Identifying the counterpart of HESS J1858+020

Paron, S.; Giacani, E.

doi:10.1051/0004-6361/200913694

Cited by 16 publications

(49 citation statements)

References 16 publications

(21 reference statements)

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“…Across the whole area, the main component at ∼53 km s −1 , already detected in the 13 CO J = 1−0 clump studied by Paron & Giacani (2010), is present. A second, less intense, component is observed mainly towards positive RA and negative Dec offsets (bottom left in the image) with a velocity of ∼64 km s −1 .…”

Section: Resultsmentioning

confidence: 61%

“…Robitaille et al (2008) • 582, we find 27 GLIMPSE sources, and by applying the abovementioned color criterion, we find only two intrinsically red sources that appear to be related to the molecular clump, called SSTGLMC G035.5768-00.5862 and SSTGLMC G035.5765-00.5909, hereafter IRS1 and IRS2, respectively. These sources were classified as class I and II, respectively in Paron & Giacani (2010) following the Allen et al (2004) classification. In view of our more complete study, we now suggest that IRS1 is very likely to be embedded in the analyzed molecular clump, while for IRS2, lying on the border of the observed region, the connection with the studied molecular feature is less compelling (see Fig.…”

Section: Young Stellar Objects In the Molecular Clumpmentioning

confidence: 99%

“…The author estimated an age of 30 000 years for the SNR and a distance of ∼10.5 kpc. Paron & Giacani (2010) studied the interstellar medium (ISM) around the very-high energy source and, on the basis of 13 CO J = 1−0 data, identified a molecular cloud composed of two clumps. One of these clumps is seen in projection over the southern border of SNR G35.6-0.4 and displays some kinematical signatures of disturbed gas, while the other clump coincides with the center of HESS J1858+020.…”

Section: Introductionmentioning

confidence: 99%

“…One of these clumps is seen in projection over the southern border of SNR G35.6-0.4 and displays some kinematical signatures of disturbed gas, while the other clump coincides with the center of HESS J1858+020. On the basis of an IR study, Paron & Giacani (2010) found evidence of star formation activity in the second aforementioned clump. They suggested that the interaction between the SNR G35.6-0.4 and the molecular gas might be responsible for the γ-ray emission.…”

Section: Introductionmentioning

confidence: 99%

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Study of the molecular clump associated with the high-energy source HESS J1858+020

Paron

Giacani

Rubio

et al. 2011

A&A

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Aims. HESS J1858+020 is a weak γ-ray source lying near the southern border of the SNR G35.6-0.4. A molecular cloud, composed of two clumps, shows signs of interaction with both the SNR and a nearby extended HII region. In particular, the southernmost clump coincides with the center of the H.E.S.S. source. We study this clump in detail to help us identify the nature of the very-high energy emission. Methods. We observed the aforementioned molecular clump using the Atacama Submillimeter Telescope Experiment (ASTE) in the 12 CO J = 3−2, 13 CO J = 3−2, HCO + J = 4−3, and CS J = 7−6 lines with an angular resolution of 22 . To complement these observations, we analyzed IR and submillimeter continuum archival data. Results. From the 12 CO and 13 CO J = 3−2 lines and the 1.1 mm continuum emission, we derive a density of between 10 3 and 10 4 cm −3 for the clump. We discover a young stellar object (YSO), probably a high mass protostar, embedded in the molecular clump. However, we do not find any evidence of molecular outflows from this YSO that would represent a thermal jet capable of generating the observed γ-rays. We conclude that the most probable origin of the TeV γ-ray emission is a hadronic interaction between the molecular gas and the cosmic rays accelerated by the shock front of the SNR G35.6-0.4.

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Section: Resultsmentioning

confidence: 61%

Section: Young Stellar Objects In the Molecular Clumpmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Study of the molecular clump associated with the high-energy source HESS J1858+020

Paron

Giacani

Rubio

et al. 2011

A&A

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“…The northern clump shows kinematical hints of shocked gas that could evidence turbulent motion of the gas. This turbulent motion was suggested to be caused by the interaction of the SNR G35.6−0.4 with the molecular cloud (Paron & Giacani 2010). In Fig.…”

Section: Molecular Cloudmentioning

confidence: 80%

Deep GMRT radio observations and a multi-wavelength study of the region around HESS J1858+020

Paredes¹,

Ishwara‐Chandra²,

Bosch‐Ramon³

et al. 2013

A&A

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Context. There are a number of very high energy sources in the Galaxy that remain unidentified. Multi-wavelength and variability studies, and catalogue searches, are powerful tools to identify the physical counterpart, given the uncertainty in the source location and extension. Aims. This work carries out a thorough multi-wavelength study of the unidentified, very high energy source HESS J1858+020 and its environs. Methods. We have performed Giant Metrewave Radio Telescope observations at 610 MHz and 1.4 GHz to obtain a deep, low-frequency radio image of the region surrounding HESS J1858+020. We analysed archival radio, infrared, and X-ray data as well. This observational information, combined with molecular data, catalogue sources, and a nearby Fermi gamma-ray detection of unidentified origin, are combined to explore possible counterparts to the very high energy source. Results. We provide with a deep radio image of a supernova remnant that might be related to the GeV and TeV emission in the region.We confirm the presence of an H ii region next to the supernova remnant and coincident with molecular emission. A potential region of star formation is also identified. We identify several radio and X-ray sources in the surroundings. Some of these sources are known planetary nebulae, whereas others may be non-thermal extended emitters and embedded young stellar objects. Three old, background Galactic pulsars also neighbour HESS J1858+020 along the line of sight. Conclusions. The region surrounding HESS J1858+020 is rich in molecular structures and non-thermal objects that may potentially be linked to this unidentified very high energy source. In particular, a supernova remnant interacting with nearby molecular clouds may be a good candidate, but a star forming region, or a non-thermal radio source of yet unclear nature, may also be behind the gamma-ray source. The neighbouring pulsars, despite being old and distant, cannot be discarded as candidates. Further observational studies are needed, however, to narrow the search for a counterpart to the HESS source.

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Kinematic Distance of Galactic Radio Objects

Zhu¹,

Wu²,

Su³

et al. 2013

Proc. IAU

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We briefly summarize the method of kinematic distances of Galactic radio objects and discuss the ambiguity in this method. Both Hi absorption and Hi self-absorption are effective tools to solve the kinematic distance ambiguity. We build the 21 cm Hi absorption spectrum of the complex G35.6-0.5, and suggest SNR G35.6-0.4, one component of the complex, is located at the near side distance of about 3.6 kpc.

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Identifying the counterpart of HESS J1858+020

Cited by 16 publications

References 16 publications

Study of the molecular clump associated with the high-energy source HESS J1858+020

Study of the molecular clump associated with the high-energy source HESS J1858+020

Deep GMRT radio observations and a multi-wavelength study of the region around HESS J1858+020

Kinematic Distance of Galactic Radio Objects

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