Summary for : (90) Antiope

DynT.TT.BT T.L B T.DDensity (g/cm^3)Δρ/ρDiameter (km)ΔD/DMass (kg)ΔM/MRefAvg.M
MBACCCaa | ChC0.82 ± 0.18   (C)22 %121.8 ± 3.42.8 %7.73e+17 ± 1.54e+1720 %SEVM
MBACCCaa | ChC0.88 ± 0.32   (C)36 %121.2 ± 2.72.2 %8.19e+17 ± 2.89e+1735 %Sw.avg
MBAC0.86 ± 0.06   (B)7 %122.2 ± 2.82.3 %8.30e+17 ± 2.00e+162 %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
(90) Antiope120.06 ± 4.003.3 % STM2004D932 0.20 1
(90) Antiope111.50 ± 5.004.5 % MDM:LO2007D381 4.28 2
(90) Antiope127.02 ± 5.094.0 % NEATM2010D642 1.03 3
(90) Antiope123.80 ± 2.111.7 % STM2011D832 0.86 4
(90) Antiope123.55 ± 2.912.4 % NEATM2011D722 0.34 5
(90) Antiope118.70 ± 2.021.7 % NEATM2011D722 2.43 6

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).

MDM:LO : Multi-Data Modeling: Lightcurves + Occultations. NEATM : Near-Earth Asteroid Thermal Model. STM : Standard Thermal Model.


EVM diam. average D = (121.8 ± 3.43) km   (ΔD/D = 3%, SNR = 35.56) Derived bulk density ρ = (0.82 ± 0.18) g/cm3   (Δρ/ρ = 22%, SNR = 4.6)


References
D38(2007):Descamps, P., Marchis, F., Michalowski, T., Vachier, F., Colas, F., Berthier, J., Assafin, M., Dunckel, P.B., Polinska, M., Pych, W., Hestroffer, D., Miller, K.P.M., Vieira-Martins, R., Birlan, M., Teng-Chuen-Yu, J.P., Peyrot, A., Payet, B., Dorseuil, J., Léonie, Y., Dijoux, T., 2007b. Figure of the double Asteroid 90 Antiope from adaptive optics and lightcurve observations. Icarus 187, 482–499.
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
(90) Antiope4.10e+17 ± 1.19e+1729 %BinImg 2002M32129.30 1
(90) Antiope8.30e+17 ± 1.99e+162 %BinImg 2007M658.22 2
(90) Antiope9.86e+17 ± 4.85e+1749 %Ephem 2019M1260.19 3

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).

BinImg : Binary imaged at optical wavelength. Ephem : Planetary ephemeris solution.


EVM mass average M = (7.729 ± 1.537) × 1017 kg   (ΔM/M = 20%, SNR = 5.0) Derived bulk density ρ = (0.82 ± 0.18) g/cm3   (Δρ/ρ = 22%, SNR = 4.6)


References
M32(2002):Merline, W.J., Weidenschilling, S.J., Durda, D.D., Margot, J.L., Pravec, P., Storrs, A.D., 2002. Asteroids Do Have Satellites. Asteroids III , 289–312.
M65(2007):Descamps, P., Marchis, F., Michalowski, T., Vachier, F., Colas, F., Berthier, J., Assafin, M., Dunckel, P.B., Polinska, M., Pych, W., Hestroffer, D., Miller, K.P.M., Vieira-Martins, R., Birlan, M., Teng-Chuen-Yu, J.P., Peyrot, A., Payet, B., Dorseuil, J., Léonie, Y., Dijoux, T., 2007. Figure of the double Asteroid 90 Antiope from adaptive optics and lightcurve observations. Icarus 187, 482–499.
M126(2019):Fienga, A., et. al, 2019. INPOP19a planetary ephemeris. Notes Scientifiques et Techniques de l'Institut de mécanique céleste,