Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.stsci.edu/science/starburst/GDL99/README Дата изменения: Fri Jun 18 23:10:41 1999 Дата индексирования: Sat Dec 22 09:26:23 2007 Кодировка: Поисковые слова: http www.stsci.edu science starburst

Paper I

Reference paper:

"Synthetic spectra of H Balmer and HeI absorption lines.
I: Stellar Library"
by Rosa M. Gonzalez Delgado & Claus Leitherer.
1999, ApJS, accepted

Abstract:

We present a grid of synthetic profiles of stellar H Balmer and HeI lines
at optical wavelengths with a sampling of 0.3 \AA. The grid spans a range
of effective temperature (Teff) between 50000 K and 4000 K, and gravity
(log g) between 0.0 and 5.0 at solar metallicity. For Teff>25000 K, NLTE
stellar atmosphere models are computed using the code TLUSTY (Hubeny
1988). For cooler stars, Kurucz (1993) LTE models are used to compute the
synthetic spectra. The grid includes the profiles of the high-order
hydrogen Balmer series and HeI lines for effective temperatures and
gravities that have not been previously synthesized. The behavior of H8
to H13 and HeI 3819 with effective temperature and gravity is very
similar to that of the lower terms of the series (e.g. Hbeta) and the
other HeI lines at longer wavelengths; therefore, they are suited for the
determination of the atmospheric parameters of stars. These lines are
potentially important to make predictions for these stellar absorption
features in galaxies with active star formation. Evolutionary synthesis
models of these lines for starburst and post-starburst galaxies are
presented in a companion paper. The full set of the synthetic stellar
spectra is available for retrieval at our websites
http://www.iaa.es/ae/e2.html and http://www.stsci.edu/science/starburst/
or on request from the authors at rosa@iaa.es.

The spectral ranges synthesized (Table 1 of the paper) are:

RANGE MAIN LINES IN RANGE
--------- ---------------------------
3720-3920 H13, H12, H11, H10, HeI 3819, H9, H8
3990-4150 HeI 4009, HeI 4026, Hd, HeI 4121, HeI 4144
4300-4400 Hg, HeI 4388
4420-4550 HeI 4471
4820-4900 Hb
4900-4950 HeI 4922

The grid of models is in Table 2 of the paper.



Files on this website:

1. The stellar library is in the gziped tar file: library.tar.gz

This tar file contains the synthetic spectra with
effective temperature between 50000 K and 4000 K,
and gravity (log g) between 0.0 and 5.0 at solar metallicity
in the files (one for each of the above wavelength ranges):

L1.dat, L2.dat, L3.dat, L4.dat, L5.dat and L6.dat

Column 1: Effective temperature ( from 4000 K to 50000 K)
Column 2: wavelength (in Angstroms)
Column 3-13: normalized spectrum for log g= 5.0, 4.5, 4.0,
3.5, 3.0, 2.5, 2.0, 1.5, 1.0, 0.5 and 0.0,
respectively.


2. The equivalent width measurements are in: Ew-stars.tar.gz

The equivalent widths of the lines were measured in the spectral
windows defined as follows::

Line Line window Continuum window

H10 3783-3813 1
H9 3823-3853 1
H8 3874-3904 1
Hd 4070-4130 2
Hg 4311-4371 3
Hb 4830-4890 4
HeI 3819 3816-3823 1
HeI 4026 4020-4031 2
HeI 4388 4381-4395 3
HeI 4471 4464-4478 5
HeI 4922 4915-4929 6

The pseudo-continuum was determined by fitting a first order polynomial
(except for the spectral range 3700-3900 A, for which we used a third
order) to the windows defined as:

(1): 3726-3729, 3740-3743, 3760-3762, 3782-3785, 3811-3812, 3869-3870,
3909-3911.
(2): 4019-4020, 4037-4038, 4060-4061, 4138-4140, 4148-4150.
(3): 4301-4305, 4310-4312, 4316-4318, 4377-4381, 4392-4394, 4397-4398.
(4): 4820-4830, 4890-4900.
(5): 4439-4440, 4445-4446, 4478-4479, 4503-4506.
(6): 4900-4902, 4905-4906, 4915-4916, 4928-4929, 4948-4950.



The tar gziped files contain the equivalent width of the Balmer lines
(Hb, Hd and H8) and HeI lines (3819, 4026, 4388, 4471 and 4922):

Ew-Hb.tab, Ew-Hd.tab, Ew-H8.tab
Ew-He3819.tab, Ew-He4026.tab, Ew-He4388.tab, Ew-4471.tab, Ew-4922.tab

Column 1: effective temperature
Column 2-9: Equivalent width of stars with gravity,
log g = 5.0, 4.5, 4.0, 3.5, 3.0, 2.5, 2.0, 1.5.

*******************************************************************************

Paper II

Reference paper:

"Synthetic spectra of H Balmer and HeI absorption lines.
II: Evolutionary synthesis models for starburst and post-starburst galaxies."
by Rosa M. Gonzalez Delgado, Claus Leitherer, & Timothy Heckman.
1999, ApJS, accepted

Abstract:

We present evolutionary stellar population synthesis models to
predict the spectrum of a single-metallicity stellar population,
with a spectral sampling of 0.3 Angstroms in five spectral regions
between 3700 A and 5000 A. The models, which are optimized for
galaxies with active star formation, synthesize the profiles of the
hydrogen Balmer series (Hbeta, Hgamma, Hdelta, H8, H9, H10, H11, H12
and H13) and the neutral helium absorption lines (HeI 4922, HeI
4471, HeI 4388, HeI 4144, HeI 4121, HeI 4026, HeI 4009 and HeI 3819)
for a burst with an age ranging from 1 Myr to 1 Gyr, and different
assumptions about the stellar initial mass function (IMF).
Continuous star formation models lasting for 1 Gyr are also
presented. The input stellar library includes NLTE absorption
profiles for stars hotter than 25000 K and LTE profiles for lower
temperatures. The temperature and gravity coverage is 4000 K
computed for solar and 1/20 sollar metallicity.

FILES
-----

1. Synthetic spectra for evolving populations


1.1 Burst models at solar metallicity (Z=0.02) with different assumptions
on the IMF are in the gziped tar files:

burst-235-1-80-Z02.tar.gz (IMF slope 2.35, Mlow=1 Msol, Mup= 80 Msol)
burst-235-1-30-Z02.tar.gz (IMF slope 2.35, Mlow=1 Msol, Mup= 30 Msol)
burst-235-5-80-Z02.tar.gz (IMF slope 2.35, Mlow=5 Msol, Mup= 80 Msol)
burst-235-10-80-Z02.tar.gz (IMF slope 2.35, Mlow=10 Msol, Mup= 80 Msol)
burst-100-1-80-Z02.tar.gz (IMF slope 1.00, Mlow=1 Msol, Mup= 80 Msol)
burst-330-1-80-Z02.tar.gz (IMF slope 3.30, Mlow=1 Msol, Mup= 80 Msol)


1.2 Burst models at Z=0.001 metallicity (1/20 Zsol) are in the gziped tar file:

burst-235-1-80-Z001.tar.gz (IMF slope 2.35, Mlow=1 Msol, Mup= 80 Msol)


Each of these tar files contains the results at different ages, from 0.01 Myr
to 1000 Myr (e.g. b1-235-1-80-Z02 is for a burst 1 Myr old).

The burst models are computed for a total mass of 10^6 Msol.


1.3 Continuous star formation models (csf) at solar metallicity (Z=0.02) are
in the gziped tar file:

csf-235-1-80-Z02.tar.gz (IMF slope 2.35, Mlow=1 Msol, Mup= 80 Msol)

This tar file contains:

csf-H10-235-1-80-Z02 (covers the spectral range: 3720-3920 A)
csf-Hd-235-1-80-Z02 (covers the spectral range: 3990-4150 A)
csf-Hg-235-1-80-Z02 (covers the spectral range: 4300-4400 A)
csf-He4471-235-1-80-Z02 (covers the spectral range: 4420-4580 A)
csf-Hb-235-1-80-Z02 (covers the spectral range: 4820-4900 A)
csf-He4922-235-1-80-Z02 (covers the spectral range: 4900-4950 A)

The csf models are computed for a star formation rate of 1 Msol/yr.


Column 1: age (yr)
Column 2: wavelength (Angstroms)
Column 3: logarithm of the total luminosity (erg/s/A)
Column 4: normalized spectrum
Column 5: logarithm of the stellar luminosity (erg/s/A)
Column 6: logarithm of the nebular continuum luminosity (erg/s/A)


2. Equivalent widths of the Balmer and He I lines are in the gziped tar file
Ew-models.tar.gz, that contains:

Ew-H-burst-235-1-80-Z02.tab (Ew of Hb, Hg, Hd, H8, H9 and H10)
Ew-He-burst-235-1-80-Z02.tab (Ew of HeI 4922, 4471, 4388, 4026 and 3819)
Ew-burst-235-1-30-Z02.tab (Ew of Hb, Hd, H8, HeI 4471, HeI 4026 and HeI 3819)
Ew-burst-235-5-80-Z02.tab (Ew of Hb, Hd, H8, HeI 4471, HeI 4026 and HeI 3819)
Ew-burst-100-1-80-Z02.tab (Ew of Hb, Hd, H8, HeI 4471, HeI 4026 and HeI 3819)
Ew-burst-330-1-80-Z02.tab (Ew of Hb, Hd, H8, HeI 4471, HeI 4026 and HeI 3819)

Ew-H-csf-235-1-80-Z02.tab (Ew of Hb, Hg, Hd, H8, H9 and H10)
Ew-He-csf-235-1-80-Z02.tab (Ew of HeI 4922, 4471, 4388, 4026 and 3819)

Ew-H-burst-235-1-80-Z001.tab (Ew of Hb, Hg, Hd, H8, H9 and H10)
Ew-He-burst-235-1-80-Z001.tab (Ew of HeI 4922, 4471, 4388, 4026 and 3819)