Far-ultraviolet to Near-infrared Observations of SN 2023ixf: A High-energy Explosion Engulfed in Complex Circumstellar Material

Teja, Rishabh Singh; Singh, Avinash; Basu, Judhajeet; Anupama, G. C.; Sahu, D. K.; Dutta, Anirban; Swain, Vishwajeet; Nakaoka, Tatsuya; Pathak, Utkarsh; Bhalerao, Varun; Barway, Sudhanshu; Kumar, Harsh; A. J., Nayana; Imazawa, Ryo; Kumar, Brajesh; Kawabata, Koji S.

doi:10.3847/2041-8213/acef20

Cited by 32 publications

(7 citation statements)

References 91 publications

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“…All of the comparison SNe are Type IIP/L SNe with the exception of SN 2013cu, which is a Type IIb (Leonard et al 2000;Gal-Yam et al 2014;Terreran et al 2016Terreran et al , 2022Yaron et al 2017;Tartaglia et al 2021). Their light curves show similarly shallow linear declines in V band, with SN 2013cu being the steepest (Bianciardi et al 2023;Hiramatsu et al 2023;Jacobson-Galan et al 2023;Teja et al 2023;Yamanaka et al 2023).…”

Section: Comparison To Other Flash Snementioning

confidence: 99%

Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf

Bostroem,

Pearson,

Shrestha

et al. 2023

ApJL

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We present the optical spectroscopic evolution of SN 2023ixf seen in subnight cadence spectra from 1.18 to 15 days after explosion. We identify high-ionization emission features, signatures of interaction with material surrounding the progenitor star, that fade over the first 7 days, with rapid evolution between spectra observed within the same night. We compare the emission lines present and their relative strength to those of other supernovae with early interaction, finding a close match to SN 2020pni and SN 2017ahn in the first spectrum and SN 2014G at later epochs. To physically interpret our observations, we compare them to CMFGEN models with confined, dense circumstellar material around a red supergiant (RSG) progenitor from the literature. We find that very few models reproduce the blended N iii (λλ4634.0,4640.6)/C iii (λλ4647.5,4650.0) emission lines observed in the first few spectra and their rapid disappearance thereafter, making this a unique diagnostic. From the best models, we find a mass-loss rate of 10−3–10−2 M ⊙ yr−1, which far exceeds the mass-loss rate for any steady wind, especially for an RSG in the initial mass range of the detected progenitor. These mass-loss rates are, however, similar to rates inferred for other supernovae with early circumstellar interaction. Using the phase when the narrow emission features disappear, we calculate an outer dense radius of circumstellar material R CSM,out ≈ 5 × 1014 cm, and a mean circumstellar material density of ρ = 5.6 × 10−14 g cm−3. This is consistent with the lower limit on the outer radius of the circumstellar material we calculate from the peak Hα emission flux, R CSM,out ≳ 9 × 1013 cm.

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Section: Comparison To Other Flash Snementioning

confidence: 99%

Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf

Bostroem,

Pearson,

Shrestha

et al. 2023

ApJL

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“…Their results are all consistent with an RSG progenitor enshrouded by a dusty envelope. The presence of dense circumstellar material (CSM) around the progenitor is also indicated by the fast rising luminosity of the SN and its early spectra with prominent and narrow nebular emission lines (Bostroem et al 2023;Hiramatsu et al 2023;Hosseinzadeh et al 2023;Jacobson-Galan et al 2023;Smith et al 2023;Teja et al 2023;Vasylyev et al 2023;Yamanaka et al 2023). However, the inferred progenitor mass is still under debate and can range from 8 to 10 M e up to ∼20 M e .…”

Section: Introductionmentioning

confidence: 99%

The Dusty Red Supergiant Progenitor and the Local Environment of the Type II SN 2023ixf in M101

Niu,

Sun,

Maund

et al. 2023

ApJL

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As one of the closest supernovae (SNe) in the last decade, SN 2023ixf is an unprecedented target to investigate the progenitor star that exploded. However, there is still significant uncertainty in the reported progenitor properties. In this work, we present a detailed study of SN 2023ixf’s progenitor with two independent analyses. We first modeled its spectral energy distribution (SED) based on Hubble Space Telescope optical, Spitzer mid-infrared (IR), and ground-based near-IR data. We find that stellar pulsation and circumstellar extinction have great impacts on SED fitting, and the result suggests a relatively massive red supergiant surrounded by C-rich dust with an initial mass of 16.2–17.4 M ⊙. The corresponding rate of mass loss occurring at least 3 yr before the SN explosion is about 2 × 10−4 M ⊙ yr−1. We also derived the star formation history of the SN environment based on resolved stellar populations, and the most recent star-forming epoch corresponds to a progenitor initial mass of 17–19 M ⊙, in agreement with that from our SED fitting. Therefore, we conclude that the progenitor of SN 2023ixf is close to the high-mass end for Type II SN progenitors.

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“…SN 2023ixf was classified as a Type II SN ) and showed a strong blue continuum and prominent optical flash-ionization features (H, He, N, and C) in its early-phase spectrum, all indicative of the presence of circumstellar medium (CSM). Interestingly, the early photometric and spectroscopic studies have revealed evidence of the interaction between the SN ejecta and a dense confined CSM that boosted the early-phase optical luminosity of the SN (Bostroem et al 2023;Hiramatsu et al 2023;Hosseinzadeh et al 2023;Jacobson-Galán et al 2023;Li et al 2023;Smith et al 2023;Teja et al 2023;Yamanaka et al 2023). The X-ray detection, starting about 4 days after the explosion, also supported the scenario of the circumstellar interaction (Chandra et al 2023;Grefenstette et al 2023;Mereminskiy et al 2023).…”

Section: Introductionmentioning

confidence: 78%

“…The foreground extinction from the Milky Way in the line of sight of SN 2023ixf is E(B − V ) MW =0.008 mag (Schlegel et al 1998;Schlafly & Finkbeiner 2011). For the host galaxy extinction, we used the result of Liu et al (2023) obtained by analyzing the spectral data from the Hobby Eberly Telescope Dark Energy Experiment, who obtained an extinction value of E(B − V ) host = 0.06 ± 0.14 mag that is slightly larger than E(B − V ) = 0.031 mag given by some previous works (Smith et al 2023;Teja et al 2023). Using the extinction law of Cardelli et al (1989) and assuming R V = 3.1, we obtain the extinction values of 0.338, 0.316, 0.221, 0.183, 0.117, and 0.095 mag accounting for both the Milky Way and host galaxy for the uvgriz bands, respectively.…”

Section: Multiband Photometric Observations and Data Reductionmentioning

confidence: 99%

Multiband Simultaneous Photometry of Type II SN 2023ixf with Mephisto and the Twin 50 cm Telescopes

Yang,

Liu,

Pan

et al. 2024

ApJ

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SN 2023ixf, recently reported in the nearby galaxy M101 at a distance of 6.85 Mpc, was one of the closest and brightest core-collapse supernovae in the last decade. In this work, we present multiwavelength photometric observation of SN 2023ixf with the Multi-channel Photometric Survey Telescope (Mephisto) in the uvgr bands and with the twin 50 cm telescopes in the griz bands. We find that the bolometric luminosity reached the maximum value of 3 × 1043 erg s−1 at 3.9 days after the explosion and fully settled onto the radioactive tail at ∼90 days. The effective temperature decreased from 3.2 × 104 K at the first observation and approached a constant of ∼(3000–4000) K after the first 2 months. The evolution of the photospheric radius is consistent with a homologous expansion with a velocity of 8700 km s−1 in the first 2 months, and it shrunk subsequently. Based on the radioactive tail, the initial nickel mass is about M Ni ∼ 0.098 M ⊙. The explosion energy and the ejecta mass are estimated to be E ≃ (1.0–5.7) × 1051 erg and M ej ≃ (3.8–16) M ⊙, respectively. The peak bolometric luminosity is proposed to be contributed by the interaction between the ejecta and the circumstellar medium (CSM). We find a shocked CSM mass of M CSM ∼ 0.013 M ⊙, a CSM density of ρ CSM ∼ 2.5 × 10−13 g cm−3, and a mass-loss rate of the progenitor of M ̇ ∼ 0.022 M ⊙ yr − 1 .

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Far-ultraviolet to Near-infrared Observations of SN 2023ixf: A High-energy Explosion Engulfed in Complex Circumstellar Material

Cited by 32 publications

References 91 publications

Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf

Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf

The Dusty Red Supergiant Progenitor and the Local Environment of the Type II SN 2023ixf in M101

Multiband Simultaneous Photometry of Type II SN 2023ixf with Mephisto and the Twin 50 cm Telescopes

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