a ߙfbcO @sdZddlmZddlZddlZddlZddlm Z ddl m Z ddl m Z mZddlmZdd lmZdd lmZdd lmZdd lmZmZdd lmZmZmZm Z ddl!m"Z"gdZ#dZ$dgddgddgdgddgddgdgdgdgdgdgdgd Z%dd d!d"d#d$d%d&d'Z&d(dd)Z'Gd*d+d+eZ(d,d-Z)dBd/d0Z*dCd1d2Z+dDd3d4Z,dEd5d6Z-dFd7d8Z.dGd9d:Z/d;d<e01DD]"Z2e2jj3ee'd"dd=e2_qd>Z4ed?e4d@dAZ5dS)Hzc This module contains convenience functions for retrieving solar system ephemerides from jplephem. )urlparseN)SkyCoord) download_file) classproperty deprecated) ScienceState)indent)units)c)CartesianRepresentationCartesianDifferential)GCRSICRSITRSTETE)get_jd12)get_bodyget_moonget_body_barycentricget_body_barycentric_posvelsolar_system_ephemerisde430)r )rr)r)r)ri+)r)ri)ri-)r)r)r)r)r)r ) sunmercuryvenusearth-moon-barycenterearthmoonmarsjupitersaturnuranusneptuneZplutorrrrrr r!)r$r%r&r)r*r+r,r-a You can either give an explicit ephemeris or use a default, which is normally a built-in ephemeris that does not require ephemeris files. To change the default to be the JPL ephemeris:: >>> from astropy.coordinates import solar_system_ephemeris >>> solar_system_ephemeris.set('jpl') # doctest: +SKIP Use of any JPL ephemeris requires the jplephem package (https://pypi.org/project/jplephem/). If needed, the ephemeris file will be downloaded (and cached). One can check which bodies are covered by a given ephemeris using:: >>> solar_system_ephemeris.bodies ('earth', 'sun', 'moon', 'mercury', 'venus', 'earth-moon-barycenter', 'mars', 'jupiter', 'saturn', 'uranus', 'neptune') c@sHeZdZdZdZdZeddZeddZe dd Z e d d Z dS) raDefault ephemerides for calculating positions of Solar-System bodies. This can be one of the following:: - 'builtin': polynomial approximations to the orbital elements. - 'de430', 'de432s', 'de440', 'de440s': short-cuts for recent JPL dynamical models. - 'jpl': Alias for the default JPL ephemeris (currently, 'de430'). - URL: (str) The url to a SPK ephemeris in SPICE binary (.bsp) format. - PATH: (str) File path to a SPK ephemeris in SPICE binary (.bsp) format. - `None`: Ensure an Exception is raised without an explicit ephemeris. The default is 'builtin', which uses the ``epv00`` and ``plan94`` routines from the ``erfa`` implementation of the Standards Of Fundamental Astronomy library. Notes ----- Any file required will be downloaded (and cached) when the state is set. The default Satellite Planet Kernel (SPK) file from NASA JPL (de430) is ~120MB, and covers years ~1550-2650 CE [1]_. The smaller de432s file is ~10MB, and covers years 1950-2050 [2]_ (and similarly for the newer de440 and de440s). Older versions of the JPL ephemerides (such as the widely used de200) can be used via their URL [3]_. .. [1] https://naif.jpl.nasa.gov/pub/naif/generic_kernels/spk/planets/aareadme_de430-de431.txt .. [2] https://naif.jpl.nasa.gov/pub/naif/generic_kernels/spk/planets/aareadme_de432s.txt .. [3] https://naif.jpl.nasa.gov/pub/naif/generic_kernels/spk/planets/a_old_versions/ builtinNcCs|dur|jS|||SN)_value get_kernel)clsvaluer5?lib/python3.9/site-packages/astropy/coordinates/solar_system.pyvalidatems zsolar_system_ephemeris.validatecCsV|jdus|jj|krP|jdur4|jjjd|_t|}|durJ||_||_|jSr0)_kernelorigindaffileclose _get_kernel)r3r4kernelr5r5r6r2vs z!solar_system_ephemeris.get_kernelcCs ||jSr0)r2r1r3r5r5r6r>szsolar_system_ephemeris.kernelcCs<|jdurdS|jdkr,dttSttSdS)Nr/)r'r#r()r1lowertuple PLAN94_BODY_NAME_TO_PLANET_INDEXkeysBODY_NAME_TO_KERNEL_SPECr?r5r5r6bodiess  zsolar_system_ephemeris.bodies) __name__ __module__ __qualname____doc__r1r8 classmethodr7r2rr>rEr5r5r5r6rMs   rcCs|dus|dkrdSzddlm}WntyBtdYn0|dkrTt}|dvrpd|}nDtj|r| |Sz t |Wn t yt d |Yn0| t |d d S) z Try importing jplephem, download/retrieve from cache the Satellite Planet Kernel corresponding to the given ephemeris. Nr/r)SPKziSolar system JPL ephemeris calculations require the jplephem package (https://pypi.org/project/jplephem/)Zjpl)rZde432sZde440Zde440szGhttps://naif.jpl.nasa.gov/pub/naif/generic_kernels/spk/planets/{:s}.bspzT{} was not one of the standard strings and could not be parsed as a file path or URLT)cache)r@Z jplephem.spkrK ImportErrorDEFAULT_JPL_EPHEMERISformatospathisfileopenr Exception ValueErrorr)r4rKr5r5r6r=s*        r=TcCs|dup|tju}d}z|r:tdur2tttj}nt|}t|d\}}|durB|}t ||\}} |dkr| } n|dkrt ||} t | | } ndt | |} |dkr| } nJz t|} Wn"tytd||Yn0t ||| }t || } t| dtjdd d }|rt| d tjtjdd d }ndt|trzt|}Wn$tytd ||Yn0n|}t|d d}t|dkr||}}t|rdnddft|d d}|D]~}||}|jdkr4|||}|r|| |j!7}n|d|dd7<n&t"||#||D]\}}||7}qFq|j!dd||_!t|dtj$d d}|rt|dtj$tjd d}|r||fn|W|s|dur|j%j&'Sn|s|dur|j%j&'0dS)aCalculate the barycentric position (and velocity) of a solar system body. Parameters ---------- body : str or other The solar system body for which to calculate positions. Can also be a kernel specifier (list of 2-tuples) if the ``ephemeris`` is a JPL kernel. time : `~astropy.time.Time` Time of observation. ephemeris : str, optional Ephemeris to use. By default, use the one set with ``astropy.coordinates.solar_system_ephemeris.set`` get_velocity : bool, optional Whether or not to calculate the velocity as well as the position. Returns ------- position : `~astropy.coordinates.CartesianRepresentation` or tuple Barycentric (ICRS) position or tuple of position and velocity. Notes ----- Whether or not velocities are calculated makes little difference for the built-in ephemerides, but for most JPL ephemeris files, the execution time roughly doubles. NZtdbr'r(r#zH{}'s position and velocity cannot be calculated with the '{}' ephemeris.pr.F)unitZxyz_axiscopyvz9{}'s position cannot be calculated with the {} ephemeris.shaper5rrrrr)rWrX)(rr1getrU_EPHEMERIS_NOTEr>r=rr@erfaZepv00Zmoon98ZpvppvZpvmpvrBKeyErrorrOZplan94r uZauZday isinstancestrrDgetattrlenZravelnpZzerosZ data_typeZcomputeZreshaperZzipZgenerateZkmr:r;r<)bodytime ephemeris get_velocityZdefault_kernelr>Zjd1Zjd2Zearth_pv_helioZ earth_pv_baryZ body_pv_baryZ moon_pv_geoZ sun_pv_baryZ body_indexZ body_pv_helioZ body_pos_baryZ body_vel_baryZ kernel_specZ jd1_shapeZbody_posvel_baryZpairZspkZposvelZ body_p_or_vZp_or_vr5r5r6_get_body_barycentric_posvels                  rjcCs t|||S)aCalculate the barycentric position and velocity of a solar system body. Parameters ---------- body : str or list of tuple The solar system body for which to calculate positions. Can also be a kernel specifier (list of 2-tuples) if the ``ephemeris`` is a JPL kernel. time : `~astropy.time.Time` Time of observation. ephemeris : str, optional Ephemeris to use. By default, use the one set with ``astropy.coordinates.solar_system_ephemeris.set`` Returns ------- position, velocity : tuple of `~astropy.coordinates.CartesianRepresentation` Tuple of barycentric (ICRS) position and velocity. See Also -------- get_body_barycentric : to calculate position only. This is faster by about a factor two for JPL kernels, but has no speed advantage for the built-in ephemeris. Notes ----- {_EPHEMERIS_NOTE} rjrfrgrhr5r5r6r7srcCst|||ddS)a*Calculate the barycentric position of a solar system body. Parameters ---------- body : str or list of tuple The solar system body for which to calculate positions. Can also be a kernel specifier (list of 2-tuples) if the ``ephemeris`` is a JPL kernel. time : `~astropy.time.Time` Time of observation. ephemeris : str, optional Ephemeris to use. By default, use the one set with ``astropy.coordinates.solar_system_ephemeris.set`` Returns ------- position : `~astropy.coordinates.CartesianRepresentation` Barycentric (ICRS) position of the body in cartesian coordinates See Also -------- get_body_barycentric_posvel : to calculate both position and velocity. Notes ----- {_EPHEMERIS_NOTE} F)rirkrlr5r5r6rXsrc Cs|durt}dtj}|}dtj}td||}|durD||7}tt|dtjkrt|||}||} || t }| t }||}qDt|||S)aCalculate the apparent position of body ``body`` relative to Earth. This corrects for the light-travel time to the object. Parameters ---------- body : str or other The solar system body for which to calculate positions. Can also be a kernel specifier (list of 2-tuples) if the ``ephemeris`` is a JPL kernel. time : `~astropy.time.Time` Time of observation. ephemeris : str, optional Ephemeris to use. By default, use the one set with ``~astropy.coordinates.solar_system_ephemeris.set`` obsgeoloc : `~astropy.coordinates.CartesianRepresentation`, optional The GCRS position of the observer Returns ------- cartesian_position : `~astropy.coordinates.CartesianRepresentation` Barycentric (ICRS) apparent position of the body in cartesian coordinates Notes ----- {_EPHEMERIS_NOTE} Ng4@gr'g:0yE>) rr[r_srrdanyZfabsZnormspeed_of_light) rfrgrh obsgeolocZdelta_light_travel_timeZ emitted_timeZlight_travel_timeZ earth_locZbody_locZearth_distancer5r5r6_get_apparent_body_positionxs"      rqc Cs`|dur|j}|dur&||\}}nd\}}t||||}t|}|t|||d}t|S)a Get a `~astropy.coordinates.SkyCoord` for a solar system body as observed from a location on Earth in the `~astropy.coordinates.GCRS` reference system. Parameters ---------- body : str or list of tuple The solar system body for which to calculate positions. Can also be a kernel specifier (list of 2-tuples) if the ``ephemeris`` is a JPL kernel. time : `~astropy.time.Time` Time of observation. location : `~astropy.coordinates.EarthLocation`, optional Location of observer on the Earth. If not given, will be taken from ``time`` (if not present, a geocentric observer will be assumed). ephemeris : str, optional Ephemeris to use. If not given, use the one set with ``astropy.coordinates.solar_system_ephemeris.set`` (which is set to 'builtin' by default). Returns ------- skycoord : `~astropy.coordinates.SkyCoord` GCRS Coordinate for the body Notes ----- The coordinate returned is the apparent position, which is the position of the body at time *t* minus the light travel time from the *body* to the observing *location*. {_EPHEMERIS_NOTE} N)NN)obstimerp obsgeovel)locationZget_gcrs_posvelrqr transform_torr) rfrgrtrhrprsZcartrepZicrsZgcrsr5r5r6rs#rcCstd|||dS)a Get a `~astropy.coordinates.SkyCoord` for the Earth's Moon as observed from a location on Earth in the `~astropy.coordinates.GCRS` reference system. Parameters ---------- time : `~astropy.time.Time` Time of observation location : `~astropy.coordinates.EarthLocation` Location of observer on the Earth. If none is supplied, taken from ``time`` (if not present, a geocentric observer will be assumed). ephemeris : str, optional Ephemeris to use. If not given, use the one set with ``astropy.coordinates.solar_system_ephemeris.set`` (which is set to 'builtin' by default). Returns ------- skycoord : `~astropy.coordinates.SkyCoord` GCRS Coordinate for the Moon Notes ----- The coordinate returned is the apparent position, which is the position of the moon at time *t* minus the light travel time from the moon to the observing *location*. {_EPHEMERIS_NOTE} r()rtrh)r)rgrtrhr5r5r6rs rcCs,g|]$}t|r|jdurd|jvr|qS)Nz{_EPHEMERIS_NOTE})callablerI).0fr5r5r6 s ry)r\z The use of _apparent_position_in_true_coordinates is deprecated because astropy now implements a True Equator True Equinox Frame (TETE), which should be used instead. z4.2cCsbt|dd}|durJ|jdt|ji}t||jdt |jdj }t |j|d}||S)z Convert Skycoord in GCRS frame into one in which RA and Dec are defined w.r.t to the true equinox and poles of the Earth rtNrm)rr)rrrt) rbrpZwith_differentialsr Zfrom_cartesianrsrrrrurZearth_locationr)ZskycoordrtZgcrs_repZ tete_framer5r5r6&_apparent_position_in_true_coordinatess  rz)NT)N)N)N)NN)NN)6rIZ urllib.parseros.pathrPZnumpyrdr]Zsky_coordinaterZastropy.utils.datarZastropy.utils.decoratorsrrZastropy.utils.staterZ astropy.utilsr Zastropyr r_Zastropy.constantsr roZrepresentationr r Zbuiltin_framesrrrrZbuiltin_frames.utilsr__all__rNrDrBr\rr=rjrrrqrrlocalsvaluesrxrOZdeprecation_msgrzr5r5r5r6sr         F#  ! 1 4 %