14 research outputs found
A Comprehensive Investigation of Gamma-Ray Burst Afterglows Detected by TESS
Gamma-ray bursts produce afterglows that can be observed across the
electromagnetic spectrum and can provide insight into the nature of their
progenitors. While most telescopes that observe afterglows are designed to
rapidly react to trigger information, the Transiting Exoplanet Survey Satellite
(TESS) continuously monitors sections of the sky at cadences between 30 minutes
and 200 seconds. This provides TESS with the capability of serendipitously
observing the optical afterglow of GRBs. We conduct the first extensive search
for afterglows of known GRBs in archival TESS data reduced with the TESSreduce
package, and detect 11 candidate signals that are temporally coincident with
reported burst times. We classify 3 of these as high-likelihood GRB afterglows
previously unknown to have been detected by TESS, one of which has no other
afterglow detection reported on the Gamma-ray Coordinates Network. We classify
5 candidates as tentative and the remainder as unlikely. Using the afterglowpy
package, we model each of the candidate light curves with a Gaussian and a top
hat model to estimate burst parameters; we find that a mean time delay of
s between the explosion and afterglow onset is required to perform
these fits. The high cadence and large field of view make TESS a powerful
instrument for localising GRBs, with the potential to observe afterglows in
cases when no other backup photometry is possible.Comment: 17 pages, 7 figures, 5 table
Probing Interstellar Dust with Infrared Echoes from the Cas A Supernova
We present the analysis of an IRS 5-38 {\mu}m spectrum and MIPS photometric
measurements of an infrared echo near the Cassiopeia A supernova remnant
observed with the Spitzer Space Telescope. We have modeled the recorded echo
accounting for PAHs, quantum-heated carbon and silicate grains, as well as
thermal carbon and silicate particles. Using the fact that optical light echo
spectroscopy has established that Cas A originated from a type IIb supernova
explosion showing an optical spectrum remarkably similar to the prototypical
type IIb SN 1993J, we use the latter to construct template data input for our
simulations. We are then able to reproduce the recorded infrared echo spectrum
by combining the emission of dust heated by the UV burst produced at the shock
breakout after the core-collapse and dust heated by optical light emitted near
the visual maximum of the supernova light curve, where the UV burst and optical
light curve characteristics are based on SN 1993J. We find a mean density of
\sim680 H cm^{-3} for the echo region, with a size of a few light years across.
We also find evidence of dust processing in the form of a lack of small PAHs
with less than \sim300 carbon atoms, consistent with a scenario of PAHs
destruction by the UV burst via photodissociation at the estimated distance of
the echo region from Cas A. Furthermore, our simulations suggest that the weak
11 {\mu}m features of our recorded infrared echo spectrum are consistent with a
strong dehydrogenated state of the PAHs. This exploratory study highlights the
potential of investigating dust processing in the interstellar medium through
infrared echoes.Comment: 16 pages, 14 figures, accepted for publication in the Astrophysical
Journa
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
Evidence for Extended Hydrogen-Poor CSM in the Three-Peaked Light Curve of Stripped Envelope Ib Supernova
We present multi-band ATLAS photometry for SN 2019tsf, a stripped-envelope
Type Ib supernova (SESN). The SN shows a triple-peaked light curve and a late
(re-)brightening, making it unique among stripped-envelope systems. The
re-brightening observations represent the latest photometric measurements of a
multi-peaked Type Ib SN to date. As late-time photometry and spectroscopy
suggest no hydrogen, the potential circumstellar material (CSM) must be H-poor.
Moreover, late (>150 days) spectra show no signs of narrow emission lines,
further disfavouring CSM interaction. On the contrary, an extended CSM
structure is seen through a follow-up radio campaign with Karl G. Jansky Very
Large Array (VLA), indicating a source of bright optically thick radio emission
at late times, which is highly unusual among H-poor SESNe. We attribute this
phenomenology to an interaction of the supernova ejecta with
spherically-asymmetric CSM, potentially disk-like, and we present several
models that can potentially explain the origin of this rare Type Ib supernova.
The warped disc model paints a novel picture, where the tertiary companion
perturbs the progenitors CSM, that can explain the multi-peaked light curves of
SNe, and here we apply it to SN 2019tsf. This SN 2019tsf is likely a member of
a new sub-class of Type Ib SNe and among the recently discovered class of SNe
that undergo mass transfer at the moment of explosionComment: 23 pages, Comments are welcome, Submitted to Ap
SN 2022oqm: A Multi-peaked Calcium-rich Transient from a White Dwarf Binary Progenitor System
We present the photometric and spectroscopic evolution of SN 2022oqm, a
nearby multi-peaked hydrogen- and helium-weak calcium-rich transient (CaRT). SN
2022oqm was detected 19.9 kpc from its host galaxy, the face-on spiral galaxy
NGC 5875. Extensive spectroscopic coverage reveals a hot (T >= 40,000 K)
continuum and carbon features observed ~1 day after discovery, SN Ic-like
photospheric-phase spectra, and strong forbidden calcium emission starting 38
days after discovery. SN 2022oqm has a relatively high peak luminosity (MB =
-17 mag) for CaRTs, making it an outlier in the population. We determine that
three power sources are necessary to explain SN 2022oqm's light curve, with
each power source corresponding to a distinct peak in its light curve. The
first peak of the light curve is powered by an expanding blackbody with a power
law luminosity, consistent with shock cooling by circumstellar material.
Subsequent peaks are powered by a double radioactive decay model, consistent
with two separate sources of photons diffusing through an optically thick
ejecta. From the optical light curve, we derive an ejecta mass and 56Ni mass of
~0.89 solar masses and ~0.09 solar masses, respectively. Detailed spectroscopic
modeling reveals ejecta that is dominated by intermediate-mass elements, with
signs that Fe-peak elements have been well-mixed. We discuss several physical
origins for SN 2022oqm and favor a white dwarf progenitor model. The inferred
ejecta mass points to a surprisingly massive white dwarf, challenging models of
CaRT progenitors.Comment: 33 pages, 17 figures, 5 tables, Submitted to Ap
Final Moments. I. Precursor Emission, Envelope Inflation, and Enhanced Mass Loss Preceding the Luminous Type II Supernova 2020tlf
International audienceWe present panchromatic observations and modeling of supernova (SN) 2020tlf, the first normal Type II-P/L SN with confirmed precursor emission, as detected by the Young Supernova Experiment transient survey. Pre-SN activity was detected in riz-bands at −130 days and persisted at relatively constant flux until first light. Soon after discovery, “flash” spectroscopy of SN 2020tlf revealed narrow, symmetric emission lines that resulted from the photoionization of circumstellar material (CSM) shed in progenitor mass-loss episodes before explosion. Surprisingly, this novel display of pre-SN emission and associated mass loss occurred in a red supergiant (RSG) progenitor with zero-age main-sequence mass of only 10–12 M , as inferred from nebular spectra. Modeling of the light curve and multi-epoch spectra with the non-LTE radiative-transfer code CMFGEN and radiation-hydrodynamical code HERACLES suggests a dense CSM limited to r ≈ 10 cm, and mass-loss rate of 10 M yr. The luminous light-curve plateau and persistent blue excess indicates an extended progenitor, compatible with an RSG model with R = 1100 R . Limits on the shock-powered X-ray and radio luminosity are consistent with model conclusions and suggest a CSM density of ρ < 2 × 10 g cm for distances from the progenitor star of r ≈ 5 × 10 cm, as well as a mass-loss rate of at larger distances. A promising power source for the observed precursor emission is the ejection of stellar material following energy disposition into the stellar envelope as a result of gravity waves emitted during either neon/oxygen burning or a nuclear flash from silicon combustion
Revealing the progenitor of SN 2021zby through analysis of the TESS shock-cooling light curve
We present early observations and analysis of the double-peaked Type IIb supernova (SN IIb) SN 2021zby. TESS 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 multiband 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 ∼0.30–0.65 M⊙ and an envelope radius of ∼120–300 R⊙. These inferred progenitor properties are similar to those of other SNe IIb with a double-peaked 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 multiband observations, particularly UV, are also necessary to fully constrain the progenitor propertie
SN 2018agk: a prototypical type Ia supernova with a smooth power-law rise in kepler (K2)
We present the 30 minutes cadence Kepler/K2 light curve of the Type Ia supernova (SN Ia) SN 2018agk, covering approximately one week before explosion, the full rise phase, and the decline until 40 days after peak. We additionally present ground-based observations in multiple bands within the same time range, including the 1 day cadence DECam observations within the first ∼5 days after the first light. The Kepler early light curve is fully consistent with a single power-law rise, without evidence of any bump feature. We compare SN 2018agk with a sample of other SNe Ia without early excess flux from the literature. We find that SNe Ia without excess flux have slowly evolving early colors in a narrow range (g − i ≈ −0.20 ± 0.20 mag) within the first ∼10 days. On the other hand, among SNe Ia detected with excess, SN 2017cbv and SN 2018oh tend to be bluer, while iPTF16abc's evolution is similar to normal SNe Ia without excess in g − i. We further compare the Kepler light curve of SN 2018agk with companion-interaction models, and rule out the existence of a typical nondegenerate companion undergoing Roche lobe overflow at viewing angles smaller than 45°
SN 2018agk:a prototypical type Ia supernova with a smooth power-law rise in Kepler (K2)
We present the 30-min cadence Kepler/K2 light curve of the Type Ia supernova
(SN Ia) SN 2018agk, covering approximately one week before explosion, the full
rise phase and the decline until 40 days after peak. We additionally present
ground-based observations in multiple bands within the same time range,
including the 1-day cadence DECam observations within the first 5 days
after the first light. The Kepler early light curve is fully consistent with a
single power-law rise, without evidence of any bump feature. We compare SN
2018agk with a sample of other SNe~Ia without early excess flux from the
literature. We find that SNe Ia without excess flux have slowly-evolving early
colors in a narrow range ( mag) within the first days. On the other hand, among SNe Ia detected with excess, SN 2017cbv and
SN 2018oh tend to be bluer, while iPTF16abc's evolution is similar to normal
SNe Ia without excess in . We further compare the Kepler light curve of SN
2018agk with companion-interaction models, and rule out the existence of a
typical non-degenerate companion undergoing Roche-lobe overflow at viewing
angles smaller than .Comment: 20 pages, 14 figures, 5 tables. Published in Ap