Summary for : (3169) Ostro

DynT.TT.BT T.L B T.DDensity (g/cm^3)Δρ/ρDiameter (km)ΔD/DMass (kg)ΔM/MRefAvg.M
MBATSXeC | Cb-2.60 ± 0.88   (C)34 %5.2 ± 0.11.6 %1.86e+14 ± 6.20e+1333 %SEVM
MBATSXeC | Cb-2.60 ± 0.88   (C)34 %5.2 ± 0.11.6 %1.86e+14 ± 6.20e+1333 %Sw.avg
MBAXe2.59 ± 0.20   (B)8 %5.2 ± 0.11.6 %1.86e+14 ± 6.20e+1333 %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)

(Indirect) density estimates

Density (g/cm^3)Δρ/ρMethodYearRefN
2.6 ± 0.207.7 %PheMu2007BD9

PheMu : Mutual eclipsing phenomena in binary systems.
References
BD9(2007):Descamps, P., Marchis, F., Michalowski, T., et al., 2007. Nature of the small main belt Asteroid 3169 Ostro. Icarus 189, 362-369.

Diameter estimates

DesignationDiameter / Err (km)ΔD/DMethodYearRefNχ2Use
(3169) Ostro5.15 ± 0.081.6 % NEATM2011D72 0.00 1

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).

NEATM : Near-Earth Asteroid Thermal Model.


EVM diam. average D = (5.2 ± 0.08) km   (ΔD/D = 2%, SNR = 64.38) Derived bulk density ρ = (2.60 ± 0.88) g/cm3   (Δρ/ρ = 34%, SNR = 3.0)


References
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.

Mass estimates

DesignationMass / Err (kg)ΔM/MMethodYearRefNχ2Use
(3169) Ostro1.86e+14 ± 6.20e+1333 %PheMu 2007M660.00 1

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).

PheMu : Mutual eclipsing phenomena in binary systems.


EVM mass average M = (1.860 ± 0.620) × 1014 kg   (ΔM/M = 33%, SNR = 3.0) Derived bulk density ρ = (2.60 ± 0.88) g/cm3   (Δρ/ρ = 34%, SNR = 3.0)


References
M66(2007):Descamps, P., Marchis, F., Michalowski, T., Colas, F., Berthier, J., Vachier, F., Teng-Chuen-Yu, J.P., Peyrot, A., Payet, B., Dorseuil, J., Léonie, Y., Dijoux, T., Berrouachdi, H., Chion Hock, C., Benard, F., 2007. Nature of the small main belt Asteroid 3169 Ostro. Icarus 189, 362–369.