67 research outputs found
Interferometric Observations of Explosive Variables: V838 Mon, Nova Aql 2005, and RS Oph
During the last two years we have used the Palomar Testbed Interferometer to
observe several explosive variable stars, including V838 Monocerotis, V1663
Aquilae and recently RS Ophiuchi. We observed V838 Monocerotis approximately 34
months after its eruption, and were able to resolve the ejecta. Observations of
V1663 Aql were obtained starting 9 days after peak brightness and continued for
10 days. We were able to resolve the milliarcsecond-scale emission and follow
the expansion of the nova photosphere. When combined with radial-velocity
information, these observations can be used to infer the distance to the nova.
Finally we have resolved the recurrent nova RS Oph and can draw some
preliminary conclusions regarding the emission morphology.Comment: 8 Pages, SPIE Astronomical Telescopes and Instrumentation 2006,
Advances in Stellar Interferometery, 6268-16
The Wide Integral Field Infrared Spectrograph: Commissioning Results and On-sky Performance
We have recently commissioned a novel infrared ( m) integral
field spectrograph (IFS) called the Wide Integral Field Infrared Spectrograph
(WIFIS). WIFIS is a unique instrument that offers a very large field-of-view
(50 x 20) on the 2.3-meter Bok telescope at
Kitt Peak, USA for seeing-limited observations at moderate spectral resolving
power. The measured spatial sampling scale is and
its spectral resolving power is and in the
( m) and ( m) modes, respectively.
WIFIS's corresponding etendue is larger than existing near-infrared (NIR)
IFSes, which are mostly designed to work with adaptive optics systems and
therefore have very narrow fields. For this reason, this instrument is
specifically suited for studying very extended objects in the near-infrared
such as supernovae remnants, galactic star forming regions, and nearby
galaxies, which are not easily accessible by other NIR IFSes. This enables
scientific programs that were not originally possible, such as detailed surveys
of a large number of nearby galaxies or a full accounting of nucleosynthetic
yields of Milky Way supernova remnants. WIFIS is also designed to be easily
adaptable to be used with larger telescopes. In this paper, we report on the
overall performance characteristics of the instrument, which were measured
during our commissioning runs in the second half of 2017. We present
measurements of spectral resolving power, image quality, instrumental
background, and overall efficiency and sensitivity of WIFIS and compare them
with our design expectations. Finally, we present a few example observations
that demonstrate WIFIS's full capability to carry out infrared imaging
spectroscopy of extended objects, which is enabled by our custom data reduction
pipeline.Comment: Published in the Proceedings of SPIE Astronomical Telescopes and
Instrumentation 2018. 17 pages, 13 figure
Adaptive Optics Imaging of the AU Microscopii Circumstellar Disk: Evidence for Dynamical Evolution
We present an H-band image of the light scattered from circumstellar dust
around the nearby (10 pc) young M star AU Microscopii (AU Mic, GJ 803, HD
197481), obtained with the Keck adaptive optics system. We resolve the disk
both vertically and radially, tracing it over 17-60 AU from the star. Our AU
Mic observations thus offer the possibility to probe at high spatial resolution
(0.04" or 0.4 AU per resolution element) for morphological signatures of the
debris disk on Solar-System scales. Various sub-structures (dust clumps and
gaps) in the AU Mic disk may point to the existence of orbiting planets. No
planets are seen in our H-band image down to a limiting mass of 1 M_Jup at >20
AU, although the existence of smaller planets can not be excluded from the
current data. Modeling of the disk surface brightness distribution at H-band
and R-band, in conjunction with the optical to sub-millimeter spectral energy
distribution, allows us to constrain the disk geometry and the dust grain
properties. We confirm the nearly edge-on orientation of the disk inferred from
previous observations, and deduce an inner clearing radius <=10 AU. We find
evidence for a lack of small grains in the inner (<60 AU) disk, either as a
result of primordial disk evolution, or because of destruction by
Poynting-Robertson and/or corpuscular drag. A change in the power-law index of
the surface brightness profile is observed near 33 AU, similar to a feature
known in the profile of the beta Pic circumstellar debris disk. By comparing
the time scales for inter-particle collisions and Poynting-Robertson drag
between the two systems, we argue that the breaks are linked to one of these
two processes.Comment: 17 pages, 7 figures, 1 table; accepted by Ap
ALMA Discovery of a Disk around the Planetary-Mass Companion Sr 12 C
We report an Atacama Large Millimeter/submillimeter Array 0.88 mm (Band 7) continuum detection of the accretion disk around SR 12 c, an ∼11 M Jup planetary-mass companion (PMC) orbiting its host binary at 980 au. This is the first submillimeter detection of a circumplanetary disk around a wide PMC. The disk has a flux density of 127 ± 14 μJy and is not resolved by the ∼0.″1 beam, so the dust disk radius is likely less than 5 au and can be much smaller if the dust continuum is optically thick. If, however, the dust emission is optically thin, then the SR 12 c disk has a comparable dust mass to the circumplanetary disk around PDS 70 c but is about five times lower than that of the ∼12 M Jup free-floating OTS 44. This suggests that disks around bound and unbound planetary-mass objects can span a wide range of masses. The gas mass estimated with an accretion rate of 10-11 M ⊙ yr-1 implies a gas-to-dust ratio higher than 100. If cloud absorption is not significant, a nondetection of 12CO(3-2) implies a compact gas disk around SR 12 c. Future sensitive observations may detect more PMC disks at 0.88 mm flux densities of ≲ 100 μJy
Reflected Light from Sand Grains in the Terrestrial Zone of a Protoplanetary Disk
We show that grains have grown to ~mm size (sand sized) or larger in the
terrestrial zone (within ~3 AU) of the protoplanetary disk surrounding the 3
Myr old binary star KH 15D. We also argue that the reflected light in the
system reaches us by back scattering off the far side of the same ring whose
near side causes the obscuration.Comment: 22 pages, 5 figures. To be published in Nature, March 13, 2008.
Contains a Supplemen
Dusty disk winds at the sublimation rim of the highly inclined, low mass YSO SU Aurigae
T Tauri stars are low-mass young stars whose disks provide the setting for
planet formation. Despite this, their structure is poorly understood. We
present new infrared interferometric observations of the SU Aurigae
circumstellar environment that offer 3 x higher resolution and better baseline
position angle coverage over previous observations. We investigate the
characteristics of circumstellar material around SU Aur, constrain the disk
geometry, composition and inner dust rim structure. The CHARA array offers
opportunities for long baseline observations, with baselines up to 331 m. Using
the CLIMB 3-telescope combiner in the K-band allows us to measure visibilities
as well as closure phase. We undertook image reconstruction for
model-independent analysis, and geometric modeling. Additionally, the fitting
of radiative transfer models constrains the physical parameters of the disk.
For the first time, a dusty disk wind is introduced to the radiative transfer
code TORUS to model protoplanetary disks. Our implementation is motivated by
theoretical dusty disk winds, where magnetic field lines drive dust above the
disk plane close to the sublimation zone. Image reconstruction reveals an
inclined disk with slight asymmetry along its minor-axis, likely due to
inclination effects obscuring the inner disk rim through absorption of incident
star light on the near-side and thermal re-emission/scattering of the far-side.
Geometric modelling of a skewed ring finds the inner rim at 0.17+/-0.02 au with
an inclination of 50.9+/-1.0 degrees and minor axis position angle 60.8+/-1.2
degrees. Radiative transfer modelling shows a flared disk with an inner radius
at 0.18 au which implies a grain size of 0.4 um and a scale height of 15.0 au
at 100 au. Among the tested radiative transfer models, only the dusty disk wind
successfully accounts for the K-band excess by introducing dust above the
mid-plane.Comment: Accepted for publication in Astronomy \& Astrophysic
High contrast imaging at the LBT: the LEECH exoplanet imaging survey
In Spring 2013, the LEECH (LBTI Exozodi Exoplanet Common Hunt) survey began
its 130-night campaign from the Large Binocular Telescope (LBT) atop Mt
Graham, Arizona. This survey benefits from the many technological achievements
of the LBT, including two 8.4-meter mirrors on a single fixed mount, dual
adaptive secondary mirrors for high Strehl performance, and a cold beam
combiner to dramatically reduce the telescope's overall background emissivity.
LEECH neatly complements other high-contrast planet imaging efforts by
observing stars at L' (3.8 m), as opposed to the shorter wavelength
near-infrared bands (1-2.4 m) of other surveys. This portion of the
spectrum offers deep mass sensitivity, especially around nearby adolescent
(0.1-1 Gyr) stars. LEECH's contrast is competitive with other extreme
adaptive optics systems, while providing an alternative survey strategy.
Additionally, LEECH is characterizing known exoplanetary systems with
observations from 3-5m in preparation for JWST.Comment: 12 pages, 5 figures. Proceedings of the SPIE, 9148-2
The LEECH Exoplanet Imaging Survey: Limits on Planet Occurrence Rates Under Conservative Assumptions
We present the results of the largest (m) direct
imaging survey for exoplanets to date, the Large Binocular Telescope
Interferometer (LBTI) Exozodi Exoplanet Common Hunt (LEECH). We observed 98
stars with spectral types from B to M. Cool planets emit a larger share of
their flux in compared to shorter wavelengths, affording LEECH an
advantage in detecting low-mass, old, and cold-start giant planets. We
emphasize proximity over youth in our target selection, probing physical
separations smaller than other direct imaging surveys. For FGK stars, LEECH
outperforms many previous studies, placing tighter constraints on the hot-start
planet occurrence frequency interior to au. For less luminous,
cold-start planets, LEECH provides the best constraints on giant-planet
frequency interior to au around FGK stars. Direct imaging survey
results depend sensitively on both the choice of evolutionary model (e.g., hot-
or cold-start) and assumptions (explicit or implicit) about the shape of the
underlying planet distribution, in particular its radial extent. Artificially
low limits on the planet occurrence frequency can be derived when the shape of
the planet distribution is assumed to extend to very large separations, well
beyond typical protoplanetary dust-disk radii ( au), and when
hot-start models are used exclusively. We place a conservative upper limit on
the planet occurrence frequency using cold-start models and planetary
population distributions that do not extend beyond typical protoplanetary
dust-disk radii. We find that of FGK systems can host a 7 to 10
planet from 5 to 50 au. This limit leaves open the
possibility that planets in this range are common.Comment: 31 pages, 13 figures, accepted to A
First Light LBT AO Images of HR 8799 bcde at 1.65 and 3.3 Microns: New Discrepancies between Young Planets and Old Brown Dwarfs
As the only directly imaged multiple planet system, HR 8799 provides a unique
opportunity to study the physical properties of several planets in parallel. In
this paper, we image all four of the HR 8799 planets at H-band and 3.3 microns
with the new LBT adaptive optics system, PISCES, and LBTI/LMIRCam. Our images
offer an unprecedented view of the system, allowing us to obtain H and 3.3$
micron photometry of the innermost planet (for the first time) and put strong
upper-limits on the presence of a hypothetical fifth companion. We find that
all four planets are unexpectedly bright at 3.3 microns compared to the
equilibrium chemistry models used for field brown dwarfs, which predict that
planets should be faint at 3.3 microns due to CH4 opacity. We attempt to model
the planets with thick-cloudy, non-equilibrium chemistry atmospheres, but find
that removing CH4 to fit the 3.3 micron photometry increases the predicted L'
(3.8 microns) flux enough that it is inconsistent with observations. In an
effort to fit the SED of the HR 8799 planets, we construct mixtures of cloudy
atmospheres, which are intended to represent planets covered by clouds of
varying opacity. In this scenario, regions with low opacity look hot and
bright, while regions with high opacity look faint, similar to the patchy cloud
structures on Jupiter and L/T transition brown-dwarfs. Our mixed cloud models
reproduce all of the available data, but self-consistent models are still
necessary to demonstrate their viability.Comment: Accepted to Ap
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