Abstract
Abstract We estimate the stellar mass for a sample of low surface brightness galaxies (LSBGs) by fitting their multiband spectral energy distributions (SEDs) to the stellar population synthesis model. The derived stellar masses (log M */M ⊙) span from 7.1 to 11.1, with a mean of log M */M ⊙ = 8.5, which is lower than that for normal galaxies. The stellar mass-to-light ratio (γ*) in each band varies little with the absolute magnitude but increases with higher M *. This trend of γ* with M * is even stronger in bluer bands. In addition, the γ* for our LSBGs slightly declines from the r band to the longer-wavelength bands. The log (j = g, r, i, and z) have relatively tight relations with optical colors of g − r and g − i. Compared with several representative γ*–color relations (MLCRs) from the literature, our MLCRs based on LSBG data are consistently among those literature MLCRs previously defined on diverse galaxy samples, and the existing minor differences between the MLCRs are caused by the differences in the SED model ingredients (including initial mass function, star formation history, and stellar population model), line fitting techniques, galaxy samples, and photometric zero-point, rather than the galaxy surface brightness itself, which distinguishes LSBGs from high surface brightness galaxies. Our LSBGs would be very likely to follow those representative MLCRs previously defined in diverse galaxy populations, if those main ingredients were taken into account.
Highlights
Galaxies with central surface brightnesses fainter than the night sky (∼ 22.5 B mag arcsec−2 ) are defined as Low Surface Brightness Galaxies (LSBGs; (e.g. Impey & Bothun 1997; Impey et al 2001; Ceccarelli et al 2012)
Compared with several representative γ∗-color relations (MLCRs) from literature, our mass-to-light - color relation (MLCR) based on low surface brightness galaxies (LSBGs) data are consistently among those literature MLCRs previously defined on diverse galaxy samples, and the existing minor differences between the MLCRs are more caused by the differences in the spectral energy distributions (SEDs) model ingredients including initial mass function, star formation history, and stellar population model, and the line fitting techniques, galaxy samples, and photometric zero-point as well, rather than the galaxy surface brightness itself which distinguishes LSBGs from HSBGs
IP13 MLCR is based on a combination of simple stellar populations (SSPs) from the isochrone data set of the Padova group which includes a revised prescription for the thermally pulsing asymptotic giant branch (TP-AGB), composite stellar populations (CSP) which are generated by convolving SSPs according to exponentially declining star formation histories (SFHs), and disc galaxy models from Portinari et al (2004)
Summary
Galaxies with central surface brightnesses fainter than the night sky (∼ 22.5 B mag arcsec−2 ) are defined as Low Surface Brightness Galaxies (LSBGs; (e.g. Impey & Bothun 1997; Impey et al 2001; Ceccarelli et al 2012). LSBGs are abundant in Hi gas but deficient in metal (≤ 1/3 solar abundance) and dust (e.g. McGaugh & Bothun 1994; Matthews et al 2001), and they have fairly low star formation rates (SFR) (e.g., Das et al 2009; Galaz et al 2011; Lei et al 2018), which are evident that only a small number of Hii regions inhabit in their diffuse disks They have lower stellar mass densities, comparing to their High Surface Brightness Galaxy (HSBG) counterparts (normal galaxies) (e.g. de Blok et al 1996; Burkholder et al 2001; O’Neil et al 2004; Trachternach et al 2006). Magnitudes in this paper are all in the AB magnitude system
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