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Article: Fermi lat discovery of extended gamma-ray emission in the direction of supernova remnant W51C

TitleFermi lat discovery of extended gamma-ray emission in the direction of supernova remnant W51C
Authors
Abdo, AAAckermann, MAjello, MBaldini, LBallet, JBarbiellini, GBaring, MGBastieri, DBaughman, BMBechtol, KBellazzini, RMcenery, JEMeurer, CMichelson, PFMitthumsiri, WMizuno, TMoiseev, AAMonte, CMonzani, MEMorselli, AMoskalenko, IVBerenji, BMurgia, SNakamori, TNolan, PLNorris, JPNuss, EOhsugi, TOkumura, AOmodei, NOrlando, EOrmes, JFBlandford, RDPaneque, DParent, DPelassa, VPepe, MPesceRollins, MPiron, FPorter, TARainò, SRando, RRazzano, MBloom, EDReimer, AReimer, OReposeur, TRitz, SRodriguez, AYRomani, RWRoth, MRyde, FSadrozinski, HFWSanchez, DBonamente, ESander, ASaz Parkinson, PMScargle, JDSchalk, TLSgrò, CSiskind, EJSmith, DASmith, PDSpandre, GSpinelli, PBorgland, AWStrickman, MSSuson, DJTajima, HTakahashi, HTakahashi, TTanaka, TThayer, JBThayer, JGThompson, DJTibaldo, LBouvier, ATibolla, OTorres, DFTosti, GTramacere, AUchiyama, YUsher, TLVasileiou, VVenter, CVilchez, NVitale, VBregeon, JWaite, APWang, PWiner, BLWood, KSYamazaki, RYlinen, TZiegler, MBrez, ABrigida, MBruel, PBurnett, THBuson, SCaliandro, GACameron, RACaraveo, PACasandjian, JMCecchi, CÇelik, ÖChekhtman, ACheung, CCChiang, JCiprini, SClaus, RCohenTanugi, JCominsky, LRConrad, JCutini, SDermer, CDDe Angelis, ADe Palma, FDigel, SWDormody, MDo Couto E Silva, EDrell, PSDubois, RDumora, DFarnier, CFavuzzi, CFegan, SJFocke, WBFortin, PFrailis, MFukazawa, YFunk, SFusco, PGargano, FGasparrini, DGehrels, NGermani, SGiavitto, GGiebels, BGiglietto, NGiordano, FGlanzman, TGodfrey, GGrenier, IAGrondin, MHGrove, JEGuillemot, LGuiriec, SHanabata, YHarding, AKHayashida, MHays, EHughes, REJackson, MSJóhannesson, GJohnson, ASJohnson, TJJohnson, WNKamae, TKatagiri, HKataoka, JKatsuta, JKawai, NKerr, MKnödlseder, JKocian, MLKuss, MLande, JLatronico, LLemoineGoumard, MLongo, FLoparco, FLott, BLovellette, MNLubrano, PMakeev, AMazziotta, MN
KeywordsAcceleration Of Particles
Ism: Individual (W51c)
Radiation Mechanisms: Non-Thermal
Issue Date2009
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2009, v. 706 n. 1 PART 2, p. L1-L6 How to Cite?
AbstractThe discovery of bright gamma-ray emission coincident with supernova remnant (SNR) W51C is reported using the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope. W51C is a middle-aged remnant (104 yr) ∼ with intense radio synchrotron emission in its shell and known to be interacting with a molecular cloud. The gamma-ray emission is spatially extended, broadly consistent with the radio and X-ray extent of SNR W51C. The energy spectrum in the 0.2-50 GeV band exhibits steepening toward high energies. The luminosity is greater than 1 × 1036 erg s-1 given the distance constraint of D > 5.5 kpc, which makes this object one of the most luminous gamma-ray sources in our Galaxy. The observed gamma-rays can be explained reasonably by a combination of efficient acceleration of nuclear cosmic rays at supernova shocks and shock-cloud interactions. The decay of neutral π mesons produced in hadronic collisions provides a plausible explanation for the gamma-ray emission. The product of the average gas density and the total energy content of the accelerated protons amounts to ̄n H Wp ≃ 5× 1051 (D/6kpc)2 erg cm-2. Electron density constraints from the radio and X-ray bands render it difficult to explain the LAT signal as due to inverse Compton scattering. The Fermi LAT source coincident with SNR W51C sheds new light on the origin of Galactic cosmic rays. © 2009. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/188382
ISSN
2023 Impact Factor: 8.8
2023 SCImago Journal Rankings: 2.766
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorAbdo, AAen_US
dc.contributor.authorAckermann, Men_US
dc.contributor.authorAjello, Men_US
dc.contributor.authorBaldini, Len_US
dc.contributor.authorBallet, Jen_US
dc.contributor.authorBarbiellini, Gen_US
dc.contributor.authorBaring, MGen_US
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dc.contributor.authorBaughman, BMen_US
dc.contributor.authorBechtol, Ken_US
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dc.contributor.authorDe Angelis, Aen_US
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dc.contributor.authorDo Couto E Silva, Een_US
dc.contributor.authorDrell, PSen_US
dc.contributor.authorDubois, Ren_US
dc.contributor.authorDumora, Den_US
dc.contributor.authorFarnier, Cen_US
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dc.contributor.authorFegan, SJen_US
dc.contributor.authorFocke, WBen_US
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dc.contributor.authorHanabata, Yen_US
dc.contributor.authorHarding, AKen_US
dc.contributor.authorHayashida, Men_US
dc.contributor.authorHays, Een_US
dc.contributor.authorHughes, REen_US
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dc.contributor.authorKatsuta, Jen_US
dc.contributor.authorKawai, Nen_US
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dc.contributor.authorKnödlseder, Jen_US
dc.contributor.authorKocian, MLen_US
dc.contributor.authorKuss, Men_US
dc.contributor.authorLande, Jen_US
dc.contributor.authorLatronico, Len_US
dc.contributor.authorLemoineGoumard, Men_US
dc.contributor.authorLongo, Fen_US
dc.contributor.authorLoparco, Fen_US
dc.contributor.authorLott, Ben_US
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dc.date.accessioned2013-09-03T04:04:38Z-
dc.date.available2013-09-03T04:04:38Z-
dc.date.issued2009en_US
dc.identifier.citationAstrophysical Journal Letters, 2009, v. 706 n. 1 PART 2, p. L1-L6en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/188382-
dc.description.abstractThe discovery of bright gamma-ray emission coincident with supernova remnant (SNR) W51C is reported using the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope. W51C is a middle-aged remnant (104 yr) ∼ with intense radio synchrotron emission in its shell and known to be interacting with a molecular cloud. The gamma-ray emission is spatially extended, broadly consistent with the radio and X-ray extent of SNR W51C. The energy spectrum in the 0.2-50 GeV band exhibits steepening toward high energies. The luminosity is greater than 1 × 1036 erg s-1 given the distance constraint of D > 5.5 kpc, which makes this object one of the most luminous gamma-ray sources in our Galaxy. The observed gamma-rays can be explained reasonably by a combination of efficient acceleration of nuclear cosmic rays at supernova shocks and shock-cloud interactions. The decay of neutral π mesons produced in hadronic collisions provides a plausible explanation for the gamma-ray emission. The product of the average gas density and the total energy content of the accelerated protons amounts to ̄n H Wp ≃ 5× 1051 (D/6kpc)2 erg cm-2. Electron density constraints from the radio and X-ray bands render it difficult to explain the LAT signal as due to inverse Compton scattering. The Fermi LAT source coincident with SNR W51C sheds new light on the origin of Galactic cosmic rays. © 2009. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectAcceleration Of Particlesen_US
dc.subjectIsm: Individual (W51c)en_US
dc.subjectRadiation Mechanisms: Non-Thermalen_US
dc.titleFermi lat discovery of extended gamma-ray emission in the direction of supernova remnant W51Cen_US
dc.typeArticleen_US
dc.identifier.emailSaz Parkinson, PM: pablosp@hku.hken_US
dc.identifier.authoritySaz Parkinson, PM=rp01803en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1088/0004-637X/706/1/L1en_US
dc.identifier.scopuseid_2-s2.0-77749266344en_US
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dc.identifier.volume706en_US
dc.identifier.issue1 PART 2en_US
dc.identifier.spageL1en_US
dc.identifier.epageL6en_US
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dc.publisher.placeUnited Kingdomen_US
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dc.identifier.scopusauthoridGiordano, F=7004517682en_US
dc.identifier.scopusauthoridGlanzman, T=13807358800en_US
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dc.identifier.scopusauthoridGuillemot, L=23018720400en_US
dc.identifier.scopusauthoridGuiriec, S=7004622879en_US
dc.identifier.scopusauthoridHanabata, Y=34879626400en_US
dc.identifier.scopusauthoridHarding, AK=7003889095en_US
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dc.identifier.scopusauthoridHays, E=6506341877en_US
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dc.identifier.scopusauthoridJohnson, AS=9332400800en_US
dc.identifier.scopusauthoridJohnson, TJ=25031350300en_US
dc.identifier.scopusauthoridJohnson, WN=35353135800en_US
dc.identifier.scopusauthoridKamae, T=22979302300en_US
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dc.identifier.scopusauthoridLubrano, P=34975071100en_US
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dc.identifier.scopusauthoridMazziotta, MN=25724434100en_US
dc.identifier.issnl2041-8205-

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