First detection of VHE γ-rays from SN 1006 by HESS

Acero F, Aharonian F, Akhperjanian AG, Anton G, De Almeida UB, Bazer-Bachi AR, Becherini Y, Behera B, Beilicke M, Bernloehr K, Bochow A, Boisson C, Bolmont J, Borrel V, Brucker J, Brun F, Brun P, Buehler R, Bulik T, Buesching I, Boutelier T, Chadwick PM, Charbonnier A, Chaves RCG, Cheesebrough A, Conrad J, Chounet LM, Clapson AC, Coignet G, Dalton M, Daniel MK, Davids ID, Degrange B, Deil C, Dickinson HJ, Djannati-Atai A, Domainko W, Drury LO, Dubois F, Dubus G, Dyks J, Dyrda M, Egberts K, Eger P, Espigat P, Fallon L, Farnier C, Fegan S, Feinstein F, Fiasson A, Foerster A, Fontaine G, Fuessling M, Gabici S, Gallant YA, Gerard L, Gerbig D, Giebels B, Glicenstein JF, Glueck B, Goret P, Göring D, Hauser D, Hauser M, Heinz S, Heinzelmann G, Henri G, Hermann G, Hinton JA, Hoffmann A, Hofmann W, Hofverberg P, Holleran M, Hoppe S, Horns D, Jacholkowska A, De Jager OC, Jahn C, Jung I, Katarzynski K, Katz U, Kaufmann S, Kerschhaggl M, Khangulyan D, Khelifi B, Keogh D, Klochkov D, Kluzniak W, Kneiske TM, Komin N, Kosack K, Kossakowski R, Lamanna G, Lemoine-Goumard M, Lenain JP, Lohse T, Marandon V, Marcowith A, Masbou J, Maurin D, Mccomb TJL, Medina MC, Mehault J, Moderski R, Moulin E, Naumann-Godo M, De Naurois M, Nedbal D, Nekrassov D, Nicholas B, Niemiec J, Nolan SJ, Ohm S, Olive JF, Wilhelmi EDO, Orford KJ, Ostrowski M, Panter M, Arribas MP, Pedaletti G, Pelletier G, Petrucci PO, Pita S, Puehlhofer G, Punch M, Quirrenbach A, Raubenheimer BC, Raue M, Rayner SM, Reimer O, Renaud M, De Los Reyes R, Rieger F, Ripken J, Rob L, Rosier-Lees S, Rowell G, Rudak B, Rulten CB, Ruppel J, Ryde F, Sahakian V, Santangelo A, Schlickeiser R, Schoeck FM, Schoenwald A, Schwanke U, Schwarzburg S, Schwemmer S, Shalchi A, Sushch I, Sikora M, Skilton JL, Sol H, Stawarz L, Steenkamp R, Stegmann C, Stinzing F, Superina G, Szostek A, Tam PH, Tavernet JP, Terrier R, Tibolla O, Tluczykont M, van Eldik C, Vasileiadis G, Venter C, Venter L, Vialle JP, Vincent P, Vink J, Vivier M, Voelk HJ, Volpe F, Vorobiov S, Wagner SJ, Ward M, Zdziarski AA, Zech A (2010)

Publication Status: Published

Publication Type: Journal article, Original article

Publication year: 2010

Journal

Publisher: EDP Sciences

Book Volume: 516

Article Number: aa13916-09

Journal Issue: 6

DOI: 10.1051/0004-6361/200913916

Abstract

Aims. Recent theoretical predictions of the lowest very high energy (VHE) luminosity of SN 1006 are only a factor 5 below the previously published HESS upper limit, thus motivating further in-depth observations of this source. Methods. Deep observations at VHE energies (above 100 GeV) were carried out with the high energy stereoscopic system (HESS) of Cherenkov Telescopes from 2003 to 2008. More than 100 h of data have been collected and subjected to an improved analysis procedure. Results. Observations resulted in the detection of VHE γ-rays from SN 1006. The measured γ-ray spectrum is compatible with a power-law, the flux is of the order of 1% of that detected from the Crab Nebula, and is thus consistent with the previously established HESS upper limit. The source exhibits a bipolar morphology, which is strongly correlated with non-thermal X-rays. Conclusions. Because the thickness of the VHE-shell is compatible with emission from a thin rim, particle acceleration in shock waves is likely to be the origin of the γ-ray signal. The measured flux level can be accounted for by inverse Compton emission, but a mixed scenario that includes leptonic and hadronic components and takes into account the ambient matter density inferred from observations also leads to a satisfactory description of the multi-wavelength spectrum. © 2010 ESO.

Authors with CRIS profile

Involved external institutions

Humboldt-Universität zu Berlin Germany (DE) École Polytechnique - Université Paris-Saclay France (FR) Max-Planck-Institut für Kernphysik (MPIK) / Max Planck Institute for Nuclear Physics Germany (DE) Durham University United Kingdom (GB) University of Paris 7 - Denis Diderot / Université Paris VII Denis Diderot France (FR) Universität Hamburg (UHH) Germany (DE) Leopold-Franzens-Universität Innsbruck / University of Innsbruck Austria (AT) Jagiellonian University / Uniwersytet Jagielloński (UJ) Poland (PL) University of Savoy Mont Blanc / Université Savoie Mont Blanc France (FR) Noordwes-Universiteit / North-West University South Africa (ZA) Nicolaus Copernicus University (NCU) / Uniwersytet Mikołaja Kopernika w Toruniu (UMK) Poland (PL) Institute of Nuclear Physics PAN / Instytut Fizyki Jądrowej im. Henryka Niewodniczańskiego PAN Poland (PL) Eberhard Karls Universität Tübingen Germany (DE) Ruprecht-Karls-Universität Heidelberg Germany (DE) Universiteit Utrecht (UU) / Utrecht University Netherlands (NL) University of Montpellier / Université Montpellier France (FR) Université Toulouse III - Paul Sabatier France (FR) Ruhr-Universität Bochum (RUB) Germany (DE) Dublin Institute for Advanced Studies (DIAS) Ireland (IE) Nicolaus Copernicus Astronomical Centre of the Polish Academy of Sciences Poland (PL) University of Paris 6 - Pierre et Marie Curie / Université Paris VI Pierre et Marie Curie (UPMC) France (FR) Université Joseph Fourier (UJF Grenoble 1) France (FR) Stockholm University / Stockholms universitet Sweden (SE) University of Leeds United Kingdom (GB) University of Adelaide Australia (AU) University of Namibia (UNAM) Namibia (NA) Univerzita Karlova v Praze / Charles University in Prague Czech Republic (CZ) Université Bordeaux 1, Sciences et Technologies France (FR) University of Warsaw / Uniwersytet Warszawski Poland (PL) Yerevan Physics Institute (YerPhI) / Երևանի Ֆիզիկայի Ինստիտուտ Armenia (AM) Royal Institute of Technology / Kungliga Tekniska Högskolan (KTH) Sweden (SE)

How to cite

APA:

Acero, F., Aharonian, F., Akhperjanian, A.G., Anton, G., De Almeida, U.B., Bazer-Bachi, A.R.,... Zech, A. (2010). First detection of VHE γ-rays from SN 1006 by HESS. Astronomy & Astrophysics, 516(6). https://dx.doi.org/10.1051/0004-6361/200913916

MLA:

Acero, F., et al. "First detection of VHE γ-rays from SN 1006 by HESS." Astronomy & Astrophysics 516.6 (2010).

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