Summary for : (136199) Eris

DynT.TT.BT T.L B T.DDensity (g/cm^3)Δρ/ρDiameter (km)ΔD/DMass (kg)ΔM/MRefAvg.M
TNO--- | --2.29 ± 0.37   (B)16 %2402.9 ± 130.55.4 %1.66e+22 ± 2.00e+201 %SEVM
TNO--- | --2.50 ± 0.77   (C)31 %2332.7 ± 239.510.3 %1.66e+22 ± 2.00e+201 %Sw.avg
TNO-2.41 ± 0.23   (B)10 %2357.8 ± 75.23.2 %1.66e+22 ± 2.00e+201 %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
(136199) Eris3000.00 ± 200.006.7 % STM2006D3512 8.91 1
(136199) Eris2400.00 ± 100.004.2 % Img-PSF2006D28 0.00 2
(136199) Eris2657.00 ± 212.358.0 % NEATM2008D512 1.43 3
(136199) Eris2326.00 ± 12.000.5 % Occ2011D82 41.02 4
(136199) Eris2420.00 ± 109.004.5 % STM2012D8712 0.02 5
(136199) Eris2454.00 ± 117.004.8 % STM2012D872 0.19 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).

Img-PSF : Profile deviation from a Point-Spread Function. NEATM : Near-Earth Asteroid Thermal Model. Occ : Stellar occultation. STM : Standard Thermal Model.


EVM diam. average D = (2402.9 ± 130.47) km   (ΔD/D = 5%, SNR = 18.42) Derived bulk density ρ = (2.29 ± 0.37) g/cm3   (Δρ/ρ = 16%, SNR = 6.1)


References
D28(2006):Brown, M.E., Schaller, E.L., Roe, H.G., Rabinowitz, D.L., Trujillo, C.A., 2006. Direct Measurement of the Size of 2003 UB313 from the Hubble Space Telescope. Astrophysical Journal 643, L61–L63.
D35(2006):Bertoldi, F., Altenhoff, W., Weiss, A., Menten, K.M., Thum, C., 2006. The trans-neptunian object UB 313 is larger than Pluto. Nature 439, 563–564.
D51(2008):Stansberry, J., Grundy, W., Brown, M.E., Cruikshank, D.P., Spencer, J.R., Trilling, D., Margot, J.L., 2008. Physical Properties of Kuiper Belt and Centaur Objects: Constraints from the Spitzer Space Telescope. The Solar System Beyond Neptune , 161–179.
D82(2011):Sicardy, B., Ortiz, J.L., Assafin, M., Jehin, E., Maury, A., Lellouch, E., Hutton, R.G., Braga-Ribas, F., Colas, F., Hestroffer, D., Lecacheux, J., Roques, F., Santos-Sanz, P., Widemann, T., Morales, N., Duffard, R., Thirouin, A., Castro-Tirado, A.J., Jelı́nek, M., Kubánek, P., Sota, A., Sánchez-Ramı́rez, R., Andrei, A.H., Camargo, J.I.B., da Silva Neto, D.N., Gomes, A.R., Martins, R.V., Gillon, M., Manfroid, J., Tozzi, G.P., Harlingten, C., Saravia, S., Behrend, R., Mottola, S., Melendo, E.G., Peris, V., Fabregat, J., Madiedo, J.M., Cuesta, L., Eibe, M.T., Ullán, A., Organero, F., Pastor, S., de Los Reyes, J.A., Pedraz, S., Castro, A., de La Cueva, I., Muler, G., Steele, I.A., Cebrián, M., Montañés-Rodrı́guez, P., Oscoz, A., Weaver, D., Jacques, C., Corradi, W.J.B., Santos, F.P., Reis, W., Milone, A., Emilio, M., Gutiérrez, L., Vázquez, R., Hernández-Toledo, H., 2011. A Pluto-like radius and a high albedo for the dwarf planet Eris from an occultation. Nature 478, 493–496.
D87(2012):Santos Sanz, P., Lellouch, E., Fornasier, S., Kiss, C., Pál, A., Müller, T., Vilenius, E., Stansberry, J., Mommert, M., Delsanti, A., Mueller, M., Bönhardt, H., Peixinho, N., Henry, F., Ortiz, J.L., Thirouin, A., Protopapa, S., Duffard, R., Szalai, N., Lim, T., Ejeta, C., Hartogh, P., Harris, A.W., Rengel, M., 2012. TNOs are Cool: A Survey of the Transneptunian Region IV. Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel Space Observatory-PACS. Astronomy & Astrophysics, 541, id.A93, 18 pp.

Mass estimates

DesignationMass / Err (kg)ΔM/MMethodYearRefNχ2Use
(136199) Eris1.66e+22 ± 2.00e+201 %BinImg 2007M690.00 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 = (1.660 ± 0.020) × 1022 kg   (ΔM/M = 1%, SNR = 83.0) Derived bulk density ρ = (2.29 ± 0.37) g/cm3   (Δρ/ρ = 16%, SNR = 6.1)


References
M69(2007):Brown, M.E., Schaller, E.L., 2007. The Mass of Dwarf Planet Eris. Science 316, 1585–.