Padua family

Short description: Asteroid family

The Padua family (FIN: 507), also known as the Lydia family, is a mid-sized family of asteroids of more than a thousand members.

The family is at least 25 million years old. Its members were previously associated to 110 Lydia, and are predominantly X-type asteroids with an albedo of approximately 0.1. Together with the Agnia family, the Padua family is the only other family to have most of its members in a nonlinear secular resonance configuration, with more than 75% of its members in a z1 librating state.[1][2][3]: 23

The Paduan (Lydian) asteroids are located in the outer part of the central asteroid belt having a semi-major axis of approximately 2.75. The family's namesake is the asteroid 363 Padua, while 110 Lydia is now a suspected interloper, despite having the same spectral type.[1][3]: 23

## Members

Some prominent members with known spectral type.[1]: 364 A list of all Paduan asteroids is given at the "Small Bodies Data Ferret".[4]

Name  | Type  | Diameter  | Albedo  | Catalog  | Refs

|
|
|
|
|

110 Lydia | X | 86 | 0.1808 | list | JPL * MPC * LCDB
363 Padua | X | 88 | 0.057 | list | JPL * MPC * LCDB
1517 Beograd | X | 36 | 0.0448 | list | JPL * MPC * LCDB
1766 Slipher | C | 20 | 0.057 | list | JPL * MPC * LCDB
2306 Bauschinger | X | 21 | 0.0526 | list | JPL * MPC * LCDB
2560 Siegma | Xc | 20 | 0.057 | list | JPL * MPC * LCDB
3020 Naudts | Sl | 16 | 0.057 | list | JPL * MPC * LCDB
3670 Northcott | X | 19 | 0.045 | list | JPL * MPC * —
5087 Emelʹyanov | X | 13 | 0.057 | list | JPL * MPC * LCDB
5103 Diviš | X | 12 | 0.074 | list | JPL * MPC * —
8450 Egorov | C | 11 | 0.058 | list | JPL * MPC * —
12281 Chaumont | X | 16 | 0.032 | list | JPL * MPC * —
Diameter and albedo figures taken from the LCDB, or, if not available, from JPL's SBDB. Also see category.

## Lydia former namesake and potential interloper

In previous works (Zappala et al. 1995), this family was named Lydia after 110 Lydia, which is an X-type asteroid in the SMASS classification (Tholen: M-type). While Lydia is still a member of the now-called Padua family (Nesvorny 2005, AstDyS), it has been suspected that it might be an interloper in its "own" family despite its matching spectral type (Carruba 2009; Mothe-Diniz et al. 2005).[1]: 369

Also, the asteroid 308 Polyxo was formerly considered the family's largest member.[5] This T-type asteroid is no longer considered a family member and is categorized as a background asteroid on AstDyS.[4][6]

## References

1. ↑ 1.0 1.1 1.2 1.3 Carruba, V. (May 2009). "The (not so) peculiar case of the Padua family". Monthly Notices of the Royal Astronomical Society 395 (1): 358–377. doi:10.1111/j.1365-2966.2009.14523.x. Bibcode: 2009MNRAS.395..358C.
2. ↑ Carruba, V.; Domingos, R. C.; Nesvorný, D.; Roig, F.; Huaman, M. E.; Souami, D. (August 2013). "A multidomain approach to asteroid families' identification". Monthly Notices of the Royal Astronomical Society 433 (3): 2075–2096. doi:10.1093/mnras/stt884. Bibcode: 2013MNRAS.433.2075C.
3. ↑ 3.0 3.1 Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. Bibcode: 2015aste.book..297N.
4. ↑ 4.0 4.1 "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Archived from the original on 16 August 2017. https://web.archive.org/web/20170816000205/http://sbntools.psi.edu/ferret/PropertySearch/familyForm.action. Retrieved 22 July 2017.
5. ↑ Ridpath, Ian (2003). Oxford Dictionary of Astronomy. Oxford University Press. ISBN 0199609055. https://books.google.com/books?id=O31j9UJ3U4oC&q=lydia+family+of+asteroids&pg=PA282. Retrieved 25 January 2016.
6. ↑ "AstDyS-2 data for (308) Polyxo". AstDyS - Asteroids Dynamic Site. https://newton.spacedys.com/astdys/index.php?pc=1.1.6&n=308. Retrieved 30 August 2017.

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