On the triple peaks of SNHunt248 in NGC 5806

Kankare, E.; Kotak, R.; Pastorello, A.; Fraser, M.; Mattila, S.; Smartt, S. J.; Bruce, Alastair; Chambers, K.; Elias‐Rosa, N.; Flewelling, H.; Fremling, C.; Harmanen, J.; Huber, M. E.; Jerkstrand, A.; Kangas, T.; Kuncarayakti, H.; Magee, M.; Magnier, E. A.; Polshaw, J.; Smith, Kenneth; Sollerman, J.; Tomasella, L.

doi:10.1051/0004-6361/201526631

Cited by 54 publications

(84 citation statements)

References 15 publications

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“…This spectrum is comparable to some of the LBV outburst spectra compiled by Smith et al (2011), as well as to the early spectra of SN 2011A (de Jaeger et al 2015). The Fe II lines reported by Kankare et al (2015) for SNhunt248 were not seen in PTF11qnf, but otherwise their spectra are comparable.…”

Section: Ptf11qnf a Sn Impostor?supporting

confidence: 85%

“…The deepest upper limits in the photometry from the P48 suggest that the absolute magnitude of PTF11qnf was M R −15 between −960 to −10 d and between +260 to +1950 d, relative to the first detection (JD 2,455,866.9). This is not a deep limit, and still allows for prediscovery variability such as that observed in SNHunt248 (Kankare et al 2015), but demonstrates that the ∼ 180 d plateau episode we observe in PTF11qnf was preceded and followed by fainter Smith et al (2010) concluded that U2773-OT was a LBV in outburst, and later studies of its 15 yr light curve led Smith et al (2016) to compare U2773-OT to the LBV star η Car. While there is a spread of ∼ 4 mag in maximum brightness, the durability of the light curves of SNHunt248, SN 2011A, and U2773-OT are similar.…”

Section: Ptf11qnf a Sn Impostor?mentioning

confidence: 73%

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Type IIn supernova light-curve properties measured from an untargeted survey sample

Nyholm

Sollerman

Tartaglia

et al. 2020

A&A

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The evolution of a Type IIn supernova (SN IIn) is governed by the interaction between the SN ejecta and a hydrogen-rich circumstellar medium (CSM). SNe IIn thus allow us to probe the late-time mass-loss history of their progenitor stars. We present a sample of SNe IIn from the untargeted, magnitude-limited surveys of the Palomar Transient Factory (PTF) and its successor, the intermediate PTF (iPTF). To date, statistics on SN IIn optical light curve properties have generally been based on small ( 10 SNe) samples from targeted SN surveys. SNe IIn found and followed by the PTF/iPTF were used to select a sample of 42 events with useful constraints on the rise times as well as with available post-peak photometry. The SNe were discovered in 2009-2016 and have at least one low-resolution classification spectrum, as well as photometry from the P48 and P60 telescopes at Palomar Observatory. We study the light-curve properties of these SNe IIn using spline fits (for the peak and the declining portion) and template matching (for the rising portion). We study the peak-magnitude distribution, rise times, decline rates, colour evolution, host galaxies, and K-corrections of the SNe in our sample. We find that the typical rise times are divided into fast and slow risers as 20 ± 8 d and 50 ± 15 d, respectively. The decline rates could possibly be divided into two groups (with slopes 0.013 ± 0.008 mag d −1 and 0.040 ± 0.014 mag d −1 ), but this division has weak statistical significance. We find no significant correlation between the peak luminosity of SNe IIn and their rise times, but the more luminous SNe IIn are generally found to be more durable and the slowly rising SNe IIn are generally found to be slowly declining. The SNe in our sample were hosted by galaxies of absolute magnitude −22 Mg −13 mag. The K-corrections at light-curve peak of the SNe in our sample are found to be within 0.2 mag for the observer's frame r-band, for SNe IIn at redshifts z < 0.25. Applying K-corrections and including also ostensibly "superluminous" SNe IIn, we find that the peak magnitudes are M r peak = −19.18 ± 1.32 mag. We conclude that the occurrence of conspicuous light-curve bumps in SNe IIn, such as in iPTF13z, is limited to 1.4 +14.6 −1.0 % of the SNe IIn. We also investigate a possible subtype of SNe IIn with a fast rise to a 50 d plateau followed by a slow, linear decline. iPTF13agz, iPTF13aki, iPTF13asr, iPTF13cuf, iPTF14bcw, iPTF14bpa, iPTF15aym, iPTF15bky, iPTF15blp, iPTF15eqr, iPTF16fb. ⋆ Based in part on observations made with the Palomar Transient Factory and intermediate Palomar Transient Factory surveys.

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Section: Ptf11qnf a Sn Impostor?supporting

confidence: 85%

Section: Ptf11qnf a Sn Impostor?mentioning

confidence: 73%

Type IIn supernova light-curve properties measured from an untargeted survey sample

Nyholm

Sollerman

Tartaglia

et al. 2020

A&A

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“…Photometrically, the double-peaked light curve of M101-OT and increasingly red color resembles the complex nature of the objects in the LRNe group, with different scaling. However, such behavior is also shown by an object interpreted as an SN impostor, such as SNHunt248, in NGC 5806 (Kankare et al 2015;Mauerhan et al 2015).…”

Section: Discussionmentioning

confidence: 88%

Common Envelope Ejection for a Luminous Red Nova in M101

Blagorodnova

Kotak

Polshaw

et al. 2017

ApJ

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We present the results of optical, near-infrared, and mid-infrared observations of M101 OT2015-1 (PSN J14021678+5426205), a luminous red transient in the Pinwheel galaxy (M101), spanning a total of 16 years. The light curve showed two distinct peaks with absolute magnitudes, on 2014 November 11 and 2015 February 17, respectively. The spectral energy distributions during the second maximum show a cool outburst temperature of »3700 K and low expansion velocities (»-300 kms −1 ) for the H I, Ca II, Ba II, and K I lines. From archival data spanning 15-8 years before the outburst, we find a single source consistent with the optically discovered transient, which we attribute to being the progenitor; it has properties consistent with being an F-type yellow supergiant with L∼8.7´10 4 L e , » T 7000 eff K, and an estimated mass of =  M1 18 1 M e . This star has likely just finished the H-burning phase in the core, started expanding, and is now crossing the Hertzsprung gap. Based on the combination of observed properties, we argue that the progenitor is a binary system, with the more evolved system overfilling the Roche lobe. Comparison with binary evolution models suggests that the outburst was an extremely rare phenomenon, likely associated with the ejection of the common envelope of a massive star. The initial mass of the primary fills the gap between the merger candidates V838 Mon (5−10 M e ) and NGC4490-OT(30 M e ).

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“…1, with the locations of the known transients in the galaxy marked. In addition to iPTF13bvn and PTF12os which we investigate in detail here, the Type IIP SN 2004dg ) and the SN impostor SN Hunt 248 (Mauerhan et al 2015a;Kankare et al 2015) (discovered in 2014) also occurred in this galaxy. SN 2004dg is present in the image stack shown in Fig.…”

Section: Host-galaxy Propertiesmentioning

confidence: 83%

PTF12os and iPTF13bvn

Fremling

Sollerman

Taddia

et al. 2016

A&A

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Context. We investigate two stripped-envelope supernovae (SNe) discovered in the nearby galaxy NGC 5806 by the (intermediate) Palomar Transient Factory [(i)PTF]. These SNe, designated PTF12os/SN 2012P and iPTF13bvn, exploded within ∼ 520 days of one another at a similar distance from the host-galaxy center. We classify PTF12os as a Type IIb SN based on our spectral sequence; iPTF13bvn has previously been classified as Type Ib having a likely progenitor with zero age main sequence (ZAMS) mass below ∼ 17 M . Because of the shared and nearby host, we are presented with a unique opportunity to compare these two SNe. Aims. Our main objective is to constrain the explosion parameters of iPTF12os and iPTF13bvn, and to put constraints on the SN progenitors. We also aim to spatially map the metallicity in the host galaxy, and to investigate the presence of hydrogen in early-time spectra of both SNe. Methods. We present comprehensive datasets collected on PTF12os and iPTF13bvn, and introduce a new automatic referencesubtraction photometry pipeline (FPipe) currently in use by the iPTF. We perform a detailed study of the light curves (LCs) and spectral evolution of the SNe. The bolometric LCs are modeled using the hydrodynamical code hyde. We analyze early spectra of both SNe to investigate the presence of hydrogen; for iPTF13bvn we also investigate the regions of the Paschen lines in infrared spectra. We perform spectral line analysis of helium and iron lines to map the ejecta structure of both SNe. We use nebular models and late-time spectroscopy to constrain the ZAMS mass of the progenitors. We also perform image registration of ground-based images of PTF12os to archival HST images of NGC 5806 to identify a potential progenitor candidate. Results. We find that our nebular spectroscopy of iPTF13bvn remains consistent with a low-mass progenitor, likely having a ZAMS mass of ∼ 12 M . Our late-time spectroscopy of PTF12os is consistent with a ZAMS mass of ∼ 15 M . We successfully identify a source in pre-explosion HST images coincident with PTF12os. The colors and absolute magnitude of this object are consistent between pre-explosion and late-time HST images, implying it is a cluster of massive stars. Our hydrodynamical modeling suggests that the progenitor of PTF12os had a compact He core with a mass of 3.25 −0.011 M of strongly mixed 56 Ni. Spectral comparisons to the Type IIb SN 2011dh indicate that the progenitor of PTF12os was surrounded by a thin hydrogen envelope with a mass lower than 0.02 M . We also find tentative evidence that the progenitor of iPTF13bvn could have been surrounded by a small amount of hydrogen prior to the explosion. This result is supported by possible weak signals of hydrogen in both optical and infrared spectra.

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On the triple peaks of SNHunt248 in NGC 5806

Cited by 54 publications

References 15 publications

Type IIn supernova light-curve properties measured from an untargeted survey sample

Type IIn supernova light-curve properties measured from an untargeted survey sample

Common Envelope Ejection for a Luminous Red Nova in M101

PTF12os and iPTF13bvn

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