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Article: Recent results from the Milagro gamma ray observatory

TitleRecent results from the Milagro gamma ray observatory
Authors
Issue Date2006
PublisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/npbps
Citation
Nuclear Physics B - Proceedings Supplements, 2006, v. 151 n. 1, p. 101-107 How to Cite?
AbstractThe Milagro gamma-ray observatory utilizes a large water Cherenkov detector to observe TeV extensive air showers produced by high energy particles impacting the Earth's atmosphere. Milagro is different from Atmospheric Cherenkov Telescopes that are used to study TeV gamma-rays in that it views a wide field (2 steradian over-head sky) and it continuously operates (>90% live time). These factors give Milagro the potential for discovery of new sources with unknown positions and times, such as gamma-ray bursts, flaring AGN, and observation of diffuse extended sources like the Galactic plane or large supernova remnants. The Milagro detector consists of a 4800 m2 pond instrumented with 723 8" PMTs which detect Cherenkov light produced by secondary air-shower particles. A sparse array of 175 4000l water tanks surrounding the central pond detector has recently been added which will extend the physical area of Milagro to 40,000 m2 and substantially increase the sensitivity of the instrument. Based on three years of operation, Milagro has established its sensitivity through the detection of the Crab plerion and active galaxy Markarian 421. A summary of the recent results from the Milagro collaboration is presented with a focus on the first observation of the galactic plane in the TeV range and evidence for two newly observed TeV sources: diffuse emission from the Cygnus Region, and evidence for an extended TeV hot spot near the EGRET unidentified 3EG J0520+2556. © 2005 Published by Elsevier B.V.
Persistent Identifierhttp://hdl.handle.net/10722/188355
ISSN
2005 Impact Factor: 0.875
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorGoodman, JAen_US
dc.contributor.authorAtkins, Ren_US
dc.contributor.authorBenbow, Wen_US
dc.contributor.authorBerley, Den_US
dc.contributor.authorBlaufuss, Een_US
dc.contributor.authorCoyne, DGen_US
dc.contributor.authorDeyoung, Ten_US
dc.contributor.authorDingus, BLen_US
dc.contributor.authorDorfan, DEen_US
dc.contributor.authorEllsworth, RWen_US
dc.contributor.authorFleysher, Len_US
dc.contributor.authorFleysher, Ren_US
dc.contributor.authorGonzalez, MMen_US
dc.contributor.authorGoodman, JAen_US
dc.contributor.authorHaines, TJen_US
dc.contributor.authorHays, Een_US
dc.contributor.authorHoffman, CMen_US
dc.contributor.authorKelley, LAen_US
dc.contributor.authorLansdell, CPen_US
dc.contributor.authorLinnemann, JTen_US
dc.contributor.authorMcenery, JEen_US
dc.contributor.authorMiller, RSen_US
dc.contributor.authorMincer, AIen_US
dc.contributor.authorMorales, MFen_US
dc.contributor.authorNemethy, Pen_US
dc.contributor.authorNoyes, Den_US
dc.contributor.authorRyan, JMen_US
dc.contributor.authorSamuelson, FWen_US
dc.contributor.authorSaz Parkinson, PMen_US
dc.contributor.authorShoup, Aen_US
dc.contributor.authorSinnis, Gen_US
dc.contributor.authorSmith, AJen_US
dc.contributor.authorSullivan, GWen_US
dc.date.accessioned2013-09-03T04:03:36Z-
dc.date.available2013-09-03T04:03:36Z-
dc.date.issued2006en_US
dc.identifier.citationNuclear Physics B - Proceedings Supplements, 2006, v. 151 n. 1, p. 101-107en_US
dc.identifier.issn0920-5632en_US
dc.identifier.urihttp://hdl.handle.net/10722/188355-
dc.description.abstractThe Milagro gamma-ray observatory utilizes a large water Cherenkov detector to observe TeV extensive air showers produced by high energy particles impacting the Earth's atmosphere. Milagro is different from Atmospheric Cherenkov Telescopes that are used to study TeV gamma-rays in that it views a wide field (2 steradian over-head sky) and it continuously operates (>90% live time). These factors give Milagro the potential for discovery of new sources with unknown positions and times, such as gamma-ray bursts, flaring AGN, and observation of diffuse extended sources like the Galactic plane or large supernova remnants. The Milagro detector consists of a 4800 m2 pond instrumented with 723 8" PMTs which detect Cherenkov light produced by secondary air-shower particles. A sparse array of 175 4000l water tanks surrounding the central pond detector has recently been added which will extend the physical area of Milagro to 40,000 m2 and substantially increase the sensitivity of the instrument. Based on three years of operation, Milagro has established its sensitivity through the detection of the Crab plerion and active galaxy Markarian 421. A summary of the recent results from the Milagro collaboration is presented with a focus on the first observation of the galactic plane in the TeV range and evidence for two newly observed TeV sources: diffuse emission from the Cygnus Region, and evidence for an extended TeV hot spot near the EGRET unidentified 3EG J0520+2556. © 2005 Published by Elsevier B.V.en_US
dc.languageengen_US
dc.publisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/npbpsen_US
dc.relation.ispartofNuclear Physics B - Proceedings Supplementsen_US
dc.titleRecent results from the Milagro gamma ray observatoryen_US
dc.typeArticleen_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1016/j.nuclphysbps.2005.07.018en_US
dc.identifier.scopuseid_2-s2.0-29644445243en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-29644445243&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume151en_US
dc.identifier.issue1en_US
dc.identifier.spage101en_US
dc.identifier.epage107en_US
dc.identifier.isiWOS:000235018800018-
dc.publisher.placeNetherlandsen_US
dc.identifier.scopusauthoridGoodman, JA=7402289255en_US
dc.identifier.scopusauthoridAtkins, R=7203037191en_US
dc.identifier.scopusauthoridBenbow, W=8251232000en_US
dc.identifier.scopusauthoridBerley, D=35236204300en_US
dc.identifier.scopusauthoridBlaufuss, E=35236361600en_US
dc.identifier.scopusauthoridCoyne, DG=7005444095en_US
dc.identifier.scopusauthoridDeYoung, T=35236784600en_US
dc.identifier.scopusauthoridDingus, BL=35313328300en_US
dc.identifier.scopusauthoridDorfan, DE=22983036300en_US
dc.identifier.scopusauthoridEllsworth, RW=7006640160en_US
dc.identifier.scopusauthoridFleysher, L=6603281083en_US
dc.identifier.scopusauthoridFleysher, R=6603340002en_US
dc.identifier.scopusauthoridGonzalez, MM=34770297100en_US
dc.identifier.scopusauthoridGoodman, JA=36606060100en_US
dc.identifier.scopusauthoridHaines, TJ=7006714318en_US
dc.identifier.scopusauthoridHays, E=35229539600en_US
dc.identifier.scopusauthoridHoffman, CM=7201824911en_US
dc.identifier.scopusauthoridKelley, LA=7102318127en_US
dc.identifier.scopusauthoridLansdell, CP=38561715700en_US
dc.identifier.scopusauthoridLinnemann, JT=35227605400en_US
dc.identifier.scopusauthoridMcEnery, JE=35230627000en_US
dc.identifier.scopusauthoridMiller, RS=55687153300en_US
dc.identifier.scopusauthoridMincer, AI=35227629900en_US
dc.identifier.scopusauthoridMorales, MF=7202590454en_US
dc.identifier.scopusauthoridNemethy, P=8413896200en_US
dc.identifier.scopusauthoridNoyes, D=7004488400en_US
dc.identifier.scopusauthoridRyan, JM=35459577200en_US
dc.identifier.scopusauthoridSamuelson, FW=6601957830en_US
dc.identifier.scopusauthoridSaz Parkinson, PM=35227979600en_US
dc.identifier.scopusauthoridShoup, A=35228129300en_US
dc.identifier.scopusauthoridSinnis, G=7402289255en_US
dc.identifier.scopusauthoridSmith, AJ=7203037191en_US
dc.identifier.scopusauthoridSullivan, GW=8251232000en_US

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