On the multiplicity of supernovae within host galaxies

Anderson, J. P.; Soto, M. G.

doi:10.1051/0004-6361/201220600

Cited by 22 publications

(28 citation statements)

References 67 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…NGC 6946 and 4303 hosted nine and six type II SNe, respectively, and only one (1948B) and two (1999gn and 2006ov) exploded in spiral arms; the rest exploded in interarm regions or outside the detectable stellar disk (Figs. 9 and 11 of Anderson & Soto 2013). This is consistent with the spiral density wave theory and the migration scenario described above.…”

Section: Type II Sn 2003gd 2013ej and 2019krlsupporting

confidence: 90%

Connection of supernovae 2002ap, 2003gd, 2013ej, and 2019krl in M 74 with atomic gas accretion and spiral structure

Michałowski

Gotkiewicz

Hjorth

et al. 2020

A&A

View full text Add to dashboard Cite

Studying the nature of various types of supernovae (SNe) is important for our understanding of stellar evolution. Observations of atomic and molecular gas in the host galaxies of gamma-ray bursts (GRBs) and SNe have recently been used to learn about the nature of the explosions themselves and the star formation events during which their progenitors were born. Based on archival data for M 74, which previously has not been investigated in the context of SN positions, we report the gas properties in the environment of the broad-lined type Ic (Ic-BL) SN 2002ap and the type II SNe 2003gd, 2013ej, and 2019krl. The SN 2002ap is located at the end of an off-centre, asymmetric, 55 kpc-long HI extension containing 7.5% of the total atomic gas in M 74, interpreted as a signature of external gas accretion. It is the fourth known case of an explosion of a presumably massive star located close to a concentration of atomic gas (after GRBs 980425, 060505, and SN 2009bb). It is unlikely that all these associations are random (at a 3σ significance), so the case of SN 2002ap adds to the evidence that the birth of the progenitors of type Ic-BL SNe and GRBs is connected with the accretion of atomic gas from the intergalactic medium. The HI extension could come from tidally disrupted companions of M 74, or be a remnant of a galaxy or a gas cloud that accreted entirely from the intragroup medium. The other (type II) SNe in M 74 are located at the outside edge of a spiral arm. This suggests that either their progenitors were born when gas was piling up there or that the SN progenitors moved away from the arm due to their orbital motions. These type II SNe do not seem to be related to gas accretion.

show abstract

Section: Type II Sn 2003gd 2013ej and 2019krlsupporting

confidence: 90%

Connection of supernovae 2002ap, 2003gd, 2013ej, and 2019krl in M 74 with atomic gas accretion and spiral structure

Michałowski

Gotkiewicz

Hjorth

et al. 2020

A&A

View full text Add to dashboard Cite

show abstract

“…With an extended galaxy sample, Anderson & Soto (2013) found that the hosts in which only a single CCSN has been found have a median absolute magnitude as low as −20.64 in B (also see Taddia et al 2013 for the cumulative distribution of the B magnitudes of the host galaxies of CCSNe). The host of SN 2012aa has absolute B magnitude ∼ −18.13.…”

Section: Comparison Of Host Propertiesmentioning

confidence: 97%

SN 2012aa: A transient between Type Ibc core-collapse and superluminous supernovae

Roy

Sollerman

Silverman

et al. 2016

A&A

View full text Add to dashboard Cite

Context. Research on supernovae (SNe) over the past decade has confirmed that there is a distinct class of events which are much more luminous (by ∼ 2 mag) than canonical core-collapse SNe (CCSNe). These events with visual peak magnitudes −21 are called superluminous SNe (SLSNe). The mechanism for powering the light curves of SLSNe is still not well understood. The proposed scenarios are circumstellar interaction, the emergence of a magnetar after core collapse, or disruption of a massive star through pair production.Aims. There are a few intermediate events which have luminosities between these two classes. They are important for constraining the nature of the progenitors of these two different populations as well as their environments and powering mechanisms. Here we study one such object, SN 2012aa. Methods. We observed and analysed the evolution of the luminous Type Ic SN 2012aa. The event was discovered by the Lick Observatory Supernova Search in an anonymous (z ≈ 0.08) galaxy. The optical photometric and spectroscopic follow-up observations were conducted over a time span of about 120 days. Results. With an absolute V -band peak of ∼ −20 mag, the SN is an intermediate-luminosity transient between regular SNe Ibc and SLSNe. SN 2012aa also exhibits an unusual secondary bump after the maximum in its light curve. For SN 2012aa, we interpret this as a manifestation of SN-shock interaction with the circumstellar medium (CSM). If we would assume a 56 Ni-powered ejecta, the quasi-bolometric light curve requires roughly 1.3 M of 56 Ni and an ejected mass of ∼ 14 M . This would also imply a high kinetic energy of the explosion, ∼ 5.4 × 10 51 ergs. On the other hand, the unusually broad light curve along with the secondary peak indicate the possibility of interaction with CSM. The third alternative is the presence of a central engine releasing spin energy that eventually powers the light curve over a long time. The host of SN 2012aa is a star-forming Sa/Sb/Sbc galaxy. Conclusions. Although the spectral properties of SN 2012aa and its velocity evolution are comparable to those of normal SNe Ibc, its broad light curve along with a large peak luminosity distinguish it from canonical CCSNe, suggesting the event to be an intermediateluminosity transient between CCSNe and SLSNe at least in terms of peak luminosity. Comparing to other SNe, we argue that SN 2012aa belongs to a subclass where CSM interaction plays a significant role in powering the SN, at least during the initial stages of evolution.

show abstract

“…For the SN rate we use the list of SN from Anderson & Soto (2013) and supplement it with SN 2017eaw (Kilpatrick & Foley 2018) and N6946-BH1 (Adams et al 2017). In the 102 years up to 2018 there have been a total of 11 core-collapse events and thus a supernova rate of 0.108 ± 0.033yr −1 , assuming the errors in the counting of the number of SNe is described by a Poisson distribution.…”

Section: Distance From the Supernova Ratementioning

confidence: 99%

“…Today most supernovae are discovered in distant galaxies and in most of these there is only one event per galaxy. There are several galaxies that have two or more observed SNe (Anderson & Soto 2013). The most extreme example is that of NGC 6946, the "Fireworks" galaxy.…”

Section: Introductionmentioning

confidence: 99%

“…The most extreme example is that of NGC 6946, the "Fireworks" galaxy. There have been 10 observed core-collapse SNe since 1917 and recently a candidate core-collapse event with no SN luminous display due to black-hole formation was discovered (Anderson & Soto 2013;Adams et al 2017;Dong & Stanek 2017). This high rate of SNe is unique and provides a novel avenue to place a constraint on the star formation rate and distance to the galaxy.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The distance, supernova rate, and supernova progenitors of NGC 6946

Eldridge

Xiao

2019

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

The distance to the fireworks galaxy NGC 6946 is highly uncertain. Recent distance estimates using the tip of the red giant branch of 7.7 to 7.8 Mpc are larger than the distance commonly assumed for studying supernovae in this galaxy of 5.9 Mpc. Here we use the high supernova rate of the galaxy to derive the star-formation rate and predict the galaxy's FUV flux. We also account for dust extinction by different methods to derive a distance of 7.9±4.0 Mpc for NGC 6946. We then use the new distance to re-evaluate the understanding of the supernova progenitors 2002hh, 2004et, 2017eaw, the possible electron capture event 2008S and the possible black-hole forming event N6946-BH1. For the latter two exotic events the new distance improves the consistency between the observed progenitors and the stellar models that give rise to these events. From our findings we strongly recommend that all future studies of NGC 6946 must use the greater distance to the galaxy of 7.72 ± 0.32 Mpc of Anand et al. (2018).

show abstract

On the multiplicity of supernovae within host galaxies

Cited by 22 publications

References 67 publications

Connection of supernovae 2002ap, 2003gd, 2013ej, and 2019krl in M 74 with atomic gas accretion and spiral structure

Connection of supernovae 2002ap, 2003gd, 2013ej, and 2019krl in M 74 with atomic gas accretion and spiral structure

SN 2012aa: A transient between Type Ibc core-collapse and superluminous supernovae

The distance, supernova rate, and supernova progenitors of NGC 6946

Contact Info

Product

Resources

About