The Type II-P Supernova 2017eaw: From Explosion to the Nebular Phase

Szalai, T.; Vinkó, J.; Könyves-Tóth, Réka; Nagy, Andrea; Bostroem, K. A.; Sárneczky, K.; Brown, P. J.; Pejcha, Ondřej; Bódi, Attila; Cseh, B.; Csörnyei, G.; Dencs, Z.; Hanyecz, O.; Ignácz, Bernadett; Kalup, Cs.; Kriskovics, L.; Ordasi, A.; Pál, András; Seli, Bálint; Sódor, Á.; Szakáts, R.; Vida, K.; Zsidi, Gabriella; Arcavi, I.; Ashall, C.; Burke, J.; Galbany, L.; Hiramatsu, D.; Hosseinzadeh, G.; Hsiao, E. Y.; Howell, D. A.; McCully, C.; Moran, S.; Rho, Jeonghee; Sand, David J.; Shahbandeh, Melissa; Valenti, S.; Wheeler, J. C.

doi:10.3847/1538-4357/ab12d0

Cited by 62 publications

(39 citation statements)

References 105 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Except for Nugent et al (2006), all other SCM distances are systematically lower than the EPM and kinematic distances. The same was found for SN2017eaw and SN2004et in Szalai et al (2019) and could be due to CSM interaction or asymmetries. The SCM method relies on a correlation between the magnitude and expansion velocity at day 50, which could break down under these conditions.…”

Section: Distance Measurementssupporting

confidence: 78%

“…A comprehensive optical and near-infrared (NIR) data set has been collected on SN2017gmr, with several major SN collaborations contributing data. These include the Las Cumbres Observatory's Global Supernova Project (e.g., Szalai et al 2019), the NOT (Nordic Optical Telescope) Un-biased Transient Survey 51 (NUTS), the Public ESO Spectroscopic Survey for Transient Objects (ePESSTO; Smartt et al 2015), the Texas Supernova Spectroscopic Survey (TS 3 ), and the Tsinghua Supernova Project (X. Wang et al 2019, in preparation). Below we briefly list the instruments/telescopes used in obtaining data for SN2017gmr, but for ease of reading an accounting of reduction procedures is included in Appendices A and B.…”

Section: Observationsmentioning

confidence: 99%

See 1 more Smart Citation

SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

2019

The Astrophysical Journal

View full text Add to dashboard Cite

We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN2017gmr from hours after discovery through the first 180 days. SN2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical light-curve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early light curve indicates a ∼500 R e progenitor radius, consistent with a rather compact red supergiant, and latetime luminosities indicate that up to 0.130±0.026 M e of 56 Ni are present, if the light curve is solely powered by radioactive decay, although the 56 Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of Hα and [O I] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first 2 days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta.

show abstract

Section: Distance Measurementssupporting

confidence: 78%

Section: Observationsmentioning

confidence: 99%

SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

2019

The Astrophysical Journal

View full text Add to dashboard Cite

show abstract

“…We recently obtained a sequence of NIR spectra of the Type IIP CCSN SN 2017eaw, which shows the onset of CO formation and newly formed carbon dust (Rho et al 2018a;Szalai et al 2019;Tinyanont et al 2019). The timing of the appearance and the evolution of CO is remarkably similar to that seen in SN 1987A and is consistent with chemically controlled dust models.…”

Section: Introductionsupporting

confidence: 58%

Near-infrared and Optical Observations of Type Ic SN 2020oi and Broad-lined Type Ic SN 2020bvc: Carbon Monoxide, Dust, and High-velocity Supernova Ejecta

Rho

Evans

Geballe

et al. 2021

ApJ

Self Cite

View full text Add to dashboard Cite

We present near-IR (NIR) and optical observations of the Type Ic supernova (SN Ic) SN 2020oi in the galaxy M100 and the broad-lined SN Ic SN 2020bvc in UGC 9379, using Gemini, Las Cumbres Observatory, Southern Astrophysical Telescope, and other ground-based telescopes. The NIR spectrum of SN 2020oi at day 63 since the explosion shows strong CO emissions and a rising K-band continuum, which is the first unambiguous dust detection from an SN Ic. Non-LTE CO modeling shows that CO is still optically thick and that the lower limit to the CO mass is 10 −3 M e. The dust temperature is 810 K, and the dust mass is ∼10 −5 M e. We explore the possibilities that the dust is freshly formed in the ejecta, heated dust in the preexisting circumstellar medium, and an infrared echo. The light curves of SN 2020oi are consistent with a STELLA model with canonical explosion energy, 0.07 M e Ni mass, and 0.7 M e ejecta mass. A model of high explosion energy of 10 52 erg, 0.4 M e Ni mass, and 6.5 M e ejecta mass with the circumstellar matter reproduces the double-peaked light curves of SN 2020bvc. We observe temporal changes of absorption features of the IR Ca II triplet, S I at 1.043 μm, and Fe II at 5169 Å. The blueshifted lines indicate high velocities, up to 60,000 km s −1 for SN 2020bvc and 20,000 km s −1 for SN 2020oi, and the expansion velocity rapidly declines before the optical maximum. We present modeled spectral signatures and diagnostics of CO and SiO molecular bands between 1.4 and 10 μm.

show abstract

“…The photometric and spectroscopic follow-up observations of SN2018ivc were obtained and coordinated through Las Cumbres Observatory's Global Supernova Project (GSP; PI: D. A. Howell), a key project to collect densely sampled optical light curves and spectra of nearby and bright SNe (e.g., Andrews et al 2019;Szalai et al 2019).…”

Section: Observationsmentioning

confidence: 99%

Discovery and Rapid Follow-up Observations of the Unusual Type II SN 2018ivc in NGC 1068

Bostroem

Valenti

Sand

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

We present the discovery and high-cadence follow-up observations of SN2018ivc, an unusual SNe II that exploded in NGC1068 (D=10.1 Mpc). The light curve of SN2018ivc declines piecewise-linearly, changing slope frequently, with four clear slope changes in the first 30 days of evolution. This rapidly changing light curve indicates that interaction between the circumstellar material and ejecta plays a significant role in the evolution. Circumstellar interaction is further supported by a strong X-ray detection. The spectra are rapidly evolving and dominated by hydrogen, helium, and calcium emission lines. We identify a rare high-velocity emission-line feature blueshifted at ∼7800 km s 1 (in Hα, Hβ, Pβ, Pγ, He I, and Ca II), which is visible from day 18 until at least day 78 and could be evidence of an asymmetric progenitor or explosion. From the overall similarity between SN2018ivc and SN1996al, the Hα equivalent width of its parent H IIregion, and constraints from pre-explosion archival Hubble Space Telescope images, we find that the progenitor of SN2018ivc could be as massive as 52 M  but is more likely <12 M . SN2018ivc demonstrates the importance of the early discovery and rapid follow-up observations of nearby supernovae to study the physics and progenitors of these cosmic explosions.

show abstract

The Type II-P Supernova 2017eaw: From Explosion to the Nebular Phase

Cited by 62 publications

References 105 publications

SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

Near-infrared and Optical Observations of Type Ic SN 2020oi and Broad-lined Type Ic SN 2020bvc: Carbon Monoxide, Dust, and High-velocity Supernova Ejecta

Discovery and Rapid Follow-up Observations of the Unusual Type II SN 2018ivc in NGC 1068

Contact Info

Product

Resources

About