246 research outputs found
HST ultraviolet spectral energy distributions for three ultraluminous infrared galaxies
We present HST Faint Object Camera ultraviolet (230 nm and 140 nm) images of
three ultraluminous infrared galaxies (ULIG: L_ir > 10^12 L_sun) selected from
the IRAS Revised Bright Galaxy Sample. The purpose is to estimate spectral
energy distributions (SEDs) to facilitate the identification of similar objects
at high redshift in deep optical, infrared, and submm surveys.
All three galaxies (VII Zw031 = IRAS F12112+0305, and IRAS F22491-1808) were
well detected at 230 nm. Two of the three were marginally detected at 140 nm.
The fluxes, together with ground-based optical and infrared photometry, are
used to compute SEDs over a wide wavelength range. The measured SEDs drop from
the optical to the ultraviolet, but the magnitude of the drop ranges from a
factor of ~3 in IRAS F22491-1808 to a factor of ~100 in VIIZw031. This is most
likely due to different internal extinctions. Such an interpretation is also
suggested by extrapolating to ultraviolet wavelengths the optical internal
extinction measured in VIIZw031. K-corrections are calculated to determine the
colors of the sample galaxies as seen at high redshifts. Galaxies like VIIZw031
have very low observed rest-frame UV fluxes which means that such galaxies at
high redshift will be extremely red or even missing in optical surveys. On the
other hand, galaxies like IRAS F12112+0305 and IRAS F22491-1808, if seen at
high redshift, would be sufficiently blue that they would not easily be
distinguished from normal field galaxies, and therefore, identified as ULIGs.
The implication is then that submillimeter surveys may be the only means of
properly identifying the majority of ULIGs at high redshift.Comment: AJ in press, TeX, 23 pages, 7 tab, 17 figs available also (at higher
resolution) from http://www.ast.cam.ac.uk~trentham/ufigs.htm
An X-ray photoelectron spectroscopy investigation of chromium conversion coatings and chromium compounds
Hexavalent and trivalent chromium based conversion coatings on zinc
electrodeposited steel have been investigated using X-ray photoelectron
spectroscopy (XPS) with the aim of elucidating their film chemistry. Furthermore, a
monochromatic Al Kα X-ray source was utilised and the spectra produced evaluated
using curve fitting software to elucidate oxidation state information. In addition, a
number of chromium compounds were investigated and used to complement the
curve fitting analysis for the conversion coatings.
High resolution Cr2p spectra from chromium compounds exhibited multiplet splitting
for Cr2O3. Additional satellite emissions can also be observed for Cr2O3 and Cr(OH)3.
Curve fitting of hexavalent chromium conversion coating (CCC) 2p3/2 spectra
contained both Cr(VI) and Cr(III) species with the content of the former slightly higher
when the X-ray beam take-off angle (TOA) was reduced to determine more surface
specific information. The Cr(III) content was determined to be mainly composed of
Cr(OH)3 with some Cr2O3. In comparison, trivalent CCCs were largely composed of
Cr2O3 as opposed to Cr(OH)3. Survey scans of both coatings revealed that the
trivalent CCCs had a higher relative zinc content
Fitting the integrated Spectral Energy Distributions of Galaxies
Fitting the spectral energy distributions (SEDs) of galaxies is an almost
universally used technique that has matured significantly in the last decade.
Model predictions and fitting procedures have improved significantly over this
time, attempting to keep up with the vastly increased volume and quality of
available data. We review here the field of SED fitting, describing the
modelling of ultraviolet to infrared galaxy SEDs, the creation of
multiwavelength data sets, and the methods used to fit model SEDs to observed
galaxy data sets. We touch upon the achievements and challenges in the major
ingredients of SED fitting, with a special emphasis on describing the interplay
between the quality of the available data, the quality of the available models,
and the best fitting technique to use in order to obtain a realistic
measurement as well as realistic uncertainties. We conclude that SED fitting
can be used effectively to derive a range of physical properties of galaxies,
such as redshift, stellar masses, star formation rates, dust masses, and
metallicities, with care taken not to over-interpret the available data. Yet
there still exist many issues such as estimating the age of the oldest stars in
a galaxy, finer details ofdust properties and dust-star geometry, and the
influences of poorly understood, luminous stellar types and phases. The
challenge for the coming years will be to improve both the models and the
observational data sets to resolve these uncertainties. The present review will
be made available on an interactive, moderated web page (sedfitting.org), where
the community can access and change the text. The intention is to expand the
text and keep it up to date over the coming years.Comment: 54 pages, 26 figures, Accepted for publication in Astrophysics &
Space Scienc
Gravitational Lensing at Millimeter Wavelengths
With today's millimeter and submillimeter instruments observers use
gravitational lensing mostly as a tool to boost the sensitivity when observing
distant objects. This is evident through the dominance of gravitationally
lensed objects among those detected in CO rotational lines at z>1. It is also
evident in the use of lensing magnification by galaxy clusters in order to
reach faint submm/mm continuum sources. There are, however, a few cases where
millimeter lines have been directly involved in understanding lensing
configurations. Future mm/submm instruments, such as the ALMA interferometer,
will have both the sensitivity and the angular resolution to allow detailed
observations of gravitational lenses. The almost constant sensitivity to dust
emission over the redshift range z=1-10 means that the likelihood for strong
lensing of dust continuum sources is much higher than for optically selected
sources. A large number of new strong lenses are therefore likely to be
discovered with ALMA, allowing a direct assessment of cosmological parameters
through lens statistics. Combined with an angular resolution <0.1", ALMA will
also be efficient for probing the gravitational potential of galaxy clusters,
where we will be able to study both the sources and the lenses themselves, free
of obscuration and extinction corrections, derive rotation curves for the
lenses, their orientation and, thus, greatly constrain lens models.Comment: 69 pages, Review on quasar lensing. Part of a LNP Topical Volume on
"Dark matter and gravitational lensing", eds. F. Courbin, D. Minniti. To be
published by Springer-Verlag 2002. Paper with full resolution figures can be
found at ftp://oden.oso.chalmers.se/pub/tommy/mmviews.ps.g
The complex physics of dusty star-forming galaxies at high redshifts as revealed by Herschel and Spitzer
We combine far-infrared photometry from Herschel (PEP/HerMES) with deep mid-infrared spectroscopy from
Spitzer to investigate the nature and the mass assembly history of a sample of 31 luminous and ultraluminous
infrared galaxies ((U)LIRGs) at z ⌠1 and 2 selected in GOODS-S with 24Όm fluxes between 0.2 and 0.5 mJy.We
model the data with a self-consistent physical model (GRASIL) which includes a state-of-the-art treatment of dust
extinction and reprocessing. We find that all of our galaxies appear to require massive populations of old (>1 Gyr)
stars and, at the same time, to host a moderate ongoing activity of star formation (SFR 100M yrâ1). The bulk of
the stars appear to have been formed a few Gyr before the observation in essentially all cases. Only five galaxies of
the sample require a recent starburst superimposed on a quiescent star formation history.We also find discrepancies
between our results and those based on optical-only spectral energy distribution (SED) fitting for the same objects;
by fitting their observed SEDs with our physical model we find higher extinctions (by ÎAV ⌠0.81 and 1.14)
and higher stellar masses (by Îlog(M ) ⌠0.16 and 0.36 dex) for z ⌠1 and z ⌠2 (U)LIRGs, respectively. The
stellar mass difference is larger for the most dust-obscured objects. We also find lower SFRs than those computed
from LIR using the Kennicutt relation due to the significant contribution to the dust heating by intermediate-age
stellar populations through âcirrusâ emission (âŒ73% and âŒ66% of the total LIR for z ⌠1 and z ⌠2 (U)LIRGs,
respectively).Department of HE and Training approved lis
SPECTRA OF YOUNG GALAXIES
Invited review, Ringberg conference on "Galaxies in the Young Universe"
(Sept94)Comment: 12 pages, uuencoded compressed Postscript fil
A First Search for coincident Gravitational Waves and High Energy Neutrinos using LIGO, Virgo and ANTARES data from 2007
We present the results of the first search for gravitational wave bursts
associated with high energy neutrinos. Together, these messengers could reveal
new, hidden sources that are not observed by conventional photon astronomy,
particularly at high energy. Our search uses neutrinos detected by the
underwater neutrino telescope ANTARES in its 5 line configuration during the
period January - September 2007, which coincided with the fifth and first
science runs of LIGO and Virgo, respectively. The LIGO-Virgo data were analysed
for candidate gravitational-wave signals coincident in time and direction with
the neutrino events. No significant coincident events were observed. We place
limits on the density of joint high energy neutrino - gravitational wave
emission events in the local universe, and compare them with densities of
merger and core-collapse events.Comment: 19 pages, 8 figures, science summary page at
http://www.ligo.org/science/Publication-S5LV_ANTARES/index.php. Public access
area to figures, tables at
https://dcc.ligo.org/cgi-bin/DocDB/ShowDocument?docid=p120000
Planck early results XVII : Origin of the submillimetre excess dust emission in the Magellanic Clouds
Peer reviewe
- âŠ