3268 De Sanctis

3268 De Sanctis, provisional designation 1981 DD, is a Vestian asteroid from the inner regions of the asteroid belt, approximately 6 kilometers (3.7 miles) in diameter. It was discovered on 26 February 1981, by European astronomers Henri Debehogne and Giovanni de Sanctis at ESO's La Silla Observatory in northern Chile. The asteroid was named after the second discoverer.[1] The assumed S-type asteroid has a rotation period of 17 hours.[2]

3268 De Sanctis
Discovery [1]
Discovered byH. Debehogne
G. de Sanctis
Discovery siteLa Silla Obs.
Discovery date26 February 1981
Designations
(3268) De Sanctis
Named after
Giovanni de Sanctis [1]
(second discoverer)
1981 DD · 1979 UQ4
1979 WZ1 · 1990 WV15
main-belt · (inner)
Flora [2] · Vesta [3]
Orbital characteristics [4]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc65.44 yr (23,902 d)
Aphelion2.6447 AU
Perihelion2.0490 AU
2.3469 AU
Eccentricity0.1269
3.60 yr (1,313 d)
329.92°
0° 16m 26.76s / day
Inclination6.3522°
221.63°
74.723°
Physical characteristics
Mean diameter
5.88 km (derived)[2]
6.033±0.120 km[5][6]
17 h[7]
0.2280±0.0056[6]
0.228±0.006[5]
0.24 (assumed)[2]
S (assumed)[2]
13.1[4] · 13.10±0.29[8]
13.32[2][6][7]

    Orbit and classification

    De Sanctis a member of the Vesta family (401) when applying the hierarchical clustering method to its proper orbital elements.[3] Vestian asteroids have a composition akin to cumulate eucrites and are thought to have originated deep within 4 Vesta's crust, possibly from the Rheasilvia crater, a large impact crater on its southern hemisphere near the South pole, formed as a result of a subcatastrophic collision.[9][10] Based on osculating Keplerian orbital elements, De Sanctis has also been classified as a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt.[2]

    The asteroid orbits the Sun in the inner main-belt at a distance of 2.0–2.6 AU once every 3 years and 7 months (1,313 days; semi-major axis of 2.35 AU). Its orbit has an eccentricity of 0.13 and an inclination of 6° with respect to the ecliptic.[4]

    The body's observation arc begins with a precovery taken at Palomar Observatory in December 1951, nearly three decades prior to its official discovery observation La Silla.[1]

    Physical characteristics

    De Sanctis is an assumed stony S-type asteroid.[2]

    Rotation period

    A first rotational lightcurve of De Sanctis was obtained from photometric observations by Polish astronomer Wiesław Wiśniewski at the University of Arizona. Lightcurve analysis gave a rotation period of 17 hours with a brightness amplitude of 0.4 magnitude (U=2).[7]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, De Sanctis measures 6.033 kilometers in diameter and its surface has an albedo of 0.228,[5][6] while the Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 – derived from 8 Flora, the parent body of the Flora family – and derives a diameter of 5.88 kilometers based on an absolute magnitude of 13.32.[2]

    Naming

    This minor planet was named by the first discoverer after the second, Giovanni de Sanctis (born 1949), an Italian astronomer at the Observatory of Turin, who closely collaborated with Henri Debehogne at the European Southern Observatory in La Silla, Chile, during the early 1980s. The official naming citation was published by the Minor Planet Center on 22 June 1986 (M.P.C. 10849).[11]

    References
    1. "3268 De Sanctis (1981 DD)". Minor Planet Center. Retrieved 15 March 2018.
    2. "LCDB Data for (3268) De Sanctis". Asteroid Lightcurve Database (LCDB). Retrieved 15 March 2018.
    3. "Asteroid 3268 De Sanctis – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
    4. "JPL Small-Body Database Browser: 3268 De Sanctis (1981 DD)" (2017-06-05 last obs.). Jet Propulsion Laboratory. Retrieved 15 March 2018.
    5. Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J.; et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal. 741 (2): 20. arXiv:1109.4096. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68.
    6. Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
    7. Wisniewski, W. Z. (March 1991). "Physical studies of small asteroids. I - Lightcurves and taxonomy of 10 asteroids". Icarus. 90 (1): 117–122. Bibcode:1991Icar...90..117W. doi:10.1016/0019-1035(91)90073-3. ISSN 0019-1035.
    8. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007.
    9. Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). Identification and Dynamical Properties of Asteroid Families. Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
    10. Kelley, Michael S.; Vilas, Faith; Gaffey, Michael J.; Abell, Paul A. (September 2003). "Quantified mineralogical evidence for a common origin of 1929 Kollaa with 4 Vesta and the HED meteorites". Icarus. 165 (1): 215–218. Bibcode:2003Icar..165..215K. doi:10.1016/S0019-1035(03)00149-0.
    11. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 15 March 2018.

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