Stellib¶
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class
beast.physicsmodel.stars.stellib.
Stellib
(*args, **kargs)[source]¶ Bases:
object
Basic stellar library class
Contructor
Attributes Summary
nbytes
return the number of bytes of the object Methods Summary
genQ
(qname, r, **kwargs)Generate a composite value from a previously calculated genSpectrum
(T0[, g0, Z0, weights])Generate a composite sprectrum Does the interpolation or uses a previously calculated interpolation Works on 1 desired star or a population of stars gen_spectral_grid_from_given_points
(pts[, …])Reinterpolate a given stellar spectral library on to an Isochrone grid get_boundaries
([dlogT, dlogg])Returns the closed boundary polygon around the stellar library with given margins get_radius
(logl, logt)Returns the radius of a star given its luminosity and temperature interp
(T0, g0, Z0, L0[, dT_max, eps])Interpolation of the T,g grid interpMany
(T0, g0, Z0, L0[, dT_max, eps, …])run interp on a list of inputs and returns reduced results plot_boundary
([ax, dlogT, dlogg])Parameters: points_inside
(xypoints[, dlogT, dlogg])Returns if a point is inside the polygon defined by the boundary of the library Attributes Documentation
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nbytes
¶ return the number of bytes of the object
Methods Documentation
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genQ
(qname, r, **kwargs)[source]¶ - Generate a composite value from a previously calculated
- interpolation Works on 1 desired star or a population of stars
Parameters: qname: str
quantity name from self.grid
r: ndarray
the result from a previous interpolation
Returns: val: ndarray
an array containing the value
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genSpectrum
(T0, g0=None, Z0=None, weights=None, **kwargs)[source]¶ Generate a composite sprectrum Does the interpolation or uses a previously calculated interpolation Works on 1 desired star or a population of stars
if T0 and g0 are iterable, it calls interpMany
Parameters: T0: float or sequence
log(Teff) of each star or a 2d-array containing the result from a previous interpolation
g0: float or sequence
log(g) of each stars
Z0: float or sequence
metallicity
weights: float or sequence
individual weights of each star
**kwargs: forwarded to interpMany
Returns: s: ndarray
an array containing the composite spectrum
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gen_spectral_grid_from_given_points
(pts, bounds={'dlogT': 0.1, 'dlogg': 0.3})[source]¶ Reinterpolate a given stellar spectral library on to an Isochrone grid
Parameters: pts: dict like structure of points
dictionary like or named data structure of points to interpolate at. pts must contain: logg surface gravity in log-scale logT log of effective temperatures (in Kelvins) logL log of luminosity in Lsun units Z metallicity
bounds: dict
sensitivity to extrapolation (see grid.get_stellib_boundaries) default: {dlogT:0.1, dlogg:0.3}
Returns: g: SpectralGrid
Spectral grid (in memory) containing the requested list of stars and associated spectra
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get_boundaries
(dlogT=0.1, dlogg=0.3, **kwargs)[source]¶ Returns the closed boundary polygon around the stellar library with given margins
Parameters: s: Stellib
Stellar library object
dlogT: float
margin in logT
dlogg: float
margin in logg
Returns: b: ndarray[float, ndim=2]
closed boundary edge points: [logT, logg]
Note
as computing the boundary could take time, it is saved in the object and only recomputed when parameters are updated
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get_radius
(logl, logt)[source]¶ Returns the radius of a star given its luminosity and temperature
- Assuming a black body, it comes:
- R ^ 2 = L / ( 4 pi sigma T ^ 4 ),
- with:
- L, luminosity in W, pi, 3.141592… sig, Stephan constant in W * m**-2 * K**-4 T, temperature in K
Parameters: logl: ndarray[float, ndim=1]
log luminosities from the isochrones, in Lsun
logt: ndarray[float, ndim=1]
log temperatures from the isochrones, in K
Returns: radii: ndarray[float, ndim=1]
array of radii in m (SI units)
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interp
(T0, g0, Z0, L0, dT_max=0.1, eps=1e-06)[source]¶ Interpolation of the T,g grid
Interpolate on the grid and returns star indices and associated weights, and Z. 3 to 12 stars are returned. It calls _interp_, but reduce the output to the relevant stars.
Parameters: T0 double
log(Teff) to obtain
g0 double
log(g) to obtain
T double
log(Teff) of the grid
g double
log(g) of the grid
dT_max: float
If, T2 (resp. T1) is too far from T compared to T1 (resp. T2), i2 (resp. i1) is not used. (see below for namings)
eps: foat
temperature sensitivity under which points are considered to have the same temperature
Returns: Returns 3 to 12 star indexes and associated weights
see __interp__
TODO: compute new weights accounting for Z
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interpMany
(T0, g0, Z0, L0, dT_max=0.1, eps=1e-06, weights=None, pool=None, nthreads=1)[source]¶ run interp on a list of inputs and returns reduced results
Interpolation of the T,g grid at Z0 metallicity
Interpolate on the grid and returns star indices and associated weights, and Z. 3 to 12 stars are returned. It calls _interp_, but reduce the output to the relevant stars.
Parameters: T0 ndarray(float)
log(Teff) to obtain
g0 ndarray(float)
log(g) to obtain
Z0 ndarray(float)
metallicity values
L0 ndarray(float)
luminosity values
dT_max: float
If, T2 (resp. T1) is too far from T compared to T1 (resp. T2), i2 (resp. i1) is not used. (see below for namings)
eps: float
temperature sensitivity under which points are considered to have the same temperature
weights: ndarray(float)
luminosity weigths to apply after interpolation
pool: Pool-like object
specify a multiprocessing pool for parallel processing
nthreads: int
number of processes to use by default
Returns: r: ndarray
Returns 3 to 12 star indexes and associated weights
see __interp__
TODO: compute new weights accounting for Z
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plot_boundary
(ax=None, dlogT=0.0, dlogg=0.0, **kwargs)[source]¶ Parameters: dlogT: float
margin in logT (see get_boundaries)
dlogg: float
margin in logg (see get_boundaries)
agg_filter: unknown
alpha: float or None
animated: [True | False]
antialiased or aa: [True | False] or None for default
axes: an :class:`~matplotlib.axes.Axes` instance
clip_box: a :class:`matplotlib.transforms.Bbox` instance
clip_on: [True | False]
clip_path: [ (:class:`~matplotlib.path.Path`, :class:`~matplotlib.transforms.Transform`) | :class:`~matplotlib.patches.Patch` | None ]
color: matplotlib color spec
contains: a callable function
edgecolor or ec: mpl color spec, or None for default, or ‘none’ for no color
facecolor or fc: mpl color spec, or None for default, or ‘none’ for no color
figure: a :class:`matplotlib.figure.Figure` instance
fill: [True | False]
gid: an id string
hatch: [ ‘/’ | ‘’ | ‘|’ | ‘-‘ | ‘+’ | ‘x’ | ‘o’ | ‘O’ | ‘.’ | ‘*’ ]
label: string or anything printable with ‘%s’ conversion.
linestyle or ls: [‘solid’ | ‘dashed’ | ‘dashdot’ | ‘dotted’]
linewidth or lw: float or None for default
lod: [True | False]
path_effects: unknown
picker: [None|float|boolean|callable]
rasterized: [True | False | None]
snap: unknown
transform: :class:`~matplotlib.transforms.Transform` instance
url: a url string
visible: [True | False]
zorder: any number
.. seealso::
Patch
For additional kwargs
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points_inside
(xypoints, dlogT=0.1, dlogg=0.3)[source]¶ Returns if a point is inside the polygon defined by the boundary of the library
Parameters: xypoints: sequence
a sequence of N logg, logT pairs.
dlogT: float
margin in logT
dlogg: float
margin in logg
Returns: r: ndarray(dtype=bool)
a boolean ndarray, True for points inside the polygon. A point on the boundary may be treated as inside or outside.
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