2019A&A...626A..65P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST01:15:12

2019A&A...626A..65P - Astronomy and Astrophysics, volume 626A, 65-65 (2019/6-1)

New composite supernova remnant toward HESS J1844-030?

PETRIELLA A.

Abstract (from CDS):


Aims. HESS J1844-030 is a newly confirmed TeV source in the direction of the X-ray pulsar wind nebula (PWN) candidate G29.4+0.1 and the complex radio source G29.37+0.1, which is likely formed by the superposition of a background radio galaxy and a Galactic supernova remnant (SNR). Many scenarios have been proposed to explain the origin of HESS J1844-030, based on several sources that are capable of producing very high energy radiation. We investigate the possible connection between the SNR, the PWN G29.4+0.1, and HESS J1844-030 to shed light on the astrophysical origin of the TeV emission.
Methods. We performed an imaging and spectral study of the X-ray emission from the PWN G29.4+0.1 using archival observations obtained with the Chandra and XMM-Newton telescopes. Public radio continuum and HI data were used to derive distance constraints for the SNR that is linked to G29.37+0.1 and to investigate the interstellar medium where it is expanding. We applied a simple model of the evolution of a PWN inside an SNR to analyze the association between G29.4+0.1 and the radio emission from G29.37+0.1. We compared the spectral properties of the system with the population of TeV PWNe to investigate if HESS J1844-030 is the very high energy counterpart of the X-ray PWN G29.4+0.1.
Results. Based on the morphology and spectral behavior in the X-ray band, we conclude that G29.4+0.1 is a PWN and that a point source embedded on it is the powering pulsar. The HI data revealed that the SNR linked to G29.37+0.1 is a Galactic source at 6.5 kpc and expanding in a nonuniform medium. From the analysis of the pulsar motion and the pressure balance at the boundary of X-ray emission, we conclude that G29.4+0.1 could be a PWN that is located inside its host remnant, forming a new composite SNR. Based on the magnetic field of the PWN obtained from the X-ray luminosity, we found that the population of electrons producing synchrotron radiation in the keV band can also produce IC photons in the TeV band. This suggests that HESS J1844-030 could be the very high energy counterpart of G29.4+0.1.

Abstract Copyright: © ESO 2019

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

CDS comments: Paragraph.1 CXOU J18443.4-030520 and CXOU J18444.1-030549 not identified (incorrect format)

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 - 2020
#notes
1 SNR G130.7+03.1 SNR 02 05 37.0 +64 49 42           ~ 565 4
2 IC 443 SNR 06 18 02.7 +22 39 36           ~ 1100 1
3 NAME Geminga Psr 06 33 54.153 +17 46 12.91           ~ 1092 0
4 HESS J1514-591 Rad 15 13 17.000 -59 04 54.00           ~ 376 3
5 SNR G327.1-01.1 SNR 15 54 32.3 -55 03 44           ~ 81 1
6 NAME Mouse Rad 17 47 15.78 -29 58 01.0           ~ 92 1
7 SNR G000.9+00.1 SNR 17 47.3 -28 09           ~ 168 1
8 PSR J1833-1034 Psr 18 33 33.612 -10 34 07.69           ~ 391 1
9 ARGO J1841-0332 gam 18 43 00.0 -03 18 00           ~ 17 0
10 MAGPIS SNR? G29.3667+0.1000 SR? 18 44 34.3 -03 07 37           ~ 5 0
11 PMN J1844-0306 Rad 18 44 36.4 -03 06 30           ~ 8 0
12 HESS J1844-030 gam 18 44 40.0 -03 06 00           ~ 5 0
13 AX J1844.8-0258 HXB 18 44 53 -02 56.0           ~ 110 0
14 SNR G029.7-00.3 SNR 18 46 25.5 -02 59 14           ~ 289 2
15 SNR G034.6-00.5 SNR 18 56 10.650 +01 13 21.30           ~ 825 2
16 SS 433 HXB 19 11 49.5645897701 +04 58 57.824087535   16.3 13.0     A7Ib: 1928 3
17 SNR G039.7-02.0 SNR 19 12 20 +04 55.0           ~ 313 1

    Equat.    Gal    SGal    Ecl

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2020.07.04-01:15:12

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