imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham Asteroid mass determination & Contribution to GR tests D. Hestroffer (IMCCE/Paris observatory)

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imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham Asteroid mass determination & Contribution to GR tests D. Hestroffer (IMCCE/Paris observatory) + S. Mouret, J Berthier (IMCCE), F. Mignard (OCA)

imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham Outline ● Gaia observation of asteroids (overview) ● Orbit improvement (precision) ● Determination of asteroids mass ● GR tests (local)

imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham Gaia Observation of Asteroids ● About 300,000 asteroids – (8 ≤) V ≤ 20 ● Scanning law – Observations around quadratures and to low elongations, including NEOs (or IEOs) ● 45° ≤ L ≤ 135° – No pointing, and varying sequences of observations ● Approx 50 observations per target over 5 years ● One-dimensional, sub-mas to mas precision

Gaia Observation of Asteroids 300,000

imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham Gaia Observation of Asteroids ● About 300,000 asteroids – (8 ≤) V ≤ 20, almost complete - but not for IEOs... ● Scanning law – Observations around quadratures and to low elongations, including NEOs (or IEOs) – No pointing, and varying sequences of observations ● One-dimensional, sub-mas to mas precision

Gaia Scanning Law ● Sun aspect  =45° ● Observations in a given range of elongations from L1 to L2

Gaia Scanning Law Observations distribution for the NEA Phaeton (a=1.27 e=0.9)

imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham Gaia Observation of Asteroids ● About 300,000 asteroids – (8 ≤) ≤ 20, almost complete - but not for IEOs... ● Scanning law – Observations around quadratures and to low elongations, including NEOs (or IEOs) ● 45° ≤ L ≤ 135° – No pointing, and varying sequences of observations ● Approx 50 observations per target over 5 years ● One-dimensional, sub-mas to mas precision

● Linearized least-squares, variance analysis ● A. dq = O-C = d  ● Jacobian matrix of PD A from ● analytical (2 body approximation, elliptic elements) ● variational equations (numerical integration, (x, dx/dt) ) ● Unknown correction vector dq=(dq i,dq g ) ● dq i per asteroid ● dq g global parameters Orbit Improvement

imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham Orbit Improvement (cont.) ● dq i per asteroid – osculating elements (da/a,de,dl o +dr, dp,dq,e.dr) – photocenter offset C(  ) = R.(a.  +b) – etc. ● dq g global parameters – global frame rotation (ecliptic and  ) – solar J 2 – GR – secular variations – asteroid mass m j, etc.

imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham Determination of Mass ● Masses from close approaches (binaries too) ● One massive perturber vs. several small targets

Determination of Mass ● About 100 potential perturbers ● Partial derivatives from variational equations. ● Exemple – dq for Mass only, over 5 years – one mass ( Ceres ) from 19 small targets – perturbations taken into account even if  (M) large

imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham Tests of GR ● Sensitivity of orbits e.d  dt ● Icarus, Phaeton ≈ Mercury (Sitarski) not radar though! ● ~1550 asteroids in present simulation 150 Trojans, 1200 MBAs, 200 NEAs   a (1-e 2 ).   a 2 (1-e 2 ) 2 Solar elongation limit

imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham ● PPN formalism – Local test ● Assuming  is known (Cassini, GAIA,...) ● Simultaneous determination of PPN  and solar quadrupole J 2 – Correlation (β+1/4e4.J 2, J 2 )=0.14 ● Rotation and rotation rate Tests of GR. 1,500 objects Mainly from NEAs

imcce.fr LISA/GAIA/SKA -- testing GR March '06 Birmingham Perspectives ● Some parameters depend on 1/√N – dJ2/dt possibly yr -1 – G/G in fact d(G.M)/dt possibly < yr -1 – Global rotation ● Consider extensive simulation with 300,000 objects (code to //) ● All PD from var. eqs. (no approx. from 2 body) ● Consider Nordtvedt  from Trojans (?, Orellana & Vucetictch), β 2 for dG (?..).