!---------------------------------------------------------------- !
!   Spectra and JWST fluxes for a population II galaxy based on   !
!  the Zackrisson et al. (2001, 2008) population synthesis model  !
!-----------------------------------------------------------------!

Model parameters
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This is a Zstars = Zgas = 0.001 (population II), single-age stellar population with initial stellar mass 1e6 Msolar.
A Salpeter IMF is adopted for stars in the mass interval from 0.08 to 120 Msolar. Nebular emission is included self-consistently with evolving emission-line ratios, assuming a hydrogen number density of 100 cm^-3, a filling factor of 0.01 and zero Lyman continuum leakage (i.e. covering factor 1.0). See Zackrisson et al. (2001) for more information on these parameters.

Spectra
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The file spectra_Z01_001_001_2.35_120_0.08_inst_n2_f0.01_1e6M_sn.dat contains rest-frame spectra (with and without nebular emission) as a function of time. 

The column F_tot includes both nebular emission and stars. Since the nebula absorbs flux shortward of the Lyman limit and re-emits it at longer wavelengths (in the form of emission lines and a nebular continuum), the fluxes are very low at wavelengths below 912 Å. The column F_stars includes the flux from stars only. By comparing the two columns F_tot and F_stars, the impact of nebular emission can be assessed, as in Zackrisson et al. (2008).

Magnitudes
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The files JWST_MIRI_ABmag_Z01_001_001_2.35_120_0.08_inst_n2_f0.01_1e6M_sn.dat and JWST_NIRcam_ABmag_Z01_001_001_2.35_120_0.08_inst_n2_f0.01_1e6M_sn.dat contain the integrated JWST broadband AB magnitudes (in MIRI and NIRCam filters, respectively) as a function of age and redshift. The stellar population mass as a function of time is also listed.

When calculating these magnitudes, the intergalactic medium (IGM) shortward of Lyman alpha (1216 Å in the rest frame) has been assumed to be completely opaque at z>6. The escape fraction of the Lyman alpha line itself is also assumed to be zero above this redshift limit. 

At z = 0.0, the magnitudes are based on an assumed distance of 10 pc. At higher redshifts, the magnitudes are based on luminosity distances calculated using Omega_M=0.27, Omega_Lambda=0.73 and H_0=72 km s^-1 Mpc^-1. Whenever the flux drops to zero due to IGM absorption in one of the JWST filters, the corresponding AB magnitude is set to 999.000.

Credit
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If you use these models, please cite:
Zackrisson, E., Bergvall, N., Olofsson, K. & Siebert, A. 2001, A&A 375, 814
Zackrisson, E., Bergvall, N. & Leitet, E. 2008, ApJL, 676, 9 

Contact
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Please contact Erik Zackrisson (ez@astro.su.se) if you have any questions or requests.
