2021A&A...655A...7H

Query : 2021A&A...655A...7H

2021A&A...655A...7H - Astronomy and Astrophysics, volume 655A, 7-7 (2021/11-1)

LMC N132D: A mature supernova remnant with a power-law gamma-ray spectrum extending beyond 8 TeV.

HESS COLLABORATION, ABDALLA H., AHARONIAN F., AIT BENKHALI F., ANGUNER E.O., ARCARO C., ARMAND C., ARMSTRONG T., ASHKAR H., BACKES M., BAGHMANYAN V., BARBOSA MARTINS V., BARNACKA A., BARNARD M., BATZOFIN R., BECHERINI Y., BERGE D., BERNLOHR K., BI B., BOTTCHER M., BOISSON C., BOLMONT J., DE BONY DE LAVERGNE M., BREUHAUS M., BROSE R., BRUN F., BULIK T., BYLUND T., CANGEMI F., CAROFF S., CASANOVA S., CATALANO J., CHAMBERY P., CHAND T., CHEN A., COTTER G., CURYLO M., DAMASCENE MBARUBUCYEYE J., DAVIDS I.D., DAVIES J., DEVIN J., DJANNATI-ATAI A., DMYTRIIEV A., DONATH A., DOROSHENKO V., DREYER L., DU PLESSIS L., DUFFY C., EGBERTS K., EINECKE S., ERNENWEIN J.-P., FEGAN S., FEIJEN K., FIASSON A., FICHET DE CLAIRFONTAINE G., FONTAINE G., LOTT F., FUSSLING M., FUNK S., GABICI S., GALLANT Y.A., GIAVITTO G., GIUNTI L., GLAWION D., GLICENSTEIN J.F., GRONDIN M.-H., HATTINGH S., HAUPT M., HERMANN G., HINTON J.A., HOFMANN W., HOISCHEN C., HOLCH T.L., HOLLER M., HORBE M., HORNS D., HUANG Z., HUBER D., JAMROZY M., JANKOWSKY F., JOSHI V., JUNG-RICHARDT I., KASAI E., KATARZYNSKI K., KATZ U., KHANGULYAN D., KHELIFI B., KLEPSER S., KLUZNIAK W., KOMIN N., KONNO R., KOSACK K., KOSTUNIN D., KRETER M., KUKEC MEZEK G., KUNDU A., LAMANNA G., LE STUM S., LEMIERE A., LEMOINE-GOUMARD M., LENAIN J.-P., LEUSCHNER F., LEVY C., LOHSE T., LUASHVILI A., LYPOVA I., MACKEY J., MAJUMDAR J., MALYSHEV D., MALYSHEV D., MARANDON V., MARCHEGIANI P., MARCOWITH A., MARES A., MARTI-DEVESA G., MARX R., MAURIN G., MEINTJES P.J., MEYER M., MITCHELL A., MODERSKI R., MOHRMANN L., MONTANARI A., MOORE C., MOULIN E., MULLER J., MURACH T., NAKASHIMA K., DE NAUROIS M., NAYERHODA A., NDIYAVALA H., NIEMIEC J., PRIYANA NOEL A., O'BRIEN P., OBERHOLZER L., ODAKA H., OHM S., OLIVERA-NIETO L., DE ONA WILHELMI E., OSTROWSKI M., PANNY S., PANTER M., PARSONS R.D., PERON G., PITA S., POIREAU V., PROKHOROV D.A., PROKOPH H., PUHLHOFER G., PUNCH M., QUIRRENBACH A., REICHHERZER P., REIMER A., REIMER O., REMY Q., RENAUD M., REVILLE B., RIEGER F., ROMOLI C., ROWELL G., RUDAK B., RUEDA RICARTE H., RUIZ-VELASCO E., SAHAKIAN V., SAILER S., SALZMANN H., SANCHEZ D.A., SANTANGELO A., SASAKI M., SCHAFER J., SCHUSSLER F., SCHUTTE H.M., SCHWANKE U., SENNIAPPAN M., SEYFFERT A.S., SHAPOPI J.N.S., SHININGAYAMWE K., SIMONI R., SINHA A., SOL H., SPECOVIUS A., SPENCER S., SPIR-JACOB M., STAWARZ L., STEENKAMP R., STEGMANN C., STEINMASSL S., STEPPA C., SUN L., TAKAHASHI T., TANAKA T., TAVERNIER T., TAYLOR A.M., TERRIER R., THIERSEN J.H.E., THORPE-MORGAN C., TLUCZYKONT M., TOMANKOVA L., TSIROU M., TSUJI N., TUFFS R., UCHIYAMA Y., VAN DER WALT D.J., VAN ELDIK C., VAN RENSBURG C., VAN SOELEN B., VASILEIADIS G., VEH J., VENTER C., VINCENT P., VINK J., VOLK H.J., WAGNER S.J., WATSON J., WERNER F., WHITE R., WIERZCHOLSKA A., WONG Y.W., YASSIN H., YUSAFZAI A., ZACHARIAS M., ZANIN R., ZARGARYAN D., ZDZIARSKI A.A., ZECH A., ZHU S.J., ZMIJA A., ZOUARI S. and ZYWUCKA N.

Abstract (from CDS):

Context. Supernova remnants (SNRs) are commonly thought to be the dominant sources of Galactic cosmic rays up to the knee of the cosmic-ray spectrum at a few PeV. Imaging Atmospheric Cherenkov Telescopes have revealed young SNRs as very-high-energy (VHE, >100 GeV) gamma-ray sources, but for only a few SNRs the hadronic cosmic-ray origin of their gamma-ray emission is indisputably established. In all these cases, the gamma-ray spectra exhibit a spectral cutoff at energies much below 100 TeV and thus do not reach the PeVatron regime.
Aims. The aim of this work was to achieve a firm detection for the oxygen-rich SNR LMC N132D in the VHE gamma-ray domain with an extended set of data, and to clarify the spectral characteristics and the localization of the gamma-ray emission from this exceptionally powerful gamma-ray-emitting SNR.
Methods. We analyzed 252 h of High Energy Stereoscopic System (H.E.S.S.) observations towards SNR N132D that were accumulated between December 2004 and March 2016 during a deep survey of the Large Magellanic Cloud, adding 104 h of observations to the previously published data set to ensure a > 5σ detection. To broaden the gamma-ray spectral coverage required for modeling the spectral energy distribution, an analysis of Fermi-LAT Pass 8 data was also included.
Results. We unambiguously detect N132D at VHE with a significance of 5.7σ. We report the results of a detailed analysis of its spectrum and localization based on the extended H.E.S.S. data set. The joint analysis of the extended H.E.S.S and Fermi-LAT data results in a spectral energy distribution in the energy range from 1.7 GeV to 14.8 TeV, which suggests a high luminosity of N132D at GeV and TeV energies. We set a lower limit on a gamma-ray cutoff energy of 8 TeV with a confidence level of 95%. The new gamma-ray spectrum as well as multiwavelength observations of N132D when compared to physical models suggests a hadronic origin of the VHE gamma-ray emission.
Conclusions. SNR N132D is a VHE gamma-ray source that shows a spectrum extending to the VHE domain without a spectral cutoff at a few TeV, unlike the younger oxygen-rich SNR Cassiopeia A. The gamma-ray emission is best explained by a dominant hadronic component formed by diffusive shock acceleration. The gamma-ray properties of N132D may be affected by an interaction with a nearby molecular cloud that partially lies inside the 95% confidence region of the source position.

Abstract Copyright: © ESO 2021

Journal keyword(s): gamma rays: general - cosmic rays - ISM: supernova remnants

Simbad objects: 30

Full paper

View the references in ADS

Number of rows : 30

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag B	Mag V	Sp type	#ref 1850 - 2023	#notes
1	NAME LMC	G	05 23 34.6	-69 45 22		0.4	~	16973	1
2	4FGL J0524.8-6938	gam	05 24 52.2	-69 38 29			~	3	0
3	SNR J052501-693842	SNR	05 25 02.3	-69 38 39			~	393	1
4	SNR B0525-66.0	SNR	05 25 27.1	-65 59 11			~	100	1
5	SNR B0535-66.0	SNR	05 35 43.1	-66 01 59			~	172	1
6	4FGL J0535.2-6736	HXB	05 36 00.01	-67 35 07.5			~	36	0
7	NAME 30 Dor C	Rad	05 36 07.70	-69 11 52.6			~	75	1
8	4FGL J0537.8-6909	gam	05 37 49.3	-69 09 53			~	7	0
9	NGC 2060	SNR	05 37 51.4466169456	-69 10 23.947092084	9.69	9.59	~	351	2
10	NAME 30 Dor Nebula	SFR	05 38 36.0	-69 05 11			~	1160	2
11	PSR B0540-69	Psr	05 40 10.84	-69 19 54.2			~	883	3
12	IC 443	SNR	06 17 34.7	+22 28 03			~	1217	1
13	NAME Pup A	SNR	08 24 07	-42 59.8			~	585	1
14	NAME Vela Jr SN	SNR	08 52.0	-46 20			~	466	2
15	ESO 134-11	HII	14 40 29	-62 38.7			~	555	1
16	SNR G318.2+00.1	SNR	14 54.8	-59 04			~	31	0
17	3EG J1639-4702	gam	16 40 30.0	-46 33 00			~	154	2
18	PSR J1640-4631	Psr	16 40 43.52	-46 31 35.4			~	55	0
19	SNR G347.3-00.5	SNR	17 12 27	-39 41.2		12.27	~	710	1
20	SNR G348.7+00.3	SNR	17 13 43.0	-38 10 12			~	119	2
21	SNR G348.5+00.1	SNR	17 14 31.780	-38 28 34.50			~	214	3
22	2CG 359+00	gam	17 45 11	-30 11.9			~	96	0
23	SNR G359.1-00.5	Rad	17 45 30	-29 57.0			~	174	1
24	SNR G006.4-00.1	SNR	18 01 22.7	-23 17 20			~	728	1
25	PSR B1800-21	Psr	18 03 51.45	-21 37 08.1			~	258	1
26	1AGLR J1807-2103	gam	18 03 52.1	-21 10 54			~	70	0
27	W 30	SNR	18 05 38	-21 36.7			~	171	1
28	SNR G034.6-00.5	SNR	18 56 10.650	+01 13 21.30			~	947	2
29	SNR G106.3+02.7	SNR	22 27.5	+60 50			~	70	1
30	NAME Cas A	SNR	23 23 24.000	+58 48 54.00		14.30	~	2724	1

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