Gamma rays from star-forming regions

Romero, Gustavo E.

doi:10.1063/1.3076825

Cited by 5 publications

(6 citation statements)

References 39 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For instance, the Herbig-Haro objects HH 219 (Hewitt et al 2012) and HH 80-81 (Yan et al 2022) have been identified as potential GeV sources. Efficient particle acceleration in star-forming regions is also expected to arise from the combined action of several protostars and young stellar clusters (Romero 2008), or by the collective action of the stellar winds of young A195, page 8 of 10 Duvidovich, L., and Petriella, A.: A&A proofs, manuscript no. aa45819-22 massive stars and SNRs within super-bubbles (Aharonian et al 2019).…”

Section: Discussionmentioning

confidence: 99%

Radio and infrared study of the supernova remnant candidate HESS J1912+101

Duvidovich

Petriella

2023

A&A

View full text Add to dashboard Cite

Aims. We provide new insights into the γ-ray emission from HESS J1912+101, a TeV supernova remnant candidate probably associated with the radio pulsar PSR J1913+1011. Methods. We obtained new observations at 1.5 GHz using the VLA in the D configuration, with the purpose of detecting the radio shell of the putative remnant. In addition, we observed a single pointing at 6.0 GHz toward PSR J1913+1011 to look for a radio pulsar wind nebula. We also studied the properties of the surrounding interstellar medium using data of the 13CO, HI, and infrared emissions, obtained from public surveys. Results. We do not find evidence of a radio shell down to the sensitivity of the new image at 1.5 GHz. We detect faint diffuse emission around PSR J1913+1011 at 6.0 GHz, which could represent a radio pulsar wind nebula powered by the pulsar. We find dense ambient gas at ~60 km s−1, which shows a good spatial correspondence with the TeV emission only in the western and eastern directions. There is also dense gas near the center of HESS J1912+101, where the TeV emission is weak. Using infrared data, we identify an active star-forming region in the western part of the shell. Conclusions. Based on the poor spatial match between the ambient gas and the TeV emission (which shows a good correlation in the western and eastern directions and an anticorrelation in the other directions), we conclude that the hadronic mechanism alone does not give a satisfactory explanation of the γ rays from HESS J1912+101. Additional contributions may come from leptonic processes in the shell of the supernova remnant, together with contributions from PSR J1913+1011 and its pulsar wind nebula and/or from the star-forming region. A confident determination of the distance to the putative remnant is necessary to determine whether these sources are associated or just appear superimposed in the line of sight.

show abstract

Section: Discussionmentioning

confidence: 99%

Radio and infrared study of the supernova remnant candidate HESS J1912+101

Duvidovich

Petriella

2023

A&A

View full text Add to dashboard Cite

show abstract

“…A signature of high-energy emission is nonthermal radio emission because particles from the same population are likely to be involved in processes at both energy ranges, at the radio through synchrotron process, and at VHE emission through inverse-Compton scattering. Moreover, the determination of counterparts of gamma-ray sources through radio observations in star-forming regions will help to clarify the role of young stars and collective wind effects in the acceleration of galactic cosmic rays (e.g., Romero et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Cygnus survey with the Giant Metrewave Radio Telescope at 325 and 610 MHz: the catalog

Benaglia

Ishwara‐Chandra

Intema

et al. 2020

A&A

View full text Add to dashboard Cite

Context. Observations at the radio continuum band below the gigahertz band are key when the nature and properties of nonthermal sources are investigated because their radio radiation is strongest at these frequencies. The low radio frequency range is therefore the best to spot possible counterparts to very high-energy (VHE) sources: relativistic particles of the same population are likely to be involved in radio and high-energy radiation processes. Some of these counterparts to VHE sources can be stellar sources. Aims. The Cygnus region in the northern sky is one of the richest in this type of sources that are potential counterparts to VHE sources. We surveyed the central ∼15 sq deg of the Cygnus constellation at the 325 and 610 MHz bands with angular resolutions and sensitivities of 10″ and 6″, and 0.5 and 0.2 mJy beam−1, respectively. Methods. The data were collected during 172 h in 2013–2017, using the Giant Metrewave Radio Telescope with 32 MHz bandwidth, and were calibrated using the SPAM routines. The source extraction was carried out with the PyBDSF tool, followed by verification through visual inspection of every putative catalog candidate source in order to determine its reliability. Results. In this first paper we present the catalog of sources, consisting of 1048 sources at 325 MHz and 2796 sources at 610 MHz. By cross-matching the sources from both frequencies with the objects of the SIMBAD database, we found possible counterparts for 143 of them. Most of the sources from the 325-MHz catalog (993) were detected at the 610 MHz band, and their spectral index α was computed adopting S(ν) ∝ να. The maximum of the spectral index distribution is at α = −1, which is characteristic of nonthermal emitters and might indicate an extragalactic population.

show abstract

“…Radio observations of protostars reveal thermal elongated jets. Strong shock waves created at end of the jets can accelerate charged particles [27]. The maximum energy to which particles are accelerated by these shock waves at the terminal ends is 3 TeV for the electrons and 60 TeV for the protons [27].…”

Section: Star Forming Regionsmentioning

confidence: 99%

“…Strong shock waves created at end of the jets can accelerate charged particles [27]. The maximum energy to which particles are accelerated by these shock waves at the terminal ends is 3 TeV for the electrons and 60 TeV for the protons [27]. Another process for particle acceleration could be due to colliding wind binaries after early massive stars are formed.…”

Section: Star Forming Regionsmentioning

confidence: 99%

“…When the strong winds of these stars collide with terminal velocities, strong shocks are created [28]. Thus, these colliding wind binaries can then accelerate electrons and protons via diffusive shock acceleration to the MeV-GeV energy range [27]. As the SFR evolves into stellar clusters and associations, CRs can be accelerated via two different ways.…”

Section: Star Forming Regionsmentioning

confidence: 99%

See 1 more Smart Citation

Cosmic-Ray Acceleration in the Cygnus OB2 Stellar Association

Hona¹

View full text Add to dashboard Cite

Gamma rays from star-forming regions

Cited by 5 publications

References 39 publications

Radio and infrared study of the supernova remnant candidate HESS J1912+101

Radio and infrared study of the supernova remnant candidate HESS J1912+101

Cygnus survey with the Giant Metrewave Radio Telescope at 325 and 610 MHz: the catalog

Cosmic-Ray Acceleration in the Cygnus OB2 Stellar Association

Contact Info

Product

Resources

About