Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S.
- Autores
- Abramowski, A.; Aharonian, Felix A.; Akhperjanian, A. G.; Anton, G.; Balenderan, S.; Balzer, A.; Barnacka, A.; Becherini, Y.; Becker Tjus, J.; Bernlöhr, K.; Birsin, E.; Bochow, A.; Boisson, C.; Bolmont, J.; Boisson, C.; Bolmont, J.; Brun, P.; Brun, F.; Casanova, S.; Cerruti, M.; Chadwick, P.M.; Charbonnier, A.; Chaves, R.C.G.; Cheesebrough, A.; Cologna, G.; Medina, Maria Clementina
- Año de publicación
- 2012
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. Vela X is a region of extended radio emission in the western part of the Vela constellation: one of the nearest pulsar wind nebulae, and associated with the energetic Vela pulsar (PSR B0833-45). Extended very-high-energy (VHE) γ-ray emission (HESS J0835-455) was discovered using the H.E.S.S. experiment in 2004. The VHE γ-ray emission was found to be coincident with a region of X-ray emission discovered with ROSAT above 1.5 keV (the so-called Vela X cocoon): a filamentary structure extending southwest from the pulsar to the centre of Vela X. Aims. A deeper observation of the entire Vela X nebula region, also including larger offsets from the cocoon, has been performed with H.E.S.S. This re-observation was carried out in order to probe the extent of the non-thermal emission from the Vela X region at TeV energies and to investigate its spectral properties. Methods. To increase the sensitivity to the faint γ-ray emission from the very extended Vela X region, a multivariate analysis method combining three complementary reconstruction techniques of Cherenkov-shower images is applied for the selection of γ-ray events. The analysis is performed with the On/Off background method, which estimates the background from separate observations pointing away from Vela X; towards regions free of γ-ray sources but with comparable observation conditions. Results. The γ-ray surface brightness over the large Vela X region reveals that the detection of non-thermal VHE γ-ray emission from the PWN HESS J0835-455 is statistically significant over a region of radius 1.2° around the position α = 08 h35m00s, δ = - 45°36′00′′ (J2000). The Vela X region exhibits almost uniform γ-ray spectra over its full extent: the differential energy spectrum can be described by a power-law function with a hard spectral index Γ = 1.32 ± 0.06stat ± 0.12sys and an exponential cutoff at an energy of (14.0 ± 1.6stat ± 2.6sys) TeV. Compared to the previous H.E.S.S. observations of Vela X the new analysis confirms the general spatial overlap of the bulk of the VHE γ-ray emission with the X-ray cocoon, while its extent and morphology appear more consistent with the (more extended) radio emission, contradicting the simple correspondence between VHE γ-ray and X-ray emissions. Morphological and spectral results challenge the interpretation of the origin of γ-ray emission in the GeV and TeV ranges in the framework of current models. © ESO, 2012.
Fil: Abramowski, A.. Universitat Hamburg; Alemania
Fil: Aharonian, Felix A.. Max Planck Institut Fur Kernphysik; Alemania
Fil: Akhperjanian, A. G.. National Academy Of Sciences Of The Republic Of Armenia; Armenia. Yerevan Physics Institute; Armenia
Fil: Anton, G.. Universitat Erlangen-Nuremberg; Alemania
Fil: Balenderan, S.. University Of Durham; Reino Unido
Fil: Balzer, A.. Universitat Erlangen-Nuremberg; Alemania
Fil: Barnacka, A.. CEA Saclay; Francia
Fil: Becherini, Y.. Université Paris Diderot - Paris 7; Francia
Fil: Becker Tjus, J.. Ruhr Universität Bochum; Alemania
Fil: Bernlöhr, K.. Max Planck Institut Fur Kernphysik; Alemania
Fil: Birsin, E.. Humboldt-universitat Zu Berlin; Alemania
Fil: Bochow, A.. Max Planck Institut Fur Kernphysik; Alemania
Fil: Boisson, C.. Université Paris Diderot - Paris 7; Francia
Fil: Bolmont, J.. Max Planck Institut Fur Kernphysik; Alemania
Fil: Boisson, C.. Université Paris Diderot - Paris 7; Francia
Fil: Bolmont, J.. Universite Pierre et Marie Curie; Francia
Fil: Brun, P.. Cea Saclay;
Fil: Brun, F.. Laboratoire Leprince-ringuet; Francia
Fil: Casanova, S.. Max Planck Institut Fur Kernphysik; Alemania
Fil: Cerruti, M.. Université Paris Diderot - Paris 7; Francia
Fil: Chadwick, P.M.. University Of Durham; Reino Unido
Fil: Charbonnier, A.. Universite Pierre et Marie Curie; Francia
Fil: Chaves, R.C.G.. Cea Saclay; Francia. Max Planck Institut Fur Kernphysik; Alemania
Fil: Cheesebrough, A.. University Of Durham; Reino Unido
Fil: Cologna, G.. Landessternwarte Heidelberg; Alemania
Fil: Medina, Maria Clementina. Cea Saclay; Francia. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina - Materia
-
Radiation mechanisms
Vela X (pulsar)
HESS J0835–455
Gamma rays
Non thermal mechanisms - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- Atribución-NoComercial-CompartirIgual 2.5 Argentina (CC BY-NC-SA 2.5 AR)
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/39888
Ver los metadatos del registro completo
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Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S.Abramowski, A.Aharonian, Felix A.Akhperjanian, A. G.Anton, G.Balenderan, S.Balzer, A.Barnacka, A.Becherini, Y.Becker Tjus, J.Bernlöhr, K.Birsin, E.Bochow, A.Boisson, C.Bolmont, J.Boisson, C.Bolmont, J.Brun, P.Brun, F.Casanova, S.Cerruti, M.Chadwick, P.M.Charbonnier, A.Chaves, R.C.G.Cheesebrough, A.Cologna, G.Medina, Maria ClementinaRadiation mechanismsVela X (pulsar)HESS J0835–455Gamma raysNon thermal mechanismshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Vela X is a region of extended radio emission in the western part of the Vela constellation: one of the nearest pulsar wind nebulae, and associated with the energetic Vela pulsar (PSR B0833-45). Extended very-high-energy (VHE) γ-ray emission (HESS J0835-455) was discovered using the H.E.S.S. experiment in 2004. The VHE γ-ray emission was found to be coincident with a region of X-ray emission discovered with ROSAT above 1.5 keV (the so-called Vela X cocoon): a filamentary structure extending southwest from the pulsar to the centre of Vela X. Aims. A deeper observation of the entire Vela X nebula region, also including larger offsets from the cocoon, has been performed with H.E.S.S. This re-observation was carried out in order to probe the extent of the non-thermal emission from the Vela X region at TeV energies and to investigate its spectral properties. Methods. To increase the sensitivity to the faint γ-ray emission from the very extended Vela X region, a multivariate analysis method combining three complementary reconstruction techniques of Cherenkov-shower images is applied for the selection of γ-ray events. The analysis is performed with the On/Off background method, which estimates the background from separate observations pointing away from Vela X; towards regions free of γ-ray sources but with comparable observation conditions. Results. The γ-ray surface brightness over the large Vela X region reveals that the detection of non-thermal VHE γ-ray emission from the PWN HESS J0835-455 is statistically significant over a region of radius 1.2° around the position α = 08 h35m00s, δ = - 45°36′00′′ (J2000). The Vela X region exhibits almost uniform γ-ray spectra over its full extent: the differential energy spectrum can be described by a power-law function with a hard spectral index Γ = 1.32 ± 0.06stat ± 0.12sys and an exponential cutoff at an energy of (14.0 ± 1.6stat ± 2.6sys) TeV. Compared to the previous H.E.S.S. observations of Vela X the new analysis confirms the general spatial overlap of the bulk of the VHE γ-ray emission with the X-ray cocoon, while its extent and morphology appear more consistent with the (more extended) radio emission, contradicting the simple correspondence between VHE γ-ray and X-ray emissions. Morphological and spectral results challenge the interpretation of the origin of γ-ray emission in the GeV and TeV ranges in the framework of current models. © ESO, 2012.Fil: Abramowski, A.. Universitat Hamburg; AlemaniaFil: Aharonian, Felix A.. Max Planck Institut Fur Kernphysik; AlemaniaFil: Akhperjanian, A. G.. National Academy Of Sciences Of The Republic Of Armenia; Armenia. Yerevan Physics Institute; ArmeniaFil: Anton, G.. Universitat Erlangen-Nuremberg; AlemaniaFil: Balenderan, S.. University Of Durham; Reino UnidoFil: Balzer, A.. Universitat Erlangen-Nuremberg; AlemaniaFil: Barnacka, A.. CEA Saclay; FranciaFil: Becherini, Y.. Université Paris Diderot - Paris 7; FranciaFil: Becker Tjus, J.. Ruhr Universität Bochum; AlemaniaFil: Bernlöhr, K.. Max Planck Institut Fur Kernphysik; AlemaniaFil: Birsin, E.. Humboldt-universitat Zu Berlin; AlemaniaFil: Bochow, A.. Max Planck Institut Fur Kernphysik; AlemaniaFil: Boisson, C.. Université Paris Diderot - Paris 7; FranciaFil: Bolmont, J.. Max Planck Institut Fur Kernphysik; AlemaniaFil: Boisson, C.. Université Paris Diderot - Paris 7; FranciaFil: Bolmont, J.. Universite Pierre et Marie Curie; FranciaFil: Brun, P.. Cea Saclay;Fil: Brun, F.. Laboratoire Leprince-ringuet; FranciaFil: Casanova, S.. Max Planck Institut Fur Kernphysik; AlemaniaFil: Cerruti, M.. Université Paris Diderot - Paris 7; FranciaFil: Chadwick, P.M.. University Of Durham; Reino UnidoFil: Charbonnier, A.. Universite Pierre et Marie Curie; FranciaFil: Chaves, R.C.G.. Cea Saclay; Francia. Max Planck Institut Fur Kernphysik; AlemaniaFil: Cheesebrough, A.. University Of Durham; Reino UnidoFil: Cologna, G.. Landessternwarte Heidelberg; AlemaniaFil: Medina, Maria Clementina. Cea Saclay; Francia. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaEDP Sciences2012-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/39888Abramowski, A.; Aharonian, Felix A.; Akhperjanian, A. G.; Anton, G.; Balenderan, S.; et al.; Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S.; EDP Sciences; Astronomy and Astrophysics; 548; 12-20120004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2012/12/aa19919-12/aa19919-12.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201219919info:eu-repo/semantics/openAccessAtribución-NoComercial-CompartirIgual 2.5 Argentina (CC BY-NC-SA 2.5 AR)https://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:50:54Zoai:ri.conicet.gov.ar:11336/39888instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 11:50:54.454CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S. |
| title |
Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S. |
| spellingShingle |
Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S. Abramowski, A. Radiation mechanisms Vela X (pulsar) HESS J0835–455 Gamma rays Non thermal mechanisms |
| title_short |
Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S. |
| title_full |
Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S. |
| title_fullStr |
Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S. |
| title_full_unstemmed |
Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S. |
| title_sort |
Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S. |
| dc.creator.none.fl_str_mv |
Abramowski, A. Aharonian, Felix A. Akhperjanian, A. G. Anton, G. Balenderan, S. Balzer, A. Barnacka, A. Becherini, Y. Becker Tjus, J. Bernlöhr, K. Birsin, E. Bochow, A. Boisson, C. Bolmont, J. Boisson, C. Bolmont, J. Brun, P. Brun, F. Casanova, S. Cerruti, M. Chadwick, P.M. Charbonnier, A. Chaves, R.C.G. Cheesebrough, A. Cologna, G. Medina, Maria Clementina |
| author |
Abramowski, A. |
| author_facet |
Abramowski, A. Aharonian, Felix A. Akhperjanian, A. G. Anton, G. Balenderan, S. Balzer, A. Barnacka, A. Becherini, Y. Becker Tjus, J. Bernlöhr, K. Birsin, E. Bochow, A. Boisson, C. Bolmont, J. Brun, P. Brun, F. Casanova, S. Cerruti, M. Chadwick, P.M. Charbonnier, A. Chaves, R.C.G. Cheesebrough, A. Cologna, G. Medina, Maria Clementina |
| author_role |
author |
| author2 |
Aharonian, Felix A. Akhperjanian, A. G. Anton, G. Balenderan, S. Balzer, A. Barnacka, A. Becherini, Y. Becker Tjus, J. Bernlöhr, K. Birsin, E. Bochow, A. Boisson, C. Bolmont, J. Brun, P. Brun, F. Casanova, S. Cerruti, M. Chadwick, P.M. Charbonnier, A. Chaves, R.C.G. Cheesebrough, A. Cologna, G. Medina, Maria Clementina |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
Radiation mechanisms Vela X (pulsar) HESS J0835–455 Gamma rays Non thermal mechanisms |
| topic |
Radiation mechanisms Vela X (pulsar) HESS J0835–455 Gamma rays Non thermal mechanisms |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
Context. Vela X is a region of extended radio emission in the western part of the Vela constellation: one of the nearest pulsar wind nebulae, and associated with the energetic Vela pulsar (PSR B0833-45). Extended very-high-energy (VHE) γ-ray emission (HESS J0835-455) was discovered using the H.E.S.S. experiment in 2004. The VHE γ-ray emission was found to be coincident with a region of X-ray emission discovered with ROSAT above 1.5 keV (the so-called Vela X cocoon): a filamentary structure extending southwest from the pulsar to the centre of Vela X. Aims. A deeper observation of the entire Vela X nebula region, also including larger offsets from the cocoon, has been performed with H.E.S.S. This re-observation was carried out in order to probe the extent of the non-thermal emission from the Vela X region at TeV energies and to investigate its spectral properties. Methods. To increase the sensitivity to the faint γ-ray emission from the very extended Vela X region, a multivariate analysis method combining three complementary reconstruction techniques of Cherenkov-shower images is applied for the selection of γ-ray events. The analysis is performed with the On/Off background method, which estimates the background from separate observations pointing away from Vela X; towards regions free of γ-ray sources but with comparable observation conditions. Results. The γ-ray surface brightness over the large Vela X region reveals that the detection of non-thermal VHE γ-ray emission from the PWN HESS J0835-455 is statistically significant over a region of radius 1.2° around the position α = 08 h35m00s, δ = - 45°36′00′′ (J2000). The Vela X region exhibits almost uniform γ-ray spectra over its full extent: the differential energy spectrum can be described by a power-law function with a hard spectral index Γ = 1.32 ± 0.06stat ± 0.12sys and an exponential cutoff at an energy of (14.0 ± 1.6stat ± 2.6sys) TeV. Compared to the previous H.E.S.S. observations of Vela X the new analysis confirms the general spatial overlap of the bulk of the VHE γ-ray emission with the X-ray cocoon, while its extent and morphology appear more consistent with the (more extended) radio emission, contradicting the simple correspondence between VHE γ-ray and X-ray emissions. Morphological and spectral results challenge the interpretation of the origin of γ-ray emission in the GeV and TeV ranges in the framework of current models. © ESO, 2012. Fil: Abramowski, A.. Universitat Hamburg; Alemania Fil: Aharonian, Felix A.. Max Planck Institut Fur Kernphysik; Alemania Fil: Akhperjanian, A. G.. National Academy Of Sciences Of The Republic Of Armenia; Armenia. Yerevan Physics Institute; Armenia Fil: Anton, G.. Universitat Erlangen-Nuremberg; Alemania Fil: Balenderan, S.. University Of Durham; Reino Unido Fil: Balzer, A.. Universitat Erlangen-Nuremberg; Alemania Fil: Barnacka, A.. CEA Saclay; Francia Fil: Becherini, Y.. Université Paris Diderot - Paris 7; Francia Fil: Becker Tjus, J.. Ruhr Universität Bochum; Alemania Fil: Bernlöhr, K.. Max Planck Institut Fur Kernphysik; Alemania Fil: Birsin, E.. Humboldt-universitat Zu Berlin; Alemania Fil: Bochow, A.. Max Planck Institut Fur Kernphysik; Alemania Fil: Boisson, C.. Université Paris Diderot - Paris 7; Francia Fil: Bolmont, J.. Max Planck Institut Fur Kernphysik; Alemania Fil: Boisson, C.. Université Paris Diderot - Paris 7; Francia Fil: Bolmont, J.. Universite Pierre et Marie Curie; Francia Fil: Brun, P.. Cea Saclay; Fil: Brun, F.. Laboratoire Leprince-ringuet; Francia Fil: Casanova, S.. Max Planck Institut Fur Kernphysik; Alemania Fil: Cerruti, M.. Université Paris Diderot - Paris 7; Francia Fil: Chadwick, P.M.. University Of Durham; Reino Unido Fil: Charbonnier, A.. Universite Pierre et Marie Curie; Francia Fil: Chaves, R.C.G.. Cea Saclay; Francia. Max Planck Institut Fur Kernphysik; Alemania Fil: Cheesebrough, A.. University Of Durham; Reino Unido Fil: Cologna, G.. Landessternwarte Heidelberg; Alemania Fil: Medina, Maria Clementina. Cea Saclay; Francia. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina |
| description |
Context. Vela X is a region of extended radio emission in the western part of the Vela constellation: one of the nearest pulsar wind nebulae, and associated with the energetic Vela pulsar (PSR B0833-45). Extended very-high-energy (VHE) γ-ray emission (HESS J0835-455) was discovered using the H.E.S.S. experiment in 2004. The VHE γ-ray emission was found to be coincident with a region of X-ray emission discovered with ROSAT above 1.5 keV (the so-called Vela X cocoon): a filamentary structure extending southwest from the pulsar to the centre of Vela X. Aims. A deeper observation of the entire Vela X nebula region, also including larger offsets from the cocoon, has been performed with H.E.S.S. This re-observation was carried out in order to probe the extent of the non-thermal emission from the Vela X region at TeV energies and to investigate its spectral properties. Methods. To increase the sensitivity to the faint γ-ray emission from the very extended Vela X region, a multivariate analysis method combining three complementary reconstruction techniques of Cherenkov-shower images is applied for the selection of γ-ray events. The analysis is performed with the On/Off background method, which estimates the background from separate observations pointing away from Vela X; towards regions free of γ-ray sources but with comparable observation conditions. Results. The γ-ray surface brightness over the large Vela X region reveals that the detection of non-thermal VHE γ-ray emission from the PWN HESS J0835-455 is statistically significant over a region of radius 1.2° around the position α = 08 h35m00s, δ = - 45°36′00′′ (J2000). The Vela X region exhibits almost uniform γ-ray spectra over its full extent: the differential energy spectrum can be described by a power-law function with a hard spectral index Γ = 1.32 ± 0.06stat ± 0.12sys and an exponential cutoff at an energy of (14.0 ± 1.6stat ± 2.6sys) TeV. Compared to the previous H.E.S.S. observations of Vela X the new analysis confirms the general spatial overlap of the bulk of the VHE γ-ray emission with the X-ray cocoon, while its extent and morphology appear more consistent with the (more extended) radio emission, contradicting the simple correspondence between VHE γ-ray and X-ray emissions. Morphological and spectral results challenge the interpretation of the origin of γ-ray emission in the GeV and TeV ranges in the framework of current models. © ESO, 2012. |
| publishDate |
2012 |
| dc.date.none.fl_str_mv |
2012-12 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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http://hdl.handle.net/11336/39888 Abramowski, A.; Aharonian, Felix A.; Akhperjanian, A. G.; Anton, G.; Balenderan, S.; et al.; Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S.; EDP Sciences; Astronomy and Astrophysics; 548; 12-2012 0004-6361 CONICET Digital CONICET |
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http://hdl.handle.net/11336/39888 |
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Abramowski, A.; Aharonian, Felix A.; Akhperjanian, A. G.; Anton, G.; Balenderan, S.; et al.; Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S.; EDP Sciences; Astronomy and Astrophysics; 548; 12-2012 0004-6361 CONICET Digital CONICET |
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