pygaia/astrometry/vectorastrometry.py
def astrometryToPhaseSpace(phi, theta, parallax, muphistar, mutheta, vrad):
  """
  From the input astrometric parameters calculate the phase space coordinates. The output phase space
  coordinates represent barycentric (i.e. centred on the Sun) positions and velocities.

  This function has no mechanism to deal with units. The code is set up such that for input astrometry
  with parallaxes and proper motions in mas and mas/yr, and radial velocities in km/s, the phase space
  coordinates are in pc and km/s. For input astrometry with parallaxes and proper motions in muas and
  muas/yr, and radial velocities in km/s, the phase space coordinates are in kpc and km/s. Only positive
  parallaxes are accepted, an exception is thrown if this condition is not met.

  NOTE that the doppler factor k=1/(1-vrad/c) is NOT used in the calculations. This is not a problem for
  sources moving at typical velocities of Galactic stars.

  THIS FUNCTION SHOULD NOT BE USED WHEN THE PARALLAXES HAVE RELATIVE ERRORS LARGER THAN ABOUT 20 PER CENT
  (see http://arxiv.org/abs/1507.02105 for example). For astrometric data with relatively large parallax
  errors you should consider doing your analysis in the data space and use forward modelling of some
  kind.

  Parameters
  ----------

  phi       - The longitude-like angle of the position of the source (radians).
  theta     - The latitude-like angle of the position of the source (radians).
  parallax  - The parallax of the source (in mas or muas, see above)
  muphistar - The proper motion in the longitude-like angle, multiplied by cos(theta) (mas/yr or muas/yr,
  see above)
  mutheta   - The proper motion in the latitude-like angle (mas/yr or muas/yr, see above)
  vrad      - The radial velocity (km/s)

  Returns
  -------

  x - The x component of the barycentric position vector (in pc or kpc).
  y - The y component of the barycentric position vector (in pc or kpc).
  z - The z component of the barycentric position vector (in pc or kpc).
  vx - The x component of the barycentric velocity vector (in km/s).
  vy - The y component of the barycentric velocity vector (in km/s).
  vz - The z component of the barycentric velocity vector (in km/s).
  """
  if any(parallax<=0.0):
    raise Exception("One or more of the input parallaxes is non-positive")
  x, y, z = sphericalToCartesian(_auMasParsec/parallax, phi, theta)
  p, q, r = normalTriad(phi, theta)
  transverseMotionArray = array([muphistar*_auKmYearPerSec/parallax, mutheta*_auKmYearPerSec/parallax,
    vrad])
  if isscalar(parallax):
    velocityArray=dot(transpose(array([p, q, r])),transverseMotionArray)
    vx = velocityArray[0]
    vy = velocityArray[1]
    vz = velocityArray[2]
  else:
    vx = zeros_like(parallax)
    vy = zeros_like(parallax)
    vz = zeros_like(parallax)
    for i in range(parallax.size):
      velocityArray = dot(transpose(array([p[:,i], q[:,i], r[:,i]])), transverseMotionArray[:,i])
      vx[i] = velocityArray[0]
      vy[i] = velocityArray[1]
      vz[i] = velocityArray[2]
  return x, y, z, vx, vy, vz
def astrometryToPhaseSpace(phi, theta, parallax, muphistar, mutheta, vrad):
  """
  From the input astrometric parameters calculate the phase space coordinates. The output phase space
  coordinates represent barycentric (i.e. centred on the Sun) positions and velocities.

  This function has no mechanism to deal with units. The code is set up such that for input astrometry
  with parallaxes and proper motions in mas and mas/yr, and radial velocities in km/s, the phase space
  coordinates are in pc and km/s. For input astrometry with parallaxes and proper motions in muas and
  muas/yr, and radial velocities in km/s, the phase space coordinates are in kpc and km/s. Only positive
  parallaxes are accepted, an exception is thrown if this condition is not met.

  NOTE that the doppler factor k=1/(1-vrad/c) is NOT used in the calculations. This is not a problem for
  sources moving at typical velocities of Galactic stars.

  THIS FUNCTION SHOULD NOT BE USED WHEN THE PARALLAXES HAVE RELATIVE ERRORS LARGER THAN ABOUT 20 PER CENT
  (see http://arxiv.org/abs/1507.02105 for example). For astrometric data with relatively large parallax
  errors you should consider doing your analysis in the data space and use forward modelling of some
  kind.

  Parameters
  ----------

  phi       - The longitude-like angle of the position of the source (radians).
  theta     - The latitude-like angle of the position of the source (radians).
  parallax  - The parallax of the source (in mas or muas, see above)
  muphistar - The proper motion in the longitude-like angle, multiplied by cos(theta) (mas/yr or muas/yr,
  see above)
  mutheta   - The proper motion in the latitude-like angle (mas/yr or muas/yr, see above)
  vrad      - The radial velocity (km/s)

  Returns
  -------

  x - The x component of the barycentric position vector (in pc or kpc).
  y - The y component of the barycentric position vector (in pc or kpc).
  z - The z component of the barycentric position vector (in pc or kpc).
  vx - The x component of the barycentric velocity vector (in km/s).
  vy - The y component of the barycentric velocity vector (in km/s).
  vz - The z component of the barycentric velocity vector (in km/s).
  """
  if any(parallax<=0.0):
    raise Exception("One or more of the input parallaxes is non-positive")
  x, y, z = sphericalToCartesian(_auMasParsec/parallax, phi, theta)
  p, q, r = normalTriad(phi, theta)
  transverseMotionArray = array([muphistar*_auKmYearPerSec/parallax, mutheta*_auKmYearPerSec/parallax,
    vrad])
  if isscalar(parallax):
    velocityArray=dot(transpose(array([p, q, r])),transverseMotionArray)
    vx = velocityArray[0]
    vy = velocityArray[1]
    vz = velocityArray[2]
  else:
    vx = zeros_like(parallax)
    vy = zeros_like(parallax)
    vz = zeros_like(parallax)
    for i in range(parallax.size):
      velocityArray = dot(transpose(array([p[:,i], q[:,i], r[:,i]])), transverseMotionArray[:,i])
      vx[i] = velocityArray[0]
      vy[i] = velocityArray[1]
      vz[i] = velocityArray[2]
  return x, y, z, vx, vy, vz
def astrometryToPhaseSpace ( phi , theta , parallax , muphistar , mutheta , vrad ) : if any ( parallax <= 0.0 ) : raise Exception ( "One or more of the input parallaxes is non-positive" ) x , y , z = sphericalToCartesian ( _auMasParsec / parallax , phi , theta ) p , q , r = normalTriad ( phi , theta ) transverseMotionArray = array ( [ muphistar * _auKmYearPerSec / parallax , mutheta * _auKmYearPerSec / parallax , vrad ] ) if isscalar ( parallax ) : velocityArray = dot ( transpose ( array ( [ p , q , r ] ) ) , transverseMotionArray ) vx = velocityArray [ 0 ] vy = velocityArray [ 1 ] vz = velocityArray [ 2 ] else : vx = zeros_like ( parallax ) vy = zeros_like ( parallax ) vz = zeros_like ( parallax ) for i in range ( parallax . size ) : velocityArray = dot ( transpose ( array ( [ p [ : , i ] , q [ : , i ] , r [ : , i ] ] ) ) , transverseMotionArray [ : , i ] ) vx [ i ] = velocityArray [ 0 ] vy [ i ] = velocityArray [ 1 ] vz [ i ] = velocityArray [ 2 ] return x , y , z , vx , vy , vz
From the input astrometric parameters calculate the phase space coordinates. The output phase space
  coordinates represent barycentric (i.e. centred on the Sun) positions and velocities.

  This function has no mechanism to deal with units. The code is set up such that for input astrometry
  with parallaxes and proper motions in mas and mas/yr, and radial velocities in km/s, the phase space
  coordinates are in pc and km/s. For input astrometry with parallaxes and proper motions in muas and
  muas/yr, and radial velocities in km/s, the phase space coordinates are in kpc and km/s. Only positive
  parallaxes are accepted, an exception is thrown if this condition is not met.

  NOTE that the doppler factor k=1/(1-vrad/c) is NOT used in the calculations. This is not a problem for
  sources moving at typical velocities of Galactic stars.

  THIS FUNCTION SHOULD NOT BE USED WHEN THE PARALLAXES HAVE RELATIVE ERRORS LARGER THAN ABOUT 20 PER CENT
  (see http://arxiv.org/abs/1507.02105 for example). For astrometric data with relatively large parallax
  errors you should consider doing your analysis in the data space and use forward modelling of some
  kind.

  Parameters
  ----------

  phi       - The longitude-like angle of the position of the source (radians).
  theta     - The latitude-like angle of the position of the source (radians).
  parallax  - The parallax of the source (in mas or muas, see above)
  muphistar - The proper motion in the longitude-like angle, multiplied by cos(theta) (mas/yr or muas/yr,
  see above)
  mutheta   - The proper motion in the latitude-like angle (mas/yr or muas/yr, see above)
  vrad      - The radial velocity (km/s)

  Returns
  -------

  x - The x component of the barycentric position vector (in pc or kpc).
  y - The y component of the barycentric position vector (in pc or kpc).
  z - The z component of the barycentric position vector (in pc or kpc).
  vx - The x component of the barycentric velocity vector (in km/s).
  vy - The y component of the barycentric velocity vector (in km/s).
  vz - The z component of the barycentric velocity vector (in km/s).
From the input astrometric parameters calculate the phase space coordinates . The output phase space coordinates represent barycentric ( i . e . centred on the Sun ) positions and velocities .