An automatic approach to exclude interlopers from asteroid families

Radović, Viktor; Novaković, Bojan; Carruba, V.; Marceta, D.

doi:10.1093/mnras/stx1273

Cited by 37 publications

(30 citation statements)

References 62 publications

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“…We found that this catalogue contains colours of 55 family members. Based on this data, and following Radović, et al (2017), we were able to reliably identify only one potential interloper, the asteroid (38685) 2000 QP 9 . However, as this object was already marked as the interloper based on its albedo, no additional asteroid has been removed from the family based on the SDSS colours.…”

Section: Membership and Spectral Reflectance Characteristicsmentioning

confidence: 89%

Analysis of the Karma asteroid family

Pavela

Novaković

Carruba

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The Karma asteroid family is a group of primitive asteroids in the middle part of the main belt, just at the outer edge of the 3J:1A mean-motion resonance. We obtained the list of the family members with 317 asteroids, and estimated that it was formed by the catastrophic disruption of a parent body that was between 34 and 41 km in diameter. Based on the V-shape method, age of the Karma family is estimated to be about 137 Myr. A detailed dynamical map of the region combined with numerical simulations allowed us to reconstruct the long-term dynamical evolution of the family, and to identify the mechanisms responsible for this evolution. The numerical simulations successfully reproduced the main features in the orbital distribution of the family members but also showed that some regions of the Karma family could be missing. A more detailed analysis revealed that these regions likely consist of very dark objects, fainter than absolute magnitude H=17, that have not yet been detected. Based on the obtained results, we concluded that magnitude-frequency distribution of family members up to H=16 mag is neither affected by dynamical erosion nor observational incompleteness, and therefore represents the result of collisional grinding of the original family population. Finally, we found that the Karma family have been supplying some asteroids to the near-Earth region via the 3J:1A resonance. Currently there should about 10 family members larger than 1 km in diameter, orbiting in the near-Earth space.

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Section: Membership and Spectral Reflectance Characteristicsmentioning

confidence: 89%

Analysis of the Karma asteroid family

Pavela

Novaković

Carruba

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…First, we need a consistent way to identify asteroid family members for the training of the algorithms. For this purpose, we turn our attention to the data base of asteroid families available at the Asteroid Families Portal (AFP, http://asteroids.matf.bg.ac.rs/fam/properelements.php: accessed on 2019 December 5; Radović et al 2017). The web-page-based algorithms allow to automatically obtain asteroid families in a data set of 631 226 asteroids with synthetic proper elements using standard HCM procedures.…”

Section: Ac H I N E L E a R N I N G C L A S S I F I C At I O N O F mentioning

confidence: 99%

“…We required the chosen families to be represented in the Radović et al (2017) catalogue, to be located in the inner, central, and outer main belt at low inclinations (see Carruba et al 2013, for a definition of these zones), since in these regions, we found the most numerous families, and also to have at least 10 members with H < 14 (we include just one case with a lower sample, that of the Massalia family, so as to have a larger number of families located in the inner main belt. This family is most likely the outcome of a cratering event, which explains the lack of bright members; Milani et al 2019).…”

Section: Ac H I N E L E a R N I N G C L A S S I F I C At I O N O F mentioning

confidence: 99%

“…We would like to thank the São Paulo State Science Foundation (FAPESP, grant 2018/20999-6), the Brazilian National Research Council (CNPq, grant 301577/2017-0, 310317/2016-9), and the Coordination for the Improvement of Higher Education Personnel (CAPES, grant 88887.374148/2019-00). We acknowledge the use of data from the Asteroid Dynamics Site (AstDys) (http://hamilton.dm.unipi.it/astdys, Knežević; Milani 2003) and the Asteroid Families Portal (AFP, http://asteroids.matf.bg.ac.rs/fam/properelements.php; Radović et al 2017). We also acknowledge the use of exercises proposed by machine learning courses at DataCamp (www.datacamp.com), which either inspired or helped in the development of the software used in this work.…”

Section: Ac K N Ow L E D G E M E N T Smentioning

confidence: 99%

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Machine learning classification of new asteroid families members

Carruba

Aljbaae

Domingos

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Asteroid families are groups of asteroids that are the product of collisions or of the rotational fission of a parent object. These groups are mainly identified in proper elements or frequencies domains. Because of robotic telescope surveys, the number of known asteroids has increased from ${\simeq}10\, 000$ in the early 1990s to more than $750\, 000$ nowadays. Traditional approaches for identifying new members of asteroid families, like the hierarchical clustering method (HCM), may struggle to keep up with the growing rate of new discoveries. Here we used machine learning classification algorithms to identify new family members based on the orbital distribution in proper (a, e, sin (i)) of previously known family constituents. We compared the outcome of nine classification algorithms from stand-alone and ensemble approaches. The extremely randomized trees (ExtraTree) method had the highest precision, enabling to retrieve up to 97 per cent of family members identified with standard HCM.

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“…The inner and outer V-shapes must be wide enough to include enough asteroids in the inner V-shape and measure a N 2 in to N out ratio high enough to identify the family V-shape. The V-shape can include interlopers or asteroids which are not part of the family V-shape if the value used for dC is used is too large (Nesvorný et al 2015;Radović et al 2017). The V-shape identification technique was tested on families identified by both Nesvorný et al (2015) and Milani et al (2014) to verify that the V-shape a c , C and α determination works on family membership definitions from either database and produces similar results.…”

Section: V-shape Identification Technique and Measurement Of αmentioning

confidence: 99%

Initial velocity V-shapes of young asteroid families

Bolin

Walsh

Morbidelli

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Ejection velocity fields of asteroid families are largely unconstrained due to the fact that members disperse relatively quickly on Myr time-scales by secular resonances and the Yarkovsky effect. The spreading of fragments in a by the Yarkovsky effect is indistinguishable from the spreading caused by the initial ejection of fragments. By examining families <20 Myrs-old, we can use the V-shape identification technique to separate family shapes that are due to the initial ejection velocity field and those that are due to the Yarkovsky effect. <20Myr-old asteroid families provide an opportunity to study the velocity field of family fragments before they become too dispersed. Only the Karin family's initial velocity field has been determined and scales inversely with diameter, D −1 .We have applied the V-shape identification technique to constrain young families' initial ejection velocity fields by measuring the curvature of their fragments' Vshape correlation in semi-major axis, a, vs. D −1 space. Curvature from a straight line implies a deviation from a scaling of D −1 . We measure the V-shape curvature of 11 young asteroid families including the 1993 FY 12 , Aeolia, Brangane, Brasilia, Clarissa, Iannini, Karin, Konig, Koronis(2), Theobalda and Veritas asteroid families. We find that the majority of asteroid families have initial ejection velocity fields consistent with ∼ D −1 supporting laboratory impact experiments and computer simulations of disrupting asteroid parent bodies.

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An automatic approach to exclude interlopers from asteroid families

Cited by 37 publications

References 62 publications

Analysis of the Karma asteroid family

Analysis of the Karma asteroid family

Machine learning classification of new asteroid families members

Initial velocity V-shapes of young asteroid families

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