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Article: Spectrum and morphology of the two brightest Milagro sources in the Cygnus region: MGRO J2019+37 and MGRO J2031+41

TitleSpectrum and morphology of the two brightest Milagro sources in the Cygnus region: MGRO J2019+37 and MGRO J2031+41
Authors
KeywordsAcceleration Of Particles
Astroparticle Physics
Gamma Rays: General
Open Clusters And Associations: Individual (Cyg Ob1, Cyg Ob2)
Pulsars: General
Issue Date2012
PublisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
Astrophysical Journal, 2012, v. 753 n. 2 How to Cite?
AbstractThe Cygnus region is a very bright and complex portion of the TeV sky, host to unidentified sources and a diffuse excess with respect to conventional cosmic-ray propagation models. Two of the brightest TeV sources, MGRO J2019+37 and MGRO J2031+41, are analyzed using Milagro data with a new technique, and their emission is tested under two different spectral assumptions: a power law and a power law with an exponential cutoff. The new analysis technique is based on an energy estimator that uses the fraction of photomultiplier tubes in the observatory that detect the extensive air shower. The photon spectrum is measured in the range 1-100 TeV using the last three years of Milagro data (2005-2008), with the detector in its final configuration. An F-test indicates that MGRO J2019+37 is better fit by a power law with an exponential cutoff than by a simple power law. The best-fitting parameters for the power law with exponential cutoff model are a normalization at 10 TeV of 7 +5 -2 × 10 -10 s -1 m -2 TeV -1, a spectral index of 2.0 +0.5 -1.0, and a cutoff energy of 29 +50 -16 TeV. MGRO J2031+41 shows no evidence of a cutoff. The best-fitting parameters for a power law are a normalization of 2.1 +0.6 -0.6 × 10 -10 s -1 m -2 TeV -1 and a spectral index of 3.22 +0.23 -0.18. The overall flux is subject to a 30% systematic uncertainty. The systematic uncertainty on the power-law indices is 0.1. Both uncertainties have been verified with cosmic-ray data. A comparison with previous results from TeV J2032+4130, MGRO J2031+41, and MGRO J2019+37 is also presented. © 2012. The American Astronomical Society. All rights reserved..
Persistent Identifierhttp://hdl.handle.net/10722/188422
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorAbdo, AAen_US
dc.contributor.authorAbeysekara, Uen_US
dc.contributor.authorAllen, BTen_US
dc.contributor.authorAune, Ten_US
dc.contributor.authorBerley, Den_US
dc.contributor.authorBonamente, Een_US
dc.contributor.authorChristopher, GEen_US
dc.contributor.authorDeyoung, Ten_US
dc.contributor.authorDingus, BLen_US
dc.contributor.authorEllsworth, RWen_US
dc.contributor.authorGalbraithFrew, JGen_US
dc.contributor.authorGonzalez, MMen_US
dc.contributor.authorGoodman, JAen_US
dc.contributor.authorHoffman, CMen_US
dc.contributor.authorHüntemeyer, PHen_US
dc.contributor.authorHui, CMen_US
dc.contributor.authorKolterman, BEen_US
dc.contributor.authorLinnemann, JTen_US
dc.contributor.authorMcenery, JEen_US
dc.contributor.authorMincer, AIen_US
dc.contributor.authorMorgan, Ten_US
dc.contributor.authorNemethy, Pen_US
dc.contributor.authorPretz, Jen_US
dc.contributor.authorRyan, JMen_US
dc.contributor.authorSaz Parkinson, PMen_US
dc.contributor.authorShoup, Aen_US
dc.contributor.authorSinnis, Gen_US
dc.contributor.authorSmith, AJen_US
dc.contributor.authorVasileiou, Ven_US
dc.contributor.authorWalker, GPen_US
dc.contributor.authorWilliams, DAen_US
dc.contributor.authorYodh, GBen_US
dc.date.accessioned2013-09-03T04:05:45Z-
dc.date.available2013-09-03T04:05:45Z-
dc.date.issued2012en_US
dc.identifier.citationAstrophysical Journal, 2012, v. 753 n. 2en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/188422-
dc.description.abstractThe Cygnus region is a very bright and complex portion of the TeV sky, host to unidentified sources and a diffuse excess with respect to conventional cosmic-ray propagation models. Two of the brightest TeV sources, MGRO J2019+37 and MGRO J2031+41, are analyzed using Milagro data with a new technique, and their emission is tested under two different spectral assumptions: a power law and a power law with an exponential cutoff. The new analysis technique is based on an energy estimator that uses the fraction of photomultiplier tubes in the observatory that detect the extensive air shower. The photon spectrum is measured in the range 1-100 TeV using the last three years of Milagro data (2005-2008), with the detector in its final configuration. An F-test indicates that MGRO J2019+37 is better fit by a power law with an exponential cutoff than by a simple power law. The best-fitting parameters for the power law with exponential cutoff model are a normalization at 10 TeV of 7 +5 -2 × 10 -10 s -1 m -2 TeV -1, a spectral index of 2.0 +0.5 -1.0, and a cutoff energy of 29 +50 -16 TeV. MGRO J2031+41 shows no evidence of a cutoff. The best-fitting parameters for a power law are a normalization of 2.1 +0.6 -0.6 × 10 -10 s -1 m -2 TeV -1 and a spectral index of 3.22 +0.23 -0.18. The overall flux is subject to a 30% systematic uncertainty. The systematic uncertainty on the power-law indices is 0.1. Both uncertainties have been verified with cosmic-ray data. A comparison with previous results from TeV J2032+4130, MGRO J2031+41, and MGRO J2019+37 is also presented. © 2012. The American Astronomical Society. All rights reserved..en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/en_US
dc.relation.ispartofAstrophysical Journalen_US
dc.subjectAcceleration Of Particlesen_US
dc.subjectAstroparticle Physicsen_US
dc.subjectGamma Rays: Generalen_US
dc.subjectOpen Clusters And Associations: Individual (Cyg Ob1, Cyg Ob2)en_US
dc.subjectPulsars: Generalen_US
dc.titleSpectrum and morphology of the two brightest Milagro sources in the Cygnus region: MGRO J2019+37 and MGRO J2031+41en_US
dc.typeArticleen_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1088/0004-637X/753/2/159en_US
dc.identifier.scopuseid_2-s2.0-84862886706en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-84862886706&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume753en_US
dc.identifier.issue2en_US
dc.identifier.isiWOS:000305912700066-
dc.publisher.placeUnited Statesen_US
dc.identifier.scopusauthoridAbdo, AA=35228697200en_US
dc.identifier.scopusauthoridAbeysekara, U=35725286500en_US
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dc.identifier.scopusauthoridKolterman, BE=16177916700en_US
dc.identifier.scopusauthoridLinnemann, JT=35393070800en_US
dc.identifier.scopusauthoridMcEnery, JE=6603930996en_US
dc.identifier.scopusauthoridMincer, AI=35228697200en_US
dc.identifier.scopusauthoridMorgan, T=35725286500en_US
dc.identifier.scopusauthoridNemethy, P=36551088700en_US
dc.identifier.scopusauthoridPretz, J=25721802200en_US
dc.identifier.scopusauthoridRyan, JM=35236204300en_US
dc.identifier.scopusauthoridSaz Parkinson, PM=23017714200en_US
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dc.identifier.scopusauthoridSmith, AJ=35313328300en_US
dc.identifier.scopusauthoridVasileiou, V=7006640160en_US
dc.identifier.scopusauthoridWalker, GP=55191316200en_US
dc.identifier.scopusauthoridWilliams, DA=34770297100en_US
dc.identifier.scopusauthoridYodh, GB=7402289255en_US

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