R1i ddlmZmZmZmZddlmZmZmZm Z ddl m Z m Z m Z gdZdddd d d d d dddd Z ddZdZdZdZy))abseinsumsqrtwhere)CAU_MC_AUDAYGS)_AVOID_DIVIDE_BY_ZEROdots length_of)sunjupitersaturnmoonvenusuranusneptuneglVAgq= .Ag4HRAg*GAged]@gS@gQ]@g(\@gA?gV3ƑyA) mercuryrearthmarsrrrrplutorrcRt|tz }|j}|j}td|D]} || } | j |j|jj} | |z } t|| } |}t| dkD|| z |}t|| k||z |}| j |j|jj} t| }t||| ||jr|d} | j |jjj} td}|j}t||| ||jr|dd|f|dd|f<y|dd|ddyy#t $r || dz} YhwxYw)aRUpdate `position` for how solar system masses will deflect its light. Given the ICRS `position` |xyz| of an object (au) that is being viewed from the `observer` also expressed as |xyz|, and given an ephemeris that can be used to determine solar system body positions, and given the time `t` and Boolean `apply_earth` indicating whether to worry about the effect of Earth's mass, and a `count` of how many major solar system bodies to worry about, this function updates `position` in-place to show how the masses in the solar system will deflect its image. Nz barycenter)jdr)rr tdbts deflectorsKeyErroratpositionaulight_time_differencerrmasses_add_deflectionanycopyshape)r#observer ephemeristinclude_earth_deflectioncounttltjd_tdbrname deflector bpositiongpvdlttclosermassdeflected_positions W/home/cursorai/projects/iching/venv/lib/python3.12/site-packages/skyfield/relativity.pyadd_deflectionr;s H  'CUUF B6E" 8!$I LL6!23<<?? (" $Hc2  sSy&3,7sSy&3,7 LL6!23<<??  (Iu=G#N ##%g& LL6!23<<??  &]]_*HiG # ) )"1%=#=> Q// 0-Q/HQK&I 8!$"67I 8sFF&%F&c\t|}||tzz }td||tz }|S)zReturns the difference in light-time, for a star, between the barycenter of the solar system and the observer (or the geocenter). z a...,a...)rr rr )r#observer_positiondisu1diflts r:r%r%bs9 H C S00 1B ;$5 6 @E Lc ||z|z }||z }t|}t|}t|}|t||dz } |t||dz } |t||dz } t| | } t| | } t| | }t|dkD}dtzt t z|zt z|zz }d| z}|t|d|| | z|| zz z|z |zz }y)ahCorrect a position vector for how one particular mass deflects light. Given the ICRS `position` |xyz| of an object (AU) together with the positions of an `observer` and a `deflector` of reciprocal mass `rmass`, this function updates `position` in-place to show how much the presence of the deflector will deflect the image of the object. rg(?g@rN)rrr rr rr )r#r+r3r8pqpepmagqmagemagphatqhatehatpdotqqdoteedotpmake_no_correctionfac1fac2s r:r'r'ts H y (B I B X D R=D R=D eD$, ,D dD#& &D dD#& &D t E t E t E Um3 8q1ut|d*U2 3D ;D (#edlUT\9:TADHJJHrAc|tz}t|}|tz }t||}|||ztzz }t d||zz }||z} d| d|zz z|z} d| z} ||z}|| |zz }|| z}y)aCorrect a relative position vector for aberration of light. Given the relative `position` |xyz| of an object (AU) from a particular observer, the `velocity` [dx,dy,dz] at which the observer is traveling (AU/day), and the light propagation delay `light_time` to the object (days), this function updates `position` in-place to give the object's apparent position due to the aberration of light. rN)r rr r r) r#velocity light_timep1magvemagbetadotcosdgammaipqrs r:add_aberrationr]s  E h E 7?D x "C %%-"77 8D #t # $F t A qC&L! !Z/A aA H H H MHrAN))numpyrrrr constantsrr r r functionsr r rr r&r;r%r'r]rAr:rcsc**++== O         45J0X$-J^rA