A Non-equipartition Shock Wave Traveling in a Dense Circumstellar Environment around SN 2020oi

Horesh, A.; Sfaradi, Itai; Ergon, M.; Barbarino, C.; Sollerman, J.; Moldón, J.; Dobie, Dougal; Schulze, S.; Williams, D.; Fremling, C.; Gal‐Yam, A.; Kulkarni, S. R.; O’Brien, Andrew; Lundqvist, Peter; Murphy, Tara; Fender, R. P.; Anand, Shreya; Belicki, Justin; Bellm, Eric C.; Coughlin, M. W.; De, Kishalay; Golkhou, V. Z.; Graham, M. J.; Green, David A.; Hankins, M.; Kasliwal, M. M.; Kupfer, Thomas; Laher, Russ R.; Masci, Frank J.; Miller, A. A.; Neill, James D.; Ofek, E. O.; Perrott, Y. C.; Porter, Michael; Reiley, Daniel J.; Rigault, M.; Rodríguez, Héctor; Rusholme, B.; Shupe, D. L.; Titterington, D.

doi:10.3847/1538-4357/abbd38

Cited by 26 publications

(49 citation statements)

References 52 publications

(75 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The extinctions we derive from marginal dips in SN 2020oi are consistent with the techniques described in Poznanski et al (2012). The estimated extinction of SN 2020oi is comparable to those of Izzo et al (2020) and Ho et al (2020c), and that of SN 2020bvc is comparable to that of Horesh et al (2020).…”

Section: Extinctionsupporting

confidence: 82%

“…The mass of the circumstellar medium (CSM) could not be tightly constrained from optical curves without detection of the first peak (observed in SN 2020bvc; see Figure 5), but the comparable model in Figure 2 assumes an upper limit to the CSM mass of 3 × 10 −4 M e , which is still consistent with the observation. It does not contradict the recent findings based on radio observations by Horesh et al (2020). Figure 4 shows optical light curves of SN 2020bvc with LCO, Konkoly, and ZTF photometry.…”

Section: Light Curves and Explosion Properties Of Sn 2020oisupporting

confidence: 82%

“…The SN has also been detected by Swift with UVW2 = 17.97 ± 0.33, UVM2 = 18.16 ± 0.34, and UVW1 = 17.54 ± 0.25 (TNS 2020-8;Ho et al 2020d). In addition, radio emission has been reported (ATel # 13398, 13400, 13401, and 13448;Horesh et al 2020;Moldon et al 2020).…”

Section: Observationsmentioning

confidence: 99%

See 2 more Smart Citations

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

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

Section: Extinctionsupporting

confidence: 82%

Section: Light Curves and Explosion Properties Of Sn 2020oisupporting

confidence: 82%

See 1 more Smart Citation

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

View full text Add to dashboard Cite

show abstract

“…A study of this SN based on ZTF optical light curve and spectroscopy will be presented in ref. (49) .…”

Section: Methods Infrared Spectropolarimetry Observationsmentioning

confidence: 99%

Infrared spectropolarimetric detection of intrinsic polarization from a core-collapse supernova

et al. 2021

Self Cite

View full text Add to dashboard Cite

Massive stars die an explosive death as a core-collapse supernova (CCSN). The exact physical processes that cause the collapsing star to rebound into an explosion is not well-understood, and the key in resolving this issue may lie in the measurement of the shape of CCSNe ejecta. Spectropolarimetry is the only way to perform this measurement for CCSNe outside of the Milky Way and Magellanic Clouds. We present an infrared (IR) spectropolarimetric detection of a CCSN, enabled by the new highly sensitive WIRC+Pol instrument at Palomar Observatory, that can observe CCSNe (M = −17 mags) out to 20 Mpc to ∼0.1% polarimetric precision. IR spectropolarimetry is less affected than optical by dust scattering in the circumstellar and interstellar media, thereby providing a more unbiased probe of the intrinsic geometry of the SN ejecta. SN 2018hna, a SN 1987A-like explosion, shows 2.0 ± 0.3% continuum polarization in the J band oriented at ∼160°on-sky at 182 d after the explosion. Assuming prolate geometry like in SN 1987A, we infer an ejecta axis ratio of <0.48 with the axis of symmetry pointing at 70°position angle. The axis ratio is similar to that of SN 1987A suggesting that they may share intrinsic geometry and inclination angle. Our data do not rule out oblate ejecta. We also observe one other core-collapse and two thermonuclear SNe in the J band. SN 2020oi, a stripped-envelope Type Ic SN in Messier 100 has p = 0.37 ± 0.09% at peak light, indicative of either a 10% asymmetry or host interstellar polarization. The SNe Ia, 2019ein and 2020ue have p <0.33% and <1.08% near peak light, indicative of asymmetries of less than 10% and 20%, respectively.

show abstract

“…Follow-up of SN 2020oi in the radio in the days after discovery revealed a potential 10 GHz source and a confirmed 44 GHz source with the VLA (Horesh & Sfaradi 2020a,b), a detection at 15.5 GHz with AMI-LA (Sfaradi et al 2020), and a detection at 5.1 GHz with e-MERLIN (Moldon et al 2020). Horesh et al (2020) presents the ZTF optical observations as well as radio data for SN 2020oi; they model the radio observations and find that the density structure of the circumstellar material in the progenitor system might not follow the expected 𝑟 −2 distribution, but that otherwise SN 2020oi is a standard Type Ic SN. Optical and near-infrared observations of SN Ic 2020oi are also presented and analyzed by Rho et al (2020), who confirm it to be a normal representative of the Type Ic class but which, uniquely, exhibits signatures of dust formation starting >60 days after explosion.…”

Section: Sn 2020oi (Sn Ic)mentioning

confidence: 94%

Supernova siblings and their parent galaxies in the Zwicky Transient Facility Bright Transient Survey

Graham

Fremling

Perley

et al. 2022

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Supernova (SN) siblings – two or more SNe in the same parent galaxy – are useful tools for exploring progenitor stellar populations as well as properties of the host galaxies such as distance, star formation rate, dust extinction, and metallicity. Since the average SN rate for a Milky Way-type galaxy is just one per century, a large imaging survey is required to discover an appreciable sample of SN siblings. From the wide-field Zwicky Transient Facility (ZTF) Bright Transient Survey (BTS; which aims for spectroscopic completeness for all transients which peak brighter than r <18.5 mag) we present 10 SN siblings in 5 parent galaxies. For each of these families we analyse the SN’s location within the host and its underlying stellar population, finding agreement with expectations that SNe from more massive progenitors are found nearer to their host core and in regions of more active star formation. We also present an analysis of the relative rates of core collapse and thermonuclear SN siblings, finding a significantly lower ratio than past SN sibling samples due to the unbiased nature of the ZTF.

show abstract

A Non-equipartition Shock Wave Traveling in a Dense Circumstellar Environment around SN 2020oi

Cited by 26 publications

References 52 publications

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

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

Infrared spectropolarimetric detection of intrinsic polarization from a core-collapse supernova

Supernova siblings and their parent galaxies in the Zwicky Transient Facility Bright Transient Survey

Contact Info

Product

Resources

About