The structure of young supernova remnants in M82

Muxlow, T. W. B.; Pedlar, A.; Wilkinson, P. N.; Axon, D. J.; Sanders, E.; Bruyn, A. G. de

doi:10.1093/mnras/266.2.455

Cited by 206 publications

(235 citation statements)

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“…Using the same value for the bulk speed as above gives a travel distance of s c = 2.5 pc. Muxlow et al (1994) found an average size of 2.4 ± 1.0 pc for the compact sources in M 82. This value is by more than one order of magnitude smaller than the one for compact sources in the Large Magellanic Cloud or the Milky Way, and therefore magnetic field strength in the mG regime is a reasonable value.…”

Section: Building Up the Halomentioning

confidence: 90%

“…Remarkable is a slight shift of the emission maximum to the west, which is visible in the higher frequency images due to their better resolution. This seems to be a consequence of the higher starforming activity in the western part of the central region of the galaxy (Muxlow et al 1994) and might even cause the difference between the extent of the spurs in the northern region. The most extended feature reaching up to ∼4.5 kpc into the halo is positioned directly north of this region.…”

Section: Radial Total Intensity Profilementioning

confidence: 99%

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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: Building Up the Halomentioning

confidence: 90%

Section: Radial Total Intensity Profilementioning

confidence: 99%

M 82 – A radio continuum and polarisation study

Adebahr

Krause

Klein

et al. 2013

A&A

104

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“…Coupled stellar population synthesis and photoionization models reveal two major episodes of star formation over the past 10 Myr (Förster Schreiber et al 2003). Numerous young supernova remnants have been detected (Muxlow et al 1994). Another peak of star formation about 150 Myr ago is inferred from the age-dating of stellar clusters (Konstantopoulos et al 2009), and 200 super star clusters, signposts of starbursts, have been found in M 82 (Melo et al 2005), spanning a wide age interval from 60 Myr to several Gyr (Gallagher & Smith 1999;de Grijs et al 2001).…”

Section: Introductionmentioning

confidence: 99%

SPIRE imaging of M 82: Cool dust in the wind and tidal streams

Roussel¹,

Wilson

Vigroux³

et al. 2010

A&A

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M 82 is a unique representative of a whole class of galaxies, starbursts with superwinds, in the Very Nearby Galaxy Survey with Herschel. In addition, its interaction with the M 81 group has stripped a significant portion of its interstellar medium from its disk. SPIRE maps now afford better characterization of the far-infrared emission from cool dust outside the disk, and sketch a far more complete picture of its mass distribution and energetics than previously possible. They show emission coincident in projection with the starburst wind and in a large halo, much more extended than the PAH band emission seen with Spitzer. Some complex substructures coincide with the brightest PAH filaments, and others with tidal streams seen in atomic hydrogen. We subtract the far-infrared emission of the starburst and underlying disk from the maps, and derive spatially-resolved far-infrared colors for the wind and halo. We interpret the results in terms of dust mass, dust temperature, and global physical conditions. In particular, we examine variations in the dust physical properties as a function of distance from the center and the wind polar axis, and conclude that more than two thirds of the extraplanar dust has been removed by tidal interaction, and not entrained by the starburst wind.

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“…Early high-resolution radio observations by Unger et al [1] and Kronberg et al [2,4] identified these sources as population of supernovae and supernova remnants. Later, more detailed work ( [3,6]) have shown that these sources are a mixture of supernova remnants and compact HII regions.…”

Section: Radio Imaging Of Nearby Supernovae and Supernova Remnants 4mentioning

confidence: 99%

“…In many nearby galaxies with high star-formation rates, such as M82 and Arp220, numerous compact radio sources are detected [1,2,3,4,5]. In these highly dust obscured regions, which incidentally is were a large amount of the Universe's star-formation is occurring, the extinction free nature of radio observations, mean that they are the only method by which these regions can be studied.…”

Section: Introductionmentioning

confidence: 99%

Radio supernovae

Beswick¹

2007

Proceedings of 8th European VLBI Network Symposium — PoS(8thEVN)

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I will briefly review the current status of radio observations of nearby supernovae and their remnants. This review will initially address observations of the radio 'light' curves of nearby corecollapse supernovae, followed by a more detailed summary of recent Very Long Baseline Interferometric observations of the expansion of nearby supernovae and their remnants. These later sections will concentrate on a few sources, namely those found in M82, SN1993J, and the recent supernova 2004et. In addition, I will discuss the many radio detections of supernovae found in the highly obscured centres of starburst galaxies, such as M82 and Arp220, where no optical detections are possible.

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The structure of young supernova remnants in M82

Cited by 206 publications

References 0 publications

M 82 – A radio continuum and polarisation study

M 82 – A radio continuum and polarisation study

SPIRE imaging of M 82: Cool dust in the wind and tidal streams

Radio supernovae

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