2024ApJ...970L..21A

Query : 2024ApJ...970L..21A

2024ApJ...970L..21A - Astrophys. J., 970, L21 (2024/July-3)

Very-high-energy γ-Ray Emission from Young Massive Star Clusters in the Large Magellanic Cloud.

AHARONIAN F., AIT BENKHALI F., ASCHERSLEBEN J., ASHKAR H., BACKES M., BARBOSA MARTINS V., BATZOFIN R., BECHERINI Y., BERGE D., BERNLOHR K., BOTTCHER M., BOLMONT J., DE BONY DE LAVERGNE M., BOROWSKA J., BROSE R., BROWN A., BRUN F., BRUNO B., BURGER-SCHEIDLIN C., CASANOVA S., CELIC J., CERRUTI M., CHAND T., CHANDRA S., CHEN A., CHIBUEZE J., CHIBUEZE O., COTTER G., CRISTOFARI P., DEVIN J., DJANNATI-ATAI A., DJUVSLAND J., DMYTRIIEV A., EGBERTS K., EINECKE S., FEIJEN K., FILIPOVIC M., FONTAINE G., FUNK S., GABICI S., GALLANT Y.A., GLICENSTEIN J.F., GLOMBITZA J., GROLLERON G., HAERER L., HESS B., HINTON J.A., HOFMANN W., HOLCH T.L., HORNS D., HUANG Z., JAMROZY M., JANKOWSKY F., JUNG-RICHARDT I., KASAI E., KATARZYNSKI K., KHATOON R., KHELIFI B., KLUZNIAK W., KOMIN N., KOSACK K., KOSTUNIN D., KUNDU A., LANG R.G., LE STUM S., LEMIERE A., LEMOINE-GOUMARD M., LENAIN J.-P., LEUSCHNER F., MACKEY J., MARANDON V., MARTI-DEVESA G., MARX R., MEHTA A., MITCHELL A., MODERSKI R., MOGHADAM M.O., MOHRMANN L., MONTANARI A., MOULIN E., DE NAUROIS M., NIEMIEC J., OHM S., OLIVERA-NIETO L., DE ONA WILHELMI E., OSTROWSKI M., PANNY S., PENSEC U., PERON G., PUHLHOFER G., QUIRRENBACH A., RAVIKULARAMAN S., REGEARD M., REIMER A., REIMER O., REN H., RENAUD M., REVILLE B., RIEGER F., ROWELL G., RUDAK B., RUIZ-VELASCO E., SABRI K., SAHAKIAN V., SALZMANN H., SANTANGELO A., SASAKI M., SCHAFER J., SCHUSSLER F., SCHUTTE H.M., SOL H., SPENCER S., STAWARZ L., STEINMASSL S., STEPPA C., STREIL K., SUSHCH I., TAYLOR A.M., TERRIER R., TSIROU M., TSUJI N., VAN ELDIK C., VECCHI M., VENTER C., VINK J., WAGNER S.J., WHITE R., WIERZCHOLSKA A., ZACHARIAS M., ZDZIARSKI A.A., ZECH A., ZYWUCKA N. (The HESS Collaboration)

Abstract (from CDS):

The Tarantula Nebula in the Large Magellanic Cloud is known for its high star formation activity. At its center lies the young massive star cluster R136, providing a significant amount of the energy that makes the nebula shine so brightly at many wavelengths. Recently, young massive star clusters have been suggested to also efficiently produce very high-energy cosmic rays, potentially beyond PeV energies. Here, we report the detection of very-high-energy γ-ray emission from the direction of R136 with the High Energy Stereoscopic System, achieved through a multicomponent, likelihood-based modeling of the data. This supports the hypothesis that R136 is indeed a very powerful cosmic-ray accelerator. Moreover, from the same analysis, we provide an updated measurement of the γ-ray emission from 30 Dor C, the only superbubble detected at TeV energies presently. The γ-ray luminosity above 0.5 TeV of both sources is (2-3) × 1035 erg s–1. This exceeds by more than a factor of 2 the luminosity of HESS J1646-458, which is associated with the most massive young star cluster in the Milky Way, Westerlund 1. Furthermore, the γ-ray emission from each source is extended with a significance of >3σ and a Gaussian width of about 30 pc. For 30 Dor C, a connection between the γ-ray emission and the nonthermal X-ray emission appears likely. Different interpretations of the γ-ray signal from R136 are discussed.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Young star clusters - Massive stars - Large Magellanic Cloud - Gamma-ray astronomy

Simbad objects: 17

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Number of rows : 17
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 LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
2 MCSNR J0525-6938 SNR 05 25 02.3 -69 38 39           ~ 446 1
3 HESS J0535-691 gam 05 35 55.0 -69 11 10           ~ 2 0
4 4FGL J0535.2-6736 HXB 05 36 00.01 -67 35 07.5           ~ 49 0
5 NAME 30 Dor C Rad 05 36 07.70 -69 11 52.6           ~ 87 1
6 NGC 2044 As* 05 36 11 -69 11.8   10.69 10.59     ~ 89 0
7 MCSNR J0536-6913 SNR 05 36 17.0 -69 13 28           ~ 16 0
8 HESS J0537-691 gam 05 37 44.0 -69 09 57           ~ 4 0
9 PSR J0537-6910 Psr 05 37 46.66 -69 10 17.1           ~ 309 1
10 NGC 2060 SNR 05 37 51.4466169456 -69 10 23.947092084   9.69 9.59     ~ 380 2
11 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1276 2
12 NGC 2070 Cl* 05 38 42 -69 06.0     7.25     ~ 406 1
13 RMC 136 Cl* 05 38 42.396 -69 06 03.36   5.81 5.40     ~ 2236 2
14 HESS J0538-691 gam 05 38 46 -69 06.2           ~ 1 0
15 HESS J1646-458 gam 16 46 00.0 -45 48 00           ~ 14 0
16 Cl Westerlund 1 OpC 16 47 02.4 -45 51 07           ~ 655 1
17 PKS J2158-3013 BLL 21 58 52.0652249880 -30 13 32.118447792   13.36 13.09 12.62   ~ 1829 1

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