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5 results on '"HFLS3"'

1. Dusty Galaxies at the Highest Redshifts

Author

Clements, David L, Greenslade, Josh, Riechers, Dominik A., Wardlow, Julie, Perez-Fournon, Ismael, Collective, The HerMES Red, HerMES, The, and Consortia, H-ATLAS

Subjects
Physics, Spire, Space and Planetary Science, HFLS3, astro-ph.GA, Astrophysics of Galaxies (astro-ph.GA), Galaxy formation and evolution, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift
Abstract

We show that the use of red colour as the basis for selecting candidate high redshift dusty galaxies from surveys made with Herschel has proved highly successful. The highest redshift such object, HFLS3, lies at z=6.34 and numerous other sources have been found. Spectroscopic followup confirms that most of these lie at z>4. These sources are found in such numbers that they represent a challenge to current models of galaxy evolution. We also examine the prospects for finding dusty galaxies at still higher redshifts. These would not appear in the SPIRE surveys from Herschel but would be detected in longer wavelength, submm, surveys. Several such `SPIRE-dropouts' have been found and are now subject to followup observations., 4 pages, 2 figures. Accepted for publication in Proceedings of IAU Symposium 319 - Galaxies at High Redshift and Their Evolution over Cosmic Time

Published
2015

2. ENVIRONMENT OF THE SUBMILLIMETER-BRIGHT MASSIVE STARBURST HFLS3 AT z similar to 6.34

Author

W. A. Osage, Alex Conley, Asantha Cooray, S. J. Oliver, D. L. Clements, Duncan Farrah, R. Gavazzi, Dominik Riechers, Denis Burgarella, J. J. Bock, J. A. Calanog, Brian Ma, C. Bridge, Hai Fu, C. M. Casey, Georgios E. Magdis, Rob Ivison, R. Marques-Chaves, B. Lo Faro, P. Martínez-Navajas, D. Rigopoulou, Douglas Scott, I. Perez-Fournon, Helmut Dannerbauer, A. Cabrera-Lavers, E. A. Gonzalez-Solares, Julie Wardlow, R. S. Bussmann, Nicolas Laporte, J. D. Vieira, Alina Streblyanska, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), AUTRES, California Institute of Technology (CALTECH), Office national des forêts (ONF), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), IOA, University of Hawai‘i [Mānoa] (UHM), University of Colorado [Boulder], Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Physics [Blacksburg], Virginia Tech [Blacksburg], Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Sussex, Department of Astronomy [Ithaca], Cornell University [New York], Department of Astronomy [Pasadena], Department of Physics [Oxford], University of Oxford, Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Office National des Forêts (ONF), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), University of Oxford [Oxford], Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Cornell University, Department of Physics, Science and Technology Facilities Council (STFC), and Science and Technology Facilities Council [2006-2012]

Subjects
Gran Telescopio Canarias, 0306 Physical Chemistry (Incl. Structural), FOS: Physical sciences, galaxies: starburst, Astrophysics, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, 0305 Organic Chemistry, HIGH-REDSHIFT GALAXIES, Luminosity, HFLS3, galaxies: high-redshift, 0103 physical sciences, STAR-FORMING GALAXIES, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics, Photometric redshift, Luminosity function (astronomy), Physics, Science & Technology, 010308 nuclear & particles physics, UV LUMINOSITY FUNCTIONS, DARK-MATTER MODEL, HUBBLE DEEP FIELD, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, 0201 Astronomical And Space Sciences, LYMAN-BREAK GALAXIES, Space and Planetary Science, ALL-SKY SURVEY, Astrophysics of Galaxies (astro-ph.GA), Physical Sciences, galaxies: luminosity function, mass function, Spectral energy distribution, DWARF/L-DWARF BINARIES, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We describe the search for Lyman-break galaxies (LBGs) near the sub-millimeter bright starburst galaxy HFLS3 at $z$$=$6.34 and a study on the environment of this massive galaxy during the end of reionization.We performed two independent selections of LBGs on images obtained with the \textit{Gran Telescopio Canarias} (GTC) and the \textit{Hubble Space Telescope} (HST) by combining non-detections in bands blueward of the Lyman-break and color selection. A total of 10 objects fulfilling the LBG selection criteria at $z$$>$5.5 were selected over the 4.54 and 55.5 arcmin$^2$ covered by our HST and GTC images, respectively. The photometric redshift, UV luminosity, and the star-formation rate of these sources were estimated with models of their spectral energy distribution. These $z$$\sim$6 candidates have physical properties and number densities in agreement with previous results. The UV luminosity function at $z$$\sim$6 and a Voronoi tessellation analysis of this field shows no strong evidence for an overdensity of relatively bright objects (m$_{F105W}$$, Comment: 14 pages, 12 figures, accepted for publication in ApJ

Published
2015

3. Dust production 680-850 million years after the Big Bang

Author

Michał J. Michałowski

Subjects
Physics, media_common.quotation_subject, Extinction (astronomy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Universe, Galaxy, Interstellar medium, Supernova, Space and Planetary Science, HFLS3, Astrophysics of Galaxies (astro-ph.GA), Asymptotic giant branch, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Large Magellanic Cloud, Astrophysics::Galaxy Astrophysics, media_common
Abstract

Dust plays an important role in our understanding of the Universe, but it is not obvious yet how the dust in the distant universe was formed. I derived the dust yields per asymptotic giant branch (AGB) star and per supernova (SN) required to explain dust masses of galaxies at z=6.3-7.5 (680-850 million years after the Big Bang) for which dust emission has been detected (HFLS3 at z=6.34, ULAS J1120+0641 at z=7.085, and A1689-zD1 at z=7.5), or unsuccessfully searched for. I found very high required yields, implying that AGB stars could not contribute substantially to dust production at these redshifts, and that SNe could explain these dust masses, but only if they do not destroy most of the dust they form (which is unlikely given the upper limits on the SN dust yields derived for galaxies where dust is not detected). This suggests that the grain growth in the interstellar medium is likely required at these early epochs., Comment: Accepted to A&A. 6 pages, 1 figure, 2 tables. V2: minor changes to match the published version

Published
2015
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4. Imaging the environment of a z= 6.3 submillimeter galaxy with SCUBA-2

Author

A. M. Swinbank, Dominik A. Riechers, Dan Bintley, Tim Jenness, Rob Ivison, James Dunlop, Peter A. R. Ade, Douglas Scott, Andy Gibb, James J. Bock, Wayne S. Holland, M. Fich, E. Chapin, Nicolas Laporte, Ian Smail, Seb Oliver, Duncan Farrah, David L. Clements, Ismael Perez-Fournon, Alain Omont, A. Cooray, James E. Geach, Scott Chapman, A. Conley, E. I. Robson, Hai Fu, and Julie Wardlow

Subjects
Structure formation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Extrapolation, FOS: Physical sciences, Astrophysics, galaxies [Radio continuum], 01 natural sciences, high-redshift [Galaxies], QB0460, galaxies [Infrared], HFLS3, 0103 physical sciences, medicine, 010303 astronomy & astrophysics, media_common, Confusion, Physics, galaxies. [Submillimeter], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Universe, Redshift, starburst [Galaxies], Gravitational lens, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), medicine.symptom, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe a search for submillimeter emission in the vicinity of one of the most distant, luminous galaxies known, HerMES FLS3 at z=6.34, exploiting it as a signpost to a potentially biased region of the early Universe, as might be expected in hierarchical structure formation models. Imaging to the confusion limit with the innovative, wide-field submillimeter bolometer camera, SCUBA-2, we are sensitive to colder and/or less luminous galaxies in the surroundings of HFLS3. We use the Millennium Simulation to illustrate that HFLS3 may be expected to have companions if it is as massive as claimed, but find no significant evidence from the surface density of SCUBA-2 galaxies in its vicinity, or their colors, that HFLS3 marks an over-density of dusty, star-forming galaxies. We cannot rule out the presence of dusty neighbours with confidence, but deeper 450-um imaging has the potential to more tightly constrain the redshifts of nearby galaxies, at least one of which likely lies at z>~5. If associations with HFLS3 can be ruled out, this could be taken as evidence that HFLS3 is less biased than a simple extrapolation of the Millennium Simulation may imply. This could suggest either that it represents a rare short-lived, but highly luminous, phase in the evolution of an otherwise typical galaxy, or that this system has suffered amplification due to a foreground gravitational lens and so is not as intrinsically luminous as claimed., 6 pages; 4 colour figures

Published
2014

5. HerMES: THE REST-FRAME UV EMISSION AND A LENSING MODEL FOR THE z=6.34 LUMINOUS DUSTY STARBURST GALAXY HFLS3

Author

D. Rigopoulou, D. L. Clements, Dominik Riechers, B. Lofaro, Darach Watson, Julie Wardlow, Caitlin M. Casey, C. Bridge, R. S. Bussmann, Rob Ivison, Duncan Farrah, J. J. Bock, W. A. Osage, Seb Oliver, Nicolas Laporte, Douglas Scott, R. Gavazzi, Marco Viero, Asantha Cooray, Georgios E. Magdis, I. Perez-Fournon, Brian Ma, Jae Calanog, Denis Burgarella, Alex Conley, Hai Fu, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rest frame, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Wavelength, Gravitational lens, 13. Climate action, Space and Planetary Science, HFLS3, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, Astrophysics::Galaxy Astrophysics, Photometric redshift, QB
Abstract

We discuss the restframe UV emission from the starbursting galaxy HFLS3 at z=6.34, discovered in Herschel/SPIRE data due to its red color in the submm wavelengths from 250-500 um. The apparent inst. SFR of HFLS3 inferred from the total FIR luminosity measured with over 15 photometric data points between 100 to 1000 um is 2900 Msun/yr. Keck/NIRC2 Ks band adaptive optics imaging data showed two potential NIR counterparts near HFLS3. Previously, the northern galaxy was taken to be in the foreground at z=2.1 while the southern galaxy was assumed to HFLS3's NIR counterpart. New HST/WFC3 and ACS imaging data show both optically bright galaxies are in the foreground at z, Submitted to ApJ, 10 pages, 6 figures

Published
2014

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