BEAST Analysis Tools

The BEAST has several tools for analyzing the results of the BEAST runs.

Star type probability

One use case of the BEAST results is to find a set of stars of a particular type with some probability. For instance, the user may want stars that are 90% likely to be high mass stars.

There are two types of stars currently implemented, though more can easily be added. When there are cuts along two parameters, the 2D PDFs are utilized. If 2D PDFs of the required parameters don’t exist, the probability of that star type will be NaN.

  • Extinguished high mass stars (star_type_probability.ext_O_star): Stars above a certain mass (default M_ini > 10 solar masses) with some minimum foreground dust column (default Av > 0.5 magnitudes). You may also wish to set a maximum Av to avoid artifacts (such as the dusty AGB stars). These stars are candidates for follow-up UV spectroscopy for extinction curves.

  • Dusty AGB stars (star_type_probability.dusty_agb): As described in Known Issues, the BEAST does not include models for dusty AGB stars, and many of them are incorrectly fit as heavily extinguished hot stars. This finds stars using their extinction (default Av > 7) and effective temperature (default logT between 3.7 and 4.2).

Below, we show an example for extinction curve candidates in phat_small.

>>> from import star_type_probability 
>>> from import fits 
>>> # calculate probabilities
>>> star_prob = star_type_probability.star_type_probability( 
        ext_O_star_params={'min_M_ini':10, 'min_Av':0.5, 'max_Av':5}
>>> # stars with >80% likelihood of being extinguished massive stars
>>> np.where(star_prob['ext_O_star'] > 0.8)[0] 
array([29, 54])
>>> # confirm their best fit masses and Av
>>> with'beast_example_phat_stats.fits') as hdu: 
        print('Masses:', hdu[1].data['M_ini_p50'][[29,54]])
        print('Av:', hdu[1].data['Av_p50'][[29,54]])
Masses: [16.84200042 15.23882141]
Av: [3.98209536 3.99047602]

Spectral type comparison

When there are spectrally typed stars in our catalogs, we would like to compare the BEAST parameters to those inferred from the spectral types. The code in beast/tools/ simplifies this comparison. It ingests the photometry catalog, stats catalog, spectral types and coordinates of comparison stars, and several settings. Here is a summary of its procedure:

  1. Convert the spectral types into an effective temperature (T_eff) and surface gravity (logg). This is done by interpolating on tables of T_eff (from Stellar Spectral Classification; R. Gray & C. Corbally) and logg (from Allen’s Astrophysical Quantities; A. Cox).

  2. For each spectrally-typed star, find all matches in the photometry catalog within a user-defined radius (default 1”). Since spectrally-typed stars are generally bright, choose the brightest source in the user-defined filter (default=’F475W’). If no match is found, all output values for this star will be set to None.

  3. Save the p16, p50, and p84 values of logT and logg for the matched BEAST star. Also calculate the number of standard deviations between the BEAST fits and star values (assuming no uncertainty on the star values).

  4. If the keyword output_filebase is set, the results will be saved into a file. Otherwise, the results will be returned in a dictionary.

Below is an example for phat_small. The spectral types are not from any real catalog, and are for illustrative purposes only. The output dictionary shows the information about the spectrally-typed star, the indices of the matched BEAST star (in both the photometry and stats catalogs), the BEAST fits, and the number of standard deviations (sigma) apart they are. The first star (A2II) is a good match to BEAST star 27. The second star (G7II) is a close, but imperfect, match to BEAST star 8. The third star (B4V) is outside the catalog footprint and therefore has no match.

>>> from import compare_spec_type 
>>> compare_spec_type.compare_spec_type( 
        'data/b15_4band_det_27_A.fits',  # Photometry catalog
        'beast_example_phat/beast_example_phat_stats.fits', # Stats catalog
        [11.2335881, 11.23342557, 1.0],  # RA
        [41.9001895, 41.90006316, 1.0],  # Dec
        ['A', 'G', 'B'],                 # Spectral type
        [2, 7, 4]                        # Subtype
        ['II', 'II', 'V'],               # Luminosity class
        match_radius=0.2                 # Match radius (arcsec)
{'spec_ra': [11.2335881, 11.23342557, 1.0],
 'spec_dec': [41.9001895, 41.90006316, 1.0],
 'spec_type': ['A 2 II', 'G 7 II', 'B 4 V'],
 'spec_teff': [9000.0, 4916.666666666667, None],
 'spec_logg': [2.7164474106543732, 1.7184474106543735, None],
 'phot_cat_ind': [27, 8, None],
 'stats_cat_ind': [27, 8, None],
 'beast_teff_p50': [9046.250020338754, 4528.230977991138, None],
 'beast_teff_p16': [8643.670633196869, 4335.617282355577, None],
 'beast_teff_p84': [9536.391362054928, 4729.401710221546, None],
 'beast_logg_p50': [2.714286917261312, 1.7684285714285717, None],
 'beast_logg_p16': [2.636272525730954, 1.7014832653061227, None],
 'beast_logg_p84': [2.799534708811963, 1.8353738775510207, None],
 'teff_sigma': [-0.11488422362383206, 1.9308757510045778, None],
 'logg_sigma': [0.025343687546173433, -0.7465969411324851, None]}