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ISM gas studies towards the TeV PWN HESS J1825-137 and northern region
Voisin, F.; Rowell, G.; Burton, M. G.; Walsh, A.; Fukui, Y.; Aharonian, F.
AA(School of Physical Science, Adelaide university, North Terrace, Adelaide, SA 5005, Australia; ), AB(School of Physical Science, Adelaide university, North Terrace, Adelaide, SA 5005, Australia), AC(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia), AD(International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth, WA 6845, Australia), AE(Department of Physics, University of Nagoya, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan), AF(Max-Planck-Institut für Kernphysik, PO Box 103980, D-69029 Heidelberg, Germany; Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland)
Monthly Notices of the Royal Astronomical Society, Volume 458, Issue 3, p.2813-2835 (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
molecular data, pulsars: individual: PSR J1826-1334, ISM: clouds, cosmic rays, gamma-rays: ISM
Abstract Copyright:
2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Bibliographic Code:


HESS J1825-137 is a pulsar wind nebula (PWN) whose TeV emission extends across ˜1 . Its large asymmetric shape indicates that its progenitor supernova interacted with a molecular cloud located in the north of the PWN as detected by previous CO Galactic survey (e.g. Lemiere, Terrier & Djannati-Ataï). Here, we provide a detailed picture of the interstellar medium (ISM) towards the region north of HESS J1825-137, with the analysis of the dense molecular gas from our 7 and 12 mm Mopra survey and the more diffuse molecular gas from the Nanten CO(1-0) and GRS 13CO(1-0) surveys. Our focus is the possible association between HESS J1825-137 and the unidentified TeV source to the north, HESS J1826-130. We report several dense molecular regions whose kinematic distance matched the dispersion measured distance of the pulsar. Among them, the dense molecular gas located at (RA, Dec.) = (18h421h,-13.282°) shows enhanced turbulence and we suggest that the velocity structure in this region may be explained by a cloud-cloud collision scenario. Furthermore, the presence of a H alpha rim may be the first evidence of the progenitor supernova remnant (SNR) of the pulsar PSR J1826-1334 as the distance between the H alpha rim and the TeV source matched with the predicted SNR radius RSNR ˜ 120 pc. From our ISM study, we identify a few plausible origins of the HESS J1826-130 emission, including the progenitor SNR of PSR J1826-1334 and the PWN G018.5-0.4 powered by PSR J1826-1256. A deeper TeV study however, is required to fully identify the origin of this mysterious TeV source.
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