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2019A&A...621A.116H - Astronomy and Astrophysics, volume 621A, 116-116 (2019/1-1)

Particle transport within the pulsar wind nebula HESS J1825-137.

HESS COLLABORATION, ABDALLA H., AHARONIAN F., AIT BENKHALI F., ANGUNER E.O., ARAKAWA M., ARCARO C., ARMAND C., ARRIETA M., BACKES M., BARNARD M., BECHERINI Y., BECKER TJUS J., BERGE D., BERNLOHR K., BLACKWELL R., BOTTCHER M., BOISSON C., BOLMONT J., BONNEFOY S., BORDAS P., BREGEON J., BRUN F., BRUN P., BRYAN M., BUCHELE M., BULIK T., BYLUND T., CAPASSO M., CAROFF S., CAROSI A., CASANOVA S., CERRUTI M., CHAKRABORTY N., CHAND T., CHANDRA S., CHAVES R.C.G., CHEN A., COLAFRANCESCO S., CONDON B., DAVIDS I.D., DEIL C., DEVIN J., DEWILT P., DIRSON L., DJANNATI-ATAI A., DMYTRIIEV A., DONATH A., DOROSHENKO V., DRURY L.O., DYKS J., EGBERTS K., EMERY G., ERNENWEIN J.-P., ESCHBACH S., FEGAN S., FIASSON A., FONTAINE G., FUNK S., FUSSLING M., GABICI S., GALLANT Y.A., GATE F., GIAVITTO G., GLAWION D., GLICENSTEIN J.F., GOTTSCHALL D., GRONDIN M.-H., HAHN J., HAUPT M., HEINZELMANN G., HENRI G., HERMANN G., HINTON J.A., HOFMANN W., HOISCHEN C., HOLCH T.L., HOLLER M., HORNS D., HUBER D., IWASAKI H., JACHOLKOWSKA A., JAMROZY M., JANKOWSKY D., JANKOWSKY F., JOUVIN L., JUNG-RICHARDT I., KASTENDIECK M.A., KATARZYNSKI K., KATSURAGAWA M., KATZ U., KERSZBERG D., KHANGULYAN D., KHELIFI B., KING J., KLEPSER S., KLUZNIAK W., KOMIN N., KOSACK K., KRAUS M., LAMANNA G., LAU J., LEFAUCHEUR J., LEMIERE A., LEMOINE-GOUMARD M., LENAIN J.-P., LESER E., LOHSE T., LOPEZ-COTO R., LYPOVA I., MALYSHEV D., MARANDON V., MARCOWITH A., MARIAUD C., MARTI-DEVESA G., MARX R., MAURIN G., MEINTJES P.J., MITCHELL A.M.W., MODERSKI R., MOHAMED M., MOHRMANN L., MOORE C., MOULIN E., MURACH T., NAKASHIMA S., DE NAUROIS M., NDIYAVALA H., NIEDERWANGER F., NIEMIEC J., OAKES L., O'BRIEN P., ODAKA H., OHM S., OSTROWSKI M., OYA I., PANTER M., PARSONS R.D., PERENNES C., PETRUCCI P.-O., 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., REIMER A., REIMER O., RENAUD M., RIEGER F., RINCHIUSO L., ROMOLI C., ROWELL G., RUDAK B., RUIZ-VELASCO E., SAHAKIAN V., SAITO S., SANCHEZ D.A., SANTANGELO A., SASAKI M., SCHLICKEISER R., SCHUSSLER F., SCHULZ A., SCHUTTE H., SCHWANKE U., SCHWEMMER S., SEGLAR-ARROYO M., SENNIAPPAN M., SEYFFERT A.S., SHAFI N., SHILON I., SHININGAYAMWE K., SIMONI R., SINHA A., SOL H., SPECOVIUS A., SPIR-JACOB M., STAWARZ L., STEENKAMP R., STEGMANN C., STEPPA C., TAKAHASHI T., TAVERNET J.-P., TAVERNIER T., TAYLOR A.M., TERRIER R., TIBALDO L., TIZIANI D., TLUCZYKONT M., TRICHARD C., 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., VOISIN F., VOLK H.J., VUILLAUME T., WADIASINGH Z., WAGNER S.J., WAGNER R.M., WHITE R., WIERZCHOLSKA A., YANG R., YONEDA H., ZABOROV D., ZACHARIAS M., ZANIN R., ZDZIARSKI A.A., ZECH A., ZEFI F., ZIEGLER A., ZORN J. and ZYWUCKA N.

Abstract (from CDS):


Context. We present a detailed view of the pulsar wind nebula (PWN) HESS J1825-137. We aim to constrain the mechanisms dominating the particle transport within the nebula, accounting for its anomalously large size and spectral characteristics.
Aims. The nebula was studied using a deep exposure from over 12 years of H.E.S.S. I operation, together with data from H.E.S.S. II that improve the low-energy sensitivity. Enhanced energy-dependent morphological and spatially resolved spectral analyses probe the very high energy (VHE, E>0.1TeV) γ-ray properties of the nebula.
Methods. The nebula emission is revealed to extend out to 1.5° from the pulsar, ∼1.5 times farther than previously seen, making HESS J1825-137, with an intrinsic diameter of ∼100pc, potentially the largest γ-ray PWN currently known. Characterising the strongly energy-dependent morphology of the nebula enables us to constrain the particle transport mechanisms. A dependence of the nebula extent with energy of R∝Eα with α=-0.29±0.04stat±0.05sys disfavours a pure diffusion scenario for particle transport within the nebula. The total γ-ray flux of the nebula above 1TeV is found to be (1.12±0.03stat±0.25sys)x10–11cm–2s–1, corresponding to ∼64% of the flux of the Crab nebula.
Results. HESS J1825-137 is a PWN with clearly energy-dependent morphology at VHE γ-ray energies. This source is used as a laboratory to investigate particle transport within intermediate-age PWNe. Based on deep observations of this highly spatially extended PWN, we produce a spectral map of the region that provides insights into the spectral variation within the nebula.

Abstract Copyright: © ESO 2019

Journal keyword(s): gamma rays: general - acceleration of particles - convection - diffusion - pulsars: general

VizieR on-line data: <Available at CDS (J/A+A/621/A116): anaacore.dat anaafull.dat anabfull.dat totspec.dat boxfits.dat list.dat fits/*>

Simbad objects: 7

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2020.08.06-09:10:22

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