12,336 research outputs found
Dust emission in star-forming dwarf galaxies: General properties and the nature of the sub-mm excess
We studied the global characteristics of dust emission in a large sample of
emission-line star-forming galaxies. The sample consists of two subsamples. One
subsample (SDSS sample) includes ~4000 compact star-forming galaxies from the
SDSS, which were also detected in all four bands at 3.4, 4.6, 12, and 22 mum of
the WISE all-sky survey. The second subsample (Herschel sample) is a sample of
28 compact star-forming galaxies observed with Herschel in the FIR range. Data
of the Herschel sample were supplemented by the photometric data from the
Spitzer observations, GALEX, SDSS, WISE, 2MASS, NVSS, and FIRST surveys, as
well as optical and Spitzer spectra and data in sub-mm and radio ranges. It is
found that warm dust luminosities of galaxies from the SDSS sample and cold and
warm dust luminosities of galaxies from the Herschel sample are strongly
correlated with Hbeta luminosities, which implies that one of the main sources
of dust heating in star-forming galaxies is ionising UV radiation of young
stars. Using the relation between warm and cold dust masses for estimating the
total dust mass in star-forming galaxies with an accuracy better than ~0.5 dex
is proposed. On the other hand, it is shown for both samples that dust
temperatures do not depend on the metallicities. The dust-to-neutral gas mass
ratio strongly declines with decreasing metallicity, similar to that found in
other studies of local emission-line galaxies, high-redshift GRB hosts, and
DLAs. On the other hand, the dust-to-ionised gas mass ratio is about one
hundred times as high implying that most of dust is located in the neutral gas.
It is found that thermal free-free emission of ionised gas in compact
star-forming galaxies might be responsible for the sub-mm emission excess. This
effect is stronger in galaxies with lower metallicities and is also positively
affected by an increased star-formation rate.Comment: 22 pages, 15 figures, accepted for publication in Astronomy and
Astrophysic
From voids to filaments: environmental transformations of galaxies in the SDSS
We investigate the impact of filament and void environments on galaxies,
looking for residual effects beyond the known relations with environment
density. We quantified the host environment of galaxies as the distance to the
spine of the nearest filament, and compared various galaxy properties within 12
bins of this distance. We considered galaxies up to 10 Mpc from
filaments, i.e. deep inside voids. The filaments were defined by a point
process (the Bisous model) from the Sloan Digital Sky Survey data release 10.
In order to remove the dependence of galaxy properties on the environment
density and redshift, we applied weighting to normalise the corresponding
distributions of galaxy populations in each bin. After the normalisation with
respect to environment density and redshift, several residual dependencies of
galaxy properties still remain. Most notable is the trend of morphology
transformations, resulting in a higher elliptical-to-spiral ratio while moving
from voids towards filament spines, bringing along a corresponding increase in
the colour index and a decrease in star formation rate. After separating
elliptical and spiral subsamples, some of the colour index and star formation
rate evolution still remains. The mentioned trends are characteristic only for
galaxies brighter than about mag. Unlike some other recent
studies, we do not witness an increase in the galaxy stellar mass while
approaching filaments. The detected transformations can be explained by an
increase in the galaxy-galaxy merger rate and/or the cut-off of extragalactic
gas supplies (starvation) near and inside filaments. Unlike voids, large-scale
galaxy filaments are not a mere density enhancement, but have their own
specific impact on the constituent galaxies, reducing the star formation rate
and raising the chances of elliptical morphology also at a fixed environment
density level.Comment: 4 pages, 3 figures, Astronomy & Astrophysics letters accepte
Combined CO & Dust Scaling Relations of Depletion Time and Molecular Gas Fractions with Cosmic Time, Specific Star Formation Rate and Stellar Mass
We combine molecular gas masses inferred from CO emission in 500 star forming
galaxies (SFGs) between z=0 and 3, from the IRAM-COLDGASS, PHIBSS1/2 and other
surveys, with gas masses derived from Herschel far-IR dust measurements in 512
galaxy stacks over the same stellar mass/redshift range. We constrain the
scaling relations of molecular gas depletion time scale (tdepl) and gas to
stellar mass ratio (Mmolgas/M*) of SFGs near the star formation main-sequence
with redshift, specific star formation rate (sSFR) and stellar mass (M*). The
CO- and dust-based scaling relations agree remarkably well. This suggests that
the CO-H2 mass conversion factor varies little within 0.6dex of the main
sequence (sSFR(ms,z,M*)), and less than 0.3dex throughout this redshift range.
This study builds on and strengthens the results of earlier work. We find that
tdepl scales as (1+z)^-0.3 *(sSFR/sSFR(ms,z,M*))^-0.5, with little dependence
on M*. The resulting steep redshift dependence of Mmolgas/M* ~(1+z)^3 mirrors
that of the sSFR and probably reflects the gas supply rate. The decreasing gas
fractions at high M* are driven by the flattening of the SFR-M* relation.
Throughout the redshift range probed a larger sSFR at constant M* is due to a
combination of an increasing gas fraction and a decreasing depletion time
scale. As a result galaxy integrated samples of the Mmolgas-SFR rate relation
exhibit a super-linear slope, which increases with the range of sSFR. With
these new relations it is now possible to determine Mmolgas with an accuracy of
0.1dex in relative terms, and 0.2dex including systematic uncertainties.Comment: ApJ accepte
- âŠ