2016A&A...586A..71A


Query : 2016A&A...586A..71A

2016A&A...586A..71A - Astronomy and Astrophysics, volume 586A, 71-71 (2016/2-1)

Deep view of the Large Magellanic Cloud with six years of Fermi-LAT observations.

ACKERMANN M., ALBERT A., ATWOOD W.B., BALDINI L., BALLET J., BARBIELLINI G., BASTIERI D., BELLAZZINI R., BISSALDI E., BLOOM E.D., BONINO R., BRANDT T.J., BREGEON J., BRUEL P., BUEHLER R., 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., COHEN-TANUGI J., CUTINI S., D'AMMANDO F., DE ANGELIS A., DE PALMA F., DESIANTE R., DIGEL S.W., DRELL P.S., FAVUZZI C., FERRARA E.C., FOCKE W.B., FRANCKOWIAK A., FUSCO P., GARGANO F., GASPARRINI D., GIGLIETTO N., GIORDANO F., GODFREY G., GRENIER I.A., GRONDIN M.-H., GUILLEMOT L., GUIRIEC S., HARDING A.K., HILL A.B., HORAN D., JOHANNESSON G., KNOEDLSEDER J., KUSS M., LARSSON S., LATRONICO L., LI J., LI L., LONGO F., LOPARCO F., LUBRANO P., MALDERA S., MARTIN P., MAYER M., MAZZIOTTA M.N., MICHELSON P.F., MIZUNO T., MONZANI M.E., MORSELLI A., MURGIA S., NUSS E., OHSUGI T., ORIENTI M., ORLANDO E., ORMES J.F., PANEQUE D., PESCE-ROLLINS M., PIRON F., PIVATO G., PORTER T.A., RAINO S., RANDO R., RAZZANO M., REIMER A., REIMER O., ROMANI R.W., SANCHEZ-CONDE M., SCHULZ A., SGRO C., SISKIND E.J., SMITH D.A., SPADA F., SPANDRE G., SPINELLI P., SUSON D.J., TAKAHASHI H., THAYER J.B., TIBALDO L., TORRES D.F., TOSTI G., TROJA E., VIANELLO G., WOOD M. and ZIMMER S.

Abstract (from CDS):

The nearby Large Magellanic Cloud (LMC) provides a rare opportunity of a spatially resolved view of an external star-forming galaxy in γ-rays. The LMC was detected at 0.1-100GeV as an extended source with CGRO/EGRET and using early observations with the Fermi-LAT. The emission was found to correlate with massive star-forming regions and to be particularly bright towards 30 Doradus. Studies of the origin and transport of cosmic rays (CRs) in the Milky Way are frequently hampered by line-of-sight confusion and poor distance determination. The LMC offers a complementary way to address these questions by revealing whether and how the γ-ray emission is connected to specific objects, populations of objects, and structures in the galaxy. We revisited the γ-ray emission from the LMC using about 73 months of Fermi-LAT P7REP data in the 0.2-100GeV range. We developed a complete spatial and spectral model of the LMC emission, for which we tested several approaches: a simple geometrical description, template-fitting, and a physically driven model for CR-induced interstellar emission. In addition to identifying PSR J0540-6919 through its pulsations, we find two hard sources positionally coincident with plerion N 157B and supernova remnant N 132D, which were also detected at TeV energies with H.E.S.S. We detect an additional soft source that is currently unidentified. Extended emission dominates the total flux from the LMC. It consists of an extended component of about the size of the galaxy and additional emission from three to four regions with degree-scale sizes. If it is interpreted as CRs interacting with interstellar gas, the large-scale emission implies a large-scale population of ∼1-100GeV CRs with a density of ∼30% of the local Galactic value. On top of that, the three to four small-scale emission regions would correspond to enhancements of the CR density by factors 2 to 6 or higher, possibly more energetic and younger populations of CRs compared to the large-scale population. An alternative explanation is that this is emission from an unresolved population of at least two dozen objects, such as pulsars and their nebulae or supernova remnants. This small-scale extended emission has a spatial distribution that does not clearly correlate with known components of the LMC, except for a possible relation to cavities and supergiant shells. The Fermi-LAT GeV observations allowed us to detect individual sources in the LMC. Three of the newly discovered sources are associated with rare and extreme objects. The 30 Doradus region is prominent in GeV γ-rays because PSR J0540-6919 and N 157B are strong emitters. The extended emission from the galaxy has an unexpected spatial distribution, and observations at higher energies and in radio may help to clarify its origin.

Abstract Copyright:

Journal keyword(s): gamma rays: galaxies - Magellanic Clouds - cosmic rays

VizieR on-line data: <Available at CDS (J/A+A/586/A71): list.dat fits/*>

Simbad objects: 39

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Number of rows : 39
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 12098 1
2 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3194 2
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10532 1
4 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6558 1
5 2FGL J0438.0-7331 BLL 04 38 36.94 -73 29 23.8           ~ 21 0
6 LHA 120-N 11 HII 04 56 51.4 -66 24 24           ~ 248 0
7 SNR B0505-67.9 SNR 05 05 42.0 -67 52 29           ~ 137 0
8 SNR J050555-680150 SNR 05 05 55.00 -68 01 54.0           ~ 82 0
9 SNR J050854-684447 SNR 05 08 58.7 -68 43 46           ~ 151 2
10 SNR B0509-67.5 SNR 05 09 31 -67 31.3           ~ 214 0
11 SNR B0519-69.0 SNR 05 19 35.14 -69 02 00.5           ~ 150 0
12 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16512 1
13 SNR J052501-693842 SNR 05 25 02.20 -69 38 39.0           ~ 385 1
14 SNR B0525-66.0 SNR 05 25 27.1 -65 59 11           ~ 96 1
15 SNR J052559-660453 SNR 05 26 00.4 -66 05 02     12.71     ~ 429 2
16 3FGL J0529.8-7242 Bla 05 29 19.0 -72 43 59           ~ 15 0
17 NGC 2004 Cl* 05 30 41.340 -67 17 21.83   9.6       ~ 273 0
18 2FGL J0532.5-7223 Bz? 05 33 44.71018 -72 16 24.3131       22.63   ~ 21 1
19 SNR J053400-695508 SNR 05 33 59.00 -69 55 00.0           ~ 63 0
20 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5102 0
21 2E 1445 Sy1 05 34 45.7 -67 38 57   17.8 17.8     ~ 13 0
22 NGC 2029 SNR 05 35 15.5 -67 34 04     12.29     ~ 99 0
23 NGC 2032 HII 05 35 23.5 -67 34 56           ~ 73 1
24 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4782 2
25 SNR B0535-66.0 SNR 05 35 43.1 -66 01 59           ~ 170 1
26 NAME 30 Dor C Superbubble Rad 05 35 50.8 -69 12 22           ~ 46 1
27 4FGL J0535.2-6736 HXB 05 36 00.01 -67 35 07.5           ~ 35 0
28 PSR J0537-6910 Psr 05 37 46.66 -69 10 17.1           ~ 264 1
29 LH 99 As* 05 37.8 -69 10           ~ 49 0
30 NGC 2060 SNR 05 37 51.4466169456 -69 10 23.947092084   9.69 9.59     ~ 344 2
31 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1908 1
32 PSR B0540-69 Psr 05 40 10.84 -69 19 54.2           ~ 863 3
33 SNR B0548-70.4 SNR 05 47 50.00 -70 24 54.0           ~ 84 0
34 ICRF J060111.2-703608 QSO 06 01 11.2488493488 -70 36 08.802829692       18.244   ~ 86 1
35 NAME Pup A SNR 08 24 07 -42 59.8           ~ 572 1
36 NAME Vela X Psr 08 33 08.880 -45 11 24.36           ~ 266 1
37 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5678 6
38 HD 203767 * 21 23 28.4132703696 +31 06 58.406012964   8.98 7.33     K2 11 0
39 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2668 1

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2023.02.01-06:07:40

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