gaia asteroids simulations - filegaia asteroid simulations: from point-like to ellipsoidal objects...
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![Page 1: GAIA asteroids simulations - fileGAIA asteroid simulations: from point-like to ellipsoidal objects Helsinki May 27-28, 2004 P. Tanga, F. Mignard (OCA) A. Cellino (OATo, Turin) J. Berthier,](https://reader031.vdocument.in/reader031/viewer/2022021912/5c65816109d3f2a36e8ce856/html5/thumbnails/1.jpg)
GAIA asteroid simulations:from point-like to ellipsoidal objects
Helsinki May 27-28, 2004
P. Tanga, F. Mignard (OCA)A. Cellino (OATo, Turin)
J. Berthier, D. Hestroffer (IMCCE, Paris)
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Goal
Implementation of physical properties (shape, spin) in the existing detection simulation
Modeling of their effects on photometry and astrometry
Statistics not in contradiction with reality
Simplified calculations to preserve simulation speed
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Assumptions
Asteroids can be modelled as 3D-ellipsoids (at 1st order)
Regular rotation (constant spin, pole)
Radius and average absolute magnitude coming from the existing catalogues are reliable
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MethodsExploitation of existing databases:
Magnusson – Kryszczynska shape (b/a, c/a), (several records/object) period,
pole
Harris lightcurve parameters shape (b/a, c/a), period
Appropriate generation of missing data
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Magnusson database, selection criteria:
If several records exist, the most recent is retainedIf several poles exists in that record, a solution is chosen at randomIf the spin period associated to that solution exists, it is selectedIf there are estimates of the b/a, c/a ratios, they are used to compute the volume-equivalent ellipsoid axes
Lightcurve parameters (Harris):
Rotation period selected when not available from MagnussonTumbling asteroid periods discarded
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Generation of physical parameters - 1Poles : uniform random distribution on the skyRotational phases at t = 0 : uniform random distributionShapes :
size range (km) <∆m> ± σ
D > 200 0.188 ± 0.028
100 < D < 200 0.181 ± 0.011
50 < D < 100 0.206 ± 0.015
20 < D < 50 0.362 ± 0.057
D < 20 0.526 ± 0.059
b/a : ∆m ~ 2.5 log (a/b)
c/b = 1. - abs(η),
<η> = 0. ± 0.5
Tedesco & Zappalà 1985
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Generation of physical parameters - 2
PeriodsLarge asteroids (D > 30 km). Well fitted by a single Maxwellian. 150 m < D < 40 km. Non-maxwellian with excess both at large and small bodies.
Distribution fitted by multiple (4) maxwellians
(Donnison 2002)
Ω⎟⎟⎠
⎞⎜⎜⎝
⎛ Ω−
Ω=<Ω ∑
=
dDfk
iikk
1
2
2/3
2
...1...1 2exp2),,(
σσπϖδϖσ
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The physical parameters file
pole coordinatesrotation period
shape parameters
![Page 10: GAIA asteroids simulations - fileGAIA asteroid simulations: from point-like to ellipsoidal objects Helsinki May 27-28, 2004 P. Tanga, F. Mignard (OCA) A. Cellino (OATo, Turin) J. Berthier,](https://reader031.vdocument.in/reader031/viewer/2022021912/5c65816109d3f2a36e8ce856/html5/thumbnails/10.jpg)
From model to lightcurvesFor each detection :
(H,G) system average magnitude at given phase angle
Physical ephemeris computation orientation on the sky
Analytic computation of geometric shading fluctuations around the average
Advantages : phase – magnitude relation preservedfast computation
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An example21 Lutetia
(normalized for the Sun and Earth distance)
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Limitations (at present)
Each object has its H, but G is unique and fixed
No complex shapes
No satellites
Phase angle – amplitude relation poorly modelled (scattering not taken into account properly)
No poles « polarization »
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Future extensionsNEO
Different values of G
Effects on astrometry : simple model of photocenter displacement
Simple scattering effectsmodel of the amplitude-phase relationship
Satellites
…suggestions !