Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

Li, W.; Wang, Xiaofeng; Vinkó, J.; Mo, Jun; Hosseinzadeh, G.; Sand, David J.; Zhang, Jujia; Lin, Han; Zhang, T.; Wang, L.; Zhang, J.; Chen, Z.; Xiang, Danfeng; Rui, Liming; Huang, Fan; Li, X.; Zhang, Xiaodan; Li, L.; Baron, E.; DerKacy, James M.; Zhao, Xulin; Sai, Hanna; Zhang, K.; Wang, Lingzhi; Howell, D. A.; McCully, C.; Arcavi, I.; Valenti, S.; Hiramatsu, D.; Burke, J.; Rest, A.; Garnavich, P.; Tucker, C.; Narayan, Gautham; Shaya, E.; Margheim, Steve; Zenteno, A.; Villar, A.; Dimitriadis, G.; Foley, R. J.; Pan, Y. C.; Coulter, D. A.; Fox, O.; Jha, Saurabh W.; Jones, D. O.; Kasen, Daniel; Kilpatrick, C. D.; Piro, Anthony L.; Riess, Adam G.; Rojas-Bravo, C.; Shappee, B. J.; Holoien, T. W. S.; Stanek, K. Z.; Drout, M. R.; Auchettl, Katie; Kochanek, C. S.; Brown, J. S.; Bose, S.; Bersier, D.; Brimacombe, J.; Chen, P.; Dong, Subo; Holmbo, S.; Muñoz, J. A.; Mutel, R. L.; Post, R. S.; Prieto, J. L.; Shields, J.; Tallon, D.; Thompson, T. A.; Vallely, P.; Villanueva, Steven; Smartt, S. J.; Smith, K.; Chambers, K.; Flewelling, H.; Huber, M. E.; Magnier, E. A.; Waters, C.; Schultz, A. S. B.; Bulger, J.; Lowe, T.; Willman, M.; Sárneczky, K.; Pál, András; Wheeler, J. C.; Bódi, Attila; Bognár, Zs.; Csák, B.; Cseh, B.; Csörnyei, G.; Hanyecz, O.; Ignácz, Bernadett; Kalup, Cs.; Könyves-Tóth, Réka; Kriskovics, L.; Ordasi, A.; Rajmon, I.; Sódor, Á.; Szabo, Robert M.; Szakáts, R.; Zsidi, Gabriella; Milne, Peter; Andrews, Jennifer E.; Smith, Nathan; Bilinski, Christopher; Brown, P. J.; Nordin, J.; Williams, S. C.; Galbany, L.; Palmerio, J.; Hook, I. M.; Inserra, C.; Maguire, K.; Cartier, R.; Razza, Alessandro; Gutiérrez, C. P.; Hermes, J. J.; Reding, Joshua S.; Kaiser, Bastian; Tonry, J.; Heinze, A.; Denneau, L.; Weiland, H.; Stalder, B.; Barentsen, Geert; Dotson, Jessie; Barclay, Thomas; Gully-Santiago, Michael; Hedges, Christina; Cody, Ann Marie; Howell, Steve B.; Coughlin, Jeffrey L.; Cleve, Jeffrey E. Van; Cardoso, José Vinícius de Miranda; Larson, K. A.; McCalmont-Everton, K. M.; Peterson, C.; Ross, S.; Reedy, Lee; Osborne, Darren; McGinn, Christopher M.; Kohnert, L.; Migliorini, L.; Wheaton, A.; Spencer, Brittany; Labonde, C.; Castillo, G. A. Rodríguez; Beerman, G.; Steward, K.; Hanley, M.; Larsen, R.; Gangopadhyay, R.; Kloetzel, R.; Weschler, T.; Nystrom, V.; Moffatt, J.; Redick, M.; Griest, K.; Packard, M.; Muszynski, M.; Kampmeier, J.; Bjella, R.; Flynn, S.; Elsaesser, Bjoern

doi:10.3847/1538-4357/aaec74

Cited by 80 publications

(78 citation statements)

References 154 publications

(196 reference statements)

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“…0.04 mag, and t Bmax =58162.7±0.3 day. Li et al (2018) also find that the light curve of ASASSN-18bt is consistent with the Milky Way reddening inferred from dust maps alone with no additional host-galaxy reddening. This is supported by the lack of observed Na ID absorption at the host galaxy's recession velocity.…”

Section: Introductionsupporting

confidence: 75%

“…Here we announce the discovery of the TypeIa SN ASASSN-18bt (SN 2018oh) in UGC 04780, which was monitored by the K2 mission, and analyze the early evolution of the exquisite K2 light curve. With a peak apparent magnitude of B max =14.31±0.03 (Li et al 2018) and a distance of 47.7Mpc, it is nearer and brighter than any other supernova detected by Kepler. In Section 2, we describe our discovery and observations of ASASSN-18bt.…”

Section: Introductionmentioning

confidence: 81%

“…Finally, we calibrated the K2 light curve using the mangled SED from fitting the PS r-band (presented in Li et al 2018) around the peak to determine the synthetic K2 peak magnitude and the absolute zero point to the K2 light curve. The K2 detections and 3σ limits are shown in Figure 2 and, for completeness, presented in Table 1.…”

Section: K2 Light Curvementioning

confidence: 99%

“…In this formalism, the IC luminosity is directly proportional to the bolometric luminosity of the supernovae. We adopt the bolometric light curve for ASASSN-18bt calculated in Li et al (2018). The deepest limits to the density of the CSM surrounding ASASSN-18bt come from the observations at ∼11−14 days postexplosion, when the bolometric luminosity was near its peak.…”

Section: X-ray Limits On Progenitor Mass Lossmentioning

confidence: 99%

“…This work is part of a number of papers analyzing ASASSN-18bt, with coordinated papers from Dimitriadis et al (2018) and Li et al (2018). Li et al (2018) investigate the nearmaximum optical properties of ASASSN-18bt and find…”

Section: Introductionmentioning

confidence: 99%

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Seeing Double: ASASSN-18bt Exhibits a Two-component Rise in the Early-time K2 Light Curve

Shappee¹,

Holoien²,

Drout³

et al. 2018

ApJ

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On 2018 February 4.41, the All-Sky Automated Survey for SuperNovae (ASAS-SN) discovered ASASSN-18bt in the K2 Campaign 16 field. With a redshift of z=0.01098 and a peak apparent magnitude of B max =14.31, ASASSN-18bt is the nearest and brightest SNe Ia yet observed by the Kepler spacecraft. Here we present the discovery of ASASSN-18bt, the K2 light curve, and prediscovery data from ASAS-SN and the Asteroid Terrestrial-impact Last Alert System. The K2 early-time light curve has an unprecedented 30-minute cadence and photometric precision for an SNIa light curve, and it unambiguously shows a ∼4 day nearly linear phase followed by a steeper rise. Thus, ASASSN-18bt joins a growing list of SNe Ia whose early light curves are not well described by a single power law. We show that a double-power-law model fits the data reasonably well, hinting that two physical processes must be responsible for the observed rise. However, we find that current models of the interaction with a nondegenerate companion predict an abrupt rise and cannot adequately explain the initial, slower linear phase. Instead, we find that existing published models with shallow 56 Ni are able to span the observed behavior and, with tuning, may be able to reproduce the ASASSN-18bt light curve. Regardless, more theoretical work is needed to satisfactorily model this and other early-time SNeIa light curves. Finally, we use Swift X-ray nondetections to constrain the presence of circumstellar material (CSM) at much larger distances and lower densities than possible with the optical light curve. For a constant-density CSM, these nondetections constrain ρ<4.5×10 5 cm −3 at a radius of 4×10 15 cm from the progenitor star. Assuming a wind-like environment, we place mass loss limits of M M 8 10 yr 6 1 <´-☉ for v w =100 km s −1 , ruling out some symbiotic progenitor systems. This work highlights the power of well-sampled early-time data and the need for immediate multiband, high-cadence follow-up for progress in understanding SNeIa.

show abstract

Section: Introductionsupporting

confidence: 75%

Section: Introductionmentioning

confidence: 81%

Section: K2 Light Curvementioning

confidence: 99%

Section: X-ray Limits On Progenitor Mass Lossmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Seeing Double: ASASSN-18bt Exhibits a Two-component Rise in the Early-time K2 Light Curve

Shappee¹,

Holoien²,

Drout³

et al. 2018

ApJ

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Early color photometry of a possible type Iax supernova 2023mnc: inferring the distance and progenitor constraints

Yang,

Zhang,

Shen

et al. 2023

Astrophys Space Sci

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Early-time radioactive signals from type Ia supernovae (SNeIa) can provide important constraints on the explosion mechanism and the progenitor system. We present observations and analysis of SN 2023mnc, a SN Ia, ∼ 7 days following its discovery. Follow-up observations were conducted in optical bands, covering phases from ∼ −4 days to ∼ 15 days relative to its r-band peak luminosity. The early photometry allows us to estimate the physical properties of the ejecta and characterize the possible divergence from a normal SN Ia; we were able to characterize it as a Type Iax supernova instead. The estimated date of explosion is t0 = 60130 MJD and implies a short rise time of trise ≈ 16 days. The apparent g-band peak magnitude and the post-peak decline rate are mmax(g) = −19.52 ± 0.47 mag and ∆m15(g) = 0.825 ± 1.635 mag, respectively. Based on the light curve fitting of standard SN Ia models, the distance modulus is predicted to be 37.98 ± 0.207 mag for g band measurements, and the SN is predicted to be 394.46 ± 38 Mpc from Earth. Assuming a 56 Ni powered radiative diffusion, the estimated bolometric light-curve peaks at 1.08 erg s -1 and indicates that only 0.05M⊙ of 56 Ni was produced, making SN 2023mnc a moderate luminosity object in the Iax class with peak absolute magnitude of MV = −16.4 mag. Comparing the observed color evolution with the predicted by different models such as deflagration-to-detonation transition and pure-deflagration scenario, the latter one is favored. The photometry of SN 2023mnc offers a unique opportunity to examine the progenitor systems and ignition process of the SNe Iax, adding weight to the population study of such sub-class SNe.

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An UBVRI calibration method based on Pan-STARRS photometric survey

Li,

Zeng,

Esamdin

et al. 2023

Astronomy and Computing

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Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

Cited by 80 publications

References 154 publications

Seeing Double: ASASSN-18bt Exhibits a Two-component Rise in the Early-time K2 Light Curve

Seeing Double: ASASSN-18bt Exhibits a Two-component Rise in the Early-time K2 Light Curve

Early color photometry of a possible type Iax supernova 2023mnc: inferring the distance and progenitor constraints

An UBVRI calibration method based on Pan-STARRS photometric survey

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