All Tables
- Table 2:
Comparison between our solar abundances (second Col.) and those of
Grevesse & Sauval (2000) (third column). For iron, the abundance
value obtained using ionised lines is also given. The number of lines
and the standard deviation of the measurements for each species are
also reported in the fourth and in the fifth column respectively.
When only three or two lines are measured (sodium and aluminum), half
of the difference between the maximum and minimum value is reported
instead of the standard deviation.
- Table 4:
Table of the typical errors associated with abundance
measurements of iron (about sixty Fe I lines), sodium (two or
three lines), and nickel (about twenty lines).
- Table 5:
EWs of the 6300.30 Å O I line derived oxygen abundances. In
both columns, the global cluster errors for the cluster refer to the
standard deviations in the abundances originating in the single stars,
while reported errors in single star abundance measurements come from
the uncertainty in the EWs. See the text for the errors due to the
parameter uncertainty.
- Table 7:
Results of our revised abundance analyses of Praesepe stars. In the
upper part of the table, theoretical parameters are used (temperature
from the photometry, gravity from the models and the temperature and
microturbulence from the fit). In the lower part of the table, we
adopted the most reliable measurements of parameters found by ignoring
constraints from photometry or models. Also these analyses confirm the
high metallicity of Praesepe is evident.
- Table 8:
Comparison between spectroscopic and computed values, i.e.
photometric temperatures and gravities computed assuming photometric
temperatures. The photometric temperatures are computed by means of
the infrared magnitudes from the 2MASS catalogue (shown in the second,
third and fourth column), which were converted into TCS colours, and
the available V magnitudes (shown in fifth column).
- Table 3:
Table of the computed abundances, all
from the neutral-element lines. In the rows with the average the
standard deviation refers to the different stellar values within the
cluster (for NGC 3680 we give half of the difference between the two
stellar values). In the other rows the standard deviations refer to
the measurements from he different lines. When no more than 3 lines
are used for a given element, half the difference between the largest
and the smallest values, rather than the standard deviation, is
given. In the case of Praesepe the errors adopted are higher than the
standard deviation: 0.10 dex.
- Table 6:
Literature data about high-resolution spectroscopic studies of
clusters that have more than one high-resolution entry. Errors refer
to the rms dispersion between stellar values, or half of the full
spread when only two or three stars are studied. From Cols. 1 to 8 we indicate the abundance measurements. In Col. 9, the number
of stars used is given; in Col. 10, the reference, in
Cols. 11 and 12, we indicate, respectively, the spectral resolution and the
instrument and/or the observatory.
- Table 9:
Compilation of high-resolution studies on open
clusters. The first panel shows the results of the abundance
analyses, while the second one summarises dataset and clusters'
properties, showing, in the given order, the number of stars used, the
reference (i.e. number in the bibliography and ``PPF'' for the present
study; some of the cited references for the abundances are
compilations of the results obtained by the same group), the spectral
resolution power, the instrument and/or the telescope employed,
clusters' Galactocentric distances and ages. The two latter values
are flagged with a letter according to the reference used:
F for
Friel & Janes (1993), B for Bragaglia & Tosi (2006), C for Carraro & Chiosi (1994) and W for the WEBDA
database.