5/27/2011 Tokoku
PEGASE v.2
Fioc and Rocca-Volmerange (1997)
CIAGLE
Constant Star Formation Age = 10 Myr
Z = 0.02, 0.01, 0.001
Calzetti et al. (2000) dust extinction E(B-V) = 0, 0.2, 0.4, 0.6
IGM attenuation : Inoue et al (2005)
1) Make Single Stellar Population Library
./SSPs
> Initial mass function? : 4.IMF_Salpeter.dat
> Lower mass (default=.100E+00 Msol)? : 0.1
> Upper mass (default=.120E+03 Msol)? : 100
> SNII ejecta: model A, B or C of Woosley & Weaver (A/B [default]/C)? : B
> Stellar winds (y [default]/n)? : y
> Prefix? : Salpeter100
> results
Salpeter100_SSPs.dat
Salpeter100_tracksZ0.0001.dat
Salpeter100_tracksZ0.0004.dat
Salpeter100_tracksZ0.004.dat
Salpeter100_tracksZ0.008.dat
Salpeter100_tracksZ0.02.dat
Salpeter100_tracksZ0.05.dat
Salpeter100_tracksZ0.1.dat
2) Make Synthesized Spectra
./scenarios
> Name of the input file? ---> Salpeter100_scenario1
> Name of the file containing the SSPs properties? ---> Salpeter100_SSPs.dat
> Fraction of close binary systems (real in [0.,1.])? ---> 0.05 (Default)
> Name of the output file? ---> Salpeter100_tau01 (Tau 0.1Gyr exponential model)
> Metallicity (mass fraction) of the ISM at t=0 (real in [0.,1.])? ---> 1.0
> Infall (y/n)? ---> n (default)
> Type of star formation scenario?
-2: file giving the SFR and the metallicity
-1: file giving the SFR
0: instantaneous burst
1: SFR=p1 from t=0 to p2
2: SFR=p2*exp(-t/p1)/p1
3: SFR=(Mgas^p1)/p2 : 1 p1=100, p2=1.0
> Consistent evolution of the stellar metallicity (y/n)? : n
> Stellar metallicity (real in [0.,1.])? : 1.0
> Mass fraction of substellar objects formed (real in [0.,1.])? : 0.0 (default)
> Galactic winds (y/n)? : n (default)
> Age of the galactic winds (Myr, real)?
> Nebular emission (y/n)? : y (default)
> Global extinction?
0: No extinction
1: Extinction for a spheroidal geometry
2: Extinction for a disk geometry: inclination-averaged
3: Extinction for a disk geometry: specific inclination
Default: 0 : 0 (default)
---N0.2
> Name of the output file : Salpeter100_tau10 (Tau 10Gyr exponential model)
>
The input file to spectra (Salpeter100_scenarios1) will be created.
Make spectral library with
./spectra
> Name of the file containing the parameters of the star formation scenarios? :
tau-model は exp(-t/tau)なので p1 が tau。
p2 の係数は規格化。1 太陽質量のガス全体のうち最終的に何太陽質量を使って星を作るかを決める。
半分だったら p2=0.5 太陽質量。ガスのほとんどが星になっていいとすると p2=1.0 太陽質量。
今の場合は
consistent evolution of the stellar metalicity = no
stellar metalicity = 1 (Zsolar)
とおいてしまっているのでガスの中でどれだけ星にするかはあまり関係ない。
Metalicity of ISM = 0.0 (Zsolar)
は上とコンシステントにするためには 1.0 (Zsolar)にしておいた方が良いかも。一応。
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SSPs [model A]
Salpeter IMF + all defaults
| SSPs |
| Model |
Salpeter100 |
| IMF |
Salpeter |
| Upper Mass |
100 Ms |
| Lower Mass |
0.1 Ms |
| SN II |
model B |
| Stellar Winds |
yes |
|
| Scenarios |
| scenario |
Salpeter100_tau01 |
Salpeter100_tau10 |
Salpeter100_tau10_ext |
| Close Binary System |
0.05 |
0.05 |
0.05 |
| Metallicity of the ISM |
1.0 |
1.0 |
1.0 |
| Infall |
no |
no |
no |
| Star Formation Scenario |
2.Exponentially decreasing
p1=100Myr(0.1Gyr)
p2=1.0 |
2.Exponentially decreasing
p1=10000Myr(10Gyr)
p2=1.0 |
2.Exponentially decreasing
p1=100Myr(0.1Gyr)
p2=1.0 |
| Consistent Evolition of the Metallicity |
no |
no |
no |
| Stellar Metallicity |
1.0 |
1.0 |
1.0 |
| Mass fraction of substellar objects formed |
0.0 |
0.0 |
0.0 |
| Galactic Wind |
no |
no |
no |
| Nebular Emission |
yes |
yes |
yes |
| Global Extinction |
no |
no |
yes |
|
awk 'NF==10 {print $1,$2}' spectra1.dat > awktest.dat
5 lines data > 1 line data
awk -f pegase_test.awk file1.dat > file2.dat
paste Ncont_wave.dat spectra_modelA_010_cont_10Myr_1.dat > test.dat
cont.
awk -f extract_sed.awk Salpeter100_tau01 > Salpeter100_tau01.sed
line
5行とりだし ＞ 一列に並べる ＞ フラックス計算
awk -f pegase_test.awk Salpeter100_tau01_line_00001_tmp1 > Salpeter100_tau01_line_00001_tmp2
paste Nline_wave.dat Salpeter100_tau01_line_00001_tmp2 > Salpeter100_tau01_line_00001_tmp3
awk -f extract_sed_line.awk Salpeter100_tau01_line_00001_tmp3 > Salpeter100_tau01_line_00001_z8
awk -f pegase_test.awk Salpeter100_tau01_line_00010_tmp1 > Salpeter100_tau01_line_00010_tmp2
paste Nline_wave.dat Salpeter100_tau01_line_00010_tmp2 > Salpeter100_tau01_line_00010_tmp3
awk -f extract_sed_line.awk Salpeter100_tau01_line_00010_tmp3 > Salpeter100_tau01_line_00010_z8
for z=0 and z=8
awk -f extract_sed.awk Salpeter100_tau01 > Salpeter100_tau01_z0.sed
awk -f extract_sed.awk Salpeter100_tau01 > Salpeter100_tau01_z8.sed
awk -f extract_sed.awk Salpeter100_tau10 > Salpeter100_tau10_z0.sed
awk -f extract_sed.awk Salpeter100_tau10 > Salpeter100_tau10_z8.sed
flux to ABmag
tau01
awk -f flax2mag.awk Salpeter100_tau01_00001_z0 > Salpeter100_tau01_00001_z0_mag
awk -f flax2mag.awk Salpeter100_tau01_00010_z0 > Salpeter100_tau01_00010_z0_mag
awk -f flax2mag.awk Salpeter100_tau01_00030_z0 > Salpeter100_tau01_00030_z0_mag
awk -f flax2mag.awk Salpeter100_tau01_00001_z8 > Salpeter100_tau01_00001_z8_mag
awk -f flax2mag.awk Salpeter100_tau01_00010_z8 > Salpeter100_tau01_00010_z8_mag
awk -f flax2mag.awk Salpeter100_tau01_00030_z8 > Salpeter100_tau01_00030_z8_mag
tau10
awk -f flax2mag.awk Salpeter100_tau10_00001_z0 > Salpeter100_tau10_00001_z0_mag
awk -f flax2mag.awk Salpeter100_tau10_00010_z0 > Salpeter100_tau10_00010_z0_mag
awk -f flax2mag.awk Salpeter100_tau10_00030_z0 > Salpeter100_tau10_00030_z0_mag
awk -f flax2mag.awk Salpeter100_tau10_00001_z8 > Salpeter100_tau10_00001_z8_mag
awk -f flax2mag.awk Salpeter100_tau10_00010_z8 > Salpeter100_tau10_00010_z8_mag
awk -f flax2mag.awk Salpeter100_tau10_00030_z8 > Salpeter100_tau10_00030_z8_mag
#for check
awk -f flax2mag_old.awk Salpeter100_tau01_00001_z0 > Salpeter100_tau01_00001_z0_mag