# Potentials in galpy¶

galpy contains a large variety of potentials in `galpy.potential`

that can be used for orbit integration, the calculation of
action-angle coordinates, as part of steady-state distribution
functions, and to study the properties of gravitational
potentials. This section introduces some of these features.

## Potentials and forces¶

Various 3D and 2D potentials are contained in galpy, list in the API page. Another way to list the latest overview of potentials included with galpy is to run

```
>>> import galpy.potential
>>> print [p for p in dir(galpy.potential) if 'Potential' in p]
['CosmphiDiskPotential',
'DehnenBarPotential',
'DoubleExponentialDiskPotential',
'EllipticalDiskPotential',
'FlattenedPowerPotential',
'HernquistPotential',
....]
```

(list cut here for brevity). Section Rotation curves explains how to initialize potentials and how to display the rotation curve of single Potential instances or of combinations of such instances. Similarly, we can evaluate a Potential instance

```
>>> from galpy.potential import MiyamotoNagaiPotential
>>> mp= MiyamotoNagaiPotential(a=0.5,b=0.0375,normalize=1.)
>>> mp(1.,0.)
-1.2889062500000001
```

Most member functions of Potential instances have corresponding
functions in the galpy.potential module that allow them to be
evaluated for lists of multiple Potential
instances. `galpy.potential.MWPotential2014`

is such a list of three
Potential instances

```
>>> from galpy.potential import MWPotential2014
>>> print MWPotential2014
[<galpy.potential_src.PowerSphericalPotentialwCutoff.PowerSphericalPotentialwCutoff instance at 0x1089b23b0>, <galpy.potential_src.MiyamotoNagaiPotential.MiyamotoNagaiPotential instance at 0x1089b2320>, <galpy.potential_src.TwoPowerSphericalPotential.NFWPotential instance at 0x1089b2248>]
```

and we can evaluate the potential by using the `evaluatePotentials`

function

```
>>> from galpy.potential import evaluatePotentials
>>> evaluatePotentials(1.,0.,MWPotential2014)
-1.3733506513947895
```

Warning

`galpy`

potentials do *not* necessarily approach zero at infinity. To compute, for example, the escape velocity or whether or not an orbit is unbound, you need to take into account the value of the potential at infinity. E.g., \(v_{\mathrm{esc}}(r) = \sqrt{2[\Phi(\infty)-\Phi(r)]}\).

Tip

As discussed in the section on physical units, potentials can be initialized and evaluated with arguments specified as a astropy Quantity with units. Use the configuration parameter `apy-units = True`

to get output values as a Quantity. See also the subsection on Initializing potentials with parameters with units below.

We can plot the potential of axisymmetric potentials (or of
non-axisymmetric potentials at phi=0) using the `plot`

member
function

```
>>> mp.plot()
```

which produces the following plot

Similarly, we can plot combinations of Potentials using
`plotPotentials`

, e.g.,

```
>>> from galpy.potential import plotPotentials
>>> plotPotentials(MWPotential2014,rmin=0.01)
```

These functions have arguments that can provide custom `R`

and `z`

ranges for the plot, the number of grid points, the number of
contours, and many other parameters determining the appearance of
these figures.

galpy also allows the forces corresponding to a gravitational potential to be calculated. Again for the Miyamoto-Nagai Potential instance from above

```
>>> mp.Rforce(1.,0.)
-1.0
```

This value of -1.0 is due to the normalization of the potential such that the circular velocity is 1. at R=1. Similarly, the vertical force is zero in the mid-plane

```
>>> mp.zforce(1.,0.)
-0.0
```

but not further from the mid-plane

```
>>> mp.zforce(1.,0.125)
-0.53488743705310848
```

As explained in Units in galpy, these forces are in
standard galpy units, and we can convert them to physical units using
methods in the `galpy.util.bovy_conversion`

module. For example,
assuming a physical circular velocity of 220 km/s at R=8 kpc

```
>>> from galpy.util import bovy_conversion
>>> mp.zforce(1.,0.125)*bovy_conversion.force_in_kmsMyr(220.,8.)
-3.3095671288657584 #km/s/Myr
>>> mp.zforce(1.,0.125)*bovy_conversion.force_in_2piGmsolpc2(220.,8.)
-119.72021771473301 #2 \pi G Msol / pc^2
```

Again, there are functions in `galpy.potential`

that allow for the
evaluation of the forces for lists of Potential instances, such that

```
>>> from galpy.potential import evaluateRforces
>>> evaluateRforces(1.,0.,MWPotential2014)
-1.0
>>> from galpy.potential import evaluatezforces
>>> evaluatezforces(1.,0.125,MWPotential2014)*bovy_conversion.force_in_2piGmsolpc2(220.,8.)
>>> -69.680720137571114 #2 \pi G Msol / pc^2
```

We can evaluate the flattening of the potential as \(\sqrt{|z\,F_R/R\,F_Z|}\) for a Potential instance as well as for a list of such instances

```
>>> mp.flattening(1.,0.125)
0.4549542914935209
>>> from galpy.potential import flattening
>>> flattening(MWPotential2014,1.,0.125)
0.61231675305658628
```

## Densities¶

galpy can also calculate the densities corresponding to gravitational potentials. For many potentials, the densities are explicitly implemented, but if they are not, the density is calculated using the Poisson equation (second derivatives of the potential have to be implemented for this). For example, for the Miyamoto-Nagai potential, the density is explicitly implemented

```
>>> mp.dens(1.,0.)
1.1145444383277576
```

and we can also calculate this using the Poisson equation

```
>>> mp.dens(1.,0.,forcepoisson=True)
1.1145444383277574
```

which are the same to machine precision

```
>>> mp.dens(1.,0.,forcepoisson=True)-mp.dens(1.,0.)
-2.2204460492503131e-16
```

Similarly, all of the potentials in `galpy.potential.MWPotential2014`

have explicitly-implemented densities, so we can do

```
>>> from galpy.potential import evaluateDensities
>>> evaluateDensities(1.,0.,MWPotential2014)
0.57508603122264867
```

In physical coordinates, this becomes

```
>>> evaluateDensities(1.,0.,MWPotential2014)*bovy_conversion.dens_in_msolpc3(220.,8.)
0.1010945632524705 #Msol / pc^3
```

We can also plot densities

```
>>> from galpy.potential import plotDensities
>>> plotDensities(MWPotential2014,rmin=0.1,zmax=0.25,zmin=-0.25,nrs=101,nzs=101)
```

which gives

Another example of this is for an exponential disk potential

```
>>> from galpy.potential import DoubleExponentialDiskPotential
>>> dp= DoubleExponentialDiskPotential(hr=1./4.,hz=1./20.,normalize=1.)
```

The density computed using the Poisson equation now requires multiple numerical integrations, so the agreement between the analytical density and that computed using the Poisson equation is slightly less good, but still better than a percent

```
>>> (dp.dens(1.,0.,forcepoisson=True)-dp.dens(1.,0.))/dp.dens(1.,0.)
0.0032522956769123019
```

The density is

```
>>> dp.plotDensity(rmin=0.1,zmax=0.25,zmin=-0.25,nrs=101,nzs=101)
```

and the potential is

```
>>> dp.plot(rmin=0.1,zmin=-0.25,zmax=0.25)
```

Clearly, the potential is much less flattened than the density.

## Close-to-circular orbits and orbital frequencies¶

We can also compute the properties of close-to-circular orbits. First of all, we can calculate the circular velocity and its derivative

```
>>> mp.vcirc(1.)
1.0
>>> mp.dvcircdR(1.)
-0.163777427566978
```

or, for lists of Potential instances

```
>>> from galpy.potential import vcirc
>>> vcirc(MWPotential2014,1.)
1.0
>>> from galpy.potential import dvcircdR
>>> dvcircdR(MWPotential2014,1.)
-0.10091361254334696
```

We can also calculate the various frequencies for close-to-circular orbits. For example, the rotational frequency

```
>>> mp.omegac(0.8)
1.2784598203204887
>>> from galpy.potential import omegac
>>> omegac(MWPotential2014,0.8)
1.2733514576122869
```

and the epicycle frequency

```
>>> mp.epifreq(0.8)
1.7774973530267848
>>> from galpy.potential import epifreq
>>> epifreq(MWPotential2014,0.8)
1.7452189766287691
```

as well as the vertical frequency

```
>>> mp.verticalfreq(1.0)
3.7859388972001828
>>> from galpy.potential import verticalfreq
>>> verticalfreq(MWPotential2014,1.)
2.7255405754769875
```

For close-to-circular orbits, we can also compute the radii of the Lindblad resonances. For example, for a frequency similar to that of the Milky Way’s bar

```
>>> mp.lindbladR(5./3.,m='corotation') #args are pattern speed and m of pattern
0.6027911166042229 #~ 5kpc
>>> print mp.lindbladR(5./3.,m=2)
None
>>> mp.lindbladR(5./3.,m=-2)
0.9906190683480501
```

The `None`

here means that there is no inner Lindblad resonance, the
`m=-2`

resonance is in the Solar neighborhood (see the section on
the Hercules stream in this documentation).

## Using interpolations of potentials¶

`galpy`

contains a general `Potential`

class `interpRZPotential`

that can be used to generate interpolations of potentials that can be
used in their stead to speed up calculations when the calculation of
the original potential is computationally expensive (for example, for
the `DoubleExponentialDiskPotential`

). Full details on how to set
this up are given here. Interpolated potentials can
be used anywhere that general three-dimensional galpy potentials can
be used. Some care must be taken with outside-the-interpolation-grid
evaluations for functions that use `C`

to speed up computations.

**NEW in v1.2**: Initializing potentials with parameters with units¶

As already discussed in the section on physical units, potentials in galpy can be specified with parameters
with units since v1.2. For most inputs to the initialization it is
straightforward to know what type of units the input Quantity needs to
have. For example, the scale length parameter `a=`

of a
Miyamoto-Nagai disk needs to have units of distance.

The amplitude of a potential is specified through the `amp=`

initialization parameter. The units of this parameter vary from
potential to potential. For example, for a logarithmic potential the
units are velocity squared, while for a Miyamoto-Nagai potential they
are units of mass. Check the documentation of each potential on the
API page for the units of the `amp=`

parameter of the potential that you are trying to initialize and
please report an Issue if
you find any problems with this.

**NEW in v1.2/UPDATED in v1.3**: General density/potential pairs with basis-function expansions¶

`galpy`

allows for the potential and forces of general,
time-independent density functions to be computed by expanding the
potential and density in terms of basis functions. This is supported
for ellipsoidal-ish as well as for disk-y density distributions, in
both cases using the basis-function expansion of the
self-consistent-field (SCF) method of Hernquist & Ostriker (1992). On its own,
the SCF technique works well for ellipsoidal-ish density
distributions, but using a trick due to Kuijken & Dubinski (1995) it can also be
made to work well for disky potentials. We first describe the basic
SCF implementation and then discuss how to use it for disky
potentials.

The basis-function approach in the SCF method is implemented in the
SCFPotential class, which is also implemented
in C for fast orbit integration. The coefficients of the
basis-function expansion can be computed using the
scf_compute_coeffs_spherical
(for spherically-symmetric density distribution),
scf_compute_coeffs_axi (for
axisymmetric densities), and scf_compute_coeffs (for the general case). The coefficients
obtained from these functions can be directly fed into the
SCFPotential initialization. The basis-function
expansion has a free scale parameter `a`

, which can be specified for
the `scf_compute_coeffs_XX`

functions and for the `SCFPotential`

itself. Make sure that you use the same `a`

! Note that the general
functions are quite slow.

The simplest example is that of the Hernquist potential, which is the lowest-order basis function. When we compute the first ten radial coefficients for this density we obtain that only the lowest-order coefficient is non-zero

```
>>> from galpy.potential import HernquistPotential
>>> from galpy.potential import scf_compute_coeffs_spherical
>>> hp= HernquistPotential(amp=1.,a=2.)
>>> Acos, Asin= scf_compute_coeffs_spherical(hp.dens,10,a=2.)
>>> print(Acos)
array([[[ 1.00000000e+00]],
[[ -2.83370393e-17]],
[[ 3.31150709e-19]],
[[ -6.66748299e-18]],
[[ 8.19285777e-18]],
[[ -4.26730651e-19]],
[[ -7.16849567e-19]],
[[ 1.52355608e-18]],
[[ -2.24030288e-18]],
[[ -5.24936820e-19]]])
```

As a more complicated example, consider a prolate NFW potential

```
>>> from galpy.potential import TriaxialNFWPotential
>>> np= TriaxialNFWPotential(normalize=1.,c=1.4,a=1.)
```

and we compute the coefficients using the axisymmetric
`scf_compute_coeffs_axi`

```
>>> a_SCF= 50. # much larger a than true scale radius works well for NFW
>>> Acos, Asin= scf_compute_coeffs_axi(np.dens,80,40,a=a_SCF)
>>> sp= SCFPotential(Acos=Acos,Asin=Asin,a=a_SCF)
```

If we compare the densities along the `R=Z`

line as

```
>>> xs= numpy.linspace(0.,3.,1001)
>>> loglog(xs,np.dens(xs,xs))
>>> loglog(xs,sp.dens(xs,xs))
```

we get

If we then integrate an orbit, we also get good agreement

```
>>> from galpy.orbit import Orbit
>>> o= Orbit([1.,0.1,1.1,0.1,0.3,0.])
>>> ts= numpy.linspace(0.,100.,10001)
>>> o.integrate(ts,hp)
>>> o.plot()
>>> o.integrate(ts,sp)
>>> o.plot(overplot=True)
```

which gives

Near the end of the orbit integration, the slight differences between the original potential and the basis-expansion version cause the two orbits to deviate from each other.

To use the SCF method for disky potentials, we use the trick from Kuijken & Dubinski (1995). This trick works by approximating the disk density as \(\rho_{\mathrm{disk}}(R,\phi,z) \approx \sum_i \Sigma_i(R)\,h_i(z)\), with \(h_i(z) = \mathrm{d}^2 H(z) / \mathrm{d} z^2\) and searching for solutions of the form

\[\Phi(R,\phi,z = \Phi_{\mathrm{ME}}(R,\phi,z) + 4\pi G\sum_i \Sigma_i(r)\,H_i(z)\,,\]

where \(r\) is the spherical radius \(r^2 = R^2+z^2\). The density which gives rise to \(\Phi_{\mathrm{ME}}(R,\phi,z)\) is not strongly confined to a plane when \(\rho_{\mathrm{disk}}(R,\phi,z) \approx \sum_i \Sigma_i(R)\,h_i(z)\) and can be obtained using the SCF basis-function-expansion technique discussed above. See the documentation of the DiskSCFPotential class for more details on this procedure.

As an example, consider a double-exponential disk, which we can
compare to the `DoubleExponentialDiskPotential`

implementation

```
>>> from galpy import potential
>>> dp= potential.DoubleExponentialDiskPotential(amp=13.5,hr=1./3.,hz=1./27.)
```

and then setup the `DiskSCFPotential`

approximation to this as

```
>>> dscfp= potential.DiskSCFPotential(dens=lambda R,z: dp.dens(R,z),
Sigma={'type':'exp','h':1./3.,'amp':1.},
hz={'type':'exp','h':1./27.},
a=1.,N=10,L=10)
```

The `dens=`

keyword specifies the target density, while the
`Sigma=`

and `hz=`

inputs specify the approximation functions
\(\Sigma_i(R)\) and \(h_i(z)\). These are specified as
dictionaries here for a few pre-defined approximation functions, but
general functions are supported as well. Care should be taken that the
`dens=`

input density and the approximation functions have the same
normalization. We can compare the density along the `R=10 z`

line as

```
>>> xs= numpy.linspace(0.3,2.,1001)
>>> semilogy(xs,dp.dens(xs,xs/10.))
>>> semilogy(xs,dscfp.dens(xs,xs/10.))
```

which gives

The agreement is good out to 5 scale lengths and scale heights and then starts to degrade. We can also integrate orbits and compare them

```
>>> from galpy.orbit import Orbit
>>> o= Orbit([1.,0.1,0.9,0.,0.1,0.])
>>> ts= numpy.linspace(0.,100.,10001)
>>> o.integrate(ts,dp)
>>> o.plot()
>>> o.integrate(ts,dscfp)
>>> o.plot(overplot=True)
```

which gives

The orbits diverge slightly because the potentials are not quite the
same, but have very similar properties otherwise (peri- and
apogalacticons, eccentricity, ...). By increasing the order of the SCF
approximation, the potential can be gotten closer to the target
density. Note that orbit integration in the `DiskSCFPotential`

is
much faster than that of the `DoubleExponentialDisk`

potential

```
>>> timeit(o.integrate(ts,dp))
1 loops, best of 3: 5.83 s per loop
>>> timeit(o.integrate(ts,dscfp))
1 loops, best of 3: 286 ms per loop
```

The SCFPotential and DiskSCFPotential can be used wherever general potentials can be used in galpy.

## The potential of N-body simulations¶

`galpy`

can setup and work with the frozen potential of an N-body
simulation. This allows us to study the properties of such potentials
in the same way as other potentials in `galpy`

. We can also
investigate the properties of orbits in these potentials and calculate
action-angle coordinates, using the `galpy`

framework. Currently,
this functionality is limited to axisymmetrized versions of the N-body
snapshots, although this capability could be somewhat
straightforwardly expanded to full triaxial potentials. The use of
this functionality requires pynbody to be installed; the potential
of any snapshot that can be loaded with `pynbody`

can be used within
`galpy`

.

As a first, simple example of this we look at the potential of a
single simulation particle, which should correspond to galpy’s
`KeplerPotential`

. We can create such a single-particle snapshot
using `pynbody`

by doing

```
>>> import pynbody
>>> s= pynbody.new(star=1)
>>> s['mass']= 1.
>>> s['eps']= 0.
```

and we get the potential of this snapshot in `galpy`

by doing

```
>>> from galpy.potential import SnapshotRZPotential
>>> sp= SnapshotRZPotential(s,num_threads=1)
```

With these definitions, this snapshot potential should be the same as
`KeplerPotential`

with an amplitude of one, which we can test as
follows

```
>>> from galpy.potential import KeplerPotential
>>> kp= KeplerPotential(amp=1.)
>>> print(sp(1.1,0.),kp(1.1,0.),sp(1.1,0.)-kp(1.1,0.))
(-0.90909090909090906, -0.9090909090909091, 0.0)
>>> print(sp.Rforce(1.1,0.),kp.Rforce(1.1,0.),sp.Rforce(1.1,0.)-kp.Rforce(1.1,0.))
(-0.82644628099173545, -0.8264462809917353, -1.1102230246251565e-16)
```

`SnapshotRZPotential`

instances can be used wherever other `galpy`

potentials can be used (note that the second derivatives have not been
implemented, such that functions depending on those will not
work). For example, we can plot the rotation curve

```
>>> sp.plotRotcurve()
```

Because evaluating the potential and forces of a snapshot is
computationally expensive, most useful applications of frozen N-body
potentials employ interpolated versions of the snapshot
potential. These can be setup in `galpy`

using an
`InterpSnapshotRZPotential`

class that is a subclass of the
`interpRZPotential`

described above and that can be used in the same
manner. To illustrate its use we will make use of one of `pynbody`

‘s
example snapshots, `g15784`

. This snapshot is used here
to illustrate `pynbody`

‘s use. Please follow the instructions there
on how to download this snapshot.

Once you have downloaded the `pynbody`

testdata, we can load this
snapshot using

```
>>> s = pynbody.load('testdata/g15784.lr.01024.gz')
```

(please adjust the path according to where you downloaded the
`pynbody`

testdata). We get the main galaxy in this snapshot, center
the simulation on it, and align the galaxy face-on using

```
>>> h = s.halos()
>>> h1 = h[1]
>>> pynbody.analysis.halo.center(h1,mode='hyb')
>>> pynbody.analysis.angmom.faceon(h1, cen=(0,0,0),mode='ssc')
```

we also convert the simulation to physical units, but set G=1 by doing the following

```
>>> s.physical_units()
>>> from galpy.util.bovy_conversion import _G
>>> g= pynbody.array.SimArray(_G/1000.)
>>> g.units= 'kpc Msol**-1 km**2 s**-2 G**-1'
>>> s._arrays['mass']= s._arrays['mass']*g
```

We can now load an interpolated version of this snapshot’s potential
into `galpy`

using

```
>>> from galpy.potential import InterpSnapshotRZPotential
>>> spi= InterpSnapshotRZPotential(h1,rgrid=(numpy.log(0.01),numpy.log(20.),101),logR=True,zgrid=(0.,10.,101),interpPot=True,zsym=True)
```

where we further assume that the potential is symmetric around the
mid-plane (z=0). This instantiation will take about ten to fiteen
minutes. This potential instance has physical units (and thus the
`rgrid=`

and `zgrid=`

inputs are given in kpc if the simulation’s
distance unit is kpc). For example, if we ask for the rotation curve,
we get the following:

```
>>> spi.plotRotcurve(Rrange=[0.01,19.9],xlabel=r'$R\,(\mathrm{kpc})$',ylabel=r'$v_c(R)\,(\mathrm{km\,s}^{-1})$')
```

This can be compared to the rotation curve calculated by `pynbody`

,
see here.

Because `galpy`

works best in a system of natural units as
explained in Units in galpy, we will convert this
instance to natural units using the circular velocity at R=10 kpc,
which is

```
>>> spi.vcirc(10.)
294.62723076942245
```

To convert to natural units we do

```
>>> spi.normalize(R0=10.)
```

We can then again plot the rotation curve, keeping in mind that the distance unit is now \(R_0\)

```
>>> spi.plotRotcurve(Rrange=[0.01,1.99])
```

which gives

in particular

```
>>> spi.vcirc(1.)
1.0000000000000002
```

We can also plot the potential

```
>>> spi.plot(rmin=0.01,rmax=1.9,nrs=51,zmin=-0.99,zmax=0.99,nzs=51)
```

Clearly, this simulation’s potential is quite spherical, which is confirmed by looking at the flattening

```
>>> spi.flattening(1.,0.1)
0.86675711023391921
>>> spi.flattening(1.5,0.1)
0.94442750306256895
```

The epicyle and vertical frequencies can also be interpolated by
setting the `interpepifreq=True`

or `interpverticalfreq=True`

keywords when instantiating the `InterpSnapshotRZPotential`

object.

## Conversion to NEMO potentials¶

NEMO is a set of tools for
studying stellar dynamics. Some of its functionality overlaps with
that of `galpy`

, but many of its programs are very complementary to
`galpy`

. In particular, it has the ability to perform N-body
simulations with a variety of poisson solvers, which is currently not
supported by `galpy`

(and likely will never be directly
supported). To encourage interaction between `galpy`

and NEMO it
is quite useful to be able to convert potentials between these two
frameworks, which is not completely trivial. In particular, NEMO
contains Walter Dehnen’s fast collisionless `gyrfalcON`

code (see
2000ApJ...536L..39D and
2002JCoPh.179...27D) and the
discussion here focuses on how to run N-body simulations using
external potentials defined in `galpy`

.

Some `galpy`

potential instances support the functions
`nemo_accname`

and `nemo_accpars`

that return the name of the
NEMO potential corresponding to this `galpy`

Potential and its
parameters in NEMO units. These functions assume that you use NEMO
with WD_units, that is, positions are specified in kpc, velocities in
kpc/Gyr, times in Gyr, and G=1. For the Miyamoto-Nagai potential
above, you can get its name in the NEMO framework as

```
>>> mp.nemo_accname()
'MiyamotoNagai'
```

and its parameters as

```
>>> mp.nemo_accpars(220.,8.)
'0,592617.11132,4.0,0.3'
```

assuming that we scale velocities by `vo=220`

km/s and positions by
`ro=8`

kpc in galpy. These two strings can then be given to the
`gyrfalcON`

`accname=`

and `accpars=`

keywords.

We can do the same for lists of potentials. For example, for
`MWPotential2014`

we do

```
>>> from galpy.potential import nemo_accname, nemo_accpars
>>> nemo_accname(MWPotential2014)
'PowSphwCut+MiyamotoNagai+NFW'
>>> nemo_accpars(MWPotential2014,220.,8.)
'0,1001.79126907,1.8,1.9#0,306770.418682,3.0,0.28#0,16.0,162.958241887'
```

Therefore, these are the `accname=`

and `accpars=`

that one needs
to provide to `gyrfalcON`

to run a simulation in
`MWPotential2014`

.

Note that the NEMO potential `PowSphwCut`

is *not* a standard
NEMO potential. This potential can be found in the nemo/ directory of
the `galpy`

source code; this directory also contains a Makefile that
can be used to compile the extra NEMO potential and install it in
the correct NEMO directory (this requires one to have NEMO
running, i.e., having sourced nemo_start).

You can use the `PowSphwCut.cc`

file in the nemo/ directory as a
template for adding additional potentials in `galpy`

to the NEMO
framework. To figure out how to convert the normalized `galpy`

potential to an amplitude when scaling to physical coordinates (like
kpc and kpc/Gyr), one needs to look at the scaling of the radial force
with R. For example, from the definition of MiyamotoNagaiPotential, we
see that the radial force scales as \(R^{-2}\). For a general
scaling \(R^{-\alpha}\), the amplitude will scale as
\(V_0^2\,R_0^{\alpha-1}\) with the velocity \(V_0\) and
position \(R_0\) of the `v=1`

at `R=1`

normalization. Therefore, for the MiyamotoNagaiPotential, the physical
amplitude scales as \(V_0^2\,R_0\). For the
LogarithmicHaloPotential, the radial force scales as \(R^{-1}\),
so the amplitude scales as \(V_0^2\).

Currently, only the `MiyamotoNagaiPotential`

, `NFWPotential`

,
`PowerSphericalPotentialwCutoff`

, `PlummerPotential`

,
`MN3ExponentialDiskPotential`

, and the `LogarithmicHaloPotential`

have this NEMO support. Combinations of the first three are also
supported (e.g., `MWPotential2014`

); they can also be combined with
spherical `LogarithmicHaloPotentials`

. Because of the definition of
the logarithmic potential in NEMO, it cannot be flattened in `z`

, so
to use a flattened logarithmic potential, one has to flip `y`

and
`z`

between `galpy`

and NEMO (one can flatten in `y`

).

## Adding potentials to the galpy framework¶

Potentials in galpy can be used in many places such as orbit
integration, distribution functions, or the calculation of
action-angle variables, and in most cases any instance of a potential
class that inherits from the general `Potential`

class (or a list of
such instances) can be given. For example, all orbit integration
routines work with any list of instances of the general `Potential`

class. Adding new potentials to galpy therefore allows them to be used
everywhere in galpy where general `Potential`

instances can be
used. Adding a new class of potentials to galpy consists of the
following series of steps (some of these are also given in the file
`README.dev`

in the galpy distribution):

- Implement the new potential in a class that inherits from
`galpy.potential.Potential`

. The new class should have an`__init__`

method that sets up the necessary parameters for the class. An amplitude parameter`amp=`

and two units parameters`ro=`

and`vo=`

should be taken as an argument for this class and before performing any other setup, the`galpy.potential.Potential.__init__(self,amp=amp,ro=ro,vo=vo,amp_units=)`

method should be called to setup the amplitude and the system of units; the`amp_units=`

keyword specifies the physical units of the amplitude parameter (e.g.,`amp_units='velocity2'`

when the units of the amplitude are velocity-squared) To add support for normalizing the potential to standard galpy units, one can call the`galpy.potential.Potential.normalize`

function at the end of the __init__ function.

The new potential class should implement some of the following functions:

`_evaluate(self,R,z,phi=0,t=0)`

which evaluates the potential itself (withoutthe amp factor, which is added in the`__call__`

method of the general Potential class).`_Rforce(self,R,z,phi=0.,t=0.)`

which evaluates the radial force in cylindrical coordinates (-d potential / d R).`_zforce(self,R,z,phi=0.,t=0.)`

which evaluates the vertical force in cylindrical coordinates (-d potential / d z).`_R2deriv(self,R,z,phi=0.,t=0.)`

which evaluates the second (cylindrical) radial derivative of the potential (d^2 potential / d R^2).`_z2deriv(self,R,z,phi=0.,t=0.)`

which evaluates the second (cylindrical) vertical derivative of the potential (d^2 potential / d z^2).`_Rzderiv(self,R,z,phi=0.,t=0.)`

which evaluates the mixed (cylindrical) radial and vertical derivative of the potential (d^2 potential / d R d z).`_dens(self,R,z,phi=0.,t=0.)`

which evaluates the density. If not given, the density is computed using the Poisson equation from the first and second derivatives of the potential (if all are implemented).`_mass(self,R,z=0.,t=0.)`

which evaluates the mass. For spherical potentials this should give the mass enclosed within the spherical radius; for axisymmetric potentials this should return the mass up to`R`

and between`-Z`

and`Z`

. If not given, the mass is computed by integrating the density (if it is implemented or can be calculated from the Poisson equation).`_phiforce(self,R,z,phi=0.,t=0.)`

: the azimuthal force in cylindrical coordinates (assumed zero if not implemented).`_phi2deriv(self,R,z,phi=0.,t=0.)`

: the second azimuthal derivative of the potential in cylindrical coordinates (d^2 potential / d phi^2; assumed zero if not given).`_Rphideriv(self,R,z,phi=0.,t=0.)`

: the mixed radial and azimuthal derivative of the potential in cylindrical coordinates (d^2 potential / d R d phi; assumed zero if not given).`OmegaP(self)`

: returns the pattern speed for potentials with a pattern speed (used to compute the Jacobi integral for orbits).If you want to be able to calculate the concentration for a potential, you also have to set self._scale to a scale parameter for your potential.

The code for

`galpy.potential.MiyamotoNagaiPotential`

gives a good template to follow for 3D axisymmetric potentials. Similarly, the code for`galpy.potential.CosmphiDiskPotential`

provides a good template for 2D, non-axisymmetric potentials.After this step, the new potential will work in any part of galpy that uses pure python potentials. To get the potential to work with the C implementations of orbit integration or action-angle calculations, the potential also has to be implemented in C and the potential has to be passed from python to C.

The

`__init__`

method should be written in such a way that a relevant object can be initialized using`Classname()`

(i.e., there have to be reasonable defaults given for all parameters, including the amplitude); doing this allows the nose tests for potentials to automatically check that your Potential’s potential function, force functions, second derivatives, and density (through the Poisson equation) are correctly implemented (if they are implemented). The continuous-integration platform that builds the galpy codebase upon code pushes will then automatically test all of this, streamlining push requests of new potentials.A few atrributes need to be set depending on the potential:

`hasC=True`

for potentials for which the forces and potential are implemented in C (see below);`self.hasC_dxdv=True`

for potentials for which the (planar) second derivatives are implemented in C;`self.isNonAxi=True`

for non-axisymmetric potentials.

- To add a C implementation of the potential, implement it in a .c file under
`potential_src/potential_c_ext`

. Look at`potential_src/potential_c_ext/LogarithmicHaloPotential.c`

for the right format for 3D, axisymmetric potentials, or at`potential_src/potential_c_ext/LopsidedDiskPotential.c`

for 2D, non-axisymmetric potentials.

For orbit integration, the functions such as:

- double LogarithmicHaloPotentialRforce(double R,double Z, double phi,double t,struct potentialArg * potentialArgs)
- double LogarithmicHaloPotentialzforce(double R,double Z, double phi,double t,struct potentialArg * potentialArgs)
are most important. For some of the action-angle calculations

- double LogarithmicHaloPotentialEval(double R,double Z, double phi,double t,struct potentialArg * potentialArgs)
is most important (i.e., for those algorithms that evaluate the potential). The arguments of the potential are passed in a

`potentialArgs`

structure that contains`args`

, which are the arguments that should be unpacked. Again, looking at some example code will make this clear. The`potentialArgs`

structure is defined in`potential_src/potential_c_ext/galpy_potentials.h`

.

3. Add the potential’s function declarations to
`potential_src/potential_c_ext/galpy_potentials.h`

4. (4. and 5. for planar orbit integration) Edit the code under
`orbit_src/orbit_c_ext/integratePlanarOrbit.c`

to set up your new
potential (in the **parse_leapFuncArgs** function).

5. Edit the code in `orbit_src/integratePlanarOrbit.py`

to set up your
new potential (in the **_parse_pot** function).

6. Edit the code under `orbit_src/orbit_c_ext/integrateFullOrbit.c`

to
set up your new potential (in the **parse_leapFuncArgs_Full** function).

7. Edit the code in `orbit_src/integrateFullOrbit.py`

to set up your
new potential (in the **_parse_pot** function).

8. (for using the actionAngleStaeckel methods in C) Edit the code in
`actionAngle_src/actionAngle_c_ext/actionAngle.c`

to parse the new
potential (in the **parse_actionAngleArgs** function).

9. Finally, add `self.hasC= True`

to the initialization of the
potential in question (after the initialization of the super class, or
otherwise it will be undone). If you have implemented the necessary
second derivatives for integrating phase-space volumes, also add
`self.hasC_dxdv=True`

.

After following the relevant steps, the new potential class can be used in any galpy context in which C is used to speed up computations.