Surveys with the Cherenkov Telescope Array

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dc.contributor.authorDubus, G.
dc.contributor.authorContreras, J.L.
dc.contributor.authorFunk, S.
dc.contributor.authorGallant, Y.
dc.contributor.authorHassan, T.
dc.contributor.authorHinton, J.
dc.contributor.authorInoue, Y.
dc.contributor.authorKnödlseder, J.
dc.contributor.authorMartin, P.
dc.contributor.authorMirabal, N.
dc.contributor.authorNaurois, M. de
dc.contributor.authorRenaud, M.
dc.contributor.authorthe CTA Consortium
dc.date.accessioned2020-09-02T17:54:34Z
dc.date.available2020-09-02T17:54:34Z
dc.date.issued2012-06-02
dc.description.abstractSurveys open up unbiased discovery space and generate legacy datasets of long-lasting value. One of the goals of imaging arrays of Cherenkov telescopes like CTA is to survey areas of the sky for faint very high energy gamma-ray (VHE) sources, especially sources that would not have drawn attention were it not for their VHE emission (e.g. the Galactic “dark accelerators”). More than half the currently known VHE sources are to be found in the Galactic Plane. Using standard techniques, CTA can carry out a survey of the region |l|<= 60°, |b| <= 2° in 250 h (1/4th the available time per year at one location) down to a uniform sensitivity of 3 mCrab (a “Galactic Plane survey”). CTA could also survey 1/4th of the sky down to a sensitivity of 20 mCrab in 370 h of observing time (an “all-sky survey”), which complements well the surveys by the Fermi/LAT at lower energies and extended air shower arrays at higher energies. Observations in (non-standard) divergent pointing mode may shorten the “all-sky survey” time to about 100 h with no loss in survey sensitivity. We present the scientific rationale for these surveys, their place in the multi-wavelength context, their possible impact and their feasibility. We find that the Galactic Plane survey has the potential to detect hundreds of sources. Implementing such a survey should be a major goal of CTA. Additionally, about a dozen blazars, or counterparts to Fermi/LAT sources, are expected to be detected by the all-sky survey, whose prime motivation is the search for extragalactic “dark accelerators”.en_US
dc.description.sponsorshipGD thanks D. Horan & S. Wakely for help with TeVCat (Fig. 1). GD and PM acknowledge support from the European Community via contract ERC-StG-200911. NM, TH and JLC acknowledge the support of the Spanish MICINN under project code FPA2010-22056-C06-06. NM gratefully acknowledges support from the Spanish MICINN through a Ramón y Cajal fellowship. The research leading to these results has received funding from the European Union’s Seventh Framework Programme ([FP7/2007-2013] [FP7/2007-2011]) under grant agreement No. 262053. We also gratefully acknowledge support from the following agencies and organisations: Ministerio de Ciencia, Tecnología e Innovación Productiva (MinCyT), Comisión Nacional de Energía Atómica (CNEA) and Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET) Argentina; State Committee of Science of Armenia; Ministry for Research, CNRS-INSU and CNRS-IN2P3, Irfu-CEA, ANR, France; Max Planck Society, BMBF, DESY, Helmholtz Association, Germany; MIUR, Italy; Netherlands Research School for Astronomy (NOVA), Netherlands Organization for Scientific Research (NWO); Ministry of Science and Higher Education and the National Centre for Research and Development, Poland; MICINN support through the National R+D+I, CDTI funding plans and the CPAN and MultiDark Consolider-Ingenio 2010 programme, Spain; Swedish Research Council, Royal Swedish Academy of Sciences financed, Sweden; Swiss National Science Foundation (SNSF), Switzerland; Leverhulme Trust, Royal Society, Science and Technologies Facilities Council, Durham University, UK; National Science Foundation, Department of Energy, Argonne National Laboratory, University of California, University of Chicago, Iowa State University, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI program), Washington University McDonnell Center for the Space Sciences, USA.en_US
dc.description.urihttps://www.sciencedirect.com/science/article/pii/S0927650512001259en_US
dc.format.extent14 pagesen_US
dc.genrejournal articlesen_US
dc.identifierdoi:10.13016/m2ilx0-3fpw
dc.identifier.citationG.Dubus et al., Surveys with the Cherenkov Telescope Array, Astroparticle Physics Volume 43, Pages 317-330 (2013), doi : https://doi.org/10.1016/j.astropartphys.2012.05.020en_US
dc.identifier.urihttps://doi.org/10.1016/j.astropartphys.2012.05.020
dc.identifier.urihttp://hdl.handle.net/11603/19573
dc.language.isoen_USen_US
dc.publisherElsevieren_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Physics Department Collection
dc.relation.ispartofUMBC Joint Center for Earth Systems Technology (JCET)
dc.relation.ispartofUMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.rightsAttribution 3.0 Unported*
dc.rights.urihttps://creativecommons.org/licenses/by/3.0/*
dc.titleSurveys with the Cherenkov Telescope Arrayen_US
dc.typeTexten_US

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