Lorentz symmetry violations can be parametrized by an effective field theory framework that contains both General Relativity and the Standard Model of particle physics, called the Standard-Model Extension or SME. We consider in this work only the pure gravitational sector of the minimal SME. We present new constraints on the SME coefficients obtained from lunar laser ranging, very long baseline interferometry, and planetary motions

Bailey, Q. G.

Bouquillon, S.

Bourgoin, A.

et al.,

Hees, A.

Lambert, S.

Le Poncin-Lafitte, C.

English

Embry-Riddle Aeronautical University

Publications 6-2016 Constraints on SME Coefficients from Lunar Laser Ranging, Very Long Baseline Interferometry, and Asteroid Orbital Dynamics C. Le Poncin-Lafitte SYRTE A. Bourgoin SYRTE A. Hees University of California, Los Angeles S. Bouquillon SYRTE S. Lambert SYRTE See next page for additional authors Follow this and additional works at: https://commons.erau.edu/publication  Part of the Astrophysics and Astronomy Commons Scholarly Commons Citation Le Poncin-Lafitte, C., Bourgoin, A., Hees, A., Bouquillon, S., Lambert, S., Bailey, Q. G., & et al. (2016). Constraints on SME Coefficients from Lunar Laser Ranging, Very Long Baseline Interferometry, and Asteroid Orbital Dynamics. , (). Retrieved from https://commons.erau.edu/publication/763 This Conference Proceeding is brought to you for free and open access by Scholarly Commons. It has been accepted for inclusion in Publications by an authorized administrator of Scholarly Commons. For more information, please contact commons@erau.edu. Authors C. Le Poncin-Lafitte, A. Bourgoin, A. Hees, S. Bouquillon, S. Lambert, Q. G. Bailey, and et al. This conference proceeding is available at Scholarly Commons: https://commons.erau.edu/publication/763 Proceedings of the Seventh Meeting on CPT and Lorentz Symmetry (CPT’16), Indiana University, Bloomington, June 20-24, 20161Constraints on SME Coefficients from Lunar Laser Ranging,Very Long Baseline Interferometry, andAsteroid Orbital DynamicsC. Le Poncin-Lafitte,1 A. Bourgoin,1 A. Hees,2 S. Bouquillon,1S. Lambert,1 G. Francou,1 M.-C. Angonin,1 Q.G. Bailey,3D. Hestroffer,4 P. David,4 F. Meynadier,1 and P. Wolf11SYRTE, Observatoire de Paris, PSL Research University, CNRSSorbonne Universite´s, UPMC Univ. Paris 06, LNE61 avenue de l’Observatoire, 75014 Paris, France2Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095, USA3Department of Physics, Embry-Riddle Aeronautical University3700 Willow Creek Road, Prescott, AZ 86301, USA4 IMCCE, Observatoire de Paris, PSL Research University, CNRSSorbonne Universite´s, UPMC Univ. Paris 06, Univ. de Lille77 avenue Denfert-Rochereau, 75014 Paris, FranceLorentz symmetry violations can be parametrized by an effective field theoryframework that contains both General Relativity and the Standard Model ofparticle physics, called the Standard-Model Extension or SME. We consider inthis work only the pure gravitational sector of the minimal SME. We presentnew constraints on the SME coefficients obtained from lunar laser ranging,very long baseline interferometry, and planetary motions.1. IntroductionThe solar system remains the most precise laboratory to test the theory ofgravity, that is to say General Relativity (GR). Constraints on deviationsfrom GR can only be obtained in an extended theoretical framework thatparametrizes such deviations. The parametrized post-Newtonian formalismis one of them and has been widely used for decades. More recently, otherphenomenological frameworks have been developed like the Standard-ModelExtension (SME), which is an extensive formalism that allows a system-atic description of Lorentz symmetry violations in all sectors of physics,including gravity. We present here new constraints on pure-gravity sectorcoefficients of the minimal SME obtained with very long baseline interfer-Proceedings of the Seventh Meeting on CPT and Lorentz Symmetry (CPT’16), Indiana University, Bloomington, June 20-24, 20162ometry (VLBI), lunar laser ranging (LLR) and planetary motions. We alsoassess the possibility to constrain them using future asteroids observationsby Gaia.2. Very long baseline interferometryVLBI is a geometric technique which measures the time difference in thearrival of a radio wavefront emitted by a distant radio source (typically aquasar) between at least two Earth-based radio telescopes, with a precisionof a few picoseconds. Although this technique is initially dedicated totracking the Earth’s rotation and enabling the realization of global referenceframes, it allows also performing fundamental physics tests by measuringthe relativistic bending of light rays due to the Sun and the planets.1,2Recently, the VLBI gravitational group delay has been derived in the SMEformalism (see Eqs. (7) and (10) from Ref. 3). Using observations betweenAugust 1979 and mid-2015 consisting of almost 6000 VLBI 24-hr sessions(corresponding to 10 million delays), we turned to a global solution inwhich we estimated s¯TT as a global parameter together with radio sourcecoordinates. We obtained3s¯TT = (−5± 8)× 10−5 , (1)with a global postfit rms of 28 ps and a χ2 per degree of freedom of 1.15.Correlations between radio source coordinates and s¯TT are lower than 0.02,the global estimate being consistent with the mean value obtained with thesession-wise solution with a slightly lower error.3. Lunar laser rangingSome years ago, a first estimate of SME coefficients with LLR data has beenobtained.4 However it was a fit of theoretical SME signatures in residuals ofLLR measurements analyzed previously in pure GR. This kind of approachis not fully satisfactory and provides order of magnitude upper limits onSME coefficients but not real estimates or constraints on them (see thediscussion in Ref. 3). Therefore, we built a new numerical lunar ephemeriscalled the Ephe´me´ride Lunaire Parisienne Nume´rique (ELPN) computedin the SME framework, taking into account effects of the SME on the or-bital dynamics and on the propagation of light.5 A global adjustment toLLR observations allows us to estimate properly some linear combinationsof SME coefficients, as illustrated in Table 1 (see also Ref. 6). Those con-straints take into account correlations between SME coefficients and otherProceedings of the Seventh Meeting on CPT and Lorentz Symmetry (CPT’16), Indiana University, Bloomington, June 20-24, 20163parameters (such as positions, velocities, masses, . . . ) and are more reliablethan the first analysis from Ref. 4.Table 1. Estimated values of SME coefficients obtained from LLR.6SME coefficients LLR estimation from Ref. 6s¯TX (−0.9± 1.0)× 10−8s¯XY (−5.7± 7.7) × 10−12s¯XZ (−2.2± 5.9) × 10−12s¯XX − s¯Y Y (+0.6± 4.2) × 10−11s¯TY + 0.43s¯TZ (+6.2± 7.9)× 10−9s¯Y Z − 22.2(s¯XX + s¯Y Y − 2s¯ZZ)(−0.5± 1.0)× 10−94. Gaia observations of solar system objectsLaunched in December 2013, the ESA Gaia mission is scanning the wholecelestial sphere once every 6 months providing high precision astrometricdata for a huge number (≈ 1 billion) of celestial bodies. In addition tostars, it is also observing solar system objects. In particular, about 360,000asteroids will regularly be observed at the sub-mas level. We simulated thetrajectories of 10,000 asteroids within the SME framework and performeda realistic covariance analysis taking into account the Gaia trajectory andscanning law (see Ref. 7 for more details about the strategy). The covari-ance analysis leads to the estimated uncertainties presented in Table 2 (seeRef. 8). These uncertainties are better than the current best estimationsof the SME parameters available in the literature.9 In particular, they arebetter than ones obtained with planetary ephemerides.10 This is due to thevariety of asteroid orbital parameters while planetary ephemerides use only8 planets with similar orbital parameters (same orbital planes and nearlycircular orbits). Therefore, the estimation of the SME coefficients withplanetary ephemerides are highly correlated, which degrades the marginal-ized SME estimates (see the discussion in Ref. 10). Using our set of as-teroids, the correlation matrix for the SME coefficients is very reasonable:the three most important correlation coefficients are 0.71, −0.68, and 0.46.All the other correlations are below 0.3. Therefore, Gaia offers a uniqueopportunity to constrain Lorentz violation through the SME formalism.5. ConclusionWe presented our latest constraints on gravity-sector SME coefficients ob-tained with LLR and VLBI observations. We highlighted also the improve-Proceedings of the Seventh Meeting on CPT and Lorentz Symmetry (CPT’16), Indiana University, Bloomington, June 20-24, 20164Table 2. Sensitivity on SME parame-ters.SME coefficients Sensitivitys¯XX − s¯Y Y 9× 10−12s¯XX + s¯Y Y − 2s¯ZZ 2× 10−11s¯XY 4× 10−12s¯XZ 2× 10−12s¯Y Z 4× 10−12s¯TX 1× 10−8s¯TY 2× 10−8s¯TZ 4× 10−8ment that we can expect from Gaia observations of asteroids in the future.A combined analysis with planetary ephemerides analysis,10 Lunar LaserRanging,4,6 atom interferometry,11 and binary pulsars12 would also be veryinteresting in order to decorrelate almost all gravity-sector SME coefficientsand produce the most stringent estimate on the SME coefficients. Our anal-ysis needs to be extended to include gravity-matter Lorentz violation in theSME framework.AcknowledgmentsQ.G.B. acknowledges financial support from the NSF Grant No. PHY-1402890 and from Sorbonne Universite´s through an “Emergence” grant.References1. S.B. Lambert and C. Le Poncin-Lafitte, Astron. Astrop. 499, 331 (2009).2. S.B. Lambert and C. Le Poncin-Lafitte, Astron. Astrop. 529, A70 (2011).3. C. Le Poncin-Lafitte, A. Hees, and S.B. Lambert, arXiv:1604.01663.4. J.B.R. Battat, J.F. Chandler, and C.W. Stubbs, Phys. Rev. Lett. 99, 241103(2007).5. Q.G. Bailey and V.A. Kostelecky´, Phys. Rev. D 74, 045001 (2006).6. A. Bourgoin, A. Hees, and S. Bouquillon, arXiv:1607.00294.7. S. Mouret, Phys. Rev. D 84, 122001 (2011).8. A. Hees, D. Hestroffer, C. Le Poncin-Lafitte, and P. David, in F. Martins etal., eds., Proceedings of the Annual Meeting of the French Society of Astron-omy and Astrophysics, SF2A, Toulouse, 2015.9. Data Tables for Lorentz and CPT Violation, V.A. Kostelecky´ and N. Russell,2016 edition, arXiv:0801.0287v9.10. A. Hees et al., Phys. Rev. D 92, 064049 (2015).11. H. Mu¨ller, S.-W. Chiow, S. Herrmann, S. Chu, and K.-Y. Chung, Phys. Rev.Lett. 100, 031101 (2008).12. L. Shao, Phys. Rev. Lett. 112, 111103 (2014).

Constraints on SME Coefficients from Lunar Laser Ranging, Very Long Baseline Interferometry, and Asteroid Orbital Dynamics

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Constraints on SME Coefficients from Lunar Laser Ranging, Very Long Baseline Interferometry, and Asteroid Orbital Dynamics

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