def apparent(self):
        """Compute an :class:`Apparent` position for this body.

        This applies two effects to the position that arise from
        relativity and shift slightly where the other body will appear
        in the sky: the deflection that the image will experience if its
        light passes close to large masses in the Solar System, and the
        aberration of light caused by the observer's own velocity.

        >>> earth.at(t).observe(mars).apparent()
        <Apparent position and velocity at date t>

        These transforms convert the position from the BCRS reference
        frame of the Solar System barycenter and to the reference frame
        of the observer.  In the specific case of an Earth observer, the
        output reference frame is the GCRS.

        """
        t = self.t
        position_au = self.position.au.copy()
        observer_data = self.observer_data
        gcrs_position = observer_data.gcrs_position

        if gcrs_position is None:
            include_earth_deflection = array((False,))
        else:
            limb_angle, nadir_angle = compute_limb_angle(
                position_au, gcrs_position)
            include_earth_deflection = nadir_angle >= 0.8

        add_deflection(position_au, observer_data.bcrs_position,
                       observer_data.ephemeris, t, include_earth_deflection)

        add_aberration(position_au, observer_data.bcrs_velocity,
                       self.light_time)

        return Apparent(position_au, t=t, observer_data=observer_data)
Compute an :class:`Apparent` position for this body.

        This applies two effects to the position that arise from
        relativity and shift slightly where the other body will appear
        in the sky: the deflection that the image will experience if its
        light passes close to large masses in the Solar System, and the
        aberration of light caused by the observer's own velocity.

        >>> earth.at(t).observe(mars).apparent()
        <Apparent position and velocity at date t>

        These transforms convert the position from the BCRS reference
        frame of the Solar System barycenter and to the reference frame
        of the observer.  In the specific case of an Earth observer, the
        output reference frame is the GCRS.