LSBs and how the
presence of dust will affect their observations from current/upcoming
surveys like JWST and LSST.
Description:
Estimated properties of the sample as given in the Table B.1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 99 1631 Properties of the sample
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See also:
J/ApJS/207/37 : IR sources spectroscopy in the AKARI NEP (Shim+, 2013)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 17 I17 --- ID HSC ID of the source
19- 26 F8.4 deg RAdeg Right Ascension of the galaxy (J2000)
28- 34 F7.4 deg DEdeg Declination of the galaxy (J2000)
36- 39 F4.2 --- z Redshift
41- 46 A6 --- f_z Redshift type (photoz or specz)
48- 51 F4.1 mag/arcsec2 mu Average r-band surface brightness
within the effective radius
53- 55 F3.1 kpc re Effective radius
57- 61 F5.2 Msun Mstar Stellar mass
63- 66 F4.2 Msun e_Mstar Stellar mass uncertainty
68- 72 F5.2 Msun/yr SFR Star formation rate
74- 78 F5.2 Msun/yr e_SFR Star formation rate uncertainty
80- 84 F5.2 Lsun LIR Total infrared luminosity
86- 89 F4.2 Lsun e_LIR Total infrared luminosity uncertainty
91- 94 F4.2 mag AV Dust attenuation in the V-band
96- 99 F4.2 mag e_AV Dust attenuation in the V-band uncertainty
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Acknowledgements:
Junais, junais(at)ncbj.gov.pl
(End) Patricia Vannier [CDS] 19-Jun-2023