Jennifer E. Andrews

Gemini North Observatory

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Co-Authors

Nathan Smith

University of Arizona

146

David J. Sand

University of Arizona

122

S. Valenti

Medical College of Wisconsin

111

M. Lundquist

W.M. Keck Observatory

D. A. Howell

Las Cumbres Observatory Global Telescope Network

J. Jencson

California Institute of Technology

S. Wyatt

University of Washington

C. McCully

Las Cumbres Observatory Global Telescope Network

G. Hosseinzadeh

University of Arizona

K. Azalee Bostroem

University of Arizona

Cooperative Institutions

University of Arizona

131

Chinese Academy of Sciences

127

Hospital Clínic de Barcelona

123

Space Telescope Science Institute

114

University of California, Berkeley

108

California Institute of Technology

Center for Astrophysics Harvard & Smithsonian

Max Planck Society

University of Chinese Academy of Sciences

Johns Hopkins University

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Late-time spectroscopy of SN 2002hh: a continued visible light echo with no shock interaction yet

Monthly Notices of the Royal Astronomical Society (2015)

Jennifer E. Andrews Nathan Smith Jon C. Mauerhan

Supernova (SN) 2002hh was unusual among core-collapse SNe because it was highly reddened, and displayed a bright infrared (IR) excess due to radiatively heated dust in its circumstellar medium (CSM). Estimates for the mass of dust responsible for the IR echo suggested the presence of a massive shell within 0.26 pc of the star. For a velocity of 5000–10 000 km s−1, this material should be hit by the SN blast wave at late times, starting at roughly 12 years post-explosion. We have obtained deep late-time spectra with the Multiple Mirror Telescope (MMT) Blue Channel spectrograph to search for any spectral signatures of ongoing shock interaction. Interaction with a strength comparable to SN 1987A's collision with the equatorial ring would be detected in our data. However, in the spectra reported here, we do not detect clear signs of strong CSM interaction, contrary to expectations based on the reported radii of the dust shell. We do, however, detect emission associated with the old SN, and we find that the broad lines in the spectrum indicate a continuation of an ongoing reflected light echo, which appears similar to the spectrum at peak luminosity for this Type II-P event.

Cassiopeia A

10.1093/mnras/stv1094

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Serendipitous detection of the dusty Type IIL SN 1980K with JWST/MIRI

Szanna Zsíros Tamás Szalai I. De Looze Arkaprabha Sarangi Melissa Shahbandeh

We present mid-infrared (mid-IR) imaging of the Type IIL supernova (SN) 1980K with the James Webb Space Telescope (JWST) more than 40 yr post-explosion. SN 1980K, located in the nearby ($D\approx7$ Mpc) "SN factory" galaxy NGC 6946, was serendipitously captured in JWST/MIRI images taken of the field of SN 2004et in the same galaxy. SN 1980K serves as a promising candidate for studying the transitional phase between young SNe and older SN remnants and also provides a great opportunity to investigate its the close environment. SN 1980K can be identified as a clear and bright point source in all eight MIRI filters from F560W up to F2550W. We fit analytical dust models to the mid-IR spectral energy distribution that reveal a large amount ($M_d \approx 0.002 {M}_{\odot}$) of Si-dominated dust at $T_{dust}\approx 150$ K (accompanied by a hotter dust/gas component), and also computed numerical SED dust models. Radiative transfer modeling of a late-time optical spectrum obtained recently with Keck discloses that an even larger ($\sim 0.24-0.58~{M}_{\odot}$) amount of dust is needed in order for selective extinction to explain the asymmetric line profile shapes observed in SN 1980K. As a conclusion, with JWST, we may see i) pre-existing circumstellar dust heated collisionally (or, partly radiatively), analogous to the equatorial ring of SN 1987A, or ii) the mid-IR component of the presumed newly-formed dust, accompanied by much more colder dust present in the ejecta (as suggested by the late-time the optical spectra).

Extinction (optical mineralogy)

Spectral energy distribution

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Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi

The Astrophysical Journal Letters (2024)

Manisha Shrestha K. Azalee Bostroem David J. Sand G. Hosseinzadeh Jennifer E. Andrews

Abstract We present high-cadence photometric and spectroscopic observations of supernova (SN) 2024ggi, a Type II SN with flash spectroscopy features, which exploded in the nearby galaxy NGC 3621 at ∼7 Mpc. The light-curve evolution over the first 30 hr can be fit by two power-law indices with a break after 22 hr, rising from M V ≈ −12.95 mag at +0.66 day to M V ≈ −17.91 mag after 7 days. In addition, the densely sampled color curve shows a strong blueward evolution over the first few days and then behaves as a normal SN II with a redward evolution as the ejecta cool. Such deviations could be due to interaction with circumstellar material (CSM). Early high- and low-resolution spectra clearly show high-ionization flash features from the first spectrum to +3.42 days after the explosion. From the high-resolution spectra, we calculate the CSM velocity to be 37 ± 4 km s −1 . We also see the line strength evolve rapidly from 1.22 to 1.49 days in the earliest high-resolution spectra. Comparison of the low-resolution spectra with CMFGEN models suggests that the pre-explosion mass-loss rate of SN 2024ggi falls in the range of 10 −3 –10 −2 M ☉ yr −1 , which is similar to that derived for SN 2023ixf. However, the rapid temporal evolution of the narrow lines in the spectra of SN 2024ggi ( R CSM ∼ 2.7 × 10 14 cm) could indicate a smaller spatial extent of the CSM than in SN 2023ixf ( R CSM ∼ 5.4 × 10 14 cm), which in turn implies a lower total CSM mass for SN 2024ggi.

Breakout

Circumstellar disk

10.3847/2041-8213/ad6907

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Identifying the SN 2022acko progenitor with JWST

arXiv (Cornell University) (2023)

Schuyler D. Van Dyk K. Azalee Bostroem Jennifer E. Andrews Yize Dong A. V. Filippenko

We report on analysis using the James Webb Space Telescope (JWST) to identify a candidate progenitor star of the Type II-plateau supernova SN 2022acko in the nearby, barred spiral galaxy NGC 1300. To our knowledge, our discovery represents the first time JWST has been used to localize a progenitor system in pre-explosion archival Hubble Space Telescope (HST) images. We astrometrically registered a JWST NIRCam image from 2023 January, in which the SN was serendipitously captured, to pre-SN HST F160W and F814W images from 2017 and 2004, respectively. An object corresponding precisely to the SN position has been isolated with reasonable confidence. That object has a spectral energy distribution (SED) and overall luminosity consistent with a single-star model having an initial mass possibly somewhat less than the canonical 8 Msun theoretical threshold for core collapse (although masses as high as 9 Msun for the star are also possible); however, the star's SED and luminosity are inconsistent with that of a super-asymptotic giant branch star which might be a forerunner of an electron-capture SN. The properties of the progenitor alone imply that SN 2022acko is a relatively normal SN II-P, albeit most likely a low-luminosity one. The progenitor candidate should be confirmed with follow-up HST imaging at late times, when the SN has sufficiently faded. This potential use of JWST opens a new era of identifying SN progenitor candidates at high spatial resolution.

Spitzer Space Telescope

Spectral energy distribution

Star (game theory)

10.48550/arxiv.2302.00274

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VizieR Online Data Catalog: Gemini/GMOS-S spectra of the type IIn SN 2010jl (Bevan+, 2020)

VizieR Online Data Catalog (2021)

Antonia Bevan Kelsie Krafton R. Wesson Jennifer E. Andrews Edward Montiel

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Evidence of weak circumstellar medium interaction in the Type II SN 2023axu

arXiv (Cornell University) (2023)

Manisha Shrestha Jeniveve Pearson S. Wyatt David J. Sand G. Hosseinzadeh

We present high-cadence photometric and spectroscopic observations of SN~2023axu, a classical Type II supernova with an absolute $V$-band peak magnitude of $-16.5 \pm 0.1$ mag. SN~2023axu was discovered by the Distance Less Than 40 Mpc (DLT40) survey within 1 day of the last non-detection in the nearby galaxy NGC 2283 at 13.7 Mpc. We modeled the early light curve using a recently updated shock cooling model that includes the effects of line blanketing and found the explosion epoch to be MJD 59971.48 $\pm$ 0.03 and the probable progenitor to be a red supergiant with a radius of 417 $\pm$ 28 $R_\odot$. The shock cooling model cannot match the rise of observed data in the $r$ and $i$ bands and underpredicts the overall UV data which points to possible interaction with circumstellar material. This interpretation is further supported by spectral behavior. We see a ledge feature around 4600 \AA\ in the very early spectra (+1.1 and +1.5 days after the explosion) which can be a sign of circumstellar interaction. The signs of circumstellar material are further bolstered by the presence of absorption features blueward of H$\alpha$ and H$\beta$ at day $>$40 which is also generally attributed to circumstellar interaction. Our analysis shows the need for high-cadence early photometric and spectroscopic data to decipher the mass-loss history of the progenitor.

Blanketing

Circumstellar envelope

Extinction (optical mineralogy)

10.48550/arxiv.2310.00162

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SN~2015da: Late-time observations of a persistent superluminous Type~IIn supernova with post-shock dust formation

arXiv (Cornell University) (2023)

Nathan Smith Jennifer E. Andrews Peter Milne A. V. Filippenko Thomas G. Brink

We present photometry and spectroscopy of the slowly evolving superluminous Type IIn SN2015da. SN2015da is extraordinary for its very high peak luminosity, and also for sustaining a high luminosity for several years. Even at 8\,yr after explosion, SN2015da remains as luminous as the peak of a normal SNII-P. The total radiated energy integrated over this time period (with no bolometric correction) is at least 1.6 FOE. Including a mild bolometric correction, adding kinetic energy of the expanding cold dense shell of swept-up circumstellar material (CSM), and accounting for asymmetry, the total explosion kinetic energy was likely 5-10 FOE. Powering the light curve with CSM interaction requires an energetic explosion and 20 Msun of H-rich CSM, which in turn implies a massive progenitor system above 30 Msun. Narrow P Cyg features show steady CSM expansion at 90 km/s, requiring a high average mass-loss rate of roughly 0.1 Msun/yr sustained for 2 centuries before explosion (although ramping up toward explosion time). No current theoretical model for single-star pre-SN mass loss can account for this. The slow CSM, combined with broad wings of H$\alpha$ indicating H-rich material in the unshocked ejecta, disfavor a pulsational pair instability model for the pre-SN mass loss. Instead, violent pre-SN binary interaction is a likely cuprit. Finally, SN2015da exhibits the characteristic asymmetric blueshift in its emission lines from shortly after peak until the present epoch, adding another well-studied superluminous SNeIIn with unambiguous evidence of post-shock dust formation.

10.48550/arxiv.2312.00253

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Evidence for late-time dust formation in the ejecta of supernova SN~1995N from emission-line asymmetries

arXiv (Cornell University) (2023)

R. Wesson Antonia Bevan M. J. Barlow I. De Looze M. Matsuura

We present a study of the dust associated with the core-collapse supernova SN~1995N. Infrared emission detected 14--15 years after the explosion was previously attributed to thermally echoing circumstellar material associated with the SN progenitor. We argue that this late-time emission is unlikely to be an echo, and is more plausibly explained by newly formed dust in the supernova ejecta, indirectly heated by the interaction between the ejecta and the CSM. Further evidence in support of this scenario comes from emission line profiles in spectra obtained 22 years after the explosion; these are asymmetric, showing greater attenuation on the red wing, consistent with absorption by dust within the expanding ejecta. The spectral energy distribution and emission line profiles at epochs later than $\sim$5000 days are both consistent with the presence of about 0.4~M$_\odot$ of amorphous carbon dust. The onset of dust formation is apparent in archival optical spectra, taken between 700 and 1700 days after the assumed explosion date. As this is considerably later than most other instances where the onset of dust formation has been detected, we argue that the explosion date must be later than previously assumed.

Line (geometry)

Spectral energy distribution

Type II supernova

Pair-instability supernova

10.48550/arxiv.2308.09028

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Issue Information Page

Journal of Cardiac Surgery (2020)

Tessa Wa Shannon Msh Alexander A. Brescia David J. Burn Alex M. Wisniewski

to get the results it gets

10.1111/jocs.14113

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Asymmetries and Circumstellar Interaction in the Type II SN 2024bch

The Astrophysical Journal (2025)

Jennifer E. Andrews Manisha Shrestha K. Azalee Bostroem Yize Dong Jeniveve Pearson

Abstract We present a comprehensive multi-epoch photometric and spectroscopic study of SN 2024bch, a nearby (19.9 Mpc) Type II supernova (SN) with prominent early high-ionization emission lines. Optical spectra from 2.8 days after the estimated explosion reveal narrow lines of H i , He ii , C iv , and N iv that disappear by day 6. High-cadence photometry from the ground and Transiting Exoplanet Survey Satellite show that the SN brightened quickly and reached a peak M V ~ −17.8 mag within a week of explosion, and late-time photometry suggests a 56 Ni mass of 0.050 M ⊙ . High-resolution spectra from days 7.9 and 43 trace the unshocked circumstellar medium (CSM) and indicate a wind velocity of 30–40 km s −1 , a value consistent with a red supergiant (RSG) progenitor. Comparisons between models and the early spectra suggest a pre-SN mass-loss rate of M ̇ ~ 1 0 − 3 – 1 0 − 2 M ⊙ yr − 1 , which is too high to be explained by quiescent mass loss from RSGs, but is consistent with some recent measurements of similar SNe. Persistent blueshifted H i and [O i ] emission lines seen in the optical and near-IR spectra could be produced by asymmetries in the SN ejecta, while the multicomponent H α may indicate continued interaction with an asymmetric CSM well into the nebular phase. SN 2024bch provides another clue to the complex environments and mass-loss histories around massive stars.

10.3847/1538-4357/ada555

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