A<i>Chandra</i>ACIS Observation of the X‐Ray–luminous SN 1988Z

Schlegel, Eric M.; Petre, Robert

doi:10.1086/504890

Cited by 34 publications

(37 citation statements)

References 33 publications

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“…Estimates for the mass‐loss rate from the progenitor of SN 1988Z vary by roughly an order of magnitude. From X‐ray observations, Schlegel & Petre (2006) find , while Williams et al (2002) estimate based on radio observations, and the models of the optical emission by Chugai & Danziger (1994) yield . While these estimates are one to two orders of magnitude less than those for SN 2008iy, we note that in each of the above estimates for a wind speed of 10 km s −1 was adopted for the progenitor of SN 1988Z.…”

Section: Discussionmentioning

confidence: 99%

“…However, the similarities to SN 1988Z suggest that SN 2008iy could continue interacting, and thus remain luminous, for several years. This would allow long‐term monitoring in the radio, X‐ray and optical, like SN 1988Z (Aretxaga et al 1999; Williams et al 2002; Schlegel & Petre 2006). We predict that SN 2008iy is a luminous radio source, like SN 1988Z (Van Dyk et al 1993), though we note that at z = 0.0411 deep observations may be necessary for detection.…”

Section: Discussionmentioning

confidence: 99%

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SN 2008iy: an unusual Type IIn Supernova with an enduring 400-d rise time

Miller

Silverman

Butler

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We present spectroscopic and photometric observations of the Type IIn supernova (SN) 2008iy. SN 2008iy showed an unprecedentedly long rise time of ∼400 d, making it the first known SN to take significantly longer than 100 d to reach peak optical luminosity. The peak absolute magnitude of SN 2008iy was Mr≈−19.1 mag, and the total radiated energy over the first ∼700 d was ∼2 × 1050 erg. Spectroscopically, SN 2008iy is very similar to the Type IIn SN 1988Z at late times and, like SN 1988Z, it is a luminous X‐ray source (both SNe had an X‐ray luminosity LX > 1041 erg s−1). SN 2008iy has a growing near‐infrared excess at late times similar to several other SNe IIn. The Hα emission‐line profile of SN 2008iy shows a narrow P Cygni absorption component, implying a pre‐SN wind speed of ∼100 km s−1. We argue that the luminosity of SN 2008iy is powered via the interaction of the SN ejecta with a dense, clumpy circumstellar medium. The ∼400‐d rise time can be understood if the number density of clumps increases with distance over a radius ∼1.7 × 1016 cm from the progenitor. This scenario is possible if the progenitor experienced an episodic phase of enhanced mass loss <1 century prior to explosion or if the progenitor wind speed increased during the decades before core collapse. We favour the former scenario, which is reminiscent of the eruptive mass‐loss episodes observed for luminous blue variable (LBV) stars. The progenitor wind speed and increased mass‐loss rates serve as further evidence that at least some, and perhaps all, Type IIn SNe experience LBV‐like eruptions shortly before core collapse. We also discuss the host galaxy of SN 2008iy, a subluminous dwarf galaxy, and offer a few reasons why the recent suggestion that unusual, luminous SNe preferentially occur in dwarf galaxies may be the result of observational biases.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

SN 2008iy: an unusual Type IIn Supernova with an enduring 400-d rise time

Miller

Silverman

Butler

et al. 2010

Monthly Notices of the Royal Astronomical Society

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“…SN 1988Z was bright in X-ray and radio emission (Schlegel & Petre 2006;Van Dyk et al 1993;Williams et al 2002), unlike SN 2006gy. The complex and unique spectral evolution of SN 2006gy will be discussed in a later paper, when more complete data are available.…”

Section: Owocki 2006) Those Events Typically Last About a Decade Or mentioning

confidence: 94%

SN 2006gy: Discovery of the Most Luminous Supernova Ever Recorded, Powered by the Death of an Extremely Massive Star like η Carinae

Smith

Foley

et al. 2007

ApJ

524

521

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We report the discovery and early observations of the peculiar Type IIn supernova (SN) 2006gy in NGC 1260. With a peak visual magnitude of about À22, it is the most luminous supernova ever recorded. Its very slow rise to maximum took $70 days, and it stayed brighter than À21 mag for about 100 days. It is not yet clear what powers the enormous luminosity and the total radiated energy of $10 51 erg, but we argue that any known mechanism-thermal emission, circumstellar interaction, or 56 Ni decay-requires a very massive progenitor star. The circumstellar interaction hypothesis would require truly exceptional conditions around the star, which, in the decades before its death, must have experienced a luminous blue variable (LBV) eruption like the 19th century eruption of Carinae. However, this scenario fails to explain the weak and unabsorbed soft X-rays detected by Chandra. Radioactive decay of 56 Ni may be a less objectionable hypothesis, but it would imply a large Ni mass of $22 M , requiring SN 2006gy to have been a pair-instability supernova where the star's core was obliterated. While this is still uncertain, SN 2006gy is the first supernova for which we have good reason to suspect a pair-instability explosion. Based on a number of lines of evidence, we eliminate the hypothesis that SN 2006gy was a ''Type IIa'' event, that is, a white dwarf exploding inside a hydrogen envelope. Instead, we propose that the progenitor was a very massive evolved object like Carinae that, contrary to expectations, failed to shed its hydrogen envelope. SN 2006gy implies that some of the most massive stars can explode prematurely during the LBV phase, never becoming Wolf-Rayet stars. SN 2006gy also suggests that they can create brilliant supernovae instead of experiencing ignominious deaths through direct collapse to a black hole. If such a fate is common among the most massive stars, then observable supernovae from Population III stars in the early universe will be more numerous than previously believed.

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“…These lines are the signature of an external physical phenomenon highly dependent on the surrounding environment, rather than of any intrinsic property of the explosion. Depending on the spatial distribution and physical properties of the CSM, these lines may persist for days ("flash spectroscopy", Gal-Yam et al 2014;Khazov et al 2016;Yaron et al 2017), weeks (e.g., SN 1998s, Li et al 1998Fassia et al 2000Fassia et al , 2001SN 2005gl, Gal-Yam et al 2007SN 2010mc, Ofek et al 2013a), or years (e.g., SN 1988Z, Danziger & Kjaer 1991Stathakis & Sadler 1991;Turatto et al 1993;van Dyk et al 1993;Chugai & Danziger 1994;Fabian & Terlevich 1996;Aretxaga et al 1999;Williams et al 2002;Schlegel & Petre 2006;Smith et al 2017;jl, Patat et al 2011Stoll et al 2011;Gall et al 2014;Ofek et al 2014c).…”

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confidence: 99%

Supernova PTF 12glz: A Possible Shock Breakout Driven through an Aspherical Wind

Soumagnac

Ofek

Gal‐Yam

et al. 2019

ApJ

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We present visible-light and ultraviolet (U V ) observations of the supernova PTF 12glz. The SN was discovered and monitored in near-U V and R bands as part of a joint GALEX and Palomar Transient Factory campaign. It is among the most energetic Type IIn supernovae observed to date (≈ 10 51 erg). If the radiated energy mainly came from the thermalization of the shock kinetic energy, we show that PTF 12glz was surrounded by ∼ 1 M of circumstellar material (CSM) prior to its explosive death. PTF 12glz shows a puzzling peculiarity: at early times, while the freely expanding ejecta are presumably masked by the optically thick CSM, the radius of the blackbody that best fits the observations grows at ≈ 8000 km s −1 . Such a velocity is characteristic of fast moving ejecta rather than optically thick CSM. This phase of radial expansion takes place before any spectroscopic signature of expanding ejecta appears in the spectrum and while both the spectroscopic data and the bolometric luminosity seem to indicate that the CSM is optically thick. We propose a geometrical solution to this puzzle, involving an aspherical structure of the CSM around PTF 12glz. By modeling radiative diffusion through a slab of CSM, we show that an aspherical geometry of the CSM can result in a growing effective radius. This simple model also allows us to recover the decreasing blackbody temperature of PTF 12glz. SLAB-Diffusion, the code we wrote to model the radiative diffusion of photons through a slab of CSM and evaluate the observed radius and temperature, is made available on-line.

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AChandraACIS Observation of the X‐Ray–luminous SN 1988Z

Cited by 34 publications

References 33 publications

SN 2008iy: an unusual Type IIn Supernova with an enduring 400-d rise time

SN 2008iy: an unusual Type IIn Supernova with an enduring 400-d rise time

SN 2006gy: Discovery of the Most Luminous Supernova Ever Recorded, Powered by the Death of an Extremely Massive Star like η Carinae

Supernova PTF 12glz: A Possible Shock Breakout Driven through an Aspherical Wind

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