Synthetic spectra from SYNTHE
The current extent of the grids is: Teff = 3500 (500) 8500 and log g = 2.0 (0.5) 4.5, and spectra are computed at a resolution of 90000.
[Fe/H] v_turb Colour
blue red CaT
380 - 500 nm 637 - 677 nm 840 - 880 nm +0.0 2 km/s p00.vt2.blue p00.vt2.red p00.vt2.CaT +0.0 5 km/s p00.vt5.blue p00.vt5.red p00.vt5.CaT -0.3 2 km/s m03.vt2.blue m03.vt2.red m03.vt2.CaT -0.3 5 km/s m03.vt5.blue m03.vt5.red m03.vt5.CaT -0.5 2 km/s m05.vt2.blue m05.vt2.red m05.vt2.CaT -0.5 5 km/s m05.vt5.blue m05.vt5.red m05.vt5.CaT A limited grid of synthetic spectra computed using John Lester's version of Kurucz' codes MOLDECK, SYNTHE and SPECSYN. The grid is located at: http://star.arm.ac.uk/~csj/synthe_models/, where you may find folders in the form
mMM.vtV.WAV/Within each folder are files with names of the form....
mMM: p00 corresponds to [Fe/H] = 0.0
m03 to [Fe/H] = -0.3, etc...
vtV: vt2 represents v_turb = 2 km/s
WAV: blue : 380 - 500 nm
red : 637 - 677 nm
CaT : 840 - 880 nm
mMMTTGG.vtV.WAV and/or mMMTTGG.WAV(If both files exist they should be equivalent). Thus the blue spectrum for a solar composition model with Teff=5500, log g=4.0, v_turb = 2 km/s would be found at .... http://star.arm.ac.uk/~csj/synthe_models/p00.vt2.blue/p005545.vt2.blue. The contents of each file is as follows:
TT: Teff / 100K
GG: log g * 10# sdsc grid [+0.0] vturb 2.0 km/s l/h 1.25
# teff = 5500.
# log g = 4.5000
# lambda/delta lambda = 90000.
# number of data points = 24701
# lambda(nm) physical flux continuum flux residual flux
380.00000 2.29043E-05 4.38229E-05 0.52266
380.00422 2.48818E-05 4.38239E-05 0.56777
499.99748 6.86839E-05 6.90442E-05 0.99478
500.00304 6.87264E-05 6.90451E-05 0.99538
The model atmospheres on which these spectra were based were taken from Kurucz' standard grid of ATLAS models:
Kurucz, R.L., 1991, in Stellar Atmopsheres: Beyond Classical Models, ed., L.Crivellari, I.Hubeny, & D.G.Hummer, NATO ASI Ser., vol. C341 (Kluwer, Dordrecht), 441.The formal solution program SYNTHE with which they were computed was presented on:
Kurucz, R.L., 1993, SAO KURUCZ CD-ROM, No 18Its implementation on Unix systems has been described by:
Jeffery, C.S., Lester, J., & Short, I. 1996, CCP7 Newslett., No. 24, 13The models presented here were computed originally for the analysis of the cool component of the remarkable binary BI Lyn, which comprises an early B-type hydrogen-deficient giant and a rapidliy rotating G giant. The work is described by
Jeffery, C.S., & Aznar Cuadrado, R. 2001, A&A 378, 936
This page is maintained by:
Simon Jeffery (firstname.lastname@example.org)
Last modified: 08/01/04