225 research outputs found
Keck and Gemini spectral characterization of Lucy mission fly-by target (152830) Dinkinesh
Recently, the inner main belt asteroid (152830) Dinkinesh was identified as
an additional fly-by target for the Lucy mission. The heliocentric orbit and
approximate absolute magnitude of Dinkinesh are known, but little additional
information was available prior to its selection as a target. In particular,
the lack of color spectrophotometry or spectra made it impossible to assign a
spectral type to Dinkinesh from which its albedo could be estimated. We set out
to remedy this knowledge gap by obtaining visible wavelength spectra with the
Keck telescope on 2022 November 23 and with Gemini-South on 2022 December 27.
The spectra measured with the Keck I/Low Resolution Imaging Spectrometer (LRIS)
and the Gemini South/Gemini Multi-Object Spectrograph South (GMOS-S) are most
similar to the average spectrum of S- and Sq-type asteroids. The most
diagnostic feature is the 151 silicate absorption feature at
0.9-1.0~micron. Small S- and Sq-type asteroids have moderately high
albedos ranging from 0.17-0.35. Using this albedo range for Dinkinesh in
combination with measured absolute magnitude, it is possible to derive an
effective diameter and surface brightness for this body. The albedo, size and
surface brightness are important inputs required for planning a successful
encounter by the Lucy spacecraft.Comment: 7 pages, 1 figure. Under review in Icaru
Modeling the Expected Performance of the REgolith X-ray Imaging Spectrometer (REXIS)
OSIRIS-REx is the third spacecraft in the NASA New Frontiers Program and is
planned for launch in 2016. OSIRIS-REx will orbit the near-Earth asteroid
(101955) Bennu, characterize it, and return a sample of the asteroid's regolith
back to Earth. The Regolith X-ray Imaging Spectrometer (REXIS) is an instrument
on OSIRIS-REx designed and built by students at MIT and Harvard. The purpose of
REXIS is to collect and image sun-induced fluorescent X-rays emitted by Bennu,
thereby providing spectroscopic information related to the elemental makeup of
the asteroid regolith and the distribution of features over its surface.
Telescopic reflectance spectra suggest a CI or CM chondrite analog meteorite
class for Bennu, where this primitive nature strongly motivates its study. A
number of factors, however, will influence the generation, measurement, and
interpretation of the X-ray spectra measured by REXIS. These include: the
compositional nature and heterogeneity of Bennu, the time-variable Solar state,
X-ray detector characteristics, and geometric parameters for the observations.
In this paper, we will explore how these variables influence the precision to
which REXIS can measure Bennu's surface composition. By modeling the
aforementioned factors, we place bounds on the expected performance of REXIS
and its ability to ultimately place Bennu in an analog meteorite class.Comment: Presented at the SPIE Optics + Photonics Conference, 18 August 2014,
San Diego, C
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Marco Polo: near Earth object sample return mission
Marco Polo is a joint European-Japanese mission of sample return from a Near Earth Object. The Marco Polo proposal was submitted to ESA on July 2007 in the framework of the Cosmic Vision 2015-2025 context, and on October 2007 passed the first evaluation process. The primary objectives of this mission is to visit a primitive NEO, belonging to a class that cannot be related to known meteorite types, to characterize it at multiple scales, and to bring samples back to Earth. Marco Polo will give us the first opportunity for detailed laboratory study of the most primitive materials that formed the planets. This will allow us to improve our knowledge on the processes which governed the origin and early evolution of the Solar System, and possibly of the life on Earth
Albedos and diameters of three Mars Trojan asteroids
We observed the Mars Trojan asteroids (5261) Eureka and (101429) 1998 VF31
and the candidate Mars Trojan 2001 FR127 at 11.2 and 18.1 microns using
Michelle on the Gemini North telescope. We derive diameters of 1.28, 0.78, and
<0.52 km, respectively, with corresponding geometric visible albedos of 0.39,
0.32, and >0.14. The albedos for Eureka and 1998 VF31 are consistent with the
taxonomic classes and compositions (S(I)/angritic and S(VII)/achrondritic,
respectively) and implied histories presented in a companion paper by Rivkin et
al. Eureka's surface likely has a relatively high thermal inertia, implying a
thin regolith that is consistent with predictions and the small size that we
derive.Comment: Icarus, in press. See companion paper 0709.1925 by Rivkin et al; two
minor typos fixe
Pluto's global surface composition through pixel-by-pixel Hapke modeling of New Horizons Ralph/LEISA data
On July 14th 2015, NASA's New Horizons mission gave us an unprecedented
detailed view of the Pluto system. The complex compositional diversity of
Pluto's encounter hemisphere was revealed by the Ralph/LEISA infrared
spectrometer on board of New Horizons. We present compositional maps of Pluto
defining the spatial distribution of the abundance and textural properties of
the volatiles methane and nitrogen ices and non-volatiles water ice and tholin.
These results are obtained by applying a pixel-by-pixel Hapke radiative
transfer model to the LEISA scans. Our analysis focuses mainly on the large
scale latitudinal variations of methane and nitrogen ices and aims at setting
observational constraints to volatile transport models. Specifically, we find
three latitudinal bands: the first, enriched in methane, extends from the pole
to 55deg N, the second dominated by nitrogen, continues south to 35deg N, and
the third, composed again mainly of methane, reaches 20deg N. We demonstrate
that the distribution of volatiles across these surface units can be explained
by differences in insolation over the past few decades. The latitudinal pattern
is broken by Sputnik Planitia, a large reservoir of volatiles, with nitrogen
playing the most important role. The physical properties of methane and
nitrogen in this region are suggestive of the presence of a cold trap or
possible volatile stratification. Furthermore our modeling results point to a
possible sublimation transport of nitrogen from the northwest edge of Sputnik
Planitia toward the south.Comment: 43 pages, 7 figures; accepted for publication in Icaru
Characterization of the near-Earth Asteroid 2002NY40
In August 2002, the near-Earth asteroid 2002 NY40, made its closest approach
to the Earth. This provided an opportunity to study a near-Earth asteroid with
a variety of instruments. Several of the telescopes at the Maui Space
Surveillance System were trained at the asteroid and collected adaptive optics
images, photometry and spectroscopy. Analysis of the imagery reveals the
asteroid is triangular shaped with significant self-shadowing. The photometry
reveals a 20-hour period and the spectroscopy shows that the asteroid is a
Q-type
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Early Observations And Analysis Of The Type Ia SN 2014J In M82
We present optical and near infrared (NIR) observations of the nearby Type Ia SN 2014J. Seventeen optical and 23 NIR spectra were obtained from 10 days before (-10d) to 10 days after (+10d) the time of maximum B-band brightness. The relative strengths of absorption features and their patterns of development can be compared at one day intervals throughout most of this period. Carbon is not detected in the optical spectra, but we identify C I lambda 1.0693 in the NIR spectra. Mg II lines with high oscillator strengths have higher initial velocities than other Mg II lines. We show that the velocity differences can be explained by differences in optical depths due to oscillator strengths. The spectra of SN 2014J show that it is a normal SN Ia, but many parameters are near the boundaries between normal and high-velocity subclasses. The velocities for OI, Mg II, Si II, S Ca a, and Fell suggest that SN 2014J has a layered structure with little or no mixing. That result is consistent with the delayed detonation explosion models. We also report photometric observations, obtained from -10d to +29d, in the UBVRIJH and K-s bands. The template fitting package SNooPy is used to interpret the light curves and to derive photometric parameters. Using R-v = 1.46, which is consistent with previous studies, SNooPy finds that A(v) = 1.80 for E(B - V)(host) = 1.23 +/- 0.06 mag. The maximum B-band brightness of -19.19 +/- 0.10 mag was reached on February 1.74 UT +/- 0.13 days and the supernova has a decline parameter, Delta m(15), of 1.12 +/- 0.02 mag.Department of Space, Government of IndiaHungarian OTKA NN-107637NSF AST-1109801, AST-1151462, AST-1211196NSF Astronomy and Astrophysics Postdoctoral Fellowship AST-1302771NASA through a grant from the Space Telescope Science Institute GO-12540NASA NAS5-26555Swedish Research CouncilSwedish National Space BoardDanish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grantAstronom
Early Observations and Analysis of the Type Ia SN 2014J in M82
We present optical and near infrared (NIR) observations of the nearby Type Ia
SN 2014J. Seventeen optical and twenty-three NIR spectra were obtained from 10
days before (10d) to 10 days after (+10d) the time of maximum -band
brightness. The relative strengths of absorption features and their patterns of
development can be compared at one day intervals throughout most of this
period. Carbon is not detected in the optical spectra, but we identify CI
1.0693 in the NIR spectra. We find that MgII lines with high
oscillator strengths have higher initial velocities than other MgII lines. We
show that the velocity differences can be explained by differences in optical
depths due to oscillator strengths. The spectra of SN 2014J show it is a normal
SN Ia, but many parameters are near the boundaries between normal and
high-velocity subclasses. The velocities for OI, MgII, SiII, SII, CaII and FeII
suggest that SN 2014J has a layered structure with little or no mixing. That
result is consistent with the delayed detonation explosion models. We also
report photometric observations, obtained from 10d to +29d, in the
and bands. SN 2014J is about 3 magnitudes fainter than a normal SN Ia at
the distance of M82, which we attribute to extinction in the host. The template
fitting package SNooPy is used to interpret the light curves and to derive
photometric parameters. Using = 1.46, which is consistent with previous
studies, SNooPy finds that for mag.
The maximum -band brightness of mag was reached on
February 1.74 UT days and the supernova had a decline parameter of
mag.Comment: 6 figures, 6 tables, submitted to the Ap
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