Dear VALD-EMS user,
this is the first of several notes on a major upgrade of VALD line
lists and user documentation on available extraction modes and line data.
We have removed the line lists for GFIRON predicted energy levels from the
standard set of VALD-EMS to reduce the load on VALD computers. It is our
experience that those lines have no real value for spectroscopic purposes
due to the large errors in their wavelengths and their uncertain term
classification which make them very difficult to identify with real
spectroscopic features. Although usually very weak, they cause a
considerable load during compilation of the line lists, especially in the
EXTRACT STELLAR mode, and increase the size of the line lists rapidly to
the upper limit defined by VALD-EMS. If users need data from these line
lists for other applications, they should contact the VALD adminstrators.
At the end of this file we have appended the new documentation for VALD-EMS
which replaces all previous releases.
With best regards,
the VALD team
==============================================================================
Vienna Atomic Line Data-Base
============================
Electronic Mail Service
written by N.E.Piskunov
Vienna, June 1994
VALDADM revision 2.0.0
May 10, 1996
1. Rationale
------------
The Vienna Atomic Line Database (VALD) is a collection of atomic line
parameters of astronomical interest and provides tools for selecting
subsets of lines for typical astrophysical applications: line
identification, chemical composition and radial velocity measurements,
model atmosphere calculations etc.
VALD Electronic Mail Service (VALD-EMS) is the main interface for
accessing VALD by external users. VALD-EMS is aimed to endorse the
following main principles of VALD access:
- subsets of spectral line lists are extracted with the tools, consistent
with the specific astronomical problem. VALD strongly discourages bulk
data transfer and concentrates more on intelligent search and extraction
procedures;
- VALD provides data sets and extraction tools suitable for several
spectroscopic applications;
- VALD is regularly updated with critically evaluated data sets. The
VALD project team experts investigate the statistical properties of the
data, extensively compare the results obtained with different data
sources, and establish the quality rating for each new source;
- VALD computers are not dedicated to the VALD project alone, so the
correct scheduling is important.
Mail access lets VALD automatically process requests and queue them for
execution on VALD computers at the most convenient time. It also allows
us to have control over the size of the data traffic and to register
VALD users.
2. How to become a VALD client?
-------------------------------
To access VALD via VALD-EMS one should register in the list of VALD
clients. This list contains INTERNET e-mail addresses from where
VALD-EMS will accept the requests. In order to do so, send an e-mail
to the VALD administrator (currently F. Kupka and N. Piskunov; for all
e-mails concerning VALD-EMS only, please avoid to use other addresses,
because that could result in a delay of the answer to your query)
with the (INTERNET) address
valdadm@galileo.ast.univie.ac.at
with your full name and your e-mail address as in the example below:
I would like to become a client of VALD. Please register me as
James Fine. My e-mail address is: jfine@not.from.this.world
Best regards, James Fine
Unemployed astronomer
If you intend to access VALD-EMS from different computers, send ALL
e-mail addresses that you intend to use.
3. VALD data sets
-----------------
When extracting line parameters with VALD-EMS, data records (in the
answer from VALD to the client) will include labels for each line,
which indicate the source of the data. Usually the label serves as a
reference to the original list, from which the gf-value of the line
has been taken from (for details see below). Currently VALD includes only
atomic lines from the following lists:
- Kurucz CD-ROM 18, December 4, 1993 edition, is the source of data
for lines with the labels:
'Bell light: Li to O'
'Bell light: F to Al'
'Bell light: Si to K'
'Bell heavy: Cu to Zn'
'Bell heavy: Ga to Ba'
'Bell heavy: La to Lu & g_Lande'
'Bell heavy: Hf to U'
'NLTE lines: He'
'NLTE lines: B'
'NLTE lines: C'
'NLTE lines: O'
'NLTE lines: Na'
'NLTE lines: Mg'
'NLTE lines: Al'
'NLTE lines: Si'
'NLTE lines: K'
'NLTE lines: Ca'
Data for La to Lu has been supplemented with experimental Lande factors,
see below.
- Kurucz CD-ROMs 20-22, July 3, 1994 edition, are the sources of data
for lines with the labels (observed energy levels only):
'GFIRON obs. energy level: Ca'
'GFIRON obs. energy level: Sc'
'GFIRON obs. energy level: Ti'
'GFIRON obs. energy level: V'
'GFIRON obs. energy level: Cr'
'GFIRON obs. energy level: Mn'
'GFIRON obs. energy level: Fe'
'GFIRON obs. energy level: Co'
'GFIRON obs. energy level: Ni'
- The following are the labels for data from R.L. Kurucz and
E. Peytremann line lists (1975, SAO Special Reports, Vol. 362):
'Kurucz-Peytremann: Li to O'
'Kurucz-Peytremann: F to Al'
'Kurucz-Peytremann: Si to K'
'KP: Ca to Ni, far UV up to 903'
'Kurucz-Peytremann: Cu to Zn'
'Kurucz-Peytremann: Ga to Ba'
'Kurucz-Peytremann: La to Lu'
'Kurucz-Peytremann: Hf to U'
The Kurucz-Peytremann 1975 data was only used as a supplement list
during the creation of a more extensive extraction from Kurucz' GFIRON
data. Usually, data was taken from this source to provide information
on lines in the far UV. After line data for Ca to Ni was extracted
directly from Kurucz' CDROMs 20-22, the Kurucz-Peytremann data is not
used any more. Thus for all extractions from VALD after August 1995, this
labels will not be found in replies by VALD-EMS.
- Martin, G.A., Fuhr, J.R., and Wiese, W.L. 1988, J. Phys. Chem. Ref. Data,
17, Suppl. 3 and 4 corresponds to the labels:
'NBS: Scandium'
'NBS: Titanium'
'NBS: Vanadium'
'NBS: Chromium'
'NBS: Manganese'
'NBS: Iron'
'NBS: Cobalt'
'NBS: Nickel'
The NBS (NIST) data for Fe 1 was merged with data from other sources
and put into 'FeI NMT Whaling and Bard & Kock' (see below), after its
wavelengths had been recalibrated. Recalibration of data for other ions
will be done continuously.
- Bizzarri, A., Huber, M.C.E., Noels, A., Grevesse, N., Bergeson, S.D.,
Tsekeris, P., Lawler, J.E., 1993, A&A 273, 707
as well as
- Ryabchikova, T.A., Hill, G.M., Landstreet, J.D., Piskunov, N.,
Sigut, T.A.A., 1994a, MNRAS 267, 697
were used to compile a list with the label:
'Ti 2 accurate gf-values'
- Pinnington, E.H., Ji, Q., Guo, B., Berends, R.W., van Hunen, J.,
1993, Can. J. Phys. 71, 470
as well as
- Sigut, T.A.A., Landstreet, J.D., 1990, MNRAS 247, 611
were used to compile a list with the label:
'Cr 2 accurate gf-values'
Both lists replace and supplement data from their corresponding 'NBS lists'.
- Komarovskij, V.A., 1991, Optica & Spectroskopia,
71, 559 (a) (Pr I, Pr II, Nd I, Nd II, Sm I, Sm II, Eu I, Eu II, Gd I,
Ho II, Dy I, Er I, Er II, Tm I, Yb I, Lu I)
- averaged solar gf-data (b) (Ce II)
- Bergstrom, H., Biemont, E., Lundberg, H., Persson, A.,
1988, Astron. Astrophys., 192, 335 (c) (Gd II)
- Komarovskij, V.A., Smirnov, Yu.M., 1994, Optica & Spectroscopia,
77, 194 (d) (Dy I, Dy II)
- Komarovskij, V.A., Smirnov, Yu.M., 1992, Optica & Spectroscopia,
73, 848 (e) (Gd I)
- Komarovskij, V.A., Smirnov, Yu.M., 1993, Optica & Spectroscopia,
75, 225 (f) (Er I)
includes experimental line parameters for the first and the second rare
earth spectra and has the reference:
'REE experimental & solar'
The following sources for gf-data:
- Martin,G.A., Fuhr,J.R., and Wiese,W.L. 1988, J. Phys. Chem. Ref. Data,
17, Suppl. 4 (a)
- O'Brian, T.R., Wicklife, M.E., Lawler J.E.,
Whaling, W., Brault, J.W. 1991, J. Opt. Soc. Am.
B8, 1185 (b)
- Bard, A., Kock, A., Kock, M. 1991, Astron.
Astrophys., 248, 315 (c)
- Bard, A., Kock, M. 1994, Astron. Astrophys.,
282, 1014 (d)
- Johansson, S., Nave, G., Celler, M., Sauval, A.J., Grevesse, N.,
Schoenfeld, W.G., Chang, E.S., Farmer, C.B. 1994, Astrophys. J.,
429, 419 (e)
are merged in a replacement file:
'FeI NMT Whaling and Bard & Kock'
For lines from this replacement file wavelengths, energies,
classification and multiplet numbers or any of these values
are taken from New FeI Multiplet Tables:
- Nave, G., Johansson, S., Learner, R.C.M., Torne, A.P.,
Brault, J.W. 1994, Astron. Astrophys. Suppl., 94, 221
When a spectral line does not exist in the NMT compilation, the multiplet
number is taken from Moore's MT and put in {}.
If the accuracy from b, c and d differs less than 2%,
gf-values for the same line are averaged in the final list.
A new replacement line list for La II, Pr II, Nd II, Sm II and Er II
has the label
'New REE interpolated gf-values'
This file compiles gf-values, obtained with new interpolation formulae
for intensities from NBS Monograph 145 (C.R. Cowley, private communication).
Wavelengths have been calibrated to match data from 'Bell heavy' for simple
replacement of gf-values for identical lines which are present in both lists.
Linelists for REE elements are now supplemented by experimental
Lande factors taken from:
- Blaise, J., Wyart, J.-F. 1984, Physica Scripta, 29, 119 - NdII lines
- Ginibre, A. 1989, Physica Scripta, 39, 694 - PrII lines
- Martin, W.C., Zalubas, R., Hagan, L. 1978, NSRDS-NBS 60 - other
REE elements (from NIST atomic line database, AEL section)
Additional data for Ga and Xe was taken from
- Ryabchikova, T. A., Smirnov, Yu. M., 1994, Russian Astron. J. 71, 83
to create
'Ga 2 accurate gf-values'
and from
- Wiese, W. L., Martin, G. A., 1980, NSRDS-NBS 68, Wavelengths and
Transition Probabilities for Atoms and Atomic Ions, Part 2. US
Government Printing Office, Washington, DC
- Ryabchikova, T. A., Smirnov, Yu. M., 1989, Astron. Tsirk. No.1534, 21
to create
'Xe 2 accurate gf-values'
VALD is constantly adding more lines, so look for the most recent
version of this document for the actual references and the corresponding
labels. Please take into account that for all modes of data extraction
except for SHOW LINE (see Section 5), data is merged from different
lists and the label refers to the source of the gf-value only. If you
need the source for atomic data, other than gf, you have to use the
SHOW LINE request (see Section 6), which enables you to see how the
data from various sources are merged for a particular line.
4. VALD-EMS request
-------------------
A VALD-EMS request is an ordinary electronic mail, sent via INTERNET to:
vald@galileo.ast.univie.ac.at or vald@131.130.36.8. Each mail can include
ONLY ONE request. The request consists of a number of lines. ONLY THE FIRST
80 CHARACTERS OF EACH LINE ARE INTERPRETED BY VALD-EMS. The request starts
with a line containing a string:
begin request
and ends with a line:
end request
Spaces are ignored and VALD is case insensitive, so the line
EndRequest
is also a valid termination for the request. All characters following the
symbol # are ignored by VALD. This can be used for comments. For example:
Begin request # this is a comment for the first line
All mail is processed at certain times of the day and valid requests
are interpreted and submitted for execution in the order of arrival.
After the request has been processed, the output file is mailed back
to the client. This file contains: VALD-EMS REQUEST NUMBER, all
diagnostic information (syntactic errors, wrong parameter values, etc.)
and the extracted parameters. If the client has difficulty identifying
the problem with his/her request, he/she should address the VALD
administrator ans supply the VALD-EMS request number, which appears on the
first line of the reply mail.
5. Types of request
-------------------
VALD-EMS currently supports 4 types of requests:
show line - extracts all information, available in VALD, about
a specific spectral line (although more than one line
could appear in the output);
extract all - extracts best atomic parameters for all spectral lines
in a given spectral window;
extract element - extracts best atomic parameters for all spectral lines
of the particular chemical element or ion in a given
spectral window;
extract stellar - extracts all spectral lines (with their best parameters),
which produce significant absorption in a stellar
atmosphere with given effective temperature and gravity.
The type of the request is indicated by one of the keywords, listed above,
placed in the second line of the request. The content of the request
depends on its type as described in the following sections. Compulsary
parameters are inclosed in angle brackets <...> while optional parameters
are put in square brackets [...].
6. SHOW LINE request
--------------------
This request must have the following format:
begin request
show line
, [spectral_number_1]
, [spectral_number_2]
...
end request
where is the central wavelength of the line in
Angstroems. determines the spectral range (it must not
exceed 1 Angstroem) from -
to + , where VALD will
search for the line. and are defined in
a conventional way: =1 corresponds to neutral atoms,
2 to singly ionized, etc. Show line requests for multiple spectral
intervals may be combined in the same request. The current limit for
multiple spectral intervals in one show line request is 100.
Example:
begin request # Start the request
show line # Select request type
4491.405, 0.02 # Search line between 4491.385
# and 4491.425 Angstroems
Fe 2 # The line is formed by singly ionized iron
# Next request starts below
6439.07, 0.01 # Search line between 6439.06
# and 6439.08 Angstroems
Ca 1 # The line is formed by neutral calcium
end request # The end of the request
The reply mail from VALD will contain the following table:
============= job.000875 =============
# begin request # Start the request
# show line # Select request type
# 4491.405, 0.02 # Search line between 4491.385
# # and 4491.425 Angstroems
# Fe 2 # The line is formed by singly ionized iron
# # Next request starts below
# 6439.07, 0.01 # Search line between 6439.06
# # and 6439.08 Angstroems
# Ca 1 # The line is formed by neutral calcium
# end request # The end of the request
===============================================================================
Wavelength window for scan: 0.020 Angstroem.
Highest ion number allowed: 5
Maximum excitation potential
for lower energy level: 50.000 eV
Lines found:
Wavelength in A Element/Ion log gf E(low) in eV E(high) in eV
Lande: eff. low high gamma.Rad gamma.Stark gamma.VdW
terms (low -> high) accuracy (multiplet or comments)
database reference for all values
------------------------------------------------------------------------------
4491.400 ( 0) Fe 2 -2.700 ( 5) 2.855 ( 0) 1.5 5.615 ( 0) 1.5
99.00 ( 0) 99.00 99.00 0.000 ( 0) 0.000 ( 0) 0.000 ( 0)
b 4F z 4F* C (37)
NBS: Iron
4491.405 ( 3) Fe 2 -2.684 ( 3) 2.856 ( 3) 1.5 5.615 ( 3) 1.5
0.42 ( 3) 0.40 0.44 8.481 ( 3) -6.599 ( 3) -7.946 ( 3)
(3F)4s b4F (5D)4p z4F
GFIRON obs. energy level: Fe
------------------------------------------------------------------------------
These data should be combined to the following lines:
(only output for short format displayed)
WL in A El/Ion log(gf) Ei[eV] Ji Ek[eV] Jk gl gam.r gam.s gam.w
------------------------------------------------------------------------------
4491.405 Fe 2 -2.700 2.856 1.5 5.615 1.5 0.42 8.481 -6.599 -7.946
NBS: Iron
------------------------------------------------------------------------------
==============================================================================
Wavelength window for scan: 0.020 Angstroem.
Highest ion number allowed: 5
Maximum excitation potential
for lower energy level: 50.000 eV
Lines found:
Wavelength in A Element/Ion log gf E(low) in eV E(high) in eV
Lande: eff. low high gamma.Rad gamma.Stark gamma.VdW
terms (low -> high) accuracy (multiplet or comments)
database reference for all values
------------------------------------------------------------------------------
6439.075 ( 4) Ca 1 0.470 ( 4) 2.526 ( 4) 3.0 4.451 ( 4) 4.0
99.00 ( 0) 99.00 99.00 7.730 ( 1) -5.350 ( 1) 0.000 ( 1)
3d4s 3D 3d4p 3F NBS
NLTE lines: Ca
6439.075 ( 3) Ca 1 0.394 ( 3) 2.526 ( 3) 3.0 4.451 ( 3) 4.0
1.12 ( 3) 1.33 1.25 7.649 ( 3) -6.072 ( 3) -7.788 ( 3)
3d4s 3D 3d4p 3F
GFIRON obs. energy level: Ca
------------------------------------------------------------------------------
These data should be combined to the following lines:
(only output for short format displayed)
WL in A El/Ion log(gf) Ei[eV] Ji Ek[eV] Jk gl gam.r gam.s gam.w
------------------------------------------------------------------------------
6439.075 Ca 1 0.470 2.526 3.0 4.451 4.0 1.12 7.649 -6.072 -7.788
NLTE lines: Ca
------------------------------------------------------------------------------
==============================================================================
0 in place of a damping parameter and 99 in place of a Lande factor
mark the absence of the corresponding data in VALD. The label given after
the parameters for each line indicates the source of the data. For the
section of SHOW LINE output following 'lines found' all quantities for
one line originate from the same source. The last section of SHOWLINE
output shows the combination of all sources, as it will appear for all
the other types of VALD request. Here the label indicates the source of
the gf-value.
7. EXTRACT ALL request
----------------------
This request must have the following format:
begin request
extract all
[long format]
[short format]
,
end request
where , are the limits of the spectral interval
in Angstroems. Note that VALD limits the total number of lines per single
mail to 1000, therefore the actual extraction may end somewhat shorter
of . [long format] tells VALD to include an extra line with
term designation into the output file. [short format] does not include
this line and is the default.
Example:
begin request # Start of the request
extract all # Request type
5700, 5701 # Wavelength range in Angstroems
end request # End of the request
As the result VALD will mail back to the client VALD-EMS request number,
the copy of the request and a subset of spectral lines between 5700 and
5701 Angstroems as shown below:
============= job.000873 =============
# begin request # Start of the request
# extract all # Request type
# 5700, 5701 # Wavelength range in Angstroems
# end request # End of the request
Damping parameters Lande
Elm Ion WL(A) Excit(eV) log(gf) Rad. Stark Waals factor Reference
'AR 2', 5700.0010, 23.6740, -2.570, 0.000, 0.000, 0.000,99.000,'Bell light: Si to K '
'FE 1', 5700.1280, 3.3010, -4.948, 7.623,-6.223,-7.870, 0.000,'GFIRON obs. ener
gy level: Fe '
'F 1', 5700.1380, 14.6830, -2.550, 0.000, 0.000, 0.000,99.000,'Bell light: F t
o Al '
'SC 1', 5700.1640, 1.4330, 0.290, 7.765,-6.129,-7.854, 0.920,'GFIRON obs. ener
gy level: Sc '
'TI 1', 5700.2140, 2.3050, -8.472, 6.806,-6.029,-7.851, 0.390,'GFIRON obs. ener
gy level: Ti '
'MN 2', 5700.2190, 11.0880, -3.078, 8.938,-5.730,-7.737, 1.830,'GFIRON obs. ener
gy level: Mn '
'CU 1', 5700.2370, 1.6420, -2.312, 0.000, 0.000, 0.000,99.000,'Bell heavy: Cu t
o Zn '
'V 2', 5700.2380, 9.0310, -2.975, 8.949,-4.885,-7.708, 2.060,'GFIRON obs. ener
gy level: V '
'CU 2', 5700.2880, 16.2350, -3.909, 0.000, 0.000, 0.000,99.000,'Bell heavy: Cu t
o Zn '
'MN 2', 5700.3880, 11.2850, -4.142, 8.585,-4.359,-7.458, 1.810,'GFIRON obs. ener
gy level: Mn '
............................................................................
The output columns contain element and ionization stage, central wavelength
in Angstroem, excitation in electron-Volts, log(gf), 3 damping constants
in logarithm (radiative, quadratic Stark and van der Waals) per sec
and per perturber at 10000 K (in the case of Stark and van der Waals
constants), mean Lande factor and the reference label. Zero in place of the
damping parameter and 99 in place of the Lande factor marks the absence of
the corresponding data in VALD. The label at the end of each line shows
the source of the oscillator strength value. The source of other parameters
may be different. The SHOW LINE request may be used to find out all
alternative values and their corresponding ranking, assigned by the VALD
team.
8. EXTRACT ELEMENT request
--------------------------
This request must have the following format:
begin request
extract element
[long format]
[short format]
, [spectral_number]
end request
where , are again the limits of the spectral
interval in Angstroem. Only the lines formed by in one or all
ionization stages will be extracted. [spectral_number] defines the
ionization stage: 1 stands for neutral atoms, 2 - for singly ionized,
etc. Currently VALD includes mostly lines up to the spectral number 5. If
[spectral_number] is omitted, the extraction is done for lines up to the
four times ionized atom.
Example:
begin request # Start of the request
extract element # Request type
5700, 5703 # Wavelength range in Angstroems
Fe 3 # Extract all lines of doubly ionized iron
end request # End of the request
The mail reply will look similar to the one above, except that only
lines of doubly ionized iron are included and each transition is
supplemented with term designation (long format):
============= job.000872 =============
# begin request # Start of the request
# extract element # Request type
# long format # Retrieve transition information
# 5700, 5720 # Wavelength range in Angstroems
# Fe 3 # Extract all lines of doubly ionized iron
# end request # End of the request
Damping parameters Lande
Elm Ion WL(A) Excit(eV) log(gf) Rad. Stark Waals factor Reference
'FE 3', 5701.0710, 25.0490, 0.118, 9.296,-4.877,-7.712, 1.280,'GFIRON obs. ener
gy level: Fe '
'FE 3', 5705.1470, 25.0320, -0.167, 9.360,-4.633,-7.518, 1.390,'GFIRON obs. ener
gy level: Fe '
'FE 3', 5706.4560, 25.4410, -2.858, 8.873,-5.844,-7.715, 1.150,'GFIRON obs. ener
gy level: Fe '
'FE 3', 5711.4150, 25.4410, -1.870, 8.854,-5.976,-7.715, 1.390,'GFIRON obs. ener
gy level: Fe '
'FE 3', 5712.8900, 25.0640, -0.136, 9.299,-4.968,-7.763, 1.140,'GFIRON obs. ener
gy level: Fe '
'FE 3', 5712.9330, 22.5440, 0.078, 9.237,-5.959,-7.764, 0.500,'GFIRON obs. ener
gy level: Fe '
'FE 3', 5713.9810, 25.0350, -0.438, 9.358,-4.633,-7.518, 1.480,'GFIRON obs. ener
gy level: Fe '
'FE 3', 5719.7350, 23.5300, -1.819, 9.436,-4.911,-7.594, 1.340,'GFIRON obs. ener
gy level: Fe '
9. EXTRACT STELLAR request
--------------------------
This request must have the following format:
begin request
extract stellar
[long format]
[short format]
,,,
[Chemical_composition]
......................
end request
where , are again the limits of the spectral
interval in Angstroem. Effective temperature and gravity
are used to select a solar abundant model atmosphere for estimating the
central depth of spectral lines. VALD has the latest models computed by
R.L. Kurucz (Kurucz CDROM 13, June 23, 1993 edition) covering a temperature
range from 3500 K to 50000 K and log g from 0. to 5. The chemical composition
is set as a log10 of the ratio of atomic number density to the total
number of atoms. The default values are solar. The abundance value must be
separated from the element name with a column (for example, Fe:-4.7).
Several values can be set on the same line, separated with commas. The
request mail can contain as many lines as needed to set the chemical
composition.
Example:
begin request # Start of the request
extract stellar # Request type
5700.,5703. # Specify wavelength range in Angstroems,
0.05, 2. # Look for lines reaching more than 0.05
# central depth and use microturbulence of
# 2 km/s
8000, 4.5 # Teff and Log g
Sr: -4.67, Cr: -3.37, # Setup specific chemical composition
Eu: -5.53
end request # End of the request
The return mail will contain the following table:
============= job.000871 =============
# begin request # Start of the request
# extract stellar # Request type
# 5700.,5703. # Specify wavelength range in Angstroems,
# 0.05, 2. # Look for lines reaching more than 0.05
# # central depth and use microturbulence of
# # 2 km/s
# 8000, 4.5 # Teff and Log g
# Sr: -4.67, Cr: -3.37, # Setup specific chemical composition
# Eu: -5.53
# end request # End of the request
5700.0000, 5703.0000, 14, 2197, 2.0, Wavelength region, lines selected, lines processed, Vmicro
Damping parameters Lande Central
Elm Ion WL(A) Excit(eV) Vmic log(gf) Rad. Stark Waals factor depth Reference
'CR 1', 5700.5180, 3.5510, 2.0, -1.440, 7.538,-5.991,-7.845, 1.330, 0.572, 'GFIRON obs. energy level: Cr '
'CR 1', 5700.5500, 3.4490, 2.0, -2.574, 7.812,-6.185,-7.822, 1.120, 0.227, 'GFIRON obs. energy level: Cr '
'S 1', 5700.5800, 7.8680, 2.0, -1.040, 0.000, 0.000, 0.000,99.000, 0.120, 'Bell light: Si to K '
'SI 1', 5701.1040, 4.9300, 2.0, -2.050, 8.310,-4.410, 0.000,99.000, 0.110, 'NLTE lines: Si '
'CR 2', 5701.4640, 3.8270, 2.0, -3.845, 8.677,-6.611,-7.929, 0.960, 0.649, 'GFIRON obs. energy level: Cr '
'FE 1', 5701.5450, 2.5590, 2.0, -2.216, 8.167,-6.052,-7.840, 1.100, 0.266, 'FeI NMT Whaling and Bard & Kock '
'CR 2', 5701.9090, 6.5780, 2.0, -4.251, 8.431,-6.647,-7.900, 1.210, 0.063, 'GFIRON obs. energy level: Cr '
'CR 1', 5702.3230, 3.4490, 2.0, -0.970, 7.797,-6.171,-7.822, 1.100, 0.638, 'GFIRON obs. energy level: Cr '
'CR 1', 5702.7060, 4.6130, 2.0, -2.089, 8.114,-6.171,-7.840, 1.040, 0.135, 'GFIRON obs. energy level: Cr '
'08000G45.KRZ',
'H : 0.91','HE: -1.05',
'LI:-10.88','BE:-10.89','B : -9.44','C : -3.48','N : -3.99','O : -3.11',
'F : -7.48','NE: -3.95','NA: -5.71','MG: -4.46','AL: -5.57','SI: -4.49',
'P : -6.59','S : -4.83','CL: -6.54','AR: -5.48','K : -6.82','CA: -5.68',
'SC: -8.94','TI: -7.05','V : -8.04','CR: -3.37','MN: -6.65','FE: -4.37',
'CO: -7.12','NI: -5.79','CU: -7.83','ZN: -7.44','GA: -9.16','GE: -8.63',
'AS: -9.67','SE: -8.69','BR: -9.41','KR: -8.81','RB: -9.44','SR: -4.67',
'Y : -9.80','ZR: -9.54','NB:-10.62','MO:-10.12','TC:-20.00','RU:-10.20',
'RH:-10.92','PD:-10.35','AG:-11.10','CD:-10.18','IN:-10.58','SN:-10.04',
'SB:-11.04','TE: -9.80','I :-10.53','XE: -9.81','CS:-10.92','BA: -9.91',
'LA:-10.82','CE:-10.49','PR:-11.33','ND:-10.54','PM:-20.00','SM:-11.04',
'EU: -5.53','GD:-10.92','TB:-11.94','DY:-10.94','HO:-11.78','ER:-11.11',
'TM:-12.04','YB:-10.96','LU:-11.28','HF:-11.16','TA:-11.91','W :-10.93',
'RE:-11.77','OS:-10.59','IR:-10.69','PT:-10.24','AU:-11.03','HG:-10.95',
'TL:-11.14','PB:-10.19','BI:-11.33','PO:-20.00','AT:-20.00','RN:-20.00',
'FR:-20.00','RA:-20.00','AC:-20.00','TH:-11.92','PA:-20.00','U :-12.51',
'NP:-20.00','PU:-20.00','AM:-20.00','CM:-20.00','BK:-20.00','CF:-20.00',
'ES:-20.00','END'
Note that for this request type the output table includes also the
microturbulence (Vmct) in km/s and the estimated central line depth
relative to continuum. We also provide the name of model atmosphere
file in the format g<10*logg>. and the abundances of the
first 99 elements. The abundances of three elements have been
substituted from the request data. However the model atmosphere used
is NOT affected by the change in composition.
10. Errors in VALD
-----------------
VALD does not guarantee in any way the absence of errors in the original
data, but we are very interested in reducing their number. Therefore we
encourage VALD users to send us error reports, so that we can notify
other users and attempt to correct the data. Please send your messages
to the VALD administrator via e-mail (valdadm@galileo.ast.univie.ac.at)
or with a regular mail to the address given below.
If data is used for spectroscopic analysis one needs to know about
the reliability of the source. The gf-values have to be used with
special care. Some of the sources contain data compilations which are
updated from time to time without prior warning by their authors (e.g.
the BELL lists). Thus there is no way to maintain a quality estimate
for EACH individual line in these lists. In addition, some lists (e.g.
GFIRON) consist of semiempirically calculated gf-values with a primary
focus on completeness of the list rather than the highest possible accuracy.
The VALD team will compile a special list for known "wrong" lines.
We will enable this compilation to be taken into account for data
extraction, too.
11. Using VALD data
-------------------
If the VALD data was used in your research work, we would appreciate the
acknowledgment of VALD and of the VALD tools that you find most useful.
We would also appreciate receiving a preprint or reprint of the relevant
papers at the following address:
VALD project
Institut fuer Astronomie
Tuerkenschanzstrasse 17,
A-1180 Wien, Austria
c/o W.W.Weiss
========================================================================
