A list of radio-loud RASS sources was constructed by finding all unresolved
RASS and VLA sources with offsets 25
(
40
) in the
central (outer) 3
3
fields.
For sources resolved in either
band, a larger offset of 60
(100
) in the central (outer) 3
3
fields was permitted to capture extended X-ray clusters
containing a radio galaxy or extended radio sources associated with an X-ray
AGN. A total of 74 reliable matches were found. Table 1 gives the
resulting RASS-VLA unresolved sources (28 matches) and Table 2
contains RASS-VLA sources where either the radio or X-ray source is
extended or multiple (46 matches representing at least 37 separate
radio sources).
The reliability of the associations was evaluated by
repeatedly recorrelating the VLA catalog with X-ray source positions randomly
shifted from the RASS positions by a range of angular distances, typically
a few arc minutes. The simulations indicate that Tables 1 and 2 have high
reliability with % spurious RASS-VLA associations. Table 3 contains
possible additional sources (34 in number) with greater angular separations.
Here the chance of spurious associations is around 50% in the central
field and 20% in the outer fields. Most of the spurious listings
will have faint (1-2 mJy) radio flux densities.
The radio and X-ray data are summarized in the first 11 columns of the tables.
Columns 1-5 are extracted from Kollgaard et al.(1994) and give
the VLA source name, peak position in J2000, integrated flux density at 1.5
GHz in mJy with its error. Secondary radio peaks which were individually
cataloged in Kollgaard et al.are also listed. Column 6 gives the name of
the corresponding ROSAT Survey source and in Col. 7 we list the positional
offsets between the VLA and the X-ray sources in arcsec.
Column 8 indicates
whether the source lies in the inner 3 (i) or outer region (o) of the
RASS NEP field. Column 9 gives the likelihood value from the EXSAS
processing. Columns 10-11 present the 0.1-2.4 keV X-ray flux (with error)
in units of 10-14 erg cm-2 s-1, assuming a power law spectrum with photon
index
and Galactic absorption.
The RASS-VLA matches were correlated with optical catalogs produced
from densitometric scans of blue plates from the Palomar Observatory Sky
Surveys (POSS). As indicated in Sect. 2.2, two systems are used: APM
scans of the POSS-I O plates and COSMOS scans of the POSS-II J plates.
Optical positions within 4 of VLA radio positions were
considered likely matches. The resulting objects are listed in Cols.
12-15 of Tables 1-3 with optical morphological class, optical minus radio
positional offsets in arcsec, and estimated B magnitudes. A few objects
with offsets up to 8
are included when the identification is
indicated in the literature or the radio source is extended. Additional
nearby optical objects are given in the table notes with offset
in arcsec. As the radio sources in
Table 2 are often extended, the absence of a listed optical
counterpart is not a reliable indication that a counterpart is not
present.
We found significant discrepancies, up to 3 magnitudes, between APM and
COSMOS blue magnitudes and, where available, between both systems and
published magnitudes. These differences are much greater than expected from
the changes in emulsion-filter combinations used for POSS-I and II. We
constructed a rough magnitude system by calibrating COSMOS measurements
to APM magnitudes for stellar sources within 1 of RASS-VLA
sources. A linear regression between COSMOS MCOR values and
gives MCOR =
. This formula was used to convert COSMOS measurements into
magnitudes when an object was found on both plates. Values are rounded to
the nearest 0.5 magnitude. However, many objects are found only in one of
the APM or COSMOS catalogs, and a cross-calibration could not be
performed in these cases. We caution that magnitudes reported in the tables are
based on heterogeneous magnitude systems, and may suffer systematic
uncertainties around
1. When a source was not detected
by either APM or COSMOS blue plates, a limiting magnitude of B > 22.5
from the deeper COSMOS plates is adopted.
In Tables 1-3, Col. 12 presents an optical morphology classification
derived in most cases from the COSMOS object catalog: E = empty field; F =
too faint to classify; G = galaxy; Gp = galaxy group; S = stellar. The Gp
classification was made by us as described in Sect. 4.2. Columns 13-14 give the
optical minus VLA positional offsets in arcsec. Column 15 gives approximate
B magnitudes derived as follows: a = APM object catalog; b = COSMOS
object catalog calibrated to APM magnitudes; c = COSMOS object
catalog.
The three objects with an "a" code occurred in the region where
no blue POSS II plate was available (one case)
or were not detected on the blue POSS II plate but were detected on
the red plate and/or POSS I.
Magnitudes without codes were obtained from the literature cited in
the table notes. Table notes give cross-identifications and associated data
obtained from the NASA Extragalactic Database (NED) or from Véron-Cetty
& Véron (1996), and indicate whether radio or X-ray extended
structure is present. Table notes also list nearby optical objects (from
COSMOS or APM catalogs) with magnitudes and in
arcsec.
Copyright The European Southern Observatory (ESO)