Detection of very-high-energy gamma-ray emission from the vicinity of PSR B1706-44 and G343.1-2.3 with H.E.S.S
The gamma-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) gamma-ray emission, HESS J1708-4...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2011, Vol.528 |
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| creator | Abramowski, A. Acero, Fabio Aharonian, F. Akhperjanian, A.G. Anton, G. Barnacka, A. Barres de Almeida, U. Bazer-Bachi, A.R. Becherini, Y. Becker, J. Behera, B. Bernlöhr, K. Bochow, A. Boisson, C. Bolmont, J. Bordas, P. Borrel, V. Brucker, J. Brun, F. Brun, P. Bulik, T. Büsching, 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. Daniel, M.K. Davids, I.D. Degrange, B. Deil, C. Dickinson, H.J. Djannati-Ataï, 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. Förster, A. Fontaine, G. Füssling, M. Gabici, S. Gallant, Y.A. Gast, H. Gérard, L. Gerbig, D. Giebels, B. Glicenstein, J.F. Glück, B. Goret, P. Göring, 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. Katarzy'Nski, K. Katz, U. Kaufmann, S. Kerschhaggl, M. Khangulyan, D. Kh'Elifi, B. Keogh, D. Klu'Zniak, W. Kneiske, T. Komin, Nu Kosack, K. Kossakowski, R. |
| description | The gamma-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) gamma-ray emission, HESS J1708-443, was detected with a statistical significance of 7 sigma, 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 HESS J1708-443 is considerably offset from the pulsar and located near the apparent center of the SNR, at RA(J2000) = 17h08m11s +/- 17s and Dec(J2000) = -44d20' +/- 4'. The source is found to be significantly more extended than the H.E.S.S. point spread function (~0.1 deg), with an intrinsic Gaussian width of 0.29 deg +/- 0.04 deg. Its integral flux between 1 and 10 TeV is ~ 3.8 x 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 Gamma = 2.0 +/- 0.1 (stat) +/- 0.2 (sys). Additional multi-wavelength data, including 330 MHz VLA observations, were used to investigate the VHE gamma-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 G343.1-2.3. |
| doi_str_mv | 10.1051/0004-6361/201015381 |
| format | Article |
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As a result of this observation campaign, a new source of very-high-energy (VHE; E > 100 GeV) gamma-ray emission, HESS J1708-443, was detected with a statistical significance of 7 sigma, 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 HESS J1708-443 is considerably offset from the pulsar and located near the apparent center of the SNR, at RA(J2000) = 17h08m11s +/- 17s and Dec(J2000) = -44d20' +/- 4'. The source is found to be significantly more extended than the H.E.S.S. point spread function (~0.1 deg), with an intrinsic Gaussian width of 0.29 deg +/- 0.04 deg. Its integral flux between 1 and 10 TeV is ~ 3.8 x 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 Gamma = 2.0 +/- 0.1 (stat) +/- 0.2 (sys). Additional multi-wavelength data, including 330 MHz VLA observations, were used to investigate the VHE gamma-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 G343.1-2.3.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0756</identifier><identifier>DOI: 10.1051/0004-6361/201015381</identifier><language>eng</language><publisher>EDP Sciences</publisher><subject>Astrophysics ; High Energy Astrophysical Phenomena ; Physics ; Sciences of the Universe</subject><ispartof>Astronomy and astrophysics (Berlin), 2011, Vol.528</ispartof><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><orcidid>0000-0002-9751-7633 ; 0000-0002-9978-2510 ; 0000-0001-8424-3621 ; 0000-0002-9199-7031 ; 0000-0002-4710-2165 ; 0000-0002-7576-7869 ; 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W.</creatorcontrib><creatorcontrib>Kneiske, T.</creatorcontrib><creatorcontrib>Komin, Nu</creatorcontrib><creatorcontrib>Kosack, K.</creatorcontrib><creatorcontrib>Kossakowski, R.</creatorcontrib><title>Detection of very-high-energy gamma-ray emission from the vicinity of PSR B1706-44 and G343.1-2.3 with H.E.S.S</title><title>Astronomy and astrophysics (Berlin)</title><description>The gamma-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) gamma-ray emission, HESS J1708-443, was detected with a statistical significance of 7 sigma, 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 HESS J1708-443 is considerably offset from the pulsar and located near the apparent center of the SNR, at RA(J2000) = 17h08m11s +/- 17s and Dec(J2000) = -44d20' +/- 4'. The source is found to be significantly more extended than the H.E.S.S. point spread function (~0.1 deg), with an intrinsic Gaussian width of 0.29 deg +/- 0.04 deg. Its integral flux between 1 and 10 TeV is ~ 3.8 x 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 Gamma = 2.0 +/- 0.1 (stat) +/- 0.2 (sys). Additional multi-wavelength data, including 330 MHz VLA observations, were used to investigate the VHE gamma-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 G343.1-2.3.</description><subject>Astrophysics</subject><subject>High Energy Astrophysical Phenomena</subject><subject>Physics</subject><subject>Sciences of the Universe</subject><issn>0004-6361</issn><issn>1432-0756</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2011</creationdate><recordtype>article</recordtype><recordid>eNqVy01LxDAUheEgCtbRX-Dm7iWZe3vTTLd-jHbhQqbuQxjTNjJNh7RU-u91QNy7OrzwHCFuCRVhQWtE1NKwoXWOhFRwSWciI825xE1hzkX2Jy7F1Th-_mROJWciPvnJ76cwRBgamH1aZBfaTvroU7tA6_reyeQW8H0YxxNr0tDD1HmYwz7EMC2n41u9gwfaoJFag4sf8MKaFclcMXyFqYNKbVWt6mtx0bjD6G9-dyXunrfvj5Xs3MEeU-hdWuzggq3uX22I-ZEtYmG4RJ6J_6e_AV-pUGQ</recordid><startdate>2011</startdate><enddate>2011</enddate><creator>Abramowski, 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of very-high-energy gamma-ray emission from the vicinity of PSR B1706-44 and G343.1-2.3 with H.E.S.S</title><author>Abramowski, A. ; Acero, Fabio ; Aharonian, F. ; Akhperjanian, A.G. ; Anton, G. ; Barnacka, A. ; Barres de Almeida, U. ; Bazer-Bachi, A.R. ; Becherini, Y. ; Becker, J. ; Behera, B. ; Bernlöhr, K. ; Bochow, A. ; Boisson, C. ; Bolmont, J. ; Bordas, P. ; Borrel, V. ; Brucker, J. ; Brun, F. ; Brun, P. ; Bulik, T. ; Büsching, 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. ; Daniel, M.K. ; Davids, I.D. ; Degrange, B. ; Deil, C. ; Dickinson, H.J. ; Djannati-Ataï, 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. ; Förster, A. ; Fontaine, G. ; Füssling, M. ; Gabici, S. ; Gallant, Y.A. ; Gast, H. ; Gérard, L. ; Gerbig, D. ; Giebels, B. ; Glicenstein, J.F. ; Glück, B. ; Goret, P. ; Göring, 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. ; Katarzy'Nski, K. ; Katz, U. ; Kaufmann, S. ; Kerschhaggl, M. ; Khangulyan, D. ; Kh'Elifi, B. ; Keogh, D. ; Klu'Zniak, W. ; Kneiske, T. ; Komin, Nu ; Kosack, K. ; Kossakowski, R.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-hal_primary_oai_HAL_in2p3_00563803v13</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2011</creationdate><topic>Astrophysics</topic><topic>High Energy Astrophysical Phenomena</topic><topic>Physics</topic><topic>Sciences of the Universe</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Abramowski, A.</creatorcontrib><creatorcontrib>Acero, Fabio</creatorcontrib><creatorcontrib>Aharonian, F.</creatorcontrib><creatorcontrib>Akhperjanian, A.G.</creatorcontrib><creatorcontrib>Anton, G.</creatorcontrib><creatorcontrib>Barnacka, A.</creatorcontrib><creatorcontrib>Barres de Almeida, U.</creatorcontrib><creatorcontrib>Bazer-Bachi, A.R.</creatorcontrib><creatorcontrib>Becherini, Y.</creatorcontrib><creatorcontrib>Becker, J.</creatorcontrib><creatorcontrib>Behera, B.</creatorcontrib><creatorcontrib>Bernlöhr, K.</creatorcontrib><creatorcontrib>Bochow, A.</creatorcontrib><creatorcontrib>Boisson, C.</creatorcontrib><creatorcontrib>Bolmont, J.</creatorcontrib><creatorcontrib>Bordas, P.</creatorcontrib><creatorcontrib>Borrel, V.</creatorcontrib><creatorcontrib>Brucker, J.</creatorcontrib><creatorcontrib>Brun, F.</creatorcontrib><creatorcontrib>Brun, 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L.O'C.</creatorcontrib><creatorcontrib>Dubois, F.</creatorcontrib><creatorcontrib>Dubus, G.</creatorcontrib><creatorcontrib>Dyks, J.</creatorcontrib><creatorcontrib>Dyrda, M.</creatorcontrib><creatorcontrib>Egberts, K.</creatorcontrib><creatorcontrib>Eger, P.</creatorcontrib><creatorcontrib>Espigat, P.</creatorcontrib><creatorcontrib>Fallon, L.</creatorcontrib><creatorcontrib>Farnier, C.</creatorcontrib><creatorcontrib>Fegan, S.</creatorcontrib><creatorcontrib>Feinstein, F.</creatorcontrib><creatorcontrib>Fernandes, M.V.</creatorcontrib><creatorcontrib>Fiasson, A.</creatorcontrib><creatorcontrib>Förster, A.</creatorcontrib><creatorcontrib>Fontaine, G.</creatorcontrib><creatorcontrib>Füssling, M.</creatorcontrib><creatorcontrib>Gabici, S.</creatorcontrib><creatorcontrib>Gallant, Y.A.</creatorcontrib><creatorcontrib>Gast, H.</creatorcontrib><creatorcontrib>Gérard, L.</creatorcontrib><creatorcontrib>Gerbig, D.</creatorcontrib><creatorcontrib>Giebels, B.</creatorcontrib><creatorcontrib>Glicenstein, J.F.</creatorcontrib><creatorcontrib>Glück, B.</creatorcontrib><creatorcontrib>Goret, P.</creatorcontrib><creatorcontrib>Göring, D.</creatorcontrib><creatorcontrib>Hague, J.D.</creatorcontrib><creatorcontrib>Hampf, D.</creatorcontrib><creatorcontrib>Hauser, M.</creatorcontrib><creatorcontrib>Heinz, S.</creatorcontrib><creatorcontrib>Heinzelmann, G.</creatorcontrib><creatorcontrib>Henri, G.</creatorcontrib><creatorcontrib>Hermann, G.</creatorcontrib><creatorcontrib>Hinton, J.A.</creatorcontrib><creatorcontrib>Hoffmann, A.</creatorcontrib><creatorcontrib>Hofmann, W.</creatorcontrib><creatorcontrib>Hofverberg, P.</creatorcontrib><creatorcontrib>Holleran, M.</creatorcontrib><creatorcontrib>Hoppe, S.</creatorcontrib><creatorcontrib>Horns, D.</creatorcontrib><creatorcontrib>Jacholkowska, A.</creatorcontrib><creatorcontrib>de Jager, O.C.</creatorcontrib><creatorcontrib>Jahn, C.</creatorcontrib><creatorcontrib>Jamrozy, M.</creatorcontrib><creatorcontrib>Jung, I.</creatorcontrib><creatorcontrib>Kastendieck, M.A.</creatorcontrib><creatorcontrib>Katarzy'Nski, K.</creatorcontrib><creatorcontrib>Katz, U.</creatorcontrib><creatorcontrib>Kaufmann, S.</creatorcontrib><creatorcontrib>Kerschhaggl, M.</creatorcontrib><creatorcontrib>Khangulyan, D.</creatorcontrib><creatorcontrib>Kh'Elifi, B.</creatorcontrib><creatorcontrib>Keogh, D.</creatorcontrib><creatorcontrib>Klu'Zniak, W.</creatorcontrib><creatorcontrib>Kneiske, T.</creatorcontrib><creatorcontrib>Komin, Nu</creatorcontrib><creatorcontrib>Kosack, K.</creatorcontrib><creatorcontrib>Kossakowski, R.</creatorcontrib><collection>Hyper Article en Ligne (HAL)</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Abramowski, A.</au><au>Acero, Fabio</au><au>Aharonian, F.</au><au>Akhperjanian, A.G.</au><au>Anton, G.</au><au>Barnacka, A.</au><au>Barres de Almeida, U.</au><au>Bazer-Bachi, A.R.</au><au>Becherini, Y.</au><au>Becker, J.</au><au>Behera, B.</au><au>Bernlöhr, K.</au><au>Bochow, A.</au><au>Boisson, C.</au><au>Bolmont, J.</au><au>Bordas, P.</au><au>Borrel, V.</au><au>Brucker, J.</au><au>Brun, F.</au><au>Brun, P.</au><au>Bulik, T.</au><au>Büsching, I.</au><au>Carrigan, S.</au><au>Casanova, S.</au><au>Cerruti, M.</au><au>Chadwick, P.M.</au><au>Charbonnier, A.</au><au>Chaves, R.C.G.</au><au>Cheesebrough, A.</au><au>Conrad, J.</au><au>Chounet, L.-M.</au><au>Clapson, A.C.</au><au>Coignet, G.</au><au>Dalton, M.</au><au>Daniel, M.K.</au><au>Davids, I.D.</au><au>Degrange, B.</au><au>Deil, C.</au><au>Dickinson, H.J.</au><au>Djannati-Ataï, A.</au><au>Domainko, W.</au><au>Drury, L.O'C.</au><au>Dubois, F.</au><au>Dubus, G.</au><au>Dyks, J.</au><au>Dyrda, M.</au><au>Egberts, K.</au><au>Eger, P.</au><au>Espigat, P.</au><au>Fallon, L.</au><au>Farnier, C.</au><au>Fegan, S.</au><au>Feinstein, F.</au><au>Fernandes, M.V.</au><au>Fiasson, A.</au><au>Förster, A.</au><au>Fontaine, G.</au><au>Füssling, M.</au><au>Gabici, S.</au><au>Gallant, Y.A.</au><au>Gast, H.</au><au>Gérard, L.</au><au>Gerbig, D.</au><au>Giebels, B.</au><au>Glicenstein, J.F.</au><au>Glück, B.</au><au>Goret, P.</au><au>Göring, D.</au><au>Hague, J.D.</au><au>Hampf, D.</au><au>Hauser, M.</au><au>Heinz, S.</au><au>Heinzelmann, G.</au><au>Henri, G.</au><au>Hermann, G.</au><au>Hinton, J.A.</au><au>Hoffmann, A.</au><au>Hofmann, W.</au><au>Hofverberg, P.</au><au>Holleran, M.</au><au>Hoppe, S.</au><au>Horns, D.</au><au>Jacholkowska, A.</au><au>de Jager, O.C.</au><au>Jahn, C.</au><au>Jamrozy, M.</au><au>Jung, I.</au><au>Kastendieck, M.A.</au><au>Katarzy'Nski, K.</au><au>Katz, U.</au><au>Kaufmann, S.</au><au>Kerschhaggl, M.</au><au>Khangulyan, D.</au><au>Kh'Elifi, B.</au><au>Keogh, D.</au><au>Klu'Zniak, W.</au><au>Kneiske, T.</au><au>Komin, Nu</au><au>Kosack, K.</au><au>Kossakowski, R.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Detection of very-high-energy gamma-ray emission from the vicinity of PSR B1706-44 and G343.1-2.3 with H.E.S.S</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2011</date><risdate>2011</risdate><volume>528</volume><issn>0004-6361</issn><eissn>1432-0756</eissn><abstract>The gamma-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) gamma-ray emission, HESS J1708-443, was detected with a statistical significance of 7 sigma, 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 HESS J1708-443 is considerably offset from the pulsar and located near the apparent center of the SNR, at RA(J2000) = 17h08m11s +/- 17s and Dec(J2000) = -44d20' +/- 4'. The source is found to be significantly more extended than the H.E.S.S. point spread function (~0.1 deg), with an intrinsic Gaussian width of 0.29 deg +/- 0.04 deg. Its integral flux between 1 and 10 TeV is ~ 3.8 x 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 Gamma = 2.0 +/- 0.1 (stat) +/- 0.2 (sys). Additional multi-wavelength data, including 330 MHz VLA observations, were used to investigate the VHE gamma-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 G343.1-2.3.</abstract><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201015381</doi><orcidid>https://orcid.org/0000-0002-9751-7633</orcidid><orcidid>https://orcid.org/0000-0002-9978-2510</orcidid><orcidid>https://orcid.org/0000-0001-8424-3621</orcidid><orcidid>https://orcid.org/0000-0002-9199-7031</orcidid><orcidid>https://orcid.org/0000-0002-4710-2165</orcidid><orcidid>https://orcid.org/0000-0002-7576-7869</orcidid><orcidid>https://orcid.org/0000-0001-8065-3252</orcidid><orcidid>https://orcid.org/0000-0002-4388-5625</orcidid><orcidid>https://orcid.org/0000-0001-5893-1797</orcidid><orcidid>https://orcid.org/0000-0001-6061-3480</orcidid><orcidid>https://orcid.org/0000-0002-2203-4880</orcidid><orcidid>https://orcid.org/0000-0003-1157-3915</orcidid><orcidid>https://orcid.org/0000-0002-7063-4418</orcidid><orcidid>https://orcid.org/0000-0001-7909-588X</orcidid><orcidid>https://orcid.org/0000-0002-2115-2930</orcidid><orcidid>https://orcid.org/0000-0001-7891-699X</orcidid><orcidid>https://orcid.org/0000-0002-6606-2816</orcidid><orcidid>https://orcid.org/0000-0001-9077-4058</orcidid><orcidid>https://orcid.org/0000-0003-0452-3805</orcidid><orcidid>https://orcid.org/0000-0002-6204-0409</orcidid><orcidid>https://orcid.org/0000-0002-5130-2514</orcidid><orcidid>https://orcid.org/0000-0003-3842-8531</orcidid><orcidid>https://orcid.org/0000-0003-4187-9560</orcidid><orcidid>https://orcid.org/0000-0003-0770-9007</orcidid><orcidid>https://orcid.org/0000-0002-0207-958X</orcidid><orcidid>https://orcid.org/0000-0001-6036-8569</orcidid><orcidid>https://orcid.org/0000-0002-7245-201X</orcidid><orcidid>https://orcid.org/0000-0002-0870-7778</orcidid><orcidid>https://orcid.org/0000-0003-3280-0582</orcidid><orcidid>https://orcid.org/0000-0001-8604-7077</orcidid><orcidid>https://orcid.org/0000-0003-1334-2993</orcidid><orcidid>https://orcid.org/0000-0002-3474-2243</orcidid><orcidid>https://orcid.org/0000-0002-1229-278X</orcidid><orcidid>https://orcid.org/0000-0003-1945-0119</orcidid><orcidid>https://orcid.org/0000-0002-5331-0606</orcidid><orcidid>https://orcid.org/0000-0002-2666-4812</orcidid><orcidid>https://orcid.org/0000-0002-3971-0910</orcidid><orcidid>https://orcid.org/0000-0001-9669-645X</orcidid><orcidid>https://orcid.org/0000-0003-4472-7204</orcidid><orcidid>https://orcid.org/0000-0002-6144-9122</orcidid><orcidid>https://orcid.org/0000-0002-9516-1581</orcidid><orcidid>https://orcid.org/0000-0003-1187-4240</orcidid><orcidid>https://orcid.org/0000-0001-7284-9220</orcidid><orcidid>https://orcid.org/0000-0002-0207-958X</orcidid><orcidid>https://orcid.org/0000-0002-6606-2816</orcidid><orcidid>https://orcid.org/0000-0002-5130-2514</orcidid><orcidid>https://orcid.org/0000-0001-5893-1797</orcidid><orcidid>https://orcid.org/0000-0003-3280-0582</orcidid><orcidid>https://orcid.org/0000-0002-7576-7869</orcidid><orcidid>https://orcid.org/0000-0002-2115-2930</orcidid><orcidid>https://orcid.org/0000-0001-8424-3621</orcidid><orcidid>https://orcid.org/0000-0002-9978-2510</orcidid><orcidid>https://orcid.org/0000-0003-1187-4240</orcidid><orcidid>https://orcid.org/0000-0001-7909-588X</orcidid><orcidid>https://orcid.org/0000-0003-0770-9007</orcidid><orcidid>https://orcid.org/0000-0001-8065-3252</orcidid><orcidid>https://orcid.org/0000-0002-6144-9122</orcidid><orcidid>https://orcid.org/0000-0001-7891-699X</orcidid><orcidid>https://orcid.org/0000-0002-0870-7778</orcidid><orcidid>https://orcid.org/0000-0003-1157-3915</orcidid><orcidid>https://orcid.org/0000-0003-3842-8531</orcidid><orcidid>https://orcid.org/0000-0002-7063-4418</orcidid><orcidid>https://orcid.org/0000-0003-1945-0119</orcidid></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-6361 |
| ispartof | Astronomy and astrophysics (Berlin), 2011, Vol.528 |
| issn | 0004-6361 1432-0756 |
| language | eng |
| recordid | cdi_hal_primary_oai_HAL_in2p3_00563803v1 |
| source | EDP Sciences; Elektronische Zeitschriftenbibliothek; EDP Sciences - Revues - Licences nationales - accès par la plateforme ISTEX |
| subjects | Astrophysics High Energy Astrophysical Phenomena Physics Sciences of the Universe |
| title | Detection of very-high-energy gamma-ray emission from the vicinity of PSR B1706-44 and G343.1-2.3 with H.E.S.S |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-11T19%3A11%3A57IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-hal&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Detection%20of%20very-high-energy%20gamma-ray%20emission%20from%20the%20vicinity%20of%20PSR%20B1706-44%20and%20G343.1-2.3%20with%20H.E.S.S&rft.jtitle=Astronomy%20and%20astrophysics%20(Berlin)&rft.au=Abramowski,%20A.&rft.date=2011&rft.volume=528&rft.issn=0004-6361&rft.eissn=1432-0756&rft_id=info:doi/10.1051/0004-6361/201015381&rft_dat=%3Chal%3Eoai_HAL_in2p3_00563803v1%3C/hal%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_id=info:pmid/&rfr_iscdi=true |