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Package ivs :: Package spectra :: Module model
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Module model

source code

Interface to stellar spectra library and functions to manipulate them.

Make a plot of the domains of all spectral grids. First collect all the grid names

>>> grids = get_gridnames()

Prepare the plot

>>> p = pl.figure()
>>> color_cycle = [pl.cm.spectral(j) for j in np.linspace(0, 1.0, len(grids))]
>>> p = pl.gca().set_color_cycle(color_cycle)

And plot all the grid points. We have to set some custom default values for some grids.

>>> for grid in grids:
...    vturb = 'ostar' in grid and 10 or 2
...    t = 0.
...    if 'marcs' in grid: t = 1.
...    teffs,loggs = get_grid_dimensions(grid=grid,vturb=vturb,t=t)
...    p = pl.plot(np.log10(teffs),loggs,'o',ms=7,label=grid)

Now take care of the plot details

>>> p = pl.xlim(pl.xlim()[::-1])
>>> p = pl.ylim(pl.ylim()[::-1])
>>> p = pl.xlabel('Effective temperature [K]')
>>> p = pl.ylabel('log( Surface gravity [cm s$^{-1}$]) [dex]')
>>> xticks = [3000,5000,7000,10000,15000,25000,35000,50000,65000]
>>> p = pl.xticks([np.log10(i) for i in xticks],['%d'%(i) for i in xticks])
>>> p = pl.legend(loc='upper left',prop=dict(size='small'))
>>> p = pl.grid()

]include figure]]ivs_spectra_model_grid.png]

Functions [hide private]
    Interface to library
 
set_defaults(**kwargs)
Set defaults of this module.		 source code
list of str
get_gridnames()
Return a list of available grid names.		 source code
 
get_file(**kwargs)
Retrieve the filename containing the specified SED grid.		 source code
 
get_table(teff=None, logg=None, vrad=0, vrot=0, **kwargs)
Retrieve synthetic spectrum.		 source code
(ndarray,ndarray)
get_grid_dimensions(**kwargs)
Retrieve possible effective temperatures and gravities from a grid.		 source code
(1Darray,1Darray,1Darray,3Darray,InterpolatingFunction)
get_grid_mesh(wave=None, teffrange=None, loggrange=None, **kwargs)
Return InterpolatingFunction spanning the available grid of spectrum models.		 source code
Variables [hide private]
  logger = logging.getLogger("SPEC.MODEL")
  defaults = dict(grid= 'atlas', z=+ 0.0, vturb= 2, band= 'vis',...
  basedir = 'spectables'
Function Details [hide private]

set_defaults(**kwargs)

source code 

Set defaults of this module.

If you give no keyword arguments, the default values will be reset.

get_gridnames()

source code 

Return a list of available grid names.

Returns: list of str
list of grid names

get_file(**kwargs)

source code 

Retrieve the filename containing the specified SED grid.

Available grids and example keywords:

  • grid='fastwind': no options
  • grid='cmfgen': no options
  • grid='marcs': options c, atm (p or s)
  • grid='ostar2002': options z,v
  • grid='bstar2006a': options z,v
  • grid='bstar2006b': options z,v
  • grid='bstar2006': options z,v,a
  • grid='atlas': options z
  • grid='heberb': no options
  • grid='hebersdb': no options
  • grid='tmapsdb': no options

Details for grid 'bstar2006':

  • metallicity in Z/Z0 with Z0 solar. z=0,0.001,0.01,0.033,0.1,0.2,0.5,1.,2
  • microturbulent velocity: v=2 or v=10 km/s
  • abundance: a='' or a='CN'. In the latter, the Helium abundance is increased to He/H=0.2, the nitrogen abundance is increased by a factor of 5, and the carbon abundance is halved (CNO cycle processed material brought to the stellar surface)

Details for grid 'heberb': LTE Grid computed for B-type stars by Uli Heber, reff: Heber et al. 2000

Details for grid 'hebersdb': LTE Grid computed for sdB stars by Uli Heber, reff: Heber et al. 2000

Details for grid 'tmapsdb': NLTE Grid computed for sdB stars using the TMAP (TUEBINGEN NLTE MODEL ATMOSPHERE PACKAGE) code. reff: Werner K., et al. 2003 and Rauch T., Deetjen J.L. 2003

Parameters:
  • grid (string) - gridname, or path to grid.

get_table(teff=None, logg=None, vrad=0, vrot=0, **kwargs)

source code 

Retrieve synthetic spectrum.

Wavelengths in angstrom, fluxes in eddington flux: erg/s/cm2/A.

It is possible to rotationally broaden the spectrum by supplying at least 'vrot' and optionally also other arguments for the rotation.rotin function. Supply vrot in km/s

It is possibility to include a radial velocity shift in the spectrum. Supply 'vrad' in km/s. (+vrad means redshift). Uses spectra.tools.doppler_shift

get_grid_dimensions(**kwargs)

source code 

Retrieve possible effective temperatures and gravities from a grid.

Returns: (ndarray,ndarray)
effective temperatures, gravities

get_grid_mesh(wave=None, teffrange=None, loggrange=None, **kwargs)

source code 

Return InterpolatingFunction spanning the available grid of spectrum models.

WARNING: the grid must be entirely defined on a mesh grid, but it does not need to be equidistant.

It is thus the user's responsibility to know whether the grid is evenly spaced in logg and teff

You can supply your own wavelength range, since the grid models' resolution are not necessarily homogeneous. If not, the first wavelength array found in the grid will be used as a template.

It might take a long a time and cost a lot of memory if you load the entire grid. Therefore, you can also set range of temperature and gravity.

Parameters:
  • wave (ndarray) - wavelength to define the grid on
  • teffrange (tuple of floats) - starting and ending of the grid in teff
  • loggrange (tuple of floats) - starting and ending of the grid in logg
Returns: (1Darray,1Darray,1Darray,3Darray,InterpolatingFunction)
wavelengths, teffs, loggs and fluxes of grid, and the interpolating function

Variables Details [hide private]

defaults

Value:
dict(grid= 'atlas', z=+ 0.0, vturb= 2, band= 'vis', t= 0.0, a= 0.0, c=\
 0.5, atm= 'p')

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