A search for radio supernovae and supernova remnants  
in the region of NGC 1569's super star clusters

Greve, A.; Tarchi, A.; Hüttemeister, Susanne; Grijs, Richard de; Hulst, J. M. van der; Garrington, S. T.; Neininger, N.

doi:10.1051/0004-6361:20011467

Cited by 32 publications

(78 citation statements)

References 40 publications

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“…However, in the case of NGC 1569, the SNRs were found to belong to the shallower sample. This result suggests that the SNRs in that galaxy are possibly more evolved, consistent with the hypothesis that NGC 1569 is currently in a post starburst stage of evolution (Greve et al 2002). Also, it indicates that the location on a Σ− D plot for a candidate radio SNR in a starburst galaxy (that is, in the shallower or steeper part of the plot) may originate from purely a "physical" evolutionary effect predicted by D&S.…”

Section: Evolutionary Tracks In the σ − D Planesupporting

confidence: 77%

“…Searches for radio supernovae and radio SNRs in these galaxies using observations made with MERLIN and the VLA are presented by Greve et al (2002) and Tarchi …”

Section: Ngc 1569 and Ngc 2146mentioning

confidence: 99%

“…Radio observations: LMC & SMC -at 1400 and 1420 MHz, respectively (Filipović et al 1998b); M 31 -at 1465 MHz (Braun & Walterbos 1993); M 33 -1420 MHz (Gordon et al 1999); IC 1613 -at 1460 MHz (Lozinskaya et al 1998); NGC 300 -at 1450 MHz (Pannuti et al 2000); NGC 6946 -at 1450 MHz (Lacey et al 1997); NGC 7793 -at 1470 MHz (Pannuti et al 2002); M 82 -at 8400 MHz (Huang et al 1994); NGC 1569 -at 1400 MHz (Greve et al 2002); NGC 2146 -at 1600 MHz (Tarchi et al 2000).…”

Section: Galaxymentioning

confidence: 99%

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The $\mathsf{\Sigma}$ – Drelation for supernova remnants in nearby galaxies

Urošević

Pannuti

Duric

et al. 2005

A&A

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Abstract. This paper examines relations between the radio surface brightness Σ and the diameter D (also known as Σ − D relations) for a sample of extragalactic supernova remnants (SNRs) as constructed from a combination of published data and data from our own surveys. Our sample of extragalactic SNRs is the largest ever devised for the purpose of analyzing Σ − D relations. The main results of this paper may be summarized as follows: (i) the empirical relations for SNRs in 10 of the 11 nearby galaxies studied have the approximately trivial Σ ∝ D −2 form, therefore limiting their interpretation as physically meaningful relations. In addition, these relations are subject to selection effects rendering them even less useful. Further Monte Carlo simulations suggest that the effect of survey sensitivity has the opposite effect of volume selection (e.g. Malmquist bias, a volume selection effect that shapes the Galactic sample) by tending to flatten the slopes toward a trivial relation. In this case, the true slopes may be steeper than the observed slopes; (ii) compact M 82 SNRs appear to follow a uniquely different Σ− D relation in comparison to the larger, older SNRs in the other 10 galaxies. Monte Carlo simulations suggest that the probability of this difference arising by chance is ≈1% to 10%, depending on what is assumed regarding the underlying SNR population; (iii) three candidate hypernova remnants were identified in our sample of 11 nearby galaxies.

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Section: Evolutionary Tracks In the σ − D Planesupporting

confidence: 77%

“…Searches for radio supernovae and radio SNRs in these galaxies using observations made with MERLIN and the VLA are presented by Greve et al (2002) and Tarchi …”

Section: Ngc 1569 and Ngc 2146mentioning

confidence: 99%

Section: Galaxymentioning

confidence: 99%

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The $\mathsf{\Sigma}$ – Drelation for supernova remnants in nearby galaxies

Urošević

Pannuti

Duric

et al. 2005

A&A

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“…Those authors also infer NGC 1569 to be a ''post-starburst'' system, which has been borne out by subsequent HST studies (e.g., Greggio et al 1998). Higher resolution observations presented in Greve et al (2002) and Lisenfeld et al (2004) find a largely thermal radio continuum, with the ''super star clusters'' (SSCs) being mostly thermal in nature. The thermal radio emission peaks coincide with the H maxima and not the stellar clusters, showing the locations of the most recent star formation.…”

Section: Radio Continuum Emission In Nearby Dwarf Starburst Galaxiesmentioning

confidence: 99%

The Nature of Radio Continuum Emission in the Dwarf Starburst Galaxy NGC 625

Cannon

Skillman²

2004

ApJ

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We present new multifrequency radio continuum imaging of the dwarf starburst galaxy NGC 625 obtained with the Very Large Array. Data at 20, 6, and 3.6 cm reveal global continuum emission dominated by free-free emission, with only mild synchrotron components. Each of the major H ii regions is detected; the individual spectral indices are thermal for the youngest regions (showing largest H emission) and nonthermal for the oldest. We do not detect any sources that appear to be associated with deeply embedded, dense, young clusters, although we have discovered one low-luminosity, obscured source that has no luminous optical counterpart and resides in the region of highest optical extinction. Since NGC 625 is a Wolf-Rayet galaxy with strong recent star formation, these radio properties suggest that the youngest star formation complexes have not yet evolved to the point where their thermal spectra are significantly contaminated by synchrotron emission. The nonthermal components are associated with regions of older star formation that have smaller ionized gas components. These results imply a range of ages for the H ii regions and radio components that agrees with our previous resolved stellar population analysis, where an extended burst of star formation has pervaded the disk of NGC 625 over the last $50 Myr. We compare the nature of radio continuum emission in selected nearby dwarf starburst and Wolf-Rayet galaxies, demonstrating that thermal radio continuum emission appears to be more common in these systems than in typical H ii galaxies with less recent star formation and more evolved stellar clusters.

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“…This structure corresponds to the western arm or filament 6 recognized in Hα images (Hodge 1974;Hunter et al 1993;Westmoquette et al 2008). The associated X-ray emission strongly infers that the filament was formed by the shock of a galactic outflow originating in the SSC A region of the disk (Martin 1998;Martin et al 2002;Greve et al 2002). Figure 2b shows the S7 image superimposed on the Hα emission in contours (Hunter & Elmegreen 2004).…”

Section: Imagingmentioning

confidence: 83%

Detection of unidentified infrared bands in a Hαfilament in the dwarf galaxy NGC 1569 with AKARI

Onaka

Matsumoto

Sakon

et al. 2010

A&A

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Context. We report the detection of unidentified infrared (UIR) bands in a filamentary structure associated with Hα emission in the starburst dwarf galaxy NGC 1569 based on imaging and spectroscopic observations of the AKARI satellite. Aims. We investigate the processing and destruction of the UIR band carriers in an outflow from NGC 1569. Methods. We performed observations of NGC 1569 for 6 infrared bands (3.2, 4.1, 7, 11, 15, and 24 μm) with the infrared camera (IRC) onboard AKARI. Near-to mid-infrared (2−13 μm) spectroscopy of a Hα filament was also carried out with the IRC. Results. The extended structure associated with a Hα filament appears bright at 7 μm. Since the IRC 7 μm band (S7) efficiently traces the 6.2 and 7.7 μm UIR band emission, the IRC imaging observations suggest that the filament is bright at the UIR band emission. Follow-up spectroscopic observations with the IRC confirm the presence of 6.2, 7.7, and 11.3 μm emission in the filament. The filament spectrum exhibits strong 11.3 μm UIR band emission relative to the 7.7 μm band compared to the galaxy disk observed with the infrared spectrograph on Spitzer. The near-infrared spectrum also suggests the presence of excess continuum emission in 2.5−5 μm in the filament. Conclusions. The presence of the UIR bands associated with a Hα filament is found by AKARI/IRC observations. The Hα filament is thought to have been formed by the galactic outflow originating from the star-formation activity in the disk of NGC 1569. The destruction timescale of the UIR band carriers in the outflow is estimated to be much shorter (∼1.3 × 10 3 yr) than the timescale of the outflow (∼5.3 Myr). Thus it is unlikely that the band carriers survive the outflow environment. Alternatively, we suggest that the band carriers in the filaments may be produced by the fragmentation of large carbonaceous grains in shocks, which produce the Hα emission. The NIR excess continuum emission cannot be accounted for by free-free emission alone and a hot dust contribution may be needed, although the free-free emission intensity estimated from H i recombination lines has a large uncertainty.

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A search for radio supernovae and supernova remnants in the region of NGC 1569's super star clusters

Cited by 32 publications

References 40 publications

The $\mathsf{\Sigma}$ – Drelation for supernova remnants in nearby galaxies

The $\mathsf{\Sigma}$ – Drelation for supernova remnants in nearby galaxies

The Nature of Radio Continuum Emission in the Dwarf Starburst Galaxy NGC 625

Detection of unidentified infrared bands in a Hαfilament in the dwarf galaxy NGC 1569 with AKARI

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