A three-dimensional solution for the orbit of the asteroidal satellite of 22 Kalliope

Marchis, Franck; Descamps, P.; Hestroffer, Daniel; Berthier, J.; Vachier, F.; Boccaletti, A.; Pater, I. de; Gavel, Don

doi:10.1016/s0019-1035(03)00195-7

Cited by 32 publications

(29 citation statements)

References 13 publications

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“…The satellite diameter is estimated to be 28 ± 2 km, derived from analyses of the mutual events and the 2006 stellar occultation (Descamps et al 2008). We focused our study on 52 observations collected with the VLT, Keck, and Gemini North 8−10 m class telescopes, with the Shane-3m Lick telescope (Marchis et al 2003) and Palomar 5m-telescope (Margot & Brown 2003, both equipped with AO systems. Recent observations collected with W.M.…”

Section: A Well-constrained Dynamical Model Of (22) Kalliope and Its mentioning

confidence: 99%

Determination of binary asteroid orbits with a genetic-based algorithm

Vachier

Berthier

Marchis

2012

A&A

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Aims. Over the past decade, discoveries of multiple and binary asteroid systems have played a significant role in our general understanding of small solar system bodies. Direct observations of satellites of asteroids are rare and difficult since they require the use of already over-subscribed facilities such as adaptive optics (AO) on large 8−10 m class telescopes and the Hubble Space Telescope (HST). The scarcity of data and the long temporal baseline of observations (up to 10 years) significantly complicate the determination of the mutual orbits of these systems. Methods. We implemented a new approach for determining the mutual orbits of directly-imaged multiple asteroids using a geneticbased algorithm. This approach was applied to several known binary asteroid systems (22 Kalliope, 3749 Balam, and 50 000 Quaoar) observed with AO systems and HST. This statistical method is fast enough to permit the search for an orbital solution across a large parameter space and without a priori information about the mutual orbit. Results. From 10 years of observation, we derived an orbital solution for Linus, companion of (22) Kalliope, with an accuracy close to the astrometric limit provided by the AO observations, assuming a purely Keplerian orbit. A search for non-Keplerian orbit confirmed that a J 2 ∼ 0 is the best-fitting solution. We show that the precession of the nodes could be detected without ambiguity, implying that Kalliope's primary may have an inhomogeneous internal structure. HST astrometric observations of Weywot, companion of the trans-Neptunian object (50 000) Quaoar, were used to derive its mass and its bulk density, which appears to be higher than the density of other TNOs. Finally, we derived a bundle of orbital solutions for (3749) Balam, with equally good fits, from the limited set of astrometric positions. They provide a realistic density between 1.3 and 3.7 g/cm 3 for this S-type asteroid.

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Section: A Well-constrained Dynamical Model Of (22) Kalliope and Its mentioning

confidence: 99%

Determination of binary asteroid orbits with a genetic-based algorithm

Vachier

Berthier

Marchis

2012

A&A

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“…In contrast, the 3749 Balam and 379 Huenna asteroid systems have loosely bound moonlet companion with semi-major axis values of and , respectively (Marchis et al, 2005a). In Tables 6a and 6b, we calculated the Hill radius for each asteroid and estimated their mass, based on their IRAS diameter and assumed the following average densities: 1.7 g/cm 3 for C-type and additional sub-class (B, F, and G) asteroids, and 2.4 g/cm 3 for S-type asteroids (Birlan, 2002); for M-type asteroids, we chose an average density of 3.5 g/cm 3 based on direct measurements reported in Ostro et al (2000) and Hestroffer et al (2002) for 216 Kleopatra and in Marchis et al (2003b) and Margot (2002) for 22 Kalliope.…”

Section: Search For Moonlet Companionsmentioning

confidence: 99%

“…Most of the recent results obtained by this technique focused on the search and analysis of secondary moonlet previously discovered around 18 main-belt asteroids. Our group focused on constraining the companion orbits of several systems: 22 Kalliope (Marchis et al, 2003b), 45 Eugenia (Marchis et al, 2004b), 87 Sylvia (Marchis et al, 2005b), 90 Antiope (Descamps et al, 2005), to name a few. These analyses provided information about the formation of those binary asteroids and gave clues about their interior structure.…”

Section: Introductionmentioning

confidence: 99%

Shape, size and multiplicity of main-belt asteroidsI. Keck Adaptive Optics survey

Marchis

Kaasalainen

Hom

et al. 2006

Icarus

109

101

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This paper presents results from a high spatial resolution survey of 33 main-belt asteroids with diameters >40 km using the Keck II Adaptive Optics (AO) facility. Five of these (45 Eugenia, 87 Sylvia, 107 Camilla, 121 Hermione, 130 Elektra) were confirmed to have satellite. Assuming the same albedo as the primary, these moonlets are relatively small (∼5% of the primary size) suggesting that they are fragments captured after a disruptive collision of a parent body or captured ejecta due to an impact. For each asteroid, we have estimated the minimum size of a moonlet that can positively detected within the Hill sphere of the system by estimating and modeling a 2-σ detection profile: in average on the data set, a moonlet located at 2/100 × R Hill (1/4 × R Hill ) with a diameter larger than 6 km (4 km) would have been unambiguously seen. The apparent size and shape of each asteroid was estimated after deconvolution using a new algorithm called AIDA. The mean diameter for the majority of asteroids is in good agreement with IRAS radiometric measurements, though for asteroids with a D < 200 km, it is underestimated on average by 6-8%. Most asteroids had a size ratio that was very close to those determined by lightcurve measurements. One observation of 104 Klymene suggests it has a bifurcated shape. The bi-lobed shape of 121 Hermione described in Marchis et al. [Marchis, F., Hestroffer, D., Descamps, P., Berthier, J., Laver, C., de Pater, I., 2005c. Icarus 178, 450-464] was confirmed after deconvolution. The ratio of contact binaries in our survey, which is limited to asteroids larger than 40 km, is surprisingly high (∼6%), suggesting that a non-single configuration is common in the main-belt. Several asteroids have been analyzed with lightcurve inversions. We compared lightcurve inversion models for plane-of-sky predictions with the observed images (9 Metis, 52 Europa, 87 Sylvia, 130 Elektra, 192 Nausikaa, and 423 Diotima, 511 Davida). The AO images allowed us to determine a unique photometric mirror pole solution, which is normally ambiguous for asteroids moving close to the plane of the ecliptic (e.g., 192 Nausikaa and 52 Europa). The photometric inversion models agree well with the AO images, thus confirming the validity of both the lightcurve inversion method and the AO image reduction technique.

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“…By comparing both one can at least test the hypothesis of constant bulk-density inside the (primary) asteroid. This has been applied to the orbit of Kalliope's companion [36]. Assuming a homogeneous primary with constant density distribution the observed geometrical flattening provides a dynamical J2 = 1 10…”

Section: Binary Systems and The Density Profilementioning

confidence: 99%

“…Six objects having interesting spin and lightcurve properties have been chosen, each observed for an HST "orbit", i.e. for a total duration of about 40 minutes (corresponding to [30][31][32][33][34][35][36][37][38][39][40]. During this time lapse two movements affect the observation: the spin of the object and its proper motion.…”

Section: The Fgs Interferometermentioning

confidence: 99%