Low‐luminosity Type II supernovae: spectroscopic and photometric evolution

By A. Pastorello, L. Zampieri, Massimo Turatto, E. Cappellaro, W. Meikle, S. Benetti, D. Branch, Eddie Baron, Ferdinando Patat, M. Armstrong and 3 more. 2003

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In this paper we present spectroscopic and photometric observations for four core-collapsed supernovae (SNe), namely SNe 1994N, 1999br, 1999eu and 2001dc. Together with SN 1997D, we show that they form a group of exceptionally low-luminosity events. These SNe have narrow spectral lines (indicating low expansion velocities) and low luminosities at every phase (significantly lower than those of typical core-collapsed supernovae). The very-low luminosity during the 56 Co radioactive decay tail indicates that the mass of 56 Ni ejected during the explosion is much smaller (M Ni 2-8 x 10 -3 M ○. ) than the average (M Ni 6-10 x 10 -2 M ○. ). Two supernovae of this group (SN 1999br and SN 2001dc) were discovered very close to the explosion epoch, allowing us to determine the lengths of their plateaux (100 d) as well as establishing the explosion epochs of the other, less completely observed SNe. It is likely that this group of SNe represent the extreme low-luminosity tail of a single continuous distribution of Type II plateau supernovae events. Their kinetic energy is also exceptionally low. Although an origin from low-mass progenitors has also been proposed for low-luminosity core-collapsed SNe, recent work provides evidence in favour of the high-mass progenitor scenario. The incidence of these low-luminosity SNe could be as high as 4-5 per cent of all Type II SNe.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/8f5d14d632628103643cfe663dd237ede7c5d164

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Citations in the corpus

• THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, background): “0.01M⊙) low-velocity Type IIP SNe is SN 1997D (MV ≈ −14.7 mag; Turatto et al. 1998), and there are now more than a dozen similar CC SNe (see, e.g., Pastorello et al. 2004, 2006; Fraser et al. 2010b).”
• NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, background): “This is due to the inferred large envelope masses for the low-luminosity SNe II-P (∼ 14 − 40 M⊙, Hendry et al. 2005) that favor massive progenitors.”
• SN 2005cs in M51 – II. Complete evolution in the optical and the near-infrared (2009, methodology): “…particular, the evolution of the expansion velocities as derived from the P-Cygni minima of Hα and Sc II λ6246 nicely matches those of other events of this family (SNe 1997D, 1999br, 1999eu, 2001dc, 2002gd, 2003Z, Turatto et al. 1998; Benetti et al. 2001; Pastorello et al. 2004; Spiro et al. 2009).”
• Optical and near infrared coverage of SN 2004et: physical parameters and comparison with other type IIP supernovae (2009, methodology): “Figure 21 shows the photospheric velocity estimated from the Scii (6246 Å) line of SN 2004et compared with the velocities for three other type IIP SNe, SN 1999br (Pastorello et al. 2004),SN 1999em (Leonard et al. 2002a) and SN 2005cs (Pastorello et al. Figure 15.”
• Nearby Supernova Rates from the Lick Observatory Supernova Search. II. The Observed Luminosity Functions and Fractions of Supernovae in a Complete Sample (2010, background): “For example, SN 1999br (Pastorello et al. 2004) is an intrinsically faint SN IIP, while SN 2002hh (Pozzo et al. 2006) is a highly reddened SN II-P in the nearby galaxy NGC 6946.”
• CHARACTERIZING THE V-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE (2014, methodology): “However, there are definite outliers from this trend; e.g. subluminous SNe II tend to have red intrinsic colors at the end of the plateau (see e.g. Pastorello et al. 2004; Spiro et al. 2014), which, if one assumed were due to extinction would lead to corrections for unreasonable amounts of…”
• Progenitors of Core-Collapse Supernovae (2009, background): “The interpretation of Nomoto et al. (2006), Zampieri et al. (2003) and Pastorello et al. (2004) is that they are initially high mass stars which result in faint explosions (see Figure 11a).”
• Young Core-Collapse Supernova Remnants and Their Supernovae (2004, background): “…supernovae are inferred to have an explosion energy 1 ; 1051 ergs, there has recently been found a class of supernovae with energies of a few times 1049 ergs (Pastorello et al. 2004), as well as some SNe Ib/c and SNe IIn with energies up to a few times 1052 ergs (e.g., Nomoto et al. 2001).”
• TOWARD CHARACTERIZATION OF THE TYPE IIP SUPERNOVA PROGENITOR POPULATION: A STATISTICAL SAMPLE OF LIGHT CURVES FROM Pan-STARRS1 (2014, methodology): “Ejected Ni mass We estimate the ejected mass of radioactive 56Ni (MNi) by comparison to the late-time light curve of SN 1987A (see Figure 17), following the method of Pastorello et al. (2004).”
• Explosions of O-Ne-Mg cores, the Crab supernova, and subluminous type II-P supernovae (2005, background): “However, due to many uncertainties this connection is far from being clear (e.g., Pastorello et al. 2004, 2005; Hamuy 2003; Zampieri et al. 2003, and refs. therein).”
• THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. II. TYPE I GRB VERSUS TYPE II GRB OPTICAL AFTERGLOWS (2008, background): “Furthermore, the less constraining upper limits cannot exclude supernovae similar to the faintest local core-collapse events (cf. Richardson et al. 2002; Pastorello et al. 2004).”
• A novel explosive process is required for the γ-ray burst GRB 060614 (2006, background): “In fact, such a supernova would be fainter than any SN ever observed.(15) A conservative upper limit on the amount of synthesized Ni 56 is 8× 10 M⊙, more than two orders of magnitude less than the typical amount synthesized by long GRB/SNe.”
• Low luminosity Type II supernovae - II. Pointing towards moderate mass precursors (2014, methodology): “…SNe IIP presented in previous works i.e. SN 1994N, SN 1997D, SN 1999br, SN 1999eu, SN 2001dc, SN 2005cs (Turatto et al. 1998; Benetti et al. 2001; Pastorello et al. 2004, 2006, 2009) and other events recently published, i.e. SN 2008bk (Van Dyk et al. 2012; Pignata et al., in preparation), SN…”
• INTERACTING SUPERNOVAE AND SUPERNOVA IMPOSTORS: SN 2009ip, IS THIS THE END? (2012, background): “As highlighted by Mauerhan et al. (2012b), the spectra from September 10 to 23 (2012a event) do closely resemble those of type II SNe (the similarity with early spectra of the under-luminous type IIP SN 2005cs shown in their Figure 2 is remarkable).”
• The Zwicky Transient Facility Bright Transient Survey. II. A Public Statistical Sample for Exploring Supernova Demographics (2020, background): “A handful of similar events are known in the literature (e.g., Pastorello et al. 2004, 2009; GalYam et al. 2011).”
• The Unprecedented Third Outburst of SN 2009ip: A Luminous Blue Variable Becomes a Supernova (2012, background): “The initial peak absolute magnitude of −14.5 measured in the first week of September was, however, more luminous than that of some of the faintest known examples of corecollapse SNe II-P such as SN 1999br (Pastorello et al. 2004).”