### Auxiliary tables for a paper OGLE-3 (AJ, **115**, 1135, 1998)
on long-period (>1 day) contact systems in the OGLE sample

#### Read Me First

The tables are in plain unformatted ASCII.

The tabulation is as follows:

inclination 30 (2.5) 90 degr

mass-ratio 0.05 (0.05) 1.0

degree of contact 0 (0.5) 1

** Note: **
All the calculations here are for the gravity brightening
exponent equal to von Zeipel's
(T_{eff} ~ g^{1.0}) at high
effective temperatures (32,000 K) in the Cousins I-band (as used by
OGLE). These calculations have an exploratory nature and are not meant
to be used for any particular system. The adopted bracketing
atmospheres (34,500 and 30,250 K) were characterized by relative fluxes
1.078 and 0.922 and by the linear limb darkening coeffecients 0.20 and
0.23.

Of note are the following properties, which distinguish the
results for hot contact systems from those for the
solar-type (W UMa) case:

- Since the I-band is far redward of the spectrum peak for hot
stars, the relative fluxes in the bracketing atmospheres differ
rather moderately;
- Because of the same reason, the limb darkening coefficients are small;
- These two effects over-compensate the influence of the stronger
gravity brightening
** producing similar perhaps even
slightly less deep eclipses than for typical solar-type systems. **

There are two tables for the hot systems:

coef 138278 bytes, 13 columns
7 characters wide

Each line contains the value of inclination (degr), mass-ratio, and
eleven cosine coefficients a0 to a10 (in light units, not magnitudes!).
There are three successive tables of the coeffecients
for three values of the degree of contact: f=0 (inner),
f=0.5, f=1 (outer).

depth of minima 43589 bytes, 4 columns
7 characters wide

Each line of the table
contains the value of inclination (degr), mass-ratio, and
the depth of both minima (in maximum light units),
1-l(0^{0}) and 1-l(180^{0}), for eclipses of more- and
less-massive components, respectively. Therefore, eg. to find the magnitude
drop at the eclipse of the more massive component, do not use the
depth tabulated here, but the light l(0^{0}), according to:
m(0) = -2.5 log l(0^{0}). The division into three parts of the table,
for the three values of the degree of contact, is the same as
for "coef_hot".

** Note: **
A very good representation of a light curve can be usually
obtained by calculating the Fourier series:
l=Sum(ai*cos(2*pi*i*phase), and then truncating the curved
part of the secondary (occultation) eclipse
at the level l(180^{0}) using the tables of the depth of secondary
minima 1-l(180^{0})).