120 research outputs found
TRIPPy: Trailed Image Photometry in Python
Photometry of moving sources typically suffers from reduced signal-to-noise
(SNR) or flux measurements biased to incorrect low values through the use of
circular apertures. To address this issue we present the software package,
TRIPPy: TRailed Image Photometry in Python. TRIPPy introduces the pill
aperture, which is the natural extension of the circular aperture appropriate
for linearly trailed sources. The pill shape is a rectangle with two
semicircular end-caps, and is described by three parameters, the trail length
and angle, and the radius. The TRIPPy software package also includes a new
technique to generate accurate model point-spread functions (PSF) and trailed
point-spread functions (TSF) from stationary background sources in sidereally
tracked images. The TSF is merely the convolution of the model PSF, which
consists of a moffat profile, and super sampled lookup table. From the TSF,
accurate pill aperture corrections can be estimated as a function of pill
radius with a accuracy of 10 millimags for highly trailed sources. Analogous to
the use of small circular apertures and associated aperture corrections, small
radius pill apertures can be used to preserve signal-to-noise of low flux
sources, with appropriate aperture correction applied to provide an accurate,
unbiased flux measurement at all SNR.Comment: 8 Figures, 11 Pages, Accepted to the Astronomical Journa
Col-OSSOS: Colors of the Interstellar Planetesimal 1I/`Oumuamua
The recent discovery by Pan-STARRS1 of 1I/2017 U1 (`Oumuamua), on an unbound
and hyperbolic orbit, offers a rare opportunity to explore the planetary
formation processes of other stars, and the effect of the interstellar
environment on a planetesimal surface. 1I/`Oumuamua's close encounter with the
inner Solar System in 2017 October was a unique chance to make observations
matching those used to characterize the small-body populations of our own Solar
System. We present near-simultaneous g, r, and J photometry
and colors of 1I/`Oumuamua from the 8.1-m Frederick C. Gillett Gemini North
Telescope, and photometry from the 4.2 m William Herschel Telescope. Our
grJ observations are directly comparable to those from the
high-precision Colours of the Outer Solar System Origins Survey (Col-OSSOS),
which offer unique diagnostic information for distinguishing between outer
Solar System surfaces. The J-band data also provide the highest signal-to-noise
measurements made of 1I/`Oumuamua in the near-infrared. Substantial, correlated
near-infrared and optical variability is present, with the same trend in both
near-infrared and optical. Our observations are consistent with 1I/`Oumuamua
rotating with a double-peaked period of hours and being a
highly elongated body with an axial ratio of at least 5.3:1, implying that it
has significant internal cohesion. The color of the first interstellar
planetesimal is at the neutral end of the range of Solar System and
solar-reflectance colors: it is like that of some dynamically excited objects
in the Kuiper belt and the less-red Jupiter Trojans.Comment: Accepted to ApJ
Col-OSSOS: The Colours of the Outer Solar System Origins Survey
The Colours of the Outer Solar System Origins Survey (Col-OSSOS) is acquiring
near-simultaneous , , and photometry of unprecedented precision with
the Gemini North Telescope, targeting nearly a hundred trans-Neptunian objects
(TNOs) brighter than mag discovered in the Outer Solar System
Origins Survey. Combining the optical and near-infrared photometry with the
well-characterized detection efficiency of the Col-OSSOS target sample will
provide the first flux-limited compositional dynamical map of the outer Solar
System. In this paper, we describe our observing strategy and detail the data
reduction processes we employ, including techniques to mitigate the impact of
rotational variability. We present optical and near-infrared colors for 35
TNOs. We find two taxonomic groups for the dynamically excited TNOs, the
neutral and red classes, which divide at . Based on simple
albedo and orbital distribution assumptions, we find that the neutral class
outnumbers the red class, with a ratio of 4:1 and potentially as high as 11:1.
Including in our analysis constraints from the cold classical objects, which
are known to exhibit unique albedos and colors, we find that within our
measurement uncertainty, our observations are consistent with the primordial
Solar System protoplanetesimal disk being neutral-class-dominated, with two
major compositional divisions in color space.Comment: Accepted to ApJS; on-line supplemental files will be available with
the AJS published version of the pape
(16) Psyche: A mesosiderite-like asteroid?
Asteroid (16) Psyche is the target of the NASA Psyche mission. It is
considered one of the few main-belt bodies that could be an exposed
proto-planetary metallic core and that would thus be related to iron
meteorites. Such an association is however challenged by both its near- and
mid-infrared spectral properties and the reported estimates of its density.
Here, we aim to refine the density of (16) Psyche to set further constraints on
its bulk composition and determine its potential meteoritic analog.
We observed (16) Psyche with ESO VLT/SPHERE/ZIMPOL as part of our large
program (ID 199.C-0074). We used the high angular resolution of these
observations to refine Psyche's three-dimensional (3D) shape model and
subsequently its density when combined with the most recent mass estimates. In
addition, we searched for potential companions around the asteroid. We derived
a bulk density of 3.99\,\,0.26\,gcm for Psyche. While such
density is incompatible at the 3-sigma level with any iron meteorites
(7.8\,gcm), it appears fully consistent with that of
stony-iron meteorites such as mesosiderites (density
4.25\,cm). In addition, we found no satellite in our images
and set an upper limit on the diameter of any non-detected satellite of
1460\,\,200}\,m at 150\,km from Psyche (0.2\%\,\,R, the
Hill radius) and 800\,\,200\,m at 2,000\,km (3\%\,\,).
Considering that the visible and near-infrared spectral properties of
mesosiderites are similar to those of Psyche, there is merit to a
long-published initial hypothesis that Psyche could be a plausible candidate
parent body for mesosiderites.Comment: 16 page
Col-OSSOS: The Distribution of Surface Classes in Neptune's Resonances
The distribution of surface classes of resonant trans-Neptunian objects
(TNOs) provides constraints on the protoplanetesimal disk and giant planet
migration. To better understand the surfaces of TNOs, the Colours of the Outer
Solar System Origins Survey (Col-OSSOS) acquired multi-band photometry of 102
TNOs, and found that the surfaces of TNOs can be well described by two surface
classifications, BrightIR and FaintIR. These classifications both include
optically red members and are differentiated predominantly based on whether
their near-infrared spectral slope is similar to their optical spectral slope.
The vast majority of cold classical TNOs, with dynamically quiescent orbits,
have the FaintIR surface classification, and we infer that TNOs in other
dynamical classifications with FaintIR surfaces share a common origin with the
cold classical TNOs. Comparison between the resonant populations and the
possible parent populations of cold classical and dynamically excited TNOs
reveal that the 3:2 has minimal contributions from the FaintIR class, which
could be explained by the secular resonance clearing the region near
the 3:2 before any sweeping capture occurred. Conversely, the fraction of
FaintIR objects in the 4:3 resonance, 2:1 resonance, and the resonances within
the cold classical belt, suggest that the FaintIR surface formed in the
protoplanetary disk between 34.6 and 47 au, though the outer bound depends on
the degree of resonance sweeping during migration. The presence and absence of
the FaintIR surfaces in Neptune's resonances provides critical constraints for
the history of Neptune's migration, the evolution of the , and the
surface class distribution in the initial planetesimal diskComment: 19 pages, 8 figures. in Press at PS
Compositional homogeneity of CM parent bodies.
CM chondrites are the most common type of hydrated meteorites, making up ∼1.5% of all falls. Whereas most CM chondrites experienced only low-temperature (∼0°C–120°C) aqueous alteration, the existence of a small fraction of CM chondrites that suffered both hydration and heating complicates our understanding of the early thermal evolution of the CM parent body(ies). Here, we provide new constraints on the collisional and thermal history of CM-like bodies from a comparison between newly acquired spectral measurements of main-belt Ch/Cgh-type asteroids (70 objects) and existing laboratory spectral measurements of CM chondrites. It first appears that the spectral variation observed among CM-like bodies is essentially due to variations in the average regolith grain size. Second, the spectral properties of the vast majority (unheated) of CM chondrites resemble both the surfaces and the interiors of CM-like bodies, implying a “low” temperature ( 100 km)—supposedly primordial—Ch/ Cgh-type main-belt asteroids likely expose the interiors of the primordial CM parent bodies, a possible consequence of impacts by small asteroids (D < 10 km) in the early solar system.The MIT component of this work is supported by NASA grant 09-NEOO009-0001, and by the National Science Foundation under grants Nos. 0506716 and 0907766. F.E.D. acknowledges support from NASA under grant No. NNX12AL26G issued through the Planetary Astronomy Program. E.A.C. thanks the Canada Foundation for Innovation, the Manitoba Research Innovations Fund, the Canadian Space Agency, the University of Winnipeg, and the Natural Sciences and Engineering Research Council of Canada for supporting the establishment and operation of the University of Winnipeg's Planetary Spectrophotometer Facility and this study.http://iopscience.iop.org/article/10.3847/0004-6256/152/3/54/met
Col-OSSOS: Z-Band Photometry Reveals Three Distinct TNO Surface Types
Several different classes of trans-Neptunian objects (TNOs) have been
identified based on their optical and near-infrared colors. As part of the
Colours of the Outer Solar System Origins Survey, we have obtained , ,
and band photometry of 26 TNOs using Subaru and Gemini Observatories.
Previous color surveys have not utilized band reflectance, and the
inclusion of this band reveals significant surface reflectance variations
between sub-populations. The colors of TNOs in and show obvious
structure, and appear consistent with the previously measured bi-modality in
. The distribution of colors of the two dynamically excited surface types
can be modeled using the two-component mixing models from Fraser \& Brown
(2012). With the combination of and , the dynamically excited
classes can be separated cleanly into red and neutral surface classes. In and , the two dynamically excited surface groups are also clearly
distinct from the cold classical TNO surfaces, which are red, with
0.85 and 0.6, while all dynamically excited objects
with similar colors exhibit redder colors. The band photometry
makes it possible for the first time to differentiate the red excited TNO
surfaces from the red cold classical TNO surfaces. The discovery of different
colors for these cold classical TNOs makes it possible to search for cold
classical surfaces in other regions of the Kuiper belt and to completely
separate cold classical TNOs from the dynamically excited population, which
overlaps in orbital parameter space.Comment: 11 pages, 2 figures, Accepted to A
The equilibrium shape of (65) Cybele: primordial or relic of a large impact?
Cybele asteroids constitute an appealing reservoir of primitive material
genetically linked to the outer Solar System, and the physical properties of
the largest members can be readily accessed by large telescopes. We took
advantage of the bright apparition of (65) Cybele in July and August 2021 to
acquire high-angular-resolution images and optical light curves of the asteroid
with which we aim to analyse its shape and bulk properties. 7 series of images
acquired with VLT/SPHERE were combined with optical light curves to reconstruct
the shape of the asteroid using the ADAM, MPCD, and SAGE algorithms. The origin
of the shape was investigated by means of N-body simulations. Cybele has a
volume-equivalent diameter of 263+/-3km and a bulk density of
1.55+/-0.19g.cm-3. Notably, its shape and rotation state are closely compatible
with those of a Maclaurin equilibrium figure. The lack of a collisional family
associated with Cybele and the higher bulk density of that body with respect to
other large P-type asteroids suggest that it never experienced any large
disruptive impact followed by rapid re-accumulation. This would imply that its
present-day shape represents the original one. However, numerical integration
of the long-term dynamical evolution of a hypothetical family shows that it is
dispersed by gravitational perturbations and chaotic diffusion over Gyrs of
evolution. The very close match between Cybele and an equilibrium figure opens
up the possibility that D>260km small bodies from the outer Solar System all
formed at equilibrium. However, we cannot rule out an old impact as the origin
of the equilibrium shape. Cybele itself is found to be dynamically unstable,
implying that it was recently (<1Ga) placed on its current orbit either through
slow diffusion from a relatively stable orbit in the Cybele region or, less
likely, from an unstable, JFC orbit in the planet-crossing region.Comment: 19 pages, 14 figures, 4 tables, accepted for publication in A&
The Main Belt Comets and ice in the Solar System
We review the evidence for buried ice in the asteroid belt; specifically the questions around the so-called Main Belt Comets (MBCs). We summarise the evidence for water throughout the Solar System, and describe the various methods for detecting it, including remote sensing from ultraviolet to radio wavelengths. We review progress in the first decade of study of MBCs, including observations, modelling of ice survival, and discussion on their origins. We then look at which methods will likely be most effective for further progress, including the key challenge of direct detection of (escaping) water in these bodies
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