Spherical overdensity masses¶
This module implements basic aspects of spherical overdensity mass definitions for dark matter halos (please see Halo Mass Definitions for an introduction).
Basics¶
For example, we can compute the spherical overdensity radius of a halo with particular mass or vice versa:
from colossus.halo import mass_so
R200m = mass_so.M_to_R(1E12, 0.0, '200m')
Mvir = mass_so.R_to_M(400.0, 1.5, 'vir')
The other functions in this module allow us to parse the mass definition strings and compute the
density thresholds, but typically the user will not need to evaluate those functions manually
since most SOrelated functions in Colossus accept mdef
as an argument. Please see the
Tutorials for more extensive code examples.
Module contents¶
parseMassDefinition (mdef) 
The type and overdensity of a given spherical overdensity mass definition. 
parseRadiusMassDefinition (rmdef) 
Parse a radius or mass identifier as well as the mass definition. 
densityThreshold (z, mdef) 
The threshold density for a given spherical overdensity mass definition. 
deltaVir (z) 
The virial overdensity in units of the critical density. 
M_to_R (M, z, mdef) 
Convert spherical overdensity mass to radius. 
R_to_M (R, z, mdef) 
Convert spherical overdensity radius to mass. 
dynamicalTime (z, mdef[, definition]) 
The dynamical time of a halo. 
Module reference¶

halo.mass_so.
parseMassDefinition
(mdef)¶ The type and overdensity of a given spherical overdensity mass definition.
Parameters:  mdef: str
The mass definition. See Halo Mass Definitions for details.
Returns:  mdef_type: str
Can either be based on the mean density (
mdef_type='m'
), the critical density (mdef_type='c'
) or the virial overdensity (mdef_type='vir'
). mdef_delta: int
The overdensity; if
mdef_type=='vir'
, the overdensity depends on redshift, and this parameter isNone
.

halo.mass_so.
parseRadiusMassDefinition
(rmdef)¶ Parse a radius or mass identifier as well as the mass definition.
Parameters:  rmdef: str
The radius or mass identifier
Returns:  radius_mass: str
Can be
R
for radius orM
for mass. mdef: str
The mdef the mass or radius are based on. See Halo Mass Definitions for details.
 mdef_type: str
Can either be based on the mean density (
mdef_type='m'
), the critical density (mdef_type='c'
) or the virial overdensity (mdef_type=='vir'
). mdef_delta: int
The overdensity; if
mdef_type=='vir'
, the overdensity depends on redshift, and this parameter isNone
.

halo.mass_so.
densityThreshold
(z, mdef)¶ The threshold density for a given spherical overdensity mass definition.
Parameters:  z: array_like
Redshift; can be a number or a numpy array.
 mdef: str
The mass definition. See Halo Mass Definitions for details.
Returns:  rho: array_like
The threshold density in physical \(M_{\odot}h^2/{\rm kpc}^3\); has the same dimensions as
z
.
See also
deltaVir
 The virial overdensity in units of the critical density.

halo.mass_so.
deltaVir
(z)¶ The virial overdensity in units of the critical density.
This function uses the fitting formula of Bryan & Norman 1998 to determine the virial overdensity. While the universe is dominated by matter, this overdensity is about 178. Once dark energy starts to matter, it decreases.
Parameters:  z: array_like
Redshift; can be a number or a numpy array.
Returns:  Delta: array_like
The virial overdensity; has the same dimensions as
z
.
See also
densityThreshold
 The threshold density for a given mass definition.

halo.mass_so.
M_to_R
(M, z, mdef)¶ Convert spherical overdensity mass to radius.
This function returns a spherical overdensity halo radius for a halo mass
M
. Note that this function is independent of the form of the density profile.Parameters:  M: array_like
Mass in \(M_{\odot}/h\); can be a number or a numpy array.
 z: float
Redshift
 mdef: str
The mass definition. See Halo Mass Definitions for details.
Returns:  R: array_like
Halo radius in physical kpc/h; has the same dimensions as
M
.
See also
R_to_M
 Convert spherical overdensity radius to mass.

halo.mass_so.
R_to_M
(R, z, mdef)¶ Convert spherical overdensity radius to mass.
This function returns a spherical overdensity halo mass for a halo radius
R
. Note that this function is independent of the form of the density profile.Parameters:  R: array_like
Halo radius in physical kpc/h; can be a number or a numpy array.
 z: float
Redshift
 mdef: str
The mass definition. See Halo Mass Definitions for details.
Returns:  M: array_like
Mass in \(M_{\odot}/h\); has the same dimensions as
R
.
See also
M_to_R
 Convert spherical overdensity mass to radius.

halo.mass_so.
dynamicalTime
(z, mdef, definition='crossing')¶ The dynamical time of a halo.
The dynamical time can be estimated in multiple ways, but is almost always based on the ratio of a distance to circular velocity. The relevant distance can be defined in different ways as indicated with the
definition
parameter. The dynamical time is more succinctly expressed as a multiple of the Hubble time which depends on the overdensity threshold and redshift.Parameters:  z: array_like
Redshift; can be a number or a numpy array.
 mdef: str
The mass definition. See Halo Mass Definitions for details.
 definition: str
An identifier for a definition of the dynamical time. Valid definitions are
crossing
(the crossing time),peri
(the time to reach the halo center, half the crossing time) andorbit
(the time to orbit around the halo, crossing time times \(\pi\)).
Returns:  t_dyn: array_like
Dynamical time in Gyr; has the same dimensions as
z
.