A New Optical Sample of Supernova Remnants in M33

Gordon, S.; Kirshner, R.; Long, Knox S.; Blair, William P.; Duric, Nebojsa; Smith, R. C.

doi:10.1086/313107

Cited by 76 publications

(150 citation statements)

References 48 publications

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“…The sample was obtained by selecting SNRs for which radio fluxes are given by Gordon et al (1999), X-ray fluxes by Pietsch et al (2004), and (optical) diameters by Gordon et al (1998). The X-ray survey of Plucinsky et al (2008), based on Chandra data, was also used to solve some cases of uncertain identification.…”

Section: Results From An Independent Sample: M 33mentioning

confidence: 99%

“…Using WebPIMMS 1 , a correction factor of ∼1.94 is evaluated: the precise value of this factor is not very important for our purposes, provided that the X-ray SNR spectra are not too different among themselves. Finally, a M 33 distance of 817 kpc (Freedman et al 2001) is assumed here; since Gordon et al (1998) use a distance of 840 kpc, for consistency we applied a small correction to their published SNR sizes. Here are our results, to be compared with those presented above.…”

Section: Results From An Independent Sample: M 33mentioning

confidence: 99%

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A statistical approach to radio emission from shell-type SNRs

Bandiera¹,

Petruk

2009

A&A

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Context. Shell-type supernova remnants (SNRs) exhibit correlations between radio surface brightness, SNR diameter, and ambient medium density, that between the first two quantities being the well known Σ-D relation. Aims. We investigate these correlations, to extract useful information about the typical evolutionary stage of radio SNRs, as well as to obtain insight into the origin of the relativistic electrons and magnetic fields responsible for the synchrotron emission observed in radio.Methods. We propose a scenario, according to which the observed correlations are the combined effect of SNRs evolving in a wide range of ambient conditions, rather than the evolutionary track of a "typical" SNR. We then develop a parametric approach to interpret the statistical data, and apply it to the data sample previously published by Berkhuijsen, as well as to a sample of SNRs in the galaxy M 33. Results. We find that SNRs cease to emit effectively in radio at a stage near the end of their Sedov evolution, and that models of synchrotron emission with constant efficiencies in particle acceleration and magnetic field amplification do not provide a close match to the data. We discuss the problem of the cumulative distribution in size, showing that the slope of this distribution does not relate to the expansion law of SNRs, as usually assumed, but only to the ambient density distribution. This solves a long-standing paradox: the almost linear cumulative distribution of SNRs led several authors to conclude that these SNRs are still in free expansion, which also implies very low ambient densities. Within this framework, we discuss the case of the starburst galaxy M 82. Conclusions. Statistical properties of SNR samples may be used to shed light on both the physics of electron acceleration and the evolution of SNRs. More precise results could be obtained by combining data of several surveys of SNRs in nearby galaxies.

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Section: Results From An Independent Sample: M 33mentioning

confidence: 99%

Section: Results From An Independent Sample: M 33mentioning

confidence: 99%

A statistical approach to radio emission from shell-type SNRs

Bandiera¹,

Petruk

2009

A&A

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“…Fig. 9 shows this correlation for confirmed SNRs in M83 and for those in three other nearby spiral galaxies with good spectrophotometry: M31 (Galarza et al 1999), M33 (Gordon et al 1998), and M81 (Lee et al 2015). The data for all the galaxies show the correlation, but the mean value is higher in M83 and the range seen in the M83 data is considerably larger than for the other galaxies, as is the scatter in values (especially at the high end of the correlation).…”

Section: Emission Line Diagnostics and Comparison With Shock Modelsmentioning

confidence: 86%

“…1.) In galaxies with abundance gradients, one usually sees a general decrease in the [N II]/Hα ratio with increasing GCD, albeit with significant scatter that may me due to factors such as varying shock conditions (Blair & Long 1997;Gordon et al 1998;Lee et al 2015) in additional to observational errors. M83 is unusual among local spirals in that its mean abundance levels are not only high, but are uniformly high over the bright optical disk, with only a slight metallicity gradient over the bright optical disk (Bresolin & Kennicutt 2002;Bresolin et al 2009).…”

Section: Emission Line Diagnostics and Comparison With Shock Modelsmentioning

confidence: 99%

A Spectroscopic Study of the Rich Supernova Remnant Population in M83^∗

Winkler

Blair

Long

2017

ApJ

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We report the results from a spectrophotometric study sampling the 300 candidate supernova remnants (SNRs) in M83 identified through optical imaging with Magellan/IMACS and HST/WFC3. Of the 118 candidates identified based on a high [S II] λλ 6716,6731 to Hα emission ratio, 117 show spectroscopic signatures of shock-heated gas, confirming them as SNRs-the largest uniform set of SNR spectra for any galaxy. Spectra of 22 objects with a high [O III] λ 5007 to Hα emission ratio, selected in an attempt to identify young ejecta-dominated SNRs like Cas A, reveal only one (previously reported) object with the broad ( 1000 km s −1 ) emission lines characteristic of ejecta-dominated SNRs, beyond the known SN1957D remnant. The other 20 [O III]-selected candidates include planetary nebulae, compact H II regions, and one background QSO. Although our spectroscopic sample includes 22 SNRs smaller than 11 pc, none of the other objects shows broad emission lines; instead their spectra stem from relatively slow (∼ 200 km s −1 ) radiative shocks propagating into the metal-rich interstellar medium of M83. With six SNe in the past century, one might expect more of M83's small-diameter SNRs to show evidence of ejecta; this appears not to be the case. We attribute their absence to several factors, including that SNRs expanding into a dense medium evolve quickly to the ISM-dominated phase, and that SNRs expanding into regions already evacuated by earlier SNe are probably very faint.

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“…If we correct for the mass ratio between our Galaxy and the galaxies M 31 and M 33, then we can expect of order 80 pulsars to be detected by a FAST survey of M 31 and about 3 pulsars in M 33. However, the supernova rate per unit mass in our Galaxy is thought to be higher than in M 31 and considerably lower than in M 33 (Berkhuijsen 1984;Gordon et al 1998). Also, since the angular extent of M 33 is about 1 quarter that of M 31, the number of pulsars found per pointing might not differ much between M 31 and M 33.…”

Section: Survey Of M 31 and M 33mentioning

confidence: 73%

Pulsar science with the Five hundred metre Aperture Spherical Telescope

Smits¹,

Lorimer

Krämer

et al. 2009

A&A

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With a collecting area of 70 000 m 2 , the Five hundred metre Aperture Spherical Telescope (FAST) will allow for great advances in pulsar astronomy. We have performed simulations to estimate the number of previously unknown pulsars FAST will find with its 19-beam or possibly 100-beam receivers for different survey strategies. With the 19-beam receiver, a total of 5200 previously unknown pulsars could be discovered in the Galactic plane, including about 460 millisecond pulsars (MSPs). Such a survey would take just over 200 days with eight hours survey time per day. We also estimate that, with about 80 six-hour days, a survey of M 31 and M 33 could yield 50-100 extra-Galactic pulsars. A 19-beam receiver would produce just under 500 MB of data per second and requires about 9 tera-ops to perform the major part of a real time analysis. We also simulate the logistics of high-precision timing of MSPs with FAST. Timing of the 50 brightest MSPs to a signal-to-noise of 500 would take about 24 h per epoch.

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A New Optical Sample of Supernova Remnants in M33

Cited by 76 publications

References 48 publications

A statistical approach to radio emission from shell-type SNRs

A statistical approach to radio emission from shell-type SNRs

A Spectroscopic Study of the Rich Supernova Remnant Population in M83^∗

Pulsar science with the Five hundred metre Aperture Spherical Telescope

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A New Optical Sample of Supernova Remnants in M33

Cited by 76 publications

References 48 publications

A statistical approach to radio emission from shell-type SNRs

A statistical approach to radio emission from shell-type SNRs

A Spectroscopic Study of the Rich Supernova Remnant Population in M83∗

Pulsar science with the Five hundred metre Aperture Spherical Telescope

Contact Info

Product

Resources

About

A Spectroscopic Study of the Rich Supernova Remnant Population in M83^∗