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) γ -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 γ -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 analysed in the context of the multiwavelength observations currently available and in the framework of both leptonic and hadronic particle acceleration scenarios. No significant γ -ray signal from G1.9+0.3 or G330.2+1.0 was detected. Upper limits (99 per cent confidence level) to the TeV flux from G1.9+0.3 and G330.2+1.0 for the assumed spectral index Γ = 2.5 were set at 5.6 × 10-13 cm-2 s-1 above 0.26 TeV and 3.2 × 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 BG1.9 ≳ 12 μG for G1.9+0.3 and to BG330 ≳ 8 μG 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.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 790-799 |
| Number of pages | 10 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 441 |
| Issue number | 1 |
| DOIs | |
| State | Published - 2014 |
Bibliographical note
Copyright:Copyright 2014 Elsevier B.V., All rights reserved.
Keywords
- Gamma-rays: ISM
- ISM: magnetic fields
- ISM: supernova remnants
- Radiation mechanisms: non-thermal
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TeV γ-ray observations of the young synchrotron-dominated SNRs G1.9+0.3 and G330.2+1.0 with H.E.S.S. / Abramowski, A.; Aharonian, F.; Ait Benkhali, F.; Akhperjanian, A. G.; Angüner, E.; Anton, G.; Balenderan, S.; Balzer, A.; Barnacka, A.; Becherini, Y.; Becker Tjus, J.; Bernlöhr, K.; Birsin, E.; Bissaldi, E.; Biteau, J.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bordas, P.; Brucker, J.; Brun, F.; Brun, P.; Bulik, T.; Carrigan, S.; Casanova, S.; Cerruti, M.; Chadwick, P. M.; Chalme-Calvet, R.; Chaves, R. C G; Cheesebrough, A.; Chrétien, M.; Colafrancesco, S.; Cologna, G.; Conrad, J.; Couturier, C.; Cui, Y.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; De Wilt, P.; Dickinson, H. J.; Djannati-Ataï, A.; Domainko, W.; Drury, L. O C; Dubus, G.; Dutson, K.; Dyks, J.; Dyrda, M.; Edwards, T.; Egberts, K.; Eger, P.; Espigat, P.; Farnier, C.; Fegan, S.; Feinstein, F.; Fernandes, M. V.; Fernandez, D.; Fiasson, A.; Fontaine, G.; Förster, A.; Füßling, M.; Gajdus, M.; Gallant, Y. A.; Garrigoux, T.; Giavitto, G.; Giebels, B.; Glicenstein, J. F.; Grondin, M. H.; Grudzińska, M.; Häffner, S.; Hahn, J.; Harris, J.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hervet, O.; Hillert, A.; Hinton, J. A.; Hofmann, W.; Hofverberg, P.; Holler, M.; Horns, D.; Jacholkowska, A.; Jahn, C.; Jamrozy, M.; Janiak, M.; Jankowsky, F.; Jung, I.; Kastendieck, M. A.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Khélifi, B.; Kieffer, M.; Klepser, S.; Klochkov, D.; Kluźniak, W.; Kneiske, T.; Kolitzus, D.; Komin, Nu; Kosack, K.; Krakau, S.; Krayzel, F.; Krüger, P. P.; Laffon, H.; Lamanna, G.; Lefaucheur, J.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. P.; Lennarz, D.; Lohse, T.; Lopatin, A.; Lu, C. C.; Marandon, V.; Marcowith, A.; Marx, R.; Maurin, G.; Maxted, N.; Mayer, M.; McComb, T. J L; Méhault, J.; Meintjes, P. J.; Menzler, U.; Meyer, M.; Moderski, R.; Mohamed, M.; Moulin, E.; Murach, T.; Naumann, C. L.; de Naurois, M.; Niemiec, J.; Nolan, S. J.; Oakes, L.; Ohm, S.; De Oña Wilhelmi, E.; Opitz, B.; Ostrowski, M.; Oya, I.; Panter, M.; Parsons, R. D.; Paz Arribas, M.; Pekeur, N. W.; Pelletier, G.; Perez, J.; Petrucci, P. O.; Peyaud, B.; Pita, S.; Poon, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Raue, M.; Reimer, A.; Reimer, O.; Renaud, M.; de los Reyes, R.; Rieger, F.; Rob, L.; Romoli, C.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Sahakian, V.; Sanchez, D. A.; Santangelo, A.; Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Sol, H.; Spengler, G.; Spies, F.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Stycz, K.; Sushch, I.; Szostek, A.; Tavernet, J. P.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tluczykont, M.; Trichard, C.; Valerius, K.; van Eldik, C.; van Soelen, B.; Vasileiadis, G.; Venter, C.; Viana, A.; Vincent, P.; Völk, H. J.; Volpe, F.; Vorster, M.; Vuillaume, T.; Wagner, S. J.; Wagner, P.; Ward, M.; Weidinger, M.; Weitzel, Q.; White, R.; Wierzcholska, A.; Willmann, P.; Wörnlein, A.; Wouters, D.; Zabalza, V.; Zacharias, M.; Zajczyk, A.; Zdziarski, A. A.; Zech, A.; Zechlin, H. S.
In: Monthly Notices of the Royal Astronomical Society, Vol. 441, No. 1, 2014, p. 790-799.Research output: Contribution to journal › Article › peer-review
}
TY - JOUR
T1 - TeV γ-ray observations of the young synchrotron-dominated SNRs G1.9+0.3 and G330.2+1.0 with H.E.S.S.
AU - Abramowski, A.
AU - Aharonian, F.
AU - Ait Benkhali, F.
AU - Akhperjanian, A. G.
AU - Angüner, E.
AU - Anton, G.
AU - Balenderan, S.
AU - Balzer, A.
AU - Barnacka, A.
AU - Becherini, Y.
AU - Becker Tjus, J.
AU - Bernlöhr, K.
AU - Birsin, E.
AU - Bissaldi, E.
AU - Biteau, J.
AU - Böttcher, M.
AU - Boisson, C.
AU - Bolmont, J.
AU - Bordas, P.
AU - Brucker, J.
AU - Brun, F.
AU - Brun, P.
AU - Bulik, T.
AU - Carrigan, S.
AU - Casanova, S.
AU - Cerruti, M.
AU - Chadwick, P. M.
AU - Chalme-Calvet, R.
AU - Chaves, R. C G
AU - Cheesebrough, A.
AU - Chrétien, M.
AU - Colafrancesco, S.
AU - Cologna, G.
AU - Conrad, J.
AU - Couturier, C.
AU - Cui, Y.
AU - Dalton, M.
AU - Daniel, M. K.
AU - Davids, I. D.
AU - Degrange, B.
AU - Deil, C.
AU - De Wilt, P.
AU - Dickinson, H. J.
AU - Djannati-Ataï, A.
AU - Domainko, W.
AU - Drury, L. O C
AU - Dubus, G.
AU - Dutson, K.
AU - Dyks, J.
AU - Dyrda, M.
AU - Edwards, T.
AU - Egberts, K.
AU - Eger, P.
AU - Espigat, P.
AU - Farnier, C.
AU - Fegan, S.
AU - Feinstein, F.
AU - Fernandes, M. V.
AU - Fernandez, D.
AU - Fiasson, A.
AU - Fontaine, G.
AU - Förster, A.
AU - Füßling, M.
AU - Gajdus, M.
AU - Gallant, Y. A.
AU - Garrigoux, T.
AU - Giavitto, G.
AU - Giebels, B.
AU - Glicenstein, J. F.
AU - Grondin, M. H.
AU - Grudzińska, M.
AU - Häffner, S.
AU - Hahn, J.
AU - Harris, J.
AU - Heinzelmann, G.
AU - Henri, G.
AU - Hermann, G.
AU - Hervet, O.
AU - Hillert, A.
AU - Hinton, J. A.
AU - Hofmann, W.
AU - Hofverberg, P.
AU - Holler, M.
AU - Horns, D.
AU - Jacholkowska, A.
AU - Jahn, C.
AU - Jamrozy, M.
AU - Janiak, M.
AU - Jankowsky, F.
AU - Jung, I.
AU - Kastendieck, M. A.
AU - Katarzyński, K.
AU - Katz, U.
AU - Kaufmann, S.
AU - Khélifi, B.
AU - Kieffer, M.
AU - Klepser, S.
AU - Klochkov, D.
AU - Kluźniak, W.
AU - Kneiske, T.
AU - Kolitzus, D.
AU - Komin, Nu
AU - Kosack, K.
AU - Krakau, S.
AU - Krayzel, F.
AU - Krüger, P. P.
AU - Laffon, H.
AU - Lamanna, G.
AU - Lefaucheur, J.
AU - Lemière, A.
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 - Marx, R.
AU - Maurin, G.
AU - Maxted, N.
AU - Mayer, M.
AU - McComb, T. J L
AU - Méhault, J.
AU - Meintjes, P. J.
AU - Menzler, U.
AU - Meyer, M.
AU - Moderski, R.
AU - Mohamed, M.
AU - Moulin, E.
AU - Murach, T.
AU - Naumann, C. L.
AU - de Naurois, M.
AU - Niemiec, J.
AU - Nolan, S. J.
AU - Oakes, L.
AU - Ohm, S.
AU - De Oña Wilhelmi, E.
AU - Opitz, B.
AU - Ostrowski, M.
AU - Oya, I.
AU - Panter, M.
AU - Parsons, R. D.
AU - Paz Arribas, M.
AU - Pekeur, N. W.
AU - Pelletier, G.
AU - Perez, J.
AU - Petrucci, P. O.
AU - Peyaud, B.
AU - Pita, S.
AU - Poon, H.
AU - Pühlhofer, G.
AU - Punch, M.
AU - Quirrenbach, A.
AU - Raab, S.
AU - Raue, M.
AU - Reimer, A.
AU - Reimer, O.
AU - Renaud, M.
AU - de los Reyes, R.
AU - Rieger, F.
AU - Rob, L.
AU - Romoli, C.
AU - Rosier-Lees, S.
AU - Rowell, G.
AU - Rudak, B.
AU - Rulten, C. B.
AU - Sahakian, V.
AU - Sanchez, D. A.
AU - Santangelo, A.
AU - Schlickeiser, R.
AU - Schüssler, F.
AU - Schulz, A.
AU - Schwanke, U.
AU - Schwarzburg, S.
AU - Schwemmer, S.
AU - Sol, H.
AU - Spengler, G.
AU - Spies, F.
AU - Stawarz, L.
AU - Steenkamp, R.
AU - Stegmann, C.
AU - Stinzing, F.
AU - Stycz, K.
AU - Sushch, I.
AU - Szostek, A.
AU - Tavernet, J. P.
AU - Tavernier, T.
AU - Taylor, A. M.
AU - Terrier, R.
AU - Tluczykont, M.
AU - Trichard, C.
AU - Valerius, K.
AU - van Eldik, C.
AU - van Soelen, B.
AU - Vasileiadis, G.
AU - Venter, C.
AU - Viana, A.
AU - Vincent, P.
AU - Völk, H. J.
AU - Volpe, F.
AU - Vorster, M.
AU - Vuillaume, T.
AU - Wagner, S. J.
AU - Wagner, P.
AU - Ward, M.
AU - Weidinger, M.
AU - Weitzel, Q.
AU - White, R.
AU - Wierzcholska, A.
AU - Willmann, P.
AU - Wörnlein, A.
AU - Wouters, D.
AU - Zabalza, V.
AU - Zacharias, M.
AU - Zajczyk, A.
AU - Zdziarski, A. A.
AU - Zech, A.
AU - Zechlin, H. S.
N1 - Copyright: Copyright 2014 Elsevier B.V., All rights reserved.
PY - 2014
Y1 - 2014
N2 - 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) γ -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 γ -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 analysed in the context of the multiwavelength observations currently available and in the framework of both leptonic and hadronic particle acceleration scenarios. No significant γ -ray signal from G1.9+0.3 or G330.2+1.0 was detected. Upper limits (99 per cent confidence level) to the TeV flux from G1.9+0.3 and G330.2+1.0 for the assumed spectral index Γ = 2.5 were set at 5.6 × 10-13 cm-2 s-1 above 0.26 TeV and 3.2 × 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 BG1.9 ≳ 12 μG for G1.9+0.3 and to BG330 ≳ 8 μG 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.
AB - 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) γ -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 γ -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 analysed in the context of the multiwavelength observations currently available and in the framework of both leptonic and hadronic particle acceleration scenarios. No significant γ -ray signal from G1.9+0.3 or G330.2+1.0 was detected. Upper limits (99 per cent confidence level) to the TeV flux from G1.9+0.3 and G330.2+1.0 for the assumed spectral index Γ = 2.5 were set at 5.6 × 10-13 cm-2 s-1 above 0.26 TeV and 3.2 × 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 BG1.9 ≳ 12 μG for G1.9+0.3 and to BG330 ≳ 8 μG 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.
KW - Gamma-rays: ISM
KW - ISM: magnetic fields
KW - ISM: supernova remnants
KW - Radiation mechanisms: non-thermal
UR - http://www.scopus.com/inward/record.url?scp=84900007602&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84900007602&partnerID=8YFLogxK
U2 - 10.1093/mnras/stu459
DO - 10.1093/mnras/stu459
M3 - Article
AN - SCOPUS:84900007602
VL - 441
SP - 790
EP - 799
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 1
ER -