Please use this identifier to cite or link to this item:
https://hdl.handle.net/2440/102504
Citations | ||
Scopus | Web of Science® | Altmetric |
---|---|---|
?
|
?
|
Type: | Journal article |
Title: | ISM gas studies towards the TeV PWN HESS J1825-137 and northern region |
Author: | Voisin, F. Rowell, G. Burton, M. Walsh, A. Fukui, Y. Aharonian, F. |
Citation: | Monthly Notices of the Royal Astronomical Society, 2016; 458(3):2813-2835 |
Publisher: | Oxford University Press |
Issue Date: | 2016 |
ISSN: | 0035-8711 1365-2966 |
Statement of Responsibility: | F. Voisin, G. Rowell, M. G. Burton, A. Walsh, Y. Fukui and F. Aharonian |
Abstract: | HESS J1825−137 is a pulsar wind nebula (PWN) whose TeV emission extends across ∼1 deg. 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 α rim may be the first evidence of the progenitor supernova remnant (SNR) of the pulsar PSR J1826−1334 as the distance between the H α 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. |
Keywords: | Molecular data; pulsars; individual; PSR J1826−1334; ISM; clouds; cosmic rays; gamma-rays; ISM |
Rights: | © 2016 The Authors |
DOI: | 10.1093/mnras/stw473 |
Published version: | http://dx.doi.org/10.1093/mnras/stw473 |
Appears in Collections: | Aurora harvest 3 Physics publications |
Files in This Item:
There are no files associated with this item.
Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.