29 research outputs found
AT2019wxt: An ultra-stripped supernova candidate discovered in electromagnetic follow-up of a gravitational wave trigger
We present optical, radio and X-ray observations of a rapidly-evolving
transient AT2019wxt (PS19hgw), discovered during the search for an
electromagnetic (EM) counterpart to the gravitational-wave (GW) trigger
S191213g (LIGO Scientific Collaboration & Virgo Collaboration 2019a). Although
S191213g was not confirmed as a significant GW event in the off-line analysis
of LIGO-Virgo data, AT2019wxt remained an interesting transient due its
peculiar nature. The optical/NIR light curve of AT2019wxt displayed a
double-peaked structure evolving rapidly in a manner analogous to currently
know ultra-stripped supernovae (USSNe) candidates. This double-peaked structure
suggests presence of an extended envelope around the progenitor, best modelled
with two-components: i) early-time shock-cooling emission and ii) late-time
radioactive Ni decay. We constrain the ejecta mass of AT2019wxt at
which indicates a significantly stripped
progenitor that was possibly in a binary system. We also followed-up AT2019wxt
with long-term Chandra and Jansky Very Large Array observations spanning
260 days. We detected no definitive counterparts at the location of
AT2019wxt in these long-term X-ray and radio observational campaigns. We
establish the X-ray upper limit at erg cm s
and detect an excess radio emission from the region of AT2019wxt. However,
there is little evidence for SN1993J- or GW170817-like variability of the radio
flux over the course of our observations. A substantial host galaxy
contribution to the measured radio flux is likely. The discovery and early-time
peak capture of AT2019wxt in optical/NIR observation during EMGW follow-up
observations highlights the need of dedicated early, multi-band photometric
observations to identify USSNe.Comment: 20 pages, 14 figures, Submitted to Ap
GROWTH on S190814bv: Deep Synoptic Limits on the Optical/Near-Infrared Counterpart to a Neutron Star-Black Hole Merger
On 2019 August 14, the Advanced LIGO and Virgo interferometers detected the high-significance gravitational wave (GW) signal S190814bv. The GW data indicated that the event resulted from a neutron star–black hole (NSBH) merger, or potentially a low-mass binary BH merger. Due to the low false-alarm rate and the precise localization (23 deg2 at 90%), S190814bv presented the community with the best opportunity yet to directly observe an optical/near-infrared counterpart to an NSBH merger. To search for potential counterparts, the GROWTH Collaboration performed real-time image subtraction on six nights of public Dark Energy Camera images acquired in the 3 weeks following the merger, covering >98% of the localization probability. Using a worldwide network of follow-up facilities, we systematically undertook spectroscopy and imaging of optical counterpart candidates. Combining these data with a photometric redshift catalog, we ruled out each candidate as the counterpart to S190814bv and placed deep, uniform limits on the optical emission associated with S190814bv. For the nearest consistent GW distance, radiative transfer simulations of NSBH mergers constrain the ejecta mass of S190814bv to be M_(ej) < 0.04 M⊙ at polar viewing angles, or M_(ej) < 0.03 M⊙ if the opacity is κ < 2 cm²g⁻¹. Assuming a tidal deformability for the NS at the high end of the range compatible with GW170817 results, our limits would constrain the BH spin component aligned with the orbital momentum to be χ < 0.7 for mass ratios Q < 6, with weaker constraints for more compact NSs
Long-rising Type II Supernovae in the Zwicky Transient Facility Census of the Local Universe
SN 1987A was an unusual hydrogen-rich core-collapse supernova originating
from a blue supergiant star. Similar blue supergiant explosions remain a small
family of events, and are broadly characterized by their long rises to peak.
The Zwicky Transient Facility (ZTF) Census of the Local Universe (CLU)
experiment aims to construct a spectroscopically complete sample of transients
occurring in galaxies from the CLU galaxy catalog. We identify 13 long-rising
(>40 days) Type II supernovae from the volume-limited CLU experiment during a
3.5 year period from June 2018 to December 2021, approximately doubling the
previously known number of these events. We present photometric and
spectroscopic data of these 13 events, finding peak r-band absolute magnitudes
ranging from -15.6 to -17.5 mag and the tentative detection of Ba II lines in 9
events. Using our CLU sample of events, we derive a long-rising Type II
supernova rate of Mpc yr,
1.4% of the total core-collapse supernova rate. This is the first
volumetric rate of these events estimated from a large, systematic,
volume-limited experiment.Comment: 32 pages, 17 figures, 5 tables. Submitted to Ap
Probing pre-supernova mass loss in double-peaked Type Ibc supernovae from the Zwicky Transient Facility
Eruptive mass loss of massive stars prior to supernova (SN) explosion is key
to understanding their evolution and end fate. An observational signature of
pre-SN mass loss is the detection of an early, short-lived peak prior to the
radioactive-powered peak in the lightcurve of the SN. This is usually
attributed to the SN shock passing through an extended envelope or
circumstellar medium (CSM). Such an early peak is common for double-peaked Type
IIb SNe with an extended Hydrogen envelope but is uncommon for normal Type Ibc
SNe with very compact progenitors. In this paper, we systematically study a
sample of 14 double-peaked Type Ibc SNe out of 475 Type Ibc SNe detected by the
Zwicky Transient Facility. The rate of these events is ~ 3-9 % of Type Ibc SNe.
A strong correlation is seen between the peak brightness of the first and the
second peak. We perform a holistic analysis of this sample's photometric and
spectroscopic properties. We find that six SNe have ejecta mass less than 1.5
Msun. Based on the nebular spectra and lightcurve properties, we estimate that
the progenitor masses for these are less than ~ 12 Msun. The rest have an
ejecta mass > 2.4 Msun and a higher progenitor mass. This sample suggests that
the SNe with low progenitor masses undergo late-time binary mass transfer.
Meanwhile, the SNe with higher progenitor masses are consistent with
wave-driven mass loss or pulsation-pair instability-driven mass loss
simulations.Comment: Submitted to ApJ. Comments are welcome. arXiv admin note: text
overlap with arXiv:2210.0572
Constraining the Kilonova Rate with Zwicky Transient Facility Searches Independent of Gravitational Wave and Short Gamma-ray Burst Triggers
The first binary neutron star merger, GW170817, was accompanied by a
radioactivity-powered optical/infrared transient called a kilonova. To date, no
compelling kilonova has been found during optical surveys of the sky,
independent of gravitational-wave triggers. In this work, we searched the first
23 months of the Zwicky Transient Facility (ZTF) data stream for candidate
kilonovae in the form of rapidly evolving transients. We combined ZTF alert
queries with forced point-spread-function photometry and nightly flux stacking
to increase our sensitivity to faint and fast transients. Automatic queries
yielded candidates, 24 of which passed quality checks and strict
selection criteria based on a grid of kilonova models tailored for both binary
neutron star and neutron star-black hole mergers. None of the candidates in our
sample was deemed a possible kilonova after thorough vetting, catalog
cross-matching, and study of their color evolution. The sources that passed our
selection criteria are dominated by Galactic cataclysmic variables. In
addition, we identified two fast transients at high Galactic latitude, one of
which is the confirmed afterglow of long-duration GRB190106A, and the other is
a possible cosmological afterglow. Using a survey simulation code, we
constrained the kilonova rate for a range of models including top-hat and
linearly decaying light curves and synthetic light curves obtained with
radiative transfer simulations. For prototypical GW170817-like kilonovae, we
constrain the rate to be Gpc yr at 95% confidence
level by requiring at least 2 high-significance detections. By assuming a
population of kilonovae with the same geometry and composition of GW170817
observed under a uniform viewing angle distribution, we obtained a constraint
on the rate of Gpc yr.Comment: Submitted for publication in Ap
Constraining the Kilonova Rate with Zwicky Transient Facility Searches Independent of Gravitational Wave and Short Gamma-Ray Burst Triggers
The first binary neutron star merger, GW170817, was accompanied by a radioactivity-powered optical/infrared transient called a kilonova. To date, no compelling kilonova has been found in all-sky optical surveys, independently of short gamma-ray burst and gravitational-wave triggers. In this work, we searched the first 23 months of the Zwicky Transient Facility (ZTF) data stream for candidate kilonovae in the form of rapidly evolving transients. We combined ZTF alert queries with forced point-spread-function photometry and nightly flux stacking to increase our sensitivity to faint and fast transients. Automatic queries yielded >11,200 candidates, 24 of which passed quality checks and selection criteria based on a grid of kilonova models tailored for both binary neutron star and neutron star–black hole mergers. None of the candidates in our sample was deemed a possible kilonova after thorough vetting. The sources that passed our selection criteria are dominated by Galactic cataclysmic variables. We identified two fast transients at high Galactic latitude, one of which is the confirmed afterglow of long-duration GRB 190106A, the other is a possible cosmological afterglow. Using a survey simulation code, we constrained the kilonova rate for a range of models including top-hat, linearly decaying light curves, and synthetic light curves obtained with radiative transfer simulations. For prototypical GW170817-like kilonovae, we constrain the rate to be R < 1775 Gpc⁻³ yr⁻¹ (95% confidence). By assuming a population of kilonovae with the same geometry and composition of GW170817 observed under a uniform viewing angle distribution, we obtained a constraint on the rate of R < 4029 Gpc⁻³ yr⁻¹
Constraining the Kilonova Rate with Zwicky Transient Facility Searches Independent of Gravitational Wave and Short Gamma-Ray Burst Triggers
The first binary neutron star merger, GW170817, was accompanied by a radioactivity-powered optical/infrared transient called a kilonova. To date, no compelling kilonova has been found in all-sky optical surveys, independently of short gamma-ray burst and gravitational-wave triggers. In this work, we searched the first 23 months of the Zwicky Transient Facility (ZTF) data stream for candidate kilonovae in the form of rapidly evolving transients. We combined ZTF alert queries with forced point-spread-function photometry and nightly flux stacking to increase our sensitivity to faint and fast transients. Automatic queries yielded >11,200 candidates, 24 of which passed quality checks and selection criteria based on a grid of kilonova models tailored for both binary neutron star and neutron star-black hole mergers. None of the candidates in our sample was deemed a possible kilonova after thorough vetting. The sources that passed our selection criteria are dominated by Galactic cataclysmic variables. We identified two fast transients at high Galactic latitude, one of which is the confirmed afterglow of long-duration GRB 190106A, the other is a possible cosmological afterglow. Using a survey simulation code, we constrained the kilonova rate for a range of models including top-hat, linearly decaying light curves, and synthetic light curves obtained with radiative transfer simulations. For prototypical GW170817-like kilonovae, we constrain the rate to be Gpc-3 yr-1 (95% confidence). By assuming a population of kilonovae with the same geometry and composition of GW170817 observed under a uniform viewing angle distribution, we obtained a constraint on the rate of R < 4029 Gpc-3 yr-1. © 2020. The American Astronomical Society