Wide-field Global VLBI and MERLIN combined monitoring of supernova remnants in M82

Fenech, Danielle; Beswick, R.; Muxlow, T. W. B.; Pedlar, A.; Argo, M. K.

doi:10.1111/j.1365-2966.2010.17144.x

Cited by 51 publications

(90 citation statements)

References 45 publications

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“…A large amount of flux in the core region of M 82 has been resolved into ∼100 independent discrete sources, which are a mixture of supernova remnants and ionised regions around newly forming star clusters (Fenech et al 2010;McDonald et al 2002;Wills et al 1997). The prior authors found indications that particles in these dense regions are suffering from free-free absorption processes inside these ionised regions and in the sources itself, which reduces the observed flux for low frequencies.…”

Section: Disentangling the Core And Halo Emissionmentioning

confidence: 99%

M 82 – A radio continuum and polarisation study

Adebahr

Krause

Klein

et al. 2013

A&A

104

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Context. The potential role of magnetic fields and cosmic ray propagation for feedback processes in the early Universe can be probed by studies of local starburst counterparts with an equivalent star-formation rate. Aims. In order to study the cosmic ray propagation and determine the magnetic field strength and dominant loss processes in the nearby prototypical starbursting galaxy M 82, a multi-frequency analysis at four radio wavelengths is presented. Methods. Archival data from the Westerbork Synthesis Radio Telescope (WSRT) was reduced and a new calibration technique introduced to reach the high dynamic ranges needed for the complex source morphology. These data were combined with archival Very Large Array (VLA) data, yielding total power maps at λ3 cm, λ6 cm, λ22 cm, and λ92 cm. Results. The data show a confinement of the emission at wavelengths of λ3/λ6 cm to the core region and a largely extended halo reaching up to 4 kpc away from the galaxy midplane at wavelengths of λ22/λ92 cm up to a sensitivity limit of 90 µJy and 1.8 mJy respectively indicating different physical processes in the core and halo regions. The results are used to calculate the magnetic field strength to 98 µG in the core region and to 24 µG in the halo regions. From the observation of ionisation losses, the filling factor of the ionised medium could be estimated to 2%. This leads to a revised view of the magnetic field distribution in the core region and the propagation processes from the core into the halo regions. Conclusions. We find that the radio emission from the core region is dominated by very dense H -regions and supernova remnants, while the surrounding medium is filled with hot X-ray and neutral gas. Cosmic rays radiating at frequencies higher than 1.4 GHz suffer from high synchrotron and inverse Compton losses in the core region and are not able to reach the halo. Even the cosmic rays radiating at longer wavelengths are only able to build up the observed kpc-sized halo, when several starbursting periods are assumed where the far-infrared and radio luminosity vary by an order of magnitude. These findings, together with the strong correlation between Hα, ionised polycyclic aromatic hydrocarbons (PAH + ), and our radio continuum data, suggest a magnetic field which is frozen into the ionised medium and driven out of the galaxy kinematically.

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Section: Disentangling the Core And Halo Emissionmentioning

confidence: 99%

M 82 – A radio continuum and polarisation study

Adebahr

Krause

Klein

et al. 2013

A&A

104

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“…One of the brightest RSN ever, SN1986J, has developed a complex and evolving morphology, and a spectrum which flattens over time (Bietenholz et al 2010a), however the lower limit on the expansion speed for the source in NGC 660 is significantly greater than the expansion seen in 1986J, or other nearby ordinary RSN which have been wellstudied on VLBI scales (e.g. Bartel et al 2002;Fenech et al 2010;Martí-Vidal et al 2011).…”

Section: A Single Luminous Radio Supernova/remnantmentioning

confidence: 99%

A new period of activity in the core of NGC 660

Argo

Bemmel

Connolly

et al. 2015

Mon. Not. R. Astron. Soc.

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The core of the nearby galaxy NGC 660 has recently undergone a spectacular radio outburst; using a combination of archival radio and Chandra X-ray data, together with new observations, the nature of this event is investigated. Radio observations made using e-MERLIN in mid-2013 show a new compact and extremely bright continuum source at the centre of the galaxy. High angular resolution observations carried out with the European VLBI Network show an obvious jet-like feature to the north east and evidence of a weak extension to the west, possibly a counter-jet. We also examine high angular resolution Hi spectra of these new sources, and the radio spectral energy distribution using the new wide-band capabilities of e-MERLIN. We compare the properties of the new object with possible explanations, concluding that we are seeing a period of new AGN activity in the core of this polar ring galaxy.

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“…SNRs in nearby galaxies, including the Andromeda Galaxy (M31 or NGC 224; Blair et al 1981;Sasaki et al 2012), NGC 300 (Millar et al 2012), M82 (Fenech et al 2010), NGC 4214 (Dopita et al 2010), NGC 5204, NGC 5585, NGC 6946, M81, andM101(Matonick &, have been studied recently. Therefore, Ia SNRs in these galaxies should be targeted for SC searches.…”

Section: Other Nearby Galaxiesmentioning

confidence: 99%

SEARCH FOR SURVIVING COMPANIONS IN TYPE Ia SUPERNOVA REMNANTS

Pan

Ricker

Taam

2014

ApJ

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The nature of the progenitor systems of type Ia supernovae (SNe Ia) is still unclear. One way to distinguish between the single-degenerate scenario and double-degenerate scenario for their progenitors is to search for the surviving companions (SCs). Using a technique that couples the results from multi-dimensional hydrodynamics simulations with calculations of the structure and evolution of main-sequence-(MS-) and helium-rich SCs, the color and magnitude of MS-and helium-rich SCs are predicted as functions of time. The SC candidates in Galactic type Ia supernova remnants (Ia SNR) and nearby extragalactic Ia SNRs are discussed. We find that the maximum detectable distance of MS SCs (helium-rich SCs) is 0.6-4 Mpc (0.4-16 Mpc), if the apparent magnitude limit is 27 in the absence of extinction, suggesting that the Large and Small Magellanic Clouds and the Andromeda Galaxy are excellent environments in which to search for SCs. However, only five Ia SNRs have been searched for SCs, showing little support for the standard channels in the singe-degenerate scenario. To better understand the progenitors of SNe Ia, we encourage the search for SCs in other nearby Ia SNRs.

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Wide-field Global VLBI and MERLIN combined monitoring of supernova remnants in M82

Cited by 51 publications

References 45 publications

M 82 – A radio continuum and polarisation study

M 82 – A radio continuum and polarisation study

A new period of activity in the core of NGC 660

SEARCH FOR SURVIVING COMPANIONS IN TYPE Ia SUPERNOVA REMNANTS

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