JamPy: Jeans Anisotropic Models for Galactic Dynamics

## The JamPy Package

Jeans Anisotropic Modelling for Galactic Dynamics

JamPy is a Python implementation of the Jeans Anisotropic Modelling (JAM) formalism for the dynamical modelling of galaxies.

This software can be used e.g. to measure the mass of supermassive black holes in galaxies, to infer their dark-matter content or to measure galaxy masses and density profiles.

The method calculates all the first and second velocity moments, for both the intrinsic and the projected kinematics, in spherical and axisymmetric geometry.

The JAM solution assuming a cylindrically-oriented velocity ellipsoid was introduced in Cappellari (2008), while the solution assuming a spherically-oriented velocity ellipsoid was introduced in Cappellari (2020)

If you use this software for your research, please cite Cappellari (2008) for the cylindrically-aligned JAM solution and Cappellari (2020) for the spherically-aligned JAM solution.

The BibTeX entry for the two main JAM papers are respectively:

@ARTICLE{Cappellari2008,
author = {{Cappellari}, Michele},
title = "{Measuring the inclination and mass-to-light ratio of axisymmetric
galaxies via anisotropic Jeans models of stellar kinematics}",
journal = {MNRAS},
eprint = {0806.0042},
year = 2008,
volume = 390,
pages = {71-86},
doi = {10.1111/j.1365-2966.2008.13754.x}
}

@ARTICLE{Cappellari2020,
author = {{Cappellari}, Michele},
title = "{Efficient solution of the anisotropic spherically-aligned axisymmetric
Jeans equations of stellar hydrodynamics for galactic dynamics}",
journal = {MNRAS},
eprint = {1907.09894},
year = 2020,
volume = 494,
pages = {4819-4837},
doi = {10.1093/mnras/staa959}
}

### Installation

install with:

pip install jampy

pip install --user jampy

pip install --upgrade jampy

### Documentation

Full documentation is contained in the individual files docstrings.

Usage examples are contained in the directory jampy/examples which is copied by pip within the global folder site-packages.

What follows is the documentation of the two main procedures of the JamPy package, extracted from their Python docstrings. The other procedures are documented in their respective docstrings.

The older JamPy routines from version < v6.0 are generally redundant, but can be imported from jampy.legacy and used like before.

## jam_axi_proj

### Purpose

This procedure calculates a prediction for all the projected first or second velocity moments for an anisotropic (three-integral) axisymmetric galaxy model.

Any of the three components of the first velocity moment or any of the six components of the symmetric velocity dispersion tensor are supported. These include the line-of-sight velocities and the components of the proper motion.

Two assumptions for the orientation of the velocity ellipsoid are supported:

### Calling Sequence

jam = jam_axi_proj(
surf_lum, sigma_lum, qobs_lum, surf_pot, sigma_pot, qobs_pot,
inc, mbh, distance, xbin, ybin, align='cyl', analytic_los=True,
beta=None, data=None, epsrel=1e-2, errors=None, flux_obs=None,
gamma=None, goodbins=None, interp=True, kappa=None, ml=None,
moment='zz', nang=10, nlos=150, nodots=False, normpsf=1.,
rbh=0.01, sigmapsf=0., step=0., vmax=None, vmin=None)

vrms = jam.model  # with moment='zz' the output is the LOS Vrms

jam.plot()   # Generate data/model comparison when data is given

See more examples in the jampy/examples folder inside site-packages.

### Input Parameters

surf_lum: array_like with shape (n,)

peak surface values of the Multi-Gaussian Expansion (MGE) Gaussians describing the surface brightness of the tracer population for which the kinematics is derived.

The units are arbitrary as they cancel out in the final results.

EXAMPLE: when one obtains the kinematics from optical spectroscopy, surf_lum contains the galaxy optical surface brightness, which has typical units of Lsun/pc^2 (solar luminosities per parsec^2).

sigma_lum: array_like with shape (n,)

dispersion (sigma) in arcseconds of the MGE Gaussians describing the distribution of the kinematic-tracer population.

qobs_lum: array_like with shape (n,)

observed axial ratio (q’) of the MGE Gaussians describing the distribution of the kinematic-tracer population.

surf_pot: array_like with shape (m,)

peak value of the MGE Gaussians describing the galaxy total-mass surface density in units of Msun/pc^2 (solar masses per parsec^2). This is the MGE model from which the model gravitational potential is computed.

EXAMPLE: with a self-consistent model, one has the same Gaussians for both the kinematic-tracer and the gravitational potential. This implies surf_pot = surf_lum, sigma_pot = sigma_lum and qobs_pot = qobs_lum. The global M/L of the model is fitted by the routine when passing the data and errors keywords with the observed kinematics.

sigma_pot: array_like with shape (m,)

dispersion in arcseconds of the MGE Gaussians describing the galaxy total-mass surface density.

qobs_pot: array_like with shape (m,)

observed axial ratio of the MGE Gaussians describing the galaxy total-mass surface density.

inc: float

inclination in degrees between the line-of-sight and the galaxy symmetry axis (0 being face-on and 90 edge-on).

mbh: float

Mass of a nuclear supermassive black hole in solar masses.

IMPORTANT: The model predictions are computed assuming surf_pot gives the total mass. In the self-consistent case, one has surf_pot = surf_lum and if requested (keyword ml) the program can scale the output model to best fit the data. The scaling is equivalent to multiplying both surf_pot and mbh by a factor M/L. To avoid mistakes, the actual mbh used by the output model is printed on the screen.

distance: float

the distance of the galaxy in Mpc. When the distance is derived from redshift one should use the angular diameter distance D_A here.

xbin: array_like with shape (p,)

X coordinates in arcseconds of the bins (or pixels) at which one wants to compute the model predictions. The X-axis is assumed to coincide with the galaxy projected major axis. The galaxy center is at (0,0).

In general the coordinates (xbin, ybin) have to be rotated to bring the galaxy major axis on the X-axis, before calling jam_axi_proj.

When no PSF/pixel convolution is performed (sigmapsf=0 or pixsize=0) there is a singularity at (0,0) which should be avoided by the user in the input coordinates.

ybin: array_like with shape (p,)

Y coordinates in arcseconds of the bins (or pixels) at which one wants to compute the model predictions. The Y-axis is assumed to coincide with the projected galaxy symmetry axis.

### Optional Keywords

align: {‘cyl’, ‘sph’}, optional.

Assumed alignment for the velocity ellipsoid during the solution of the Jeans equations.

• align='cyl' assumes a cylindrically-aligned velocity ellipsoid using the solution of Cappellari (2008)

• align='sph' assumes a spherically-aligned velocity ellipsoid using the solution of Cappellari (2020)

analytic_los: bool, optional

This is True (default) if the line-of-sight integral is performed analytically and False if it is done via numerical quadrature.

An analytic integral is only possible with align='cyl' and only for the second velocity moments. For this reason, when comparing the two second-moment solutions with align='cyl' and align='sph', it may be preferable to set analytic_los=False to ensure that numerical interpolation error is exactly the same in both cases.

When align='sph', or when the user requests a first velocity moment, this keyword is automatically set to False.

beta: array_like with shape (n,)

radial anisotropy of the individual kinematic-tracer MGE Gaussians (Default: beta=np.zeros(n)):

beta = 1 - (sigma_th/sigma_r)^2  # with align=sph
beta = 1 - (sigma_z/sigma_R)^2   # with align=cyl
data: array_like with shape (p,), optional

observed first or second velocity moment used to fit the model.

EXAMPLE: In the common case where one has only line-of-sight velocities the second moment is given by:

Vrms = np.sqrt(velBin**2 + sigBin**2)

at the coordinates positions given by the vectors xbin and ybin.

If data is set and ml is negative or None, then the model is fitted to the data, otherwise, the adopted ml is used and just the chi**2 is returned.

epsrel: float, optional

Relative error requested for the numerical computation of the intrinsic moments (before line-of-sight quadrature). (Default: epsrel=1e-2)

errors: array_like with shape (p,), optional

1sigma uncertainty associated with the data measurements.

EXAMPLE: In the case where the data are given by the Vrms = np.sqrt(velBin**2 + sigBin**2), from the error propagation:

errors = np.sqrt((dVel*velBin)**2 + (dSig*sigBin)**2)/Vrms,

where velBin and sigBin are the velocity and dispersion in each bin and dVel and dSig are the corresponding 1sigma uncertainties. (Default: constant errors = 0.05*np.median(data))

flux_obs: array_like with shape (p,), optional

Optional mean surface brightness of each bin for plotting.

gamma: array_like with shape (n,)

tangential anisotropy of the individual kinematic-tracer MGE Gaussians (Default: gamma=np.zeros(n)):

gamma = 1 - (sigma_phi/sigma_r)^2  # with align=sph
gamma = 1 - (sigma_phi/sigma_R)^2  # with align=cyl
goodbins: array_like with shape (p,)

Boolean vector with values True for the bins/spaxels which have to be included in the fit (if requested) and in the chi**2 calculation. (Default: fit all bins).

interp: bool, optional

This keyword is for advanced use only! Set interp=False to force no-interpolation on the sky plane. In this way jam.vel and jam.vel2 contain all the first and second velocity moments at the input coordinates (xbin, ybin), without PSF convolution. By default interp=True and one should generally not change this.

IMPORTANT: If sigmapsf=0 or pixsize=0 or interp=False then PSF convolution is not performed.

This keyword is mainly useful for testing against analytic results or to compute all moments, including proper motions, simultaneously.

kappa: float, optional

When kappa=None (default) the first velocity moments are scaled in such a way that the projected angular momentum of the data and model is the same [equation 52 of Cappellari (2008)]. When kappa=1 the model first velocity moments are output without any scaling.

ml: float, optional

Mass-to-light ratio (M/L) to multiply the values given by surf_pot. Setting this keyword is completely equivalent to multiplying the output model by np.sqrt(M/L) after the fit. This implies that the BH mass is also scaled and becomes mbh*ml.

If ml=None (default) the M/L is fitted from the data and the best-fitting M/L is returned in output. The BH mass of the model is also scaled and becomes mbh*ml.

moment: {‘x’, ‘y’, ‘z’, ‘xx’, ‘yy’, ‘zz’, ‘xy’, ‘xz’, ‘yz’}, optional

String specifying the component of the velocity first or second moments requested by the user in output. All values ar in km/s.

• moment='x' gives the first moment <V_x'> of the proper motion in the direction orthogonal to the projected symmetry axis.

• moment='y' gives the first moment <V_y'> of the proper motion in the direction parallel to the projected symmetry axis.

• moment='z' gives the first moment Vlos = <V_z'> of the line-of-sight velocity.

• moment='xx' gives sqrt<V_x'^2> of the component of the proper motion dispersion tensor in the direction orthogonal to the projected symmetry axis.

• moment='yy' gives sqrt<V_y'^2> of the component of the proper motion dispersion tensor in the direction parallel to the projected symmetry axis.

• moment='zz' (default) gives the usual line-of-sight Vrms = sqrt<V_z'^2>.

• moment='xy' gives the mixed component <V_x'V_y'> of the proper motion dispersion tensor.

• moment='xz' gives the mixed component <V_x'V_z'> of the proper motion dispersion tensor.

• moment='yz' gives the mixed component <V_y'V_z'> of the proper motion dispersion tensor.

nang: int, optional

The number of linearly-spaced intervals in the eccentric anomaly at which the model is evaluated before interpolation and PSF convolution. (default: nang=10)

nlos: int (optional)

Number of values used for the numerical line-of-sight quadrature. (default nlos=150)

nodots: bool, optional

Set to True to hide the dots indicating the centers of the bins in the linearly-interpolated two-dimensional map (default False).

normpsf: array_like with shape (q,)

fraction of the total PSF flux contained in the circular Gaussians describing the PSF of the kinematic observations. The PSF will be used for seeing convolution of the model kinematics. It has to be np.sum(normpsf) = 1.

The number of logarithmically spaced radial positions at which the model is evaluated before interpolation and PSF convolution. One may want to increase this value if the model has to be evaluated over many orders of magnitude in radius (default: nrad=20).

pixang: float, optional

Angle between the observed spaxels and the galaxy major axis X. This angle only rotates the spaxels around their centers, not the whole coordinate system (xbin, ybin), which must be rotated independently by the user before calling jam_axi_proj. Using the keyword is generally unnecessary.

pixsize: float, optional

Size in arcseconds of the (square) spatial elements at which the kinematics is obtained. This may correspond to the side of the spaxel or lenslets of an integral-field spectrograph. This size is used to compute the kernel for the seeing and aperture convolution.

IMPORTANT: If sigmapsf=0 or pixsize=0 or interp=False then PSF convolution is not performed.

plot: bool

When data is not None setting this keyword produces a plot with the data/model comparison at the end of the calculation.

quiet: bool

Set this keyword to avoid printing values on the console.

rbh: float, optional

This scalar gives the sigma in arcsec of the Gaussian representing the central black hole of mass MBH [See Section 3.1.2 of Cappellari (2008)] The gravitational potential is indistinguishable from a point source for radii > 2*rbh, so the default rbh=0.01 arcsec is appropriate in most current situations.

When using different units as input, e.g. pc instead of arcsec, one should check that rbh is not too many order of magnitude smaller than the spatial resolution of the data.

sigmapsf: array_like with shape (q,)

dispersion in arcseconds of the circular Gaussians describing the PSF of the kinematic observations.

IMPORTANT: If sigmapsf=0 or pixsize=0 or interp=False then PSF convolution is not performed.

IMPORTANT: PSF convolution is done by creating a 2D image, with pixels size given by step=max(sigmapsf, pixsize/2)/4, and convolving it with the PSF + aperture. If the input radii are very large compared to step, the 2D image may require a too large amount of memory. If this is the case one may compute the model predictions at small radii with a first call to jam_axi_proj with PSF convolution, and the model predictions at large radii with a second call to jam_axi_proj without PSF convolution.

step: float, optional

Spatial step for the model calculation and PSF convolution in arcsec. This value is automatically computed by default as step=max(sigmapsf,pixsize/2)/4. It is assumed that when pixsize or sigmapsf are large, high-resolution calculations are not needed. In some cases, however, e.g. to accurately estimate the central Vrms in a very cuspy galaxy inside a large aperture, one may want to override the default value to force smaller spatial pixels using this keyword.

vmax: float, optional

Maximum value of the data to plot.

vmin: float, optional

Minimum value of the data to plot.

### Output Parameters

Stored as attributes of the jam_axi_proj class.

.chi2: float

Reduced chi**2, namely per degree of freedom, describing the quality of the fit:

d, m = (data/errors)[goodbins], (model/errors)[goodbins]
chi2 = ((d - m)**2).sum()/goodbins.sum()

When no data are given in input, this is returned as np.nan.

.flux: array_like with shape (p,)

PSF-convolved MGE surface brightness of each bin in Lsun/pc^2, used to plot the isophotes of the kinematic-tracer on the model results.

.kappa: float

Ratio by which the model was scaled to fit the observed velocity [defined by equation 52 of Cappellari (2008)]

.ml: float

Best fitting M/L by which the mass was scaled to fit the observed moments.

.model: array_like with shape (p,)

Model predictions for the selected velocity moments for each input bin (xbin, ybin). This attribute is the main output from the program.

Any of the six components of the symmetric proper motion dispersion tensor {'xx', 'yy', 'zz', 'xy', 'xz', 'yz'}, or any of the three first velocity moments {'x', 'y', 'z'} can be returned in output. The desired model output is selected using the moment keyword. See the moment documentation for details.

.vel: array_like with shape (3, p)

This attribute generally contains an intermediate result of the calculation and should not be used. Instead, the output kinematic model predictions are contained in the .model attribute.

However, for advanced use only, when setting interp=False and analytic_los=False, this attribute contains the first velocity moments for all the x, y and z components, not PSF convolved, at the sky coordinates (xbin, ybin).

.vel2: array_like with shape (3, 3, p)

This attribute generally contains an intermediate result of the calculation and should not be used. Instead, the output kinematic model predictions are contained in the .model attribute.

However, for advanced use only, when setting interp=False and analytic_los=False, this attribute contains the full 3x3 second velocity moment tensor, not PSF convolved, at the sky coordinates (xbin, ybin).

## jam_axi_intr

### Purpose

This procedure calculates all the intrinsic first and second velocity moments for an anisotropic axisymmetric galaxy model.

This program is useful e.g. to model the kinematics of galaxies like our Milky Way, for which the intrinsic moments can be observed directly, or to compute starting conditions for N-body numerical simulations of galaxies.

Two assumptions for the orientation of the velocity ellipsoid are supported:

### Calling Sequence

jam = jam_axi_intr(
dens_lum, sigma_lum, qintr_lum, dens_pot, sigma_pot, qintr_pot,
mbh, Rbin, zbin, align='cyl', beta=None, data=None,
epsrel=1e-2, errors=None, gamma=None, goodbins=None,
plot=True, proj_cyl=False, quiet=False, rbh=1)

# The meaning of the output is different depending on align
sig2R, sig2z, sig2phi, v2phi = jam.model  # with align='cyl'
sig2r, sig2th, sig2phi, v2phi = jam.model  # with align='sph'

jam.plot()   # Generate data/model comparison

### Input Parameters

dens_lum: array_like with shape (n,)

vector containing the peak value of the MGE Gaussians describing the intrinsic density of the tracer population for which the kinematics is derived. The units are arbitarary as they cancel out in the final results. Typical units are e.g. Lsun/pc^3 (solar luminosities per parsec^3)

sigma_lum: array_like with shape (n,)

vector containing the dispersion (sigma) in pc of the MGE Gaussians describing the galaxy kinematic-tracer population.

qintr_lum: array_like with shape (n,)

vector containing the intrinsic axial ratio (q) of the MGE Gaussians describing the galaxy kinematic-tracer population.

surf_pot: array_like with shape (m,)

vector containing the peak value of the MGE Gaussians describing the galaxy total-mass density in units of Msun/pc^3 (solar masses per parsec^3). This is the MGE model from which the model gravitational potential is computed.

sigma_pot: array_like with shape (m,)

vector containing the dispersion in pc of the MGE Gaussians describing the galaxy total-mass density.

qintr_pot: array_like with shape (m,)

vector containing the intrinsic axial ratio of the MGE Gaussians describing the galaxy total-mass density.

mbh: float

Mass of a nuclear supermassive black hole in solar masses.

Rbin: array_like with shape (p,)

Vector with the R coordinates in pc of the bins (or pixels) at which one wants to compute the model predictions. This is the first cylindrical coordinate (R, z) with the galaxy center at (0,0).

There is a singularity at (0, 0) which should be avoided by the user in the input coordinates.

zbin: array_like with shape (p,)

Vector with the z coordinates in pc of the bins (or pixels) at which one wants to compute the model predictions. This is the second cylindrical coordinate (R, z), with the z-axis coincident with the galaxy symmetry axis.

### Optional Keywords

align: {‘cyl’, ‘sph’} optional

If align='cyl' the program computes the solution of the Jeans equations with cylindrically-aligned velocity ellipsoid, presented in Cappellari (2008). If align='sph' the spherically-aligned solution of Cappellari (2020) is returned.

beta: array_like with shape (n,)

Vector with the axial anisotropy of the individual kinematic-tracer MGE Gaussians (Default: beta=np.zeros(n)):

beta = 1 - (sigma_th/sigma_r)^2  # with align=sph
beta = 1 - (sigma_z/sigma_R)^2   # with align=cyl
data: array_like of shape (4, p), optional

Four input vectors with the observed values of:

• [sigR, sigz, sigphi, vrms_phi] in km/s, when align='cyl' (or align='sph' and proj_cyl=True).

vrms_phi is the square root of the velocity second moment in the tangential direction. If the velocities vphi_j are measured from individual stars then vrms_phi = sqrt(mean(vphi_j^2)). One can also use the relation vrms_phi = sqrt(vphi^2 + sigphi^2), where vphi = mean(vphi_j) and sigphi = std(vphi_j)

• [sigr, sigth, sigphi, vrms_phi] in km/s, when align='sph', where vrms_phi is defined above.

epsrel: float, optional

Relative error requested for the numerical quadratures, before interpolation (Default: epsrel=1e-2).

errors: array_like of shape (4, p), optional

1sigma uncertainties on data, in the same format (default 5 km/s).

gamma: array_like with shape (n,)

Vector with the tangential anisotropy of the individual kinematic-tracer MGE Gaussians (Default: gamma=np.zeros(n)):

gamma = 1 - (sigma_phi/sigma_r)^2  # with align=sph
gamma = 1 - (sigma_phi/sigma_R)^2  # with align=cyl
goodbins: array_like with shape (4, p), optional

Boolean vector of the same shape as data with values True for the bins which have to be included in the fit (if requested) and chi^2 calculation (Default: fit all bins).

interp: bool, optional

If interp=False no interpolation is performed and the model is computed at every set of input (R, z) coordinates. If interp=True (default), the model is interpolated if the number of requested input (R, z) coordinates is larger than nang*nrad.

ml: float, optional

Mass-to-light ratio M/L. If ml=None (default) the M/L is fitted to the data and the best-fitting value is returned in output. The mbh is also scaled and becomes mbh*ml. If ml=1 no scaling is applied to the model.

nang: int, optional

The number of linearly-spaced intervals in the eccentric anomaly at which the model is evaluated before interpolation (default: nang=10).

nodots: bool, optional

Set to True to hide the dots indicating the centers of the bins in the two-dimensional map (default False).

The number of logarithmically spaced radial positions at which the model is evaluated before interpolation. One may want to increase this value if the model has to be evaluated over many orders of magnitude in radius (default: nrad=20).

plot: bool, optional

If plot=True (default) and data is not None, produce a plot of the data-model comparison at the end of the calculation.

proj_cyl: bool, optional

If align='sph' and proj_cyl=True, the function projects the spherically-aligned moments to cylindrical coordinates and returns the [sig2R, sig2z, sig2phi, v2phi] components as in the case align='cyl'. This is useful for a direct comparison of results with either the spherical or cylindrical alignment, as it allows one to fit the same data with both modelling assumptions.

quiet: bool, optional

If quiet=False (default), print the best-fitting M/L and chi2 at the end for the calculation.

rbh: float, optional

This scalar gives the sigma in pc of the Gaussian representing the central black hole of mass mbh [See Section 3.1.2 of Cappellari (2008)]. The gravitational potential is indistinguishable from a point source for radii > 2*rbh, so the default rbh=1 pc is appropriate for observations taken with current telescopes.

### Output Parameters

Returned as attributes of the jam_axi_intr class.

.chi2: float

Reduced chi^2 (chi^2/DOF) describing the quality of the fit:

d = (data/errors)[goodbins]
m = (model/errors)[goodbins]
chi2 = ((d - m)**2).sum()/goodbins.sum()
.flux: array_like with shape (p,)

Vector with the MGE luminosity density at each (R, z) location in Lsun/pc^3, used to plot the isophotes on the model results.

.ml: float

Best fitting M/L. This value is fitted while ignoring sigphi and it is strictly independent of the adopted tangential anisotropy gamma.

.model: array_like with shape (4, p)
• Contains [sig2R, sig2z, sig2phi, v2phi] with align='cyl'

• Contains [sig2r, sig2th, sig2phi, v2phi] with align='sph'

where the above quantities are defined as follows:

sig2R (sig2r): array_like with shape (p,)

squared intrinsic dispersion in (km/s)^2 along the R (r) direction at each (R, z) location.

sig2z (sig2th): array_like with shape (p,)

squared intrinsic dispersion in (km/s)^2 along the z (th) direction at each (R, z) location.

sig2phi: array_like with shape (p,)

squared intrinsic dispersion in (km/s)^2 along the tangential phi direction at each (R, z) location.

v2phi: array_like with shape (p,)

the second velocity moment in (km/s)^2 along the tangential phi direction at each (R, z) location.

The mean velocity along the tangential direction can be computed as vphi = np.sqrt(v2phi - sig2phi)

NOTE: I return squared velocities instead of taking the square root, to allow for negative values (unphysical solutions).

This software is provided as is without any warranty whatsoever. Permission to use, for non-commercial purposes is granted. Permission to modify for personal or internal use is granted, provided this copyright and disclaimer are included in all copies of the software. All other rights are reserved. In particular, redistribution of the code is not allowed.

## Changelog

V6.4.0: MC, Oxford, 3 October 2022
• jam_sph_proj: Created this new function by renaming the procedure legacy.jam_sph_rms and changing its interface to be consistent with the axisymmetric version.

• jam_sph_proj: Included special isotropic formula for testing.

• jam_sph_proj: Included Osipkov-Merritt anisotropy for testing.

• jam_sph_proj: Simplified integrand with formulas of Cappellari (2020) and using recurrence relations to reduce calls to special functions.

• jam_sph_proj: More efficient TANH transformation of the integration variable following Cappellari (2020).

• jam_sph_intr: New function to compute the intrinsic moments in spherical symmetry.

• jam_axi_proj: Removed fixed minimum radius limit in pc for the interpolation without PSF convolution. This avoids the risk of artificial truncation when using small arbitrary spatial coordinates for testing.

• New procedure examples.jam_dark_halo_bayes_example.py.

• Renamed quadva as quad1d with modified interface and new singular keyword to skip transforming the integration variable.

V6.3.3: MC, Oxford, 7 July 2021
• jam_axi_proj: Clarified meaning of interp keyword in dosctring. Thanks to Kai Zhu (nao.cas.cn) for the feedback.

• jam_axi_proj: print “No PSF/pixel convolution” when interp == False.

V6.3.2: MC, Oxford, 28 April 2021
• Use the new jam_axi_proj instead of legacy software in the examples.

• Removed redundant legacy examples.

V6.3.1: MC, Oxford, 11 November 2020
• jam_axi_proj: New keyword analytic_los to chose between numeric or analytic line-of-sight integral for the second velocity moment, when align='cyl'.

• jam_axi_proj: Increased default value of nlos keyword.

• jam_axi_proj: Raise an error if rbh is too small.

• jam_axi_proj and jam_axi_intr: Removed **kwargs argument and included new nodots keyword passed to plot_velfield.

V6.2.1: MC, Oxford, 15 September 2020
• jam_axi_proj: Fixed program stop when data == ml == None. Thank to Bitao Wang (pku.edu.cn) for reporting.

V6.2.0: MC, Oxford, 17 August 2020
• jam_axi_proj: Avoid possible division by zero after convolution, when the tracer MGE is much smaller than the field of view.

• jam_axi_proj: Removed minimum-radius clipping in vmom_proj.

• jam_axi_proj: New interp keyword to force no-interpolation when using the full first and second velocity moments simultaneously.

• Made jam.plot() callable after jam_axi_proj or jam_axi_intr.

• New axisymmetric analytic vs MGE test in mge_vcirc_example.

• Fixed Numpy 1.9 VisibleDeprecationWarning.

• Updated documentation.

V6.1.5: MC, Oxford, 23 July 2020
• Fixed program stop in first velocity moment without input data, introduced in V6.1.2. Thanks to Bitao Wang (pku.edu.cn) for reporting.

• Implemented the kappa input keyword as scalar.

V6.1.4: MC, Oxford, 16 July 2020
• Added kappa to the returned parameters of jam_axi_proj.

• Compute both velocity and Vrms in jam_axi_proj_example.

V6.1.3: MC, Oxford, 13 July 2020
• Fixed program stop in legacy.jam_axi_vel due to a variable name typo introduced in V6.1.2.

V6.1.2: MC, Oxford, 20 June 2020
• jam_axi_proj: Fixed input ml being ignored. Thanks to Sabine Thater (univie.ac.at) and Takafumi Tsukui (grad.nao.ac.jp) for reporting.

• jam_axi_rms: I reduced the interpolation error before the PSF convolution for all the rotines in the legacy sub-folder, as already implemented in the new jam_axi_proj. Thanks to Takafumi Tsukui (grad.nao.ac.jp) for reporting differences.

• jam_axi_intr: Request input data = [sigR, sigz, sigphi, vrms_phi] instead of data = [sigR, sigz, sigphi, vphi].

• jam_axi_intr: exclude sigphi from ml fitting. These two changes make the fitted ml strictly independent of the adopted tangential anisotropy gamma.

V6.0.1: MC, Oxford, 23 April 2020
• Fixed model output when fitting ml. Thanks to Selina Nitschai (mpia-hd.mpg.de) for reporting.

V6.0.0: MC, Oxford, 22 April 2020
• Major changes to the whole jampy package: from this version I include the new spherically-aligned solution of the Jeans equations from Cappellari (2020, MNRAS).

• Two new functions jam_axi_intr and jam_axi_proj now provide either the intrinsic or the projected moments, respectively, for both the spherically-aligned and cylindrically-aligned JAM solutions.

• I moved the previous procedures jam_axi_rms, jam_axi_vel and jam_sph_rms to the jampy.legacy folder.

V5.0.23: MC, Oxford, 31 October 2019
• Use analytic mge_surf in convolution.

V5.0.22: MC, Oxford, 21 March 2019
• Reformatted documentation of all procedures.

V5.0.21: MC, Oxford, 14 February 2019
• Significant speedup of mge_vcirc.

• Formatted documentation.

• Created package-wide CHANGELOG: before this version, the CHANGELOG file only refers to the procedure jam_axi_rms.

V5.0.16: MC, Oxford, 27 September 2018
• Fixed clock DeprecationWarning in Python 3.7.

V5.0.15: MC, Oxford, 12 May 2018
• Dropped Python 2.7 support.

V5.0.14: MC, Oxford, 17 April 2018
• Fixed MatplotlibDeprecationWarning in Matplotlib 2.2.

• Changed imports for jam as a package.

• Removed example.

V5.0.13: MC, Oxford, 7 March 2018
• Check that PSF is normalized.

V5.0.12: MC, Oxford, 22 January 2018
• Print a message when no PSF convolution was performed.

• Broadcast kernel and MGE convolution loops.

• Fixed missing tensor in assertion test.

V5.0.11: MC, Oxford, 10 September 2017
• Make default step depend on sigmapsf regardless of pixsize.

V5.0.10: MC, Oxford, 10 August 2017
• Raise an error if goodbins is all False.

V5.0.9: MC, Oxford, 17 March 2017
• Included flux_obs keyword. Updated documentation.

• Fixed DeprecationWarning in Numpy 1.12.

V5.0.8: MC, Oxford, 17 February 2017
• Use odd kernel size for convolution.

• Fixed corner case with coordinates falling outside the interpolation region, due to finite machine precision.

V5.0.7: MC, Oxford, 23 February 2016
• Scale rmsModel by the input M/L also when rms is not given. Thanks to Alex Grainger (Oxford) for pointing out the inconsistency.

• Pass **kwargs for plotting.

V5.0.6: MC, Oxford, 18 September 2015
• Plot bad bins on the data.

V5.0.5: MC, Oxford, 23 May 2015
• Changed meaning of goodbins to be a boolean vector.

V5.0.4: MC, Sydney, 5 February 2015
• Introduced further checks on matching input sizes.

V5.0.3: MC, Oxford, 31 October 2014
• Modified final plot layout.

V5.0.2: MC, Oxford, 25 May 2014
• Support both Python 2.7 and Python 3.

V5.0.1: MC, Oxford, 24 February 2014
• Plot bi-symmetrized V_rms as in IDL version.

V5.0.0: MC, Paranal, 11 November 2013
• Translated from IDL into Python.

V4.1.5: MC, Paranal, 8 November 2013
• Use renamed CAP_* routines to avoid potential naming conflicts.

V4.1.4: MC, Oxford, 12 February 2013
• Include _EXTRA and RANGE keywords for plotting.

V4.1.3: MC, Oxford, 1 February 2013
• Output FLUX in Lsun/pc^2.

V4.1.2: MC, Oxford, 28 May 2012
• Updated documentation.

V4.1.1: MC, Oxford, 8 December 2011
• Only calculates FLUX if required.

V4.1.0: MC, Oxford 19 October 2010
• Included TENSOR keyword to calculate any of the six components of the symmetric proper motion dispersion tensor (as in note 5 of the paper).

V4.0.9: MC, Oxford, 15 September 2010
• Plot and output with FLUX keyword the PSF-convolved MGE surface brightness.

V4.0.8: MC, Oxford, 09 August 2010
• Use linear instead of smooth interpolation. After feedback from Eric Emsellem.

V4.0.7: MC, Oxford, 01 March 2010
• Forces q_lum && q_pot < 1.

V4.0.6: MC, Oxford, 08 February 2010
• The routine TEST_JAM_AXISYMMETRIC_RMS with the usage example now adopts a more realistic input kinematics.

• Updated documentation.

V4.0.5: MC, Oxford, 6 July 2009
• Skip unnecessary interpolation when computing a few points without PSF convolution. After feedback from Eric Emsellem.

V4.0.4: MC, Oxford, 29 May 2009
• Compute FLUX even when not plotting.

V4.0.3: MC, Oxford 4 April 2009

V4.0.2: MC, Oxford, 21 November 2008
• Added keywords NRAD and NANG. Thanks to Michael Williams for reporting possible problems with too coarse interpolation.

V4.0.1: MC, Windhoek, 29 September 2008
• Bug fix: when ERMS was not given, the default was not properly set. Included keyword STEP. The keyword FLUX is now only used for output: the surface brightness for plotting is computed from the MGE model.

V4.0.0: MC, Oxford, 11 September 2008
• Implemented PSF convolution using interpolation on a polar grid. Dramatic speed-up of calculation. Further documentation.

V3.2.0: MC, Oxford, 14 August 2008
• Updated documentation.

V3.1.3: MC, Oxford, 12 August 2008
• First released version.

V2.0.0: MC, Oxford, 20 September 2007
• Introduced new solution of the MGE Jeans equations with constant anisotropy sig_R = b*sig_z.

V1.0.0: Michele Cappellari, Vicenza, 19 November 2003
• Written and tested

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