Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.

A. Abramowski, F. Acero, F. Aharonian, A. G. Akhperjanian, G. Anton, A. Barnacka, U. Barres De Almeida, A. R. Bazer-Bachi, Y. Becherini, J. Becker, B. Behera, K. Bernlohr, A. Bochow, C. Boisson, J. Bolmont, P. Bordas, V. Borre, J. Brucker, F. Brun, P. BrunT. Bulik, I. Busching, S. Carrigan, S. Casanova, M. Cerruti, P. M. Chadwick, A. Charbonnier, R. C G Chaves, A. Cheesebrough, J. Conrad, L. M. Chounet, A. C. Clapson, G. Coignet, M. Dalton, M. K. Danie, I. D. Davids, B. Degrange, C. Deil, H. J. Dickinson, A. Djannati-Atai, W. Domainko, L. O C Drury, F. Dubois, G. Dubus, J. Dyks, M. Dyrda, K. Egberts, P. Eger, P. Espigat, L. Fallon, C. Farnier, S. Fegan, F. Feinstein, M. V. Fernandes, A. Fiasson, A. Forster, G. Fontaine, M. Fusling, S. Gabici, Y. A. Gallant, H. Gast, L. Gerard, D. Gerbig, B. Giebels, J. F. Glicenstein, B. Gluck, P. Goret, D. Goring, J. D. Hague, D. Hampf, M. Hauser, S. Heinz, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, A. Hoffmann, W. Hofmann, P. Hofverberg, M. Holleran, S. Hoppe, D. Horns, A. Jacholkowska, O. C. De Jager, C. Jahn, M. Jamrozy, I. Jung, M. A. Kastendieck, K. Katarzyński, U. Katz, S. Kaufmann, M. Kerschhagg, D. Khangulyan, B. Khelifi, D. Keogh, W. Kluźzniak, T. Kneiske, Nu Komin, K. Kosack, R. Kossakowski, H. Laffont, G. Lamanna, M. Lemoine-Goumard, J. P. Lenain, D. Lennarz, T. Lohse, A. Lopatin, C. C. Lu, V. Marandon, A. Marcowith, J. Masbou, D. Maurin, N. Maxted, T. J L McComb, M. C. Medina, J. Mehault, R. Moderski, E. Moulin, M. Naumann-Godo, M. De Naurois, D. Nedbal, D. Nekrassov, N. Nguyen, B. Nicholas, J. Niemiec, S. J. Nolan, S. Ohm, J. F. Olive, E. Ona De Wilhelmi, B. Opitz, M. Ostrowski, M. Panter, M. Paz Arribas, G. Pedaletti, G. Pelletier, P. O. Petrucci, S. Pita, G. Puhlhofer, M. Punch, A. Quirrenbach, M. Raue, S. M. Rayner, A. Reimer, O. Reimer, M. Renaud, R. De Los Reyes, F. Rieger, J. Ripken, L. Rob, S. Rosier-Lees, G. Rowell, B. Rudak, C. B. Rulten, J. Ruppel, F. Ryde, V. Sahakian, A. Santangelo, R. Schlickeiser, F. M. Schock, A. Schonwald, U. Schwanke, S. Schwarzburg, S. Schwemmer, A. Shalchi, I. Sushch, M. Sikora, J. L. Skilton, H. Sol, G. Spengler, Stawarz, R. Steenkamp, C. Stegmann, F. Stinzing, A. Szostek, P. H. Tam, J. P. Tavernet, R. Terrier, O. Tibolla, M. Tluczykont, K. Valerius, C. Van Eldik, G. Vasileiadis, C. Venter, J. P. Vialle, A. Viana, P. Vincent, M. Vivier, H. J. Volk, F. Volpe, S. Vorobiov, S. J. Wagner, M. Ward, A. Wierzcholska, A. Zajczyk, A. A. Zdziarski, A. Zech, H. S. Zechlin, G. Dubner, E. Giacani

Research output: Contribution to journalArticle

15 Scopus citations

Abstract

The γ-ray pulsar PSR B1706-44 and the adjacent supernova remnant (SNR) candidate G343.1-2.3 were observed by H.E.S.S. during a dedicated observation campaign in 2007. As a result of this observation campaign, a new source of very-high-energy (VHE; E > 100 GeV) γ-ray emission, H.E.S.S.J1708-443, was detected with a statistical significance of 7σ, although no significant point-like emission was detected at the position of the energetic pulsar itself. In this paper, the morphological and spectral analyses of the newly-discovered TeV source are presented. The centroid of H.E.S.S.J1708-443 is considerably offset from the pulsar and located near the apparent center of the SNR, at αJ2000 = 17h08 m11s ± 17s and δJ2000 = -44°20′ ± 4′. The source is found to be significantly more extended than the H.E.S.S. point spread function (∼0.1°), with an intrinsic Gaussian width of 0.29° ± 0.04°. Its integral flux between 1 and 10 TeV is ~ 3.8 × 10-12 ph cm-2 s -1, equivalent to 17% of the Crab Nebula flux in the same energy range. The measured energy spectrum is well-fit by a power law with a relatively hard photon index Γ = 2.0 ± 0.1stat ± 0.2 sys. Additional multi-wavelength data, including 330 MHz VLA observations, were used to investigate the VHE γ-ray source's possible associations with the pulsar wind nebula of PSR B1706-44 and/or with the complex radio structure of the partial shell-type SNR G 343.1-2.3.

Original languageEnglish (US)
Article numberA143
JournalAstronomy and Astrophysics
Volume528
DOIs
StatePublished - 2011

Keywords

  • ISM: individual objects: G343.1-2.3
  • gamma rays: general
  • pulsars: individual: PSRB1706-44

Fingerprint Dive into the research topics of 'Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.'. Together they form a unique fingerprint.

  • Cite this

    Abramowski, A., Acero, F., Aharonian, F., Akhperjanian, A. G., Anton, G., Barnacka, A., Barres De Almeida, U., Bazer-Bachi, A. R., Becherini, Y., Becker, J., Behera, B., Bernlohr, K., Bochow, A., Boisson, C., Bolmont, J., Bordas, P., Borre, V., Brucker, J., Brun, F., ... Giacani, E. (2011). Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S. Astronomy and Astrophysics, 528, [A143]. https://doi.org/10.1051/0004-6361/201015381