127 research outputs found
Constraining multiple systems with GAIA
GAIA will provide observations of some multiple asteroid and dwarf systems.
These observations are a way to determine and improve the quantification of
dynamical parameters, such as the masses and the gravity fields, in these
multiple systems. Here we investigate this problem in the cases of Pluto's and
Eugenia's system. We simulate observations reproducing an approximate planning
of the GAIA observations for both systems, as well as the New Horizons
observations of Pluto. We have developed a numerical model reproducing the
specific behavior of multiple asteroid system around the Sun and fit it to the
simulated observations using least-square method, giving the uncertainties on
the fitted parameters. We found that GAIA will improve significantly the
precision of Pluto's and Charon's mass, as well as Petit Prince's orbital
elements and Eugenia's polar oblateness.Comment: 5 pages, accepted by Planetary and Space Science, Gaia GREAT-SSO-Pis
The Resolved Asteroid Program - Size, shape, and pole of (52) Europa
With the adaptive optics (AO) system on the 10 m Keck-II telescope, we
acquired a high quality set of 84 images at 14 epochs of asteroid (52) Europa
on 2005 January 20. The epochs covered its rotation period and, by following
its changing shape and orientation on the plane of sky, we obtained its
triaxial ellipsoid dimensions and spin pole location. An independent
determination from images at three epochs obtained in 2007 is in good agreement
with these results. By combining these two data sets, along with a single epoch
data set obtained in 2003, we have derived a global fit for (52) Europa of
diameters (379x330x249) +/- (16x8x10) km, yielding a volume-equivalent
spherical-diameter of 315 +/- 7 km, and a rotational pole within 7 deg of [RA;
Dec] = [257,+12] in an Equatorial J2000 reference frame (ECJ2000: 255,+35).
Using the average of all mass determinations available forEuropa, we derive a
density of 1.5 +/- 0.4, typical of C-type asteroids. Comparing our images with
the shape model of Michalowski et al. (A&A 416, 2004), derived from optical
lightcurves, illustrates excellent agreement, although several edge features
visible in the images are not rendered by the model. We therefore derived a
complete 3-D description of Europa's shape using the KOALA algorithm by
combining our imaging epochs with 4 stellar occultations and 49 lightcurves. We
use this 3-D shape model to assess these departures from ellipsoidal shape.
Flat facets (possible giant craters) appear to be less distinct on (52) Europa
than on other C-types that have been imaged in detail. We show that fewer giant
craters, or smaller craters, is consistent with its expected impact history.
Overall, asteroid (52) Europa is still well modeled as a smooth triaxial
ellipsoid with dimensions constrained by observations obtained over several
apparitions.Comment: Accepted for publication in Icaru
Physical Properties of (2) Pallas
We acquired and analyzed adaptive-optics imaging observations of asteroid (2)
Pallas from Keck II and the Very Large Telescope taken during four Pallas
oppositions between 2003 and 2007, with spatial resolution spanning 32-88 km
(image scales 13-20 km/pix). We improve our determination of the size, shape,
and pole by a novel method that combines our AO data with 51 visual
light-curves spanning 34 years of observations as well as occultation data.
The shape model of Pallas derived here reproduces well both the projected
shape of Pallas on the sky and light-curve behavior at all the epochs
considered. We resolved the pole ambiguity and found the spin-vector
coordinates to be within 5 deg. of [long, lat] = [30 deg., -16 deg.] in the
ECJ2000.0 reference frame, indicating a high obliquity of ~84 deg., leading to
high seasonal contrast. The best triaxial-ellipsoid fit returns radii of a=275
km, b= 258 km, and c= 238 km. From the mass of Pallas determined by
gravitational perturbation on other minor bodies [(1.2 +/- 0.3) x 10-10 Solar
Masses], we derive a density of 3.4 +/- 0.9 g.cm-3 significantly different from
the density of C-type (1) Ceres of 2.2 +/- 0.1 g.cm-3. Considering the spectral
similarities of Pallas and Ceres at visible and near-infrared wavelengths, this
may point to fundamental differences in the interior composition or structure
of these two bodies.
We define a planetocentric longitude system for Pallas, following IAU
guidelines. We also present the first albedo maps of Pallas covering ~80% of
the surface in K-band. These maps reveal features with diameters in the 70-180
km range and an albedo contrast of about 6% wrt the mean surface albedo.Comment: 16 pages, 8 figures, 6 table
Ultraviolet and visible photometry of asteroid (21) Lutetia using the Hubble Space Telescope
The asteroid (21) Lutetia is the target of a planned close encounter by the
Rosetta spacecraft in July 2010. To prepare for that flyby, Lutetia has been
extensively observed by a variety of astronomical facilities. We used the
Hubble Space Telescope (HST) to determine the albedo of Lutetia over a wide
wavelength range, extending from ~150 nm to ~700 nm. Using data from a variety
of HST filters and a ground-based visible light spectrum, we employed synthetic
photometry techniques to derive absolute fluxes for Lutetia. New results from
ground-based measurements of Lutetia's size and shape were used to convert the
absolute fluxes into albedos. We present our best model for the spectral energy
distribution of Lutetia over the wavelength range 120-800 nm. There appears to
be a steep drop in the albedo (by a factor of ~2) for wavelengths shorter than
~300 nm. Nevertheless, the far ultraviolet albedo of Lutetia (~10%) is
considerably larger than that of typical C-chondrite material (~4%). The
geometric albedo at 550 nm is 16.5 +/- 1%. Lutetia's reflectivity is not
consistent with a metal-dominated surface at infrared or radar wavelengths, and
its albedo at all wavelengths (UV-visibile-IR-radar) is larger than observed
for typical primitive, chondritic material. We derive a relatively high FUV
albedo of ~10%, a result that will be tested by observations with the Alice
spectrograph during the Rosetta flyby of Lutetia in July 2010.Comment: 14 pages, 2 tables, 8 figure
Adaptive Optics for Astronomy
Adaptive Optics is a prime example of how progress in observational astronomy
can be driven by technological developments. At many observatories it is now
considered to be part of a standard instrumentation suite, enabling
ground-based telescopes to reach the diffraction limit and thus providing
spatial resolution superior to that achievable from space with current or
planned satellites. In this review we consider adaptive optics from the
astrophysical perspective. We show that adaptive optics has led to important
advances in our understanding of a multitude of astrophysical processes, and
describe how the requirements from science applications are now driving the
development of the next generation of novel adaptive optics techniques.Comment: to appear in ARA&A vol 50, 201
Analyses showing how religiosity, social activities, and drug-related beliefs mediate relationships between post-high school experiences and substance use
https://deepblue.lib.umich.edu/bitstream/2027.42/137877/1/occ50.pd
A low density of 0.8 g/cc for the Trojan binary asteroid 617 Patroclus
The Trojan population consists of two swarms of asteroids following the same
orbit as Jupiter and located at the L4 and L5 Lagrange points of the
Jupiter-Sun system (leading and following Jupiter by 60 degrees). The asteroid
617 Patroclus is the only known binary Trojan (Merline et al. 2001). The orbit
of this double system was hitherto unknown. Here we report that the components,
separated by 680 km, move around the system centre of mass, describing roughly
a circular orbit. Using the orbital parameters, combined with thermal
measurements to estimate the size of the components, we derive a very low
density of 0.8 g/cc. The components of Patroclus are therefore very porous or
composed mostly of water ice, suggesting that they could have been formed in
the outer part of the solar system.Comment: 10 pages, 3 figures, 1 tabl
Near-Infrared Spectroscopy of Trojan Asteroids: Evidence for Two Compositional Groups
The Trojan asteroids remain quite poorly understood, yet their physical
properties provide unique perspective on chemical and dynamical processes that
shaped the Solar System. The current study was undertaken to investigate
surface compositions of these objects. We present 66 new near-infrared (NIR;
0.7 to 2.5 microns) spectra of 58 Trojans, including members of both the
leading and trailing swarms. We also include in the analysis previously
published NIR spectra of 13 Trojans (3 of which overlap with the new sample).
This data set permits not only a direct search for compositional signatures,
but also a search for patterns that may reveal clues to the origin of the
Trojans. We do not report any confirmed absorption features in the new spectra.
Analysis of the spectral slopes, however, reveals an interesting bimodality
among the NIR data. The two spectral groups identified appear to be equally
abundant in the leading and trailing swarms. The spectral groups are not a
result of family membership; they occur in the background, non-family
population. The average albedos of the two groups are the same within
uncertainties (0.051\pm0.016 and 0.055\pm0.016). No correlations between
spectral slope and any other physical or orbital parameter are detected, with
the exception of a possible weak correlation with inclination among the
less-red spectral group. Synthesizing these results with previously published
properties, we conclude that the two spectral groups represent objects with
different intrinsic compositions. We further suggest that while the less-red
group originated near Jupiter or in the main asteroid belt, the redder spectral
group originated farther out in the Solar System. If correct, the Trojan swarms
offer the most readily accessible large reservoir of Kuiper Belt material as
well as a unique reservoir for the study of material from the middle part of
the solar nebula.Comment: Astronomical Journal, in press 38 manuscript pages 3 tables 7 Figures
(color online, B&W for print) 1 appendi
Near-Infrared Mapping and Physical Properties of the Dwarf-Planet Ceres
We study the physical characteristics (shape, dimensions, spin axis
direction, albedo maps, mineralogy) of the dwarf-planet Ceres based on
high-angular resolution near-infrared observations. We analyze adaptive optics
J/H/K imaging observations of Ceres performed at Keck II Observatory in
September 2002 with an equivalent spatial resolution of ~50 km. The spectral
behavior of the main geological features present on Ceres is compared with
laboratory samples. Ceres' shape can be described by an oblate spheroid (a = b
= 479.7 +/- 2.3 km, c = 444.4 +/- 2.1 km) with EQJ2000.0 spin vector
coordinates RA = 288 +/- 5 deg. and DEC = +66 +/- 5 deg. Ceres sidereal period
is measured to be 9.0741 +/- 0.0001 h. We image surface features with diameters
in the 50-180 km range and an albedo contrast of ~6% with respect to the
average Ceres albedo. The spectral behavior of the brightest regions on Ceres
is consistent with phyllosilicates and carbonate compounds. Darker isolated
regions could be related to the presence of frost.Comment: 11 pages, 8 Postscript figures, Accepted for publication in A&
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