Open Access
Table B.1
Methods included in SsODNet.
| Method | Name | Description | Reference |
|---|---|---|---|
| SPACE | Rendez-vous with a spacecraft | The results are based on data which had an encounter (flyby or orbit) with the target | Belton et al. (1992) |
| STM | Standard Thermal Model | Diameter and albedo derived by fitting mid-infrared data with a simple thermal model of non-rotating spheres | Lebofsky et al. (1986) |
| NEATM | Near-Earth Asteroid Thermal Model | Diameter, albedo, beaming derived by fitting mid-infrared data with a simple thermal model | Harris & Davies (1999) |
| TPM | ThermoPhysical Model | Diameter, albedo, thermal inertia derived by fitting mid-infrared data with a thermal model taking into account the spin, shape of the target | Lagerros (1996) |
| PhaseFunction | Albedo determined from the phase function | Albedo determined from the phase function | Belskaya & Shevchenko (2000) |
| LC | Lightcurve | Rotation period determined from optical light curves | Zessewitsch (1932) |
| Comet-Break | Mass from break-up | Mass estimated from the break-up of the comet | Solem (1994) |
| FRM | Fast Rotating Model | Diameter and albedo derived by fitting mid-infrared data with a simple thermal model of rapidly non-rotating spheres | Lebofsky & Spencer (1989) |
| NESTM | Night Emission Simulated Thermal Model | Diameter, albedo, beaming derived by fitting mid-infrared data with an adapted NEATM | Wolters & Green (2009) |
| Speckle | Triaxial ellipsoid from speckle interferometry | 3D shape modeled as tri-axial ellipsoid using speckle interferometry | Drummond et al. (1985) |
| Interferometry | Optical and Infrared Interferometry | Diameter derived from interferometric visibilities in the optical or infrared | Delbò et al. (2009) |
| Occ | Stellar Occultation | Apparent size measured during a stellar occultation | Dunham & Mallen (1979) |
| IM | Apparent shape from direct imaging | Apparent size/shape measured on disk-resolved images | Marchis et al. (2006) |
| IM-PSF | Diameter from PSF deviation | Estimate of diameter from the deviation of the PSF compared with a star | Brown & Trujillo (2004) |
| TE-IM | Triaxial ellipsoid from disk-resolved imaging | 3D shape modeled as tri-axial ellipsoid using disk-resolved images | Drummond (2000) |
| TE-Occ | Triaxial ellipsoid from stellar occultation | 3D shape modeled as tri-axial ellipsoid using stellar occultations | Drummond & Cocke (1989) |
| ADAM | All-Data Asteroid Model | 3D shape model obtained from a combined use of stellar occultations, optical light curves, disk-resolved images, interferometric fringes | Viikinkoski et al. (2015) |
| KOALA | Knitted Occultation, Adaptive-optics, and Lightcurves Analysis | The results are obtained from the combined use of stellar occultation, optical light curves, and disk-resolved images | Carry et al. (2010) |
| Radar | Radar shape modeling | 3D shape model based on radar Delay-Doppler data | Hudson & Ostro (1994) |
| Radar-LC | Combined radar and light curve shape modeling | 3D shape model based on radar Delay-Doppler and optical light curve data | Hudson et al. (1997) |
| SAGE | Shaping Asteroids with Genetic Evolution | 3D shape model based on light curves, found by genetic evolution | Bartczak & Dudzmski (2018) |
| Polarimetry | Albedo determined from polarimetry | Albedo determined from polarimetry | Cellino et al. (1999) |
| A-M | Amplitude-Magnitude | Determination of the spin axis from the amplitude of light curves | Zappala et al. (1983) |
| TE | Triaxial ellipsoid from light curves | Determination of the spin axis, modeling the light curves with a triaxial ellipsoid | Hanuš et al. (2021) |
| LCI | Lightcurve Inversion | Spin and convex 3-D shape determined from optical light curves | Kaasalainen & Torppa (2001) |
| LC+Occ | Scaling of Lightcurve Inversion Model with Stellar Occultations | 3D shape model from light-curve inversion scaled using stellar occultation(s) | Ďurech et al. (2011) |
| LC+IM | Scaling of Lightcurve Inversion Model with direct imaging | 3D shape model from a light-curve inversion scaled using disk-resolved image(s) | Hanuš et al. (2013b) |
| LC+TPM | Scaling of light-curve inversion model with the thermophysical model | 3D shape model from a light-curve inversion scaled using a thermophysical model on mid-infrared data | Hanuš et al. (2015) |
| LC-TPM | Combined light-curve inversion and thermophysical modeling | 3D shape modeling from simultaneous a light-curve inversion and thermophysical model of mid-infrared data | Ďurech et al. (2017) |
| EPHEM | Mass from ephemerides | The mass is determined from general ephemerides of the Solar System | Baer & Chesley (2008) |
| DEFLECT | Mass from close encounter deflection | The mass is determined from the orbital deflection of smaller asteroids | Standish & Hellings (1989) |
| Bin-IM | Mass from optical imaging a binary system | Mass from a binary system imaged in the optical | Merline et al. (1999) |
| Bin-Radar | Mass from radar observations of a binary system | Mass from a binary system observed by radar echoes | Ostro et al. (2006) |
| Bin-PheMu | Mass from mutual phenomena in a binary system | Mass from a binary system from the timings and shape of mutual event from light curves | Pravec et al. (2000) |
| Bin-Genoid | Orbit and mass from a multiple asteroidal system using Genoid algorithm | Orbital elements and mass determination from a multiple asteroidal system with Genoid | Vachier et al. (2012) |
| Yarkovsky | Mass from Yarkovsky drift | Determination of the mass from the measured Yarkovsky drift | Chesley et al. (2014) |
| Comet-NGF | Mass from non-gravitational forces | Mass estimated from the non-gravitational acceleration | Davidsson et al. (2007) |
| Spec | Reflectance spectroscopy | Reflectance spectroscopy | McCord et al. (1970) |
| Phot | Multi-filter photometry | Multi-band photometry | DeMeo & Carry (2013) |
| Astrometry(O) | Yarkovsky drift from optical astrometry | Determination of the semi-major drift due to Yarkovsky using astrometry from optical observations | Chesley et al. (2003) |
| Astrometry(O+R) | Yarkovsky drift from optical astrometry and radar delays | Determination of the semi-major drift due to Yarkovsky using astrometry from optical observations and radar delays | Chesley et al. (2003) |
| Family_age | Yarkovsky drift from family age | Determination of the semi-major drift due to Yarkovsky using the age of the dynamical family | Carruba et al. (2017) |
| HCM | Hierarchical Clustering Method | Determination of family membership by hierarchical clustering of proper elements | Zappala et al. (1990) |
| V-Shape | Yarkovsky V-shape identification of asteroid families | Determination of family membership by identification of the Yarkovsky print in (semi-major axis, 1/diameter) plane | Bolin et al. (2017) |
| abs | Colors derived from absolute magnitudes | Colors computed from the absolute magnitudes in the two filters | Mahlke et al. (2021) |
| lc_cor | Colors derived from apparent magnitudes corrected for light curves | Colors computed from the apparent magnitudes, corrected for short-term variability introduced by light curves | Erasmus et al. (2019) |
| app | Colors derived from apparent magnitudes | Colors computed from the apparent magnitudes | Sykes et al. (2000) |
| Yarkovsky_drift | Thermal inertia derived from Yarkovsky drift | Determination of the thermal inertia based on the measured strength of the Yarkovsky effect | Fenucci et al. (2021) |
| serendipitous | Phase curve from serendipitous observations | Determination of the parameters of the phase function from serendipitous observations (from surveys) | Oszkiewicz et al. (2011) |
| targeted | Phase curve from targeted observations | Determination of the parameters of the phase function from targeted observations (generally a reduction to the light curve maxima) | Gehrels (1956) |
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