Massive star mergers and the recent transient in NGC 4490: a more massive cousin of V838 Mon and V1309 Sco

Smith, Nathan; Andrews, Jennifer E.; Dyk, Schuyler D. Van; Mauerhan, Jon C.; Kasliwal, M. M.; Bond, Howard E.; Filippenko, A. V.; Clubb, K. I.; Graham, M. L.; Perley, D.; Jencson, J.; Bally, John; Úbeda, Leonardo; Sabbi, E.

doi:10.1093/mnras/stw219

Cited by 98 publications

(139 citation statements)

References 79 publications

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“…An LRN, observationally, appears with persistently redder colors than a classical nova and luminosities that range from slightly fainter than classical novae to several magnitudes more luminous (e.g., Kimeswenger et al 2002;Smith et al 2016). The physical interpretation of the LRN optical/IR outburst is the merger of a close binary (Tylenda et al 2011;Ivanova et al 2013;MacLeod et al 2017).…”

Section: V1324 Sco: a Classical Novamentioning

confidence: 98%

A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

Finzell

Chomiuk

Metzger

et al. 2018

ApJ

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It has recently been discovered that some, if not all, classical novae emit GeV gamma-rays during outburst, but the mechanisms involved in the production ofgamma-rays are still not well understood. We present here a comprehensive multiwavelength data set-from radio to X-rays-for the most gamma-ray-luminous classical nova to date, V1324 Sco. Using this data set, we show that V1324 Sco is a canonical dusty Fe II-type nova, with a maximum ejecta velocity of 2600 km s −1 and an ejecta mass of a few´-10 5  M . There is also evidence for complex shock interactions, including a double-peaked radio light curve which shows high brightness temperatures at early times. To explore why V1324Sco was so gamma-ray luminous, we present a model of the nova ejecta featuring strong internal shocks and find that higher gamma-ray luminosities result from higher ejecta velocities and/or mass-loss rates. Comparison of V1324Sco with other gamma-ray-detected novae does not show clear signatures of either, and we conclude that a larger sample of similarly well-observed novae is needed to understand the origin and variation of gamma-rays in novae.

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Section: V1324 Sco: a Classical Novamentioning

confidence: 98%

A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

Finzell

Chomiuk

Metzger

et al. 2018

ApJ

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“…However, such events may produce luminous infrared flares (Bally & Zinnecker 2005) and may be a major source of transient luminosity, kinetic energy, and momentum feedback in the self-regulation of star formation in regions forming dense star clusters and massive stars. Smith et al (2016) found a luminous visual transient, NGC4490-OT, in the galaxy NGC4490. This object is a candidate massive stellar merger event similar to but more luminous than V838 Mon.…”

Section: Explosive Outflows and Infrared-transientsmentioning

confidence: 97%

The ALMA View of the OMC1 Explosion in Orion

Bally¹,

Ginsburg²,

Arce

et al. 2017

ApJ

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Most massive stars form in dense clusters where gravitational interactions with otherstars may be common. The two nearest forming massive stars, the BN object and Source I, located behind the Orion Nebula, were ejected with velocities of ∼29 and ∼13 km s −1 about 500 years ago by such interactions. This event generated an explosion in the gas. New ALMA observations show in unprecedented detail, a roughly spherically symmetric distribution of over a hundred 12 CO J=2−1 streamers with velocities extending from V LSR =−150 to +145 km s −1 . The streamer radial velocities increase (or decrease) linearly with projected distance from the explosion center, forming a "Hubble Flow" confined to within 50″ of the explosion center. They point toward the high proper-motion, shockexcited H 2 and [Fe II] "fingertips" and lower-velocity CO in the H 2 wakes comprising Orionʼs "fingers." In some directions, the H 2 "fingers" extend more than a factor of two farther from the ejection center than the CO streamers. Such deviations from spherical symmetry may be caused by ejecta running into dense gas or the dynamics of the N-body interaction that ejected the stars and produced the explosion. This ∼10 48 erg event may have been powered by the release of gravitational potential energy associated with the formation of a compact binary or a protostellar merger. Orion may be the prototype for a new class of stellar explosiozn responsible for luminous infrared transients in nearby galaxies.

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“…The equilibrium temperature radius provides an estimate of the physical size of the hot, circumstellar dust and is given by (e.g., Smith et al 2016) is assumed for the calculation. Note that if the heating of the mid-IR emitting dust is instead dominated locally by collisions with hot electrons in a post-shock environment (e.g., Dwek 1987;Dwek et al 2008), R Eq will not reflect the physical size of the system.…”

Section: Properties Of Thementioning

confidence: 99%

“…We consider the following (possibly overlapping) hypotheses for the nature of SN2010da: an SN2008S-like transient, an outburst from an LBV/sgB[e]-HMXB, a presumed stellar merger event like V1309Sco (Tylenda et al 2011),V838Mon (Bond et al 2003, Afşar & Bond 2007)or the recently identified NGC 4490-OT (Smith et al 2016), or a low-luminosity supernova explosion (e.g., electron-capture).…”

Section: On the Nature Of Sn2010damentioning

confidence: 99%

“…The prospect of SN2010da corresponding to a merger event is interesting given the increasing attention on stellar mergers (e.g., Smith et al 2016); however, this interpretation is unlikely due to the SN2010da's high X-ray luminosity and late-time rebrightening. Additionally, the smoothly declining optical light curve following the initial outburst of SN2010da (Figure 4) is not consistent with the almost periodic peaks exhibited from merger candidates V838 Mon and NGC 4490 OT.…”

Section: A Stellar Merger?mentioning

confidence: 99%

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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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Massive star mergers and the recent transient in NGC 4490: a more massive cousin of V838 Mon and V1309 Sco

Cited by 98 publications

References 79 publications

A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

The ALMA View of the OMC1 Explosion in Orion

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

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