2014ApJ...793...64A

Query : 2014ApJ...793...64A

2014ApJ...793...64A - Astrophys. J., 793, 64 (2014/September-3)

The spectrum and morphology of the Fermi bubbles.

ACKERMANN M., ALBERT A., ATWOOD W.B., BALDINI L., BALLET J., BARBIELLINI G., BASTIERI D., BELLAZZINI R., BISSALDI E., BLANDFORD R.D., BLOOM E.D., BOTTACINI E., BRANDT T.J., BREGEON J., BRUEL P., BUEHLER R., BUSON S., CALIANDRO G.A., CAMERON R.A., CARAGIULO M., CARAVEO P.A., CAVAZZUTI E., CECCHI C., CHARLES E., CHEKHTMAN A., CHIANG J., CHIARO G., CIPRINI S., CLAUS R., COHEN-TANUGI J., CONRAD J., CUTINI S., D'AMMANDO F., DE ANGELIS A., DE PALMA F., DERMER C.D., DIGEL S.W., DI VENERE L., DO COUTO E SILVA E., DRELL P.S., FAVUZZI C., FERRARA E.C., FOCKE W.B., FRANCKOWIAK A., FUKAZAWA Y., FUNK S., FUSCO P., GARGANO F., GASPARRINI D., GERMANI S., GIGLIETTO N., GIORDANO F., GIROLETTI M., GODFREY G., GOMEZ-VARGAS G.A., GRENIER I.A., GUIRIEC S., HADASCH D., HARDING A.K., HAYS E., HEWITT J.W., HOU X., JOGLER T., JOHANNESSON G., JOHNSON A.S., JOHNSON W.N., KAMAE T., KATAOKA J., KNODLSEDER J., KOCEVSKI D., KUSS M., LARSSON S., LATRONICO L., LONGO F., LOPARCO F., LOVELLETTE M.N., LUBRANO P., MALYSHEV D., MANFREDA A., MASSARO F., MAYER M., MAZZIOTTA M.N., McENERY J.E., MICHELSON P.F., MITTHUMSIRI W., MIZUNO T., MONZANI M.E., MORSELLI A., MOSKALENKO I.V., MURGIA S., NEMMEN R., NUSS E., OHSUGI T., OMODEI N., ORIENTI M., ORLANDO E., ORMES J.F., PANEQUE D., PANETTA J.H., PERKINS J.S., PESCE-ROLLINS M., PETROSIAN V., PIRON F., PIVATO G., RAINO S., RANDO R., RAZZANO M., RAZZAQUE S., REIMER A., REIMER O., SANCHEZ-CONDE M., SCHAAL M., SCHULZ A., SGRO C., SISKIND E.J., SPANDRE G., SPINELLI P., STAWARZ L., STRONG A.W., SUSON D.J., TAHARA M., TAKAHASHI H., THAYER J.B., TIBALDO L., TINIVELLA M., TORRES D.F., TOSTI G., TROJA E., UCHIYAMA Y., VIANELLO G., WERNER M., WINER B.L., WOOD K.S., WOOD M. and ZAHARIJAS G.

Abstract (from CDS):

The Fermi bubbles are two large structures in the gamma-ray sky extending to 55° above and below the Galactic center. We analyze 50 months of Fermi Large Area Telescope data between 100 MeV and 500 GeV above 10° in Galactic latitude to derive the spectrum and morphology of the Fermi bubbles. We thoroughly explore the systematic uncertainties that arise when modeling the Galactic diffuse emission through two separate approaches. The gamma-ray spectrum is well described by either a log parabola or a power law with an exponential cutoff. We exclude a simple power law with more than 7σ significance. The power law with an exponential cutoff has an index of 1.9±0.2 and a cutoff energy of 110±50 GeV. We find that the gamma-ray luminosity of the bubbles is 4.4_–0.9^+2.4 x 10³⁷ erg/s. We confirm a significant enhancement of gamma-ray emission in the southeastern part of the bubbles, but we do not find significant evidence for a jet. No significant variation of the spectrum across the bubbles is detected. The width of the boundary of the bubbles is estimated to be 3.4_–2.6^+3.7 deg. Both inverse Compton (IC) models and hadronic models including IC emission from secondary leptons fit the gamma-ray data well. In the IC scenario, synchrotron emission from the same population of electrons can also explain the WMAP and Planck microwave haze with a magnetic field between 5 and 20 µG.

Abstract Copyright: ∼

Journal keyword(s): astroparticle physics - cosmic rays - Galaxy: general - Galaxy: halo - gamma rays: diffuse background - methods: data analysis

Simbad objects: 8

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Number of rows : 8

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Mag I	Sp type	#ref 1850 - 2026	#notes
1	NAME Magellanic Stream	HVC	00 32	-30.0						~	1079	1
2	M 31	AGN	00 42 44.330	+41 16 07.50	4.86	4.36	3.44			~	13622	1
3	M 33	GiG	01 33 50.8965749232	+30 39 36.630403128	6.17	6.27	5.72			~	6226	1
4	NAME Magellanic Clouds	GrG	03 00	-71.0						~	7988	0
5	NAME Loop I	SR?	15 01	-38.7						~	414	2
6	* rho Oph	**	16 25 35.11766	-23 26 49.8150	4.30	4.85	4.63	4.27	3.96	B2IV+B2V	670	0
7	NAME Fermi Bubbles	bub	17 45	-29.0						~	525	0
8	NAME Galactic Center	reg	17 45 39.60213	-29 00 22.0000						~	16269	0

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