816 research outputs found
Extragalactic Source Counts in the Spitzer 24-micron Band: What Do We Expect From ISOCAM 15-micron Data and Models?
The comparison between the new Spitzer data at 24 micron and the previous
ISOCAM data at 15 micron is a key tool to understand galaxy properties and
evolution in the infrared and to interpret the observed number counts, since
the combination of Spitzer with the ISO cosmological surveys provides for the
first time the direct view of the Universe in the Infrared up to z~2. We
present the prediction in the Spitzer 24-micron band of a phenomenological
model for galaxy evolution derived from the 15-micron data. Without any ``a
posteriori'' update, the model predictions seem to agree well with the recently
published 24-micron extragalactic source counts, suggesting that the peak in
the 24-micron counts is dominated by ``starburst'' galaxies like those detected
by ISOCAM at 15 micron, but at higher redshifts (1 < z < 2 instead of 0.5 < z <
1.5).Comment: 8 pages: 4 pages of main text + 5 postscript figures, use aastex.
Accepted for publication in ApJL. Replaced with the proof version (added
missing references and corrected a few sentences
Endocytic pathways and membrane recycling involve the actin filaments in tobacco pollen tubes
The pollen tube is a tip growing cell that plays a fundamental role in the fertilization process of higher plants. Pollen tube growth is based on transport and accumulation of secretory vesicles. The incorporation of new segments of PM largely exceeds the quantity of membrane required for the extension, so the excess of PM must be removed by endocytosis. Recent studies showed internalization of subapical PM domains that were mainly recycled to exocytosis through the Golgi apparatus and a second mainly degradative pathway involving PM retrieval at the tip. The movements of the endomembrane system during the pollen tube growth depends on the concerted action and integrity of the cytoskeleton. In this study we disturb the system of cortical actin filaments using Latrunculin B to verify modifications in endocytosis, using specific FM dyes in time-lapse experiments and by ultrastructural experiments using charged Nanogold. Our results demonstrate that the system of cortical microfilaments determines a strong reduction of endocytosis in the subapical regions and consequently the alteration of recycling through the Golgi and the inhibition of the degradative pathways
Star formation properties of sub-mJy radio sources
We investigate the star formation properties of ~800 sources detected in one
of the deepest radio surveys at 1.4 GHz. Our sample spans a wide redshift range
(~0.1 - 4) and about four orders of magnitude in star formation rate (SFR). It
includes both star forming galaxies (SFGs) and active galactic nuclei (AGNs),
further divided into radio-quiet and radio-loud objects. We compare the SFR
derived from the far infrared luminosity, as traced by Herschel, with the SFR
computed from their radio emission. We find that the radio power is a good SFR
tracer not only for pure SFGs but also in the host galaxies of RQ AGNs, with no
significant deviation with redshift or specific SFR. Moreover, we quantify the
contribution of the starburst activity in the SFGs population and the
occurrence of AGNs in sources with different level of star formation. Finally
we discuss the possibility of using deep radio survey as a tool to study the
cosmic star formation history.Comment: 18 pages, 14 figures, 1 table (available in its entirety as ancillary
data
Microtubule depolymerization affects endocytosis and exocytosis in the tip and influences endosome movement in tobacco pollen tubes
Polarized organization of the cytoplasm of growing pollen tubes is maintained by coordinated function of actin filaments (AFs) and microtubules (MTs). AFs convey post-Golgi secretory vesicles to the tip where some fuse with specific domains of the plasma membrane (PM). Secretory activity is balanced by PM retrieval that maintains cell membrane economy and regulates the polarized composition of the PM, by dividing lipids/proteins between the shank and the tip. Although AFs play a key role in PM internalization in the shank, the role of MTs in exoendocytosis needs to be characterized. The present results show that integrity of the MT cytoskeleton is necessary to control exoendocytosis events in the tip. MT polymerization plays a role in promoting PM invagination in the apex of tobacco pollen tubes since Nocodazole affected PM internalization in the tip and subsequent migration of endocytic vesicles from the apex for degradation. MT depolymerization in the apex and shank was associated with misallocation of a significantly greater amount of internalized PM to the Golgi apparatus and its early recycling to the secretory pathway. FRAP experiments also showed that MT depolymerization in the tip region influenced the rate of exocytosis in the central domain of the apical PM
The dust and cold gas content of local star forming galaxies
We use dust masses () derived from far-infrared data and molecular
gas masses () based on CO luminosity, to calibrate proxies based on a
combination of the galaxy Balmer decrement, disk inclination and gas
metallicity. We use such proxies to estimate and in the
local SDSS sample of star-forming galaxies (SFGs). We study the distribution of
and along and across the Main Sequence (MS) of SFGs. We
find that and increase rapidly along the MS with
increasing stellar mass (), and more marginally across the MS with
increasing SFR (or distance from the relation). The dependence on is
sub-linear for both and . Thus, the fraction of dust
() and molecular gas mass () decreases monotonically towards
large . The star formation efficiency (SFE, the inverse of the molecular
gas depletion time) depends strongly on the distance from the MS and it is
constant along the MS. As nearly all galaxies in the sample are central
galaxies, we estimate the dependence of and on the host
halo mass and find a tight anti-correlation. As the region where the MS is
bending is numerically dominated by massive halos, we conclude that the bending
of the MS is due to lower availability of molecular gas mass in massive halos
rather than a lower efficiency in forming stars.Comment: Accepted for publication in MNRAS, 12 pages, 9 figure
Clustering of galaxies at 3.6 microns in the Spitzer Wide-area Infrared Extragalactic legacy survey
We investigate the clustering of galaxies selected in the 3.6 micron band of
the Spitzer Wide-area Infrared Extragalactic (SWIRE) legacy survey. The angular
two-point correlation function is calculated for eleven samples with flux
limits of S_3.6 > 4-400 mujy, over an 8 square degree field. The angular
clustering strength is measured at >5-sigma significance at all flux limits,
with amplitudes of A=(0.49-29)\times10^{-3} at one degree, for a power-law
model, A\theta^{-0.8}. We estimate the redshift distributions of the samples
using phenomological models, simulations and photometric redshifts, and so
derive the spatial correlation lengths. We compare our results with the GalICS
(Galaxies In Cosmological Simulations) models of galaxy evolution and with
parameterized models of clustering evolution. The GalICS simulations are
consistent with our angular correlation functions, but fail to match the
spatial clustering inferred from the phenomological models or the photometric
redshifts. We find that the uncertainties in the redshift distributions of our
samples dominate the statistical errors in our estimates of the spatial
clustering. At low redshifts (median z<0.5) the comoving correlation length is
approximately constant, r_0=6.1\pm0.5h^{-1} Mpc, and then decreases with
increasing redshift to a value of 2.9\pm0.3h^{-1} Mpc for the faintest sample,
for which the median redshift is z=1. We suggest that this trend can be
attributed to a decrease in the average galaxy and halo mass in the fainter
flux-limited samples, corresponding to changes in the relative numbers of
early- and late-type galaxies. However, we cannot rule out strong evolution of
the correlation length over 0.5<z<1.Comment: 14 pages, 9 (colour) figures. Published in MNRA
The Bright and Dark Sides of High-Redshift starburst galaxies from {\it Herschel} and {\it Subaru} observations
We present rest-frame optical spectra from the FMOS-COSMOS survey of twelve
\textit{Herschel} starburst galaxies, with Star Formation Rate
(SFR) elevated by 8, on average, above the star-forming Main Sequence
(MS). Comparing the H to IR luminosity ratio and the Balmer Decrement
we find that the optically-thin regions of the sources contain on average only
percent of the total SFR whereas percent comes from an
extremely obscured component which is revealed only by far-IR observations and
is optically-thick even in H. We measure the [NII]/H
ratio, suggesting that the less obscured regions have a metal content similar
to that of the MS population at the same stellar masses and redshifts. However,
our objects appear to be metal-rich outliers from the metallicity-SFR
anticorrelation observed at fixed stellar mass for the MS population. The
[SII]/[SII] ratio from the average spectrum indicates an
electron density , larger than what
estimated for MS galaxies but only at the 1.5 level. Our results
provide supporting evidence that high- MS outliers are the analogous of
local ULIRGs, and are consistent with a major merger origin for the starburst
event.Comment: 6 pages, 4 figures, Accepted for publication in ApJ Letter
Dust temperature and CO-to-H2 conversion factor variations in the SFR-M* plane
Deep Herschel imaging and 12CO(2-1) line luminosities from the IRAM PdBI are
combined for a sample of 17 galaxies at z>1 from the GOODS-N field. The sample
includes galaxies both on and above the main sequence (MS) traced by
star-forming galaxies in the SFR-M* plane. The far-infrared data are used to
derive dust masses, Mdust. Combined with an empirical prescription for the
dependence of the gas-to-dust ratio on metallicity (GDR), the CO luminosities
and Mdust values are used to derive for each galaxy the CO-to-H2 conversion
factor, alpha_co. Like in the local Universe, the value of alpha_co is a factor
of ~5 smaller in starbursts compared to normal star-forming galaxies (SFGs). We
also uncover a relation between alpha_co and dust temperature (Tdust; alpha_co
decreasing with increasing Tdust) as obtained from modified blackbody fits to
the far-infrared data. While the absolute normalization of the alpha_co(Tdust)
relation is uncertain, the global trend is robust against possible systematic
biases in the determination of Mdust, GDR or metallicity. Although we cannot
formally distinguish between a step and a smooth evolution of alpha_co with the
dust temperature, we can conclude that in galaxies of near-solar metallicity, a
critical value of Tdust=30K can be used to determine whether the appropriate
alpha_co is closer to the starburst value (1.0 Msun(K kms pc^2)^-1, if
Tdust>30K) or closer to the Galactic value (4.35 Msun (K kms pc^2)^-1, if
Tdust<30K). This indicator has the great advantage of being less subjective
than visual morphological classifications of mergers/SFGs, which can be
difficult at high z because of the clumpy nature of SFGs. In the absence of
far-infrared data, the offset of a galaxy from the main sequence (i.e.,
log[SSFR(galaxy)/SSFR_MS(M*,z)]) can be used to identify galaxies requiring the
use of an alpha_co conversion factor lower than the Galactic value.Comment: Accepted for publication in Astronomy and Astrophysics (A&A); 15
pages, 6 figures; V2: updated reference lis
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