Erratum: “Infrared Fabry‐Perot Imaging of M82 [Fe<scp>ii</scp>] Emission. II. Tracing Extragalactic Supernova Remnants” (ApJ, 476, 105 [1997])

Greenhouse, Matthew A.; Satyapal, S.; Woodward, C. E.; Fischer, J.; Thompson, K. L.; Forrest, W. J.; Pipher, J. L.; Raines, S. N.; Smith, Hazel; Watson, D. M.; Rudy, R. J.

doi:10.1086/304432

Cited by 15 publications

(26 citation statements)

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“…We suspect that the remnants are primarily interacting with a low density gas, and the [Fe II] emission is from radiative shock waves in clouds. The positions of the remnants extend to a larger distance from the center of M82 than do the radio remnants (Greenhouse et al 1997). The [Fe II] remnants should be weak nonthermal radio sources; based on the surface brightness -diameter relation approximately followed by radio remnants (Huang et al 1994), we estimate radio fluxes of ∼ 0.01 − 0.04 mJy.…”

Section: The Compact Remnants In M82mentioning

confidence: 80%

“…The [Fe II] remnants should be weak nonthermal radio sources; based on the surface brightness -diameter relation approximately followed by radio remnants (Huang et al 1994), we estimate radio fluxes of ∼ 0.01 − 0.04 mJy. As noted by Greenhouse et al (1997), the high radio background in M82 makes faint sources difficult to detect. Ulvestad & Antonucci (1997) have studied compact radio sources in NGC 253 with a resolution of 1 pc.…”

Section: The Compact Remnants In M82mentioning

confidence: 99%

“…However, we estimate that the line is somewhat below the expected detection limit of the AIRES echelle spectrograph on SOFIA. Greenhouse et al (1997) have detected 6 sources of [Fe II] 1.2 and 1.6 µm line emission that they identify as shock emission from supernova remnants. The emission does not coincide with that from the radio remnants.…”

Section: The Compact Remnants In M82mentioning

confidence: 99%

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The Nature of the Compact Supernova Remnants in Starburst Galaxies

Chevalier

Fransson²

2001

The Astrophysical Journal

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Radio observations of starburst regions in galaxies have revealed groups of compact nonthermal sources that may be radiative supernova remnants expanding in the interclump medium of molecular clouds. Because of the high pressure in starburst regions, the interclump medium may have a density ~ 10^3 H atoms cm^{-3} in a starburst nucleus like M82 and ~ 10^4 H atoms cm^{-3} in an ultraluminous galaxy like Arp 220. In M82, our model can account for the sizes, the slow evolution, the high radio luminosities, and the low X-ray luminosities of the sources. We predict expansion velocities ~ 500 km/s, which is slower than the one case measured by VLBI techniques. Although we predict the remnants to be radiative, the expected radiation is difficult to detect because it is at infrared wavelengths and the starburst is itself very luminous; one detection possibility is broad [OI] 63 micron line emission at the positions of the radio remnants. The more luminous and compact remnants in Arp 220 can be accounted for by the higher molecular cloud density. In our model, the observed remnants lose most of the supernova energy to radiation. Other explosions in a lower density medium may directly heat a hot, low density interstellar component, leading to the superwinds that are associated with starburst regions.Comment: 11 pages, 1 figure, ApJ submitte

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Section: The Compact Remnants In M82mentioning

confidence: 80%

Section: The Compact Remnants In M82mentioning

confidence: 99%

Section: The Compact Remnants In M82mentioning

confidence: 99%

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The Nature of the Compact Supernova Remnants in Starburst Galaxies

Chevalier

Fransson²

2001

The Astrophysical Journal

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“…Radio continuum and [FeII] emission do not always correspond, even in a specific SNR. For instance, Greenhouse et al (1997) find that there is little correlation between the radio continuum and [FeII] line emission in radio-loud SNRs in M 82 and suggest that the SNR emission characteristics change as a function of age. In addition, Alonso-Herrero et al (2003) obtained high-resolution HST [FeII] images of M 82 and NGC 253 and find compact [FeII] emission in only 30-50% of radio all SNRs.…”

Section: Introductionmentioning

confidence: 99%

[FeII] as a tracer of supernova rate in nearby starburst galaxies

Rosenberg

Werf

Israel

2012

A&A

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Context. Supernovae play an integral role in the feedback of processed material into the ISM of galaxies making them responsible for much of the chemical enrichment of the universe. The rate of supernovae can also reveal star formation histories. These rates are usually measured through the nonthermal radio continuum luminosity; however, a correlation between near-infrared [FeII] emission and supernova remnants has also been noted. Aims. We aim to find a quantitative relationship between the [FeII] at 1.26 μm ([FeII] 1.26 ) luminosity and the supernova rate in a sample of 11 nearby starburst galaxy centers. Methods. We performed a pixel-pixel analysis of this correlation on SINFONI data cubes. Using Brγ equivalent width and luminosity as the only observational inputs into the Starburst 99 model, we derived the supernova rate at each pixel and have thus created maps of supernova rates. We then compared these morphologically and quantitatively to the [FeII] 1.26 luminosity. Results. We have found that a strong linear and morphological correlation exists between supernova rate and [FeII] 1.26 on a pixel-topixel basis. This relation is valid for normal star-forming galaxies but breaks down for extreme ultraluminous galaxies. Conclusions. The supernova rates derived from the Starburst 99 model are in good agreement with the radio derived supernova rates, which underlines the strength of using [FeII] emission as a tracer of supernova rate. With the strong correlation found in this sample of galaxies, we conclude that [FeII] 1.26 emission can generally be used to derive accurate supernova rates on either a pixel-pixel or integrated galactic basis.

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“…For galaxies dominated by typical stellar UV fields, a simple linear proportionality between the [ Ne ii] luminosity and the Lyman continuum luminosity is expected from photoionization models . Measurements of the [ Fe ii]/[ Ne ii] emission-line ratio in starburst galaxies could thus provide a sensitive measure of the supernova content of galaxies (Greenhouse et al 1991(Greenhouse et al , 1996Moorwood & Oliva 1988) and hence an estimate of the degree of grain processing and destruction. Furthermore, an increased SN rate or shock wave intensity, indicated by a higher [ Fe ii]/[ Ne ii], would be highly suggestive that in low-metallicity galaxies destruction by SN shocks is responsible for the absence of PAHs.…”

Section: Introductionmentioning

confidence: 99%