Asteroid Discovery and Characterization with the Large Synoptic Survey Telescope

Jones, Lynne; Jurić, Mario; Ivezić, Željko

doi:10.1017/s1743921315008510

Cited by 37 publications

(27 citation statements)

References 8 publications

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“…In the short-term, it would be useful to confirm the tumbling state of 121514 and to check whether 101429 rotates in a prograde or retrograde sense since this determines the sign of the Yarkovsky acceleration acting on it. In the longer term, facilities such as PanSTARRS (Jedicke et al, 2007;Wainscoat et al, 2015), GAIA and, especially, the Large Synoptic Survey Telescope (Lynne Jones et al, 2015) will improve the current level of population completeness of the Trojans (shown here to be H lim ≃ 20) by several magnitudes and should discover a few hundred additional members of the Eureka family (Christou, A. A., IAU 2018 Coll.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Population control of Mars Trojans by the Yarkovsky & YORP effects

Christou

Borisov

Dell’Oro

et al. 2020

Icarus

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We explore the hypothesis that the population of Martian Trojans is the result of a balance between the production of new asteroids ("YORPlets") through the YORP effect and their eventual escape from the Trojan clouds through Yarkovsky-driven orbital evolution. Our principal observables are: (5261) Eureka, its family of 8 asteroids and the family-less Trojans (101429) 1998 VF 31 & (121514) 1999 UJ 7 . We model the population evolution as a birth-death random process and assume it is in a steady state. We then simulate the discovery of Trojans to-date and find that family members of 101429 and 121514, if they exist, are intrinsically more difficult to detect than Eureka's.Their non-discovery can be used as evidence of their non-existence only under the assumption that their brightness relative to the parent asteroid is similar to that in the Eureka family. To find out how efficiently Mars Trojans are lost from the Trojan clouds due to the Yarkovsky effect, we carry out dynamical simulations of test particles originating from these parent bodies. We find that objects originating from Eureka and 121514 begin escaping after ∼1 Gyr, but that those from 101429 are already lost by that time, probably due to that asteroid's proximity to an eccentricity-type secular resonance within Mars's co-orbital region. This is the likely cause behind the absence of Trojans in the orbital vicinity of 101429. In contrast, the solitary status of 121514 points to an intrinsic inability of the asteroid to produce YORPlets during the most recent ∼20% of the solar system's history, a finding potentially related to 121514's present, low angular momentum rotational state, unless the Eureka family formed rapidly during a single fission event.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Population control of Mars Trojans by the Yarkovsky & YORP effects

Christou

Borisov

Dell’Oro

et al. 2020

Icarus

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“…We surveyed 155.3 deg 2 of sky near the invariable plane at a range of heliocentric longitudes to moving-target limiting magnitudes (m r ) ranging from m r = 24.1 to 25.2. Three-quarters of the survey goes deeper than the forthcoming Large Synoptic Survey Telescope will reach in single observations (Jones et al 2016).…”

Section: Introductionmentioning

confidence: 96%

OSSOS. VII. 800+ Trans-Neptunian Objects—The Complete Data Release

Bannister

Gladman

Kavelaars

et al. 2018

ApJS

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135

164

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The Outer Solar System Origins Survey (OSSOS), a wide-field imaging program in 2013-2017 with the CanadaFrance-Hawaii Telescope, surveyed 155 deg 2 of sky to depths of m r = 24.1-25.2. We present 838 outer solar system discoveries that are entirely free of ephemeris bias. This increases the inventory of trans-Neptunian objects (TNOs) with accurately known orbits by nearly 50%. Each minor planet has 20-60 Gaia/Pan-STARRS-calibrated astrometric measurements made over 2-5 oppositions, which allows accurate classification of their orbits within the trans-Neptunian dynamical populations. The populations orbiting in mean-motion resonance with Neptune are key to understanding Neptune's early migration. Our 313 resonant TNOs, including 132 plutinos, triple the available characterized sample and include new occupancy of distant resonances out to semimajor axis a ∼ 130 au. OSSOS doubles the known population of the nonresonant Kuiper Belt, providing 436 TNOs in this region, all with exceptionally high-quality orbits of a uncertainty σ a 0.1%; they show that the belt exists from a  37 au, with a lower perihelion bound of 35au. We confirm the presence of a concentrated low-inclination a ; 44 au "kernel" population and a dynamically cold population extending beyond the 2:1 resonance. We finely quantify the survey's observational biases. Our survey simulator provides a straightforward way to impose these biases on models of the trans-Neptunian orbit distributions, allowing statistical comparison to the discoveries. The OSSOS TNOs, unprecedented in their orbital precision for the size of the sample, are ideal for testing concepts of the history of giant planet migration in the solar system.

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“…The Large Synoptic Survey Telescope is expected to detect hundreds of new TNOs because of its incredible sky coverage and cadence. The LSST main survey of 18,000 square degrees has a single-image limiting magnitude of m r = 24.5 (Ivezić et al 2008;Jones et al 2016), shallower than much of OSSOS. It will thus provide comparatively few high-q TNOs, due to the steep TNO size distribution.…”

Section: Discussionmentioning

confidence: 99%

OSSOS. XIII. Fossilized Resonant Dropouts Tentatively Confirm Neptune’s Migration Was Grainy and Slow

Lawler

Pike

Kaib

et al. 2019

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The migration of Neptune's resonances through the proto-Kuiper belt has been imprinted in the distribution of small bodies in the outer Solar System. Here we analyze five published Neptune migration models in detail, focusing on the high pericenter distance (high-q) trans-Neptunian Objects (TNOs) near Neptune's 5:2 and 3:1 mean-motion resonances, because they have large resonant populations, are outside the main classical belt, and are relatively isolated from other strong resonances. We compare the observationally biased output from these dynamical models with the detected TNOs from the Outer Solar System Origins Survey, via its Survey Simulator. All of the four new OSSOS detections of high-q non-resonant TNOs are on the Sunward side of the 5:2 and 3:1 resonances. We show that even after accounting for observation biases, this asymmetric distribution cannot be drawn from a uniform distribution of TNOs at 2σ confidence. As shown by previous work, our analysis here tentatively confirms that the dynamical model that uses grainy slow Neptune migration provides the best match to the real high-q TNO orbital data. However, due to extreme observational biases, we have very few high-q TNO discoveries with which to statistically constrain the models. Thus, this analysis provides a framework for future comparison between the output from detailed, dynamically classified Neptune migration simulations and the TNO discoveries from future well-characterized surveys. We show that a deeper survey (to a limiting r-magnitude of 26.0) with a similar survey area to OSSOS could statistically distinguish between these five Neptune migration models.

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Asteroid Discovery and Characterization with the Large Synoptic Survey Telescope

Cited by 37 publications

References 8 publications

Population control of Mars Trojans by the Yarkovsky & YORP effects

Population control of Mars Trojans by the Yarkovsky & YORP effects

OSSOS. VII. 800+ Trans-Neptunian Objects—The Complete Data Release

OSSOS. XIII. Fossilized Resonant Dropouts Tentatively Confirm Neptune’s Migration Was Grainy and Slow

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