J/A+A/523/A64 UV properties of starbursts (Raiter+, 2010)
Predicted UV properties of very metal-poor starburst galaxies.
Raiter A., Schaerer D., Fosbury R.
<Astron. Astrophys. 523, A64 (2010)>
=2010A&A...523A..64R 2010A&A...523A..64R
ADC_Keywords: Models, atmosphere ; Models, evolutionary ; Populations, stellar ;
Spectra, ultraviolet
Keywords: galaxies: high-redshift - galaxies: evolution - galaxies: starburst -
early Universe
Abstract:
We have computed evolutionary synthesis models covering metallicities
from PopIII to solar, a wide range of IMFs, and two star-formation
histories (bursts and constant star-formation). The detailed
predictions these models, including their time dependence, are given
here. The predicted quantities include ionising fluxes, UV continuum
properties, recombination line strengths (for Lyα, HeII and
other lines), as well as several other quantities of interest. The
models provided here cover a wider range of parameter space than our
earlier calculations (Schaerer, 2003A&A...397..527S 2003A&A...397..527S, Cat. VI/109).
Description:
Computed with the popisomc code (Version 2.53) of Daniel Schaerer.
This data, additional files (including SEDs), and additional
information also available on the Webpage:
http://obswww.unige.ch/sfr/models/uvproperties/
maintained by Daniel Schaerer.
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 1M☉ (as indicated by
"total mass" in the file headers).
Other normalisations are sometimes used elsewhere (e.g. Starburst99
output is normalised to 106M☉).
- for SFR=const all the absolute quantities are scaled to a star
formation rate of 1M☉/yr.
NOTE ON THE UPPER MASS CUT-OFF (mup):
Depending on the availability of stellar tracks at different
metallicities, some models listed as mup=500M☉ have an
effective upper mass cut-off of mup=120-150M☉.
In practice this applies to models at metallicities Z=0.0004, where
mup=150M☉, and at Z≥0.001, where mup=120M☉. For all
very low metallicities (Z≤1.e-5), where the IMF may indeed extend
to very high stellar masses, tracks for masses up to mup=500M☉
have been used.
NOTE ON THE STAR-FORMATION HISTORY CODE (sfh):
Depending on the lower mass cut-off of the IMF the models have been
computed up to different maximum ages. Generally the models cover
ages from zero (104yr in practice) to 1Gyr and the output is
printed in steps of 1Myr (although computed internally on a 0.1Myr
timestep). These models are denoted by sfh='is5' and 'cs5'.
For IMFs containing only massive stars (i.e. lower mass
cut-off=50M☉) the maximum is naturally much lower, and may
vary from case to case. The output is given in steps of 0.1Myr here.
These models are denoted by sfh='is4' and 'cs4'.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
initial.dat 26 128 *List of available sets
type20.dat 244 112820 Main output (file corresponding to output described
in Schaerer & Vacca, 1998ApJ...497..618S 1998ApJ...497..618S) plus
additional quantities (last four columns)
type21.dat 240 112820 Output related to Wolf-Rayet stars (file
corresponding to output described in
Schaerer & Vacca, 1998ApJ...497..618S 1998ApJ...497..618S)
type22.dat 297 112820 Nebular recombination lines and Lyα absorption
type23.dat 148 112820 Colors (filter bandpasses as in Starburst99,
Leitherer et al., 1999ApJS..123....3L 1999ApJS..123....3L)
type24.dat 170 112820 UV spectral information
type25.dat 176 112820 Ionising flux, UV luminosities and slopes -
NEW in v2.53
--------------------------------------------------------------------------------
Note on initial.dat:
8 metallicities * 6 IMF * 5 SF-histories * 3 mass cutt-off interval
--------------------------------------------------------------------------------
See also:
http://webast.ast.obs-mip.fr/sfr/ : Models homepage
Byte-by-byte Description of file: initial.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Z Code for metallicity Z (G1)
7- 9 A3 --- ttt [ge0] Tracks (G1)
11- 14 A4 --- IMF IMF type (G1)
16- 18 I3 --- mup Upper mass cut-off of IMF in M☉ (G1)
20- 22 I3 --- low Lower mass cut-off of IMF in M☉ (G1)
24- 26 A3 --- sfh Code for star formation history (G1)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: type20.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Z Code for metallicity Z (G1)
6 A1 --- --- [_]
7- 9 A3 --- ttt [ge0] Tracks (G1)
10 A1 --- --- [_]
11- 14 A4 --- IMF IMF type (G1)
15 A1 --- --- [_]
16- 18 I3 solMass mup Upper mass cut-off of IMF in M☉ (G1)
19 A1 --- --- [_]
20- 22 I3 solMass low Lower mass cut-off of IMF in M☉ (G1)
23 A1 --- --- [_]
24- 26 A3 --- sfh Code for star formation history (G1)
27- 29 A3 --- --- [.20] (G1)
32- 40 E9.5 [yr] log(Age) Age
42- 48 F7.3 mag Mbol Bolometric magnitude
51- 56 F6.3 [s-1] log(Q0) Lyman continuum photon flux (Q0=QH)
58- 64 F7.3 [s-1] log(Q1) He0 ionising photon flux (Q1=QHe)
66- 72 F7.3 [s-1] log(Q2) He+ ionising photon flux (Q0=QHe+)
75- 82 E8.3 --- NOstar Number of O stars
84- 90 E7.2 --- WR/(WR+O) Ratio of WR to WR+O stars
92- 98 E7.2 --- WR/O Ratio of WR to O stars
100-106 E7.2 --- WNL/(WR+O) Ratio of WNL (late WN) to WR+O stars
108-114 E7.2 --- WNE/(WR+O) Ratio of WNE (early WN) to WR+O stars
116-122 E7.2 --- WC/(WR+O) Ratio of WC to WR+O stars WC/(WR+O)
124-131 F8.3 0.1nm EWHb Nebular Hβ equivalent width (G2)
133-140 E8.3 10-7W LHb Nebular Hβ luminosity (G2)
142-149 F8.3 0.1nm EWHeI Nebular HeI 4471 equivalent width
(CAUTION: Saturation effect !) (G2)
151-158 E8.3 --- LHeI Nebular HeI 4471 luminosity
(in Hβ unit) (G2)
160-167 F8.3 0.1nm EWHeII Nebular HeII 4686 equivalent width (G2)
169-176 E8.3 --- LHeII Nebular HeII 4686 luminosity
(in Hβ unit) (G2)
178-185 F8.3 0.1nm EWWR WR bump (CIII/IV 4650 + HeII 4686)
equivalent width
187-194 E8.3 --- LWR WR bump (CIII/IV 4650 + HeII 4686)
luminosity (in Hβ unit) (G2)
196-203 F8.3 0.1nm EWCI CI V-WR equivalent width
205-212 E8.3 --- LCI CI V-WR luminosity (in Hβ unit) (G2)
215-220 F6.3 mag Balmer Balmer jump, defined as
-2.5*log(F(3640Å)/F(3650Å)
223-228 F6.3 [s-1] log(QH2) Ionising photon flux in Lyman-Werner band
(QH2=QLW)
231-236 F6.3 eV E(Q) Average energy per photon in Lyman-continuum
239-244 F6.3 eV E(QHe+) Average energy per photon with E>54eV
--------------------------------------------------------------------------------
Byte-by-byte Description of file: type21.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Z Code for metallicity Z (G1)
6 A1 --- --- [_]
7- 9 A3 --- ttt [ge0] Tracks (G1)
10 A1 --- --- [_]
11- 14 A4 --- IMF IMF type (G1)
15 A1 --- --- [_]
16- 18 I3 solMass mup Upper mass cut-off of IMF in M☉ (G1)
19 A1 --- --- [_]
20- 22 I3 solMass low Lower mass cut-off of IMF in M☉ (G1)
23 A1 --- --- [_]
24- 26 A3 --- sfh Code for star formation history (G1)
27- 29 A3 --- --- [.21] (G1)
32- 40 E9.5 [yr] log(Age) Age
43- 45 F3.1 --- WNLType Average WNL subtype (late WN)
50- 52 F3.1 --- WCType Average WC subtype
55- 61 F7.2 0.1nm EWHa Nebular Hα equivalent width (G2)
63- 70 E8.3 --- LHa Nebular Hα luminosity
(in Hβ unit) (G2)
72- 78 F7.2 0.1nm EWHb Nebular Hβ equivalent width (G2)
80- 87 E8.3 10-7W LHb Nebular Hβ luminosity (G2)
90- 95 F6.2 0.1nm EWHe1640 Stellar He1640 equivalent width
97-104 E8.3 --- LHe Stellar He1640 luminosity
(in Hβ unit) (G2)
108-112 F5.2 0.1nm EWN4640 Stellar N4640 equivalent width
114-121 E8.3 --- LN Stellar N4640 luminosity
(in Hβ unit) (G2)
123-129 F7.2 0.1nm EWC4650 Stellar C4650 equivalent width
131-138 E8.3 --- LC4650 Stellar C4650 luminosity
(in Hβ unit) (G2)
141-146 F6.2 0.1nm EWHe4686 Stellar He4686 equivalent width
148-155 E8.3 --- LHe4686 Stellar He4686 luminosity
(in Hβ unit) (G2)
159-163 F5.2 0.1nm EWH4861 Stellar H4861 equivalent width
165-172 E8.3 --- LH4861 Stellar H4861 luminosity
(in Hβ unit) (G2)
176-180 F5.2 0.1nm EWC5696 Stellar C5696 equivalent width
182-189 E8.3 --- LC5696 Stellar C5996 luminosity
(in Hβ unit) (G2)
191-197 F7.2 0.1nm EWC5808 Stellar C5808 equivalent width
199-206 E8.3 --- LC5808 Stellar C5808 luminosity
(in Hβ unit) (G2)
209-214 F6.2 0.1nm EWH6560 Stellar H6560 equivalent width
216-223 E8.3 --- LH6560 Stellar H6560 luminosity
(in Hβ unit) (G2)
227-231 F5.2 0.1nm EWHe5412 Stellar He5412 equivalent width
233-240 E8.3 --- LHe5412 Stellar He5412 luminosity
(in Hβ unit) (G2)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: type22.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Z Code for metallicity Z (G1)
6 A1 --- --- [_]
7- 9 A3 --- ttt [ge0] Tracks (G1)
10 A1 --- --- [_]
11- 14 A4 --- IMF IMF type (G1)
15 A1 --- --- [_]
16- 18 I3 solMass mup Upper mass cut-off of IMF in M☉ (G1)
19 A1 --- --- [_]
20- 22 I3 solMass low Lower mass cut-off of IMF in M☉ (G1)
23 A1 --- --- [_]
24- 26 A3 --- sfh Code for star formation history (G1)
27- 29 A3 --- --- [.22] (G1)
31- 39 E9.4 [yr] log(Age) Age
42- 47 F6.3 [s-1] log(Q0) Lyman continuum photon flux (Q0=QH)
49- 55 F7.3 [s-1] log(Q1) He0 ionising photon flux (Q1=QHe)
57- 63 F7.3 [s-1] log(Q2) He+ ionising photon flux (Q0=QHe+)
65- 72 E8.3 10-7W LHb Hβ luminosity (G2)
74- 81 F8.3 0.1nm EWHLya Lymanα equivalent width (G2)
83- 90 E8.3 --- IHLya Lymanα intensity relative to
Hβ (G2)
92- 99 F8.3 0.1nm EWHa Hα equivalent width (G2)
101-108 E8.3 --- IHa Hα intensity relative to Hβ (G2)
110-117 F8.3 0.1nm EWHb Hβ equivalent width (G2)
119-126 E8.3 --- IHb [1.00E+00] Hβ intensity relative
to Hβ (G2)
129-135 F7.3 0.1nm EWHeI HeI 4471 equivalent width
(CAUTION: Saturation effect !) (G2)
137-144 E8.3 --- IHeI HeI 4471 intensity relative to Hβ (G2)
147-153 F7.3 0.1nm EWHeII1640 HeII1640 equivalent width (G2)
155-162 E8.3 --- IHeII1640 HeII1640 intensity relative to Hβ (G2)
165-171 F7.3 0.1nm EWHeII4686 HeII4686 equivalent width (G2)
173-180 E8.3 --- IHeII4686 HeII4686 intensity relative to Hβ (G2)
184-189 F6.3 0.1nm EWHeII3203 HeII3203 equivalent width (G2)
191-198 E8.3 --- IHeII3203 HeII3203 intensity relative to Hβ (G2)
202-207 F6.3 0.1nm EWHeII4541 HeII4541 equivalent width (G2)
209-216 E8.3 --- IHeII4541 HeII4541 intensity relative to Hβ
219-225 F7.3 0.1nm LyaAbs Lyα absorption equivalent width (1)
227-234 E8.3 --- ILyaAbs Lyα absorption intensity relative
to Hβ (1)
237-243 F7.3 0.1nm LyaAbsc Lyα absorption computed EXCLUDING
nebular continuum equivalent width (1)
245-252 E8.3 10+4W/m FcontLya Continuum flux (stellar+nebular) at
Lyα (in erg/s/Å units) (1)
255-261 F7.3 0.1nm LyaAbs2 Lyα absorption equivalent width (2)
263-270 E8.3 --- ILyaAbs2 Lyα absorption intensity relative
to Hβ (2)
273-279 F7.3 0.1nm LyaAbsc2 Lyα absorption computed EXCLUDING
nebular continuum equivalent width (2)
281-288 E8.3 10+4W/m FcontLya2 Continuum flux (stellar+nebular) at
Lyα (in erg/s/Å units) (2)
292-297 F6.3 eV E(Q) Average energy per photon in
Lyman-continuum
--------------------------------------------------------------------------------
Note (1): Quantities related to Lya absorption. The pivot wavelengths used to
determine the continuum at Lya are 1160 and 1250Å.
Note (2): Quantities related to Lya absorption, using 1190 and 1240Å as the
two wavelength pivots (following Valls-Gabaud, 1993ApJ...419....7V 1993ApJ...419....7V).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: type23.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Z Code for metallicity Z (G1)
6 A1 --- --- [_]
7- 9 A3 --- ttt [ge0] Tracks (G1)
10 A1 --- --- [_]
11- 14 A4 --- IMF IMF type (G1)
15 A1 --- --- [_]
16- 18 I3 solMass mup Upper mass cut-off of IMF in M☉ (G1)
19 A1 --- --- [_]
20- 22 I3 solMass low Lower mass cut-off of IMF in M☉ (G1)
23 A1 --- --- [_]
24- 26 A3 --- sfh Code for star formation history (G1)
27- 29 A3 --- --- [.23] (G1)
31- 39 E9.4 [yr] log(Age) Age
44- 49 F6.3 mag (130-V) (130-V) colour index
52- 57 F6.3 mag (210-V) (210-V) colour index
60- 65 F6.3 mag (U-B) (U-B) colour index
68- 73 F6.3 mag (B-V) (B-V) colour index
76- 81 F6.3 mag (V-R) (V-R) colour index
84- 89 F6.3 mag (V-I) (V-I) colour index
92- 97 F6.3 mag (V-J) (V-J) colour index
100-105 F6.3 mag (V-H) (V-H) colour index
108-113 F6.3 mag (V-K) (V-K) colour index
116-121 F6.3 mag (V-L) (V-L) colour index
124-130 F7.3 mag VMAG Absolute V magnitude
133-139 F7.3 mag BMAG Absolute B magnitude
142-148 F7.3 mag Mbol Bolometric magnitude
--------------------------------------------------------------------------------
Byte-by-byte Description of file: type24.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Z Code for metallicity Z (G1)
6 A1 --- --- [_]
7- 9 A3 --- ttt [ge0] Tracks (G1)
10 A1 --- --- [_]
11- 14 A4 --- IMF IMF type (G1)
15 A1 --- --- [_]
16- 18 I3 solMass mup Upper mass cut-off of IMF in M☉ (G1)
19 A1 --- --- [_]
20- 22 I3 solMass low Lower mass cut-off of IMF in M☉ (G1)
23 A1 --- --- [_]
24- 26 A3 --- sfh Code for star formation history (G1)
27- 29 A3 --- --- [.24] (G1)
31- 39 E9.4 [yr] log(Age) Age
43- 49 F7.3 mag Mbol Bolometric magnitude
55- 60 F6.3 [uW/nm] log(L15SB) Average UV luminosity at 1500Å
(over ±20Å band), in erg/s/Å
66- 71 F6.3 [uW/nm] log(L1500) Average UV luminosity at 1500Å
(over ±150Å band), in erg/s/Å
77- 82 F6.3 [uW/nm] log(L2800) Average UV luminosity at 2800Å
(over ±280Å band), in erg/s/Å
85- 90 F6.3 --- beta1550 UV slope 1300-1800Å using
STELLAR + NEBULAR cont. emission (1)
93- 98 F6.3 --- beta2500 UV slope 2200-2800Å using
STELLAR + NEBULAR cont. emission (1)
101-106 F6.3 --- beta2000 UV slope 1800-2200Å using
STELLAR + NEBULAR cont. emission (1)
109-114 F6.3 --- beta1550* UV slope 1300-1800Å using pure
STELLAR emission (1)
117-122 F6.3 --- beta2500* UV slope 2200-2800Å using pure
STELLAR emission (1)
125-130 F6.3 --- beta2000* UV slope 1800-2200Å using pure
STELLAR emission (1)
133-138 F6.3 [uW/nm] log(L900) Average luminosity 912- in erg/s/Å (2)
141-146 F6.3 [---] log(Lybrk) Lyman-break amplitude Lybrk=912+/912-
149-154 F6.3 [uW/nm] log(L1460) Average UV luminosity at 1195Å
(over ±85Å band)
157-162 F6.3 --- beta1460 UV slope between 1195 (±85)Å and
1738 (±127)Å
166-170 F5.3 --- betaGR UV slope computed using Steidel G,R filter
curves (cf. Shapley et al.,
2003ApJ...588...65S 2003ApJ...588...65S) (3)
--------------------------------------------------------------------------------
Note (1): The slope beta is defined by F(λ)∝~λβ.
Note (2): Where 912+ is the average flux in F(λ) units
over 1080-1120Å, and 912- the same over 870-900Å.
Note (3): do not use! untested and incomplete information.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: type25.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Z Code for metallicity Z (G1)
6 A1 --- --- [_]
7- 9 A3 --- ttt [ge0] Tracks (G1)
10 A1 --- --- [_]
11- 14 A4 --- IMF IMF type (G1)
15 A1 --- --- [_]
16- 18 I3 solMass mup Upper mass cut-off of IMF
in M☉ (G1)
19 A1 --- --- [_]
20- 22 I3 solMass low Lower mass cut-off of IMF
in M☉ (G1)
23 A1 --- --- [_]
24- 26 A3 --- sfh Code for star formation history (G1)
27- 29 A3 --- --- [.25] (G1)
31- 39 E9.4 [yr] log(Age) Age
42- 47 F6.3 [s-1] log(Q0) Lyman continuum photon flux (Q0=QH)
50- 55 F6.3 [uW/nm] log(Q0/L1500) Ionising photon flux per 1500Å
luminosity (in erg/s/Å)
60- 66 F7.3 mag Mbol Bolometric magnitude
72- 77 F6.3 [uW/nm] log(L15SB) Average UV luminosity at 1500Å
(over ±20Å band), in erg/s/Å
83- 88 F6.3 [uW/nm] log(L1500) Average UV luminosity at 1500Å
(over ±150Å band), in erg/s/Å
91- 96 F6.3 [uW/nm] log(L2800) Average UV luminosity at 2800Å
(over ±280Å band), in erg/s/Å
99-104 F6.3 --- beta1550 UV slope 1300-1800Å using
STELLAR + NEBULAR continuum emission (1)
107-112 F6.3 --- beta2500 UV slope 2200-2800Å using
STELLAR + NEBULAR continuum emission (1)
115-120 F6.3 --- beta2000 UV slope 1800-2200Å using
STELLAR + NEBULAR continuum emission (1)
123-128 F6.3 --- beta1550* UV slope 1300-1800Å using pure
STELLAR emission (1)
131-136 F6.3 --- beta2500* UV slope 2200-2800Å using pure
STELLAR emission (1)
139-144 F6.3 --- beta2000* UV slope 1800-2200Å using pure
STELLAR emission (1)
147-152 F6.3 [uW/nm] log(L900) Average luminosity 912- (2)
155-160 F6.3 --- log(Lybrk) Lyman-break amplitude Lyb=912+/912- (2)
164-168 F5.3 --- neb/1500 Contribution of the nebular continuum to
the total continuum at 1500Å (3)
172-176 F5.3 --- neb/2800 Contribution of the nebular continuum to
the total continuum at 2800Å (4)
--------------------------------------------------------------------------------
Note (1): The slope beta is defined by F(λ)∝~λβ.
Note (2): where 912+ is the average flux in F_lambda units over 1080-1120Å,
and 912- the same over 870-900Å
Note (3): Averaged over the same spectral range as for log(L1500).
Note (4): Averaged over the same spectral range as for log(L2800).
--------------------------------------------------------------------------------
Global notes:
Note (G1): General nomenclature of filenames:
* For PopIII models : pop3tttimfmuplow_sfh.xx
* Other metallicities : e*imfmuplowsfh.xx
where:
e* = Metallicity Z, as
e-70: Z=1.e-7;
e-50: Z=1.e-5;
e0004: Z=0.0004;
e001: Z=0.001;
e004: Z=0.004;
e008: Z=0.008;
e020: Z=0.020
ttt = tracks used for PopIII models, as:
ge0: combined set of tracks with NO mass loss;
mdt: including some tracks with mass loss
imf = IMF type, as:
sal : Salpeter law (α=2.35).
sca : Scalo (1986, Fund. Cosmic Phys., 11, 1) IMF
(3 powerlaws, α=2.70 for M>2M☉);
logA: log-normal distribution: case A from Tumlinson;
logB: log-normal distribution: case B from Tumlinson;
logE: log-normal distribution: case E from Tumlinson;
l05 : Larson (1998MNRAS.301..569L 1998MNRAS.301..569L) IMF with Mc=5M☉
mup = upper mass cut-off of IMF (in solar masses)
low = lower mass cut-off of IMF (in solar masses)
sfh = star formation history, as:
is4: bursts up to 400Myr (step of 0.1Myr in age);
is5: bursts up to 1Gyr (output given for steps of 1Myr in age);
cs4: constant star formation up to an age of max 100Myr
(step of 0.1Myr in age);
cs5: constant star formation up to an age of 1Gyr;
(output given for steps of 1Myr in age)
xx = file extension indicating the type of output, as:
20: Main output, as in Schaerer & Vacca, 1998ApJ...497..618S 1998ApJ...497..618S;
21: output for WR lines;
22: recombination lines;
23: colors of integrated population;
24: UV luminosities and colors, UV slopes;
25: Ionising flux, UV luminosities, and UV slopes
The 6 files *.20, *.21, *.22, *.23, *.24 and *.25 are called a "model set".
Note (G2): The NEBULAR emission line predictions given in the type20.dat
and type21.dat files are computed assuming an fixed electron
temperature Te=10kK (as mentioned in header), whereas the nebular
continuous emission may be computed with a variable Te ! Therefore
these predictions may i) be inconsistent and, ii) differ from the ones
given in the type22.dat files.
--> Use preferentially the predictions in type22.dat!!
The relative WR/Hbeta luminosities (=intensities) may simply be
rescaled by the ratio between the Hbeta luminosities given in
type20.dat/type21.dat. However, for these quantities the differences
are of the order of 6% only.
--------------------------------------------------------------------------------
Acknowledgements:
Daniel Schaerer, Daniel.Schaerer(at)unige.ch
References:
Schaerer, Properties of massive Pop III stars, 2002A&A...382...28S 2002A&A...382...28S
Leitherer et al., Starburst99, 1999ApJS..123....3L 1999ApJS..123....3L
Schaerer and Vacca, New models for WR and O stars, 1998ApJ...497..618S 1998ApJ...497..618S
(End) Patricia Vannier [CDS] 06-Sep-2010