Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp

S. Vasylyev, Sergiy; Vogl, Christian; Yang 杨, Yi 轶; Filippenko, Alexei V.; Brink, Thomas G.; Brown, Peter J.; Matheson, Thomas; Modjaz, Maryam; Gal-Yam, Avishay; Mazzali, Paolo A.; de Jaeger, Thomas; Patra, Kishore C.; Stewart, Gabrielle E.

doi:10.3847/2041-8213/ad0e6b

Cited by 3 publications

(1 citation statement)

References 42 publications

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“…These effects are included in their latest analytical model. Line blanketing in the UV is observed in the few earlytime UV spectra of SNe II (Brown et al 2007;Vasylyev et al 2022Vasylyev et al , 2023Bostroem et al 2023a;Zimmerman et al 2024). Recently, Zimmerman et al (2024) confirmed the presence of emission lines from highly ionized species in the UV, as well as photospheric absorption features that appear in the UV while the optical spectrum is still a smooth continuum around T ∼ 15,000 K. 3.…”

Section: Color Evolutionmentioning

confidence: 88%

The Early Ultraviolet Light Curves of Type II Supernovae and the Radii of Their Progenitor Stars

Irani,

Morag,

Gal-Yam

et al. 2024

ApJ

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We present a sample of 34 normal Type II supernovae (SNe II) detected with the Zwicky Transient Facility, with multiband UV light curves starting at t ≤ 4 days after explosion, and X-ray observations. We characterize the early UV-optical color, provide empirical host-extinction corrections, and show that the t > 2 day UV-optical colors and the blackbody evolution of the sample are consistent with shock cooling (SC) regardless of the presence of “flash ionization” features. We present a framework for fitting SC models that can reproduce the parameters of a set of multigroup simulations up to 20% in radius and velocity. Observations of 15 SNe II are well fit by models with breakout radii <1014 cm. Eighteen SNe are typically more luminous, with observations at t ≥ 1 day that are better fit by a model with a large >1014 cm breakout radius. However, these fits predict an early rise during the first day that is too slow. We suggest that these large-breakout events are explosions of stars with an inflated envelope or with confined circumstellar material (CSM). Using the X-ray data, we derive constraints on the extended (∼1015 cm) CSM density independent of spectral modeling and find that most SN II progenitors lose M ̇ < 10 − 4 M ⊙ yr − 1 up to a few years before explosion. We show that the overall observed breakout radius distribution is skewed to higher radii due to a luminosity bias. We argue that the 66 − 22 + 11 % of red supergiants (RSGs) explode as SNe II with breakout radii consistent with the observed distribution of RSGs, with a tail extending to large radii, likely due to the presence of CSM.

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Section: Color Evolutionmentioning

confidence: 88%

The Early Ultraviolet Light Curves of Type II Supernovae and the Radii of Their Progenitor Stars

Irani,

Morag,

Gal-Yam

et al. 2024

ApJ

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The complex circumstellar environment of supernova 2023ixf

Zimmerman,

Irani,

Chen

et al. 2024

Nature

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Circumstellar Interaction in the Ultraviolet Spectra of SN 2023ixf 14–66 Days After Explosion

Bostroem,

Sand,

Dessart

et al. 2024

ApJL

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SN 2023ixf was discovered in M101 within a day of the explosion and rapidly classified as a Type II supernova with flash features. Here we present ultraviolet (UV) spectra obtained with the Hubble Space Telescope 14, 19, 24, and 66 days after the explosion. Interaction between the supernova ejecta and circumstellar material (CSM) is seen in the UV throughout our observations in the flux of the first three epochs and asymmetric Mg ii emission on day 66. We compare our observations to CMFGEN supernova models that include CSM interaction ( M ̇ < 10 − 3 M ⊙ yr−1) and find that the power from CSM interaction is decreasing with time, from L sh ≈ 5 × 1042 erg s−1 to L sh ≈ 1 × 1040 erg s−1 between days 14 and 66. We examine the contribution of individual atomic species to the spectra on days 14 and 19, showing that the majority of the features are dominated by iron, nickel, magnesium, and chromium absorption in the ejecta. The UV spectral energy distribution of SN 2023ixf sits between that of supernovae, which show no definitive signs of CSM interaction, and those with persistent signatures assuming the same progenitor radius and metallicity. Finally, we show that the evolution and asymmetric shape of the Mg ii λ λ 2796, 2802 emission are not unique to SN 2023ixf. These observations add to the early measurements of dense, confined CSM interaction, tracing the mass-loss history of SN 2023ixf to ∼33 yr prior to the explosion and the density profile to a radius of ∼5.7 × 1015 cm. They show the relatively short evolution from a quiescent red supergiant wind to high mass loss.

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Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp

Cited by 3 publications

References 42 publications

The Early Ultraviolet Light Curves of Type II Supernovae and the Radii of Their Progenitor Stars

The Early Ultraviolet Light Curves of Type II Supernovae and the Radii of Their Progenitor Stars

The complex circumstellar environment of supernova 2023ixf

Circumstellar Interaction in the Ultraviolet Spectra of SN 2023ixf 14–66 Days After Explosion

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