Summary for : (511) Davida

DynT.TT.BT T.L B T.DDensity (g/cm^3)Δρ/ρDiameter (km)ΔD/DMass (kg)ΔM/MRefAvg.M
MBACCX | X-2.68 ± 0.98   (C)37 %298.8 ± 16.35.4 %3.74e+19 ± 1.23e+1933 %SEVM
MBACCX | X-2.67 ± 0.62   (C)23 %293.6 ± 11.13.8 %3.53e+19 ± 7.10e+1820 %Sw.avg
MBAC2.43 ± 0.79   (C)33 %298.3 ± 11.94.0 %3.38e+19 ± 1.02e+1930 %C?

Average asteroid densities (g/cm^3):
C = 1.3 ± 0.6, B = 2.4 ± 0.5, S = 2.7 ± 0.5, M = 3.5 ± 1.0, P = 2.8 ± 1.6, X = 1.9 ± 0.8, Xc = 4.9 ± 0.9, Xk = 4.2 ± 0.7 (Ref)

Additional resources:
3D Model | JPL New Horizons | Minor Planet Center | Wikipedia (these auto-generated links might not work)

Note: The density estimates have been ranked from (A) to (E), corresponding to the relative error: (B) less than 20%, (C) between 20 and 50%, (D) between 50 and 100%, and (E) more than 100%. (A) stands for (presumably) reliable estimates (accuracy better than 20%), based on more than 5 mass estimates and 5 diameter estimates, or a spacecraft encounter. Apparently unrealistic densities (ρ > 8) are tagged with (X).

EVM: average by using the Expected Value Method (Ref). w.avg: weighted average (with w = 1/err^2).

T.T: Tholen Tax Class. T.B: Bus & Binzel Tax Class. T T.L: S3OS2 Lazarro (Tholen) Tax Class. T.L B: S3OS2 Lazarro (Bus & Binzel) Tax Class. T.D: DeMeo Tax Class.

Ref: S = SiMDA, C = Carry (2012)

Diameter estimates

DesignationDiameter / Err (km)ΔD/DMethodYearRefNχ2Use
(511) Davida326.05 ± 5.301.6 % STM2004D931 26.53 1
(511) Davida316.00 ± 5.001.6 % Img2006D34 11.90 2
(511) Davida289.00 ± 21.007.3 % Img-TE2007D39 0.22 3
(511) Davida314.75 ± 12.303.9 % STM2010D64 1.69 4
(511) Davida335.33 ± 14.354.3 % NEATM2010D64 6.50 5
(511) Davida290.98 ± 4.191.4 % STM2011D83 3.44 6
(511) Davida276.23 ± 3.271.2 % NEATM2011D7212 47.44 7
(511) Davida290.44 ± 2.260.8 % NEATM2011D72 13.53 8

plot, average diameter and derived density

All

Notes (N):
1: This estimate is discarded for the average diameter (and derived density) calculation in Carry (2012).
2: This estimate is discarded for the average diameter (and derived density) calculation in SiMDA (catalog).

Img : Apparent size in disk-resolved imaging. Img-TE : Triaxial ellipsoid model from images. NEATM : Near-Earth Asteroid Thermal Model. STM : Standard Thermal Model.


EVM diam. average D = (298.8 ± 16.25) km   (ΔD/D = 5%, SNR = 18.38) Derived bulk density ρ = (2.68 ± 0.98) g/cm3   (Δρ/ρ = 37%, SNR = 2.7)


References
D34(2006):Marchis, F., Kaasalainen, M., Hom, E.F.Y., Berthier, J., Enriquez, J., Hestroffer, D., Le Mignant, D., de Pater, I., 2006. Shape, size and multiplicity of main-belt asteroids. Icarus 185, 39–63.
D39(2007):Conrad, A.R., Dumas, C., Merline, W.J., Drummond, J.D., Campbell, R.D., Goodrich, R.W., Le Mignant, D., Chaffee, F.H., Fusco, T., Kwok, S.H., Knight, R.I., 2007. Direct measurement of the size, shape, and pole of 511 Davida with Keck AO in a single night. Icarus 191, 616–627.
D64(2010):Ryan, E.L., Woodward, C.E., 2010. Rectified Asteroid Albedos and Diameters from IRAS and MSX Photometry Catalogs. Astronomical Journal 140, 933–943.
D72(2011):Masiero, J.R., Mainzer, A.K., Grav, T., Bauer, J.M., Cutri, R.M., Dailey, J., Eisenhardt, P.R.M., McMillan, R.S., Spahr, T.B., Skrutskie, M.F., Tholen, D., Walker, R.G., Wright, E.L., DeBaun, E., Elsbury, D., Gautier, IV, T., Gomillion, S., Wilkins, A., 2011. Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters. Astrophysical Journal 741, 68.
D83(2011):Usui, F., Kuroda, D., Müller, T.G., Hasegawa, S., Ishiguro, M., Ootsubo, T., Ishihara, D., Kataza, H., Takita, S., Oyabu, S., Ueno, M., Matsuhara, H., Onaka, T., 2011. Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey. Publications of the Astronomical Society of Japan 63, 1117–1138.
D93(2004):Tedesco, E.F., Noah, P.V., Noah, M.C., Price, S.D., 2004. IRAS Minor Planet Survey. NASA Planetary Data System. IRAS-A-FPA-3-RDR-IMPS-V6.0.

Mass estimates

DesignationMass / Err (kg)ΔM/MMethodYearRefNχ2Use
(511) Davida6.64e+19 ± 5.57e+188 %Deflec 2001M261227.19 1
(511) Davida4.77e+19 ± 4.77e+1810 %Deflec 2002M314.70 2
(511) Davida4.77e+19 ± 4.77e+1810 %Deflec 2004M424.70 3
(511) Davida4.38e+19 ± 1.99e+185 %Deflec 2008M72210.48 4
(511) Davida2.45e+19 ± 2.45e+1810 %Ephem 2009M8627.54 5
(511) Davida3.96e+19 ± 8.09e+1820 %Ephem 2010M930.08 6
(511) Davida3.77e+19 ± 1.97e+185 %Deflec 2011M950.03 7
(511) Davida1.71e+19 ± 1.18e+1969 %Ephem 2011M1032.95 8
(511) Davida2.42e+19 ± 7.49e+1831 %Deflec 2011M973.09 9
(511) Davida2.77e+19 ± 5.20e+1819 %Deflec 2011M973.45 10
(511) Davida2.61e+19 ± 6.03e+1823 %Deflec 2011M973.48 11
(511) Davida2.21e+19 ± 9.21e+1842 %Deflec 2011M972.74 12
(511) Davida1.81e+19 ± 4.77e+1826 %Ephem 2011M10016.30 13
(511) Davida3.00e+19 ± 9.94e+173 %OrbFitN 2014M123254.33 14
(511) Davida5.61e+19 ± 4.75e+188 %Deflec 2017M125215.52 15
(511) Davida3.32e+19 ± 3.46e+1810 %Deflec 2017M12521.44 16
(511) Davida6.82e+19 ± 8.29e+1812 %Deflec 2017M125213.84 17
(511) Davida5.11e+19 ± 6.80e+1813 %Deflec 2017M12524.08 18
(511) Davida2.90e+19 ± 6.96e+1824 %Deflec 2017M12521.43 19
(511) Davida6.58e+19 ± 2.15e+1933 %Deflec 2017M12521.75 20
(511) Davida5.35e+19 ± 1.75e+1933 %Deflec 2017M12520.85 21
(511) Davida4.36e+19 ± 2.29e+185 %Deflec 2017M125237.31 22
(511) Davida4.46e+19 ± 3.24e+187 %Ephem 2019M1265.00 23

plot, average mass and derived density

All

Notes (N):
1: This estimate is discarded for the average mass (and derived density) calculation in Carry (2012).
2: This estimate is discarded for the average mass (and derived density) calculation in SiMDA (catalog).
3: This estimate is an average of individual solutions listed before under the same reference (e.g. M125).

Deflec : Orbital deflection (close encounter) of one or several test asteroids (classical LSQ). Ephem : Planetary ephemeris solution. OrbFitN : Simultaneous multi-asteroid astrometric orbit solution (similar to 'Ephem').


EVM mass average M = (3.736 ± 1.225) × 1019 kg   (ΔM/M = 33%, SNR = 3.0) Derived bulk density ρ = (2.68 ± 0.98) g/cm3   (Δρ/ρ = 37%, SNR = 2.7)


References
M26(2001):Michalak, G., 2001. Determination of asteroid masses. II. (6) Hebe, (10) Hygiea, (15) Eunomia, (52) Europa, (88) Thisbe, (444) Typtis, (511) Davida and (704) Interamnia. Astronomy and Astrophysics 374, 703–711.
M31(2002):Chernetenko, Y.A., Kochetova, O.M., 2002. Masses of some large minor planets, in: B. Warmbein (Ed.), Asteroids, Comets, and Meteors: ACM 2002, pp. 437–440.
M42(2004):Kochetova, O.M., 2004. Determination of Large Asteroid Masses by the Dynamical Method. Solar System Research 38, 66–75.
M72(2008):Baer, J., Milani, A., Chesley, S.R., Matson, R.D., 2008. An Observational Error Model, and Application to Asteroid Mass Determination, in: Bulletin of the American Astronomical Society, p. 493.
M86(2009):Folkner, W.M., Williams, J.G., Boggs, D.H., 2009. The planetary and lunar ephemeris de 421. IPN Progress Report 42, 1–34.
M93(2010):Fienga, A., Manche, H., Kuchynka, P., Laskar, J., Gastineau, M., 2010. INPOP10a. Scientific Notes.
M95(2011):Baer, J., Chesley, S.R., Matson, R.D., 2011. Astrometric Masses of 26 Asteroids and Observations on Asteroid Porosity. Astronomical Journal 141, 143–155.
M97(2011):Zielenbach, W., 2011. Mass Determination Studies of 104 Large Asteroids. Astronomical Journal 142, 120–128.
M100(2011):Fienga, A., Kuchynka, P., Laskar, J., Manche, H., Gastineau, M., 2011. Asteroid mass determinations with INPOP planetary ephemerides. EPSC-DPS Joint Meeting 2011 , 1879.
M103(2011):Konopliv, A.S., Asmar, S.W., Folkner, W.M., Karatekin, Ö., Nunes, D.C., Smrekar, S.E., Yoder, C.F., Zuber, M.T., 2011. Mars high resolution gravity fields from MRO, Mars seasonal gravity, and other dynamical parameters. Icarus 211, 401–428.
M123(2014):Goffin, E., 2014. Astrometric asteroid masses: a simultaneous determination. Astronomy & Astrophysics, Volume 565, id.A56, 8 pp.
M125(2017):Baer, J., Chesley, S.R., 2017. Simultaneous Mass Determination for Gravitationally Coupled Asteroids. The Astronomical Journal, Volume 154, Issue 2, article id. 76, 11 pp.
M126(2019):Fienga, A., et. al, 2019. INPOP19a planetary ephemeris. Notes Scientifiques et Techniques de l'Institut de mécanique céleste,