Embedded star clusters as sources of high-energy cosmic rays

Maurin, G.; Marcowith, A.; Komin, Nu.; Krayzel, F.; Lamanna, G.

doi:10.1051/0004-6361/201628465

Cited by 15 publications

(13 citation statements)

References 44 publications

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“…SFRs are thus expected to be sites of efficient cosmic-ray acceleration through different processes (Bykov 2014). Models include diffusive acceleration by the shockwaves of SNRs (Caprioli 2015) and by the termination shock of massive stellar winds (Lang et al 2005), as well as stochastic acceleration by the magnetic turbulence induced by all those shockwaves (Bykov & Toptygin 2001;Maurin et al 2016). The Cygnus Cocoon is the only SFR firmly associated with an extended γ-ray source seen by the LAT (Ackermann et al 2011).…”

Section: Crab Nebula (Fhesj05345+2201)mentioning

confidence: 99%

The Search for Spatial Extension in High-latitude Sources Detected by the Fermi Large Area Telescope

Ackermann¹,

Ajello²,

Baldini³

et al. 2018

ApJS

187

162

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We present a search for spatial extension in high-latitude (>  | | b 5) sources in recent Fermi point source catalogs. The result is the Fermi High-Latitude Extended Sources Catalog, which provides source extensions (or upper limits thereof) and likelihood profiles for a suite of tested source morphologies. We find 24extended sources, 19 of which were not previously characterized as extended. These include sources that are potentially associated with supernova remnants and star-forming regions. We also found extended γ-ray emission in the vicinity of the CenA radio lobes and-at GeV energies for the first time-spatially coincident with the radio emission of the SNR CTA 1, as well as from the Crab Nebula. We also searched for halos around active galactic nuclei, which are predicted from electromagnetic cascades induced by the e + e − pairs that are deflected in intergalactic magnetic fields. These pairs are produced when γ-rays interact with background radiation fields. We do not find evidence for extension in individual sources or in stacked source samples. This enables us to place limits on the flux of the extended source components, which are then used to constrain the intergalactic magnetic field to be stronger than 3×10 −16 G for a coherence length λ10 kpc, even when conservative assumptions on the source duty cycle are made. This improves previous limits by several orders of magnitude.

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Section: Crab Nebula (Fhesj05345+2201)mentioning

confidence: 99%

The Search for Spatial Extension in High-latitude Sources Detected by the Fermi Large Area Telescope

Ackermann¹,

Ajello²,

Baldini³

et al. 2018

ApJS

187

162

View full text Add to dashboard Cite

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“…This would indicate that the particle acceleration in the Cygnus cocoon is not a special case and that other young massive SFRs have capabilities to accelerate particles via the same mechanism. However, a recent work by Maurin et al (2016) has shown that the H II regions powered by young stellar clusters such as the Rosetta and Orion Nebulae are not detected by the Fermi-LAT. This could be explained by the different bubble sizes; the G25 bubble and Cygnus cocoon are larger than the H II regions by more than an order of magnitude.…”

Section: Acceleration In Young Massive Sfrsmentioning

confidence: 99%

Extended Gamma-Ray Emission from the G25.0+0.0 Region: A Star-forming Region Powered by the Newly Found OB Association?

Katsuta

Uchiyama

Funk

2017

ApJ

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We report a study of extended γ-ray emission with the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope, which is likely to be the second case of a γ-ray detection from a star-forming region (SFR) in our Galaxy. The LAT source is located in the G25 region, 1. • 7×2. • 1 around (l, b) = (25. • 0, 0. • 0). The γ-ray emission is found to be composed of two extended sources and one point-like source. The extended sources have a similar sizes of about 1. • 4 × 0. • 6. An ∼ 0. • 4 diameter sub-region of one has a photon index of Γ = 1.53 ± 0.15; and is spatially coincident with HESS J1837−069, likely a pulsar wind nebula. The other parts of the extended sources have a photon index of Γ = 2.1 ± 0.2 without significant spectral curvature. Given their spatial and spectral properties, they have no clear associations with sources at other wavelengths. Their γ-ray properties are similar to those of the Cygnus cocoon SFR, the only firmly established γ-ray detection of an SFR in the Galaxy. Indeed, we find bubble-like structures of atomic and molecular gas in G25, which may be created by a putative OB association/cluster. The γ-ray emitting regions appear confined in the bubble-like structure; similar properties are also found in the Cygnus cocoon. In addition, using observations with the XMM-Newton we find a candidate young massive OB association/cluster G25.18+0.26 in the G25 region. We propose that the extended γ-ray emission in G25 is associated with an SFR driven by G25.18+0.26. Based on this scenario, we discuss possible acceleration processes in the SFR and compare them with the Cygnus cocoon.

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“…Notice, however, that the earlier census of a possible GeV emission from another sample of YMSCs did not lead to any significant gamma-ray signal (Maurin et al 2016). In that paper the authors analysed the Fermi telescope observations of YMSCs associated with the Rosette and Orion Nebulae (of luminosities below 10 37 erg s −1 ), NGC2175, NGC2467 and some others.…”

Section: Gamma Rays From Massive Star Clustersmentioning

confidence: 98%

“…The main damping process in HII regions is the turbulent damping (Farmer andGoldreich 2004, Lazarian 2016). We consider the following parameters: n g = 1000 cm −3 , the magnetic field B = 10 µG and gas temperature T ∼ 10 4 K (Maurin et al 2016 20 motions. The numerical modeling of this turbulence finds rms speed v t of the turbulent velocity of the order ∼ 10 km s −1 , slightly supersonic (Medina et al 2014).…”

Section: Supernova Remnants and Superbubblesmentioning

confidence: 99%

High-Energy Particles and Radiation in Star-Forming Regions

et al. 2020

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Non-thermal particles and high-energy radiation can play a role in the dynamical processes in star-forming regions and provide an important piece of the multiwavelength observational picture of their structure and components. Powerful stellar winds and supernovae in compact clusters of massive stars and OB associations are known to be favourable sites of high-energy particle acceleration and sources of non-thermal radiation and neutrinos. Namely, young massive stellar clusters are likely sources of the PeV (petaelectronvolt) regime cosmic rays (CRs). They can also be responsible for the cosmic ray composition, e.g., 22 Ne/ 20 Ne anomalous isotopic ratio in CRs. Efficient particle acceleration can be accompanied by super-adiabatic amplification of the fluctuating magnetic fields in the systems converting a part of kinetic power of the winds and supernovae into the magnetic energy through the CR-driven instabilities. The escape and CR propagation in the vicinity of the sources are affected by the non-linear CR feedback. These effects are expected to be important in starburst galaxies, which produce high-energy neutrinos and gamma-rays. We give a brief review of the theoreti-A. M. Bykov

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Embedded star clusters as sources of high-energy cosmic rays

Cited by 15 publications

References 44 publications

The Search for Spatial Extension in High-latitude Sources Detected by the Fermi Large Area Telescope

The Search for Spatial Extension in High-latitude Sources Detected by the Fermi Large Area Telescope

Extended Gamma-Ray Emission from the G25.0+0.0 Region: A Star-forming Region Powered by the Newly Found OB Association?

High-Energy Particles and Radiation in Star-Forming Regions

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