A New Class of Luminous Transients and a First Census of Their Massive Stellar Progenitors

Thompson, Todd A.; Prieto, J. L.; Stanek, K. Z.; Kistler, Matthew D.; Beacom, J. F.; Kochanek, C. S.

doi:10.1088/0004-637x/705/2/1364

Cited by 205 publications

(427 citation statements)

References 104 publications

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“…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

123

135

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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.

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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

123

135

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“…Smith et al 2008) rather than electron capture SNe (Thompson et al 2009), the mass range for such events will be extended downwards into the 10−20 M regime (e.g. Berger et al 2009).…”

Section: The Extragalactic Sne Impostersmentioning

confidence: 99%

Bolometric luminosity variations in the luminous blue variable AFGL2298

Clark¹,

Crowther

Larionov

et al. 2009

A&A

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Aims. We characterise the variability in the physical properties of the luminous blue variable AFGL 2298 (IRAS 18576+0341) between 1989−2008. Methods. In conjunction with published data from 1989−2001, we have undertaken a long term (2001−2008) near-IR spectroscopic and photometric observational campaign for this star and utilise a non-LTE model atmosphere code to interpret these data. Results. We find AFGL 2298 to have been highly variable during the two decades covered by the observational datasets. Photometric variations of ≥1.6 mag have been observed in the JHK wavebands; however, these are not accompanied by correlated changes in near-IR colour. Non-LTE model atmosphere analysis of 4 epochs of K band spectroscopy obtained between 2001−7 suggests that the photometric changes of AFGL 2298 were driven by expansion and contraction of the stellar photosphere accompanied by comparatively small changes in the stellar temperature (ΔT * ∼ 4.5 kK). Unclumped mass loss rates throughout this period were modest and directly comparable to those of other highly luminous (candidate) LBVs. However, the main finding of this analysis was that the bolometric luminosity of AFGL 2298 appears to have varied by at least a factor of ∼2 between 1989−2008, with it being one of the most luminous stars in the Galaxy during maximum. Comparison to other LBVs that have undergone non bolometric luminosity conserving "eruptions" shows such events to be heterogeneous, with AFGL 2298 the least extreme example. These results -and the diverse nature of both the quiescent LBVs and associated ejecta -may offer support to the suggestion that more than one physical mechanism is responsible for such behaviour.

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“…The initial classification as an SN, however, was immediately contradicted by its low outburst luminosity (M V ∼−10.3 at maximum; Khan et al 2010). Mid-infrared (IR) photometry from archival Spitzer imaging data revealed that the progenitor of SN2010da heavily obscured and shared a similar position in a mid-IR color-magnitude diagram (CMD) as luminous blue variable (LBV) candidates (Massey et al 2007; Thompson et al 2009;Khan et al 2010;Laskar et al 2010). Follow-up optical spectroscopy of SN2010da supported the claim that it was not a true SN, but instead resembled an LBV-like outburst Elias-Rosa et al 2010).…”

Section: Introductionmentioning

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

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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.

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A New Class of Luminous Transients and a First Census of Their Massive Stellar Progenitors

Cited by 205 publications

References 104 publications

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

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

Bolometric luminosity variations in the luminous blue variable AFGL2298

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

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