Revealing the extended radio emission from the gamma-ray binary HESS J0632+057

After the detection of a 321-days periodicity in X-rays, HESS J0632+057 can be robustly considered a new member of the selected group of gamma-ray binaries. These sources are known to show extended radio structure at scales of milliarcseconds (mas). Aims. We present the expected extended radio emiss...

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Autores: Moldón Vara, Francisco Javier, Ribó Gomis, Marc, Paredes i Poy, Josep Maria
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2011
País:España
Recursos:Universidad de Barcelona
Repositorio:Dipòsit Digital de la UB
OAI Identifier:oai:diposit.ub.edu:2445/122842
Acesso em linha:https://hdl.handle.net/2445/122842
Access Level:acceso abierto
Palavra-chave:Estels binaris de raigs X
Raigs gamma
X-ray binaries
Gamma rays
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oai_identifier_str oai:diposit.ub.edu:2445/122842
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repository_id_str
spelling Revealing the extended radio emission from the gamma-ray binary HESS J0632+057Moldón Vara, Francisco JavierRibó Gomis, MarcParedes i Poy, Josep MariaEstels binaris de raigs XRaigs gammaX-ray binariesGamma raysAfter the detection of a 321-days periodicity in X-rays, HESS J0632+057 can be robustly considered a new member of the selected group of gamma-ray binaries. These sources are known to show extended radio structure at scales of milliarcseconds (mas). Aims. We present the expected extended radio emission on mas scales from HESS J0632+057. Methods. We observed HESS J0632+057 with the European VLBI Network (EVN) at 1.6 GHz in two epochs: during the January/February 2011 X-ray outburst and 30 days later. Results. The VLBI image obtained during the outburst shows a compact ~0.4 mJy radio source, whereas 30 days later the source has faded and appears extended, with a projected size of ~75 AU. The peak of the emission is displaced between runs 21+/-5 AU, which is bigger than the orbit size. The position of the radio source is compatible with the Be star MWC 148, which sets the proper motion of the binary system below 3 mas yr^-1 in each coordinate. The brightness temperature of the source is above 2 \times 10^6 K. We compare the multiwavelength properties of HESS J0632+057 with those of the previously known gamma-ray binaries. Conclusions. HESS J0632+057 displays extended and variable non-thermal radio emission. Its morphology, size, and displacement at AU scales are similar to those found in the other gamma-ray binaries, PSR B1259-63, LS 5039 and LS I +61 303, supporting a similar nature for HESS J0632+057.EDP Sciences2011info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionapplication/pdfhttps://hdl.handle.net/2445/122842Articles publicats en revistes (Física Quàntica i Astrofísica)reponame:Dipòsit Digital de la UBinstname:Universidad de BarcelonaInglésReproducció del document publicat a: https://doi.org/10.1051/0004-6361/201117764Astronomy & Astrophysics, 2011, vol. 533, num. L7https://doi.org/10.1051/0004-6361/201117764info:eu-repo/grantAgreement/EC/FP7/261525(c) The European Southern Observatory (ESO), 2011info:eu-repo/semantics/openAccessoai:diposit.ub.edu:2445/1228422026-05-27T06:46:51Z
dc.title.none.fl_str_mv Revealing the extended radio emission from the gamma-ray binary HESS J0632+057
title Revealing the extended radio emission from the gamma-ray binary HESS J0632+057
spellingShingle Revealing the extended radio emission from the gamma-ray binary HESS J0632+057
Moldón Vara, Francisco Javier
Estels binaris de raigs X
Raigs gamma
X-ray binaries
Gamma rays
title_short Revealing the extended radio emission from the gamma-ray binary HESS J0632+057
title_full Revealing the extended radio emission from the gamma-ray binary HESS J0632+057
title_fullStr Revealing the extended radio emission from the gamma-ray binary HESS J0632+057
title_full_unstemmed Revealing the extended radio emission from the gamma-ray binary HESS J0632+057
title_sort Revealing the extended radio emission from the gamma-ray binary HESS J0632+057
dc.creator.none.fl_str_mv Moldón Vara, Francisco Javier
Ribó Gomis, Marc
Paredes i Poy, Josep Maria
author Moldón Vara, Francisco Javier
author_facet Moldón Vara, Francisco Javier
Ribó Gomis, Marc
Paredes i Poy, Josep Maria
author_role author
author2 Ribó Gomis, Marc
Paredes i Poy, Josep Maria
author2_role author
author
dc.subject.none.fl_str_mv Estels binaris de raigs X
Raigs gamma
X-ray binaries
Gamma rays
topic Estels binaris de raigs X
Raigs gamma
X-ray binaries
Gamma rays
description After the detection of a 321-days periodicity in X-rays, HESS J0632+057 can be robustly considered a new member of the selected group of gamma-ray binaries. These sources are known to show extended radio structure at scales of milliarcseconds (mas). Aims. We present the expected extended radio emission on mas scales from HESS J0632+057. Methods. We observed HESS J0632+057 with the European VLBI Network (EVN) at 1.6 GHz in two epochs: during the January/February 2011 X-ray outburst and 30 days later. Results. The VLBI image obtained during the outburst shows a compact ~0.4 mJy radio source, whereas 30 days later the source has faded and appears extended, with a projected size of ~75 AU. The peak of the emission is displaced between runs 21+/-5 AU, which is bigger than the orbit size. The position of the radio source is compatible with the Be star MWC 148, which sets the proper motion of the binary system below 3 mas yr^-1 in each coordinate. The brightness temperature of the source is above 2 \times 10^6 K. We compare the multiwavelength properties of HESS J0632+057 with those of the previously known gamma-ray binaries. Conclusions. HESS J0632+057 displays extended and variable non-thermal radio emission. Its morphology, size, and displacement at AU scales are similar to those found in the other gamma-ray binaries, PSR B1259-63, LS 5039 and LS I +61 303, supporting a similar nature for HESS J0632+057.
publishDate 2011
dc.date.none.fl_str_mv 2011
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv https://hdl.handle.net/2445/122842
url https://hdl.handle.net/2445/122842
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv Reproducció del document publicat a: https://doi.org/10.1051/0004-6361/201117764
Astronomy & Astrophysics, 2011, vol. 533, num. L7
https://doi.org/10.1051/0004-6361/201117764
info:eu-repo/grantAgreement/EC/FP7/261525
dc.rights.none.fl_str_mv (c) The European Southern Observatory (ESO), 2011
info:eu-repo/semantics/openAccess
rights_invalid_str_mv (c) The European Southern Observatory (ESO), 2011
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv Articles publicats en revistes (Física Quàntica i Astrofísica)
reponame:Dipòsit Digital de la UB
instname:Universidad de Barcelona
instname_str Universidad de Barcelona
reponame_str Dipòsit Digital de la UB
collection Dipòsit Digital de la UB
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,301603

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