Where possible we use the IRAS FSC position and band fluxes instead of the IRAS PSC entries. Due to an improved position determination in the IRAS FSC the IRAS names for identical objects may differ between the PSC and the FSC. Below we list PSC and FSC names for identical objects.
Table 3: IRAS PSC galaxies and ROSAT All-Sky Survey II sources separated by
less than 100 arcsec. Column 1 gives the object's name in the Faint Source or Point
Source Catalog. If an object is known under a different name in the NED database,
that name is given in Col. 2; a galaxy may have multiple names from listings
in different catalogues. NED counterparts
within a distance of 2 arcmin from the ROSAT position (their total number is given
in Col. 3) are listed in subsequent rows; at most nine are listed. The RASS II
position is given in decimal degrees in Cols. 4 and 5, the NED
position in Cols. 6
and 7, the NED morphological type and object classification in Col. 8, the
optical magnitude in Col. 9, major and minor apparent galaxy diameter (in arcmin)
in Cols. 10 and 11, radial velocity in Col. 12; 1for velocities larger 50 000 km
s-1 the nondimensional redshift is given. Column 13 lists our classification
grade of the X-ray to correlation quality (see Sect. 2.3): objects with grade 1 and 2 are
secure identifications, and for them the soft X-ray and far-infrared properties
are listed in Tables 4 and 5. Objects with classification grades 3, 4, 5 or 9 are
not considered secure identifications
Table 4: X-ray and far-infrared properties of galaxies detected in RASS II. A
power-law spectral model is used with photon index 
and absorbing
hydrogen column density 
equal to the Galactic value along the line
of sight to convert the PSPC count rates (Col. 4) to 0.1-2.4 keV energy
fluxes (Col. 14). The PSC name is listed in Col. 1, the RASS II position, and
0.1-2.4 keV count rate with corresponding error in subsequent columns. For
objects with correlation grade 2 (Col. 7) the initial RASS II
count rate (also
given in the images) was reduced by the contribution of apparently
unassociated
emission. The number of source photons (corrected for grade 2 objects), the
total RASS exposure time, and the Galactic absorption column density are
given in Cols. 5, 6, and 8,
respectively. Column 9 lists the redshift given by NED. Columns 10 to 13 give
the PSC fluxes. Column 15 gives the integrated 40-120 
m flux.
The 0.1-2.4 keV and 40-120 m luminosities of Cols. 16 and 17 are derived
using Eq. (7) of Schmidt & Green (1986). The luminosities are only given
for radial velocities larger than 1000 km s-1
Table 5: Soft X-ray and far-infrared properties of galaxies detected
in RASS with
more than 100 photons. X-ray spectral properties are derived
from a power law spectral
fit with free spectral photon index and absorbing column, under
the constraint that
the absorption column be at least as large as the Galactic value.
Column 2 lists the
Galactic hydrogen column density, Cols. 3 to 5 the best power law
model fit's
absorbing column (the Galactic absorption column is given with
error zero in
Col. 3 when in the spectral fit the absorbing column was limited by the
Galactic value), the monochromatic flux at 1 keV in units of
photons cm-2
s-1 keV-1, the photon index, and 
. The observed
0.1-2.4 keV count
rate is given in Col. 7. Columns 8 and 9 list the total exposure
time during
the ROSAT All-Sky Survey and the detected number of photons,
respectively. The modeled
flux in the 0.1-2.4 keV and 40 - 120 m energy bands
are given in Cols. 11
and 12, respectively. Column 10 gives the NED redshifts
with which, if available,
the soft X-ray (Col. 11) and far-infrared (Col. 12) fluxes were converted
to luminosities (Cols. 13-14). Differing assumed continuum slopes in the
soft X-ray and FIR may result in differences
between 
and 
because of variant K-corrections
in the X-ray and FIR bands
