171 research outputs found
SN 2022joj: A Potential Double Detonation with a Thin Helium shell
We present photometric and spectroscopic data for SN 2022joj, a nearby
peculiar Type Ia supernova (SN Ia) with a fast decline rate ( mag). SN 2022joj shows exceedingly red colors, with a value of
approximately mag during its initial stages, beginning from
days before maximum brightness. As it evolves the flux shifts towards the
blue end of the spectrum, approaching mag around maximum
light. Furthermore, at maximum light and beyond, the photometry is consistent
with that of typical SNe Ia. This unusual behavior extends to its spectral
characteristics, which initially displayed a red spectrum and later evolved to
exhibit greater consistency with typical SNe Ia. We consider two potential
explanations for this behavior: double detonation from a helium shell on a
sub-Chandrasekhar-mass white dwarf and Chandrasekhar-mass models with a shallow
distribution of . The shallow nickel models could not reproduce
the red colors in the early light curves. Spectroscopically, we find strong
agreement between SN 2022joj and double-detonation models with white dwarf
masses around 1 and thin He-shell between 0.01 and 0.02
. Moreover, the early red colors are explained by
line-blanketing absorption from iron-peak elements created by the double
detonation scenario in similar mass ranges. However, the nebular spectra
composition in SN 2022joj deviates from expectations for double detonation, as
we observe strong [Fe III] emission instead of [Ca II] lines as anticipated
from double detonation models. More detailed modeling, e.g., including viewing
angle effects, is required to test if double detonation models can explain the
nebular spectra
Revealing the progenitor of SN 2021zby through analysis of the shock-cooling light curve
We present early observations and analysis of the double-peaked Type IIb
supernova (SN IIb) 2021zby. captured the prominent early shock cooling
peak of SN 2021zby within the first 10 days after explosion with a
30-minute cadence. We present optical and near-infrared spectral series of SN
2021zby, including three spectra during the shock cooling phase. Using a
multi-band model fit, we find that the inferred properties of its progenitor
are consistent with a red supergiant or yellow supergiant, with an envelope
mass of 0.3-3.0 M and an envelope radius of 50-350. These inferred progenitor properties are similar to those of other
SNe IIb with double-peak feature, such as SNe 1993J, 2011dh, 2016gkg and
2017jgh. This study further validates the importance of the high cadence and
early coverage in resolving the shape of the shock cooling light curve, while
the multi-band observations, especially UV, is also necessary to fully
constrain the progenitor properties.Comment: 12 pages, 5 figures, 2 tables, submitted to ApJ
Spatial Models of Abundance and Habitat Preferences of Commerson’s and Peale’s Dolphin in Southern Patagonian Waters
Funding: This research was possible with the support of the Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET). Funding for travel to and accommodation for NAD in Aberdeen, Scotland was provided by CONICET and Cetacean Society International. The work of NAD was part of a postdoctoral fellowship funded by CONICET. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript.Peer reviewedPublisher PD
The assessment, serial evaluation, and subsequent sequelae of acute kidney injury (ASSESS-AKI) study: design and methods
<p>Abstract</p> <p>Background</p> <p>The incidence of acute kidney injury (AKI) has been increasing over time and is associated with a high risk of short-term death. Previous studies on hospital-acquired AKI have important methodological limitations, especially their retrospective study designs and limited ability to control for potential confounding factors.</p> <p>Methods</p> <p>The Assessment, Serial Evaluation, and Subsequent Sequelae of Acute Kidney Injury (ASSESS-AKI) Study was established to examine how a hospitalized episode of AKI independently affects the risk of chronic kidney disease development and progression, cardiovascular events, death, and other important patient-centered outcomes. This prospective study will enroll a cohort of 1100 adult participants with a broad range of AKI and matched hospitalized participants without AKI at three Clinical Research Centers, as well as 100 children undergoing cardiac surgery at three Clinical Research Centers. Participants will be followed for up to four years, and will undergo serial evaluation during the index hospitalization, at three months post-hospitalization, and at annual clinic visits, with telephone interviews occurring during the intervening six-month intervals. Biospecimens will be collected at each visit, along with information on lifestyle behaviors, quality of life and functional status, cognitive function, receipt of therapies, interim renal and cardiovascular events, electrocardiography and urinalysis.</p> <p>Conclusions</p> <p>ASSESS-AKI will characterize the short-term and long-term natural history of AKI, evaluate the incremental utility of novel blood and urine biomarkers to refine the diagnosis and prognosis of AKI, and identify a subset of high-risk patients who could be targeted for future clinical trials to improve outcomes after AKI.</p
Strong Carbon Features and a Red Early Color in the Underluminous Type Ia SN 2022xkq
We present optical, infrared, ultraviolet, and radio observations of SN
2022xkq, an underluminous fast-declining type Ia supernova (SN Ia) in NGC 1784
( Mpc), from to 180 days after explosion. The
high-cadence observations of SN 2022xkq, a photometrically transitional and
spectroscopically 91bg-like SN Ia, cover the first days and weeks following
explosion which are critical to distinguishing between explosion scenarios. The
early light curve of SN 2022xkq has a red early color and exhibits a flux
excess which is more prominent in redder bands; this is the first time such a
feature has been seen in a transitional/91bg-like SN Ia. We also present 92
optical and 19 near-infrared (NIR) spectra, beginning 0.4 days after explosion
in the optical and 2.6 days after explosion in the NIR. SN 2022xkq exhibits a
long-lived C I 1.0693 m feature which persists until 5 days post-maximum.
We also detect C II 6580 in the pre-maximum optical spectra. These
lines are evidence for unburnt carbon that is difficult to reconcile with the
double detonation of a sub-Chandrasekhar mass white dwarf. No existing
explosion model can fully explain the photometric and spectroscopic dataset of
SN 2022xkq, but the considerable breadth of the observations is ideal for
furthering our understanding of the processes which produce faint SNe Ia.Comment: 38 pages, 16 figures, accepted for publication in ApJ, the figure 15
input models and synthetic spectra are now available at
https://zenodo.org/record/837925
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Ground-based and JWST observations of SN 2022pul. I. Unusual signatures of carbon, oxygen, and circumstellar interaction in a peculiar type Ia supernova
Nebular-phase observations of peculiar Type Ia supernovae (SNe Ia) provide important constraints on progenitor scenarios and explosion dynamics for both these rare SNe and the more common, cosmologically useful SNe Ia. We present observations from an extensive ground- and space-based follow-up campaign to characterize SN 2022pul, a super-Chandrasekhar mass SN Ia (alternatively "03fg-like" SN), from before peak brightness to well into the nebular phase across optical to mid-infrared (MIR) wavelengths. The early rise of the light curve is atypical, exhibiting two distinct components, consistent with SN Ia ejecta interacting with dense carbon–oxygen (C/O)-rich circumstellar material (CSM). In the optical, SN 2022pul is most similar to SN 2012dn, having a low estimated peak luminosity (MB = −18.9 mag) and high photospheric velocity relative to other 03fg-like SNe. In the nebular phase, SN 2022pul adds to the increasing diversity of the 03fg-like subclass. From 168 to 336 days after peak B-band brightness, SN 2022pul exhibits asymmetric and narrow emission from [O i] λλ6300, 6364 (FWHM ≈ 2000 km s−1), strong, broad emission from [Ca ii] λλ7291, 7323 (FWHM ≈ 7300 km s−1), and a rapid Fe iii to Fe ii ionization change. Finally, we present the first ever optical-to-MIR nebular spectrum of an 03fg-like SN Ia using data from JWST. In the MIR, strong lines of neon and argon, weak emission from stable nickel, and strong thermal dust emission (with T ≈ 500 K), combined with prominent [O i] in the optical, suggest that SN 2022pul was produced by a white dwarf merger within C/O-rich CSM
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