Документ взят из кэша поисковой машины. Адрес
оригинального документа
: http://star.arm.ac.uk/~csj/lines/lte/html/lines.lte.html
Дата изменения: Thu Nov 15 23:49:29 2001 Дата индексирования: Sat Dec 22 01:47:05 2007 Кодировка: Поисковые слова: interacting galaxies |
For calculating model spectra of early-type helium stars in LTE, we maintain a database of atomic data for, mostly, blue-visual absorption lines of light elements. The data is sorted with one file for each ion.
For each absorption line included, the database includes the wavelength, oscillator strength, radiative, collisional and van der Waal's damping constants (where available), the excitation energy of the lower-level in the transition, the multplet number (from Moore's revised multiplet tables). A reference for each of the oscillator strengths and damping constants is also given. The database is dynamic, with new lines being added as required. Some vetting is applied to ensure that only the most reliable data are included. Consequently the database is quite dynamic, with corrections and updates being included at arbitrary times.
A combined linelist can be constructed for use (eg) with SPECTRUM by executing the C-Shell program lte_line. All the files necesary to run lte_line are available as a gzipped tar file. Usage should make reference to the original article describing this database (Jeffery C.S., 1991, Newsletter on 'Analysis of Astronomical Spectra', No. 16, p. 17), in addition to references to specific data sources.
The linelists have been reformatted. Damping constants have been converted to natural gammas. Damping constants and oscillator strengths are now stored as logarithms. The conversion was carried out by Philip Dufton, QUB. Consequently the description by Jeffery (1991) is partially out of date as it refers to the units and format of the data.
A number of utilities used to convert various linelist formats have been developed over the years. These are provided here "as is" with no guarantees.
The number of lines in each file is given for each ion.
Ion | I = 0 | II = + | III = ++ | IV = +++ |
Helium | He I 367 |
He I 2 |
||
Lithium | Li I 2 |
|||
Carbon | C I 15 |
C II 60 |
C III 27 |
C IV 10 |
Nitrogen | N II 220 |
N III 23 |
||
Oxygen | O I 6 |
O II 262 |
O III 6 |
|
Neon | Ne I 17 |
Ne II 33 |
||
Magnesium | Mg II 12 |
|||
Aluminium | Al II 10 |
Al III 18 |
||
Silicon | Si I 1 |
Si II 19 |
Si III 26 |
Si IV 14 |
Phosphor | P II 24 |
P III 6 |
P IV 1 |
|
Sulphur | S II 88 |
S III 32 |
||
Chlorine | Cl II 33 |
|||
Argon | A II 96 |
|||
Calcium | Ca II 21 |
|||
Titanium | Ti II 45 |
|||
Chromium | Cr II 5 |
|||
Iron | Fe I 101 |
Fe II 59 |
Fe III 12 |
|
Nickel |
lte_line | C-shell script to construct a composite linelist given specified ions |
lte_conv | A Fortan utility to convert old linelist to new format. It will work on both complete linelists (including the atomic data at the start and references at the end) or raw ion files (such as Ni2.d). |
In fact spectrum is much more powerful than the B-star tag suggests. It may be used to model a wide variety of stellar spectra in LTE and HSE, providing they are warm enough not to contain molecules. Consequentky, more estensive linelists may be reuqired to construct genuinley useful synthetic spectra. There are many sources of atomic data; the following utilities enable these to be imcorporated with existing QUB linelists. | |
vald_qub | A Fortran utility to convert linelists downloaded from the Vienna Atomic Line Database into the new QUB format. |
synspec_qub | A Fortran utility to convert linelists in SYNSPEC format into the new QUB format. |
lte_select | A Fortran utility to
manipulate QUB-format linelists. It starts by reading in an optional
initial linelist (QUB format) which will not be changed. An additional linelist (QUB format) is read in, it may be in the form of a Hubeny list, sorted by wavelength, or in some other order. Individual lines may be selected using various criteria including one or more of the following: wavelength region ions oscillator strength Examples of use: |
This page is maintained by: Simon Jeffery (csj@star.arm.ac.uk) Last modified: 13/11/01 |
The Armagh Observatory is not responsible for the content of external internet sites |