248 research outputs found
Physical Properties of Galaxies from z=2-4
The epoch of galaxy assembly from 2<=z<=4 marks a critical stage during the
evolution of today's galaxy population. During this period the star-formation
activity in the Universe was at its peak level, and the structural patterns
observed among galaxies in the local Universe were not yet in place. A variety
of novel techniques have been employed over the past decade to assemble
multiwavelength observations of galaxies during this important epoch. In this
primarily observational review, I present a census of the methods used to find
distant galaxies and the empirical constraints on their multiwavelength
luminosities and colors. I then discuss what is known about the stellar content
and past histories of star formation in high-redshift galaxies; their
interstellar contents including dust, gas, and heavy elements; and their
structural and dynamical properties. I conclude by considering some of the most
pressing and open questions regarding the physics of high-redshift galaxies,
which are to be addressed with future facilities.Comment: ARA&A Volume 49, in press; 123 pages, 18 figure
Substructure within the SSA22 protocluster at
We present the results of a densely sampled spectroscopic survey of the SSA22
protocluster at . Our sample with Keck/LRIS spectroscopy
includes 106 Ly Emitters (LAEs) and 40 Lyman Break Galaxies (LBGs) at
. These galaxies are contained within the region in
which the protocluster was discovered, which also hosts the maximum galaxy
overdensity in the SSA22 region. The redshift histogram of our spectroscopic
sample reveals two distinct peaks, at (blue, 43 galaxies) and
(red, 103 galaxies). Furthermore, objects in the blue and red peaks
are segregated on the sky, with galaxies in the blue peak concentrating towards
the western half of the field. These results suggest that the blue and red
redshift peaks represent two distinct structures in physical space. Although
the double-peaked redshift histogram is traced in the same manner by LBGs and
LAEs, and brighter and fainter galaxies, we find that nine out of 10 X-ray AGNs
in SSA22, and all seven spectroscopically-confirmed giant Ly "blobs,"
reside in the red peak. We combine our dataset with sparsely sampled
spectroscopy from the literature over a significantly wider area, finding
preliminary evidence that the double-peaked structure in redshift space extends
beyond the region of our dense spectroscopic sampling. In order to fully
characterize the three-dimensional structure, dynamics, and evolution of
large-scale structure in the SSA22 overdensity, we require the measurement of
large samples of LAE and LBG redshifts over a significantly wider area, as well
as detailed comparisons with cosmological simulations of massive cluster
formation.Comment: 6 pages, 4 figures, Accepted to ApJ Letter
Biases in metallicity measurements from global galaxy spectra: the effects of flux-weighting and diffuse ionized gas contamination
Galaxy metallicity scaling relations provide a powerful tool for
understanding galaxy evolution, but obtaining unbiased global galaxy gas-phase
oxygen abundances requires proper treatment of the various line-emitting
sources within spectroscopic apertures. We present a model framework that
treats galaxies as ensembles of HII and diffuse ionized gas (DIG) regions of
varying metallicities. These models are based upon empirical relations between
line ratios and electron temperature for HII regions, and DIG strong-line ratio
relations from SDSS-IV MaNGA IFU data. Flux-weighting effects and DIG
contamination can significantly affect properties inferred from global galaxy
spectra, biasing metallicity estimates by more than 0.3 dex in some cases. We
use observationally-motivated inputs to construct a model matched to typical
local star-forming galaxies, and quantify the biases in strong-line ratios,
electron temperatures, and direct-method metallicities as inferred from global
galaxy spectra relative to the median values of the HII region distributions in
each galaxy. We also provide a generalized set of models that can be applied to
individual galaxies or galaxy samples in atypical regions of parameter space.
We use these models to correct for the effects of flux-weighting and DIG
contamination in the local direct-method mass-metallicity and fundamental
metallicity relations, and in the mass-metallicity relation based on
strong-line metallicities. Future photoionization models of galaxy line
emission need to include DIG emission and represent galaxies as ensembles of
emitting regions with varying metallicity, instead of as single HII regions
with effective properties, in order to obtain unbiased estimates of key
underlying physical properties.Comment: 37 pages, 29 figures, 4 tables. Accepted to ApJ. See Figures 15-17
for typical global galaxy biases in strong-line ratios, electron
temperatures, and direct-method metallicitie
The Rest Frame Ultraviolet Spectra of UV-Selected Active Galactic Nuclei at z ~ 2-3
We present new results for a sample of 33 narrow-lined UV-selected active
galactic nuclei (AGNs), identified in the course of a spectroscopic survey for
star-forming galaxies at z ~ 2-3. The rest-frame UV composite spectrum for our
AGN sample shows several emission lines characteristic of AGNs, as well as
interstellar absorption features seen in star-forming Lyman Break Galaxies
(LBGs). We report a detection of NIV]1486, which has been observed in
high-redshift radio galaxies, as well as in rare optically-selected quasars.
The UV continuum slope of the composite spectrum is significantly redder than
that of a sample of non-AGN UV-selected star forming galaxies. Blueshifted SiIV
absorption provides evidence for outflowing highly-ionized gas in these objects
at speeds of ~ 10^(3) km/s, quantitatively different from what is seen in the
outflows of non-AGN LBGs. Grouping the individual AGNs by parameters such as
Ly-alpha equivalent width, redshift, and UV continuum magnitude allows for an
analysis of the major spectroscopic trends within the sample. Stronger Ly-alpha
emission is coupled with weaker low-ionization absorption, which is similar to
what is seen in the non-AGN LBGs, and highlights the role that cool
interstellar gas plays in the escape of Ly-alpha photons. However, the AGN
composite does not show the same trends between Ly-alpha strength and
extinction seen in the non-AGN LBGs. These results represent the first such
comparison at high-redshift between star-forming galaxies and similar galaxies
that host AGN activity.Comment: 13 pages, 6 figures, accepted by Ap
The Kinematics of CIV in Star-Forming Galaxies at z~1.2
We present the first statistical sample of rest-frame far-UV spectra of
star-forming galaxies at z~1. These spectra are unique in that they cover the
high-ionization CIV{\lambda}{\lambda}1548, 1550 doublet. We also detect
low-ionization features such as SiII{\lambda}1527, FeII{\lambda}1608,
AlII{\lambda}1670, NiII{\lambda}{\lambda}1741, 1751 and SiII{\lambda}1808, and
intermediate-ionization features from AlIII{\lambda}{\lambda}1854, 1862.
Comparing the properties of absorption lines of lower- and higher- ionization
states provides a window into the multi-phase nature of circumgalactic gas. Our
sample is drawn from the DEEP2 survey and spans the redshift range 1.01 < z <
1.35 ( = 1.25). By isolating the interstellar CIV absorption from the
stellar P-Cygni wind profile we find that 69% of the CIV profiles are
blueshifted with respect to the systemic velocity. Furthermore, CIV shows a
small but significant blueshift relative to FeII (offset of the best-fit linear
regression -76 26 km/s). At the same time, the CIV blueshift is on
average comparable to that of MgII{\lambda}{\lambda}2796, 2803. At this point,
in explaining the larger blueshift of CIV absorption at the ~ 3-sigma level, we
cannot distinguish between the faster motion of highly-ionized gas relative to
gas traced by FeII, and filling in on the red side from resonant CIV emission.
We investigate how far-UV interstellar absorption kinematics correlate with
other galaxy properties using stacked spectra. These stacking results show a
direct link between CIV absorption and the current SFR, though we only observe
small velocity differences among different ionization states tracing the
outflowing ISM.Comment: 21 pages, 14 figures, ApJ, accepte
Physical Properties of a Pilot Sample of Spectroscopic Close Pair Galaxies at z ~ 2
We use Hubble Space Telescope Wide-Field Camera 3 (HST/WFC3) rest-frame
optical imaging to select a pilot sample of star-forming galaxies in the
redshift range z = 2.00-2.65 whose multi-component morphologies are consistent
with expectations for major mergers. We follow up this sample of major merger
candidates with Keck/NIRSPEC longslit spectroscopy obtained in excellent seeing
conditions (FWHM ~ 0.5 arcsec) to obtain Halpha-based redshifts of each of the
morphological components in order to distinguish spectroscopic pairs from false
pairs created by projection along the line of sight. Of six pair candidates
observed, companions (estimated mass ratios 5:1 and 7:1) are detected for two
galaxies down to a 3sigma limiting emission-line flux of ~ 10^{-17} erg/s/cm2.
This detection rate is consistent with a ~ 50% false pair fraction at such
angular separations (1-2 arcsec), and with recent claims that the
star-formation rate (SFR) can differ by an order of magnitude between the
components in such mergers. The two spectroscopic pairs identified have total
SFR, SFR surface densities, and stellar masses consistent on average with the
overall z ~ 2 star forming galaxy population.Comment: 11 pages, 5 figures. Accepted for publication in Ap
The Direct Detection of Lyman Continuum Emission from Star-forming Galaxies at z~3
We present the results of rest-frame UV spectroscopic observations of a sample of 14 z ~ 3 star-forming galaxies in the SSA 22a field. These spectra are characterized by unprecedented depth in the Lyman continuum region. For the first time, we have detected escaping ionizing radiation from individual galaxies at high redshift, with 2 of the 14 objects showing significant emission below the Lyman limit. We also measured the ratio of emergent flux density at 1500 Å to that in the Lyman continuum region, for the individual detections (C49 and D3) and the sample average. If a correction for the average IGM opacity is applied to the spectra of the objects C49 and D3, we find f_(1500)/f_(900,corr,C49) = 4.5 and f_(1500)/f_(900,corr,D3) = 2.9. The average emergent flux density ratio in our sample is = 22, implying an escape fraction ~4.5 times lower than inferred from the composite spectrum from Steidel and coworkers. If this new estimate is representative of LBGs, their contribution to the metagalactic ionizing radiation field is J_ν(900) ~ 2.6 × 10^(-22) ergs s^(-1) cm^(-2) Hz^(-1) sr^(-1), comparable to the contribution of optically selected quasars at the same redshift. The sum of the contributions from galaxies and quasars is consistent with recent estimates of the level of the ionizing background at z ~ 3, inferred from the H I Lyα forest optical depth. There is significant variance among the emergent far-UV spectra in our sample, yet the factors controlling the detection or nondetection of Lyman continuum emission from galaxies are not well determined. Because we do not yet understand the source of this variance, significantly larger samples will be required to obtain robust constraints on the galaxy contribution to the ionizing background at z ~ 3 and beyond
Understanding large-scale structure in the SSA22 protocluster region using cosmological simulations
We investigate the nature and evolution of large-scale structure within the
SSA22 protocluster region at using cosmological simulations. A
redshift histogram constructed from current spectroscopic observations of the
SSA22 protocluster reveals two separate peaks at (blue) and (red). Based on these data, we report updated overdensity and mass
calculations for the SSA22 protocluster. We find ,
for the blue and red peaks, respectively, and
for the entire region. These overdensities
correspond to masses of , , and
for the red, blue, and
total peaks, respectively. We use the Small MultiDark Planck (SMDPL) simulation
to identify comparably massive protoclusters, and uncover the
underlying structure and ultimate fate of the SSA22 protocluster. For this
analysis, we construct mock redshift histograms for each simulated
protocluster, quantitatively comparing them with the observed SSA22 data. We
find that the observed double-peaked structure in the SSA22 redshift histogram
corresponds not to a single coalescing cluster, but rather the proximity of a
protocluster and at least one cluster progenitor. Such associations in the SMDPL simulation are
easily understood within the framework of hierarchical clustering of dark
matter halos. We finally find that the opportunity to observe such a phenomenon
is incredibly rare, with an occurrence rate of 7.4h^3 \mbox{ Gpc}^{-3}.Comment: 13 pages, 8 figures, Accepted to Ap
The Kinematics of Morphologically Selected z~2 Galaxies in the GOODS-N Field
We present near-IR spectra of H-alpha emission from 13 galaxies at z~2 in the
GOODS-N field. The galaxies were selected primarily because they appear to have
elongated morphologies, and slits were aligned with the major axes (as
determined from the rest-frame UV emission) of 11 of the 13. If the galaxies
are elongated because they are highly inclined, alignment of the slit and major
axis should maximize the observed velocity and reveal velocity shear, if
present. In spite of this alignment, we see spatially resolved velocity shear
in only two galaxies. We show that the seeing makes a large difference in the
observed velocity spread of a tilted emission line, and use this information to
place limits on the velocity spread of the ionized gas of the galaxies in the
sample: we find that all 13 have v_{0.5} < 110 km/s, where v_{0.5} is the
velocity shear (half of the velocity range of a tilted emission line) that
would be observed under our best seeing conditions of ~0.5". When combined with
previous work, our data also indicate that aligning the slit along the major
axis does not increase the probability of observing a tilted emission line. We
then focus on the one-dimensional velocity dispersion \sigma, which is much
less affected by the seeing, and see that the elongated subsample exhibits a
significantly lower velocity dispersion than galaxies selected at random from
our total H-alpha sample, not higher as one might have expected. We also see
some evidence that the elongated galaxies are less reddened than those randomly
selected using only UV colors. Both of these results are counter to what would
be expected if the elongated galaxies were highly inclined disks. It is at
least as likely that the galaxies' elongated morphologies are due to merging
subunits.Comment: 9 pages, 5 figures. Accepted for publication in Ap
A High-Resolution Hubble Space Telescope Study of Apparent Lyman Continuum Leakers at
We present follow-up observations of 16
candidate LyC emitters in the HS1549+1919 field. With these data, we
obtain high spatial-resolution photometric redshifts of all sub-arcsecond
components of the LyC candidates in order to eliminate foreground contamination
and identify robust candidates for leaking LyC emission. Of the 16 candidates,
we find one object with a robust LyC detection that is not due to foreground
contamination. This object (MD5) resolves into two components; we refer to the
LyC-emitting component as MD5b. MD5b has an observed 1500\AA\ to 900\AA\
flux-density ratio of , compatible with
predictions from stellar population synthesis models. Assuming minimal IGM
absorption, this ratio corresponds to a relative (absolute) escape fraction of
% (%). The stellar
population fit to MD5b indicates an age of Myr, which is in the
youngest 10% of the sample and the youngest third of typical
Lyman break galaxies, and may be a contributing factor to its LyC detection. We
obtain a revised, contamination-free estimate for the comoving specific
ionizing emissivity at , indicating (with large uncertainties) that
star-forming galaxies provide roughly the same contribution as QSOs to the
ionizing background at this redshift. Our results show that foreground
contamination prevents ground-based LyC studies from obtaining a full
understanding of LyC emission from star-forming galaxies. Future
progress in direct LyC searches is contingent upon the elimination of
foreground contaminants through high spatial-resolution observations, and upon
acquisition of sufficiently deep LyC imaging to probe ionizing radiation in
high-redshift galaxies.Comment: 31 pages, 5 tables, 19 figures. Accepted to ApJ. Version with
full-resolution figures is available at:
http://www.astro.ucla.edu/~aes/Mostardi_HST_LyC.pd
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