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

Paredes, J. M.; Ishwara‐Chandra, C. H.; Bosch‐Ramon, V.; Zabalza, V.; Iwasawa, K.; Ribó, M.

doi:10.1051/0004-6361/201322306

Cited by 11 publications

(21 citation statements)

References 42 publications

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“…HESS J1858+020 has an association with the HE γ-ray source 3FGL J1857.9+0210 and is close to, but offset from, SNR G35.6−0.4. A dedicated study (Paredes et al 2014) did not find any compelling X-ray counterpart, although multiple possible scenarios were investigated, including CRilluminated molecular clouds.…”

Section: Hess J1503−582 Is Also a New Hgps Source And Does Notmentioning

confidence: 97%

The H.E.S.S. Galactic plane survey

Abdalla¹,

Abramowski²,

Aharonian³

et al. 2018

A&A

346

155

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We present the results of the most comprehensive survey of the Galactic plane in very high-energy (VHE) γ-rays, including a public release of Galactic sky maps, a catalog of VHE sources, and the discovery of 16 new sources of VHE γ-rays. The High Energy Spectroscopic System (H.E.S.S.) Galactic plane survey (HGPS) was a decade-long observation program carried out by the H.E.S.S. I array of Cherenkov telescopes in Namibia from 2004 to 2013. The observations amount to nearly 2700 h of quality-selected data, covering the Galactic plane at longitudes from ℓ = 250° to 65° and latitudes |b|≤ 3°. In addition to the unprecedented spatial coverage, the HGPS also features a relatively high angular resolution (0.08° ≈ 5 arcmin mean point spread function 68% containment radius), sensitivity (≲1.5% Crab flux for point-like sources), and energy range (0.2–100 TeV). We constructed a catalog of VHE γ-ray sources from the HGPS data set with a systematic procedure for both source detection and characterization of morphology and spectrum. We present this likelihood-based method in detail, including the introduction of a model component to account for unresolved, large-scale emission along the Galactic plane. In total, the resulting HGPS catalog contains 78 VHE sources, of which 14 are not reanalyzed here, for example, due to their complex morphology, namely shell-like sources and the Galactic center region. Where possible, we provide a firm identification of the VHE source or plausible associations with sources in other astronomical catalogs. We also studied the characteristics of the VHE sources with source parameter distributions. 16 new sources were previously unknown or unpublished, and we individually discuss their identifications or possible associations. We firmly identified 31 sources as pulsar wind nebulae (PWNe), supernova remnants (SNRs), composite SNRs, or gamma-ray binaries. Among the 47 sources not yet identified, most of them (36) have possible associations with cataloged objects, notably PWNe and energetic pulsars that could power VHE PWNe.

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Section: Hess J1503−582 Is Also a New Hgps Source And Does Notmentioning

confidence: 97%

The H.E.S.S. Galactic plane survey

Abdalla¹,

Abramowski²,

Aharonian³

et al. 2018

A&A

346

155

View full text Add to dashboard Cite

show abstract

“…Similarly, for HESS J1858+020, (Paredes et al 2014) note the rich molecular environment and suggest that the non-thermal emission may arise from interactions between a SNR and nearby clouds. The predictions of our model that clouds should be detectable in gammarays in this region is therefore consistent with the data.…”

mentioning

confidence: 88%

“…B1, where a group of three clouds overlap with HESS J1857+026 and HESS J1858+020. Both of these sources remain unidentified, although it is known that there is substantial molecular material in the vicinity (Paredes et al 2014). HESS J1857+026 was best described by two components that were merged to a single source in the HGPS, whereas the MAGIC collaboration favour a two-source interpretation, associating MAGIC J1857.2+0263 with the pulsar PSR J1856+0245, whilst MAGIC J1857.6+0297 remains unidentified (MAGIC Collaboration 2014; H.E.S.S.…”

mentioning

confidence: 99%

Using interstellar clouds to search for Galactic PeVatrons: gamma-ray signatures from supernova remnants

Mitchell

Rowell

Celli

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Interstellar clouds can act as target material for hadronic cosmic rays; gamma rays subsequently produced through inelastic proton-proton collisions and spatially associated with such clouds can provide a key indicator of efficient particle acceleration. However, even in the case that particle acceleration proceeds up to PeV energies, the system of accelerator and nearby target material must fulfil a specific set of conditions in order to produce a detectable gamma-ray flux. In this study, we rigorously characterise the necessary properties of both cloud and accelerator. By using available Supernova Remnant (SNR) and interstellar cloud catalogues, we produce a ranked shortlist of the most promising target systems, those for which a detectable gamma-ray flux is predicted, in the case that particles are accelerated to PeV energies in a nearby SNR. We discuss detection prospects for future facilities including CTA, LHAASO and SWGO; and compare our predictions with known gamma-ray sources. The four interstellar clouds with the brightest predicted fluxes >100 TeV identified by this model are located at (l,b) = (330.05, 0.13), (15.82, -0.46), (271.09, -1.26), and (21.97, -0.29). These clouds are consistently bright under a range of model scenarios, including variation in the diffusion coefficient and particle spectrum. On average, a detectable gamma-ray flux is more likely for more massive clouds; systems with lower separation distance between the SNR and cloud; and for slightly older SNRs.

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“…The nearby radio source G35.6−0.4 located northwest of HESS J1858+020 was identified as a SNR by Green (2009). The radio boundary of this SNR is clearly shown in the 1.4GHz image with VGPS (Stil et al 2006;Zhu et al 2013) and the 610 MHz image with GMRT (Paredes et al 2014).…”

Section: Introductionmentioning

confidence: 99%

HESS J1858+020: A GeV-TeV source possibly powered by CRs from SNR G35.6-0.4

Cui,

Xin,

Liu

et al. 2021

Preprint

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Context. The supernova remnant (SNR) G35.6−0.4 shows a non-thermal radio shell, however, no γ-ray or X-ray counterparts have been found for it thus far. One TeV source, HESS J1858+020, was found near the SNR and this source is spatially associated with some clouds at 3.6 kpc. Aims. To attain a better understanding of the origin of HESS J1858+020, we further investigate the association between SNR cosmic rays (CRs) and the clouds through the Fermi-LAT analysis and hadronic modeling. Methods. We performed the Fermi-LAT analysis to explore the GeV emission in and around the SNR. We explored the SNR physics with previously observed multi-wavelength data. We built a hadronic model using runaway CRs of the SNR to explain the GeV-TeV observation.Results. We found a hard GeV source (SrcX2) that is spatially coincident with both HESS J1858+020 and a molecular cloud complex at 3.6 kpc. In addition, a soft GeV source (SrcX1) was found at the northern edge of the SNR. The GeV spectrum of SrcX2 connects well with the TeV spectrum of HESS J1858+020. The entire γ-ray spectrum ranges from several GeV up to tens of TeV and it follows a power-law with an index of ∼2.15. We discuss several pieces of observational evidence to support the middle-aged SNR argument. Using runaway CRs from the SNR, our hadronic model explains the GeV-TeV emission at HESS J1858+020, with a diffusion coefficient that is much lower than the Galactic value.

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

Cited by 11 publications

References 42 publications

The H.E.S.S. Galactic plane survey

The H.E.S.S. Galactic plane survey

Using interstellar clouds to search for Galactic PeVatrons: gamma-ray signatures from supernova remnants

HESS J1858+020: A GeV-TeV source possibly powered by CRs from SNR G35.6-0.4

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