Volume 509, January 2010
|Number of page(s)||3|
|Published online||14 January 2010|
Letter to the Editor
Identifying the counterpart of HESS J1858+020
Instituto de Astronomía y Física del Espacio (CONICET-UBA),
CC 67, Suc. 28, 1428 Buenos Aires, Argentina e-mail: email@example.com
Accepted: 14 December 2009
Aims. HESS J1858+020 is a weak γ-ray source that does not have any clear cataloged counterpart at any wavelengths. Recently, the source G35.6-0.4 was re-identified as a SNR. The HESS source lies towards the southern border of this remnant. The purpose of this work is to investigate the interstellar medium around the mentioned sources to look for possible counterparts of the very high energy emission.
Methods. Using the 13CO J=1–0 line from the Galactic Ring Survey and mid-IR data from GLIMPSE we analyze the environs of HESS J1858+020 and SNR G35.6-0.4.
Results. The 13CO data show the presence of a molecular cloud towards the southern border of SNR G35.6-0.4 and at the same distance as the remnant. This cloud is composed of two molecular clumps, one over the SNR shell and the other located at the center of HESS J1858+020. We estimate a molecular mass and a density of and ~500 cm-3 respectively for each clump. Considering the gamma-ray flux observed towards HESS J1858+020, we estimate that a molecular cloud with a density of at least 150 cm-3 could explain the very high energy emission hadronically. Thus, we suggest that the γ-ray emission detected in HESS J1858+020 is due to hadronic mechanism. Additionally, analyzing mid-IR emission, we find that the region is active in star formation, which could be considered as an alternative or complementary possibility to explain the very high energy emission.
Key words: ISM: clouds / ISM: supernova remnants / gamma rays: ISM / ISM: individual objects: HESS J1858+020
© ESO, 2010
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