Spatially Resolved Properties of Galaxies from CANDELS+MUSE: Radial Extinction Profile and Insights on Quenching

Abstract

Studying the internal processes of individual galaxies at kilo-parsec scales is crucial in enhancing our understanding of galaxy formation and evolution processes. In this work, we investigate the distribution of star formation rate (SFR), specific SFR (sSFR), and dust attenuation across individual galaxies for a sample of 32 galaxies selected from the MUSE-Wide Survey at 0.1 < z < 0.42 with a dynamic range in stellar masses between 10 7.7 and 10 10.3 M . We take advantage of the high spatial resolution of the MUSE integral-field spectrograph and measure reliable spatially resolved Hα and Hβ emission line maps for individual galaxies. We also derive resolved stellar mass, SFR and dust maps using pixel-by-pixel SED fitting on high resolution multi-band HST /ACS and HST /WFC3 data from the CANDELS survey. By combining these, we analyze the radial profile of various physical parameters across these galaxies. We observe a radial dependence in both stellar and nebular color excess profiles peaking at the inner regions of galaxies. We also find the color excess profiles to most strongly correlate with the integrated sSFRs of galaxies. The median sSFR Hα radial profiles of galaxies in our sample show a 0.8 dex increase from the central regions outward. This increase compared to the almost flat median radial profile of sSFR SED , which traces longer timescales of star formation, is in favor of the inside-out quenching of star formation. We bring further evidence for this quenching scenario from the locus of different subregions of galaxies on the SFR-M * and sSFR-M * relations.

SDSS-IV MaNGA: spatially resolved dust attenuation in spiral galaxies

“…Of these quantities, the median local A V, gas depends most strongly on stellar mass: its average value increases for increasing stellar mass. This finding is in agreement with those of other authors, who report higher average values for the local A V, gas for higher-mass galaxies (Nelson et al 2015a;Jafariyazani et al 2019). By contrast, the median local A V, stars does not change appreciably between each stellar mass category (although see González Delgado et al 2015 andGoddard et al 2016, both of whom do find higher average values for A V, stars in galaxies with higher stellar masses.…”

“…This behaviour suggests that the radial gradients seen in the local A V, gas , both in this work and in other work (e.g. Nelson et al 2015a;Jafariyazani et al 2019) cannot be attributed to a radial gradient in the diffuse ISM alone.…”

“…These findings are in agreement with previous work: both González Delgado et al (2015) as well as Goddard et al (2016) find that dust attenuation affecting the stellar populations exhibits a similar radial gradient for both CALIFA survey galaxies and MaNGA galaxies, respectively. Furthermore, both Nelson et al (2015a) and Jafariyazani et al (2019) show that dust attenuation derived from measurements of the Balmer decrement declines radially in a very similar manner for both 3D-HST survey galaxies and MUSE-Wide survey galaxies, respectively. Moreover, these authors also report steeper radial gradients for higher-mass galaxies for both the local A V, stars (González Delgado et al 2015;Goddard et al 2016) and for the local A V, gas (Nelson et al 2015a;Jafariyazani et al 2019).…”

“…Furthermore, both Nelson et al (2015a) and Jafariyazani et al (2019) show that dust attenuation derived from measurements of the Balmer decrement declines radially in a very similar manner for both 3D-HST survey galaxies and MUSE-Wide survey galaxies, respectively. Moreover, these authors also report steeper radial gradients for higher-mass galaxies for both the local A V, stars (González Delgado et al 2015;Goddard et al 2016) and for the local A V, gas (Nelson et al 2015a;Jafariyazani et al 2019). Again, this behaviour can be seen in the plots of Fig.…”

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

“…morphology, existence of a bar). Jafariyazani et al (2019) found a spatially resolved MS in galaxies at 0.1 < z < 0.42 observed with MUSE. Medling et al (2018) estimated the MS from ∼ 800 galaxies in the Sydney AAO Multi-object Integral Field Galaxy Survey (SAMI, Croom et al 2012) at z < 0.1, finding a slope of 1.0.…”