We assemble a large set of 2-10 GHz radio flux density measurements and upper limits of 294 different supernovae (SNe), from the literature and our own and archival data. Only 31% of the SNe were detected. We characterize the SN lightcurves near the peak using a two-parameter model, with tpk being the time to rise to a peak and Lpk the spectral luminosity at that peak. Over all SNe in our sample at D<100 Mpc, we find that tpk=101.7±0.9 d, and that Lpk=1025.5±1.6 erg s−1 Hz−1, and therefore that generally, 50% of SNe will have Lpk<1025.5 erg s−1 Hz−1. These Lpk values are ~30 times lower than those for only detected SNe. Types I b/c and II (excluding IIn's) have similar mean values of Lpk but the former have a wider range, whereas Type IIn SNe have ~10 times higher values with Lpk=1026.5±1.1 erg s−1 Hz−1. As for tpk, Type I b/c have tpk of only 101.1±0.5 d while Type II have tpk=101.6±1.0 and Type IIn the longest timescales with tpk=103.1±0.7 d. We also estimate the distribution of progenitor mass-loss rates, M˙, and find the mean and standard deviation of log10(M˙/Msol) yr−1 are −5.4±1.2 (assuming vwind=1000 km s−1) for Type I~b/c SNe, and −6.9±1.4 (assuming vwind=10 km s−1 for Type II SNe excluding Type IIn.

The Radio Luminosity-Risetime Function of Core-Collapse Supernovae

The results of multi-epoch observations of the southern starburst galaxy, NGC 253, with the Australian Long Baseline Array at 2.3 GHz are presented. As with previous radio interferometric observations of this galaxy, no new sources were discovered. By combining the results of this survey with Very Large Array observations at higher frequencies from the literature, spectra were derived and a free-free absorption model was fitted of 20 known sources in NGC 253. The results were found to be consistent with previous studies. The supernova remnant, 5.48-43.3, was imaged with the highest sensitivity and resolution to date, revealing a two-lobed morphology. Comparisons with previous observations of similar resolution give an upper limit of 104 km s–1 for the expansion speed of this remnant. We derive a supernova rate of <0.2 yr–1 for the inner 300 pc using a model that improves on previous methods by incorporating an improved radio supernova peak luminosity distribution and by making use of multi-wavelength radio data spanning 21 yr. A star formation rate of SFR(M ≥ 5 M ☉) < 4.9 M ☉ yr–1 was also estimated using the standard relation between supernova and star formation rates. Our improved estimates of supernova and star formation rates are consistent with studies at other wavelengths. The results of our study point to the possible existence of a small population of undetected supernova remnants, suggesting a low rate of radio supernova production in NGC 253.

Multi-epoch very long baseline interferometric observations of the nuclear starburst region of ngc 253: improved modeling of the supernova and star formation rates

Supernova 2010as in NGC 6000

Supernova 2008bk in NGC 7793

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Supernova 2010as in NGC 6000

Supernova 2008bk in NGC 7793