Kinematics: A Clean Diagnostic for Separating Supernova Remnants from H ii Regions in Nearby Galaxies

Points, Sean; Long, Knox S.; Winkler, P. F.; Blair, William P.

doi:10.3847/1538-4357/ab4e98

Cited by 19 publications

(14 citation statements)

References 31 publications

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“…As recently emphasized by Points et al (2019), with sufficiently high spectral resolution, SNRs (at least ones with significant shock velocities) can be separated from H II regions kinematically on the basis of their line widths. Indeed, Ideally all of the values would lie along the "dotted-dashed" curves, but modest scatter is present.…”

Section: Resultsmentioning

confidence: 93%

Supernova Remnants in M83 as Observed with MUSE

Long

Blair

Winkler

et al. 2022

ApJ

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Here we describe a new study of the supernova remnants (SNRs) and SNR candidates in nearby face-on spiral galaxy M83, based primarily on MUSE integral field spectroscopy. Our revised catalog of SNR candidates in M83 has 366 objects, 81 of which are reported here for the first time. Of these, 229 lie within the MUSE observation region, 160 of which have spectra with [S ii]:Hα ratios exceeding 0.4, the value generally accepted as confirmation that an emission nebula is shock-heated. Combined with 51 SNR candidates outside the MUSE region with high [S ii]:Hα ratios, there are 211 spectroscopically confirmed SNRs in M83, the largest number of confirmed SNRs in any external galaxy. MUSE’s combination of relatively high spectral resolution and broad wavelength coverage has allowed us to explore two other properties of SNRs that could serve as the basis of future SNR searches. Specifically, most of the objects identified as SNRs on the basis of [S ii]:Hα ratios exhibit more velocity broadening and lower ratios of [S iii]:[S ii] emission than H ii regions. A search for nebulae with the very broad emission lines expected from young, rapidly expanding remnants revealed none, except for the previously identified B12-174a. The SNRs identified in M83 are, with few exceptions, middle-aged interstellar medium (ISM) dominated ones. Smaller-diameter candidates show a larger range of velocity broadening and a larger range of gas densities than the larger-diameter objects, as expected if the SNRs expanding into denser gas brighten and then fade from view at smaller diameters than those expanding into a more tenuous ISM.

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Section: Resultsmentioning

confidence: 93%

Supernova Remnants in M83 as Observed with MUSE

Long

Blair

Winkler

et al. 2022

ApJ

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“…As recently emphasized by Points et al (2019), with sufficiently high spectral resolution, SNRs (at least ones with significant shock velocities) can be separated from H II regions kinematically on the basis of their line widths. Indeed, McLeod et al (2021) have used MUSE spectra to confirm a number of SNRs in NGC300.…”

Section: Comparison To Previous Spectramentioning

confidence: 93%

Supernova Remnants in M83 as Observed with MUSE

Long,

Blair,

Winkler

et al. 2022

Preprint

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Here we describe a new study of the SNRs and SNR candidates in nearby face-on spiral galaxy M83, based primarily on MUSE integral field spectroscopy. Our revised catalog of SNR candidates in M83 has 366 objects, 81 of which are reported here for the first time. Of these, 229 lie within the MUSE observation region, 160 of which have spectra with [S II]:Hα ratios exceeding 0.4, the value generally accepted as confirmation that an emission nebula is shock-heated. Combined with 51 SNR candidates outside the MUSE region with high [S II]:Hα ratios, there are 211 spectroscopically-confirmed SNRs in M83, the largest number of confirmed SNRs in any external galaxy. MUSE's combination of relatively high spectral resolution and broad wavelength coverage has allowed us to explore two other properties of SNRs that could serve as the basis of future SNR searches. Specifically, most of the objects identified as SNRs on the basis of [S II]:Hα ratios exhibit more velocity broadening and lower ratios of [S III]:[S II] emission than H II regions. A search for nebulae with the very broad emission lines expected from young, rapidly expanding remnants revealed none, except for the previously identified B12-174a. The SNRs identified in M83 are, with few exceptions, middle-aged ISMdominated ones. Smaller diameter candidates show a larger range of velocity broadening and a larger range of gas densities than the larger diameter objects, as expected if the SNRs expanding into denser gas brighten and then fade from view at smaller diameters than those expanding into a more tenuous ISM.

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“…The supernova remnants (SNRs) spectra (e.g., Long et al 2019) are of the AGN-like or the intermediate BPT types. The SNRs exibit the gas velocity dispersion higher than that in H II regions (e.g., Points et al 2019). Those characteristics of SNRs resemble that of the off-centered AGN-like spot in the galaxy M-8716-12703.…”

Section: Spot In the Galaxy M-8716-12703: Comparison To Agn In Galaxy...mentioning

confidence: 94%

MaNGA galaxies with off-centered spots of enhanced gas velocity dispersion

Pilyugin,

Cedres,

Zinchenko

et al. 2021

Preprint

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Off-centered spots of the enhanced gas velocity dispersion, σ, are revealed in some galaxies from the Mapping Nearby Galaxies at Apache Point Observatory survey (MaNGA). Aiming to clarify the origin of the spots of enhanced σ, we examine the distributions of the surface brightness, the line-of-sight velocity, the oxygen abundance, the gas velocity dispersion, and the Baldwin-Phillips-Terlevich (BPT) spaxel classification in seven galaxies. We find that the enhanced σ spots in six galaxies can be attributed to a (minor) interaction with a satellite. Three galaxies in our sample have a very close satellite (the separation in the sky plane is comparable to the optical radius of the galaxy). The spots of enhanced σ in those galaxies are located at the edge of the galaxy close to the satellite. The spots of enhanced σ in three other galaxies are related to bright spots in the photometric B band within the galaxy, which can be due to the projection of a satellite in the line of sight of the galaxy. The oxygen abundances in the spots in these three galaxies are reduced. This suggests that the low-metallicity gas from the satellite is mixed with the interstellar medium of the disk, that is, the gas exchange between the galaxy and its satellite takes place. The spectra of the spaxels within a spot are usually H II-region-like, suggesting that the interaction (gas infall) in those galaxies does not result in appreciable shocks. In contrast, the spot of the enhanced σ in the galaxy M-8716-12703 is associated with an off-centered active galactic nucleus-like (AGN-like) radiation distribution. One can suggest that the spot of the enhanced σ in the M-8716-12703 galaxy is different in origin, or that the characteristics of gas infall in this case differs from that in other galaxies.

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Kinematics: A Clean Diagnostic for Separating Supernova Remnants from H ii Regions in Nearby Galaxies

Cited by 19 publications

References 31 publications

Supernova Remnants in M83 as Observed with MUSE

Supernova Remnants in M83 as Observed with MUSE

Supernova Remnants in M83 as Observed with MUSE

MaNGA galaxies with off-centered spots of enhanced gas velocity dispersion

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