A&A/2002/2980

The transition from Population III to normal galaxies: Lyalpha and He II 
Lambda1640 emission and the ionising properties of high redshift starburst 
galaxies

Authors: D  Schaerer.

Keywords
Cosmology: early Universe -- Galaxies: stellar content --
Stars: general  -- Stars: fundamental parameters -- Stars: atmospheres

Description of output files from population synthesis models
============================================================

Computed with pop_iso_25 code Version 2.5

Mainly for studies of Ly-a and HeII emission, and ionising fluxes 
of PopIII and metal-poor stellar populations / starbursts.

This data, additional files (including SEDs), and additional 
information also available on the Webpage:
	  http://webast.ast.obs-mip.fr/sfr/
maintained by the author.

1) FILES:
=========

General nomenclature of filenames:
* For PopIII models
	pop3_ttt_imf_mup_low_sfh.n
* other metallicities
	e*_imf_mup_low_sfh.n
Where:
	e*	Metallicity Z (e.g. e020, e001 for Z=0.020, 0.001, and
                e-70 for Z=1.e-7)
	ttt	Indicates tracks (ge0: combined set of tracks 
		with NO mass loss, mdt: including some tracks with
		mass loss)
	imf	IMF type
		- sal		Salpeter (alpha=2.35)
		- ume		bi-modal popIII IMF
		- number	slope alpha (e.g. 235 = Salpeter)
	mup	upper mass cut-off of IMF in Msun
	low	lower mass cut-off of IMF in Msun
	sfh     code for starformation history:
		- isb	instantaneous burst
		- csf	constant star formation (over certain duration)
		SPECIAL for Ly-a computations:
		- is1	bursts up to ~ 50-100 Myr (step of 0.1 Myr in age)
		- is3	bursts up to ~ 10 Myr (step of 0.02 Myr in age)
		- cs1   constant SF corresponding to is1
		- cs3   constant SF corresponding to is3
		- cs4   constant SF up to age of 400 Myr
	n	file extension with number of output file:
		- 20    Main output file         
		- 21    Output file for WR lines 
		- 22    Recombination lines
		- 23    Colors of integrated population
		- 24    UV luminosities and colors, UV slopes

The 5 files *.20, *.21, *.22, *.23, and *.24 are called a "model set"			
The available model sets are listed below (2).

Each file contains a header including detailed information about
all the adopted input parameters, the content of the files and the
output units used. See description below (3).

IMPORTANT NOTE ON UNITS for burst models and SFR=const:
- for instantaneous burst models all the absolute output quantities are normalised
  to a total burst mass of 1 Msun (as indicated by "total mass" in the file headers).
  Other normalisations are sometimes used elsewhere (e.g. Starburst99 output is normalised
  to 1.e+6 Msun).
- for SFR=const all the absolute quantities are scaled to a star formation rate of 
  1 Msun / yr.

IMPORTANT NOTE FOR MODELS with SFR=const:
Depending on the quantity of interest the timescale to reach equilibrium
(in other words an asymptotic value) may differ. For these reasons
various cases for SFR=const have been computed. For most quantities
the files with sfh=cs1 (up to age of 50-100 Myr) are appropriate. 
However, for the determination of the flux in the Lyman-Werner band (Q_H2=Q_LW) 
for example, a longer timescape is required. The files with sfh=cs4 (up to ages 
of 400 Myr) should then be used.
 					
2) LIST OF ALL AVAILABLE MODEL SETS
===================================

* The sets are grouped by metallicity in different directories.
* The gzipped tar file "allmodels_schaerer.tar.gz" (gzipped size
  5.4 MB, unzipped size 64 MB) contains all the available files/sets.
* The following sets are available:

Z    ttt IMF mup low sfh	model set name			directory name 
---------------------------------------------------------------------------------
pop3 ge0 sal 100 001 cs1        pop3_ge0_sal_100_001 cs1	pop3
pop3 ge0 sal 100 001 cs4	pop3_ge0_sal_100_001 cs4	"
pop3 ge0 sal 100 001 is1	pop3_ge0_sal_100_001 is1	"
pop3 ge0 sal 500 001 cs1	pop3_ge0_sal_500_001 cs1	"
pop3 ge0 sal 500 001 cs4	pop3_ge0_sal_500_001 cs4	"
pop3 ge0 sal 500 001 is1	pop3_ge0_sal_500_001_is1	"
pop3 ge0 sal 500 050 cs1	pop3_ge0_sal_500_050_cs1	"
pop3 ge0 sal 500 050 is1	pop3_ge0_sal_500_050_is1	"

e-70     sal 100 001 cs1	e-70_sal_100_001_cs1		e-70
e-70     sal 100 001 cs4	e-70_sal_100_001_cs4		"
e-70     sal 100 001 is1	e-70_sal_100_001_is1		"
e-70     sal 500 001 cs1	e-70_sal_500_001_cs1		"
e-70     sal 500 001 cs4	e-70_sal_500_001_cs4		"
e-70     sal 500 001 is1	e-70_sal_500_001_is1		"
e-70     sal 500 050 cs1	e-70_sal_500_050_cs1		"
e-70     sal 500 050 is1	e-70_sal_500_050_is1		"

e-50     sal 100 001 cs1	e-50_sal_100_001_cs1		e-50
e-50     sal 100 001 cs4	e-50_sal_100_001_cs4		"
e-50     sal 100 001 is1	e-50_sal_100_001_is1		"
e-50     sal 500 001 cs1	e-50_sal_500_001_cs1		"
e-50     sal 500 001 cs4	e-50_sal_500_001_cs4		"
e-50     sal 500 001 is1	e-50_sal_500_001_is1		"
e-50     sal 500 050 cs1	e-50_sal_500_050_cs1		"
e-50     sal 500 050 is1	e-50_sal_500_050_is1		"

e0004    sal 100 001 cs1	e0004_sal_100_001_cs1		e0004
e0004    sal 100 001 cs3	e0004_sal_100_001_cs3           "
e0004    sal 100 001 cs4	e0004_sal_100_001_cs4           "
e0004    sal 100 001 is1	e0004_sal_100_001_is1           "
e0004    sal 100 001 is3	e0004_sal_100_001_is3           "
e0004    sal 150 001 cs1	e0004_sal_150_001_cs1           "
e0004    sal 150 001 cs3	e0004_sal_150_001_cs3           "
e0004    sal 150 001 cs4	e0004_sal_150_001_cs4           "
e0004    sal 150 001 is1	e0004_sal_150_001_is1		"
e0004    sal 150 001 is3	e0004_sal_150_001_is3		"

e001     sal 100 001 cs1	e001_sal_100_001_cs1		e001
e001     sal 100 001 cs3	e001_sal_100_001_cs3		"
e001     sal 100 001 cs4	e001_sal_100_001_cs4		"
e001     sal 100 001 is1	e001_sal_100_001_is1		"
e001     sal 100 001 is3	e001_sal_100_001_is3		"

e004     sal 100 001 cs1	e004_sal_100_001_cs1		e004
e004     sal 100 001 cs4	e004_sal_100_001_cs4		"
e004     sal 100 001 is1	e004_sal_100_001_is1		"

e008     sal 100 001 cs1	e008_sal_100_001_cs1		e008
e008     sal 100 001 cs4	e008_sal_100_001_cs4		"
e008     sal 100 001 is1	e008_sal_100_001_is1		"

e020     sal 100 001 cs1	e020_sal_100_001_cs1		e020
e020     sal 100 001 cs4	e020_sal_100_001_cs4		"
e020     sal 100 001 is1	e020_sal_100_001_is1		"

e040     sal 100 001 cs1	e040_sal_100_001_cs1		e040
e040     sal 100 001 cs4	e040_sal_100_001_cs4		"
e040     sal 100 001 is1	e040_sal_100_001_is1		"

3) DESCRIPTION OF FILE CONTENT:
===============================

------------------------------------------------------------------------
File *.20 (main output): 
-- file corresponding to output described
in Schaerer & Vacca (1998, ApJ, 497, 618)
plus additional quantities (cols 22-25)

------------------------------
column  content   unit
------------------------------
1	log(age)  [yr]   
2	Mbol      [mag]
3	log(Q_0)  [s^-1] Q_0=Q_H  = Lyman continuum photon flux
4	log(Q_1)  [s^-1] Q_1=Q_He = He0 ionising photon flux 
5	log(Q_2)  [s^-1] Q_0=Q_He+= He+ ionising photon flux
6	# O-stars 
7	WR/(WR+O) 
8	WR/O   
9	WNL = WNL/(WR+O)
10	WNE = WNE/(WR+O)    
11	WC  = WC/(WR+O)
12$	nebular H_beta	EW [A]      
13$	  "	  	luminosity [erg s^-1]
14$	nebular HeI 4471 EW [A]   CAUTION: Saturation effect !       
15$        "	  	luminosity [H_beta]           
16$	nebular HeII 4686 EW [A]         
17$        "       	luminosity [H_beta]
18	WR bump	(CIII/IV 4650 + HeII 4686) EW [A]          
19$        "	  luminosity [H_beta]
20	CI V-WR   EW [A] 
21$        "       luminosity [H_beta]
22      Balmer jump [magnitudes] 
                         -- defined as -2.5*log(F_lambda=3640/F_lambda=3650)
23      log(Q_H2) [s^-1] Q_H2=Q_LW= ionising photon flux in Lyman-Werner band
24	E(Q)	  [eV] average energy per photon in Lyman-continuum
25	E(QHe+)	  [eV] average energy per photon with E > 54 eV

Notes:
$ the NEBULAR emission line predictions given in the *.20 and *.21 files 
  are computed assuming an fixed electron temperature Te=10 kK (as mentioned 
  in header), whereas the nebular continous emission may be computed
  with a variable Te ! Therefore these predictions may i) be inconsistent 
  and, ii) differ from the ones given in the *.22 files.
  --> Use preferrentially the predictions in *.22 !!

------------------------------------------------------------------------
File *.21 (output related to Wolf-Rayet stars): 
-- file corresponding to output described
in Schaerer & Vacca (1998, ApJ, 497, 618)

------------------------------
column  content   unit
------------------------------
1	log(age)  [yr]
2       average WNL subtype
3       average WC  subtype
4*	nebular H_alpha EW [A]
5*        "    		luminosity [H_beta]
6*	nebular H_beta	EW [A]      
7*	  "	  	luminosity [erg s^-1]
8	stellar He1640	EW [A]
9*        "       	luminosity [H_beta]
10	stellar N_4640	EW [A]
11*       "       	luminosity [H_beta]
12	stellar C_4650	EW [A]
13*       "       	luminosity [H_beta]
14	stellar He4686	EW [A]
15*       "       	luminosity [H_beta]
16	stellar H_4861	EW [A]
17*       "       	luminosity [H_beta]
18	stellar C_5696  EW [A]
19*       "       	luminosity [H_beta]
20	stellar C_5808	EW [A]
21*       "       	luminosity [H_beta]
22	stellar H_6560	EW [A]
23*       "      	luminosity [H_beta]
24	stellar He5412	EW [A]
25*       "       	luminosity [H_beta]

Notes:
* the NEBULAR emission line predictions given in the *.20 and *.21 files 
  are computed assuming an fixed electron temperature Te=10 kK (as mentioned 
  in header), whereas the nebular continous emission may be computed
  with a variable Te ! Therefore these predictions may i) be inconsistent 
  and, ii) differ from the ones given in the *.22 files.
  --> The relative WR/Hbeta luminosities (=intensities) may simply
      be rescaled by the ratio between the Hbeta luminosities
      given in *.20/*.21. However, for these quantities the differences 
      are of the order of 6% only.

------------------------------------------------------------------------
File *.22 (Nebular recombination lines - NEW V2.4):

------------------------------
column  content   unit
------------------------------
1	log(age)  [yr]
2	log(Q_0)  [s^-1] 
3	log(Q_1)  [s^-1] 
4	log(Q_2)  [s^-1] 
5$	H_beta	  luminosity [erg s^-1]
6$	H_Lya	  EW [A]
7$	  "       I/Hb     
8$	H_alpha   EW [A]
9$        "       I/Hb
10$	H_beta	  EW [A]      
11$	  "	  I/Hb
12$	HeI 4471  EW [A]   CAUTION: Saturation effect !       
13$       "	  I/Hb    
14$	HeII_1640 EW [A]
15$         "      I/Hb 
16$	HeII_4686 EW [A]
17$       "       I/Hb 
18$	HeII_3203 EW [A]
19$       "       I/Hb 
20$     HeII_4541 EW [A]
21        "       I/Hb 

Notes:
$ the NEBULAR emission line predictions given in the *.20 and *.21 files 
  are computed assuming an fixed electron temperature Te=10 kK (as mentioned 
  in header), whereas the nebular continous emission may be computed
  with a variable Te ! Therefore these predictions may i) be inconsistent 
  and, ii) differ from the ones given in the *.22 files.
  --> Use preferrentially the predictions in *.22 !!

------------------------------------------------------------------------
File *.23 (Colors)
-- filter bandpasses as in Starburst99 (Leitherer et al. 1999, ApJS, 123, 3)

------------------------------
column  content   unit
------------------------------
1       log(age)  [yr]
2	(130-V)
3	(210-V)
4       (U-B)
5       (B-V) 
6       (V-R)
7       (V-I)
8       (V-J)
9       (V-H)
10      (V-K)
11      (V-L)
12      M_V
13      M_B
14      M_BOL

------------------------------------------------------------------------
File *.24 (UV spectral information)

------------------------------
column  content   unit
------------------------------
1       log(age)  [yr]
2	M_BOL
3	log(L_1500) [erg s^-1 A^-1] average UV luminosity at 1500 Ang 
				    (over +- 20 Ang band)
4	log(L_1500) [erg s^-1 A^-1] average UV luminosity at 1500 Ang 
				    (over +-150 Ang band)
5	log(L_2800) [erg s^-1 A^-1] average UV luminosity at 2800 Ang 
				    (over +-280 Ang band)
6+	beta_1550   UV slope 1300-1800 Ang using STELLAR + NEBULAR cont.emission
7+	beta_2500   UV slope 2200-2800 Ang        "
8+	beta_2000   UV slope 1800-2200 Ang        "
9+	beta_1550*  UV slope 1300-1800 Ang using pure STELLAR emission
10+	beta_2500*  UV slope 2200-2800 Ang        "
11+	beta_2000*  UV slope 1800-2200 Ang        "
12	log(L_900)  [erg s^-1 A^-1]  log of average luminosity 912- (cf. definition below)
13	log(Lyb-SB99) log of Lyman-break amplitude Lyb=912+/912-, where 912+
		      is the average flux in F_lambda units over 1080-1120 Ang,
		      and 912- the same over 870-900 Ang

Notes:
+ the slope beta is defined by F_lambda ~ lambda ^ beta

------------------------------------------------------------------------

4) KNOWN PROBLEMS / BUGS
========================

- Model sets e0004_sal_150_001_cs4 and e0004_sal_100_001_cs4:
	the WR mass limit is erroneously set to 61 Msun instead
	of 85 Msun. The results with the correct mass limit are identical.
  files not updates - ds / 15 nov 02


-- end of file
