1,973 research outputs found
Towards understanding the relation between the gas and the attenuation in galaxies at kpc scales
[abridged]
Aims. The aim of the present paper is to provide new and more detailed
relations at the kpc scale between the gas surface density and the face-on
optical depth directly calibrated on galaxies, in order to compute the
attenuation not only for semi-analytic models but also observationally as new
and upcoming radio observatories are able to trace gas ever farther in the
Universe.
Methods. We have selected a sample of 4 nearby resolved galaxies and a sample
of 27 unresolved galaxies from the Herschel Reference Survey and the Very
Nearby Galaxies Survey, for which we have a large set of multi-wavelength data
from the FUV to the FIR including metallicity gradients for resolved galaxies,
along with radio HI and CO observations. For each pixel in resolved galaxies
and for each galaxy in the unresolved sample, we compute the face-on optical
depth from the attenuation determined with the CIGALE SED fitting code and an
assumed geometry. We determine the gas surface density from HI and CO
observations with a metallicity-dependent XCO factor.
Results. We provide new, simple to use, relations to determine the face-on
optical depth from the gas surface density, taking the metallicity into
account, which proves to be crucial for a proper estimate. The method used to
determine the gas surface density or the face-on optical depth has little
impact on the relations except for galaxies that have an inclination over 50d.
Finally, we provide detailed instructions on how to compute the attenuation
practically from the gas surface density taking into account possible
information on the metallicity.
Conclusions. Examination of the influence of these new relations on simulated
FUV and IR luminosity functions shows a clear impact compared to older oft-used
relations, which in turn could affect the conclusions drawn from studies based
on large scale cosmological simulations.Comment: 24 pages, 21 figures, accepted for publication in A&
A Further Look Into Quenching: Tearing Apart The Main Sequence Into Its Bulge, Disk And Gas Content
PowerPoint of Galaxy Evolution across Time conference: https://galaxiesinparis.sciencesconf.orgGalaxie
A hyper luminous starburst at z=4.72 magnified by a lensing galaxy pair at z=1.48
International audienceWe serendipitously discovered in the Herschel Reference Survey an extremely bright infrared source with S500 ∼ 120 mJy in the line of sight of the Virgo cluster which we name Red Virgo 4 (RV4). Based on IRAM/EMIR and IRAM/NOEMA detections of the CO(5−4), CO(4−3), and [CI] lines, RV4 is located at a redshift of 4.724, yielding a total observed infrared luminosity of 1.1 ± 0.6 × 1014 L⊙. At the position of the Herschel emission, three blobs are detected with the VLA at 10 cm. The CO(5−4) line detection of each blob confirms that they are at the same redshift with the same line width, indicating that they are multiple images of the same source. In Spitzer and deep optical observations, two sources, High-z Lens 1 (HL1) West and HL1 East, are detected at the center of the three VLA/NOEMA blobs. These two sources are placed at z = 1.48 with X-shooter spectra, suggesting that they could be merging and gravitationally lensing the emission of RV4. HL1 is the second most distant lens known to date in strong lensing systems. Constrained by the position of the three VLA/NOEMA blobs, the Einstein radius of the lensing system is 2.2″ ± 0.2 (20 kpc). The high redshift of HL1 and the large Einstein radius are highly unusual for a strong lensing system. In this paper, we present the insterstellar medium properties of the background source RV4. Different estimates of the gas depletion time yield low values suggesting that RV4 is a starburst galaxy. Among all high-z submillimeter galaxies, this source exhibits one of the lowest L[CI] to LIR ratios, 3.2 ± 0.9 × 10−6, suggesting an extremely short gas depletion time of only 14 ± 5 Myr. It also shows a relatively high L[CI] to LCO(4−3) ratio (0.7 ± 0.2) and low LCO(5−4) to LIR ratio (only ∼50% of the value expected for normal galaxies) hinting at low density of gas. Finally, we discuss the short depletion time of RV4. It can be explained by either a very high star formation efficiency, which is difficult to reconcile with major mergers simulations of high-z galaxies, or a rapid decrease of star formation, which would bias the estimate of the depletion time toward an artificially low value
PACS photometry of the Herschel Reference Survey - Far-infrared/sub-millimeter colours as tracers of dust properties in nearby galaxies
We present Herschel/PACS 100 and 160 micron integrated photometry for the 323
galaxies in the Herschel Reference Survey (HRS), a K-band-, volume-limited
sample of galaxies in the local Universe. Once combined with the Herschel/SPIRE
observations already available, these data make the HRS the largest
representative sample of nearby galaxies with homogeneous coverage across the
100-500 micron wavelength range. In this paper, we take advantage of this
unique dataset to investigate the properties and shape of the
far-infrared/sub-millimeter spectral energy distribution in nearby galaxies. We
show that, in the stellar mass range covered by the HRS (8<log(M*/Msun)<12),
the far-infrared/sub-millimeter colours are inconsistent with a single modified
black-body having the same dust emissivity index beta for all galaxies. In
particular, either beta decreases, or multiple temperature components are
needed, when moving from metal-rich/gas-poor to metal-poor/gas-rich galaxies.
We thus investigate how the dust temperature and mass obtained from a single
modified black-body depend on the assumptions made on beta. We show that, while
the correlations between dust temperature, galaxy structure and star formation
rate are strongly model dependent, the dust mass scaling relations are much
more reliable, and variations of beta only change the strength of the observed
trends.Comment: 26 pages, 8 figures, 2 tables. Accepted for publication in MNRA
MB 700 Anthropology for Christian Mission
Textbook: Cultural Anthropology: An Applied Perspective, fifth edition by Gary Ferraro Readings: Anthropology and Christian Mission: A Reader, Darrell Whiteman (ed.)Customs and Cultures by Eugene Nidahttps://place.asburyseminary.edu/syllabi/2521/thumbnail.jp
Linking dust emission to fundamental properties in galaxies: The low-metallicity picture
In this work, we aim at providing a consistent analysis of the dust
properties from metal-poor to metal-rich environments by linking them to
fundamental galactic parameters. We consider two samples of galaxies: the Dwarf
Galaxy Survey (DGS) and KINGFISH, totalling 109 galaxies, spanning almost 2 dex
in metallicity. We collect infrared (IR) to submillimetre (submm) data for both
samples and present the complete data set for the DGS sample. We model the
observed spectral energy distributions (SED) with a physically-motivated dust
model to access the dust properties. Using a different SED model (modified
blackbody), dust composition (amorphous carbon), or wavelength coverage at
submm wavelengths results in differences in the dust mass estimate of a factor
two to three, showing that this parameter is subject to non-negligible
systematic modelling uncertainties. For eight galaxies in our sample, we find a
rather small excess at 500 microns (< 1.5 sigma). We find that the dust SED of
low-metallicity galaxies is broader and peaks at shorter wavelengths compared
to more metal-rich systems, a sign of a clumpier medium in dwarf galaxies. The
PAH mass fraction and the dust temperature distribution are found to be driven
mostly by the specific star-formation rate, SSFR, with secondary effects from
metallicity. The correlations between metallicity and dust mass or total-IR
luminosity are direct consequences of the stellar mass-metallicity relation.
The dust-to-stellar mass ratios of metal-rich sources follow the well-studied
trend of decreasing ratio for decreasing SSFR. The relation is more complex for
highly star-forming low-metallicity galaxies and depends on the chemical
evolutionary stage of the source (i.e., gas-to-dust mass ratio). Dust growth
processes in the ISM play a key role in the dust mass build-up with respect to
the stellar content at high SSFR and low metallicity. (abridged)Comment: 44 pages (20 pages main body plus 5 Appendices), 11 figures, 9
tables, accepted for publication in A&
Cold Dust but Warm Gas in the Unusual Elliptical Galaxy NGC 4125
Data from the Herschel Space Observatory have revealed an unusual elliptical galaxy, NGC 4125, which has strong and extended submillimeter emission from cold dust but only very strict upper limits to its CO and Hi emission. Depending on the dust emissivity, the total dust mass is 2-5 x 10(6) M-circle dot. While the neutral gas-to-dust mass ratio is extremely low (= 10(4) K faster than the dust is evaporated. If galaxies like NGC 4125, where the far-infrared emission does not trace neutral gas in the usual manner, are common at higher redshift, this could have significant implications for our understanding of high redshift galaxies and galaxy evolution.Canadian Space AgencyNatural Sciences and Engineering Research Council of CanadaAgenzia Spaziale Italiana (ASI) I/005/11/0BMVIT (Austria)ESA-PRODEX (Belgium)CEA/CNES (France)DLR (Germany)ASI/INAF (Italy)CICYT/MCYT (Spain)CSA (Canada)NAOC (China)CEA, (France)CNES (France)CNRS (France)ASI (Italy)MCINN (Spain)SNSB (Sweden)STFC (UK)NASA (USA)National Aeronautics and Space AdministrationAstronom
Welcome to the Twilight Zone: The Mid-Infrared Properties of Poststarburst Galaxies
We investigate the optical and Wide-field Survey Explorer (WISE) colors of
"E+A" identified post-starburst galaxies, including a deep analysis on 190
post-starbursts detected in the 2{\mu}m All Sky Survey Extended Source Catalog.
The post-starburst galaxies appear in both the optical green valley and the
WISE Infrared Transition Zone (IRTZ). Furthermore, we find that post-starbursts
occupy a distinct region [3.4]-[4.6] vs. [4.6]-[12] WISE colors, enabling the
identification of this class of transitioning galaxies through the use of
broad-band photometric criteria alone. We have investigated possible causes for
the WISE colors of post-starbursts by constructing a composite spectral energy
distribution (SED), finding that mid-infrared (4-12{\mu}m) properties of
post-starbursts are consistent with either 11.3{\mu}m polycyclic aromatic
hydrocarbon emission, or Thermally Pulsating Asymptotic Giant Branch (TP-AGB)
and post-AGB stars. The composite SED of extended post- starburst galaxies with
22{\mu}m emission detected with signal to noise >3 requires a hot dust
component to produce their observed rising mid-infrared SED between 12 and
22{\mu}m. The composite SED of WISE 22{\mu}m non-detections (S/N<3), created by
stacking 22{\mu}m images, is also flat, requiring a hot dust component. The
most likely source of this mid-infrared emission of these E+A galaxies is a
buried active galactic nucleus. The inferred upper limit to the Eddington
ratios of post-starbursts are 1e-2 to 1e-4, with an average of 1e-3. This
suggests that AGNs are not radiatively dominant in these systems. This could
mean that including selections able to identify active galactic nuclei as part
of a search for transitioning and post-starburst galaxies would create a more
complete census of the transition pathways taken as a galaxy quenches its star
formation.Comment: 13 pages, 11 figures, accepted for publication in the Astrophysical
Journa
Infrared color selection of massive galaxies at z > 3
We introduce a new color-selection technique to identify high-redshift,
massive galaxies that are systematically missed by Lyman-break selection. The
new selection is based on the H_{160} and IRAC 4.5um bands, specifically H -
[4.5] > 2.25 mag. These galaxies, dubbed "HIEROs", include two major
populations that can be separated with an additional J - H color. The
populations are massive and dusty star-forming galaxies at z > 3 (JH-blue) and
extremely dusty galaxies at z < 3 (JH-red). The 350 arcmin^2 of the GOODS-N and
GOODS-S fields with the deepest HST/WFC3 and IRAC data contain 285 HIEROs down
to [4.5] 3) HIEROs, which
have a median photometric redshift z ~4.4 and stellar massM_{*}~10^{10.6} Msun,
and are much fainter in the rest-frame UV than similarly massive Lyman-break
galaxies (LBGs). Their star formation rates (SFRs) reaches ~240 Msun yr^{-1}
leading to a specific SFR, sSFR ~4.2 Gyr^{-1}, suggesting that the sSFRs for
massive galaxies continue to grow at z > 2 but at a lower growth rate than from
z=0 to z=2. With a median half-light radius of 2 kpc, including ~20% as compact
as quiescent galaxies at similar redshifts, JH-blue HIEROs represent perfect
star-forming progenitors of the most massive (M_{*} > 10^{11.2} Msun) compact
quiescent galaxies at z ~ 3 and have the right number density. HIEROs make up
~60% of all galaxies with M_{*} > 10^{10.5} Msun identified at z > 3 from their
photometric redshifts. This is five times more than LBGs with nearly no overlap
between the two populations. While HIEROs make up 15-25% of the total SFR
density at z ~ 4-5, they completely dominate the SFR density taking place in
M_{*} >10^{10.5} Msun galaxies, and are therefore crucial to understanding the
very early phase of massive galaxy formation.Comment: ApJS, in pres
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