2011A&A...526A..82E


C.D.S. - SIMBAD4 rel 1.7 - 2019.09.16CEST23:20:08

2011A&A...526A..82E - Astronomy and Astrophysics, volume 526A, 82-82 (2011/2-1)

A multi-wavelength study of the unidentified TeV gamma-ray source HESS J1626-490.

EGER P., ROWELL G., KAWAMURA A., FUKUI Y., ROLLAND L. and STEGMANN C.

Abstract (from CDS):

To explore the nature of the unidentified very-high-energy (VHE, E>100GeV) gamma-ray source HESSJ1626-490, we investigated the region in X-ray, sub-millimeter, and infrared energy bands. So far only detected with the HESS array of imaging atmospheric Cherenkov telescopes, HESSJ1626-490 could not be unambiguously identified with any source seen at lower energies. Therefore, we analyzed data from an archival XMM-Newton observation, pointed towards HESSJ1626-490, to classify detected X-ray point sources according to their spectral properties and their near-infrared counterparts from the 2MASS catalog. Furthermore, we characterized in detail the diffuse X-ray emission from a region compatible with the extended VHE signal. To characterize the interstellar medium surrounding HESSJ1626-490 we analyzed 12CO(J=1-0) molecular line data from the Nanten Galactic plane survey, HI data from the Southern Galactic Plane Survey (SGPS) and Spitzer data from the GLIMPSE and MIPSGAL surveys. None of the detected X-ray point sources fulfills the energy requirements to be considered as the synchrotron radiation counterpart to the VHE source assuming an inverse-Compton (IC) emission scenario. We did not detect any diffuse X-ray excess emission originating in the region around HESSJ1626-490 above the Galactic background and the derived upper limit for the total X-ray flux disfavors a purely leptonic emission scenario for HESSJ1626-490. We found a good morphological match between molecular and atomic gas in the -27km/s to -18km/s line-of-sight velocity range and HESSJ1626-490. The cloud has a mass of 1.8x104M and is located at a mean kinematic distance of d=1.8kpc. Furthermore, we found a density depression in the HI gas at a similar distance, which is spatially consistent with the SNRG335.2+00.1. We discuss various scenarios for the VHE emission, including the CO molecular cloud being a passive target for cosmic ray protons accelerated by the nearby SNRG335.2+00.1.

Abstract Copyright:

Journal keyword(s): acceleration of particles - ISM: supernova remnants - ISM: clouds - ISM: individual objects: HESS J1626-490 - X-rays: ISM - submillimeter: ISM

Nomenclature: Figs 8-9: [ERK2011] AN (Nos D1-D2, R1-R2).

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 IC 443 SNR 06 18 02.7 +22 39 36           ~ 1066 1
2 * alf Gem ** 07 34 35.87319 +31 53 17.8160 1.63 1.62 1.58 1.51 1.52 A1V+A2Vm 233 0
3 HESS J1514-591 Rad 15 13 17.000 -59 04 54.00           ~ 366 3
4 1RXS J162504.0-490918 X 16 25 04.003 -49 09 18.50           ~ 2 0
5 HD 147633 ** 16 25 17.58322 -49 08 52.3567   9.44 8.92 8.27   G2V 54 0
6 3FHL J1626.3-4915 BLL 16 26 01 -49 17.3           ~ 11 0
7 HESS J1626-490 gam 16 26 04.0 -49 05 13           ~ 13 0
8 [R2003] 427 ? 16 26.4 -49 14           ~ 2 0
9 SNR G335.2+00.1 SNR 16 27 45.000 -48 47 00.00           ~ 35 0
10 NAME Big Dipper LXB 16 28 05.5318316228 -49 12 40.011030945           ~ 204 0
11 2MASS J16281083-4838560 HXB 16 28 10.83 -48 38 56.1           OBsg 31 1
12 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 10915 0
13 SNR G006.4-00.1 SNR 18 01 22.7 -23 17 20           ~ 627 1
14 PSR B1823-13 Psr 18 26 13.06 -13 34 48.1           ~ 343 1

    Equat.    Gal    SGal    Ecl

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2019.09.16-23:20:08

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