SAX2TO10 Catalog
This catalog presents the results of a 2 - 10 keV BeppoSAX survey
based on 140 high galactic latitude Medium Energy Concentrator Spectrometers
(MECS) fields, 12 of which are deep exposures of ``blank'' parts of the sky.
The limiting sensitivity is 5 x 10-14 erg/cm2/s (or mW/m2) where about 25%
of the Cosmic X-ray Background (CXB) is resolved into discrete sources. The
log N - log S function, built with a statistically complete sample of 177
sources, is steep and in good agreement with the counts derived from ASCA
surveys.
SAXAO Catalog
The SAXAO database contains the list of the all accepted AO1/AO2/AO3/A04/AO5
SAX CORE and GO program proposals, approved for the first year of operations.
The database also includes targets scheduled for the Science Verification
Phase (SVP) (from launch, 30 April 1996, till August 1996). The CORE program
includes proposals led by Principal Investigator belonging to Italian or
Dutch institutions, to the Space Science Department of ESA or to the Max
Planck Institute for Extraterrestial Physics in Garching. Approximately 80
percent of the first year observing time is allocated to the CORE program.
The remaining 20 percent of time for the first year operations is reserved
for the GO program. For the AO2 60 percent is allocated to the CORE
program and 40 percent to the GO. For the AO3 and AO4 50 percent is allocated
to the CORE program and 50 percent to the GO. More information on the SAX
mission is available at the following address http://www.asdc.asi.it and also
https://heasarc.gsfc.nasa.gov/docs/sax/saxgof.html.
SAXGRBMGRB Catalog
This is the catalog of gamma-ray bursts (GRBs) detected with the Gamma Ray
Burst Monitor (GRBM) aboard the BeppoSAX satellite. It includes 1082 GRBs
with 40 - 700 keV fluences in the range from 1.3 x 10-7 to 4.5 x 10-4
erg/cm2, and 40 - 700 keV peak fluxes from 3.7x10-8 to 7.0 x 10-5
erg/cm2/s. Some relevant parameters of each GRB are reported in the catalog.
SAXHELLAS Catalog
The BeppoSAX High Energy Large Area Survey (HELLAS) has surveyed about 85
deg2 of sky in the 4.5 - 10 keV band down to a flux of 4 - 5 x 10-14
erg/cm2/s using 142 high Galactic latitude (|b| > 20o) observations made
by the BeppoSAX Medium Energy Concentrator Spectrometer (MECS). The source
surface density of 16.9 +/- 6.4 deg2 at the survey limit corresponds to a
resolved fraction of the 5 - 10 keV X-ray background (XRB) of the order of
20-30 per cent.
Hardness ratio analysis indicates that the spectra of a substantial fraction
of the HELLAS sources (at least one-third) are harder than a alphaE = 0.6
power law. This hardness may be caused by large absorbing columns. The
hardness ratio analysis also indicates that many HELLAS sources may have a
spectrum more complex than a single absorbed power law. A soft component,
superimposed on a strongly cut-off power law, is likely to be present in
several sources.
There is no overlap among the 142 fields used and, wherever possible, multiple
observations of the same field have been merged in one single pointing to
increase the sensitivity. Fields were selected among public data (such as that
of March 1999) and the authors' proprietary data. Fields centered on bright
extended sources and bright Galactic sources were excluded from the survey, as
were fields close to the Large Magellanic Cloud (LMC), Small Magellanic Cloud
(SMC) and M 33. Most of the fields have exposures between 30 and 100 ks, and
20 fields have an exposure higher than 80 ks (see Fig. 1 of reference paper).
Sources were detected in images accumulated between 4.5 and 10 keV.
Source count rates in four bands (1.3 - 10 keV, total or T; 1.3 - 2.5 keV,
low band or L; 2.5 - 4.5 keV, middle band or M; 4.5 - 10 keV, high band or H)
were extracted and corrected for the energy-dependent vignetting
and for the MECS PSF. The count rates were converted to fluxes using a
conversion factor of 7.8 x 10-11 erg cm-2 s-1 (5 - 10 keV flux)
per one '3 ECS count' (4.5 - 10 keV) appropriate for a power-law spectrum with
alphaE = 0:6. The factor is not strongly sensitive to the spectral shape,
owing to the narrow band: thus, for alphaE = 0.4 and 0.8 it is 8.1 and 7.6
x 10-11 erg cm-2 s-1, respectively. A conversion factor of 9:9
x 10-11 erg cm-2 s-1 per one '3 MECS count' has been used for sources
under the 550 micron (um) beryllium strongback supporting the MECS window to
account for the reduced detector sensitivity.
SAXHELLASR Catalog
This table contains results of a complete radio follow-up obtained with the
VLA and ATCA radio telescopes down to a 6-cm flux limit of about 0.3 mJy
(3-sigma) of all the 147 X-ray sources detected in the BeppoSAX HELLAS survey
(Fiore et al. 2001, MNRAS, 327, 771). The authors found 53 X-ray/radio likely
associations, corresponding to about one-third of the X-ray sample. Using the
two-point spectral index alpharo = 0.35 they divided all the HELLAS X-ray
sources into radio-quiet and radio-loud. They have 26 sources classified as
radio-loud objects, corresponding to 18 per cent of the HELLAS sample. In
agreement with previous results, the identified radio-loud sources are
associated mainly with Type 1 active galactic nuclei (AGNs) with L5-10keV
>~ 1044 erg/s, while all the identified Type 2 AGNs and emission-line
galaxies are radio-quiet objects with L5-10keV <~ 1044 erg/s.
The 20 HELLAS sources with Declinations south of -40o were observed with
the ATCA, while the 127 sources with more northerly Declinations were observed
with the VLA. For these latter sources a complete covering at 20 cm down to
the 5-sigma flux limit of 2.5 mJy is already available with the NRAO/VLA Sky
Survey (NVSS) while the FIRST survey (Faint Images of the Radio Sky at Twenty
centimeters) is available only for 27 HELLAS sources (5-sigma limit of ~ 1
mJy).In order to obtain information also on the radio spectral properties of
the HELLAS sources the authors adopted the following strategy. All the 147
HELLAS sources were observed at 6 cm down to a 1 -sigma flux limit of ~ 0.10
- 0.25 mJy. For the 20 HELLAS sources observed with the ATCA, they took
advantage of the fact that the 6 and 3 cm receivers of the ATCA share a common
feed-horn and they observed simultaneously also at 3 cm, obtaining a 3-cm flux
limit of ~ 0.22 mJy (1-sigma level).
Starting from the radio position of the 53 X-ray/radio associations, the
authors searched for optical counterparts within 5 arcseconds from the radio
position using the optical positions of the 61 HELLAS sources identified by La
Franca et al. (2002, ApJ, 570, 100 = LF02), the USNO-A2.0 1 optical catalog,
the APM 2 optical catalog and the NASA Extragalactic Database (NED). 24
X-ray/radio associations have been identified with sources in LF02 (10 Type 1
AGN, 4 Type 2 AGN, 2 BL Lacs, 3 Clusters, 4 ELGs and 1 Radio galaxy), 1 has
been identified with a z = 0.708 Radio galaxy in the Lockman Hole using NED
(see Table 2 source 116 in Lehmann et al. 2000, A&A, 354, 35 for a description
of this source), 13 have an optical (R-band) identification in the USNO and/or
APM catalogue while 15 X-ray/radio associations do not have an optical
identification brighter than R=20.
SAXNFILOG Catalog
The SAXNFILOG database contains the SAX Narrow Field Instruments (NFI)
approved pointings, but it also served as an observations log.
It includes data taken during AO1, AO2, AO3, A04 and AO5 cycles and the Science
Verification Phase (SVP).
SAXWFCCAT Catalog
This table contains the catalog of X-ray sources detected by the
two Wide Field Cameras (WFCs) in complete observations on board BeppoSAX
during its 6 years of operational lifetime, i.e., between April 1996 and
April 2002. The BeppoSAX WFCs were coded mask instruments sensitive in the
2 - 28 keV energy band with a 40 x 40 square degree fields of view,
pointing in opposite directions and perpendicularly to the BeppoSAX
Narrow Field Instruments (NFI). The WFCs were usually operated
simultaneously to NFI observations, each lasting up to several days.
The WFCs observed thus the entire sky several times with a typical
sensitivity of 2 to 10 mCrab.
A systematic analysis of all WFC observations in the BeppoSAX archive
has been carried out using the latest post-mission release of the WFC
analysis software and calibrations. The catalog includes 253
distinct sources, obtained from a total sample of 8253 WFC detections.
SAXWFCCAT2 Catalog
During the operational life of the Italian/Dutch X-ray satellite (1996-2002),
BeppoSAX, its two Wide Field Cameras (WFCs) performed observations that
covered the full sky at different epochs. Although the majority of the
analyses performed on BeppoSAX WFC data concentrated on the detection of
transient sources, the authors have now applied the same techniques developed
for the INTEGRAL/IBIS survey so as to produce a similar analysis of the
BeppoSAX WFC data. This work represents the first unbiased source list
compilation produced from the overall WFC data set which is optimized for
faint persistent source detection. This approach recovered 182 more sources
compared to the previous WFC catalog reported in Verrecchia et al. (2007,
A&A, 472, 705; the HEASARC SAXWFCCAT table). The present catalog contains 404
sources detected between 3 and 17 keV, 10 of which are yet to be seen by the
new generation of telescopes.
SAXWFCLOG Catalog
The SAXWFCLOG database contains the SAX WFCs observations log for the AO
cycles and the Science Verification Phase (SVP).
The two WFCs are located at 90 degrees from the NFI and set 180 degrees
apart. The field of view is 40 deg X 40 deg and the coordinates given
in this databases are the pointing positions.
The database is updated regularly to include the most recent timeline, and
updates are provided by the SAX-Science Data Center in Rome.
