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A photometric redshift of z ∼ 9.4 for GRB 090429B

Cucchiara, A; Levan, A. J.; Fox, Derek B; Tanvir, Nial R; Ukwatta, T. N.; Berger, E; Kruhler, T; Kupcu Yoldas, A; Wu, X. Y.; Toma, K; Greiner, J; Schmidt, Brian; Dopita, Michael; Wolf, Christian; Sakamoto, T; Roth, K C; Fruchter, A S

Description

Gamma-ray bursts (GRBs) serve as powerful probes of the early universe, with their luminous afterglows revealing the locations and physical properties of star-forming galaxies at the highest redshifts, and potentially locating first-generation (Population III) stars. Since GRB afterglows have intrinsically very simple spectra, they allow robust redshifts from low signal-to-noise spectroscopy, or photometry. Here we present a photometric redshift of z ∼9.4 for the Swift detected GRB090429B based...[Show more]

dc.contributor.authorCucchiara, A
dc.contributor.authorLevan, A. J.
dc.contributor.authorFox, Derek B
dc.contributor.authorTanvir, Nial R
dc.contributor.authorUkwatta, T. N.
dc.contributor.authorBerger, E
dc.contributor.authorKruhler, T
dc.contributor.authorKupcu Yoldas, A
dc.contributor.authorWu, X. Y.
dc.contributor.authorToma, K
dc.contributor.authorGreiner, J
dc.contributor.authorSchmidt, Brian
dc.contributor.authorDopita, Michael
dc.contributor.authorWolf, Christian
dc.contributor.authorSakamoto, T
dc.contributor.authorRoth, K C
dc.contributor.authorFruchter, A S
dc.date.accessioned2015-12-13T22:15:39Z
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1885/70497
dc.description.abstractGamma-ray bursts (GRBs) serve as powerful probes of the early universe, with their luminous afterglows revealing the locations and physical properties of star-forming galaxies at the highest redshifts, and potentially locating first-generation (Population III) stars. Since GRB afterglows have intrinsically very simple spectra, they allow robust redshifts from low signal-to-noise spectroscopy, or photometry. Here we present a photometric redshift of z ∼9.4 for the Swift detected GRB090429B based on deep observations with Gemini-North, the Very Large Telescope, and the GRB Optical and Near-infrared Detector. Assuming a Small Magellanic Cloud dust law (which has been found in a majority of GRB sight lines), the 90% likelihood range for the redshift is 9.06 < z < 9.52, although there is a low-probability tail toward somewhat lower redshifts. Adopting Milky Way or Large Magellanic Cloud dust laws leads to very similar conclusions, while a Maiolino law does allow somewhat lower redshift solutions, though in all cases the most likely redshift is found to be z > 7. The non-detection of the host galaxy to deep limits (Y(AB) ∼28, which would correspond roughly to 0.001L* at z = 1) in our late-time optical and infrared observations with the Hubble Space Telescope strongly supports the extreme-redshift origin of GRB090429B, since we would expect to have detected any low-z galaxy, even if it were highly dusty. Finally, the energetics of GRB 090429B are comparable to those of other GRBs and suggest that its progenitor is not greatly different from those of lower redshift bursts.
dc.description.sponsorshipPart of the funding for GROND (both hardware as well as personnel) was generously granted by the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). T.K. acknowledges support by the DFG cluster of excellence “Origin and Structure of the Universe.” A.R. acknowledges funding from the Science and Technology Funding Council. The Dark Cosmology Centre is funded by the Danish National Research Foundation. F.O.E. acknowledges funding of his Ph.D. through the Deutscher Akademischer Austausch-Dienst (DAAD).
dc.format12 pages
dc.publisherIOP Publishing
dc.rights© 2011. The American Astronomical Society. Author/s retain copyright.
dc.sourceAstrophysical Journal, The
dc.subjectKeywords: early universe; galaxies: high-redshift; gamma-ray burst: individual (GRB 090429R); techniques: photometric
dc.titleA photometric redshift of z ∼ 9.4 for GRB 090429B
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume736
dc.date.issued2011
local.identifier.absfor020106 - High Energy Astrophysics; Cosmic Rays
local.identifier.ariespublicationf2965xPUB2330
local.identifier.ariespublicationu4630950xPUB144
local.type.statusPublished Version
local.contributor.affiliationCucchiara, A, Pennsylvania State University
local.contributor.affiliationLevan, A. J., University of Warwick
local.contributor.affiliationFox, Derek B, Pennsylvania State University
local.contributor.affiliationTanvir, Nial R, University of Leicester
local.contributor.affiliationUkwatta, T. N. , The George Washington University
local.contributor.affiliationBerger, E, Harvard-Smithsonian Center for Astrophysics
local.contributor.affiliationKruhler, T, Max Planck Institut for Extraterrestrial Physics
local.contributor.affiliationKupcu Yoldas, A, European Southern Observatory
local.contributor.affiliationWu, X. Y., Pennsylvania State University
local.contributor.affiliationToma, K, Pennsylvania State University
local.contributor.affiliationGreiner, J, Max Planck Institut for Extraterrestrial Physics
local.contributor.affiliationSchmidt, Brian, College of Physical and Mathematical Sciences, The Australian National University
local.contributor.affiliationDopita, Michael, College of Physical and Mathematical Sciences, The Australian National University
local.contributor.affiliationWolf, Christian, University of Oxford
local.contributor.affiliationSakamoto, T, NASA Goddard Space Flight Center
local.contributor.affiliationRoth, K C, Gemini Observatory
local.contributor.affiliationFruchter, A S, Space Telescope Science Institute
local.identifier.essn1538-4357
local.bibliographicCitation.issue1
local.bibliographicCitation.startpage12
local.identifier.doi10.1088/0004-637X/736/1/7
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciences
dc.date.updated2016-02-24T08:25:10Z
local.identifier.scopusID2-s2.0-80051505229
local.identifier.thomsonID000292645600007
dcterms.accessRightsOpen Access
dc.provenancehttp://www.sherpa.ac.uk/romeo/issn/0004-637X/ Author can archive publisher's version/PDF. Publisher's version/PDF may be used on any website or authors' institutional repository (Sherpa/Romeo as of 18/9/2018)
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