== Selected macronova models data from Wollaeger et al. (2017), arXiv:1705.07084 ==

The light curves and spectra were computed using the Los Alamos Institutional 
Computing resources. This data distribution has been approved for an unlimited 
public release (LA-UR-17-27847)


Model    morphology    components         nuc.heating   m_dyn+m_wind   v_dyn+v_wind
-----------------------------------------------------------------------------------
 SAd     spherical     dynamical-ejecta   power-law        0.014          0.125
 SAw1    spherical     wind               power-law        0.014          0.125
 SAw2    spherical     wind               power-law        0.014          0.125
 gamA2   axisymmetric  dyn.ejecta+wind    FRDM          0.013+0.005    0.132+0.08
 gamB2   axisymmetric  dyn.ejecta+wind    FRDM          0.014+0.005    0.125+0.08
 DZ2     axisymmetric  dyn.ejecta+wind    power-lawx10  0.013+0.005    0.132+0.08
===================================================================================

Contents of the archive:
1. Broadband magnitudes and bolometric luminosity for spherically-symmetric models:
   - SAd_mags_2016-11-20.dat
   - SAw1_mags_2016-11-20.dat
   - SAw2_mags_2016-11-20.dat
   Format of the columns:
   1:time[d] 2:bolometric luminosity[erg/s]    
   2-9: AB magnitudes in eight bands: grizyJHK

2. Spectra for spherically-symmetric models:
   - SAd_spec_2016-11-20.dat
   - SAw1_spec_2016-11-20.dat
   - SAw2_spec_2016-11-20.dat
   Data is organized in blocks, separated by two empty lines.
   Each block corresponds to a single timestep, starts with an header line.
   Columns in each block:
   1-2: wavelength bin[cm]
   3: flux at R=10pc [erg/(s*Angstrom*cm2)]

3. Broadband magnitudes and bolometric luminosity for axisymmetric models:
   - gamA2_mags_2017-03-20.dat   
   - gamB2_mags_2017-03-20.dat
   - DZ2_mags_2017-03-20.dat
   Data is organized in blocks, separated by two empty lines. The first block 
   represents bolometric luminosity as a function of time. The rest eight 
   blocks are broadband magnitudes (grizyJHK).
   
   Format of the columns in the first block:
   1:iteration 2:time[d] 
   3-29: bolometric luminosity in k-th angular bin [erg/s]
   
   Format of the columns in the rest of the blocks:
   1:iteration 2:time[d]  
   3-29: AB magnitude for k-th angular bin

4. Spectra for axisymmetric models:
   - gamA2_spec_2017-03-20.dat   
   - gamB2_spec_2017-03-20.dat
   - DZ2_spec_2017-03-20.dat
   Data is organized in blocks, separated by two empty lines.
   Each block corresponds to a single timestep, starts with an header line.
   1-2: wavelength bin [cm]
   3-29: flux into angular bin at R=10pc [erg/(s*Angstrom*cm2)]

5. Axisymmetric bins: each bin covers equal amount of solid angle,
   or equally spaced intervals in cos\theta.
   I.e., the i-th bin (from 1 to Nbins) covers:

      \cos{\theta} \in [1 - i*2/Nbins, 1 - (i-1)*2/Nbins].

   To put this differently, for the i-th bin \theta \in [a_i, b_i] the formulae are:

    a_i = arccos[1 - i*2/Nbins]
    b_i = arccos[1 - (i-1)*2/Nbins]

   We are using Nbins = 27, our bins are, for instance:
    - first bin: theta from 0 to 22.19';
    - second bin: from 22.19' to 31.59'
      ...
    - 14th bin: from 87.87' to 92.12'
      ...
    - 27th bin: from 157.81' to 180'.

