The Renovated Thacher Observatory and First Science Results

Swift, Jonathan J.; Andersen, Karina; Arculli, Toby; Browning, Oakley; Ding, Jeffrey; Edwards, N. C.; Fanning, Tomás; Geyer, John B.; Huber, Grace; Jin-Ngo, Dylan; Kelliher, Ben; Kirkpatrick, Colin; Kirkpatrick, Liam; Klink, Douglas; Lavine, Connor; Lawrence, George N.; Lawrence, Yousef; Cyrus, Leung, Feng Lin; Luebbers, Julien; Myles, J.; O'Neill, Theo; Osuna, Jaime; Phipps, Peter; Rahman, Gazi; Rosenbaum, Teddy; Stacey, Holland; Stacey, Piper; Tang, Hadrien; Wood, Asher; Wilcox, Alejandro; Vyhnal, Christopher R.; Grace, Yang,; Yim, Jennifer; Yin, Yao; Zhang, Jack; Foley, R. J.; Gardner, Paul; Stafford, Greg; Rowe, D.J.; Ivarsen, K.; Hedrick, Richard

doi:10.1088/1538-3873/ac5aca

Cited by 4 publications

(1 citation statement)

References 43 publications

(55 reference statements)

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“…We observed SN 2023bee with the LCO 1 m telescope network in uBVgriz bands, the 1 m telescope at Lulin Observatory using the Lulin Compact Imager, and with the Thacher 0.7 m telescope in Ojai, CA from 2023 February 2 to March 11 in the griz bands (Swift et al 2022). Using the photpipe imaging and reduction pipeline (Rest et al 2005(Rest et al , 2014, we performed bad-pixel masking, reprojecting the data to a common pixel scale and pointing center using SWarp (Bertin 2010), photometry with DoPhot (Schechter et al 1993), and photometric calibration using the Pan- STARRS 3π (Flewelling et al 2020) and SkyMapper photometric catalogs (Onken et al 2019).…”

Section: Photometrymentioning

confidence: 99%

Flight of the Bumblebee: the Early Excess Flux of Type Ia Supernova 2023bee Revealed by TESS, Swift, and Young Supernova Experiment Observations

Wang,

Rest,

Dimitriadis

et al. 2024

ApJ

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We present high-cadence ultraviolet through near-infrared observations of the Type Ia supernova (SN Ia) 2023bee at D = 32 ± 3 Mpc, finding excess flux in the first days after explosion, particularly in our 10 minutes cadence TESS light curve and Swift UV data. Compared to a few other normal SNe Ia with early excess flux, the excess flux in SN 2023bee is redder in the UV and less luminous. We present optical spectra of SN 2023bee, including two spectra during the period where the flux excess is dominant. At this time, the spectra are similar to those of other SNe Ia but with weaker Si ii, C ii, and Ca ii absorption lines, perhaps because the excess flux creates a stronger continuum. We compare the data to several theoretical models on the origin of early excess flux in SNe Ia. Interaction with either the companion star or close-in circumstellar material is expected to produce a faster evolution than observed. Radioactive material in the outer layers of the ejecta, either from double detonation explosion or from a 56Ni clump near the surface, cannot fully reproduce the evolution either, likely due to the sensitivity of early UV observable to the treatment of the outer part of ejecta in simulation. We conclude that no current model can adequately explain the full set of observations. We find that a relatively large fraction of nearby, bright SNe Ia with high-cadence observations have some amount of excess flux within a few days of explosion. Considering potential asymmetric emission, the physical cause of this excess flux may be ubiquitous in normal SNe Ia.

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Section: Photometrymentioning

confidence: 99%

Flight of the Bumblebee: the Early Excess Flux of Type Ia Supernova 2023bee Revealed by TESS, Swift, and Young Supernova Experiment Observations

Wang,

Rest,

Dimitriadis

et al. 2024

ApJ

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Type II-P supernova progenitor star initial masses and SN 2020jfo: direct detection, light-curve properties, nebular spectroscopy, and local environment

Kilpatrick¹,

Izzo

Bentley

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present optical, ultraviolet, and infrared data of the type II supernova (SN II) 2020jfo at 14.5 Mpc. This wealth of multiwavelength data allows to compare different metrics commonly used to estimate progenitor masses of SN II for the same object. Using its early light curve, we infer SN 2020jfo had a progenitor radius of ≈700 R⊙, consistent with red supergiants of initial mass MZAMS =11–13 M⊙. The decline in its late-time light curve is best fit by a 56Ni mass of 0.018±0.007 M⊙ consistent with that ejected from SN II-P with ≈13 M⊙ initial mass stars. Early spectra and photometry do not exhibit signs of interaction with circumstellar matter, implying that SN 2020jfo experienced weak mass loss within the final years prior to explosion. Our spectra at >250 days are best fit by models from 12 M⊙ initial mass stars. We analyzed integral field unit spectroscopy of the stellar population near SN 2020jfo, finding its massive star population had a zero age main sequence mass of 9.7$\substack{+2.5\\ -1.3}~{\rm M}_{\odot }$. We identify a single counterpart in pre-explosion imaging and find it has an initial mass of at most $7.2\substack{+1.2\\ -0.6}~{\rm M}_{\odot }$. We conclude that the inconsistency between this mass and indirect mass indicators from SN 2020jfo itself is most likely caused by extinction with AV = 2–3 mag due to matter around the progenitor star, which lowered its observed optical luminosity. As SN 2020jfo did not exhibit extinction at this level or evidence for interaction with circumstellar matter between 1.6–450 days from explosion, we conclude that this material was likely confined within ≈3000 R⊙ from the progenitor star.

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Weak Mass Loss from the Red Supergiant Progenitor of the Type II SN 2021yja

Hosseinzadeh

Kilpatrick

Dong

et al. 2022

ApJ

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We present high-cadence optical, ultraviolet (UV), and near-infrared data of the nearby (D ≈ 23 Mpc) Type II supernova (SN) 2021yja. Many Type II SNe show signs of interaction with circumstellar material (CSM) during the first few days after explosion, implying that their red supergiant (RSG) progenitors experience episodic or eruptive mass loss. However, because it is difficult to discover SNe early, the diversity of CSM configurations in RSGs has not been fully mapped. SN 2021yja, first detected within ≈ 5.4 hours of explosion, shows some signatures of CSM interaction (high UV luminosity and radio and x-ray emission) but without the narrow emission lines or early light-curve peak that can accompany CSM. Here we analyze the densely sampled early light curve and spectral series of this nearby SN to infer the properties of its progenitor and CSM. We find that the most likely progenitor was an RSG with an extended envelope, encompassed by low-density CSM. We also present archival Hubble Space Telescope imaging of the host galaxy of SN 2021yja, which allows us to place a stringent upper limit of ≲ 9 M ☉ on the progenitor mass. However, this is in tension with some aspects of the SN evolution, which point to a more massive progenitor. Our analysis highlights the need to consider progenitor structure when making inferences about CSM properties, and that a comprehensive view of CSM tracers should be made to give a fuller view of the last years of RSG evolution.

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The Renovated Thacher Observatory and First Science Results

Cited by 4 publications

References 43 publications

Flight of the Bumblebee: the Early Excess Flux of Type Ia Supernova 2023bee Revealed by TESS, Swift, and Young Supernova Experiment Observations

Flight of the Bumblebee: the Early Excess Flux of Type Ia Supernova 2023bee Revealed by TESS, Swift, and Young Supernova Experiment Observations

Type II-P supernova progenitor star initial masses and SN 2020jfo: direct detection, light-curve properties, nebular spectroscopy, and local environment

Weak Mass Loss from the Red Supergiant Progenitor of the Type II SN 2021yja

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