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 language | English (US) |
|---|---|
| Article number | A143 |
| Journal | Astronomy and Astrophysics |
| Volume | 528 |
| DOIs | |
| State | Published - 2011 |
Keywords
- ISM: individual objects: G343.1-2.3
- gamma rays: general
- pulsars: individual: PSRB1706-44
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Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S. / 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.; Brun, P.; Bulik, T.; Busching, I.; Carrigan, S.; Casanova, S.; Cerruti, M.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C G; Cheesebrough, A.; Conrad, J.; Chounet, L. M.; Clapson, A. C.; Coignet, G.; Dalton, M.; Danie, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; Dickinson, H. J.; Djannati-Atai, A.; Domainko, W.; Drury, L. O C; Dubois, F.; Dubus, G.; Dyks, J.; Dyrda, M.; Egberts, K.; Eger, P.; Espigat, P.; Fallon, L.; Farnier, C.; Fegan, S.; Feinstein, F.; Fernandes, M. V.; Fiasson, A.; Forster, A.; Fontaine, G.; Fusling, M.; Gabici, S.; Gallant, Y. A.; Gast, H.; Gerard, L.; Gerbig, D.; Giebels, B.; Glicenstein, J. F.; Gluck, B.; Goret, P.; Goring, D.; Hague, J. D.; Hampf, D.; Hauser, M.; Heinz, S.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Hofverberg, P.; Holleran, M.; Hoppe, S.; Horns, D.; Jacholkowska, A.; De Jager, O. C.; Jahn, C.; Jamrozy, M.; Jung, I.; Kastendieck, M. A.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Kerschhagg, M.; Khangulyan, D.; Khelifi, B.; Keogh, D.; Kluźzniak, W.; Kneiske, T.; Komin, Nu; Kosack, K.; Kossakowski, R.; Laffont, H.; Lamanna, G.; Lemoine-Goumard, M.; Lenain, J. P.; Lennarz, D.; Lohse, T.; Lopatin, A.; Lu, C. C.; Marandon, V.; Marcowith, A.; Masbou, J.; Maurin, D.; Maxted, N.; McComb, T. J L; Medina, M. C.; Mehault, J.; Moderski, R.; Moulin, E.; Naumann-Godo, M.; De Naurois, M.; Nedbal, D.; Nekrassov, D.; Nguyen, N.; Nicholas, B.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Olive, J. F.; De Wilhelmi, E. Ona; Opitz, B.; Ostrowski, M.; Panter, M.; Arribas, M. Paz; Pedaletti, G.; Pelletier, G.; Petrucci, P. O.; Pita, S.; Puhlhofer, G.; Punch, M.; Quirrenbach, A.; Raue, M.; Rayner, S. M.; Reimer, A.; Reimer, O.; Renaud, M.; De Los Reyes, R.; Rieger, F.; Ripken, J.; Rob, L.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Ryde, F.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; Schock, F. M.; Schonwald, A.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Sushch, I.; Sikora, M.; Skilton, J. L.; Sol, H.; Spengler, G.; Stawarz; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Szostek, A.; Tam, P. H.; Tavernet, J. P.; Terrier, R.; Tibolla, O.; Tluczykont, M.; Valerius, K.; Van Eldik, C.; Vasileiadis, G.; Venter, C.; Vialle, J. P.; Viana, A.; Vincent, P.; Vivier, M.; Volk, H. J.; Volpe, F.; Vorobiov, S.; Wagner, S. J.; Ward, M.; Wierzcholska, A.; Zajczyk, A.; Zdziarski, A. A.; Zech, A.; Zechlin, H. S.; Dubner, G.; Giacani, E.
In: Astronomy and Astrophysics, Vol. 528, A143, 2011.Research output: Contribution to journal › Article › peer-review
}
TY - JOUR
T1 - Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.
AU - Abramowski, A.
AU - Acero, F.
AU - Aharonian, F.
AU - Akhperjanian, A. G.
AU - Anton, G.
AU - Barnacka, A.
AU - Barres De Almeida, U.
AU - Bazer-Bachi, A. R.
AU - Becherini, Y.
AU - Becker, J.
AU - Behera, B.
AU - Bernlohr, K.
AU - Bochow, A.
AU - Boisson, C.
AU - Bolmont, J.
AU - Bordas, P.
AU - Borre, V.
AU - Brucker, J.
AU - Brun, F.
AU - Brun, P.
AU - Bulik, T.
AU - Busching, I.
AU - Carrigan, S.
AU - Casanova, S.
AU - Cerruti, M.
AU - Chadwick, P. M.
AU - Charbonnier, A.
AU - Chaves, R. C G
AU - Cheesebrough, A.
AU - Conrad, J.
AU - Chounet, L. M.
AU - Clapson, A. C.
AU - Coignet, G.
AU - Dalton, M.
AU - Danie, M. K.
AU - Davids, I. D.
AU - Degrange, B.
AU - Deil, C.
AU - Dickinson, H. J.
AU - Djannati-Atai, A.
AU - Domainko, W.
AU - Drury, L. O C
AU - Dubois, F.
AU - Dubus, G.
AU - Dyks, J.
AU - Dyrda, M.
AU - Egberts, K.
AU - Eger, P.
AU - Espigat, P.
AU - Fallon, L.
AU - Farnier, C.
AU - Fegan, S.
AU - Feinstein, F.
AU - Fernandes, M. V.
AU - Fiasson, A.
AU - Forster, A.
AU - Fontaine, G.
AU - Fusling, M.
AU - Gabici, S.
AU - Gallant, Y. A.
AU - Gast, H.
AU - Gerard, L.
AU - Gerbig, D.
AU - Giebels, B.
AU - Glicenstein, J. F.
AU - Gluck, B.
AU - Goret, P.
AU - Goring, D.
AU - Hague, J. D.
AU - Hampf, D.
AU - Hauser, M.
AU - Heinz, S.
AU - Heinzelmann, G.
AU - Henri, G.
AU - Hermann, G.
AU - Hinton, J. A.
AU - Hoffmann, A.
AU - Hofmann, W.
AU - Hofverberg, P.
AU - Holleran, M.
AU - Hoppe, S.
AU - Horns, D.
AU - Jacholkowska, A.
AU - De Jager, O. C.
AU - Jahn, C.
AU - Jamrozy, M.
AU - Jung, I.
AU - Kastendieck, M. A.
AU - Katarzyński, K.
AU - Katz, U.
AU - Kaufmann, S.
AU - Kerschhagg, M.
AU - Khangulyan, D.
AU - Khelifi, B.
AU - Keogh, D.
AU - Kluźzniak, W.
AU - Kneiske, T.
AU - Komin, Nu
AU - Kosack, K.
AU - Kossakowski, R.
AU - Laffont, H.
AU - Lamanna, G.
AU - Lemoine-Goumard, M.
AU - Lenain, J. P.
AU - Lennarz, D.
AU - Lohse, T.
AU - Lopatin, A.
AU - Lu, C. C.
AU - Marandon, V.
AU - Marcowith, A.
AU - Masbou, J.
AU - Maurin, D.
AU - Maxted, N.
AU - McComb, T. J L
AU - Medina, M. C.
AU - Mehault, J.
AU - Moderski, R.
AU - Moulin, E.
AU - Naumann-Godo, M.
AU - De Naurois, M.
AU - Nedbal, D.
AU - Nekrassov, D.
AU - Nguyen, N.
AU - Nicholas, B.
AU - Niemiec, J.
AU - Nolan, S. J.
AU - Ohm, S.
AU - Olive, J. F.
AU - De Wilhelmi, E. Ona
AU - Opitz, B.
AU - Ostrowski, M.
AU - Panter, M.
AU - Arribas, M. Paz
AU - Pedaletti, G.
AU - Pelletier, G.
AU - Petrucci, P. O.
AU - Pita, S.
AU - Puhlhofer, G.
AU - Punch, M.
AU - Quirrenbach, A.
AU - Raue, M.
AU - Rayner, S. M.
AU - Reimer, A.
AU - Reimer, O.
AU - Renaud, M.
AU - De Los Reyes, R.
AU - Rieger, F.
AU - Ripken, J.
AU - Rob, L.
AU - Rosier-Lees, S.
AU - Rowell, G.
AU - Rudak, B.
AU - Rulten, C. B.
AU - Ruppel, J.
AU - Ryde, F.
AU - Sahakian, V.
AU - Santangelo, A.
AU - Schlickeiser, R.
AU - Schock, F. M.
AU - Schonwald, A.
AU - Schwanke, U.
AU - Schwarzburg, S.
AU - Schwemmer, S.
AU - Shalchi, A.
AU - Sushch, I.
AU - Sikora, M.
AU - Skilton, J. L.
AU - Sol, H.
AU - Spengler, G.
AU - Stawarz,
AU - Steenkamp, R.
AU - Stegmann, C.
AU - Stinzing, F.
AU - Szostek, A.
AU - Tam, P. H.
AU - Tavernet, J. P.
AU - Terrier, R.
AU - Tibolla, O.
AU - Tluczykont, M.
AU - Valerius, K.
AU - Van Eldik, C.
AU - Vasileiadis, G.
AU - Venter, C.
AU - Vialle, J. P.
AU - Viana, A.
AU - Vincent, P.
AU - Vivier, M.
AU - Volk, H. J.
AU - Volpe, F.
AU - Vorobiov, S.
AU - Wagner, S. J.
AU - Ward, M.
AU - Wierzcholska, A.
AU - Zajczyk, A.
AU - Zdziarski, A. A.
AU - Zech, A.
AU - Zechlin, H. S.
AU - Dubner, G.
AU - Giacani, E.
PY - 2011
Y1 - 2011
N2 - 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.
AB - 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.
KW - ISM: individual objects: G343.1-2.3
KW - gamma rays: general
KW - pulsars: individual: PSRB1706-44
UR - http://www.scopus.com/inward/record.url?scp=79952746402&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=79952746402&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201015381
DO - 10.1051/0004-6361/201015381
M3 - Article
AN - SCOPUS:79952746402
VL - 528
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A143
ER -