Institution
Jet Propulsion Laboratory
Facility•La Cañada Flintridge, California, United States•
About: Jet Propulsion Laboratory is a facility organization based out in La Cañada Flintridge, California, United States. It is known for research contribution in the topics: Mars Exploration Program & Telescope. The organization has 8801 authors who have published 14333 publications receiving 548163 citations. The organization is also known as: JPL & NASA JPL.
Topics: Mars Exploration Program, Telescope, Galaxy, Coronagraph, Planet
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Paris Diderot University1, University College London2, European Space Agency3, University of California, Irvine4, INAF5, University of Edinburgh6, Cardiff University7, Imperial College London8, Max Planck Society9, California Institute of Technology10, Jet Propulsion Laboratory11, University of La Laguna12, Spanish National Research Council13, Aix-Marseille University14, University of British Columbia15, University of Bologna16, University of Colorado Boulder17, Goddard Space Flight Center18, University of Sussex19, University of Padua20, UK Astronomy Technology Centre21, Korea Astronomy and Space Science Institute22, University of Paris-Sud23, Institut d'Astrophysique de Paris24, Seoul National University25, University of Manchester26, Rutherford Appleton Laboratory27, University of Lethbridge28, University of Oxford29, University of Hertfordshire30
TL;DR: In this paper, the spectral energy distribution fit of the far-IR (FIR) flux densities obtained with the PACS and SPIRE instruments onboard Herschel was analyzed for galaxies in the redshift range 0.1 to 0.5.
Abstract: We study the dust properties of galaxies in the redshift range 0.1 less than or similar to z less than or similar to 2.8 observed by the Herschel Space Observatory in the field of the Great Observatories Origins Deep Survey-North as part of the PACS Extragalactic Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) key programmes. Infrared (IR) luminosity (L-IR) and dust temperature (T-dust) of galaxies are derived from the spectral energy distribution fit of the far-IR (FIR) flux densities obtained with the PACS and SPIRE instruments onboard Herschel. As a reference sample, we also obtain IR luminosities and dust temperatures of local galaxies at z \textless 0.1 using AKARI and IRAS data in the field of the Sloan Digital Sky Survey. We compare the L-IR-T-dust relation between the two samples and find that the median T-dust of Herschel-selected galaxies at z greater than or similar to 0.5 with L-IR greater than or similar to 5 x 10(10) L-circle dot appears to be 2-5 K colder than that of AKARI-selected local galaxies with similar luminosities, and the dispersion in T-dust for high-z galaxies increases with L-IR due to the existence of cold galaxies that are not seen among local galaxies. We show that this large dispersion of the L-IR-T-dust relation can bridge the gap between local star-forming galaxies and high-z submillimetre galaxies (SMGs). We also find that three SMGs with very low T-dust (less than or similar to 20 K) covered in this study have close neighbouring sources with similar 24-mu m brightness, which could lead to an overestimation of FIR/(sub) millimetre fluxes of the SMGs.
177 citations
California Institute of Technology1, University of California, San Diego2, Imperial College London3, University of Sussex4, National Radio Astronomy Observatory5, Jet Propulsion Laboratory6, University of Padua7, Spanish National Research Council8, University of Paris-Sud9, Cornell University10, University of Kent11, DSM12, Cardiff University13
TL;DR: In this paper, the authors characterize the Spitzer Wide-area Infrared Extragalactic Legacy Survey (SWIRE) galaxy populations in the SWIRE validation field within the Lockman Hole, based on the 3.6-24 μm Spitzer data and deep U, g', r', i' optical imaging within an area ~1/3 deg2 for ~16,000 Spitzer SWIRE sources.
Abstract: We characterize the Spitzer Wide-area Infrared Extragalactic Legacy Survey (SWIRE) galaxy populations in the SWIRE validation field within the Lockman Hole, based on the 3.6-24 μm Spitzer data and deep U, g', r', i' optical imaging within an area ~1/3 deg2 for ~16,000 Spitzer SWIRE sources. The entire SWIRE survey will discover over 2.3 million galaxies at 3.6 μm and almost 350,000 at 24 μm; ~70,000 of these will be five-band 3.6-24 μm detections. The colors cover a broad range, generally well represented by redshifted spectral energy distributions of known galaxy populations; however, significant samples of unusually blue objects in the [3.6]-[4.5] color are found, as well as many objects very red in the 3.6-24 μm mid-IR. Nine of these are investigated and are interpreted as star-forming systems, starbursts, and active galactic nuclei (AGNs) from z = 0.37 to 2.8, with luminosities from LIR = 1010.3 to 1013.7 L.
177 citations
University of California, Irvine1, UK Astronomy Technology Centre2, Cornell University3, Harvard University4, University of Maryland, College Park5, European Space Agency6, Paris Diderot University7, Rutgers University8, California Institute of Technology9, Jet Propulsion Laboratory10, University of Hawaii11, Complutense University of Madrid12, Dalhousie University13, Imperial College London14, University of Colorado Boulder15, Virginia Tech16, National Radio Astronomy Observatory17, University of Oxford18, University of British Columbia19, University of La Laguna20, Spanish National Research Council21, INAF22, University of Sussex23, Institut d'Astrophysique de Paris24, University College London25, University of the Western Cape26
TL;DR: It is concluded that gas-rich major galaxy mergers with intense star formation can form the most massive elliptical galaxies by z ≈ 1.5.
Abstract: Stellar archaeology shows that massive elliptical galaxies formed rapidly about ten billion years ago with star-formation rates of above several hundred solar masses per year. Their progenitors are probably the submillimetre bright galaxies at redshifts z greater than 2. Although the mean molecular gas mass (5 × 10(10) solar masses) of the submillimetre bright galaxies can explain the formation of typical elliptical galaxies, it is inadequate to form elliptical galaxies that already have stellar masses above 2 × 10(11) solar masses at z ≈ 2. Here we report multi-wavelength high-resolution observations of a rare merger of two massive submillimetre bright galaxies at z = 2.3. The system is seen to be forming stars at a rate of 2,000 solar masses per year. The star-formation efficiency is an order of magnitude greater than that of normal galaxies, so the gas reservoir will be exhausted and star formation will be quenched in only around 200 million years. At a projected separation of 19 kiloparsecs, the two massive starbursts are about to merge and form a passive elliptical galaxy with a stellar mass of about 4 × 10(11) solar masses. We conclude that gas-rich major galaxy mergers with intense star formation can form the most massive elliptical galaxies by z ≈ 1.5.
176 citations
University of California, Berkeley1, United States Naval Research Laboratory2, Lawrence Berkeley National Laboratory3, Goethe University Frankfurt4, State University of New York at Plattsburgh5, Jacobs Engineering Group6, Heidelberg University7, Carnegie Institution for Science8, Field Museum of Natural History9, University of Leicester10, University of Washington11, University of Kent12, Ghent University13, University of New Mexico14, European Synchrotron Radiation Facility15, University of Chicago16, Washington University in St. Louis17, Max Planck Society18, International Space Science Institute19, Natural History Museum20, Argonne National Laboratory21, École normale supérieure de Lyon22, university of lille23, Ames Research Center24, University of Stuttgart25, Jet Propulsion Laboratory26
TL;DR: The Stardust Interstellar Dust Collector captured seven particles and returned to Earth for laboratory analysis have features consistent with an origin in the contemporary interstellar dust stream and more than 50 spacecraft debris particles were also identified as discussed by the authors.
Abstract: Seven particles captured by the Stardust Interstellar Dust Collector and returned to Earth for laboratory analysis have features consistent with an origin in the contemporary interstellar dust stream. More than 50 spacecraft debris particles were also identified. The interstellar dust candidates are readily distinguished from debris impacts on the basis of elemental composition and/or impact trajectory. The seven candidate interstellar particles are diverse in elemental composition, crystal structure, and size. The presence of crystalline grains and multiple iron-bearing phases, including sulfide, in some particles indicates that individual interstellar particles diverge from any one representative model of interstellar dust inferred from astronomical observations and theory.
176 citations
03 Mar 2009
TL;DR: In this paper, an introduction to the near-Earth laser communication technology is presented, which includes the atmospheric effects, laser transmitter, receiver, optomechanical assembly, laser beam acquisition tracking and pointing, modulation and coding.
Abstract: This chapter is an introduction to the near-Earth laser communication technology. By near-Earth, we mean high-altitude platforms and Earth-orbiting satellites. Justification for high bandwidth delivery capability as well as key advantages and challenges of laser communications are discussed in detail. Critical elements of each subassembly are introduced and elaborated separately for the flight and the ground subsystems. These include the atmospheric effects, laser transmitter, receiver, optomechanical assembly, laser beam acquisition tracking and pointing, modulation and coding. Past successful optical communications links and upcoming field demonstrations and major operational use cases are also summarized here. Each of the following chapters expands on these topics in much greater detail.
176 citations
Authors
Showing all 9033 results
| Name | H-index | Papers | Citations |
|---|---|---|---|
| B. P. Crill | 148 | 486 | 111895 |
| George Helou | 144 | 662 | 96338 |
| H. K. Eriksen | 141 | 474 | 104208 |
| Charles R. Lawrence | 141 | 528 | 104948 |
| W. C. Jones | 140 | 395 | 97629 |
| Gianluca Morgante | 138 | 478 | 98223 |
| Jean-Paul Kneib | 138 | 805 | 89287 |
| Kevin M. Huffenberger | 138 | 402 | 93452 |
| Robert H. Brown | 136 | 1174 | 79247 |
| Federico Capasso | 134 | 1189 | 76957 |
| Krzysztof M. Gorski | 132 | 380 | 105912 |
| Olivier Doré | 130 | 427 | 104737 |
| Mark E. Thompson | 128 | 527 | 77399 |
| Clive Dickinson | 123 | 501 | 80701 |
| Daniel Stern | 121 | 788 | 69283 |