Source code for astropy.coordinates.builtin_frames.itrs

# Licensed under a 3-clause BSD style license - see LICENSE.rst

from astropy.coordinates.attributes import EarthLocationAttribute, TimeAttribute
from astropy.coordinates.baseframe import BaseCoordinateFrame, base_doc
from astropy.coordinates.representation import (
    CartesianDifferential,
    CartesianRepresentation,
)
from astropy.utils.decorators import format_doc

from .utils import DEFAULT_OBSTIME, EARTH_CENTER

__all__ = ["ITRS"]

doc_footer = """
    Other parameters
    ----------------
    obstime : `~astropy.time.Time`
        The time at which the observation is taken.  Used for determining the
        position of the Earth and its precession.
    location : `~astropy.coordinates.EarthLocation`
        The location on the Earth.  This can be specified either as an
        `~astropy.coordinates.EarthLocation` object or as anything that can be
        transformed to an `~astropy.coordinates.ITRS` frame. The default is the
        centre of the Earth.
"""


[docs]@format_doc(base_doc, components="", footer=doc_footer) class ITRS(BaseCoordinateFrame): """ A coordinate or frame in the International Terrestrial Reference System (ITRS). This is approximately a geocentric system, although strictly it is defined by a series of reference locations near the surface of the Earth (the ITRF). For more background on the ITRS, see the references provided in the :ref:`astropy:astropy-coordinates-seealso` section of the documentation. This frame also includes frames that are defined *relative* to the center of the Earth, but that are offset (in both position and velocity) from the center of the Earth. You may see such non-geocentric coordinates referred to as "topocentric". Topocentric ITRS frames are convenient for observations of near Earth objects where stellar aberration is not included. One can merely subtract the observing site's EarthLocation geocentric ITRS coordinates from the object's geocentric ITRS coordinates, put the resulting vector into a topocentric ITRS frame and then transform to `~astropy.coordinates.AltAz` or `~astropy.coordinates.HADec`. The other way around is to transform an observed `~astropy.coordinates.AltAz` or `~astropy.coordinates.HADec` position to a topocentric ITRS frame and add the observing site's EarthLocation geocentric ITRS coordinates to yield the object's geocentric ITRS coordinates. On the other hand, using ``transform_to`` to transform geocentric ITRS coordinates to topocentric ITRS, observed `~astropy.coordinates.AltAz`, or observed `~astropy.coordinates.HADec` coordinates includes the difference between stellar aberration from the point of view of an observer at the geocenter and stellar aberration from the point of view of an observer on the surface of the Earth. If the geocentric ITRS coordinates of the object include stellar aberration at the geocenter (e.g. certain ILRS ephemerides), then this is the way to go. Note to ILRS ephemeris users: Astropy does not currently consider relativistic effects of the Earth's gravatational field. Nor do the `~astropy.coordinates.AltAz` or `~astropy.coordinates.HADec` refraction corrections compute the change in the range due to the curved path of light through the atmosphere, so Astropy is no substitute for the ILRS software in these respects. """ default_representation = CartesianRepresentation default_differential = CartesianDifferential obstime = TimeAttribute(default=DEFAULT_OBSTIME) location = EarthLocationAttribute(default=EARTH_CENTER) @property def earth_location(self): """ The data in this frame as an `~astropy.coordinates.EarthLocation` class. """ from astropy.coordinates.earth import EarthLocation cart = self.represent_as(CartesianRepresentation) return EarthLocation(x=cart.x, y=cart.y, z=cart.z)
# Self-transform is in intermediate_rotation_transforms.py with all the other # ITRS transforms