VERITAS Observations of Day-scale Flaring of M 87 in 2010 April
- Autores
- Aliu, E.; Arlen, T.; Aune, T.; Beilicke, M.; Benbow, W.; Bouvier, A.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; Byrum, K.; Cannon, A.; Cesarini, A.; Ciupik, L.; Collins Hughes, E.; Connolly, M. P.; Cui, W.; Dickherber, R.; Duke, C.; Errando, M.; Falcone, A.; Finley, J. P.; Finnegan, G.; Fortson, N.; Furniss, A.; Galante, N.; Gall, D.; Godambe, S.; Griffin, S.; Grube, J.; Pichel, Ana Carolina; The Veritas Collaboration
- Año de publicación
- 2012
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- VERITAS has been monitoring the very-high-energy (VHE; E > 100 GeV) gamma-ray activity of the radio galaxy M 87 since 2007. During 2008, flaring activity on a timescale of a few days was observed with a peak flux of (0.70 ± 0.16) x 10^-11 cm^-2 s^-1 at energies above 350 GeV. In 2010 April, VERITAS detected a flare from M 87 with peak flux of (2.71 ± 0.68) × 10^-11 cm^-2 s^-1 for E > 350 GeV. The source was observed for six consecutive nights during the flare, resulting in a total of 21 hr of good-quality data. The most rapid flux variation occurred on the trailing edge of the flare with an exponential flux decay time of 0.90 +0.22 -0.15 days. The shortest detected exponential rise time is three times as long, at 2.87 +1.65 -0.99 days. The quality of the data sample is such that spectral analysis can be performed for three periods: rising flux, peak flux, and falling flux. The spectra obtained are consistent with power-law forms. The spectral index at the peak of the flare is equal to 2.19 ± 0.07. There is some indication that the spectrum is softer in the falling phase of the flare than the peak phase, with a confidence level corresponding to 3.6 standard deviations. We discuss the implications of these results for the acceleration and cooling rates of VHE electrons in M 87 and the constraints they provide on the physical size of the emitting region.
Fil: Aliu, E.. Columbia University; Estados Unidos
Fil: Arlen, T.. University of California; Estados Unidos
Fil: Aune, T.. University of California; Estados Unidos
Fil: Beilicke, M.. University of Washington; Estados Unidos
Fil: Benbow, W.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Bouvier, A.. University of California; Estados Unidos
Fil: Bradbury, S. M.. University of Leeds; Reino Unido
Fil: Buckley, J. H.. University of Washington; Estados Unidos
Fil: Bugaev, V.. University of Washington; Estados Unidos
Fil: Byrum, K.. Argonne National Laboratory; Estados Unidos
Fil: Cannon, A.. University College Dublin; Irlanda
Fil: Cesarini, A.. National University of Ireland Galway; Irlanda
Fil: Ciupik, L.. Adler Planetarium and Astronomy Museum; Estados Unidos
Fil: Collins Hughes, E.. University College Dublin; Irlanda
Fil: Connolly, M. P.. National University of Ireland Galway; Irlanda
Fil: Cui, W.. Purdue University; Estados Unidos
Fil: Dickherber, R.. University of Washington; Estados Unidos
Fil: Duke, C.. Grinnell College; Estados Unidos
Fil: Errando, M.. Columbia University; Estados Unidos
Fil: Falcone, A.. Pennsylvania State University; Estados Unidos
Fil: Finley, J. P.. Purdue University; Estados Unidos
Fil: Finnegan, G.. University of Utah; Estados Unidos
Fil: Fortson, N.. University Of Minnesota; Estados Unidos
Fil: Furniss, A.. University of California; Estados Unidos
Fil: Galante, N.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Gall, D.. University of Iowa; Estados Unidos
Fil: Godambe, S.. University of Utah; Estados Unidos
Fil: Griffin, S.. McGill University; Canadá
Fil: Grube, J.. Adler Planetarium and Astronomy Museum; Estados Unidos
Fil: Pichel, Ana Carolina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: The Veritas Collaboration. - Materia
-
galaxies: individual (M 87, VER J1230+123)
gamma rays: galaxies - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/18849
Ver los metadatos del registro completo
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VERITAS Observations of Day-scale Flaring of M 87 in 2010 AprilAliu, E.Arlen, T.Aune, T.Beilicke, M.Benbow, W.Bouvier, A.Bradbury, S. M.Buckley, J. H.Bugaev, V.Byrum, K.Cannon, A.Cesarini, A.Ciupik, L.Collins Hughes, E.Connolly, M. P.Cui, W.Dickherber, R.Duke, C.Errando, M.Falcone, A.Finley, J. P.Finnegan, G.Fortson, N.Furniss, A.Galante, N.Gall, D.Godambe, S.Griffin, S.Grube, J.Pichel, Ana CarolinaThe Veritas Collaborationgalaxies: individual (M 87, VER J1230+123)gamma rays: galaxieshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1VERITAS has been monitoring the very-high-energy (VHE; E > 100 GeV) gamma-ray activity of the radio galaxy M 87 since 2007. During 2008, flaring activity on a timescale of a few days was observed with a peak flux of (0.70 ± 0.16) x 10^-11 cm^-2 s^-1 at energies above 350 GeV. In 2010 April, VERITAS detected a flare from M 87 with peak flux of (2.71 ± 0.68) × 10^-11 cm^-2 s^-1 for E > 350 GeV. The source was observed for six consecutive nights during the flare, resulting in a total of 21 hr of good-quality data. The most rapid flux variation occurred on the trailing edge of the flare with an exponential flux decay time of 0.90 +0.22 -0.15 days. The shortest detected exponential rise time is three times as long, at 2.87 +1.65 -0.99 days. The quality of the data sample is such that spectral analysis can be performed for three periods: rising flux, peak flux, and falling flux. The spectra obtained are consistent with power-law forms. The spectral index at the peak of the flare is equal to 2.19 ± 0.07. There is some indication that the spectrum is softer in the falling phase of the flare than the peak phase, with a confidence level corresponding to 3.6 standard deviations. We discuss the implications of these results for the acceleration and cooling rates of VHE electrons in M 87 and the constraints they provide on the physical size of the emitting region.Fil: Aliu, E.. Columbia University; Estados UnidosFil: Arlen, T.. University of California; Estados UnidosFil: Aune, T.. University of California; Estados UnidosFil: Beilicke, M.. University of Washington; Estados UnidosFil: Benbow, W.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Bouvier, A.. University of California; Estados UnidosFil: Bradbury, S. M.. University of Leeds; Reino UnidoFil: Buckley, J. H.. University of Washington; Estados UnidosFil: Bugaev, V.. University of Washington; Estados UnidosFil: Byrum, K.. Argonne National Laboratory; Estados UnidosFil: Cannon, A.. University College Dublin; IrlandaFil: Cesarini, A.. National University of Ireland Galway; IrlandaFil: Ciupik, L.. Adler Planetarium and Astronomy Museum; Estados UnidosFil: Collins Hughes, E.. University College Dublin; IrlandaFil: Connolly, M. P.. National University of Ireland Galway; IrlandaFil: Cui, W.. Purdue University; Estados UnidosFil: Dickherber, R.. University of Washington; Estados UnidosFil: Duke, C.. Grinnell College; Estados UnidosFil: Errando, M.. Columbia University; Estados UnidosFil: Falcone, A.. Pennsylvania State University; Estados UnidosFil: Finley, J. P.. Purdue University; Estados UnidosFil: Finnegan, G.. University of Utah; Estados UnidosFil: Fortson, N.. University Of Minnesota; Estados UnidosFil: Furniss, A.. University of California; Estados UnidosFil: Galante, N.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Gall, D.. University of Iowa; Estados UnidosFil: Godambe, S.. University of Utah; Estados UnidosFil: Griffin, S.. McGill University; CanadáFil: Grube, J.. Adler Planetarium and Astronomy Museum; Estados UnidosFil: Pichel, Ana Carolina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: The Veritas Collaboration.Iop Publishing2012-02-20info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/18849Aliu, E.; Arlen, T.; Aune, T.; Beilicke, M.; Benbow, W.; et al.; VERITAS Observations of Day-scale Flaring of M 87 in 2010 April; Iop Publishing; Astrophysical Journal; 746; 2; 20-2-2012; 1-7; 1410004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/746/2/141info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1112.4518info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/746/2/141/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:22:46Zoai:ri.conicet.gov.ar:11336/18849instacron: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 11:22:46.594CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
VERITAS Observations of Day-scale Flaring of M 87 in 2010 April |
| title |
VERITAS Observations of Day-scale Flaring of M 87 in 2010 April |
| spellingShingle |
VERITAS Observations of Day-scale Flaring of M 87 in 2010 April Aliu, E. galaxies: individual (M 87, VER J1230+123) gamma rays: galaxies |
| title_short |
VERITAS Observations of Day-scale Flaring of M 87 in 2010 April |
| title_full |
VERITAS Observations of Day-scale Flaring of M 87 in 2010 April |
| title_fullStr |
VERITAS Observations of Day-scale Flaring of M 87 in 2010 April |
| title_full_unstemmed |
VERITAS Observations of Day-scale Flaring of M 87 in 2010 April |
| title_sort |
VERITAS Observations of Day-scale Flaring of M 87 in 2010 April |
| dc.creator.none.fl_str_mv |
Aliu, E. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Collins Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Duke, C. Errando, M. Falcone, A. Finley, J. P. Finnegan, G. Fortson, N. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Grube, J. Pichel, Ana Carolina The Veritas Collaboration |
| author |
Aliu, E. |
| author_facet |
Aliu, E. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Collins Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Duke, C. Errando, M. Falcone, A. Finley, J. P. Finnegan, G. Fortson, N. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Grube, J. Pichel, Ana Carolina The Veritas Collaboration |
| author_role |
author |
| author2 |
Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Collins Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Duke, C. Errando, M. Falcone, A. Finley, J. P. Finnegan, G. Fortson, N. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Grube, J. Pichel, Ana Carolina The Veritas Collaboration |
| 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 author author author author author author author |
| dc.subject.none.fl_str_mv |
galaxies: individual (M 87, VER J1230+123) gamma rays: galaxies |
| topic |
galaxies: individual (M 87, VER J1230+123) gamma rays: galaxies |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
VERITAS has been monitoring the very-high-energy (VHE; E > 100 GeV) gamma-ray activity of the radio galaxy M 87 since 2007. During 2008, flaring activity on a timescale of a few days was observed with a peak flux of (0.70 ± 0.16) x 10^-11 cm^-2 s^-1 at energies above 350 GeV. In 2010 April, VERITAS detected a flare from M 87 with peak flux of (2.71 ± 0.68) × 10^-11 cm^-2 s^-1 for E > 350 GeV. The source was observed for six consecutive nights during the flare, resulting in a total of 21 hr of good-quality data. The most rapid flux variation occurred on the trailing edge of the flare with an exponential flux decay time of 0.90 +0.22 -0.15 days. The shortest detected exponential rise time is three times as long, at 2.87 +1.65 -0.99 days. The quality of the data sample is such that spectral analysis can be performed for three periods: rising flux, peak flux, and falling flux. The spectra obtained are consistent with power-law forms. The spectral index at the peak of the flare is equal to 2.19 ± 0.07. There is some indication that the spectrum is softer in the falling phase of the flare than the peak phase, with a confidence level corresponding to 3.6 standard deviations. We discuss the implications of these results for the acceleration and cooling rates of VHE electrons in M 87 and the constraints they provide on the physical size of the emitting region. Fil: Aliu, E.. Columbia University; Estados Unidos Fil: Arlen, T.. University of California; Estados Unidos Fil: Aune, T.. University of California; Estados Unidos Fil: Beilicke, M.. University of Washington; Estados Unidos Fil: Benbow, W.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Bouvier, A.. University of California; Estados Unidos Fil: Bradbury, S. M.. University of Leeds; Reino Unido Fil: Buckley, J. H.. University of Washington; Estados Unidos Fil: Bugaev, V.. University of Washington; Estados Unidos Fil: Byrum, K.. Argonne National Laboratory; Estados Unidos Fil: Cannon, A.. University College Dublin; Irlanda Fil: Cesarini, A.. National University of Ireland Galway; Irlanda Fil: Ciupik, L.. Adler Planetarium and Astronomy Museum; Estados Unidos Fil: Collins Hughes, E.. University College Dublin; Irlanda Fil: Connolly, M. P.. National University of Ireland Galway; Irlanda Fil: Cui, W.. Purdue University; Estados Unidos Fil: Dickherber, R.. University of Washington; Estados Unidos Fil: Duke, C.. Grinnell College; Estados Unidos Fil: Errando, M.. Columbia University; Estados Unidos Fil: Falcone, A.. Pennsylvania State University; Estados Unidos Fil: Finley, J. P.. Purdue University; Estados Unidos Fil: Finnegan, G.. University of Utah; Estados Unidos Fil: Fortson, N.. University Of Minnesota; Estados Unidos Fil: Furniss, A.. University of California; Estados Unidos Fil: Galante, N.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Gall, D.. University of Iowa; Estados Unidos Fil: Godambe, S.. University of Utah; Estados Unidos Fil: Griffin, S.. McGill University; Canadá Fil: Grube, J.. Adler Planetarium and Astronomy Museum; Estados Unidos Fil: Pichel, Ana Carolina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: The Veritas Collaboration. |
| description |
VERITAS has been monitoring the very-high-energy (VHE; E > 100 GeV) gamma-ray activity of the radio galaxy M 87 since 2007. During 2008, flaring activity on a timescale of a few days was observed with a peak flux of (0.70 ± 0.16) x 10^-11 cm^-2 s^-1 at energies above 350 GeV. In 2010 April, VERITAS detected a flare from M 87 with peak flux of (2.71 ± 0.68) × 10^-11 cm^-2 s^-1 for E > 350 GeV. The source was observed for six consecutive nights during the flare, resulting in a total of 21 hr of good-quality data. The most rapid flux variation occurred on the trailing edge of the flare with an exponential flux decay time of 0.90 +0.22 -0.15 days. The shortest detected exponential rise time is three times as long, at 2.87 +1.65 -0.99 days. The quality of the data sample is such that spectral analysis can be performed for three periods: rising flux, peak flux, and falling flux. The spectra obtained are consistent with power-law forms. The spectral index at the peak of the flare is equal to 2.19 ± 0.07. There is some indication that the spectrum is softer in the falling phase of the flare than the peak phase, with a confidence level corresponding to 3.6 standard deviations. We discuss the implications of these results for the acceleration and cooling rates of VHE electrons in M 87 and the constraints they provide on the physical size of the emitting region. |
| publishDate |
2012 |
| dc.date.none.fl_str_mv |
2012-02-20 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
| format |
article |
| status_str |
publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/18849 Aliu, E.; Arlen, T.; Aune, T.; Beilicke, M.; Benbow, W.; et al.; VERITAS Observations of Day-scale Flaring of M 87 in 2010 April; Iop Publishing; Astrophysical Journal; 746; 2; 20-2-2012; 1-7; 141 0004-637X CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/18849 |
| identifier_str_mv |
Aliu, E.; Arlen, T.; Aune, T.; Beilicke, M.; Benbow, W.; et al.; VERITAS Observations of Day-scale Flaring of M 87 in 2010 April; Iop Publishing; Astrophysical Journal; 746; 2; 20-2-2012; 1-7; 141 0004-637X CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
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info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/746/2/141 info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1112.4518 info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/746/2/141/meta |
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openAccess |
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Iop Publishing |
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