Summary for : (66063) 1998 RO1

DynT.TT.BT T.L B T.DDensity (g/cm^3)Δρ/ρDiameter (km)ΔD/DMass (kg)ΔM/MRefAvg.M
NEA--- | --2.15 ± 1.56   (D)73 %0.7 ± 0.117.5 %3.60e+11 ± 1.80e+1150 %SEVM
NEA--- | --2.11 ± 1.53   (D)72 %0.7 ± 0.117.5 %3.60e+11 ± 1.80e+1150 %Sw.avg
NEAS2.79 ± 1.47   (D)53 %0.7 ± 0.116.2 %3.60e+11 ± 1.80e+1150 %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
1.5 ± 1.1576.7 %PheMu2009BD11
4.1 ± 1.8043.9 %PheMu2009BD11

PheMu : Mutual eclipsing phenomena in binary systems.
References
BD11(2009):Scheirich, P., Pravec, P., 2009. Modeling of lightcurves of binary asteroids. Icarus 200, 531-547.

Diameter estimates

DesignationDiameter / Err (km)ΔD/DMethodYearRefNχ2Use
(66063) 1998 RO10.56 ± 0.1628.6 % NEATM2008D43 0.60 1
(66063) 1998 RO10.80 ± 0.1518.7 % Radar2012D89 0.60 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).

NEATM : Near-Earth Asteroid Thermal Model. Radar : Radar imaging.


EVM diam. average D = (0.7 ± 0.12) km   (ΔD/D = 18%, SNR = 5.71) Derived bulk density ρ = (2.15 ± 1.56) g/cm3   (Δρ/ρ = 73%, SNR = 1.4)


References
D43(2008):Wolters, S.D., Green, S.F., McBride, N., Davies, J.K., 2008. Thermal infrared and optical observations of four near-Earth asteroids. Icarus 193, 535–552.
D89(2012):Benner (ref. ?). See: Carry, B., 2012. Density of asteroids. Planetary and Space Science, Volume 73, Issue 1, p. 98-118.

Mass estimates

DesignationMass / Err (kg)ΔM/MMethodYearRefNχ2Use
(66063) 1998 RO13.60e+11 ± 1.80e+1150 %PheMu 2009M830.00 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 = (3.600 ± 1.800) × 1011 kg   (ΔM/M = 50%, SNR = 2.0) Derived bulk density ρ = (2.15 ± 1.56) g/cm3   (Δρ/ρ = 73%, SNR = 1.4)


References
M83(2009):Scheirich, P., Pravec, P., 2009. Modeling of lightcurves of binary asteroids. Icarus 200, 531–547.