2023A&A...672A.103H

Query : 2023A&A...672A.103H

2023A&A...672A.103H - Astronomy and Astrophysics, volume 672A103 (2023/4-1)

HESS J1809-193: A halo of escaped electrons around a pulsar wind nebula?

HESS COLLABORATION, AHARONIAN F., AIT BENKHALI F., ASCHERSLEBEN J., ASHKAR H., BACKES M., BARBOSA MARTINS V., BATZOFIN R., BECHERINI Y., BERGE D., BOTTCHER M., BOISSON C., BOLMONT J., BOROWSKA J., BOUYAHIAOUI M., BRADASCIO F., BREUHAUS M., BROSE R., BRUN F., BRUNO B., BULIK T., BURGER-SCHEIDLIN C., BYLUND T., CAROFF S., CASANOVA S., CELIC J., CERRUTI M., CHAMBERY P., CHAND T., CHEN A., CHIBUEZE J., CHIBUEZE O., DAMASCENE MBARUBUCYEYE J., DJANNATI-ATAI A., DMYTRIIEV A., EINECKE S., ERNENWEIN J.-P., FEIJEN K., FILIPOVIC M., FONTAINE G., FUSSLING M., FUNK S., GABICI S., GALLANT Y.A., GHAFOURIZADEH S., GIAVITTO G., GIUNTI L., GLAWION D., GOSWAMI P., GROLLERON G., GRONDIN M.-H., HAERER L., HINTON J.A., HOFMANN W., HOLCH T.L., HOLLER M., HORNS D., HUANG Z., JAMROZY M., JANKOWSKY F., JOSHI V., JUNG-RICHARDT I., KASAI E., KATARZYNSKI K., KHELIFI B., KLUZNIAK W., KOMIN N., KOSACK K., KOSTUNIN D., LANG R.G., LE STUM S., LEITL F., LEMIERE A., LEMOINE-GOUMARD M., LENAIN J.-P., LEUSCHNER F., LOHSE T., LUASHVILI A., LYPOVA I., MACKEY J., MALYSHEV D., MALYSHEV D., MARANDON V., MARCHEGIANI P., MARCOWITH A., MARINOS P., MARTI-DEVESA G., MARX R., MITCHELL A., MODERSKI R., MOHRMANN L., MONTANARI A., MOULIN E., MULLER J., NAKASHIMA K., DE NAUROIS M., NIEMIEC J., NOEL A.P., OHM S., OLIVERA-NIETO L., DE ONA WILHELMI E., OSTROWSKI M., PANNY S., PANTER M., PARSONS R.D., PROKHOROV D.A., PUHLHOFER G., PUNCH M., QUIRRENBACH A., REICHHERZER P., REIMER A., REIMER O., RENAUD M., REVILLE B., RIEGER F., ROWELL G., RUDAK B., SAHAKIAN V., SANTANGELO A., SASAKI M., SCHUTTE H.M., SCHWANKE U., SHAPOPI J.N.S., SOL H., SPECOVIUS A., SPENCER S., STAWARZ L., STEENKAMP R., STEINMASSL S., SUSHCH I., SUZUKI H., TAKAHASHI T., TANAKA T., TERRIER R., THORPE-MORGAN C., TSIROU M., TSUJI N., UCHIYAMA Y., VAN ELDIK C., VECCHI M., VEH J., VENTER C., VINK J., WACH T., WAGNER S.J., WHITE R., WIERZCHOLSKA A., WONG Y.W., ZACHARIAS M., ZARGARYAN D., ZDZIARSKI A.A., ZECH A., ZOUARI S. and ZYWUCKA N.

Abstract (from CDS):

Context. HESS J1809-193 is an unassociated very-high-energy γ-ray source located on the Galactic plane. While it has been connected to the nebula of the energetic pulsar PSR J1809-1917, supernova remnants and molecular clouds present in the vicinity also constitute possible associations. Recently, the detection of γ-ray emission up to energies of ∼100 TeV with the HAWC observatory has led to renewed interest in HESS J1809-193.
Aims. We aim to understand the origin of the γ-ray emission of HESS J1809-193.
Methods. We analysed 93.2 h of data taken on HESS J1809-193 above 0.27 TeV with the High Energy Stereoscopic System (H.E.S.S.), using a multi-component, three-dimensional likelihood analysis. In addition, we provide a new analysis of 12.5 yr of Fermi-LAT data above 1 GeV within the region of HESS J1809-193. The obtained results are interpreted in a time-dependent modelling framework.
Results. For the first time, we were able to resolve the emission detected with H.E.S.S. into two components: an extended component (modelled as an elongated Gaussian with a 1-σ semi-major and semi-minor axis of ∼0.62° and ∼0.35°, respectively) that exhibits a spectral cutoff at ∼13 TeV, and a compact component (modelled as a symmetric Gaussian with a 1-σ radius of ∼0.1°) that is located close to PSR J1809-1917 and shows no clear spectral cutoff. The Fermi-LAT analysis also revealed extended γ-ray emission, on scales similar to that of the extended H.E.S.S. component.
Conclusions. Our modelling indicates that based on its spectrum and spatial extent, the extended H.E.S.S. component is likely caused by inverse Compton emission from old electrons that form a halo around the pulsar wind nebula. The compact component could be connected to either the pulsar wind nebula or the supernova remnant and molecular clouds. Due to its comparatively steep spectrum, modelling the Fermi-LAT emission together with the H.E.S.S. components is not straightforward.

Abstract Copyright: © The Authors 2023

Journal keyword(s): acceleration of particles - radiation mechanisms: non-thermal - pulsars: individual: PSR J1809-1917 - gamma rays: general

Simbad objects: 15

goto Full paper

goto View the references in ADS

Number of rows : 15
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 Vela X Psr 08 33 08.880 -45 11 24.36           ~ 302 1
2 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2446 1
3 HESS J1702-420 gam 17 02 44.0 -42 00 57           ~ 46 0
4 1AGLR J1807-2103 gam 18 03 52.1 -21 10 54           ~ 79 0
5 Fermi J1808.2-2029 gam 18 08 00.0 -20 24 00           ~ 20 0
6 PSR J1809-1917 Psr 18 09 43.147 -19 17 38.10           ~ 128 1
7 SNR G011.1+00.1 SNR 18 09.8 -19 12           ~ 32 0
8 AX J1809.8-1943 Psr 18 09 51.07 -19 43 51.8           ~ 532 0
9 SNR G011.0+00.0 SNR 18 10.1 -19 25           ~ 43 1
10 3FGL J1810.1-1910 gam 18 10 11 -19 10.1           ~ 13 0
11 HESS J1809-193 gam 18 10 31 -19 18.0           ~ 70 1
12 PSR J1811-1926 Psr 18 11 29.15 -19 25 25.4           ~ 136 1
13 3FGL J1811.3-1927c gam 18 11 32.8 -19 25 39           ~ 13 0
14 NAME AGPS 273.4-17.8 SNR 18 13 35.05 -17 49 58.1           ~ 145 2
15 PSR B1823-13 Psr 18 26 13.06 -13 34 48.1           ~ 460 1

To bookmark this query, right click on this link: simbad:objects in 2023A&A...672A.103H and select 'bookmark this link' or equivalent in the popup menu