2,341 research outputs found
Evidence for a Gradual Decline in the Universal Rest-Frame UV Luminosity Density for z < 1
We have utilized various magnitude-limited samples drawn from an extremely
deep and highly complete spectroscopic redshift survey of galaxies observed in
seven colors in the Hawaii Survey Fields and the Hubble Deep Field to
investigate the evolution of the universal rest-frame ultraviolet luminosity
density from z = 1 to the present. The multi-color data (U', B, V, R, I, J,
HK') enable the sample selection to be made in the rest-frame ultraviolet for
the entire redshift range. Due to the large sample size and depth (U_{AB} =
24.75, B_{AB} = 24.75, I_{AB} = 23.5), we are able to accurately determine the
luminosity density to z = 1. We do not confirm the very steep evolution
reported by Lilly et al. (1996) but instead find a shallower slope,
approximately (1+z)^{1.5} for q0 = 0.5, which would imply that galaxy formation
is continuing smoothly to the present time rather than peaking at z = 1. Much
of the present formation is taking place in smaller galaxies. Detailed
comparisons with other recent determinations of the evolution are presented.Comment: 37 pages including 18 figures. Also available at
http://www.ifa.hawaii.edu/~acowie/uvlum.html To be published in the August,
1999 Astronomical Journal (accepted April 22, 1999
The Changing AGN Population
We investigate how the fraction of broad-line sources in the AGN population
changes with X-ray luminosity and redshift. We first construct the rest-frame
hard-energy (2-8 keV) X-ray luminosity function (HXLF) at z=0.1-1 using Chandra
Lockman Hole-Northwest wide-area data, Chandra Deep Field-North 2 Ms data,
other Chandra deep field data, and the ASCA Large Sky Survey data. We find that
broad-line AGNs dominate above 3e43 ergs/s and have a mean luminosity of 1.3e44
ergs/s. Type II AGNs can only become an important component of the X-ray
population at Seyfert-like X-ray luminosities. We then construct z=0.1-0.5 and
z=0.5-1 HXLFs and compare them with both the local HXLF measured from HEAO-1 A2
survey data and the z=1.5-3 HXLF measured from soft-energy (0.5-2 keV) Chandra
and ROSAT data. We find that the number density of >1e44 ergs/s sources
(quasars) steadily declines with decreasing redshift, while the number density
of 1e43-1e44 ergs/s sources peaks at z=0.5-1. Strikingly, however, the number
density of broad-line AGNs remains roughly constant with redshift while their
average luminosities decline at the lower redshifts, showing another example of
cosmic downsizing.Comment: Accepted by The Astrophysical Journal Letters, 5 page
Approaching Reionization: The Evolution of the Lyman Alpha Forest from Redshifts Four to Six
We analyze the Ly alpha forest properties of a sample of 15 high redshift
quasars lying between z = 4.42 and z = 5.75, using high signal-to-noise spectra
obtained with ESI on the Keck II 10 m telescope. The distribution of
transmissions in the Ly alpha region in this redshift range is shown to be
consistent with that found in lambda cold dark matter simulations with a
smoothly evolving ionization rate as a function of redshift. The extrapolation
of the ionizing flux to z = 6.05 lies a factor of two higher than a 2 sigma
upper limit placed by Cen & McDonald (2001) at this redshift, based on the
Becker et al. (2001) spectra of the z = 6.28 quasar SDSS 1030+0524. However,
the data are also consistent with models in which there is substantial
variation of the ionization parameter about the mean value, and in this case,
dark gaps such as those seen by Becker et al. become much more likely. We
conclude that further data are needed before we can be sure that we have seen
the epoch of reionization. We also summarize the damped Ly alpha systems seen
in these quasar lines of sight and measure their metallicities and kinematic
properties. We argue that the mean DLA metallicity has dropped substantially by
z = 5 compared with its value at z < 4.Comment: 17 pages, including 13 figures. Accepted for publication in
Astronomical Journal (May 2002
A Submillimeter and Radio Survey of Gamma-Ray Burst Host Galaxies: A Glimpse into the Future of Star Formation Studies
We present the first comprehensive search for submillimeter and radio
emission from the host galaxies of twenty well-localized gamma-ray bursts
(GRBs). With the exception of a single source, all observations were undertaken
months to years after the GRB explosions to ensure negligible contamination
from the afterglows. We detect the host galaxy of GRB 000418 in both the sub-mm
and radio, and the host galaxy of GRB 000210 only in the sub-mm. These
observations, in conjunction with the previous detections of the host galaxies
of GRB 980703 and GRB 010222, indicate that about 20% of GRB host galaxies are
ultra-luminous and have star formation rates of about 500 M_sun/yr. As an
ensemble, the non-detected hosts have a star formation rate of about 100
M_sun/yr (5-sigma) based on their radio emission. The detected and ensemble
star formation rates exceed the optical values by an order of magnitude,
indicating significant dust obscuration. In the same vein, the ratio of
bolometric dust luminosity to UV luminosity for the hosts detected in the
sub-mm and radio ranges from 20-800, and follows the known trend of increasing
obscuration with increasing bolometric luminosity. We also show that, both as a
sample and individually, the GRB host galaxies have bluer R-K colors as
compared with galaxies selected in the sub-mm in the same redshift range. This
possibly indicates that the stellar populations in the GRB hosts are on average
younger, supporting the massive stellar progenitor scenario for GRBs, but it is
also possible that GRB hosts are on average less dusty.Comment: Submitted to ApJ; 36 pages, 3 tables, 7 figures; updated reference
Optical identification of ISO far-infrared sources in the Lockman Hole using a deep VLA 1.4 GHz continuum survey
By exploiting the far-infrared(FIR) and radio correlation, we have performed
the Likelihood-Ratio analysis to identify optical counterparts to the
far-infrared sources in the Lockman Hole. Using the likelihood ratio analysis
and the associated reliability, 44 FIR sources have been identified with radio
sources. Redshifts have been obtained for 29 out of 44 identified sources. One
hyper-luminous infrared galaxy (HyLIRG) with and four ultraluminous infrared
galaxies (ULIRGs) are identified in our sample. The space density of the FIR
sources at z = 0.3-0.6 is 4.6\times 10^{-5}Mpc^{-3}, implying a rapid evolution
of the ULIRG population. Most of \ISO FIR sources have their FIR-radio ratios
similar to star-forming galaxies ARP 220 and M82. At least seven of our FIR
sources show evidence for the presence of an active galactic nucleus (AGN) in
optical emission lines, radio continuum excess, or X-ray activity. Three out of
five (60%) of the ULIRG/HyLIRGs are AGN galaxies. Five of the seven AGN
galaxies are within the ROSAT X-ray survey field, and two are within the
XMM-Newton survey fields. X-ray emission has been detected in only one source,
1EX030, which is optically classified as a quasar. The non-detection in the
XMM-Newton 2-10 keV band suggests a very thick absorption obscuring the central
source of the two AGN galaxies. Several sources have an extreme FIR luminosity
relative to the optical R-band, L(90\mu\mathrm{m})/L(R) > 500, which is rare
even among the local ULIRG population. While source confusion or blending might
offer an explanation in some cases, they may represent a new population of
galaxies with an extreme activity of star formation in an undeveloped stellar
system -- i.e., formation of bulges or young ellipticals.Comment: 55 pages, 16 figures. To appear in A
Optically Faint Microjansky Radio Sources
We report on the identifications of radio sources from our survey of the
Hubble Deep Field and the SSA13 fields, both of which comprise the deepest
radio surveys to date at 1.4 GHz and 8.5 GHz respectively. About 80% of the
microjansky radio sources are associated with moderate redshift starburst
galaxies or AGNs within the I magnitude range of 17 to 24 with a median of I =
22 mag. Thirty-one (20%) of the radio sources are: 1) fainter than 25 mag,
with two objects in the HDF 28.5, 2) often identified with very red
objects 4, and 3) not significantly different in radio properties than
the brighter objects. We suggest that most of these objects are associated with
heavily obscured starburst galaxies with redshifts between 1 and 3. However,
other mechanisms are discussed and cannot be ruled out with the present
observations.Comment: to appear in Astrophysical Journal Letters, 3 figures, 1 tabl
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