FERMI-LAT OBSERVATIONS OF THE GEMINGA PULSAR
| Title: | FERMI-LAT OBSERVATIONS OF THE GEMINGA PULSAR |
|---|---|
| Authors: | ABDO AA; ACKERMANN M; AJELLO M; BALDINI L; BALLET J; BARBIELLINI G; BAUGHMAN BM; BECHTOL K; BELLAZZINI R; BERENJI B; BIGNAMI GF; BLANDFORD RD; BLOOM ED; BONAMENTE E; BORGLAND AW; BREGEON J; BREZ A; BRIGIDA M; BRUELI P; BURNETT TH; CALIANDRO GA; CAMERON RA; CARAVEO PA; CASANDJIAN JM; CECCHI C; CELIK O; CHARLES E; CHEKHTMAN A; CHEUNG CC; CHIANG J; CIPRINI S; CLAUS R; COHEN TANUGI J; CONRAD J; DERMER CD; DE PALMA F; DORMODY M; DOCOUTO SILVA E; DRELL PS; DUBOIS R; DUMORA D; EDMONDS Y; FARNIER C; FAVUZZI C; FEGAN SJ; FOCKE WB; FORTIN P; FRAILIS M; FURAZAWA Y; FUNK S; FUSCO P; GARGANO F; GASPARRINI D; GEHRELS N; GERMANI S; GIAVITTO G; GIGLIETTO N; GIORDANO F; GLANZMAN T; GODFREY G; GRENIER IA; GRONDIN MH; GROVE JE; GUILLEMOT L; GUIRIEC S; HADASCH D; HARDINO AK; HAYS E; HUGHES RE; JOHANNESSON G; JOHNSON AS; JOHNSON TJ; JOHNSON WN; KAMAE T; KATAGIRI H; KATAOKA J; KAWAI N; KERR M; KNODLSEDER J; KUSS M; LANDE J; LATRONICO L; LEMOINE GOUMARD M; LONGO F; LOPARCO F; LOTT B; LOVELLETTE MN; LUBRANO P; MAKEEV A; MARELLI M; MAZZIOTTA MN; MCENERY JE; MEURER C; MICHELSON PF; MITTHUMSIRI W; MIZUNO T; MOISEEV AA; MONTE C; MONZANI ME; MORSELLI A; MOSKALENK IV; MURGIA S; NOLAN PL; NORRIS JP; NUSS E; OHSUGI T; OMODEI N; ORLANDO E; ORMES JF; OZAKI M; PANEQUE D; PANETTA JH; PARENT D; PELASSA V; PEPE M; PESCE ROLLINS M; PIRON F; PORTER TA; RAINO S; RAYI PS; RAZZANO M; REIMER A; REIMER O; REPOSEUR T; ROCHESTER LS; RODRIGUEZ AY; ROMANI RW; ROTH M; RYDE F; SADROZINSKI HFW; SANDER A; SAZ PARKINSON PM; SCARGLE JD; SGRO C; SISKIND EJ; SMITH DA; SMITH PD; SPANDRE G; SPINELLI P; STRICKMAN MS; SUSON DJ; TAKAHASHI H; TAKAHASHI T; TANAKA T; THAYER JB; THAYER JG; THOMPSON DJ; TORRES DF; TOSTI G; TRAMACERE A; USHER TL; VAN ETTEN A; VASILEIOU V; VENTER C; VILCHEZ N; VITALE V; WAITE AP; WANG P; WATTERS K; WINER BL; WOOD KS; YLINEN T; ZIEGLER M.; BASTIERI, DENIS; RANDO, RICCARDO; TIBALDO, LUIGI |
| Contributors: | Abdo, Aa; Ackermann, M; Ajello, M; Baldini, L; Ballet, J; Barbiellini, G; Bastieri, Deni; Baughman, Bm; Bechtol, K; Bellazzini, R; Berenji, B; Bignami, Gf; Blandford, Rd; Bloom, Ed; Bonamente, E; Borgland, Aw; Bregeon, J; Brez, A; Brigida, M; Brueli, P; Burnett, Th; Caliandro, Ga; Cameron, Ra; Caraveo, Pa; Casandjian, Jm; Cecchi, C; Celik, O; Charles, E; Chekhtman, A; Cheung, Cc; Chiang, J; Ciprini, S; Claus, R; COHEN TANUGI, J; Conrad, J; Dermer, Cd; DE PALMA, F; Dormody, M; DOCOUTO SILVA, E; Drell, P; Dubois, R; Dumora, D; Edmonds, Y; Farnier, C; Favuzzi, C; Fegan, Sj; Focke, Wb; Fortin, P; Frailis, M; Furazawa, Y; Funk, S; Fusco, P; Gargano, F; Gasparrini, D; Gehrels, N; Germani, S; Giavitto, G; Giglietto, N; Giordano, F; Glanzman, T; Godfrey, G; Grenier, Ia; Grondin, Mh; Grove, Je; Guillemot, L; Guiriec, S; Hadasch, D; Hardino, Ak; Hays, E; Hughes, Re; Johannesson, G; Johnson, A; Johnson, Tj; Johnson, Wn; Kamae, T; Katagiri, H; Kataoka, J; Kawai, N; Kerr, M; Knodlseder, J; Kuss, M; Lande, J; Latronico, L; LEMOINE GOUMARD, M; Longo, F; Loparco, F; Lott, B; Lovellette, Mn; Lubrano, P; Makeev, A; Marelli, M; Mazziotta, Mn; Mcenery, Je; Meurer, C; Michelson, Pf; Mitthumsiri, W; Mizuno, T; Moiseev, Aa; Monte, C; Monzani, Me |
| Publication Year: | 2010 |
| Collection: | Padua Research Archive (IRIS - Università degli Studi di Padova) |
| Description: | We report on the Fermi-LAT observations of the Geminga pulsar, the second brightest non-variable GeV source in the γ-ray sky and the first example of a radio-quiet γ-ray pulsar. The observations cover one year, from the launch of the Fermi satellite through 2009 June 15. A data sample of over 60,000 photons enabled us to build a timing solution based solely on γ-rays. Timing analysis shows two prominent peaks, separated by Δ = 0.497 ± 0.004 in phase, which narrow with increasing energy. Pulsed γ-rays are observed beyond 18 GeV, precluding emission below 2.7 stellar radii because of magnetic absorption. The phase-averaged spectrum was fitted with a power law with exponential cutoff of spectral index Γ = (1.30 ± 0.01 ± 0.04), cutoff energy E0 = (2.46 ± 0.04 ± 0.17) GeV, and an integral photon flux above 0.1 GeV of (4.14 ± 0.02 ± 0.32) × 10^(–6) cm^(–2) s^(–1). The first uncertainties are statistical and the second ones are systematic. The phase-resolved spectroscopy shows a clear evolution of the spectral parameters, with the spectral index reaching a minimum value just before the leading peak and the cutoff energy having maxima around the peaks. The phase-resolved spectroscopy reveals that pulsar emission is present at all rotational phases. The spectral shape, broad pulse profile, and maximum photon energy favor the outer magnetospheric emission scenarios. |
| Document Type: | article in journal/newspaper |
| Language: | unknown |
| Relation: | info:eu-repo/semantics/altIdentifier/wos/WOS:000281596000025; volume:720; firstpage:272; lastpage:283; numberofpages:12; journal:THE ASTROPHYSICAL JOURNAL; https://hdl.handle.net/11577/2427411 |
| DOI: | 10.1088/0004-637X/720/1/272 |
| Availability: | https://hdl.handle.net/11577/2427411; https://doi.org/10.1088/0004-637X/720/1/272 |
| Accession Number: | edsbas.B0F732CF |
| Database: | BASE |