Bibcode
Calvi, R.; Vulcani, B.; Poggianti, B. M.; Moretti, A.; Fritz, J.; Fasano, G.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society, Volume 481, Issue 3, p.3456-3469
Advertised on:
12
2018
Citations
22
Refereed citations
22
Description
Exploiting a sample of 680 star-forming galaxies from the Padova
Millennium Galaxy Group Catalog (PM2GC; Calvi, Poggianti & Vulcani
2011) in the range 0.038 ≤ z ≤ 0.104, we present a detailed
analysis of the star formation rate (SFR)-stellar mass (M*)
and specific SFR (SSFR)-M* relations as a function of
environment. We adopt three different parametrizations of environment to
probe different scales. We consider separately (1) galaxies in groups,
binary and single systems, defined in terms of a friends-of-friends
algorithm, (2) galaxies located at different projected local densities,
and (3) galaxies in haloes of different mass. Overall, above
logM*/M > 10.25 and SSFR > 10-12
yr-1, the SFR-M*, and SSFR-M* relations
do not depend on environment, when the global environment is used, while
when the halo mass is considered, high-mass haloes might have a
systematically lower (S)SFR-M⋆ relation. Finally, when
local densities are exploited, at any given mass galaxies in less dense
environments have systematically higher values of SFR. All the relations
are characterized by a large scatter (σ ˜ 0.6), which is due
to the coexistence of galaxies of different morphological types. Indeed,
at any given mass, late types are characterized by systematically higher
values of SFR and SSFR than S0s and ellipticals. Galaxies of the same
morphology show similar trends in all the environments, but their
incidence strongly depends on environment and on the environmental
parametrization adopted, with late types generally becoming less common
in denser environments, contrasted by the increase of ellipticals and/or
S0s. Our results suggest that in the local Universe morphology and local
interactions, probed by the local density parametrization, have dominant
roles in driving the characteristics of the SFR-M* relation.