The 2008 Luminous Optical Transient in the Nearby Galaxy NGC 300

Bond, Howard E.; Bedin, L. R.; Bonanos, A. Z.; Humphreys, R. M.; Monard, L. A. G.; Prieto, J. L.; Walter, Frederick M.

doi:10.1088/0004-637x/695/2/l154

Cited by 148 publications

(293 citation statements)

References 30 publications

Supporting

Mentioning

277

Contrasting

Order By: Relevance

“…It is enticing, though, that the amount of asymmetry seems to be inversely related to the hydrogen envelope mass , and references therein), which is consistent with the generally expected picture. If the hydrogen envelope buries all signs of a jet, even a weak amount of subsequent hydrogen recombination may produce a luminous red nova-like event (Kulkarni et al 2007;Bond et al 2009;Thompson et al 2009), as has been speculated by Quataert & Kasen (2012).…”

Section: Counterparts Of Events With Jet Formationmentioning

confidence: 86%

Gravitational Waves From Fallback Accretion Onto Neutron Stars

Piro

Thrane

2012

ApJ

View full text Add to dashboard Cite

Massive stars generally end their lives as neutron stars (NSs) or black holes (BHs), with NS formation typically occurring at the low-mass end and collapse to a BH more likely at the high-mass end. In an intermediate regime, with a mass range that depends on the uncertain details of rotation and mass loss during the star's life, an NS is initially formed, which then experiences fallback accretion and collapse to a BH. The electromagnetic consequence of such an event is not clear. Depending on the progenitor's structure, possibilities range from a long gamma-ray burst to a Type II supernova (which may or may not be jet powered) to a collapse with a weak electromagnetic signature. Gravitational waves (GWs) provide the exciting opportunity to peer through the envelope of a dying massive star and directly probe what is occurring inside. We explore whether fallback onto young NSs can be detected by ground-based interferometers. When the incoming material has sufficient angular momentum to form a disk, the accretion spins up the NS sufficiently to produce non-axisymmetric instabilities and gravitational radiation at frequencies of ∼700-2400 Hz for ∼30-3000 s until collapse to a BH occurs. Using a realistic excess cross-power search algorithm, we show that such events are detectable by Advanced LIGO out to ≈17 Mpc. From the rate of nearby core-collapse supernovae in the past five years, we estimate that there will be ∼1-2 events each year that are worth checking for fallback GWs. The observation of these unique GW signatures coincident with electromagnetic detections would identify the transient events that are associated with this channel of BH formation, while providing information about the protoneutron star progenitor.

show abstract

Section: Counterparts Of Events With Jet Formationmentioning

confidence: 86%

Gravitational Waves From Fallback Accretion Onto Neutron Stars

Piro

Thrane

2012

ApJ

View full text Add to dashboard Cite

show abstract

“…The heavily dust-enshrouded nature of the progenitor, and the low peak visual luminosity compared to core-collapse SNe, seem at first to suggest that SN 2010da was an intermediateluminosity transient similar to NGC300 OT2008-1 (Bond et al 2009;Humphreys et al 2011) and SN 2008S (Thompson et al 2009;Kochanek 2011). However, the post-outburst evolution of SN2010da is significantly different from those of SN2008S and NGC300 OT2008-1, both of which are prototypes of this class of transient.…”

Section: On the Nature Of Sn2010damentioning

confidence: 99%

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

Lau

Kasliwal

Bond

et al. 2016

ApJ

Self Cite

View full text Add to dashboard Cite

We present multi-epoch mid-infrared (IR) photometry and the optical discovery observations of the "impostor" supernova (SN) 2010da in NGC300 using new and archival Spitzer Space Telescope images and ground-based observatories. The mid-infrared counterpart of SN2010da was detected as Spitzer Infrared Intensive Transient Survey (SPIRITS)14bme in the SPIRITS, an ongoing systematic search for IR transients. Before erupting on 2010 May 24, the SN2010da progenitor exhibited a constant mid-IR flux at 3.6 and only a slight ∼10% decrease at 4.5 μm between 2003 November and 2007 December. A sharp increase in the 3.6 μm flux followed by a rapid decrease measured ∼150 days before and ∼80 days after the initial outburst, respectively, reveal a mid-IR counterpart to the coincident optical and high luminosity X-ray outbursts. At late times, after the outburst (∼2000 days), the 3.6 and 4.5 μm emission increased to over a factor of twotimes the progenitor flux and is currently observed (as of 2016 Feb) to be fading, but still above the progenitor flux. We attribute the re-brightening mid-IR emission to continued dust production and increasing luminosity of the surviving system associated with SN2010da. We analyze the evolution of the dust temperature (T d ∼700-1000 K), mass (M d ∼0.5-3.8×10 −7 M e ), luminosity (L IR ∼1.3-3.5×10 4 L e ), and the equilibrium temperature radius (R eq ∼6.4-12.2 au) in order to resolve the nature of SN2010da. We address the leading interpretation of SN2010da as an eruption from a luminous blue variable high-mass X-ray binary (HMXB) system. We propose that SN2010da is instead a supergiant (sg)B[e]-HMXB based on similar luminosities and dust masses exhibited by two other known sgB[e]-HMXB systems. Additionally, the SN2010da progenitor occupies a similar region on a mid-IR color-magnitude diagram (CMD) with known sgB[e] stars in the Large Magellanic Cloud. The lower limit estimated for the orbital eccentricity of the sgB[e]-HMXB (e>0.82) from X-ray luminosity measurements is high compared to known sgHMXBs and supports the claim that SN2010da may be associated with a newly formed HMXB system.

show abstract

“…Additionally there have been discoveries of 7 Luminous Blue Variables (LBVs) in outburst and three optical transients whose nature is still debated (SN 2008S, NGC 300-2008OT, SN2010da). A possible SN origin from a massive star (>7−8 M ) has been proposed for SN 2008S and NGC 300-2008OT by a number of authors (Prieto et al 2008;Thompson et al 2009;Botticella et al 2009;Pumo et al 2009;Kochanek 2011) but is disputed by others who favour an outbursting massive star event (Smith et al 2009;Berger et al 2009;Bond et al 2009;Humphreys et al 2011). To be conservative, we will not consider these two transients as genuine CC SNe in our main analysis but we will include them in our discussion of the detectability of CC SNe, since their faint detection magnitudes ( We restrict our comparison between the CC SN rate and the SFR estimates to the last 13 yr (1998)(1999)(2000)(2001)(2002)(2003)(2004)(2005)(2006)(2007)(2008)(2009)(2010), assuming a constant and continuous intensity level of surveillance (i.e., a control time of 13 years).…”

Section: Sn Samplementioning

confidence: 99%

A comparison between star formation rate diagnostics and rate of core collapse supernovae within 11 Mpc

Botticella

Smartt

Kennicutt

et al. 2012

A&A

119

135

View full text Add to dashboard Cite

Aims. The core collapse supernova rate provides a strong lower limit for the star formation rate (SFR). Progress in using it as a cosmic SFR tracer requires some confidence that it is consistent with more conventional SFR diagnostics in the nearby Universe. This paper compares standard SFR measurements based on Hα, far ultraviolet (FUV) and total infrared (TIR) galaxy luminosities with the observed core collapse supernova rate in the same galaxy sample. The comparison can be viewed from two perspectives. Firstly, by adopting an estimate of the minimum stellar mass to produce a core collapse supernova one can determine a SFR from supernova numbers. Secondly, the radiative SFR can be assumed to be robust and then the supernova statistics provide a constrain on the minimum stellar mass for core collapse supernova progenitors. Methods. The novel aspect of this study is that Hα, FUV and TIR luminosities are now available for a complete galaxy sample within the local 11 Mpc volume and the number of discovered supernovae in this sample within the last 13 years is high enough to perform a meaningful statistical comparison. We exploit the multi-wavelength dataset from 11 HUGS, a volume-limited survey designed to provide a census of SFR in the Local Volume. There are 14 supernovae discovered in this sample of galaxies within the last 13 years. Although one could argue that this may not be complete, it is certainly a robust lower limit. Results. Assuming a lower limit for core collapse of 8 M (as proposed by direct detections of SN progenitor stars and white dwarf progenitors), the core-collapse supernova rate matches the SFR from the FUV luminosity. However, the SFR based on Hα luminosity is lower than these two estimates by a factor of nearly 2. If we assume that the FUV or Hα based luminosities are a true reflection of the SFR, we find that the minimum mass for core collapse supernova progenitors is 8 ± 1 M and 6 ± 1 M , respectively. Conclusions. The estimate of the minimum mass for core collapse supernova progenitors obtained exploiting FUV data is in good agreement with that from the direct detection of supernova progenitors. The concordant results by these independent methods point toward a constraint of 8 ± 1 M on the lower mass limit for progenitor stars of core collapse supernovae.

show abstract

The 2008 Luminous Optical Transient in the Nearby Galaxy NGC 300

Cited by 148 publications

References 30 publications

Gravitational Waves From Fallback Accretion Onto Neutron Stars

Gravitational Waves From Fallback Accretion Onto Neutron Stars

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

A comparison between star formation rate diagnostics and rate of core collapse supernovae within 11 Mpc

Contact Info

Product

Resources

About