VLBI observations of 23 hot spots in the starburst galaxy M82

Bartel, N.; Ratner, M. I.; Rogers, A. E. E.; Shapiro, I. I.; Bonometti, R. J.; Cohen, N. L.; Gorenstein, M. V.; Marcaide, J. M.; Preston, R. A.

doi:10.1086/165847

Cited by 51 publications

(39 citation statements)

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“…2, this source has a distinct bi-polar structure, not typical of the more ring-like nature expected of supernova remnants. Observations of this source at 2.3 GHz and 5 GHz showed a structure indicative of an elongated shell, hence its initial classification as a SNR [13,14]. Further observations at 1.6 GHz using the EVN confirmed this elongated structure, sized 20×10 mas [10].…”

Section: 95+575mentioning

confidence: 91%

Supernova remnants in the central starburst region of M82

Fenech¹,

Muxlow

Beswick³

et al. 2007

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

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Global VLBI observations of the central kiloparsec of M82 at 1.6 GHz, attaining an angular resolution of 4 mas, were made on 3 Mar 2005. We present detailed images of four of the brightest, most compact supernova remnants as seen in these observations. These data are the fifth epoch of 1.6-GHz VLBI observations of M82, the first of which was made in December 1986, enabling study of these compact sources over a 19 year timescale. We will also discuss MERLIN 1.6-GHz observations made simultaneously, which have been combined with the global VLBI data, to produce high fidelity images of a large number of the known supernova remnants and HII regions in M82.8th European VLBI Network Symposium

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Section: 95+575mentioning

confidence: 91%

Supernova remnants in the central starburst region of M82

Fenech¹,

Muxlow

Beswick³

et al. 2007

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

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“…4) -and corresponding luminosities L 2.1−10 keV = 2.4 × 10 40 and 6 × 10 39 erg s −1 -imply populations of < ∼ 2.4 × 10 3 and < ∼ 600 luminous ( > ∼ 10 37 erg s −1 ) X-ray binaries (if the hard components are totally produced by X-ray binaries). This means that these local SBGs host a factor 4-16 times more high-luminosity X-ray binaries than the Galaxy: assuming a universal stellar IMF, a similar proportion holds between the respective SFRs (a compatible result is based on radio SN rates, see Bartel et al 1987). This estimate is compatible with the hypothesis of an X-ray-binary-related origin of the hard component of SBG spectra.…”

Section: Fig 2 Bepposax Spectrum Of M 82 With Superposed: (Top)mentioning

confidence: 98%

X-ray spectral components of starburst galaxies

Peršić

Rephaeli

2002

A&A

124

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Abstract. X-ray emission processes in starburst galaxies (SBGs) are assessed, with the aim of identifying and characterizing the main spectral components. Our survey of spectral properties, complemented with a model for the evolution of galactic stellar populations, leads to the prediction of a complex spectrum. Comparing the predicted spectral properties with current X-ray measurements of the nearby SBGs M 82 and N253, we draw the following tentative conclusions: 1) X-ray binaries with accreting neutron stars are the main contributors in the 2-15 keV band, and could be responsible for the yet uninterpreted hard component required to fit the observed 0.5-10 keV spectra of SBGs; 2) diffuse thermal plasma contributes at energies < ∼ 1 keV; 3) nonthermal emission, from Compton scattering of FIR and CMB radiation fields photons off supernova-accelerated relativistic electrons, and AGN-like emission, are likely be the dominant emission at energies > ∼ 30 keV; 4) supernova remnants make a relatively minor contribution to the X-ray continuum but may contribute appreciably to the Fe-K emission at 6.7 keV.

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“…The only other imaged radio supernova is SN 1986J, and its geometry is less circular than either SN 1993J or SN 1987A (Bartel et al 1991). Furthermore, young supernova remnants in M82 have been imaged, and they are also less circular (e.g., Pedlar et al 1999 ;Bartel et al 1987). Di †erent ejecta characteristics and/or circumstellar environments may have contributed to the asymmetries.…”

Section: Constraint On Asymmetry Of the Explosionmentioning

confidence: 99%

SN 1993J VLBI. I. The Center of the Explosion and a Limit on Anisotropic Expansion

Bietenholz

Bartel

Rupen

2001

ApJ

Self Cite

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Phase-referenced VLBI observations of supernova 1993J at 24 epochs, from 50 days after shock breakout to the present, allowed us to determine the coordinates of the explosion center relative to the quasistationary core of the host galaxy M81 with an accuracy of 45 kas and to determine the nominal proper motion of the geometric center of the radio shell with an accuracy of 9 kas yr~1. The uncertainties correspond to 160 AU for the position and 160 km s~1 for the proper motion at the distance of the source of 3.63 Mpc. After correcting for the expected galactic proper motion of the supernova around the core of M81 using H I rotation curves, we obtain a peculiar proper motion of the radio shell center of only 320^160 km s~1 to the south, which limits any possible one-sided expansion of the shell. We also Ðnd that the shell is highly circular, the outer contours in fact being circular to within 3%. Combining our proper-motion values with the degree of circular symmetry, we Ðnd that the expansion of the shock front from the explosion center is isotropic to within 5.5% in the plane of the sky. This is a more fundamental result on isotropic expansion than can be derived from the circularity of the images alone. The brightness of the radio shell, however, varies along the ridge and systematically changes with time. The degree of isotropy in the expansion of the shock front contrasts with the asymmetries and polarization found in optical spectral lines. Asymmetric density distributions in the ejecta, or more likely in the circumstellar medium, are favored to reconcile the radio and optical results. We see no sign of any disklike density distribution of the circumstellar material, with the average axis ratio of the radio shell of SN 1993J being less than 1.04.

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VLBI observations of 23 hot spots in the starburst galaxy M82

Cited by 51 publications

References 0 publications

Supernova remnants in the central starburst region of M82

Supernova remnants in the central starburst region of M82

X-ray spectral components of starburst galaxies

SN 1993J VLBI. I. The Center of the Explosion and a Limit on Anisotropic Expansion

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