72 research outputs found
Spectroscopic Identification of Massive Galaxies at z~2.3 with Strongly Suppressed Star Formation
We present first results of a spectroscopic survey targeting K-selected
galaxies at z=2.0-2.7 using the GNIRS instrument on Gemini-South. We obtained
near-infrared spectra with a wavelength coverage of 1.0-2.5 micron for 26
K-bright galaxies (K<19.7) selected from the MUSYC survey using photometric
redshifts. We successfully derived spectroscopic redshifts for all 26 galaxies
using rest-frame optical emission lines or the redshifted Balmer/4000 Angstrom
break. Twenty galaxies have spectroscopic redshifts in the range 2.0<z<2.7, for
which bright emission lines like Halpha and [OIII] fall in atmospheric windows.
Surprisingly, we detected no emission lines for nine of these 20 galaxies. The
median 2 sigma upper limit on the rest-frame equivalent width of Halpha for
these nine galaxies is ~10 Angstrom. The stellar continuum emission of these
same nine galaxies is best fitted by evolved stellar population models. The
best-fit star formation rate (SFR) is zero for five out of nine galaxies, and
consistent with zero within 1 sigma for the remaining four. Thus, both the
Halpha measurements and the independent stellar continuum modeling imply that
45% of our K-selected galaxies are not forming stars intensely. This high
fraction of galaxies without detected line emission and low SFRs may imply that
the suppression of star formation in massive galaxies occurs at higher redshift
than is predicted by current CDM galaxy formation models. However, obscured
star formation may have been missed, and deep mid-infrared imaging is needed to
clarify this situation.Comment: Accepted for publication in ApJ Letter
TOP2A and EZH2 Provide Early Detection of an Aggressive Prostate Cancer Subgroup.
Purpose: Current clinical parameters do not stratify indolent from aggressive prostate cancer. Aggressive prostate cancer, defined by the progression from localized disease to metastasis, is responsible for the majority of prostate cancer–associated mortality. Recent gene expression profiling has proven successful in predicting the outcome of prostate cancer patients; however, they have yet to provide targeted therapy approaches that could inhibit a patient\u27s progression to metastatic disease. Experimental Design: We have interrogated a total of seven primary prostate cancer cohorts (n = 1,900), two metastatic castration-resistant prostate cancer datasets (n = 293), and one prospective cohort (n = 1,385) to assess the impact of TOP2A and EZH2 expression on prostate cancer cellular program and patient outcomes. We also performed IHC staining for TOP2A and EZH2 in a cohort of primary prostate cancer patients (n = 89) with known outcome. Finally, we explored the therapeutic potential of a combination therapy targeting both TOP2A and EZH2 using novel prostate cancer–derived murine cell lines. Results: We demonstrate by genome-wide analysis of independent primary and metastatic prostate cancer datasets that concurrent TOP2A and EZH2 mRNA and protein upregulation selected for a subgroup of primary and metastatic patients with more aggressive disease and notable overlap of genes involved in mitotic regulation. Importantly, TOP2A and EZH2 in prostate cancer cells act as key driving oncogenes, a fact highlighted by sensitivity to combination-targeted therapy. Conclusions: Overall, our data support further assessment of TOP2A and EZH2 as biomarkers for early identification of patients with increased metastatic potential that may benefit from adjuvant or neoadjuvant targeted therapy approaches. ©2017 AACR
Effect of the supporting electrolyte anion on the thickness of PSS/PAH multilayer films and on their permeability to an electroactive probe.
Quartz crystal microbalance and cyclic voltammetry are used to investigate the influence of the supporting salt of polyelectrolyte solutions on the buildup and the structure of PSS/PAH polyelectrolyte multilayers (PSS: poly(4-styrene sulfonate); PAH: poly(allylamine hydrochloride)). This film constitutes a model polyelectrolyte multilayer system. The supporting electrolytes were sodium salts where the nature of the anion was changed by following the Hofmeister series from cosmotropic to chaotropic anions (F-, Cl-, NO3-, ClO4-). For all the investigated anions, the film thickness increases linearly with the number of deposition steps.Wefind that chaotropic anions lead to larger thickness increments per bilayer during the film buildup than cosmotropic ones, confirming results found on PSS/PDADMA multilayers (PDADMA:poly(diallyldimethylammonium)). Films constituted by more than nine PSS/PAH bilayers are still permeable to hexacyanoferrate(II) ions, Fe(CN)(6)4-, whatever the nature of the supporting salt anion. On the other hand, these films are impermeable to ruthenium(II) hexamine ions, Ru(NH3)(6)2+, after the third PAH layer in the presence of NaF, NaCl, or NaNO3. These results are explained by the presence of an excess of positive charges in the film, which leads to a positive Donnan potential. We find that this potential is more positive when more chaotropic anions are used during the film buildup. We also find that a film constructed in the presence of chaotropic anions swells and becomes more permeable to Fe(CN)(6)4- ions when the film is brought into contact with a solution containing more cosmotropic anions. All our experimental findings can be explained by a strong interaction between chaotropic anions with the NH3+groups of PAH that is equivalent, as far as the multilayer buildup and electrochemical response is concerned, to a deprotonation of PAH as it is observed when the film is constructed at a higher pH. We thus arrive to a coherent explanation of the effect of the nature of the anions of the supporting electrolyte on the polyelectrolyte multilayer. We also find that great care must be taken when investigating polyelectrolyte multilayer films by electrochemical probing because electrochemical reactions involving the probes can appreciably modify the multilayer structure.journal articleresearch support, non-u.s. gov't2009 Feb 17importe
A Public, K-Selected, Optical-to-Near-Infrared Catalog of the Extended Chandra Deep Field South (ECDFS) from the MUltiwavelength Survey by Yale-Chile (MUSYC)
We present a new K-selected, optical-to-near-infrared photometric catalog of
the Extended Chandra Deep Field South (ECDFS), making it publicly available to
the astronomical community. The dataset is founded on publicly available
imaging, supplemented by original zJK imaging data obtained as part of the
MUltiwavelength Survey by Yale-Chile (MUSYC). The final photometric catalog
consists of photometry derived from nine band U-K imaging covering the full
0.5x0.5 sq. deg. of the ECDFS, plus H band data for approximately 80% of the
field. The 5sigma flux limit for point-sources is K = 22.0 (AB). This is also
the nominal completeness and reliability limit of the catalog: the empirical
completeness for 21.75 < K < 22.00 is 85+%. We have verified the quality of the
catalog through both internal consistency checks, and comparisons to other
existing and publicly available catalogs. As well as the photometric catalog,
we also present catalogs of photometric redshifts and restframe photometry
derived from the ten band photometry. We have collected robust spectroscopic
redshift determinations from published sources for 1966 galaxies in the
catalog. Based on these sources, we have achieved a (1sigma) photometric
redshift accuracy of Dz/(1+z) = 0.036, with an outlier fraction of 7.8%. Most
of these outliers are X-ray sources. Finally, we describe and release a utility
for interpolating restframe photometry from observed SEDs, dubbed InterRest.
Particularly in concert with the wealth of already publicly available data in
the ECDFS, this new MUSYC catalog provides an excellent resource for studying
the changing properties of the massive galaxy population at z < 2. (Abridged)Comment: Re-submitted to ApJSS after a first referee report. 27 pages, 17
figures. MUSYC data is freely available from http://astro.yale.edu/MUSYC .
Links to phot-z and restframe photometry catalogs, as well as to InterRest
access and documentation, including a full walkthrough, can be found at
http://www.strw.leidenuniv.nl/~ent
The near-infrared luminosity function of cluster galaxies beyond redshift one
We determined the K band luminosity function (LF) of cluster galaxies at
redshift z~1.2, using near-infrared images of three X-ray luminous clusters at
z=1.11,1.24,1.27. The composite LF was derived down to M*+4, by means of
statistical background subtraction, and is well described by a Schechter
function with K*=20.5 AB mag and alpha=-1.
From the K band composite LF we derived the stellar mass function of cluster
galaxies. Using available X-ray mass profiles we determined the M/L ratios of
these three clusters, which tend to be lower than those measured in the local
universe.
With these data, no significant difference can be seen between the shapes of
the cluster galaxies LF and the LF of field galaxies at similar redshift.
We also found no significant evolution out to z ~1.2 in the bright (<M*+4)
part of the cluster galaxies LF probed in this study, apart from a brightening
of ~1.3 mag of the characteristic magnitude of the high redshift LF. We
confirm, and extend to higher redshift, the result from previous work that the
redshift evolution of the characteristic magnitude M* is consistent with
passive evolution of a stellar population formed at z>2.
The results obtained in this work support and extend previous findings that
most of the stars in bright galaxies were formed at high redshift, and that
K-bright (M>10^11 Msun) galaxies were already in place at z ~ 1.2, at least in
the central regions of X-ray luminous clusters. Together with recent results on
the field galaxies stellar mass function, this implies that most of the stellar
mass is already assembled in massive galaxies by z ~ 1, both in low and high
density environments.Comment: 16 pages, 10 figures, to appear in A&
The Hubble Space Telescope Wide Field Camera 3 Early Release Science data: Panchromatic Faint Object Counts for 0.2-2 microns wavelength
We describe the Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) Early
Release Science (ERS) observations in the Great Observatories Origins Deep
Survey (GOODS) South field. The new WFC3 ERS data provide calibrated, drizzled
mosaics in the UV filters F225W, F275W, and F336W, as well as in the near-IR
filters F098M (Ys), F125W (J), and F160W (H) with 1-2 HST orbits per filter.
Together with the existing HST Advanced Camera for Surveys (ACS) GOODS-South
mosaics in the BViz filters, these panchromatic 10-band ERS data cover 40-50
square arcmin at 0.2-1.7 {\mu}m in wavelength at 0.07-0.15" FWHM resolution and
0.090" Multidrizzled pixels to depths of AB\simeq 26.0-27.0 mag (5-{\sigma})
for point sources, and AB\simeq 25.5-26.5 mag for compact galaxies.
In this paper, we describe: a) the scientific rationale, and the data taking
plus reduction procedures of the panchromatic 10-band ERS mosaics; b) the
procedure of generating object catalogs across the 10 different ERS filters,
and the specific star-galaxy separation techniques used; and c) the reliability
and completeness of the object catalogs from the WFC3 ERS mosaics. The
excellent 0.07-0.15" FWHM resolution of HST/WFC3 and ACS makes star- galaxy
separation straightforward over a factor of 10 in wavelength to AB\simeq 25-26
mag from the UV to the near-IR, respectively.Comment: 51 pages, 71 figures Accepted to ApJS 2011.01.2
PTP1B Is an Androgen Receptor–Regulated Phosphatase That Promotes the Progression of Prostate Cancer
First spectroscopic observations of the galaxies that reionized the Universe
Low-mass galaxies in the early universe are believed to be the building
blocks of present-day galaxies. These fledgling systems likely played a pivotal
role in cosmic reionization, a major phase transition from neutral Hydrogen to
ionized plasma around 600-800 Myr after the Big Bang. However, these galaxies
have eluded comprehensive spectroscopic studies owing to their extreme
faintness. Here we report the first spectroscopic analysis of 8 ultra-faint
galaxies during the epoch of reionization with absolute magnitudes between
M to mag (down to 0.005 ). The
combination of ultra-deep NIRSpec (Near-Infrared Spectrograph) observations and
the strong gravitational lensing boost of Abell~2744 allow us to derive the
first spectroscopic constraints on the prevalence of faint galaxies and their
ionizing properties during the Universe's first billion years. We find that
faint galaxies are prodigious producers of ionizing photons with log(/ Hz erg) =, a factor of 4 larger than canonical
values. This means that the total rate of ionizing photons produced by galaxies
exceeds that needed for reionization, even for modest values of escape fraction
( =5%). These findings provide robust evidence that faint galaxies
were the main drivers of cosmic reionization at .Comment: 29 pages, 7 figures, 2 table
The 3D-HST Survey: <i>Hubble Space Telescope</i> WFC3/G141 Grism Spectra, Redshifts, and Emission Line Measurements for ~ 100,000 Galaxies
We present reduced data and data products from the 3D-HST survey, a 248-orbit Treasury program. The survey obtained WFC3 G141 grism spectroscopy in four of the five CANDELS fields: AEGIS, COSMOS, GOODS-S, and UDS, along with WFC3 imaging, parallel ACS G800L spectroscopy, and parallel imaging. In a previous paper, we presented photometric catalogs in these four fields and in GOODS-N, the fifth CANDELS field. Here we describe and present the WFC3 G141 spectroscopic data, again augmented with data from GO-1600 in GOODS-N (PI: B. Weiner). We developed software to automatically and optimally extract interlaced two-dimensional (2D) and one-dimensional (1D) spectra for all objects in the Skelton et al. (2014) photometric catalogs. The 2D spectra and the multi-band photometry were fit simultaneously to determine redshifts and emission line strengths, taking the morphology of the galaxies explicitly into account. The resulting catalog has redshifts and line strengths (where available) for 22,548 unique objects down to (79,609 unique objects down to ). Of these, 5459 galaxies are at and 9621 are at , where Hα falls in the G141 wavelength coverage. The typical redshift error for galaxies is , i.e., one native WFC3 pixel. The limit for emission line fluxes of point sources is erg . All 2D and 1D spectra, as well as redshifts, line fluxes, and other derived parameters, are publicly available
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