Institution
Space Telescope Science Institute
Facility•Baltimore, Maryland, United States•
About: Space Telescope Science Institute is a facility organization based out in Baltimore, Maryland, United States. It is known for research contribution in the topics: Galaxy & Stars. The organization has 2448 authors who have published 14154 publications receiving 947296 citations. The organization is also known as: STScI.
Topics: Galaxy, Stars, Star formation, Redshift, Population
Papers published on a yearly basis
Papers
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TL;DR: In this article, the authors presented new parallax measurements of 7 long-period (> 10 days) Milky Way Cepheids using astrometry from spatial scanning of WFC3 on HST.
Abstract: We present new parallax measurements of 7 long-period (> 10 days) Milky Way Cepheids (SS CMa, XY Car, VY Car, VX Per, WZ Sgr, X Pup and S Vul) using astrometry from spatial scanning of WFC3 on HST. Observations were obtained at 6 month intervals over 4 years. The distances are 1.7--3.6 kpc with a mean precision of 45 microarcseconds and a best of 29 microarcseconds (SNR = 14). The accuracy of the parallaxes is demonstrated through independent analyses of >100 reference stars. This raises to 10 the number of long-period Cepheids with significant parallax measurements, 8 obtained from this program. We also present high-precision F555W, F814W, and F160W magnitudes of these Cepheids, allowing a direct, zeropoint-independent comparison to >1800 extragalactic Cepheids in the hosts of 19 SNeIa. This sample addresses two outstanding systematic uncertainties affecting prior comparisons of Milky Way and extragalactic Cepheids used to calibrate H_0: their dissimilarity of periods and photometric systems. Comparing the new parallaxes to their predicted values derived from reversing the distance ladder gives a ratio (or independent scale for H_0) of 1.037+/-0.036, consistent with no change and inconsistent at the 3.5 sigma level with a ratio of 0.91 needed to match the value predicted by Planck+LCDM. Using these data instead to augment the Riess et al. (2016) measurement of H_0 improves the precision to 2.3%, yielding 73.48+/-1.66 km/s/Mpc, and tension with Planck+LCDM increases to 3.7 sigma. The future combination of Gaia parallaxes and HST spatial scanning photometry of 50 Milky Way Cepheids can support a < 1% calibration of H_0.
342 citations
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Max Planck Society1, University of Maryland, Baltimore County2, University of California, Berkeley3, INAF4, University of Paris5, California Institute of Technology6, Harvard University7, University of Hawaii8, Space Telescope Science Institute9, ETH Zurich10, Institut d'Astrophysique de Paris11, Tohoku University12, Ehime University13, University of Arizona14
TL;DR: In this paper, the discrepancy between estimates of the total baryon mass fraction obtained from observations of the cosmic microwave background (CMB) and of galaxy groups/clusters persists when a large sample of groups is considered.
Abstract: We investigate if the discrepancy between estimates of the total baryon mass fraction obtained from observations of the cosmic microwave background (CMB) and of galaxy groups/clusters persists when a large sample of groups is considered. To this purpose, 91 candidate X-ray groups/poor clusters at redshift 0.1 ≤ z ≤ 1 are selected from the COSMOS 2 deg^2 survey, based only on their X-ray luminosity and extent. This sample is complemented by 27 nearby clusters with a robust, analogous determination of the total and stellar mass inside R_(500). The total sample of 118 groups and clusters with z ≤ 1 spans a range in M_(500) of ~10^(13)-10^(15) M_☉. We find that the stellar mass fraction associated with galaxies at R_(500) decreases with increasing total mass as M^(–0.37 ± 0.04)_(500), independent of redshift. Estimating the total gas mass fraction from a recently derived, high-quality scaling relation, the total baryon mass fraction (f^(stars+gas)_(500) = f^(stars)_(500) + f^(gas)_(500)) is found to increase by ~25%, when M_(500) increases from = 5 × 10^(13) M_☉ to = 7 × 10^(14) M_☉. After consideration of a plausible contribution due to intracluster light (11%-22% of the total stellar mass) and gas depletion through the hierarchical assembly process (10% of the gas mass), the estimated values of the total baryon mass fraction are still lower than the latest CMB measure of the same quantity (WMAP5), at a significance level of 3.3σ for groups of = 5 × 10^(13) M_☉. The discrepancy decreases toward higher total masses, such that it is 1σ at = 7 × 10^(14) M_☉. We discuss this result in terms of nongravitational processes such as feedback and filamentary heating.
341 citations
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Arizona State University1, University of California, Riverside2, Carnegie Institution for Science3, University of California, Davis4, Ohio State University5, Liverpool John Moores University6, University of St Andrews7, Universities Space Research Association8, Space Telescope Science Institute9, University of Virginia10, Goddard Space Flight Center11, Max Planck Society12, University of Washington13, University of Massachusetts Amherst14, University of Oxford15, Cardiff University16, Australian National University17, University of Hawaii at Manoa18, New Mexico State University19, INAF20, California Institute of Technology21, Ames Research Center22
TL;DR: The panchromatic 10-band ERS data from 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 is described in this article.
Abstract: 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 arcmin2 at 0.2-1.7 μm in wavelength at 007-015 FWHM resolution and 0090 Multidrizzled pixels to depths of AB 26.0-27.0 mag (5σ) for point sources, and AB 25.5-26.5 mag for compact galaxies. In this paper, we describe (1) the scientific rationale, and the data taking plus reduction procedures of the panchromatic 10-band ERS mosaics, (2) the procedure of generating object catalogs across the 10 different ERS filters, and the specific star-galaxy separation techniques used, and (3) the reliability and completeness of the object catalogs from the WFC3 ERS mosaics. The excellent 007-015 FWHM resolution of HST/WFC3 and ACS makes star-galaxy separation straightforward over a factor of 10 in wavelength to AB 25-26 mag from the UV to the near-IR, respectively. Our main results are: (1) proper motion of faint ERS stars is detected over 6 years at 3.06 ± 0.66 mas year–1 (4.6σ), consistent with Galactic structure models; (2) both the Galactic star counts and the galaxy counts show mild but significant trends of decreasing count slopes from the mid-UV to the near-IR over a factor of 10 in wavelength; (3) combining the 10-band ERS counts with the panchromatic Galaxy and Mass Assembly survey counts at the bright end (10 mag AB 20 mag) and the Hubble Ultra Deep Field counts in the BVizYsJH filters at the faint end (24 mag AB 30 mag) yields galaxy counts that are well measured over the entire flux range 10 mag AB 30 mag for 0.2-2 μm in wavelength; (4) simple luminosity+density evolution models can fit the galaxy counts over this entire flux range. However, no single model can explain the counts over this entire flux range in all 10 filters simultaneously. More sophisticated models of galaxy assembly are needed to reproduce the overall constraints provided by the current panchromatic galaxy counts for 10 mag AB 30 mag over a factor of 10 in wavelength.
341 citations
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Tel Aviv University1, Spanish National Research Council2, Johns Hopkins University3, Space Telescope Science Institute4, University of California, Santa Cruz5, Goddard Space Flight Center6, Princeton University7, Pontifical Catholic University of Chile8, Leiden University9, Pennsylvania State University10, Istituto di Scienza e Tecnologie dell'Informazione11, University of Arizona12, European Southern Observatory13, W.M. Keck Observatory14
TL;DR: In this article, a flexible light deflection field was constructed to predict the appearance and positions of counterimages of the largest known gravitational lens, A1689, and the model was refined as new counterimages were identified and incorporated to improve the model, yielding a total of 106 images of 30 multiply lensed background galaxies.
Abstract: We analyze deep multicolor Advanced Camera images of the largest known gravitational lens, A1689. Radial and tangential arcs delineate the critical curves in unprecedented detail, and many small counterimages are found near the center of mass. We construct a flexible light deflection field to predict the appearance and positions of counterimages. The model is refined as new counterimages are identified and incorporated to improve the model, yielding a total of 106 images of 30 multiply lensed background galaxies, spanning a wide redshift range, 1.0 < z < 5.5. The resulting mass map is more circular in projection than the clumpy distribution of cluster galaxies, and the light is more concentrated than the mass within r < 50 kpc h-1. The projected mass profile flattens steadily toward the center with a shallow mean slope of d log ?/d log r -0.55 ? 0.1, over the observed range r < 250 kpc h-1, matching well an NFW profile, but with a relatively high concentration, Cvir = 8.2. A softened isothermal profile (rcore = 20 ? 2'') is not conclusively excluded, illustrating that lensing constrains only projected quantities. Regarding cosmology, we clearly detect the purely geometric increase of bend angles with redshift. The dependence on the cosmological parameters is weak owing to the proximity of A1689, z = 0.18, constraining the locus, ?M + ?? ? 1.2. This consistency with standard cosmology provides independent support for our model, because the redshift information is not required to derive an accurate mass map. Similarly, the relative fluxes of the multiple images are reproduced well by our best-fitting lens model.
341 citations
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California Institute of Technology1, University of Arizona2, University of Cambridge3, Dalhousie University4, European Southern Observatory5, McGill University6, Max Planck Society7, University of Pennsylvania8, University of Chicago9, Harvard University10, Jet Propulsion Laboratory11, University of Missouri12, Argonne National Laboratory13, National Radio Astronomy Observatory14, University of California, Davis15, University of California, Berkeley16, University of Florida17, University College London18, University of Colorado Boulder19, Lawrence Berkeley National Laboratory20, University of California, Los Angeles21, Australia Telescope National Facility22, University of Michigan23, Carnegie Institution for Science24, Space Telescope Science Institute25, Case Western Reserve University26, School of the Art Institute of Chicago27, Yale University28, University of Paris-Sud29
TL;DR: A redshift survey at a wavelength of three millimetres, targeting carbon monoxide line emission from the star-forming molecular gas in the direction of extraordinarily bright millimetre-wave-selected sources, indicating that the fraction of dusty starburst galaxies at high redshifts is greater than previously thought.
Abstract: In the past decade, our understanding of galaxy evolution has been revolutionized by the discovery that luminous, dusty starburst galaxies were 1,000 times more abundant in the early Universe than at present. It has, however, been difficult to measure the complete redshift distribution of these objects, especially at the highest redshifts (z > 4). Here we report a redshift survey at a wavelength of three millimetres, targeting carbon monoxide line emission from the star-forming molecular gas in the direction of extraordinarily bright millimetre-wave-selected sources. High-resolution imaging demonstrates that these sources are strongly gravitationally lensed by foreground galaxies. We detect spectral lines in 23 out of 26 sources and multiple lines in 12 of those 23 sources, from which we obtain robust, unambiguous redshifts. At least 10 of the sources are found to lie at z > 4, indicating that the fraction of dusty starburst galaxies at high redshifts is greater than previously thought. Models of lens geometries in the sample indicate that the background objects are ultra-luminous infrared galaxies, powered by extreme bursts of star formation.
340 citations
Authors
Showing all 2468 results
Name | H-index | Papers | Citations |
---|---|---|---|
Donald P. Schneider | 242 | 1622 | 263641 |
David J. Schlegel | 193 | 600 | 193972 |
Timothy M. Heckman | 170 | 754 | 141237 |
Anton M. Koekemoer | 168 | 1127 | 106796 |
Peter Capak | 147 | 679 | 70483 |
William T. Reach | 131 | 535 | 90496 |
P. A. Caraveo | 129 | 688 | 63239 |
Mauro Giavalisco | 128 | 412 | 69967 |
Neta A. Bahcall | 127 | 392 | 93589 |
Tommaso Treu | 126 | 715 | 49090 |
Mark Dickinson | 124 | 389 | 66770 |
Henry C. Ferguson | 121 | 513 | 73032 |
David C. Koo | 119 | 568 | 49040 |
Adam G. Riess | 118 | 363 | 117310 |
Jesper Sollerman | 118 | 726 | 53436 |