Understanding the scatter in the spatially resolved star formation main sequence of local massive spiral galaxies

Abstract

We investigate the relation between star formation rate (SFR) and stellar mass (M * ) in sub-galactic (∼ 1kpc) scale of 93 local (0.01 < z < 0.02) massive (M * > 10 10.5 M ) spiral galaxies. To derive spatially-resolved SFR and stellar mass, we perform so-called pixelto-pixel SED fitting, which fits an observed spatially-resolved multiband SED with a library of model SEDs using Bayesian statistics approach. We use 2 bands (FUV and NUV ) and 5 bands (u, g, r, i, and z) imaging data from Galaxy Evolution Explorer (GALEX) and Sloan Digital Sky Survey (SDSS), respectively. We find a tight nearly linear relation between the local surface density of SFR (Σ SFR ) and stellar mass (Σ * ) which has flattening in high Σ * . The near linear relation between Σ * and Σ SFR suggests constant sSFR throughout the galaxies, and the scatter of the relation is directly related to that of sSFR. Therefore, we analyse the variation of sSFR in various scales. More massive galaxies on average have lower sSFR throughout them than less massive galaxies. We also find that barred galaxies have lower sSFR in a core region than non-barred galaxies. However, in the outside region, sSFR of barred and non-barred galaxies are similar and lead to the similar total sSFR.

SDSS-IV MaNGA-resolved Star Formation and Molecular Gas Properties of Green Valley Galaxies: A First Look with ALMA and MaNGA

“…Recently, it has been found that kiloparsec-scale S SFR traces well with the underlying * S for star-forming galaxies (Sánchez et al 2013;Cano-Díaz et al 2016;Abdurróuf & Akiyama 2017;Hsieh et al 2017). This relation may be responsible for the observed tight correlation between the global SFR and * M .…”

Outflows in star-forming galaxies: Stacking analyses of resolved winds and the relation to their hosts’ properties

“…Since the discovery of the galaxy Main Sequence (MS) and the development of basic frameworks to describe a galaxy's position relative to it, much work has gone into determining the prevalence and influence of outflows relative to the MS (e.g., Chen et al 2010;Rubin et al 2014;Cicone et al 2016;Roberts-Borsani & Saintonge 2018;Concas et al 2019). The arrival of large IFU surveys such as MaNGA, SAMI and CALIFA, has also revealed a resolved MS (Sánchez et al 2013;Cano-Díaz et al 2016;González Delgado et al 2016;Abdurro'uf, & Akiyama 2017;Hsieh et al 2017;Maragkoudakis et al 2017), indicative of a link between small scale processes and the integrated properties of galaxies. As such, it is interesting to look at the prevalence and properties of outflows over such a resolved sequence.…”

A panchromatic spatially resolved analysis of nearby galaxies – I. Sub-kpc-scale main sequence in grand-design spirals

“…4.2) that usually span the range 0.7 − 1.1 despite using different SFR tracers and different redshift and stellar mass ranges for the analysis (i.e. Pérez et al 2013;Wuyts et al 2013;Hemmati et al 2014;Cano-Díaz et al 2016;González Delgado et al 2016;Abdurro'uf & Akiyama 2017;Abdurro'uf 2018;Hall et al 2018;Cano-Díaz et al 2019). It is worth noting that several of the literature works implement the orthogonal distance regression (ODR) method to find the location of the MS relation.…”

“…These results suggest that the global relation is set locally, possibly by the surface density of molecular gas (Lin et al 2017). Exploiting pixel-by-pixel Spectral Energy Distribution (SED) fitting, Abdurro'uf & Akiyama (2017) analysed the spatially resolved MS in a sample of 93 local massive galaxies on ∼ kpc scales. They find that the slope of the relation varies dramatically (from 0.3 to 0.99) depending on the range of Σ used for fitting, somehow recalling the bending of the MS observed in the integrated MS relation (e.g.…”