Rosa M. González Delgado & Claus Leitherer, 1999, Astrophysical Journal Supplements accepted.
A grid is presented of synthetic profiles of stellar H Balmer and HeI lines at optical wavelengths with a sampling of 0.3 Å. 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. Hb) 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 have also been computed. The full set of the synthetic stellar spectra is available for retrieval here below and at our american website http://www.stsci.edu/science/starburst/ .
The main spectral lines synthesized are:
spectral range | main lines |
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 |
Column 1: Effective Temperature (from 4000 K to 50000 K).
Column 2: Wavelength (in Angstroms).
Cols. 3-13: normalized spectrum for the 11 values of
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.
The equivalent widths of the lines have been measured in the following spectral windows:
line | ew window | continuum |
H8 | 3874-3904 | 1 |
Hd | 4070-4130, 4086-4116 | 2 |
Hg | 4311-4371, 4830-4890 | 3 |
Hb | 4830-4890, 4846-4876 | 4 |
HeI 3819 | 3816-3823 | 1 |
HeI 4009 | 4006-4012 | 2 |
HeI 4026 | 4020-4031 | 2 |
HeI 4121 | 4118-4124 | 2 |
HeI 4143 | 4139-4148 | 2 |
HeI 4388 | 4381-4395 | 3 |
HeI 4471 | 4464-4478 | 5 |
HeI 4922 | 4915-4929 | 6 |
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 |
Ew-Hb.tab, Ew-Hd.tab, Ew-H8.tab,
Ew-He3819.tab, Ew-He4026.tab, Ew-He4388.tab, Ew-He4471.tab, Ew-He4922.tab,
The format of each of these files is:
Column 1: Effective Temperature
Cols. 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.