2020A&A...644A.112H

Query : 2020A&A...644A.112H

2020A&A...644A.112H - Astronomy and Astrophysics, volume 644A112-112 (2020/12-1)

An extreme particle accelerator in the Galactic plane: HESS J1826-130.

HESS COLLABORATION, ABDALLA H., ADAM R., 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., BECHERINI Y., BERGE D., BERNLOHR K., BI B., BOTTCHER M., BOISSON C., BOLMONT J., DE BONY DE LAVERGNE M., BORDAS P., BREUHAUS M., BRUN F., BRUN P., BRYAN M., BUCHELE M., BULIK T., BYLUND T., CAROFF S., CAROSI A., CASANOVA S., CHAND T., CHANDRA S., CHEN A., COTTER G., CURYLO M., DAMASCENE MBARUBUCYEYE J., DAVIDS I.D., DAVIES J., DEIL C., DEVIN J., DEWILT P., DIRSON L., DJANNATI-ATAI A., DMYTRIIEV A., DONATH A., DOROSHENKO V., DUFFY C., DYKS J., EGBERTS K., EICHHORN F., EINECKE S., EMERY G., ERNENWEIN J.-P., FEIJEN K., FEGAN S., FIASSON A., FICHET DE CLAIRFONTAINE G., FONTAINE G., FUNK S., FUSSLING M., GABICI S., GALLANT Y.A., GIAVITTO G., GIUNTI L., GLAWION D., GLICENSTEIN J.F., GOTTSCHALL D., GRONDIN M.-H., HAHN J., HAUPT M., HERMANN G., HINTON J.A., HOFMANN W., HOISCHEN C., HOLCH T.L., HOLLER M., HORBE M., HORNS D., HUBER D., JAMROZY M., JANKOWSKY D., JANKOWSKY F., JARDIN-BLICQ A., JOSHI V., JUNG-RICHARDT I., KASAI E., KASTENDIECK M.A., KATARZYNSKI K., KATZ U., KHANGULYAN D., KHELIFI B., KLEPSER S., KLUZNIAK W., KOMIN N., KONNO R., KOSACK K., KOSTUNIN D., KRETER M., LAMANNA G., LEMIERE A., LEMOINE-GOUMARD M., LENAIN J.-P., LEVY C., LOHSE T., 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., MOHAMED M., MOHRMANN L., MONTANARI A., MOORE C., MORRIS P., MOULIN E., MULLER J., MURACH T., NAKASHIMA K., NAYERHODA A., DE NAUROIS M., NDIYAVALA H., NIEDERWANGER F., NIEMIEC J., OAKES L., O'BRIEN P., ODAKA H., OHM S., OLIVERA-NIETO L., DE ONA WILHELMI E., OSTROWSKI M., OYA I., PANTER M., PANNY S., PARSONS R.D., PERON G., PEYAUD B., PIEL Q., PITA S., POIREAU V., PRIYANA NOEL A., PROKHOROV D.A., PROKOPH H., PUHLHOFER G., PUNCH M., QUIRRENBACH A., RAAB S., RAUTH R., REICHHERZER P., REIMER A., REIMER O., REMY Q., RENAUD M., RIEGER F., RINCHIUSO L., ROMOLI C., ROWELL G., RUDAK B., RUIZ-VELASCO E., SAHAKIAN V., SAILER S., SANCHEZ D.A., SANTANGELO A., SASAKI M., SCALICI M., SCHUSSLER F., SCHUTTE H.M., SCHWANKE U., SCHWEMMER S., SEGLAR-ARROYO M., SENNIAPPAN M., SEYFFERT A.S., SHAFI N., SHININGAYAMWE K., SIMONI R., SINHA A., SOL H., SPECOVIUS A., SPENCER S., SPIR-JACOB M., STAWARZ L., SUN L., STEENKAMP R., STEGMANN C., STEINMASSL S., STEPPA C., TAKAHASHI T., TAVERNIER T., TAYLOR A.M., TERRIER R., TIZIANI D., TLUCZYKONT M., TOMANKOVA L., TRICHARD C., TSIROU M., 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., VUILLAUME T., WADIASINGH Z., WAGNER S.J., WATSON J., WERNER F., WHITE R., WIERZCHOLSKA A., WONG Y.W., YUSAFZAI A., ZACHARIAS M., ZANIN R., ZARGARYAN D., ZDZIARSKI A.A., ZECH A., ZHU S.J., ZIEGLER A., ZORN J., ZOUARI S. and ZYWUCKA N.

Abstract (from CDS):

The unidentified very-high-energy (VHE; E>0.1TeV) γ-ray source, HESS J1826-130, was discovered with the High Energy Stereoscopic System (HESS) in the Galactic plane. The analysis of 215h of HESS data has revealed a steady γ-ray flux from HESS J1826-130, which appears extended with a half-width of 0.21°±0.02stat°± 0.05sys°. The source spectrum is best fit with either a power-law function with a spectral index Γ=1.78±0.10stat± 0.20sys and an exponential cut-off at 15.2–3.2+5.5TeV, or a broken power-law with Γ1=1.96±0.06stat±0.20sys, Γ2=3.59±0.69stat±0.20sys for energies below and above Ebr=11.2±2.7TeV, respectively. The VHE flux from HESS J1826-130 is contaminated by the extended emission of the bright, nearby pulsar wind nebula, HESS J1825-137, particularly at the low end of the energy spectrum. Leptonic scenarios for the origin of HESS J1826-130 VHE emission related to PSR J1826-1256 are confronted by our spectral and morphological analysis. In a hadronic framework, taking into account the properties of dense gas regions surrounding HESS J1826-130, the source spectrum would imply an astrophysical object capable of accelerating the parent particle population up to ≥200TeV. Our results are also discussed in a multiwavelength context, accounting for both the presence of nearby supernova remnants, molecular clouds, and counterparts detected in radio, X-rays, and TeV energies.

Abstract Copyright: © H.E.S.S. Collaboration 2020

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

Simbad objects: 12

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Number of rows : 12
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 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
2 HESS J1641-463 gam 16 41 01.7 -46 18 11           ~ 27 0
3 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 16269 0
4 SNR G018.1-00.2 SNR 18 24 37.0 -13 15 18           ~ 48 1
5 eHWC J1825-134 gam 18 25.0 -13 26           ~ 21 0
6 2HWC J1825-134 gam 18 25.8 -13 24           ~ 10 0
7 SNR G018.6-00.2 SNR 18 25.9 -12 50           ~ 32 0
8 AX J1826.1-1300 X 18 26 04.9 -12 59 48           ~ 5 0
9 SNR G018.45-00.42 SR? 18 26 06 -13 03.3           ~ 7 0
10 PSR J1826-1256 Psr 18 26 08.570 -12 56 33.53           ~ 152 1
11 PSR B1823-13 Psr 18 26 13.06 -13 34 48.1           ~ 460 1
12 V* V479 Sct HXB 18 26 15.0561548880 -14 50 54.247274304 12.02 12.23 11.27 11.04   ON6V((f))z 613 2

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