35 research outputs found
High Contrast L' Band Adaptive Optics Imaging to Detect Extrasolar Planets
We are carrying out a survey to search for giant extrasolar planets around
nearby, moderate-age stars in the mid-infrared L' and M bands (3.8 and 4.8
microns, respectively), using the Clio camera with the adaptive optics system
on the MMT telescope. To date we have observed 7 stars, of a total 50 planned,
including GJ 450 (distance about 8.55pc, age about 1 billion years, no real
companions detected), which we use as our example here. We report the methods
we use to obtain extremely high contrast imaging in L', and the performance we
have obtained. We find that the rotation of a celestial object over time with
respect to a telescope tracking it with an altazimuth mount can be a powerful
tool for subtracting telescope-related stellar halo artifacts and detecting
planets near bright stars. We have carried out a thorough Monte Carlo
simulation demonstrating our ability to detect planets as small as 6 Jupiter
masses around GJ 450. The division of a science data set into two independent
parts, with companions required to be detected on both in order to be
recognized as real, played a crucial role in detecting companions in this
simulation. We mention also our discovery of a previously unknown faint stellar
companion to another of our survey targets, HD 133002. Followup is needed to
confirm this as a physical companion, and to determine its physical properties.Comment: 8 pages, 4 figure
First On-Sky High Contrast Imaging with an Apodizing Phase Plate
We present the first astronomical observations obtained with an Apodizing
Phase Plate (APP). The plate is designed to suppress the stellar diffraction
pattern by 5 magnitudes from 2-9 lambda/D over a 180 degree region. Stellar
images were obtained in the M' band (4.85 microns) at the MMTO 6.5m telescope,
with adaptive wavefront correction made with a deformable secondary mirror
designed for low thermal background observations. The measured PSF shows a halo
intensity of 0.1% of the stellar peak at 2 lambda/D (0.36 arcsec), tapering off
as r^{-5/3} out to radius 9 lambda/D. Such a profile is consistent with
residual errors predicted for servo lag in the AO system.
We project a 5 sigma contrast limit, set by residual atmospheric
fluctuations, of 10.2 magnitudes at 0.36 arcsec separation for a one hour
exposure. This can be realised if static and quasi-static aberrations are
removed by differential imaging, and is close to the sensitivity level set by
thermal background photon noise for target stars with M'>3. The advantage of
using the phase plate is the removal of speckle noise caused by the residuals
in the diffraction pattern that remain after PSF subtraction. The APP gives
higher sensitivity over the range 2-5 lambda/D compared to direct imaging
techniques.Comment: 22 pages, 5 figures, 1 table, ApJ accepte
Constraints on the Progenitor of SN 2016gkg From Its Shock-Cooling Light Curve
SN 2016gkg is a nearby Type IIb supernova discovered shortly after explosion.
Like several other Type IIb events with early-time data, SN 2016gkg displays a
double-peaked light curve, with the first peak associated with the cooling of a
low-mass extended progenitor envelope. We present unprecedented
intranight-cadence multi-band photometric coverage of the first light-curve
peak of SN 2016gkg obtained from the Las Cumbres Observatory Global Telescope
network, the Asteroid Terrestrial-impact Last Alert System, the Swift satellite
and various amateur-operated telescopes. Fitting these data to analytical
shock-cooling models gives a progenitor radius of ~25-140 solar radii with
~2-30 x 10^-2 solar masses of material in the extended envelope (depending on
the model and the assumed host-galaxy extinction). Our radius estimates are
broadly consistent with values derived independently (in other works) from HST
imaging of the progenitor star. However, the shock-cooling model radii are on
the lower end of the values indicated by pre-explosion imaging. Hydrodynamical
simulations could refine the progenitor parameters deduced from the
shock-cooling emission and test the analytical models.Comment: Accepted by ApJ
Deep Drilling in the Time Domain with DECam: Survey Characterization
This paper presents a new optical imaging survey of four deep drilling fields
(DDFs), two Galactic and two extragalactic, with the Dark Energy Camera (DECam)
on the 4 meter Blanco telescope at the Cerro Tololo Inter-American Observatory
(CTIO). During the first year of observations in 2021, 4000 images covering
21 square degrees (7 DECam pointings), with 40 epochs (nights) per field
and 5 to 6 images per night per filter in , , , and/or , have
become publicly available (the proprietary period for this program is waived).
We describe the real-time difference-image pipeline and how alerts are
distributed to brokers via the same distribution system as the Zwicky Transient
Facility (ZTF). In this paper, we focus on the two extragalactic deep fields
(COSMOS and ELAIS-S1), characterizing the detected sources and demonstrating
that the survey design is effective for probing the discovery space of faint
and fast variable and transient sources. We describe and make publicly
available 4413 calibrated light curves based on difference-image detection
photometry of transients and variables in the extragalactic fields. We also
present preliminary scientific analysis regarding Solar System small bodies,
stellar flares and variables, Galactic anomaly detection, fast-rising
transients and variables, supernovae, and active galactic nuclei.Comment: 22 pages, 17 figures, 2 tables. Accepted to MNRA
SN 2017dio: A Type-Ic Supernova Exploding in a Hydrogen-rich Circumstellar Medium
SN 2017dio shows both spectral characteristics of a type-Ic supernova (SN) and signs of a hydrogen-rich circumstellar medium (CSM). Prominent, narrow emission lines of H and He are superposed on the continuum. Subsequent evolution revealed that the SN ejecta are interacting with the CSM. The initial SN Ic identification was confirmed by removing the CSM interaction component from the spectrum and comparing with known SNe Ic, and reversely, adding a CSM interaction component to the spectra of known SNe Ic and comparing them to SN 2017dio. Excellent agreement was obtained with both procedures, reinforcing the SN Ic classification. The light curve constrains the pre-interaction SN Ic peak absolute magnitude to be around Mg = −17.6 mag. No evidence of significant extinction is found, ruling out a brighter luminosity required by a SN Ia classification. These pieces of evidence support the view that SN 2017dio is a SN Ic, and therefore the first firm case of a SN Ic with signatures of hydrogen-rich CSM in the early spectrum. The CSM is unlikely to have been shaped by steady-state stellar winds. The mass loss of the progenitor star must have been intense, ˙M 0.02 (ǫH/0.01)−1 (vwind/500 km s−1) (vshock/10000 km s−1)−3 M⊙ yr−1, peaking at a few decades before the SN. Such a high mass loss rate might have been experienced by the progenitor through eruptions or binary stripping. Keywords: supernovae: general — supernovae: individual (SN 2017dio)</p
Diving below the spin-down limit:constraints on gravitational waves from the energetic young pulsar PSR J0537-6910
We present a search for continuous gravitational-wave signals from the young, energetic X-ray pulsar PSR J0537-6910 using data from the second and third observing runs of LIGO and Virgo. The search is enabled by a contemporaneous timing ephemeris obtained using NICER data. The NICER ephemeris has also been extended through 2020 October and includes three new glitches. PSR J0537-6910 has the largest spin-down luminosity of any pulsar and is highly active with regards to glitches. Analyses of its long-term and inter-glitch braking indices provided intriguing evidence that its spin-down energy budget may include gravitational-wave emission from a time-varying mass quadrupole moment. Its 62 Hz rotation frequency also puts its possible gravitational-wave emission in the most sensitive band of LIGO/Virgo detectors. Motivated by these considerations, we search for gravitational-wave emission at both once and twice the rotation frequency. We find no signal, however, and report our upper limits. Assuming a rigidly rotating triaxial star, our constraints reach below the gravitational-wave spin-down limit for this star for the first time by more than a factor of two and limit gravitational waves from the l = m = 2 mode to account for less than 14% of the spin-down energy budget. The fiducial equatorial ellipticity is limited to less than about 3 x 10⁻⁵, which is the third best constraint for any young pulsar
Search for anisotropic gravitational-wave backgrounds using data from Advanced LIGO and Advanced Virgo's first three observing runs
We report results from searches for anisotropic stochastic gravitational-wave
backgrounds using data from the first three observing runs of the Advanced LIGO
and Advanced Virgo detectors. For the first time, we include Virgo data in our
analysis and run our search with a new efficient pipeline called {\tt PyStoch}
on data folded over one sidereal day. We use gravitational-wave radiometry
(broadband and narrow band) to produce sky maps of stochastic
gravitational-wave backgrounds and to search for gravitational waves from point
sources. A spherical harmonic decomposition method is employed to look for
gravitational-wave emission from spatially-extended sources. Neither technique
found evidence of gravitational-wave signals. Hence we derive 95\%
confidence-level upper limit sky maps on the gravitational-wave energy flux
from broadband point sources, ranging from and on the
(normalized) gravitational-wave energy density spectrum from extended sources,
ranging from , depending on direction () and spectral index
(). These limits improve upon previous limits by factors of . We also set 95\% confidence level upper limits on the frequency-dependent
strain amplitudes of quasimonochromatic gravitational waves coming from three
interesting targets, Scorpius X-1, SN 1987A and the Galactic Center, with best
upper limits range from a factor of
improvement compared to previous stochastic radiometer searches.Comment: 23 Pages, 9 Figure
Search for continuous gravitational wave emission from the Milky Way center in O3 LIGO--Virgo data
We present a directed search for continuous gravitational wave (CW) signals
emitted by spinning neutron stars located in the inner parsecs of the Galactic
Center (GC). Compelling evidence for the presence of a numerous population of
neutron stars has been reported in the literature, turning this region into a
very interesting place to look for CWs. In this search, data from the full O3
LIGO--Virgo run in the detector frequency band have been
used. No significant detection was found and 95 confidence level upper
limits on the signal strain amplitude were computed, over the full search band,
with the deepest limit of about at .
These results are significantly more constraining than those reported in
previous searches. We use these limits to put constraints on the fiducial
neutron star ellipticity and r-mode amplitude. These limits can be also
translated into constraints in the black hole mass -- boson mass plane for a
hypothetical population of boson clouds around spinning black holes located in
the GC.Comment: 25 pages, 5 figure
Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO-Virgo Run O3a
We search for gravitational-wave transients associated with gamma-ray bursts
detected by the Fermi and Swift satellites during the first part of the third
observing run of Advanced LIGO and Advanced Virgo (1 April 2019 15:00 UTC - 1
October 2019 15:00 UTC). 105 gamma-ray bursts were analyzed using a search for
generic gravitational-wave transients; 32 gamma-ray bursts were analyzed with a
search that specifically targets neutron star binary mergers as short gamma-ray
burst progenitors. We describe a method to calculate the probability that
triggers from the binary merger targeted search are astrophysical and apply
that method to the most significant gamma-ray bursts in that search. We find no
significant evidence for gravitational-wave signals associated with the
gamma-ray bursts that we followed up, nor for a population of unidentified
subthreshold signals. We consider several source types and signal morphologies,
and report for these lower bounds on the distance to each gamma-ray burst
All-sky search for continuous gravitational waves from isolated neutron stars in the early O3 LIGO data
We report on an all-sky search for continuous gravitational waves in the frequency band 20-2000 Hz and with a frequency time derivative in the range of [-1.0; +0.1] x 10(-8) Hz/s. Such a signal could be produced by a nearby, spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the LIGO data from the first six months of Advanced LIGO's and Advanced Virgo's third observational run, O3. No periodic gravitational wave signals are observed, and 95% confidence-level (C.L.) frequentist upper limits are placed on their strengths. The lowest upper limits on worst-case (linearly polarized) strain amplitude h(0) are similar to 1.7 x 10(-25) near 200 Hz. For a circularly polarized source (most favorable orientation), the lowest upper limits are similar to 6.3 x 10(-26). These strict frequentist upper limits refer to all sky locations and the entire range of frequency derivative values. For a populationaveraged ensemble of sky locations and stellar orientations, the lowest 95% C.L. upper limits on the strain amplitude are similar to 1.4 x 10(-25). These upper limits improve upon our previously published all-sky results, with the greatest improvement (factor of similar to 2) seen at higher frequencies, in part because quantum squeezing has dramatically improved the detector noise level relative to the second observational run, O2. These limits are the most constraining to date over most of the parameter space searched