Summary for : (3749) Balam

DynT.TT.BT T.L B T.DDensity (g/cm^3)Δρ/ρDiameter (km)ΔD/DMass (kg)ΔM/MRefAvg.M
MBA--- | --8.81 ± 3.15   (X)36 %4.8 ± 0.611.9 %5.09e+14 ± 1.99e+134 %SEVM
MBA--- | --9.60 ± 10.22   (X)106 %4.7 ± 1.735.5 %5.09e+14 ± 1.99e+134 %Sw.avg
MBAS2.83 ± 3.64   (E)129 %7.0 ± 3.042.9 %5.09e+14 ± 2.00e+134 %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
(3749) Balam7.00 ± 3.0042.9 % H-mag2002D7 0.54 1
(3749) Balam4.65 ± 0.214.5 % NEATM2011D7212 0.49 2

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).

H-mag : Crude estimate from absolute magnitude. NEATM : Near-Earth Asteroid Thermal Model.


EVM diam. average D = (4.8 ± 0.57) km   (ΔD/D = 12%, SNR = 8.44) Derived bulk density ρ = (8.81 ± 3.15) g/cm3   (Δρ/ρ = 36%, SNR = 2.8)


References
D7(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.
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
(3749) Balam5.09e+14 ± 1.99e+134 %BinImg 2008M730.00 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).

BinImg : Binary imaged at optical wavelength.


EVM mass average M = (5.090 ± 0.199) × 1014 kg   (ΔM/M = 4%, SNR = 25.6) Derived bulk density ρ = (8.81 ± 3.15) g/cm3   (Δρ/ρ = 36%, SNR = 2.8)


References
M73(2008):Marchis, F., Descamps, P., Berthier, J., Hestroffer, D., Vachier, F., Baek, M., Harris, A.W., Nesvorný, D., 2008. Main belt binary asteroidal systems with eccentric mutual orbits. Icarus 195, 295–316.