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Article: Detection of the Small Magellanic Cloud in gamma-rays with Fermi /LAT

TitleDetection of the Small Magellanic Cloud in gamma-rays with Fermi /LAT
Authors
Abdo, AAAckermann, MAjello, MBaldini, LBallet, JBarbiellini, GBastieri, DBechtol, KBellazzini, RBerenji, BBlandford, RDNaumannGodo, MNolan, PLNorris, JPNuss, EOhsugi, TOkumura, AOmodei, NOrlando, EOrmes, JFPanetta, JHBloom, EDParent, DPelassa, VPepe, MPesceRollins, MPiron, FPorter, TARainò, SRando, RRazzano, MReimer, ABonamente, EReimer, OReposeur, TRipken, JRitz, SRomani, RWSadrozinski, HFWSander, ASaz Parkinson, PMScargle, JDSgrò, CBorgland, AWSiskind, EJSmith, DASmith, PDSpandre, GSpinelli, PStrickman, MSStrong, AWSuson, DJTakahashi, HTakahashi, TBouvier, ATanaka, TThayer, JBThayer, JGThompson, DJTibaldo, LTorres, DFTosti, GTramacere, AUchiyama, YUsher, TLBrandt, TJVandenbroucke, JVasileiou, VVilchez, NVitale, VWaite, APWang, PWiner, BLWood, KSYang, ZYlinen, TBregeon, JZiegler, MBrez, ABrigida, MBruel, PBuehler, RBuson, SCaliandro, GACameron, RACaraveo, PACarrigan, SCasandjian, JMCecchi, CÇelik, ÖCharles, EChekhtman, ACheung, CCChiang, JCiprini, SClaus, RCohenTanugi, JConrad, JDermer, CDDe Palma, FDigel, SWDo Couto E Silva, EDrell, PSDubois, RDumora, DFavuzzi, CFegan, SJFukazawa, YFunk, SFusco, PGargano, FGasparrini, DGehrels, NGermani, SGiglietto, NGiordano, FGiroletti, MGlanzman, TGodfrey, GGrenier, IAGrondin, MHGrove, JEGuiriec, SHadasch, DHarding, AKHayashida, MHays, EHoran, DHughes, REJean, PJóhannesson, GJohnson, ASJohnson, WNKamae, TKatagiri, HKataoka, JKerr, MKnödlseder, JKuss, MLande, JLatronico, LLee, SHLemoineGoumard, MLlena Garde, MLongo, FLoparco, FLovellette, MNLubrano, PMakeev, AMartin, PMazziotta, MNMcenery, JEMichelson, PFMitthumsiri, WMizuno, TMonte, CMonzani, MEMorselli, AMoskalenko, IVMurgia, SNakamori, T
KeywordsAcceleration Of Particles
Cosmic Rays
Gamma Rays: General
Magellanic Clouds
Issue Date2010
PublisherEDP Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy And Astrophysics, 2010, v. 523 n. 3 How to Cite?
AbstractContext. The flux of gamma rays with energies greater than 100 MeV is dominated by diffuse emission coming from cosmic-rays (CRs) illuminating the interstellar medium (ISM) of our Galaxy through the processes of Bremsstrahlung, pion production and decay, and inverse-Compton scattering. The study of this diffuse emission provides insight into the origin and transport of cosmic rays. Aims.We searched for gamma-ray emission from the Small Magellanic Cloud (SMC) in order to derive constraints on the cosmic-ray population and transport in an external system with properties different from the Milky Way. Methods.We analysed the first 17 months of continuous all-sky observations by the Large Area Telescope (LAT) of the Fermi mission to determine the spatial distribution, flux and spectrum of the gamma-ray emission from the SMC. We also used past radio synchrotron observations of the SMC to study the population of CR electrons specifically. Results.We obtained the first detection of the SMC in high-energy gamma rays, with an integrated >100MeV flux of (3.7±0.7)×10-8 ph cm-2 s-1, with additional systematic uncertainty of ≤16%. The emission is steady and from an extended source ∼3. in size. It is not clearly correlated with the distribution of massive stars or neutral gas, nor with known pulsars or supernova remnants, but a certain correlation with supergiant shells is observed. Conclusions.The observed flux implies an upper limit on the average CR nuclei density in the SMC of ∼15% of the value measured locally in the Milky Way. The population of high-energy pulsars of the SMC may account for a substantial fraction of the gamma-ray flux, which would make the inferred CR nuclei density even lower. The average density of CR electrons derived from radio synchrotron observations is consistent with the same reduction factor but the uncertainties are large. From our current knowledge of the SMC, such a low CR density does not seem to be due to a lower rate of CR injection and rather indicates a smaller CR confinement volume characteristic size. © 2010 ESO.
Persistent Identifierhttp://hdl.handle.net/10722/188401
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446
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.authorBastieri, Den_US
dc.contributor.authorBechtol, Ken_US
dc.contributor.authorBellazzini, Ren_US
dc.contributor.authorBerenji, Ben_US
dc.contributor.authorBlandford, RDen_US
dc.contributor.authorNaumannGodo, Men_US
dc.contributor.authorNolan, PLen_US
dc.contributor.authorNorris, JPen_US
dc.contributor.authorNuss, Een_US
dc.contributor.authorOhsugi, Ten_US
dc.contributor.authorOkumura, Aen_US
dc.contributor.authorOmodei, Nen_US
dc.contributor.authorOrlando, Een_US
dc.contributor.authorOrmes, JFen_US
dc.contributor.authorPanetta, JHen_US
dc.contributor.authorBloom, EDen_US
dc.contributor.authorParent, Den_US
dc.contributor.authorPelassa, Ven_US
dc.contributor.authorPepe, Men_US
dc.contributor.authorPesceRollins, Men_US
dc.contributor.authorPiron, Fen_US
dc.contributor.authorPorter, TAen_US
dc.contributor.authorRainò, Sen_US
dc.contributor.authorRando, Ren_US
dc.contributor.authorRazzano, Men_US
dc.contributor.authorReimer, Aen_US
dc.contributor.authorBonamente, Een_US
dc.contributor.authorReimer, Oen_US
dc.contributor.authorReposeur, Ten_US
dc.contributor.authorRipken, Jen_US
dc.contributor.authorRitz, Sen_US
dc.contributor.authorRomani, RWen_US
dc.contributor.authorSadrozinski, HFWen_US
dc.contributor.authorSander, Aen_US
dc.contributor.authorSaz Parkinson, PMen_US
dc.contributor.authorScargle, JDen_US
dc.contributor.authorSgrò, Cen_US
dc.contributor.authorBorgland, AWen_US
dc.contributor.authorSiskind, EJen_US
dc.contributor.authorSmith, DAen_US
dc.contributor.authorSmith, PDen_US
dc.contributor.authorSpandre, Gen_US
dc.contributor.authorSpinelli, Pen_US
dc.contributor.authorStrickman, MSen_US
dc.contributor.authorStrong, AWen_US
dc.contributor.authorSuson, DJen_US
dc.contributor.authorTakahashi, Hen_US
dc.contributor.authorTakahashi, Ten_US
dc.contributor.authorBouvier, Aen_US
dc.contributor.authorTanaka, Ten_US
dc.contributor.authorThayer, JBen_US
dc.contributor.authorThayer, JGen_US
dc.contributor.authorThompson, DJen_US
dc.contributor.authorTibaldo, Len_US
dc.contributor.authorTorres, DFen_US
dc.contributor.authorTosti, Gen_US
dc.contributor.authorTramacere, Aen_US
dc.contributor.authorUchiyama, Yen_US
dc.contributor.authorUsher, TLen_US
dc.contributor.authorBrandt, TJen_US
dc.contributor.authorVandenbroucke, Jen_US
dc.contributor.authorVasileiou, Ven_US
dc.contributor.authorVilchez, Nen_US
dc.contributor.authorVitale, Ven_US
dc.contributor.authorWaite, APen_US
dc.contributor.authorWang, Pen_US
dc.contributor.authorWiner, BLen_US
dc.contributor.authorWood, KSen_US
dc.contributor.authorYang, Zen_US
dc.contributor.authorYlinen, Ten_US
dc.contributor.authorBregeon, Jen_US
dc.contributor.authorZiegler, Men_US
dc.contributor.authorBrez, Aen_US
dc.contributor.authorBrigida, Men_US
dc.contributor.authorBruel, Pen_US
dc.contributor.authorBuehler, Ren_US
dc.contributor.authorBuson, Sen_US
dc.contributor.authorCaliandro, GAen_US
dc.contributor.authorCameron, RAen_US
dc.contributor.authorCaraveo, PAen_US
dc.contributor.authorCarrigan, Sen_US
dc.contributor.authorCasandjian, JMen_US
dc.contributor.authorCecchi, Cen_US
dc.contributor.authorÇelik, Öen_US
dc.contributor.authorCharles, Een_US
dc.contributor.authorChekhtman, Aen_US
dc.contributor.authorCheung, CCen_US
dc.contributor.authorChiang, Jen_US
dc.contributor.authorCiprini, Sen_US
dc.contributor.authorClaus, Ren_US
dc.contributor.authorCohenTanugi, Jen_US
dc.contributor.authorConrad, Jen_US
dc.contributor.authorDermer, CDen_US
dc.contributor.authorDe Palma, Fen_US
dc.contributor.authorDigel, SWen_US
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.authorFavuzzi, Cen_US
dc.contributor.authorFegan, SJen_US
dc.contributor.authorFukazawa, Yen_US
dc.contributor.authorFunk, Sen_US
dc.contributor.authorFusco, Pen_US
dc.contributor.authorGargano, Fen_US
dc.contributor.authorGasparrini, Den_US
dc.contributor.authorGehrels, Nen_US
dc.contributor.authorGermani, Sen_US
dc.contributor.authorGiglietto, Nen_US
dc.contributor.authorGiordano, Fen_US
dc.contributor.authorGiroletti, Men_US
dc.contributor.authorGlanzman, Ten_US
dc.contributor.authorGodfrey, Gen_US
dc.contributor.authorGrenier, IAen_US
dc.contributor.authorGrondin, MHen_US
dc.contributor.authorGrove, JEen_US
dc.contributor.authorGuiriec, Sen_US
dc.contributor.authorHadasch, Den_US
dc.contributor.authorHarding, AKen_US
dc.contributor.authorHayashida, Men_US
dc.contributor.authorHays, Een_US
dc.contributor.authorHoran, Den_US
dc.contributor.authorHughes, REen_US
dc.contributor.authorJean, Pen_US
dc.contributor.authorJóhannesson, Gen_US
dc.contributor.authorJohnson, ASen_US
dc.contributor.authorJohnson, WNen_US
dc.contributor.authorKamae, Ten_US
dc.contributor.authorKatagiri, Hen_US
dc.contributor.authorKataoka, Jen_US
dc.contributor.authorKerr, Men_US
dc.contributor.authorKnödlseder, Jen_US
dc.contributor.authorKuss, Men_US
dc.contributor.authorLande, Jen_US
dc.contributor.authorLatronico, Len_US
dc.contributor.authorLee, SHen_US
dc.contributor.authorLemoineGoumard, Men_US
dc.contributor.authorLlena Garde, Men_US
dc.contributor.authorLongo, Fen_US
dc.contributor.authorLoparco, Fen_US
dc.contributor.authorLovellette, MNen_US
dc.contributor.authorLubrano, Pen_US
dc.contributor.authorMakeev, Aen_US
dc.contributor.authorMartin, Pen_US
dc.contributor.authorMazziotta, MNen_US
dc.contributor.authorMcenery, JEen_US
dc.contributor.authorMichelson, PFen_US
dc.contributor.authorMitthumsiri, Wen_US
dc.contributor.authorMizuno, Ten_US
dc.contributor.authorMonte, Cen_US
dc.contributor.authorMonzani, MEen_US
dc.contributor.authorMorselli, Aen_US
dc.contributor.authorMoskalenko, IVen_US
dc.contributor.authorMurgia, Sen_US
dc.contributor.authorNakamori, Ten_US
dc.date.accessioned2013-09-03T04:05:23Z-
dc.date.available2013-09-03T04:05:23Z-
dc.date.issued2010en_US
dc.identifier.citationAstronomy And Astrophysics, 2010, v. 523 n. 3en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/10722/188401-
dc.description.abstractContext. The flux of gamma rays with energies greater than 100 MeV is dominated by diffuse emission coming from cosmic-rays (CRs) illuminating the interstellar medium (ISM) of our Galaxy through the processes of Bremsstrahlung, pion production and decay, and inverse-Compton scattering. The study of this diffuse emission provides insight into the origin and transport of cosmic rays. Aims.We searched for gamma-ray emission from the Small Magellanic Cloud (SMC) in order to derive constraints on the cosmic-ray population and transport in an external system with properties different from the Milky Way. Methods.We analysed the first 17 months of continuous all-sky observations by the Large Area Telescope (LAT) of the Fermi mission to determine the spatial distribution, flux and spectrum of the gamma-ray emission from the SMC. We also used past radio synchrotron observations of the SMC to study the population of CR electrons specifically. Results.We obtained the first detection of the SMC in high-energy gamma rays, with an integrated >100MeV flux of (3.7±0.7)×10-8 ph cm-2 s-1, with additional systematic uncertainty of ≤16%. The emission is steady and from an extended source ∼3. in size. It is not clearly correlated with the distribution of massive stars or neutral gas, nor with known pulsars or supernova remnants, but a certain correlation with supergiant shells is observed. Conclusions.The observed flux implies an upper limit on the average CR nuclei density in the SMC of ∼15% of the value measured locally in the Milky Way. The population of high-energy pulsars of the SMC may account for a substantial fraction of the gamma-ray flux, which would make the inferred CR nuclei density even lower. The average density of CR electrons derived from radio synchrotron observations is consistent with the same reduction factor but the uncertainties are large. From our current knowledge of the SMC, such a low CR density does not seem to be due to a lower rate of CR injection and rather indicates a smaller CR confinement volume characteristic size. © 2010 ESO.en_US
dc.languageengen_US
dc.publisherEDP Sciences. The Journal's web site is located at http://www.aanda.orgen_US
dc.relation.ispartofAstronomy and Astrophysicsen_US
dc.subjectAcceleration Of Particlesen_US
dc.subjectCosmic Raysen_US
dc.subjectGamma Rays: Generalen_US
dc.subjectMagellanic Cloudsen_US
dc.titleDetection of the Small Magellanic Cloud in gamma-rays with Fermi /LATen_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.doi10.1051/0004-6361/201014855en_US
dc.identifier.scopuseid_2-s2.0-78449261568en_US
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dc.identifier.volume523en_US
dc.identifier.issue3en_US
dc.identifier.isiWOS:000285346600050-
dc.publisher.placeFranceen_US
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dc.identifier.scopusauthoridLoparco, F=7202709535en_US
dc.identifier.scopusauthoridLovellette, MN=35274970000en_US
dc.identifier.scopusauthoridLubrano, P=35229539600en_US
dc.identifier.scopusauthoridMakeev, A=26655530300en_US
dc.identifier.scopusauthoridMartin, P=34975071100en_US
dc.identifier.scopusauthoridMazziotta, MN=7102598972en_US
dc.identifier.scopusauthoridMcEnery, JE=25724434100en_US
dc.identifier.scopusauthoridMichelson, PF=7410011980en_US
dc.identifier.scopusauthoridMitthumsiri, W=7404848681en_US
dc.identifier.scopusauthoridMizuno, T=35353364200en_US
dc.identifier.scopusauthoridMonte, C=35229502100en_US
dc.identifier.scopusauthoridMonzani, ME=25637485000en_US
dc.identifier.scopusauthoridMorselli, A=35229880000en_US
dc.identifier.scopusauthoridMoskalenko, IV=8954352500en_US
dc.identifier.scopusauthoridMurgia, S=15755916900en_US
dc.identifier.scopusauthoridNakamori, T=26425112800en_US

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