# A closer look at orbit integration¶

## Orbit initialization¶

### Standard initialization¶

Orbits can be initialized in various
coordinate frames. The simplest initialization gives the initial
conditions directly in the Galactocentric cylindrical coordinate frame
(or in the rectangular coordinate frame in one dimension). `Orbit()`

automatically figures out the dimensionality of the space from the
initial conditions in this case. In three dimensions initial
conditions are given either as `[R,vR,vT,z,vz,phi]`

or one can
choose not to specify the azimuth of the orbit and initialize with
`[R,vR,vT,z,vz]`

. Since potentials in galpy are easily initialized
to have a circular velocity of one at a radius equal to one, initial
coordinates are best given as a fraction of the radius at which one
specifies the circular velocity, and initial velocities are best
expressed as fractions of this circular velocity. For example,

```
>>> from galpy.orbit import Orbit
>>> o= Orbit([1.,0.1,1.1,0.,0.1,0.])
```

initializes a fully three-dimensional orbit, while

```
>>> o= Orbit([1.,0.1,1.1,0.,0.1])
```

initializes an orbit in which the azimuth is not tracked, as might be useful for axisymmetric potentials.

In two dimensions, we can similarly specify fully two-dimensional
orbits `o=Orbit([R,vR,vT,phi])`

or choose not to track the azimuth
and initialize with `o= Orbit([R,vR,vT])`

.

In one dimension we simply initialize with `o= Orbit([x,vx])`

.

### Initialization with physical units¶

Orbits are normally used in galpy’s *natural coordinates*. When Orbits
are initialized using a distance scale `ro=`

and a velocity scale
`vo=`

, then many Orbit methods return quantities in physical
coordinates. Specifically, physical distance and velocity scales are
specified as

```
>>> op= Orbit([1.,0.1,1.1,0.,0.1,0.],ro=8.,vo=220.)
```

All output quantities will then be automatically be specified in physical units: kpc for positions, km/s for velocities, (km/s)^2 for energies and the Jacobi integral, km/s kpc for the angular momentum o.L() and actions, 1/Gyr for frequencies, and Gyr for times and periods. See below for examples of this.

The actual initial condition can also be specified in physical units. For example, the Orbit above can be initialized as

```
>>> from astropy import units
>>> op= Orbit([8.*units.kpc,22.*units.km/units.s,242*units.km/units.s,0.*units.kpc,22.*units.km/units.s,0.*units.deg])
```

In this case, it is unnecessary to specify the `ro=`

and `vo=`

scales; when they are not specified, `ro`

and `vo`

are set to the
default values from the configuration file. However, if they are specified, then those values
rather than the ones from the configuration file are used.

Tip

If you do input and output in physical units, the internal unit conversion specified by `ro=`

and `vo=`

does not matter!

Inputs to any Orbit method can also be specified with units as an astropy Quantity. galpy’s natural units are still used under the hood, as explained in the section on physical units in galpy. For example, integration times can be specified in Gyr if you want to integrate for a specific time period.

If for any output you do *not* want the output in physical units, you
can specify this by supplying the keyword argument
`use_physical=False`

.

### Initialization from observed coordinates or astropy `SkyCoord`

¶

For orbit integration and characterization of observed stars or
clusters, initial conditions can also be specified directly as
observed quantities when `radec=True`

is set (see further down in
this section on how to use an `astropy`

SkyCoord
instead). In this case a full three-dimensional orbit is initialized
as `o= Orbit([RA,Dec,distance,pmRA,pmDec,Vlos],radec=True)`

where RA and Dec are expressed in degrees, the distance is expressed
in kpc, proper motions are expressed in mas/yr (pmra = pmra’ *
cos[Dec] ), and `Vlos`

is the heliocentric line-of-sight velocity
given in km/s. The observed epoch is currently assumed to be
J2000.00. These observed coordinates are translated to the
Galactocentric cylindrical coordinate frame by assuming a Solar motion
that can be specified as either `solarmotion='hogg'`

(2005ApJ…629..268H),
`solarmotion='dehnen'`

(1998MNRAS.298..387D) or
`solarmotion='schoenrich'`

(default; 2010MNRAS.403.1829S). A circular
velocity can be specified as `vo=220`

in km/s and a value for the
distance between the Galactic center and the Sun can be given as
`ro=8.0`

in kpc (e.g., 2012ApJ…759..131B). While the
inputs are given in physical units, the orbit is initialized assuming
a circular velocity of one at the distance of the Sun (that is, the
orbit’s position and velocity is scaled to galpy’s *natural* units
after converting to the Galactocentric coordinate frame, using the
specified `ro=`

and `vo=`

). The parameters of the coordinate
transformations are stored internally, such that they are
automatically used for relevant outputs (for example, when the RA of
an orbit is requested). An example of all of this is:

```
>>> o= Orbit([20.,30.,2.,-10.,20.,50.],radec=True,ro=8.,vo=220.)
```

However, the internally stored position/velocity vector is

```
>>> print(o.vxvv)
# [1.1480792664061401, 0.1994859759019009, 1.8306295160508093, -0.13064400474040533, 0.58167185623715167, 0.14066246212987227]
```

and is therefore in *natural* units.

Tip

Initialization using observed coordinates can also use units. So, for example, proper motions can be specified as `2*units.mas/units.yr`

.

Similarly, one can also initialize orbits from Galactic coordinates
using `o= Orbit([glon,glat,distance,pmll,pmbb,Vlos],lb=True)`

, where
glon and glat are Galactic longitude and latitude expressed in
degrees, and the proper motions are again given in mas/yr ((pmll =
pmll’ * cos[glat] ):

```
>>> o= Orbit([20.,30.,2.,-10.,20.,50.],lb=True,ro=8.,vo=220.)
>>> print(o.vxvv)
# [0.79959714332811838, 0.073287283885367677, 0.5286278286083651, 0.12748861331872263, 0.89074407199364924, 0.0927414387396788]
```

When `radec=True`

or `lb=True`

is set, velocities can also be
specified in Galactic coordinates if `UVW=True`

is set. The input is
then `[RA,Dec,distance,U,V,W]`

, where the velocities are expressed
in km/s. U is, as usual, defined as -vR (minus vR).

Finally, orbits can also be initialized using an
`astropy.coordinates.SkyCoord`

object. For example, the (ra,dec)
example from above can also be initialized as:

```
>>> from astropy.coordinates import SkyCoord
>>> import astropy.units as u
>>> c= SkyCoord(ra=20.*u.deg,dec=30.*u.deg,distance=2.*u.kpc,
pm_ra_cosdec=-10.*u.mas/u.yr,pm_dec=20.*u.mas/u.yr,
radial_velocity=50.*u.km/u.s)
>>> o= Orbit(c)
```

In this case, you can still specify the properties of the
transformation to Galactocentric coordinates using the standard
`ro`

, `vo`

, `zo`

, and `solarmotion`

keywords, or you can use
the `SkyCoord`

Galactocentric frame specification
and these are propagated to the `Orbit`

instance. For example,

```
>>> from astropy.coordinates import CartesianDifferential
>>> c= SkyCoord(ra=20.*u.deg,dec=30.*u.deg,distance=2.*u.kpc,
pm_ra_cosdec=-10.*u.mas/u.yr,pm_dec=20.*u.mas/u.yr,
radial_velocity=50.*u.km/u.s,
galcen_distance=8.*u.kpc,z_sun=15.*u.pc,
galcen_v_sun=CartesianDifferential([10.0,235.,7.]*u.km/u.s))
>>> o= Orbit(c)
```

A subtlety here is that the `galcen_distance`

and `ro`

keywords
are not interchangeable, because the former is the distance between
the Sun and the Galactic center and `ro`

is the projection of this
distance onto the Galactic midplane. Another subtlety is that the
`astropy`

Galactocentric frame is a right-handed frame, while galpy
normally uses a left-handed frame, so the sign of the x component of
`galcen_v_sun`

is the opposite of what it would be in
`solarmotion`

. Because the Galactocentric frame in `astropy`

does
not specify the circular velocity, but only the Sun’s velocity, you
still need to specify `vo`

to use a non-default circular velocity.

When orbits are initialized using `radec=True`

, `lb=True`

, or
using a `SkyCoord`

physical scales `ro=`

and `vo=`

are
automatically specified (because they have defaults of `ro=8`

and
`vo=220`

). Therefore, all output quantities will be specified in
physical units (see above). If you do want to get outputs in galpy’s
natural coordinates, you can turn this behavior off by doing

```
>>> o.turn_physical_off()
```

All outputs will then be specified in galpy’s natural coordinates.

### Initializing multiple objects at once¶

In all of the examples above, the `Orbit`

instance corresponds to a
single object, but `Orbit`

instances can also contain and analyze
multiple objects at once. This makes handling `Orbit`

instances
highly convenient and also allows for efficient handling of multiple
objects. Many of the most computationally-intense methods have been
parallelized (orbit integration; analytic eccentricity, zmax,
etc. calculation; action-angle calculations) and some other methods
switch to more efficient algorithms for larger numbers of objects
(e.g., `rguiding`

, `rE`

, `LcE`

).

All of the methods for initializing `Orbit`

instances above work for
multiple objects. Specifically, the initial conditions can be:

- Array of arbitrary shape (shape,phasedim); needs to be in internal units (for Quantity input; see ‘list’ option below or use a SkyCoord):
in Galactocentric cylindrical coordinates with phase-space coordinates arranged as [R,vR,vT(,z,vz,phi)];

[ra,dec,d,mu_ra, mu_dec,vlos] or [l,b,d,mu_l, mu_b, vlos] in [deg,deg,kpc,mas/yr,mas/yr,km/s], or [ra,dec,d,U,V,W] or [l,b,d,U,V,W] in [deg,deg,kpc,km/s,km/s,kms] (ICRS where relevant; mu_ra = mu_ra * cos dec and mu_l = mu_l * cos ); use the

`radec=`

,`lb=`

, and`UVW=`

keywords as before

astropy (>v3.0) SkyCoord with arbitrary shape, including velocities;

- lists of initial conditions, entries can be
individual Orbit instances (of single objects)

Regular or Quantity arrays arranged as in the first bullet above (so things like [R,vR,vT,z,vz,phi], where R, vR, … can be arbitrary shape regular or Quantity arrays)

list of Quantities (so things like [R1,vR1,..,], where R1, vR1, … are scalar Quantities

None: assumed to be the Sun; if None occurs in a list it is assumed to be the Sun

*and all other items in the list are assumed to be [ra,dec,…]*; cannot be combined with Quantity listslists of scalar phase-space coordinates arranged as in the first bullet above (so things like [R,vR,…] where R,vR are scalars in internal units

The solar parameters `ro`

, `zo`

, `vo`

, and `solarmotion`

can also be specified as arrays with the same shape as the resulting `Orbit`

instance. This can be useful, for example, when sampling over the uncertainty in the Sun’s position and velocity in the Milky Way.

Tip

For multiple object initialization using an array or SkyCoord, arbitrary input shapes are supported.

An example initialization with an array is:

```
>>> vxvvs= numpy.array([[1.,0.1,1.,0.1,-0.2,1.5],[0.1,0.3,1.1,-0.3,0.4,2.]])
>>> orbits= Orbit(vxvvs)
>>> print(orbits.R())
# [ 1. 0.1]
```

and with a SkyCoord:

```
>>> numpy.random.seed(1)
>>> nrand= 30
>>> ras= numpy.random.uniform(size=nrand)*360.*u.deg
>>> decs= 90.*(2.*numpy.random.uniform(size=nrand)-1.)*u.deg
>>> dists= numpy.random.uniform(size=nrand)*10.*u.kpc
>>> pmras= 20.*(2.*numpy.random.uniform(size=nrand)-1.)*20.*u.mas/u.yr
>>> pmdecs= 20.*(2.*numpy.random.uniform(size=nrand)-1.)*20.*u.mas/u.yr
>>> vloss= 200.*(2.*numpy.random.uniform(size=nrand)-1.)*u.km/u.s
# Without any custom coordinate-transformation parameters
>>> co= SkyCoord(ra=ras,dec=decs,distance=dists,
pm_ra_cosdec=pmras,pm_dec=pmdecs,
radial_velocity=vloss,
frame='icrs')
>>> orbits= Orbit(co)
>>> print(orbits.ra()[:3],ras[:3])
# [ 1.50127922e+02 2.59316818e+02 4.11749371e-02] deg [ 1.50127922e+02 2.59316818e+02 4.11749342e-02] deg
```

As before, you can use the `SkyCoord`

Galactocentric frame
specification here.

An example initialization with array input for `ro`

is:

```
>>> vxvvs= numpy.array([[1.,0.1,1.,0.1,-0.2,1.5] for ii in range(2)])
>>> orbits= Orbit(vxvvs,ro=numpy.array([8.,8.5]))
>>> print(orbits.R())
# [ 8. 8.5]
```

Array inputs can also be used for `zo`

, `vo`

, and `solarmotion`

. When using arrays,
their shapes need to agree with the shape of the resulting `Orbit`

instance (for
`solarmotion`

, the shape needs to be `[3,*shape_orbit]`

).

`Orbit`

instances containing multiple objects act like numpy arrays
in many ways, but have some subtly different behaviors for some
functions. For example, one can do:

```
>>> print(len(orbits))
# 30
>>> print(orbits.shape)
# (30,)
>>> print(orbits.size)
# 30
>>> orbits.reshape((6,5)) # reshape is done inplace
>>> print(len(orbits))
# 6
>>> print(orbits.shape)
# (6,5)
>>> print(orbits.size)
# 30
>>> sliced_orbits= orbits[:3,1:5] # Extract a subset using numpy's slicing rules
>>> print(sliced_orbits.shape)
# (3,4)
>>> single_orbit= orbits[1,3] # Extract a single object
>>> print(single_orbit.shape)
# ()
```

Slicing creates a new `Orbit`

instance. When slicing an `Orbit`

instance that has been integrated, the integrated orbit will be
transferred to the new instance.

The shape of the `Orbit`

instances is retained for all relevant
outputs. Continuing on from the previous example (where `orbits`

has
shape `(6,5)`

after we reshaped it), we have:

```
>>> print(orbits.R().shape)
# (6,5)
>>> print(orbits.L().shape)
# (6,5,3)
```

After orbit integration, evaluating `orbits.R(times)`

would return
an array with shape `(6,5,ntimes)`

here.

### Initialization from an object’s name¶

A convenience method, `Orbit.from_name`

, is also available to initialize
orbits from the name of an object. For example, for the star Lacaille 8760:

```
>>> o= Orbit.from_name('Lacaille 8760', ro=8., vo=220.)
>>> [o.ra(), o.dec(), o.dist(), o.pmra(), o.pmdec(), o.vlos()]
# [319.31362023999276, -38.86736390000036, 0.003970940656277758, -3258.5529999996584, -1145.3959999996205, 20.560000000006063]
```

but this also works for globular clusters, e.g., to obtain Omega Cen’s orbit and current location in the Milky Way do:

```
>>> o= Orbit.from_name('Omega Cen')
>>> from galpy.potential import MWPotential2014
>>> ts= numpy.linspace(0.,100.,2001)
>>> o.integrate(ts,MWPotential2014)
>>> o.plot()
>>> plot([o.R()],[o.z()],'ro')
```

We see that Omega Cen is currently close to its maximum distance from both the Galactic center and from the Galactic midplane (note that Omega Cen’s phase-space coordinates were updated internally in `galpy`

after this plot was made and the orbit is now slightly different).

Similarly, you can do:

```
>>> o= Orbit.from_name('LMC')
>>> [o.ra(), o.dec(), o.dist(), o.pmra(), o.pmdec(), o.vlos()]
# [80.894200000000055, -69.756099999999847, 49.999999999999993, 1.909999999999999, 0.2290000000000037, 262.19999999999993]
```

It is also possible to initialize using multiple names, for example:

```
>>> o= Orbit.from_name(['LMC','SMC'])
>>> print(o.ra(),o.dec(),o.dist())
# [ 80.8942 13.1583] deg [-69.7561 -72.8003] deg [ 50. 60.] kpc
```

The names are stored in the `name`

attribute:

```
>>> print(o.name)
# ['LMC', 'SMC']
```

The `Orbit.from_name`

method attempts to resolve the name of the
object in SIMBAD, and then use the observed coordinates found there to
generate an `Orbit`

instance. In order to query SIMBAD,
`Orbit.from_name`

requires the astroquery package to be installed. A
small number of objects, mainly Milky Way globular clusters and dwarf
satellite galaxies, have their phase-space coordinates stored in a
file that is part of galpy and for these objects the values from this
file are used rather than querying SIMBAD. `Orbit.from_name`

supports tab completion in IPython/Jupyter for this list of objects

The `Orbit.from_name`

method also allows you to load some
collections of objects in a simple manner. Currently, three
collections are supported: ‘MW globular clusters’, ‘MW satellite
galaxies’, and ‘solar system’. Specifying ‘MW globular clusters’ loads
all of the Milky-Way globular clusters with data from Gaia EDR3:

```
>>> o= Orbit.from_name('MW globular clusters')
>>> print(len(o))
# 161
>>> print(o.name)
# ['NGC5286' 'Terzan12' 'Arp2', ... ]
>>> print(o.r())
# [ 8.4418065 2.99042499 21.55042257 ...]
```

It is then easy to, for example, integrate the orbits of all Milky-Way globular clusters in `MWPotential2014`

and plot them in 3D:

```
>>> ts= numpy.linspace(0.,300.,1001)
>>> o.integrate(ts,MWPotential2014)
>>> o.plot3d(alpha=0.4)
>>> xlim(-100.,100.)
>>> ylim(-100.,100)
>>> gca().set_zlim3d(-100.,100);
```

Similarly, ‘MW satellite galaxies’ loads all of the Milky-Way satellite galaxies from Pace et al. (2022):

```
>>> o= Orbit.from_name('MW satellite galaxies')
>>> print(len(o))
# 50
>>> print(o.name)
# ['AntliaII' 'AquariusII' 'BootesI' 'BootesII' 'BootesIII' 'CanesVenaticiI'
'CanesVenaticiII' 'Carina' 'CarinaII' 'CarinaIII' 'ColumbaI'
'ComaBerenices' 'CraterII' 'Draco' 'DracoII' 'EridanusII' 'Fornax'
'GrusI' 'GrusII' 'Hercules' 'HorologiumI' 'HydraII' 'HydrusI' 'LMC'
'LeoI' 'LeoII' 'LeoIV' 'LeoV' 'PegasusIII' 'PhoenixI' 'PhoenixII'
'PiscesII' 'ReticulumII' 'ReticulumIII' 'SMC' 'SagittariusII' 'Sculptor'
'Segue1' 'Segue2' 'Sextans' 'Sgr' 'TriangulumII' 'TucanaII' 'TucanaIII'
'TucanaIV' 'TucanaV' 'UrsaMajorI' 'UrsaMajorII' 'UrsaMinor' 'Willman1']
>>> print(o.r())
# [132.93721433 105.41442453 63.66115037 39.83901891 45.52928256
209.7700823 160.60534628 107.16399152 38.24845108 28.9274277
187.46809402 43.16546984 116.44003784 75.80593376 23.71949352
367.79884477 149.18728196 123.27421442 50.52704455 125.11664692
79.292941 148.20468685 25.74545627 49.60813235 261.93577755
235.49080095 151.95997497 169.77910104 213.08771512 418.76813979
81.18196715 182.15380106 32.72475876 91.96956471 60.28760354
63.35088903 83.99141137 27.77404178 42.42833236 95.44075955
19.06561359 34.54212398 54.28214129 21.05199179 44.4906331
51.92586773 101.87656784 40.73034335 78.06428801 42.6385771 ] kpc
```

and we can integrate and plot them in 3D as above:

```
>>> o.plot3d(alpha=0.4)
>>> xlim(-400.,400.)
>>> ylim(-400.,400)
>>> gca().set_zlim3d(-400.,400)
```

Because `MWPotential2014`

has a relatively low-mass dark-matter halo, a bunch of the satellites are unbound (to make them bound, you can increase the mass of the halo by, for example, multiplying it by 1.5, as in `MWPotential2014[2]*= 1.5`

).

Finally, for illustrative purposes, the solar system is included as a
collection as well. The solar system is set up such that the center of
what is normally the Galactocentric coordinate frame in `galpy`

is
now the solar system barycenter and the coordinate frame is a
heliocentric one. The solar system data are taken from Bovy et
al. (2010)
and they represent the positions and planets on April 1, 2009. To load
the solar system do:

```
>>> o= Orbit.from_name('solar system')
```

Giving for example:

```
>>> print(o.name)
# ['Mercury', 'Venus', 'Earth', 'Mars', 'Jupiter', 'Saturn', 'Uranus', 'Neptune']
```

You can then, for example, integrate the solar system for 10 years as follows

```
>>> import astropy.units as u
>>> from galpy.potential import KeplerPotential
>>> from galpy.util.conversion import get_physical
>>> kp= KeplerPotential(amp=1.*u.Msun,**get_physical(o)) # Need to use **get_physical to get the ro= and vo= parameters, which differ from the default for the solar system
>>> ts= numpy.linspace(0.,10.,1001)*u.yr
>>> o.integrate(ts,kp)
>>> o.plot(d1='x',d2='y')
```

which gives

Note that, as usual, physical outputs are in kpc, leading to very small numbers!

Tip

Setting up an `Orbit`

instance *without* arguments will return an Orbit instance representing the Sun: `o= Orbit()`

. This instance has physical units *turned on by default*, so methods will return outputs in physical units unless you `o.turn_physical_off()`

.

Warning

Orbits initialized using `Orbit.from_name`

have physical output *turned on by default*, so methods will return outputs in physical units unless you `o.turn_physical_off()`

.

## Orbit integration¶

After an orbit is initialized, we can integrate it for a set of times
`ts`

, given as a numpy array. For example, in a simple logarithmic
potential we can do the following

```
>>> from galpy.potential import LogarithmicHaloPotential
>>> lp= LogarithmicHaloPotential(normalize=1.)
>>> o= Orbit([1.,0.1,1.1,0.,0.1,0.])
>>> import numpy
>>> ts= numpy.linspace(0,100,10000)
>>> o.integrate(ts,lp)
```

to integrate the orbit from `t=0`

to `t=100`

, saving the orbit at
10000 instances. In physical units, we can integrate for 10 Gyr as follows

```
>>> from astropy import units
>>> ts= numpy.linspace(0,10.,10000)*units.Gyr
>>> o.integrate(ts,lp)
```

Warning

When the integration times are not specified using a Quantity, they are assumed to be in natural units.

If we initialize the Orbit using a distance scale `ro=`

and a
velocity scale `vo=`

, then Orbit plots and outputs will use physical
coordinates (currently, times, positions, and velocities)

```
>>> op= Orbit([1.,0.1,1.1,0.,0.1,0.],ro=8.,vo=220.) #Use Vc=220 km/s at R= 8 kpc as the normalization
>>> op.integrate(ts,lp)
```

An `Orbit`

instance containing multiple objects can be integrated in
the same way and the orbit integration will be performed in parallel
on machines with multiple cores. For the fast C integrators (see
below), this parallelization is done using OpenMP in C
and requires one to set the `OMP_NUM_THREADS`

environment variable
to control the number of cores used. The Python integrators are
parallelized in Python and by default also use the `OMP_NUM_THREADS`

variable to set the number of cores (but for the Python integrators
this can be overwritten). A simple example is

```
>>> vxvvs= numpy.array([[1.,0.1,1.,0.1,-0.2,1.5],[0.1,0.3,1.1,-0.3,0.4,2.]])
>>> orbits= Orbit(vxvvs)
>>> orbits.integrate(ts,lp)
>>> print(orbits.R(ts).shape)
# (2,10000)
>>> print(orbits.R(ts))
# [[ 1. 1.00281576 1.00563403 ..., 1.05694767 1.05608923
# 1.0551804 ]
# [ 0.1 0.18647825 0.27361065 ..., 3.39447863 3.34992543
# 3.30527001]]
```

## Orbit integration in non-inertial frames¶

The default assumption in `galpy`

is that the frame that an orbit is
integrated in is an inertial one. However, `galpy`

also supports
orbit integration in non-inertial frames that are rotating or whose
center is accelerating (or a combination of the two). When a frame is
not an inertial frame, fictitious forces such as the centrifugal
and Coriolis forces need to be taken into account. `galpy`

implements
all of the necessary forces as part of the
NonInertialFrameForce class. objects
of this class are instantiated with arbitrary three-dimensional rotation
frequencies (and their time derivative) and/or arbitrary three-dimensional
acceleration of the origin. The class documentation linked to above
provides full mathematical details on the rotation and acceleration
of the non-inertial frame.

We can then, for example, integrate the orbit of the Sun in the LSR frame,
that is, the frame that is corotating with that of the circular orbit
at the location of the Sun. To do this for `MWPotential2014`

, do

```
>>> from galpy.potential import MWPotential2014, NonInertialFrameForce
>>> nip= NonInertialFrameForce(Omega=1.) # LSR has Omega=1 in natural units
>>> o= Orbit() # Orbit() is the orbit of the Sun in the inertial frame
>>> o.turn_physical_off() # To use internal units
>>> o= Orbit([o.R(),o.vR(),o.vT()-1.,o.z(),o.vz(),o.phi()]) # Convert to the LSR frame
>>> ts= numpy.linspace(0.,20.,1001)
>>> o.integrate(ts,MWPotential2014+nip)
>>> o.plot(d1='x',d2='y')
```

which gives

we can compare this to integrating the orbit in the inertial frame and displaying it in the non-inertial LSR frame as follows:

```
>>> o.plot(d1='x',d2='y') # Repeat plot from above
>>> o= Orbit() # Orbit() is the orbit of the Sun in the inertial frame
>>> o.turn_physical_off() # To use internal units
>>> o.integrate(ts,MWPotential2014)
>>> o.plot(d1='R*cos(phi-t)',d2='R*sin(phi-t)',overplot=True) # Omega = 1, so Omega t = t
```

which gives

We can also do all of the above in physical units, in which case the first example above becomes

```
>>> from galpy.potential import MWPotential2014, NonInertialFrameForce
>>> from astropy import units
>>> nip= NonInertialFrameForce(Omega=220./8.*units.km/units.s/units.kpc)
>>> o= Orbit() # Orbit() is the orbit of the Sun in the inertial frame
>>> o= Orbit([o.R(quantity=True),o.vR(quantity=True),
o.vT(quantity=True)-220.*units.km/units.s,
o.z(quantity=True),o.vz(quantity=True),
o.phi(quantity=True)]) # Convert to the LSR frame
>>> ts= numpy.linspace(0.,20.,1001)
>>> o.integrate(ts,MWPotential2014+nip)
>>> o.plot(d1='x',d2='y')
```

We can also provide the `Omega=`

frequency as an arbitrary function of time.
In this case, the frequency must be returned in internal units and the input
time of this function must be in internal units as well (use the routines in
galpy.util.conversion for converting from physical to
internal units; you need to *divide* by these to go from physical to internal).
For the example above, this would amount to setting

```
>>> nip= NonInertialFrameForce(Omega=lambda t: 1.,Omegadot=lambda t: 0.)
```

Note that when we supply `Omega`

as a function, it is necessary to specify
its time derivative as well as `Omegadot`

(all again in internal units).

We give an example of having the origin of the non-inertial frame accelerate in the Example: Including the Milky Way center’s barycentric acceleration due to the Large Magellanic Cloud in orbit integrations section below.

## Displaying the orbit¶

After integrating the orbit, it can be displayed by using the
`plot()`

function. The quantities that are plotted when `plot()`

is called depend on the dimensionality of the orbit: in 3D the (R,z)
projection of the orbit is shown; in 2D either (X,Y) is plotted if the
azimuth is tracked and (R,vR) is shown otherwise; in 1D (x,vx) is
shown. E.g., for the example given above at the start of the
Orbit integration section above,

```
>>> o.plot()
```

gives

If we do the same for the Orbit that has physical distance and velocity scales associated with it, we get the following

```
>>> op.plot()
```

If we call `op.plot(use_physical=False)`

, the quantities will be
displayed in natural galpy coordinates.

Plotting an `Orbit`

instance that consists of multiple objects plots
all objects at once, e.g.,

```
>>> orbits.plot()
```

gives

Other projections of the orbit can be displayed by specifying the quantities to plot. E.g.,

```
>>> o.plot(d1='x',d2='y')
```

gives the projection onto the plane of the orbit:

while

```
>>> o.plot(d1='R',d2='vR')
```

gives the projection onto (R,vR):

We can also plot the orbit in other coordinate systems such as Galactic longitude and latitude

```
>>> o.plot('k.',d1='ll',d2='bb')
```

which shows

or RA and Dec

```
>>> o.plot('k.',d1='ra',d2='dec')
```

See the documentation of the o.plot function and the o.ra(), o.ll(), etc. functions on how to provide the necessary parameters for the coordinate transformations.

It is also possible to plot quantities computed from the basic Orbit
outputs like `o.x()`

, `o.r()`

, etc. For this to work, the numexpr module needs to be installed;
this can be done using `pip`

or `conda`

. Then you can ask for
plots like

```
>>> o.plot(d1='r',d2='vR*R/r+vz*z/r')
```

where `d2=`

converts the velocity to spherical coordinates (this is
currently not a pre-defined option). This gives the following orbit
(which is closed in this projection, because we are using a spherical
potential):

You can also do more complex things like

```
>>> o.plot(d1='x',d2='y')
>>> o.plot(d1='R*cos(phi-{:f}*t)'.format(o.Op(quantity=False)),
d2='R*sin(phi-{:f}*t)'.format(o.Op(quantity=False)),
overplot=True)
```

which shows the orbit in the regular `(x,y)`

frame as well as in a
`(x,y)`

frame that is rotating at the angular frequency of the
orbit. When doing more complex calculations like this, you need to
make sure that you are getting the units right: parameters `param`

in the expression you provide are directly evaluated as `o.param()`

,
which depending on how you setup the object may or may not return
output in physical units. The expression above is safe, because
`o.Op`

evaluated like this will be in a consistent unit system with
the rest of the expression. Expressions cannot contain astropy
Quantities (these cannot be parsed by the parser), which is why
`quantity=False`

is specified; this is also used internally.

Finally, it is also possible to plot arbitrary functions of time with
`Orbit.plot`

, by specifying `d1=`

or `d2=`

as a function. For
example, to display the orbital velocity in the spherical radial
direction, which we also did with the expression above, you can do the
following

```
>>> o.plot(d1='r',
d2=lambda t: o.vR(t)*o.R(t)/o.r(t)+o.vz(t)*o.z(t)/o.r(t),
ylabel='v_r')
```

For a function like this, just specifying it as the expression
`d2='vR*R/r+vz*z/r'`

is much more convenient, but expressions that
cannot be parsed automatically could be directly given as a function.

## Animating the orbit¶

Warning

Animating orbits is a new, experimental feature at this time that may be changed in later versions. It has only been tested in a limited fashion. If you are having problems with it, please open an Issue and list all relevant details about your setup (python version, jupyter version, browser, any error message in full). It may also be helpful to check the javascript console for any errors.

In a jupyter notebook or in jupyterlab (jupyterlab versions >= 0.33) you can also create an animation of an orbit *after* you have integrated it. For example, to do this for the `op`

orbit from above (but only integrated for 2 Gyr to create a shorter animation as an example here), do

```
>>> op.animate()
```

This will create the following animation

Tip

There is currently no option to save the animation within `galpy`

, but you could use screen capture software (for example, QuickTime’s Screen Recording feature) to record your screen while the animation is running and save it as a video.

`animate`

has options to specify the width and height of the resulting animation, and it can also animate up to three projections of an orbit at the same time. For example, we can look at the orbit in both (x,y) and (R,z) at the same time with

```
>>> op.animate(d1=['x','R'],d2=['y','z'],width=800)
```

which gives

You can also animate orbit in 3D with an optional Milky Way galaxy centered at the origin

```
>>> op.animate3d(mw_plane_bg=True)
```

which gives