TeV γ-ray observations of the young synchrotron-dominated SNRs G1.9+0.3 and G330.2+1.0 with H.E.S.S.
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A. Abramowski
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F. Aharonian
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A. G. Akhperjanian
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E. Angüner
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G. Anton
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S. Balenderan
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Agnès Balzer
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A. Barnacka
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Y. Becherini
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J. Becker Tjus
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K. Bernlöhr
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E. Birsin
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E. Bissaldi
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M. Böttcher
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C. Boisson
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P. Bordas
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J. Brucker
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F. Brun
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P. Brun
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T. Bulik
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S. Carrigan
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S. Casanova
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M. Cerruti
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P. M. Chadwick
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R. C. G. Chaves
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A. Cheesebrough
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S. Colafrancesco
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G. Cologna
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J. Conrad
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Y. Cui
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M. K. Daniel
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I. D. Davids
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C. Deil
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P. Dewilt
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H. J. Dickinson
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W. Domainko
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L. O'C. Drury
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G. Dubus
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K. Dutson
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J. Dyks
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M. Dyrda
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T. Edwards
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K. Egberts
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P. Eger
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C. Farnier
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S. Fegan
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M. V. Fernandes
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A. Fiasson
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A. Förster
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M. Füssling
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M. Gajdus
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G. Giavitto
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J. F. Glicenstein
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M. -H. Grondin
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M. Grudzińska
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S. Häffner
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J. Hahn
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J. Harris
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G. Heinzelmann
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G. Henri
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G. Hermann
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A. Hillert
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J. A. Hinton
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W. Hofmann
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P. Hofverberg
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M. Holler
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D. Horns
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C. Jahn
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M. Jamrozy
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M. Janiak
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F. Jankowsky
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I. Jung
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M. A. Kastendieck
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K. Katarzyński
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U. Katz
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S. Kaufmann
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S. Klepser
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D. Klochkov
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W. Kluźniak
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T. Kneiske
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D. Kolitzus
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Nu. Komin
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D. Lennarz
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T. Lohse
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A. Lopatin
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C. -C. Lu
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V. Marandon
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Alexandre Marcowith
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R. Marx
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N. Maxted
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M. Mayer
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P. J. Meintjes
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U. Menzler
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M. Meyer
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R. Moderski
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M. Mohamed
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Emmanuel Moulin
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T. Murach
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I. Oya
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M. Panter
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N. W. Pekeur
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G. Pelletier
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J. Perez
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P. -O. Petrucci
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B. Peyaud
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H. Poon
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G. Pühlhofer
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M. Punch
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A. Quirrenbach
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M. Raue
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A. Reimer
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O. Reimer
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Matthieu Renaud
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R. de Los Reyes
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F. Rieger
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L. Rob
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C. Romoli
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G. Rowell
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V. Sahakian
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A. Santangelo
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R. Schlickeiser
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F. Schüssler
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A. Schulz
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S. Schwarzburg
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S. Schwemmer
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G. Spengler
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F. Spies
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Ł. Stawarz
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R. Steenkamp
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C. Stegmann
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K. Stycz
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B. van Soelen
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George Vasileiadis
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C. Venter
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A. Viana
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H. J. Völk
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F. Volpe
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M. Vorster
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T. Vuillaume
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S. J. Wagner
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P. Wagner
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M. Ward
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M. Weidinger
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Q. Weitzel
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R. White
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A. Wierzcholska
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P. Willmann
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A. Wörnlein
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D. Wouters
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V. Zabalza
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M. Zacharias
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A. Zajczyk
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A. A. Zdziarski
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A. Zech
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H. -S. Zechlin
- Function : Author
Abstract
The non-thermal nature of the X-ray emission from the shell-type supernova remnants (SNRs) G1.9+0.3 and G330.2+1.0 is an indication of intense particle acceleration in the shock fronts of both objects. This suggests that the SNRs are prime candidates for very-high-energy (VHE; E $>$ 0.1 TeV) {\gamma}-ray observations. G1.9+0.3, recently established as the youngest known SNR in the Galaxy, also offers a unique opportunity to study the earliest stages of SNR evolution in the VHE domain. The purpose of this work is to probe the level of VHE {\gamma}-ray emission from both SNRs and use this to constrain their physical properties. Observations were conducted with the H.E.S.S. (High Energy Stereoscopic System) Cherenkov telescope array over a more than six-year period spanning 2004-2010. The obtained data have effective livetimes of 67 h for G1.9+0.3 and 16 h for G330.2+1.0. The data are analyzed in the context of the multi-wavelength observations currently available and in the framework of both leptonic and hadronic particle acceleration scenarios. No significant {\gamma}-ray signal from G1.9+0.3 or G330.2+1.0 was detected. Upper limits (99% confidence level) to the TeV flux from G1.9+0.3 and G330.2+1.0 for the assumed spectral index {\Gamma} = 2.5 were set at 5.6 $\times$ 10$^{-13}$ cm$^{-2}$ s$^{-1}$ above 0.26 TeV and 3.2 $\times$ 10$^{-12}$ cm$^{-2}$ s$^{-1}$ above 0.38 TeV, respectively. In a one-zone leptonic scenario, these upper limits imply lower limits on the interior magnetic field to B$_{\mathrm{G1.9}}$ $\gtrsim$ 11 {\mu}G for G1.9+0.3 and to B$_{\mathrm{G330}}$ $\gtrsim$ 8 {\mu}G for G330.2+1.0. In a hadronic scenario, the low ambient densities and the large distances to the SNRs result in very low predicted fluxes, for which the H.E.S.S. upper limits are not constraining.