The IBIS soft gamma-ray sky after 1000 INTEGRAL orbitsBased on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), Czech Republic and Poland, and with the participation of Russia and the USA.

The IBIS soft gamma-ray sky after 1000 INTEGRAL orbits

Abstract

We report here an all-sky soft gamma-ray source catalog based on IBIS observations performed during the first 1000 orbits of INTEGRAL. The database for the construction of the source list consists of all good quality data available from launch in 2002 up to the end of 2010. This corresponds to 110 Ms of scientific public observations with a concentrated coverage on the Galactic Plane and extragalactic deep exposures. This new catalog includes 939 sources above a 4.5 sigma significance threshold detected in the 17-100 keV energy band, of which 120 represent previously undiscovered soft gamma-ray emitters. The source positions are determined, mean fluxes are provided in two main energy bands, and are reported together with the overall source exposure. Indicative levels of variability are provided, and outburst times and durations are given for transient sources. Comparison is made with previous IBIS catalogs, and those from other similar missions.

gamma-rays: observations, surveys, Galaxy:general

1 Introduction

More than eleven years of observations in the energy range from 5 keV up to 10 MeV have been performed with the INTEGRAL observatory, which was selected as the M2 mission within ESA’s Horizon 2000 programme. The observing time of INTEGRAL is awarded competitively via a general programme which is open to the community at large, and includes Targets of Opportunity, normal observations and Key Programmes. The latter category consists of deep observations requiring a few Ms observing time, and may accommodate various different requests from the observer community for amalgamated single or multiple targets within the selected sky fields. Typical observation times range between 100 ks and more than two weeks, and a number of the programmes have provided regular monitoring of the Galaxy by returning to the same area of sky on multiple occasions.

Survey observations with INTEGRAL make full use of the large field of view of the IBIS coded mask telescope, one of the two main instruments on board. IBIS, with its large field of view (28 x 28, 9 x 9 fully coded), excellent imaging and spectral capability is ideal for survey work (Ubertini et al., 2003). The imaging system provides a location accuracy of 0.5-4 depending on the source strength. For the large numbers of newly-detected unidentified sources, these localizations are sufficiently good to enable searches for their soft X-ray counterparts. Results presented here are derived from ISGRI (Lebrun et al., 2003), the low energy array on IBIS, a pixelated CdTe detector operating in the energy band 17-1000 keV.

Since 2004, a sequence of IBIS survey catalogs (Bird et al., 2004, 2006, 2007, 2010) based on data from the ISGRI detector system have been published at regular intervals, making use of an ever-increasing dataset as new observations become publicly available. The last edition of the IBIS survey (Bird et al., 2010), comprising 723 sources, was released in 2010, and was based on INTEGRAL data collected between 2003 February and 2008 April. The overall content of this unbiased catalog comprised known AGNs (35% ), X-ray binaries (31%), pulsars and other sources (5%) while 29% of the sources were unknown or detected for the first time with INTEGRAL. A large number of observations at X-ray wavelengths with Swift, XMM and Chandra followed in order to obtain better position determinations and hence a more reliable optical identification. Other INTEGRAL-based catalogs have been produced, and focus on specific sky areas such as the Galactic Plane (Krivonos et al., 2012, 2010) or on specific source classes (Revnivtsev et al., 2008a; Lutovinov et al., 2007, 2013; Bassani et al., 2006; Malizia et al., 2012; Revnivtsev et al., 2008b; Scaringi et al., 2010a; Beckman et al., 2009; Sazonov et al., 2007). Another catalog produced in 2008 (Bouchet et al., 2008) was based on SPI (the other primary wide-field instrument on INTEGRAL) observations. Apart from just one variable source, all the objects listed in that publication were included in the 4th IBIS/ISGRI survey catalog (hereafter “cat4”) (Bird et al., 2010).

The most recent INTEGRAL survey (Krivonos et al, 2012) is based on nine years of averaged sky images and lists only those sources detected along the Galactic Plane () in three energy bands (17-60, 17-35 and 35-80 keV); it includes 402 objects exceeding a 4.7 detection threshold on the nine years average map.

In all, the total number of INTEGRAL-discovered sources (i.e. those with an IGR designation) from the various catalogs up to the end of 2013 consists of 560 IGR detections, of which only 39% remain unidentified. In large part this unidentified fraction can be attributed to transient sources for which rapid follow-up was not available.

A noteworthy innovation is the SIX catalog (Bottacini et al., 2012) based on a new approach developed to survey the sky at hard X-ray energies (18-55 keV energy band) by combining the observations of Swift/BAT and INTEGRAL/IBIS to enhance the exposure time and reduce systematic uncertainties. This survey may be considered a survey from a virtual new hard X-ray mission, and should provide higher sensitivity than individual instrument surveys. The method has been applied to 6200 deg of extragalactic sky (20% of the entire extragalactic sky) and lists 113 sources mostly of extragalactic nature: 91 AGNs, 2 clusters of galaxies, 3 Galactic sources, 3 previously detected X-ray sources, and 14 unidentified sources. Suppression of systematics is a key feature of this method, and no false detections due to statistical or systematic fluctuations are expected by the authors.

Here we present an update to the 4th IBIS/ISGRI catalog with data collected up to INTEGRAL orbit 1000, i.e. up to the end of 2010, that now comprises over 900 sources. For this updated database, we again made use of the ‘bursticity’ tool to improve detection of sources showing high variability and provide enhanced weak transient source detection. In particular, we use improved algorithms to provide a critical re-analysis of the methods used in Bird et al.(2010) and give additional quality flagging in order to reduce the expected levels of false detections in this new work. Details on the analysis and production of this new catalog (hereafter “this work” or “cat1000”) are in sections 2 and 3, and comparison with the more recent similar catalogs is provided in section 5.

2 Data analysis and catalog construction

2.1 Input dataset

For this work, all publicly available INTEGRAL data obtained up to the end of 2010 has been processed. This may be compared to cat4, that used public data up to April 2007 (plus Public and Core Programme data up to April 2008). During each satellite orbit (revolution; approximately three days) INTEGRAL operates by dividing each observation into a sequence of short pointings (science windows or scw) with a typical duration of 2 ks. Our dataset extends from revolution twelve onwards, and includes the performance verification, calibration, original core programme (including Galactic Centre Deep Exposure and Galactic Plane Scans) and all pointed observations selected in the various observer AO phases up to revolution 1000 (December 2010). All data from revolution twelve onwards were processed unless flagged as Bad Time Intervals (flagging is provided by the INTEGRAL Science Data Centre, ISDC) for a total of 73000 scws (cf. 39548 for cat4). The input catalog used was the INTEGRAL reference catalog v31, that includes all sources of the 4th IBIS/ISGRI catalog, further updated for any new INTEGRAL detected sources published via papers and ATELs since 2010. A final cleaning catalog containing all previously declared INTEGRAL-detected sources was created and used as the input catalog for all pipeline processing.

The total exposure in the dataset (the sum of exposures of all initially selected scw) is 124 Ms (cf. 70 Ms in cat4), and the resulting all-sky exposure distribution is shown in Figure 1 (upper).

Figure 1: (upper) Overall exposure map for 18-60 keV processing; the features of residual filtering (section 2.2.1) can be seen around the positions of the brightest sources. (lower) The exposure along the Galactic Plane resulting from all exposures, but dominated by the Galactic Bulge and Galactic Plane Scan programmes.

As a result of the Core Programme and Key Programmes that operated from 2006, the Galactic Bulge is well covered with 12 Ms and the entire Galactic Plane has a coverage of at least 300 ks, rising dramatically in areas where specific sources have been targeted. The Galactic anti-centre region has been less well covered due to mission planning constraints as this region is competing with the Galactic Centre for observing time. The exposure profile along the Galactic Plane is shown in Figure 1 (lower).

The fraction of sky exposed to a certain level is shown in Figure 2 which emphasises the different exposure patterns in the Galactic Plane () and the extra-galactic sky(). In the Galactic Plane, 75% of the sky is covered to better than 1 Ms, while only 20% of the extragalactic sky is covered to the same level. Overall, around one third of the sky is covered to 1 Ms level, and 90% of the sky is covered to 100 ks.

Figure 2: Fraction of sky covered as a function of exposure time.

2.2 Data processing and pipeline processing

The data processing was performed with the Standard OSA 9.0 software to produce sky images of individual scws in five different energy bands (17-30, 30-60, 18-60, 20-40 and 20-100 keV). For mosaic construction, source searching, candidate list production, and final source selection we have been largely following the 4th IBIS catalog procedure as described in Bird et al, 2010. In the following sections, we only report the main changes with respect to the earlier methodology.

Mosaic construction

Each scw image was tagged with its rms (after removal of sources) to act as an indicator of overall image quality. The primary aim of this step is to remove data taken during periods of enhanced background during solar activity or soon after perigee passage. Filtering was applied based on the rms value of the image background, such that the rms should not exceed a limit of 2 above the mean image rms for the whole dataset. This function somewhat overlaps with the BTI flagging provided by the ISDC, but we still removed around 5400 of the science windows that exceed this rms limit, for a loss of 11 Ms or 8% to the total exposure. We note that there is a clearly increasing trend in the image rms throughout the mission, especially in the energy bands extending below 20 keV. In future analyses, an adaptive time-varying rms filter may be required if this trend continues, but for now we used a constant threshold, and accepted a slightly higher rejection fraction in the later parts of the mission.

Although they are still processed, data taken in staring mode are not used in the construction of the final sky mosaic images as they contribute a far higher level of systematic noise than the standard dithered observations (although this effect is less pronounced from OSA 9 onwards). Some 1290 science windows in the input dataset were flagged as consisting of staring data, representing a further exposure loss of 3.2 Ms (2.5%) in map construction.

After removal of high-rms and staring data, approximately 67000 scws remained in the dataset, with a total exposure of 110 Ms. The selected science windows were then combined using a proprietary image mosaic tool which statistically averages the images from multiple input maps. This process has been optimised to allow the creation of all-sky maps based on large numbers of input science windows. Mosaics were constructed for five energy bands (see Section 2.2) with 2.4 pixel resolution, significantly oversampling the intrinsic system PSF. Mosaics were made in four projections: centred on the Galactic Center, on the Galactic anti-center, north Galactic polar and south Galactic polar. These multiple projections are intended to present the automatic source detection algorithms with source PSFs with the minimum possible distortion.

Previous catalogs have employed various timescales on which mosaics were constructed in an attempt to optimise the detection of new sources with a variety of duty cycles. We have simplified our approach, and initially constructed mosaics on only revolution and whole-archive timescales. Revolution maps are optimised to detect sources active on timescales of the order of a day and persistent sources can best be detected in an all-archive accumulation of all available high-quality data.

Candidate list construction

Maps were searched with two different algorithms, one the standard SExtractor tool (Bertin & Arnouts, 1996), the other designed specifically to compensate for the varying levels of systematic background found in INTEGRAL/IBIS mosaics. In total, 60 all-sky maps (and variants) and over 19000 revolution maps were constructed and searched. An initial candidate source list was created by iteratively merging the excess lists from each map into a base list which took the cleaning catalog as a starting point. In this way, merging commences with the best reference positions for each source, and the process also ensures that all previously declared sources are checked for their presence in the new dataset. A merge radius of 8 was used, and a new candidate was added to the base list if it exceeded a detection threshold of 4.5 in an all-archive map, or 6 in a revolution map, and could not be associated with an already listed source. The higher threshold for revolution maps is essential to remove false excesses caused by noise in these lower exposure maps. In addition to this higher threshold for revolution map excesses, a number of revolutions11 were excluded from this process due to high noise levels associated with solar activity, these being 124–129 (inclusive), 217–218, 234, 252–254, 276–277, 315, 341–342, 349, 352–356, 506–509. This process resulted in a list of 3759 excesses which was manually inspected to ensure that blended sources flagged in previous catalogs survived the merging process.

2.3 Final source list construction

Light curves were constructed for every candidate source in the five standard energy bands. A search for variable source emission was then performed on those light curves by using the ‘bursticity’ method - i.e. identifying the time window within which the source significance was optimised. Time windows in the range 0.5 days up to the full duration of the light curve were tested. Once the optimum detection time window was determined, an additional map - the ‘burst map’ - was constructed by mosaicking only those scw falling in the best time interval and using the energy band established by ’bursticity’. This method optimises the detection of any known or suspected source that emits on any timescale longer than a science window. Following this procedure, an improved significance has been obtained for 200 sources.

The final source list filtering was carried out manually. Experienced operators were presented with all the relevant data - as well as visual inspection of the maps themselves, derived parameters such as persistent significance in five energy bands, burst significance and timescales in five energy bands, local systematic levels, local image residual levels, and the total number of maps each source was detected in were quantified. A final acceptance of each putative source was made on the basis of this overall data. The overall flow of data through the analysis chain is shown in Figure 3, which also shows the selection/rejection criteria applied at each stage.

Figure 3: Data analysis and source selection flowchart, showing the filtering criteria applied at each stage.

2.4 False positive rates

The false positive rate (FPR; the fraction of ‘fake’ sources in the catalog) is a key parameter, and depends strongly on the methods used to identify, examine and verify the excesses.

The false positive rate for persistent sources found in inspection of IBIS mosaic images has been well established for previous catalogs (Bird et al., 2004, 2006, 2007, 2010; Krivonos et al., 2010) and can be quantified by inspection of a histogram of either the pixel significance values in the mosaics, or the significances of the detected excesses. We follow the method of cat4 and fit the pixel distribution (Figure 4) with a Gaussian noise component and a power law component representing the sources. The point at which the noise population contributes 1% of the source population can therefore be estimated at between 4.5 and 5 sigma, and these values have typically been used in prior catalog constructions. In this work, the threshold for 1% FPR is 4.8 sigma, the same as that quoted for cat4, while above the formal 4.5 sigma threshold, a total of 2.6% of the sources may be due to the noise component. We note however, that in the significance range between 4.5 and 4.8 sigma, the fraction of false sources may be as much as 25% and have indicated this in the table with a WARN flag.

Figure 4: Pixel significance distribution for the 18-60 keV all-sky mosaic significance map. The distribution is modelled as a sum of noise (green) and source (red) contributions. The dashed vertical line is at 4.5.

The false positive rate arising from the bursticity method is much harder to quantify. A large number of trials are performed each time a light curve is tested, and the confidence levels for any ’detection’ must therefore be assessed carefully. An analytical approach to this is unlikely to yield a satisfactory result, as the 3000 light curves tested are of markedly different lengths and temporal structures (the data gaps come from the observing strategy of the telescope). Since both length and structure of the light curve affect the number of valid trials performed, they also affect the confidence limits, and we should formally assign limits on each light curve, but this is too cumbersome, and we adopt a simulation approach on the ensemble of light curves.

We created new light curves by randomisation of existing light curves that were selected to have no source signal. For a light curve containing N data points, N swaps of (time, flux/error) pairs were performed to randomise the light curve while retaining the original overall time structure. The advantage of this method is that a very large number of random light curves can be generated. However, the assumption in this method is that the noise in the light curve is purely statistical white-noise, as any correlated noise would be removed by the randomisation.

The distribution of burst significances detected in 10000 randomised light curves derived from a medium length (2650 scw) light curve is shown in Figure 5. For this typical light curve length, 10% of the ’bursticity’ tests resulted in a detection above 4.5 sigma. Corresponding values for short (550 scw) and long (10700 scw) light curves were 0.1% and 10% respectively. In all these tests, less than 1% of iterations generated a detection above 6 sigma.

Figure 5: Maximum burst significances discovered in 10000 randomly generated light curves containing 2650 science windows with a realistic time structure and noise distribution.

We performed a second set of simulations based on inversion of the 3000 excess light curves. Each source flux light curve was subjected to a sigma clipping algorithm to remove bright positive detections above the 5 level, and then inverted about zero flux. In the assumption that the noise flux distribution from coded mask deconvolution is Gaussian distributed around a mean of zero, this results in light curves with the same noise and time structure as the original light curves. These light curves will retain any systematic noise and also will maintain any longer-term noise structures (red noise) present in the originals, but should effectively contain no signal flux. Analysis of these light curves should represent a worst case scenario in terms of the derived false positive rate when compared to the purely statistical, white noise light curves made in the first approach. Using this approach, a ‘burst’ of greater than 4.5 sigma is seen in 12.7% of the light curve analyses, and a ‘burst’ of greater than 6 sigma is seen in 3.5% of the light curve analyses; this falls to 2% at the 7 sigma level.

Combining the results of these two simulation approaches, we can estimate that the mean false alarm rate above a 6 sigma threshold is between 1% (statistical best case) and 3.5% (systematic worst case) for a single light curve. Once we impose the additional requirement that the bursts are temporally aligned in more than one energy band, the statistical probability falls enormously due to the small burst duration compared to the overall light curve length. In a purely statistical sense, the probability falls to 1% even above 4.5 as typical burst durations are 1% of the light curve duration. However, we must caution that some of the systematic effects occasionally seen (e.g. poor ghost source removal) will potentially generate noise simultaneously across all bands, so the final inspection processes are still vital to remove ’ghosts’ and areas of noise in maps. We pessimistically assume a final 1% false positive rate in the overall bursticity method when requiring simultaneous bursts in more than one band. Based on these simulations and our experience from cat4, we believe the false positive probability for sources detected on short timescales (70 days) and at low significance is higher than the overall levels, and we have again indicated this in the table with a WARN flag. See Section 4 and Figure 7 for further information.

Overall, we estimate the false positive rate in this catalog is 25% for sources detected between 4.5 and 4.8 sigma in persistent maps, 1% for sources detected above 4.8 sigma in persistent maps, and (pessimistically) 1% for sources detected via the bursticity method. Thus we anticipate 30 false positives in a catalog of 939 sources, i.e. 3.5%, with a roughly equal number coming from each detection method.

2.5 Galactic Center Localizations

Figure 6: IBIS/ISGRI mosaic significance map of the Galactic Centre region and resulting sources from the analysis. The white box represents the central region.

The central region of the Galaxy represents a challenging area for the INTEGRAL/IBIS map analysis. The presence of unresolved sources (and presumably many sources below the formal detection threshold creating a non-uniform background) means that the maps in this area are dominated by systematic effects and the usual statistical limits for source discovery do not apply. As a consequence, we have been extremely conservative in this region, and in fact all the sources listed are already present in the INTEGRAL Reference Catalog. Because of the complex and unresolved source distribution, the data quality for these sources may be lower than for isolated sources away from the Galactic Centre. In the source list, we indicate this with a flag (GCFLAG) with the following two values: GCFLAG=1 means that the source lies within the GC box, and is detected by our standard methods. Furthermore, the source is sufficiently resolved that we can estimate the flux and position from our maps; nevertheless we expect that the detection may be affected by nearby unresolved faint sources and the quantitative data should be treated with caution; GCFLAG=2 means that there is clear evidence of emission from the source position in one or more of our maps, but it lies within an unresolved emission region. Therefore we cannot unambiguously attribute the emission to the source, and we therefore supply the reference catalog position only. The fluxes are almost certainly contaminated by emission from nearby unresolved sources, or indeed resolved ones - in one case, two nearby sources (SAX J1750.82900 and IGR J175072856) are blended in stacked images of the region, but may be temporally identified as they outburst at different times, and the derived positions are unambiguously different. Nevertheless, cross-contamination of fluxes in this region is an ever-present problem. Using this approach, there are 23 sources falling within the Galactic Centre zone, of which 11 have GCFLAG=2.

We have cross-checked our results and sources in this area with the results from the bulge monitoring project12 which provides a more regular monitoring and so regularly detects transient sources; nevertheless, we have no real contradictions with their database. The differences that do exist, apart from occasional naming differences, are in fact due either to sources detected after revolution 1000 or to our detection acceptance threshold.

3 The Table Data

The name of the source is given following the convention to quote wherever possible the name declared at the time of the first X-ray detection. The names are given in bold for the 300 sources added to the catalog since cat4.

The astrometric coordinates of the source positions were extracted from the mosaics by the barycentring routines built into SExtractor 2.5. In almost all cases, the position for a source was extracted from the map yielding the highest source significance. In a few cases, primarily for blended sources, other maps were chosen in order to minimise the interference of other sources. Simultaneous fitting of multiple Gaussian PSFs was used in the most difficult cases - these sources are indicated as blended in the notes accompanying the table. The point source location error of IBIS is highly dependent upon the significance of the source detected (Gros et al., 2003; Scaringi et al., 2010b). We use the formulation of Gros et al. (2003), combined with the significance of the detection used to locate the source, in order to define an error on the source position. The source localisation errors quoted are for the 90% confidence limit.

The mean fluxes quoted in the table as and are the time-averaged fluxes over the whole dataset derived in two energy bands (20–40 and 40–100 keV). These are provided for compatibility with past catalogs and as a general reference value. However, as previously noted, their relevance as an average measure diminishes as the dataset increases and the average time of activity for many of the sources is much shorter than the on-source exposure. For variable sources, we provide a variability indicator: a flag of Y indicates a bursticity (ie a 10% increase in significance can be obtained by selecting a single contiguous subset of the data) and a slightly variable source. A flag of YY indicates a bursticity of (ie a 400% increase in significance) indicating a strongly variable source. The significances quoted are the highest significance in any single map, since this gives the best indication of the robustness of source detection. However, it should be noted that the flux and significance values may derive from different energy bands and/or subsets of the data, and may initially appear contradictory. A brief commentary indicates the detection method for each source - here the term ‘persistent’ means that the source detection is optimised in a mosaic of all data, but the detection may actually derive from a number of outbursts or flares, but no single outburst optimises the detection. For sources detected during an outburst, the MJD and duration are indicated. Warning flags are appended to some sources to indicate their position in the Galactic Center, or to warn of detections subject to higher false positive rates due to lower significance or shorter duration (see section 2.4).

The type of the source is encoded into up to four flags, which are explained in the table footnotes. We have followed the convention of (Liu et al., 2007) wherever possible. The exposure quoted is the total effective exposure on the source after all filtering of the data has been carried out.

4 Detailed comparison with 4th IBIS/ISGRI catalog

632 of the 723 sources detected in the 4th IBIS/ISGRI catalog are listed in this new catalog, while 4 are not included because of the new methods employed to analyse the Galactic Centre, and 87 are not included because they did not pass the new acceptance thresholds.

The sources that were given in cat4, but are not detected by the cat1000 analysis have been subjected to further inspection. While we would always expect some false positives in any catalog, the number of ÔmissingÕ cat4 sources is far in excess of the expected level quoted in cat4. In total, 87 cat4 sources are not confirmed in cat1000, and breaking this subset of sources down by detection type, there is a clear trend towards these (assumed) false positives coming from the shorter outburst detections (Figure 7, left).

Figure 7: Analysis of the false positive rates for the transient detection performed in cat4. A cat4 source is rejected as potentially a false positive if it cannot be recovered by the improved and more stringent acceptance criteria used in this work. (left) the fraction of sources rejected as a function of the source detection duration shows a clear trend towards more false positives for shorter outbursts, error bars indicate statistical uncertainties due to source numbers. (right) adding the source significance as a second parameter shows that short, low-significance outbursts contribute a very high fraction of the rejected sources.

Further analysis of the 87 rejected sources shows that only 25 sources come from the stacked whole dataset maps, that are optimised for persistent source detection. Even then, many of these ÔpersistentÕ sources derive from low exposure (less than 200 ks) areas of the maps so may be thought of as short exposure detections. Another 14 rejected sources derive from burst maps, which may be of any exposure but tend towards shorter timescales, 31 from revolution (so ks exposure) maps, and 17 from short sequences of revolutions. The other very clear (and expected trend) is towards low significance detections; only 12 of the missing cat4 sources were originally attributed a significance greater than 6 sigma. These trends are illustrated in Figure 7 (right) that shows the fraction of sources rejected between cat4 and cat1000 as a function of both duration and significance. We would expect a rejection rate of 1% based on the expected noise content of the persistent maps, but the rejection rates for sources that were detected on short timescales (70 days) and at relatively low significance () were much higher than that; in the worst case for the short outbursts below 5, only 1 in 2 sources have been confirmed by the new analysis. Outside of the region bounded by duration 70 days and significance the rejection fraction falls to the expected levels. These results are consistent with, and may be explained in the context of, the simulations described in Section 2.4.

For the sources that are identified in shorter periods (bursts, revolutions, sequences) we have cross-checked the outbursts detected in cat1000 against those found in cat4. In many cases there is no time correlation, and we must conclude that these cat4 excesses were probably random bright periods in the light curve of a random point of sky, and should be considered false detections. We note here that the methods employed in cat1000 are much more robust, as all five main energy bands are searched for outbursts, and we expect time correlation between the bursts in at least two of the bands. Furthermore we have operated with a much higher significance threshold for short outburst detection. However, these improved methods used in this work still only partially protect against the other likely explanation of false short bursts in cat4. Specifically, a short sequence of science windows where the data is hard to analyse due to noise, blended sources or an incomplete catalog may give rise to strong image artefacts, and we have to assume the same conditions may persist from cat4 to cat1000. Therefore detection of a burst at the same time in cat4 and cat1000, although strongly indicative, on its own is not considered 100% confirmation of source detection.

We must assume that those few rejected sources that were originally detected in persistent maps (i.e. by compiling all observations) and with long exposures were spurious detections of artefacts induced by the previous imaging software version, and now better suppressed in OSA 9.0. Numerous changes were implemented in the software, instrument response models and reference catalogs between OSA 7.0 and OSA 9.0. The use of a newer, improved base ‘cleaning’ catalog will certainly have played a part in reducing the image noise levels. Long-term source variability should not cause a previously known source to be rejected. Since these previously detected sources are automatically included in our analysis, they should be detected despite a declining flux - we are confident that the bursticity analysis successfully identifies them as active during the earlier mission phases.

Following removal of those sources not confirmed in this work, we can re-analyse the source type distribution for the confirmed cat4 sources. The modified source type distribution (Figure 8(left) and Table 1) shows the success of the various follow-up campaigns, in that only 16% of the confirmed cat4 sources now lack association with a specific type of object. Conversely, follow-ups on the 87 ÔmissingÕ cat4 sources have largely failed to identify clear counterparts, with only 3 likely and 10 possible AGNs associations being reported. Some random correlation with sources is to be expected, and in the extragalactic sky this is most likely to produce correlations with the isotropic source populations (mostly AGNs and CVs). Nevertheless, this low rate of association with known objects gives us further confidence that we have successfully identified a subset of likely false positive excesses.

5 Results

This new catalog lists 939 sources detected with a systematic analysis of all public observations collected up to the end of 2010 and consisting of eight years of INTEGRAL data. Of these sources, 881 have a significance above 5 level and can be considered more secure detections, while the rest have a lower significance in the range 4.5 to 5 .

307 sources in this catalog are new entries with respect to cat4 (these are shown in bold font in the source list); some of them have been previously declared as INTEGRAL detections, or have already been included in the INTEGRAL reference catalog (Ebisawa et al., 2003). In particular, 60 sources have previously been discovered and reported in the literature with IGR designations. A further set of 127 are already listed either in other hard X-ray catalogues, mainly that of Swift/BAT, or previously reported elsewhere. Therefore the remaining 120 sources are reported as soft gamma-ray emitters for the first time in this work.

Figure 8: Source type distributions for (left) confirmed cat4 sources; (center) new cat1000 sources added since cat4; (right) cat 1000 overall

Table 1 shows the source distribution by class in this new catalog - as in previous catalogs the same main source classes are detected (HMXB, LMXB, CV and AGN), including a large fraction of unassociated sources (23%). The same data are presented graphically in Figure 8 (center and right)

Type cat4 cat1000 new cat1000 overall
Src % Src % Src %
AGN 250 40% 119 39% 369 39%
? 100 16% 119 39% 219 23%
LMXB 106 17% 23 7.5% 129 14%
HMXB 96 15% 20 6.5% 116 12%
CV 42 7% 14 5% 56 6%
SNR 10 2% 0 1% 10 1%
XB 6 1% 3 1% 9 1%
PSR 5 1% 3 1% 8 1%
Cluster 4 1% 3 1% 7 1%
PWN 5 1% 0 1% 5 1%
SGR 2 1% 1 1% 3 1%
AXP 2 1% 0 1% 2 1%
GRB 1 1% 1 1% 2 1%
RSCVn 1 1% 1 1% 2 1%
Mol cloud 1 1% 0 1% 1 1%
XP 1 1% 0 1% 1 1%
Total 632 307 939
Table 1: Source type numbers for (left) confirmed cat4 sources; (center) new cat1000 sources added since cat4; (right) cat 1000 overall

Compared to cat4 (Figure 8 (left)), there seems to be a slight change in the type fractions, i.e. overall the fraction of Galactic sources continues to reduce following the trend seen in previous catalogs. However, if we consider only the new entries (see Figure 8 centre panel), it is evident that there is a large fraction of sources (39%) that still need to be identified and among them a significant number could eventually be of a Galactic nature.

This opens the path to a large program of follow-up work/observations as has been successfully performed in the past. The follow-up program started ten years ago with the release of the first IBIS catalog (Bird et al. 2004) and continued thereafter. Typically, the presence of a soft X-ray source in the IBIS error box has been used to reduce the soft gamma-ray positional uncertainty and hence enable optical and NIR follow-up observations. This process has been performed either by cross-checking with a number of available X-ray catalogs (e.g. with ROSAT see Stephen et al. (2005, 2006)), using IBIS itself (50%), or using additional observations with other missions such as Swift (27%), Chandra (17%), XMM (5%).

As recently reviewed by Masetti et al. (2013), teams have so far pinpointed the nature of about 240 sources which represents a large fraction of the unidentified objects listed in all previous IBIS surveys. The majority of these sources are AGN (61%) followed by X-ray binaries (25%) and Cataclysmic Variables (CVs, 12%). Most of the AGN are local Seyfert galaxies of type 1 and 2 while the largest fraction of Galactic binaries have a high mass companion.

Overall this follow-up program has highlighted the key role played by INTEGRAL in discovering new classes of high mass X-ray binaries (absorbed objects and supergiant fast X-ray transients), in detecting AGNs in the Zone of Avoidance i.e. the area of the sky that is obscured by the Milky Way (Kraan-Kortoweg et al, 2000) and at high redshifts, as well as in confirming a population of magnetic CVs emitting above 20 keV. Follow-up work on unassociated sources in this new catalog has already started and hopefully will lead to further identifications.

6 Comparison with other recent soft gamma-ray catalogs

In this section we make a brief comparison between this catalog and two other soft gamma-ray surveys.

The first is that of Krivonos et al. (2012), which includes a very similar dataset (up to revolution 1013) but only considers sources in the Galactic Plane. In addition Krivonos et al. (2012) used different software methods and slightly different energy bands within their data analysis to achieve a claimed identification completeness of 0.91. As well as allowing them to perform population studies on a good statistical basis (see Lutovinov et al., 2013), this level of completeness provides a good comparison for this work. Krivonos et al. (2012) identified 392 sources above a 5 detection threshold, and this number increases to 402 if the detection threshold is lowered to 4.8. Comparison with our catalog indicates that only 15 of their sources are not present in our list, and of those, 12 have a detection significance below 5 in at least one of the three energy bands used in the Krivonos catalog. The degree of agreement is thus 99%, consistent with the statistical uncertainties associated with the two methods.

Figure 9: (upper) Distribution of sources detected by INTEGRAL/IBIS (red) and Swift/BAT (blue) as a function of Galactic longitude. (upper panel) sky region within 10 of the Galactic Plane; (lower panel) sky more than 10 from the Plane.

Secondly, we have also cross-correlated our source list with that of the 70 month Swift/BAT survey (Baumgartner et al., 2013). This catalog reports 1171 hard X-ray sources detected above a significance threshold of 4.8 in the 14–195 keV energy band. So far this is the most sensitive and uniform survey in the soft gamma-ray band, reaching a limiting flux sensitivity of erg/s/cm over 90% of the sky. Due to the satellite observing strategy, the Swift/BAT all-sky survey is very uniform which explains why most of the reported sources (about 60%) are of extragalactic nature. Comparing the catalog of this work with that of Baumgartner et al. (2013) results in 565 correlations within a distance of 400. Of these 311 are of extragalactic nature, 246 are Galactic sources and the rest lack a precise association. Figure 9 shows the number of sources detected by BAT and IBIS as a function of Galactic longitude, either within 10 of the Galactic Plane (upper panel), or more than 10 from the Plane (lower panel). The differences between these two surveys is immediately apparent. It is clear that INTEGRAL has been more effective at finding soft gamma-ray emitting sources along the Galactic Plane, and particularly along the directions of the spiral arms. Swift/BAT, as a result of its larger FOV and more uniform all-sky exposure, is more effective on the extragalactic sky. Thus Figure 9 emphasizes the great complementarity between these two missions, and the source catalogs they produce.

6.1 Concluding comments

As predicted in the 4th IBIS catalog, with the further data available from AO6 and AO7, this latest catalog shows a large increase in the populations in the sky beyond the Galactic Plane - seen in both the AGNs class (more than 100 new sources) and CVs. As with all previous catalogs exploiting new datasets, there is a large fraction (23%) of unidentified sources that will require further study, and a robust follow-up programme is essential for the weak persistent examples. Transient detections represent a greater challenge for follow-up due to the serendipitous nature of their discovery. A characterisation of the transients based on their outburst duration, timing and spectral properties, and quiescent emission will be needed to further identify their nature(s).

Once again, the soft gamma-ray sky has shown itself to be both well populated and highly variable, as the advent of missions with survey capabilities like INTEGRAL and Swift have demonstrated over the last ten years, and continue to demonstrate. Both INTEGRAL and Swift continue their highly complementary monitoring programmes, and continue to discover new sources. Studies using long term light curves and spectral evolution are now possible and can be performed well beyond 100 keV. With the information reported in the current work and in combination with the recent results from the 11-years survey above 100 keV (Krivonos et al., 2015) one can already derive a hardness ratio in the energy bands 20–100/100–150 keV and may understand the general properties of the 108 common sources. We believe this will prove an invaluable data set to study the high energy behaviour of different classes of sources. By comparing these catalogue data with observations performed at lower (X-ray band) and higher (MeV and GeV bands) energies, it will be possible to create broadband spectra and therefore a unique and comprehensive view of many of the objects in our sky.

We acknowledge the founding from Italian Space agency financial and programmatic support via ASI/INAF agreement n.2013-025-R.0. ABH acknowledges support from a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme (FP7/2007Ð2013) under grant agreement no. 275861. This research has made use of: data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC) provided by NASA Goddard Space Flight Center; the SIMBAD database operated at CDS, Strasburg, France; the NASA /IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology , under contract with NASA.
Name13 RA Dec Error14 F20-4015 F40-10016 Type17 Vari18 Signif19 Exposure20
IGR J00040+7020 1.006 70.321 2.84 0.80.1 1.00.2 AGN, Sy2 9.2 3391
Detected as a persistent source in the 20-100 keV band.
IGR J00234+6141 5.74 61.685 2.66 0.70.1 0.30.1 CV, IP 9.9 4777
Detected as a persistent source in the 17-30 keV band.
GRB041219A 6.117 62.843 1.44 0.1 0.30.1 GRB YY 20.1 4812
     IGR J00245+6251 Detected in a 0.6 day outburst from MJD=53358.0.
4U 0022+63 6.321 64.159 2.21 0.70.1 0.80.1 SNR 12.2 4718
Detected as a persistent source in the 18-60 keV band.
IGR J00256+6821 6.374 68.357 2.44 0.70.1 1.10.1 AGN, Sy2 10.9 4072
Detected as a persistent source in the 20-100 keV band.
V709 Cas 7.204 59.289 0.61 4.40.1 2.70.1 CV, IP 60.1 4517
     RX J0028.8+5917 Detected as a persistent source in the 18-60 keV band.
IGR J00291+5934 7.263 59.572 0.41 2.00.1 2.40.1 LMXB, XP, T Y 109.7 4537
Detected in a 12.3 day outburst from MJD=53337.5.
IGR J00333+6122 8.326 61.462 2.55 0.70.1 0.90.1 AGN, Sy1.5 10.4 4697
Detected as a persistent source in the 20-100 keV band.
SWIFT J0034.5-7904 8.579 -79.11 5.14 0.70.2 0.6 AGN, Sy1 4.8 1153
     1RXS J003422.2-790525 Detected as a persistent source in the 17-30 keV band.
1ES 0033+595 8.969 59.835 1.50 1.40.1 0.90.1 AGN, BL Lac 19.1 4520
Detected as a persistent source in the 17-30 keV band.
IGR J00370+6122 9.29 61.36 1.97 0.70.1 0.90.1 HMXB, XP, Sg Y 13.9 4666
Detected in a 2.4 day outburst from MJD=53000.4.
1RXS J004504.8+620803 11.248 62.083 3.64 0.50.1 0.30.1 AGN? 7.0 4558
Detected as a persistent source in the 20-40 keV band.
IGR J00465-4005 11.586 -40.096 5.24 0.7 1.90.7 AGN, Sy2 4.7 212
Detected as a persistent source in the 20-100 keV band.
IGR J00486-4241 12.151 -42.719 5.42 1.00.4 2.20.7 ? 4.5 214
Detected as a persistent source in the 20-100 keV band.
Mrk 348 12.196 31.957 1.50 6.00.4 6.70.7 AGN, Sy2 19.1 228
Detected as a persistent source in the 18-60 keV band.
IGR J00515-7328 12.996 -73.49 4.39 0.3 0.6 HMXB YY 5.7 1294
Detected in a 6.6 day outburst from MJD=54989.9.
RX J0053.8-7226 13.479 -72.446 3.12 0.50.2 0.90.3 HMXB, XP, Be, T Y 8.3 1290
Detected in a 5.5 day outburst from MJD=52844.0.
SWIFT J0055.4+4612 13.85 46.203 4.06 1.90.3 1.0 CV, IP 6.2 507
     1RXS J005528.0+461143 Detected as a persistent source in the 20-40 keV band.
gam Cas 14.161 60.703 0.63 4.60.1 1.40.1 HMXB, Be 57.5 4228
Detected as a persistent source in the 17-30 keV band.
Mrk 352 14.976 31.843 5.11 1.00.4 2.60.7 AGN, Sy1 4.8 209
     SWIFT J0059.4+3150 Detected as a persistent source in the 18-60 keV band.
IGR J01021+6612 15.534 66.211 4.06 0.40.1 0.50.1 ? 6.2 3962
Detected as a persistent source in the 17-30 keV band.
IGR J01054-7253 16.173 -72.901 1.86 1.50.2 0.80.3 HMXB, XP, Be Y 14.9 1296
Detected in a 19.7 day outburst from MJD=54988.6.
IGR J01085-4550 17.115 -45.848 5.35 0.7 2.00.9 ? Y 4.6 278
Detected in a 246.5 day outburst from MJD=53679.3. Flags: WARN
Mrk 1152 18.562 -14.844 4.86 1.40.5 2.00.9 AGN, Sy1.5 5.1 126
     SWIFT J0113.8-1450 Detected as a persistent source in the 18-60 keV band.
IGR J01157+6941 18.895 69.689 3.74 0.40.1 1.00.2 ? 6.8 3000
Detected as a persistent source in the 20-100 keV band.
SMC X-1 19.271 -73.443 0.41 16.20.2 3.00.3 HMXB, XP 114.2 1304
Detected as a persistent source in the 17-30 keV band.
1A 0114+650 19.511 65.292 0.41 9.70.1 5.60.2 HMXB, XP 112.1 3575
Detected as a persistent source in the 18-60 keV band.
4U 0115+634 19.633 63.74 0.20 27.60.1 8.10.2 HMXB, XP Y 826.6 3629
Detected in a 14.7 day outburst from MJD=53260.4.
RX J0119.5-7301 20.077 -73.059 5.04 0.3 0.6 ? Y 4.9 1300
Detected in a 3.2 day outburst from MJD=52843.8.
Fairall 9 20.917 -58.774 3.49 1.80.3 2.10.5 AGN, Sy1.2 7.3 528
     SWIFT J0123.8-5847 Detected as a persistent source in the 20-100 keV band.
NGC 526A 20.976 -35.065 3.95 2.80.5 3.30.9 AGN, Sy1.9 6.4 141
Detected as a persistent source in the 20-100 keV band.
IGR J01295+5011 22.364 50.183 4.61 0.50.2 0.7 ? Y 5.4 948
Detected in a 1.1 day outburst from MJD=53003.2. Flags: WARN
IGR J01363+6610 23.956 66.212 3.62 0.2 0.4 HMXB, Be, T YY 7.0 2976
Detected in a 25.5 day outburst from MJD=53101.3.
ESO 297-G18 24.655 -40.011 3.46 2.70.4 3.20.7 AGN, Sy2 7.4 242
Detected as a persistent source in the 20-100 keV band.
4U 0142+614 26.593 61.751 1.06 1.70.1 4.40.2 AXP 28.9 2651
Detected as a persistent source in the 20-100 keV band.
RX J0146.9+6121 26.751 61.357 1.91 1.10.1 0.60.2 HMXB, XP, Be, T Y 14.4 2612
     V831 Cas Detected in a 812.9 day outburst from MJD=52636.5.
IGR J01529-3531 28.2 -35.495 4.78 1.80.6 2.0 ? 5.2 136
Detected as a persistent source in the 17-30 keV band.
IGR J01528-0326 28.204 -3.447 2.72 1.20.1 1.40.3 AGN, Sy2 9.7 1474
Detected as a persistent source in the 18-60 keV band.
IGR J01528-0845 28.234 -8.769 5.28 0.50.1 0.5 AGN? 4.7 1431
Detected as a persistent source in the 18-60 keV band.
IGR J01545+6437 28.605 64.62 3.74 0.50.1 0.4 AGN, Sy2 6.8 2491
Detected as a persistent source in the 17-30 keV band.
IGR J01572-7259 29.318 -72.976 3.02 1.00.2 1.00.3 HMXB, XP, Be? Y 8.6 1303
     IGR J015712-7259 Detected in a 676.8 day outburst from MJD=54806.9.
IGR J01583+6713 29.576 67.224 1.99 0.30.1 0.4 HMXB, XP?, Be, T Y 13.8 2315
Detected in a 4.1 day outburst from MJD=53709.3.
Mrk 584 30.099 2.711 4.25 0.50.2 1.50.3 AGN, Sy1.8 5.9 1093
Detected as a persistent source in the 20-100 keV band.
NGC 788 30.277 -6.816 0.99 3.60.1 4.10.2 AGN, Sy2 31.6 1706
Detected as a persistent source in the 18-60 keV band.
Mrk 1018 31.534 -0.284 3.09 1.10.1 1.30.2 AGN, Sy1 8.4 1550
Detected as a persistent source in the 18-60 keV band.
IGR J02086-1742 32.145 -17.659 3.55 1.40.2 0.90.4 AGN, Sy1.2 7.2 768
Detected as a persistent source in the 18-60 keV band.
IGR J02097+5222 32.407 52.445 2.39 1.70.2 1.90.3 AGN, Sy1 11.2 913
Detected as a persistent source in the 18-60 keV band.
Mrk 590 33.625 -0.811 3.88 0.60.1 0.70.2 AGN, Sy1 6.5 1662
Detected as a persistent source in the 18-60 keV band.
SWIFT J0216.3+5128 34.113 51.424 3.79 1.00.2 1.20.4 AGN, Sy2? 6.7 780
Detected as a persistent source in the 18-60 keV band.
SWIFT J0218.0+7348 34.398 73.833 3.15 1.20.2 2.00.4 AGN, QSO, Blazar 8.2 1009
Detected as a persistent source in the 20-100 keV band.
IGR J02242+2356 36.068 23.939 4.25 1.40.5 3.40.9 ? Y 5.9 164
Detected in a 621.3 day outburst from MJD=54834.2.
IGR J02252+3748 36.314 37.802 4.64 1.30.3 0.9 ? 5.4 366
Detected as a persistent source in the 18-60 keV band.
Mrk 1040 37.061 31.311 2.79 2.70.3 2.30.5 AGN, Sy1.5 9.4 354
Detected as a persistent source in the 18-60 keV band.
IGR J02341+0228 38.525 2.464 3.39 0.80.2 1.00.3 AGN, QSO 7.6 1288
     QSO B0231+022 Detected as a persistent source in the 30-60 keV band.
IGR J02343+3229 38.583 32.506 2.74 2.10.3 2.40.4 AGN, Sy2, Liner 9.6 492
Detected as a persistent source in the 18-60 keV band.
NGC 985 38.657 -8.788 2.18 1.20.1 1.90.2 AGN, Sy1.5 12.4 1412
Detected as a persistent source in the 18-60 keV band.
LS I+61 303 40.132 61.229 2.08 1.60.1 2.30.3 HMXB, M 13.1 1476
     GT 0236+610 Detected as a persistent source in the 18-60 keV band.
NGC 1052 40.27 -8.256 2.87 1.10.1 1.40.3 AGN, Sy2, Liner 9.1 1380
Detected as a persistent source in the 18-60 keV band.
RBS 345 40.567 5.53 4.78 0.80.2 1.30.4 AGN, Sy1 5.2 828
Detected as a persistent source in the 18-60 keV band.
NGC 1068 40.67 -0.013 2.43 1.60.2 1.40.3 AGN, Sy2 11.0 1263
Detected as a persistent source in the 18-60 keV band.
IGR J02447+7046 41.178 70.775 4.78 0.4 0.7 AGN YY 5.2 1128
Detected in a 3.4 day outburst from MJD=52955.7.
QSO B0241+62 41.233 62.463 1.25 2.90.2 3.90.3 AGN, Sy1.2 23.7 1422
Detected as a persistent source in the 18-60 keV band.
SWIFT J0249.1+2627 42.259 26.509 3.79 0.90.3 1.30.4 AGN, Sy2 Y 6.7 571
Detected in a 1579.3 day outburst from MJD=53821.7.
IGR J02504+5443 42.674 54.704 3.34 1.10.2 1.50.3 AGN, Sy2 7.7 1032
Detected as a persistent source in the 20-100 keV band.
MCG-02-08-014 43.097 -8.511 4.54 0.80.2 0.60.3 AGN, Sy2? 5.5 1074
Detected as a persistent source in the 18-60 keV band.
NGC 1142 43.801 -0.184 1.42 3.30.2 4.00.3 AGN, Sy2 20.4 815
Detected as a persistent source in the 18-60 keV band.
XY Ari 44.017 19.44 3.73 2.10.3 1.40.6 CV, IP 6.8 416
     H 0253+193 Detected as a persistent source in the 18-60 keV band.
IGR J02564-5232 44.126 -52.533 4.78 1.70.3 1.60.6 ? 5.2 334
Detected as a persistent source in the 20-100 keV band.
MCG -02-08-038 44.937 -10.77 4.86 0.90.2 1.20.4 AGN, Sy1 5.1 778
     SWIFT J0300.0-1048 Detected as a persistent source in the 20-100 keV band.
NGC 1194 45.942 -1.147 4.18 1.00.2 1.70.4 AGN, Sy2 6.0 581
Detected as a persistent source in the 20-100 keV band.
XMMSL1 J030715.5-545536 46.73 -54.908 5.04 1.20.4 1.4 ? 4.9 255
Detected as a persistent source in the 18-60 keV band.
PKS 0312-770 47.843 -76.819 4.95 0.60.2 0.80.3 AGN, Sy1/QSO 5.0 1373
     SWIFT J0311.8-7653 Detected as a persistent source in the 18-60 keV band.
B3 0309+411B 48.258 41.334 4.46 0.50.2 0.6 AGN, Sy1 Y 5.6 952
Detected in a 1.1 day outburst from MJD=53218.7.
SWIFT J0318.7+6828 49.76 68.43 4.61 1.00.2 0.8 AGN, Sy1.9 Y 5.4 841
Detected in a 1404.5 day outburst from MJD=52636.5.
NGC 1275 49.951 41.512 1.28 3.10.2 1.40.3 AGN, Sy1.5, Liner 23.1 1034
Detected as a persistent source in the 18-60 keV band.
IGR J03199+7402 49.964 74.043 4.86 1.30.3 1.70.6 ? 5.1 479
Detected as a persistent source in the 20-100 keV band.
1H 0323+342 51.172 34.179 3.59 0.90.1 0.90.3 AGN, NLS1 7.1 1410
Detected as a persistent source in the 20-100 keV band.
IGR J03248-0223 51.233 -2.403 4.86 2.90.6 2.1 ? 5.1 114
Detected as a persistent source in the 17-30 keV band.
GK Per 52.799 43.905 1.93 2.20.2 0.90.3 CV, IP 14.3 1084
Detected as a persistent source in the 20-40 keV band.
IGR J03334+3718 53.328 37.303 2.96 1.20.1 1.10.2 AGN, Sy1.5 8.8 1466
Detected as a persistent source in the 18-60 keV band.
NGC 1365 53.402 -36.138 4.44 2.60.5 2.0 AGN, Sy1.9 5.6 117
Detected as a persistent source in the 18-60 keV band.
EXO 0331+530 53.75 53.173 0.18 147.90.2 24.90.3 HMXB, XP, Be, T Y 1794.1 1004
Detected in a 50.1 day outburst from MJD=53364.9.
NRAO 140 54.112 32.308 2.25 1.50.1 1.40.3 AGN, QSO, Blazar 12.0 1493
Detected as a persistent source in the 18-60 keV band.
ESO 548-G081 55.478 -21.258 4.13 1.70.5 4.71.0 AGN, Sy1 Y 6.1 101
Detected in a 1.3 day outburst from MJD=53931.3.
IGR J03532-6829 58.239 -68.522 3.30 0.80.1 1.00.2 AGN, BL Lac Y 7.8 1764
Detected in a 2424.9 day outburst from MJD=52641.4.
SWIFT J0353.7+3711 58.34 37.136 5.01 0.30.1 0.70.2 AGN, Liner Y 4.9 1654
Detected in a 0.6 day outburst from MJD=54494.0.
X Per 58.846 31.046 0.29 28.50.2 34.00.3 HMXB, XP, Be 227.6 1442
     4U 0352+309 Detected as a persistent source in the 18-60 keV band.
4C +62.08 59.099 62.714 4.95 0.6 0.9 AGN, Sy1, QSO Y 5.0 532
     IGR J03564+6242 Detected in a 947.5 day outburst from MJD=53394.6.
SWIFT J0357.6+4153 59.461 41.9 3.73 0.80.1 1.00.3 AGN 6.8 1598
Detected as a persistent source in the 20-100 keV band.
3C 098 59.686 10.42 4.01 1.60.3 2.60.6 AGN, Sy2 6.3 265
Detected as a persistent source in the 20-100 keV band.
IGR J03599+5043 59.973 50.728 4.01 0.70.2 1.20.3 ? Y 6.3 1331
Detected in a 2303.8 day outburst from MJD=52816.5.
IGR J04069+5042 61.73 50.702 4.25 0.3 0.6 ? Y 5.9 1389
Detected in a 535.8 day outburst from MJD=52888.9.
4C 03.8 61.856 3.702 3.55 1.50.3 2.50.5 AGN, Sy2 7.2 317
Detected as a persistent source in the 20-100 keV band.
3C 111 64.589 38.027 0.93 4.20.2 5.40.3 AGN, Sy1 34.2 1606
Detected as a persistent source in the 18-60 keV band.
IGR J04221+4856 65.53 48.95 4.46 0.70.2 0.5 AGN, Sy1 5.6 1569
Detected as a persistent source in the 18-60 keV band.
LEDA 15023 65.951 4.145 3.47 1.30.2 1.10.4 AGN, Sy2 7.4 667
Detected as a persistent source in the 18-60 keV band.
3C 120 68.296 5.354 1.20 3.80.2 4.30.3 AGN, Sy1.5 25.0 927
Detected as a persistent source in the 18-60 keV band.
RX J0440.9+4431 70.247 44.53 0.55 3.40.1 2.70.3 HMXB, Be Y 70.5 1639
Detected in a 3.2 day outburst from MJD=55442.2.
UGC 3142 70.945 28.972 2.01 1.80.3 2.30.4 AGN, Sy1 13.6 705
Detected as a persistent source in the 20-100 keV band.
SWIFT J0444.1+2813 71.04 28.172 3.50 0.60.2 1.10.3 AGN, Sy2 Y 7.3 734
Detected in a 1611.8 day outburst from MJD=52919.0.
SWIFT J0451.5-6949 72.778 -69.801 2.08 0.80.1 0.4 HMXB, XP Y 13.1 2250
     SWIFT J045106.8-694803 Detected in a 1403.3 day outburst from MJD=54185.0.
SWIFT J0450.7-5813 72.843 -58.163 4.46 0.70.2 1.40.3 AGN, Sy1.5 5.6 1030
Detected as a persistent source in the 20-100 keV band.
MCG -01-13-025 72.897 -3.697 4.19 0.70.2 1.00.3 AGN, Sy1.2 6.0 1228
     SWIFT J0451.4-0346 Detected as a persistent source in the 18-60 keV band.
LEDA 168563 73.02 49.546 1.96 1.70.2 1.90.3 AGN, Sy1 14.0 1499
Detected as a persistent source in the 18-60 keV band.
SWIFT J0453.4+0404 73.379 4.034 2.64 1.20.1 0.70.3 AGN, Sy2 10.0 1509
Detected as a persistent source in the 18-60 keV band.
IGR J04539+4502 73.46 45.038 4.69 0.60.1 0.50.3 ? 5.3 1584
Detected as a persistent source in the 18-60 keV band.
ESO 33-G02 73.998 -75.541 1.60 1.90.1 1.80.2 AGN, Sy2 17.7 1919
Detected as a persistent source in the 18-60 keV band.
IGR J04571+4527 74.281 45.464 3.30 1.00.1 0.5 CV, IP?, DM 7.8 1566
Detected as a persistent source in the 17-30 keV band.
IGR J05007-7047 75.192 -70.743 2.64 0.80.1 0.80.2 HMXB, Be, T Y 10.0 2286
Detected in a 52.7 day outburst from MJD=55378.3.
SGR 0501+4516 75.278 45.276 4.32 0.3 0.5 SGR, T Y 5.8 1521
Detected in a 9.7 day outburst from MJD=54697.2.
LEDA 075258 75.541 3.518 3.79 0.60.1 0.90.2 AGN, Sy1 6.7 1675
Detected as a persistent source in the 18-60 keV band.
V1062 Tau 75.615 24.756 2.02 1.60.2 1.10.3 CV, IP 13.5 1045
Detected as a persistent source in the 20-100 keV band.
SWIFT J0505.8-2351 76.44 -23.854 2.28 2.90.3 3.50.5 AGN, Sy2 11.8 400
Detected as a persistent source in the 18-60 keV band.
IGR J05081+1722 77.036 17.345 3.55 0.90.2 0.60.2 AGN, Sy2 Y 7.2 1275
     SWIFT J0508.1+1727 Detected in a 1119.3 day outburst from MJD=52733.2.
4U 0517+17 77.69 16.499 1.05 3.40.2 3.40.2 AGN, Sy1.5 29.4 1270
Detected as a persistent source in the 18-60 keV band.
4U 0513-40 78.527 -40.044 2.82 2.80.3 1.90.6 LMXB, B, G 9.3 290
Detected as a persistent source in the 18-60 keV band.
SWIFT J0515.3+1854 78.845 18.95 2.82 0.90.2 1.20.2 AGN, Sy2 Y 9.3 1357
Detected in a 932.8 day outburst from MJD=54402.8.
IGR J05157+1238 78.908 12.673 4.04 0.3 0.5 ? YY 6.2 1327
Detected in a 1.6 day outburst from MJD=55258.7.
Ark 120 79.048 -0.15 1.14 2.90.1 3.10.2 AGN, Sy1 26.6 1862
Detected as a persistent source in the 18-60 keV band.
SWIFT J0516.3+1928 79.094 19.483 3.23 0.90.2 0.90.2 AGN, Sy2 8.0 1254
Detected as a persistent source in the 20-100 keV band.
SWIFT J0519.5-3140 79.899 -32.657 2.12 2.40.2 3.00.4 AGN, Sy1.5 12.8 576
Detected as a persistent source in the 18-60 keV band.
PICTOR A 79.957 -45.779 4.25 2.70.5 1.7 AGN, Sy1, Liner 5.9 144
Detected as a persistent source in the 20-40 keV band.
LMC X-2 80.155 -71.982 3.23 0.50.1 0.50.2 LMXB, Z 8.0 2284
Detected as a persistent source in the 17-30 keV band.
PKS 0521-36 80.71 -36.468 4.86 0.70.2 1.60.5 AGN, Sy1 5.1 481
Detected as a persistent source in the 18-60 keV band.
RX J0525.3+2413 81.344 24.226 2.99 1.60.2 0.4 CV, IP 8.7 1333
Detected as a persistent source in the 20-40 keV band.
IGR J05288-6840 82.289 -68.718 4.78 0.40.1 0.4 ? Y 5.2 2363
Detected in a 157.4 day outburst from MJD=55333.3.
3A 0527-329 82.35 -32.811 1.58 3.70.2 1.60.4 CV, IP 18.0 606
     TV Col Detected as a persistent source in the 17-30 keV band.
IGR J05305-6559 82.637 -65.984 2.69 2.00.1 1.20.2 HMXB 9.8 2292
Detected as a persistent source in the 18-60 keV band.
PKS 0528+134 82.735 13.532 3.09 0.80.2 0.70.2 AGN, QSO, Blazar Y 8.4 1383
Detected in a 2333.9 day outburst from MJD=52910.6.
EXO 053109-6609.2 82.805 -66.118 1.35 2.00.1 1.20.2 HMXB, Be, T Y 21.7 2292
Detected in a 63.2 day outburst from MJD=55356.2.
LMC X-4 83.207 -66.37 0.29 23.60.1 7.40.2 HMXB, XP 223.5 2306
Detected as a persistent source in the 20-40 keV band.
Crab 83.633 22.014 0.16 1000.50.1 1000.10.2 PWN, PSR 10011.7 2398
     4U 0531+21 Detected as a persistent source in the 18-60 keV band.
IGR J05346-5759 83.71 -58.028 4.13 1.10.2 0.6 CV, Nova-like 6.1 1103
     TW Pic Detected as a persistent source in the 17-30 keV band.
1A 0535+262 84.727 26.316 0.18 63.20.1 35.50.2 HMXB, XP, Be, T Y 1316.7 1469
Detected in a 5.7 day outburst from MJD=55289.5.
LMC X-1 84.911 -69.743 1.00 2.40.1 1.60.2 HMXB, BH Y 31.4 2353
Detected in a 75.9 day outburst from MJD=52641.4.
QSO J0539-2839 84.967 -28.611 3.84 0.80.2 1.50.4 AGN, QSO, Blazar 6.6 646
Detected as a persistent source in the 20-100 keV band.
PSR B0540-69.3 85.032 -69.335 1.31 1.90.1 1.80.2 PWN, PSR 22.4 2380
Detected as a persistent source in the 18-60 keV band.
IGR J05414-6858 85.361 -69.024 2.55 0.2 0.4 HMXB, Be, T Y 10.4 2344
Detected in a 52.7 day outburst from MJD=55333.5.
BY Cam 85.704 60.859 4.01 1.70.3 1.50.5 CV, P 6.3 461
     4U 0541+60 Detected as a persistent source in the 18-60 keV band.
SWIFT J0544.4+5909 86.086 59.141 4.69 1.40.3 1.0 AGN, Sy2 5.3 520
Detected as a persistent source in the 20-40 keV band.
IGR J05470+5034 86.812 50.64 4.54 0.70.2 0.7 AGN, Sy2 Y 5.5 919
     SWIFT J0547.3+5042 Detected in a 59.6 day outburst from MJD=55062.0.
IGR J05511-1218 87.776 -12.322 4.86 1.20.2 0.9 ? 5.1 675
Detected as a persistent source in the 18-60 keV band.
NGC 2110 88.047 -7.456 0.58 10.10.2 13.10.3 AGN, Sy2 64.2 1040
Detected as a persistent source in the 18-60 keV band.
IGR J05549+6318 88.683 63.314 4.61 0.6 1.20.5 ? 5.4 478
Detected as a persistent source in the 30-60 keV band.
MCG+08-11-011 88.723 46.439 0.85 7.50.2 8.10.4 AGN, Sy1.5 38.5 752
Detected as a persistent source in the 18-60 keV band.
4U 0557-385 89.508 -38.334 4.54 1.20.3 1.0 AGN, Sy1.2 Y 5.5 423
Detected in a 252.9 day outburst from MJD=53956.7.
SWIFT J0558.0+5352 89.531 53.912 3.18 1.70.3 1.70.4 CV, IP, DQ? 8.1 696
     RX J0558.0+5353 Detected as a persistent source in the 18-60 keV band.
IRAS 05589+2828 90.54 28.471 1.29 2.80.2 2.90.3 AGN, Sy1 22.8 1011
Detected as a persistent source in the 20-100 keV band.
SWIFT J0601.9-8636 91.413 -86.631 3.84 1.30.3 1.30.5 AGN, Sy2 Y 6.6 492
     ESO 005-G004 Detected in a 36.5 day outburst from MJD=52843.8.
IGR J06058-2755 91.45 -27.911 5.38 1.00.2 0.9 AGN, Sy1.5 4.6 534
Detected as a persistent source in the 18-60 keV band.
IGR J06123+3713 93.073 37.236 4.25 1.20.4 1.10.6 ? Y 5.9 337
Detected in a 0.9 day outburst from MJD=54706.1. Flags: WARN
Mrk 3 93.901 71.037 1.13 4.70.2 6.50.4 AGN, Sy2 26.8 649
Detected as a persistent source in the 20-100 keV band.
4U 0614+091 94.28 9.137 0.45 22.20.3 14.80.5 LMXB, B, A 97.2 422
Detected as a persistent source in the 18-60 keV band.
IGR J06212+5443 95.314 54.675 4.86 1.00.3 1.40.5 ? Y 5.1 488
Detected in a 1.6 day outburst from MJD=55064.5. Flags: WARN
IGR J06239-6052 95.94 -60.979 2.75 1.10.2 1.20.3 AGN, Sy2 9.6 1347
Detected as a persistent source in the 18-60 keV band.
SWIFT J0623.8-3215 95.979 -32.185 5.04 1.20.3 1.1 AGN, Sy2 4.9 339
Detected as a persistent source in the 20-40 keV band.
IGR J06253+7334 96.342 73.602 4.27 1.20.2 0.8 CV, IP 5.9 701
     MU Cam Detected as a persistent source in the 17-30 keV band.
IGR J06293-1359 97.327 -13.998 4.86 0.80.2 0.8 ? Y 5.1 857
Detected in a 1611.4 day outburst from MJD=52875.3.
IGR J06323+1048 98.073 10.803 3.95 0.6 1.0 ? YY 6.4 315
Detected in a 6.9 day outburst from MJD=52930.2.
PKS 0637-752 98.944 -75.271 3.59 0.70.1 1.20.2 AGN, QSO, Blazar 7.1 1792
     SWIFT J0635.9-7515 Detected as a persistent source in the 18-60 keV band.
SWIFT J0640.4-2554 100.045 -25.83 3.95 2.10.4 1.80.6 AGN, Sy1.2 6.4 361
     ESO 490-IG026 Detected as a persistent source in the 20-40 keV band.
IGR J06415+3251 100.368 32.861 2.79 2.00.3 1.80.5 AGN, Sy2 9.4 222
Detected as a persistent source in the 18-60 keV band.
IGR J06414-4329 100.375 -43.501 5.38 2.00.7 2.4 ? Y 4.6 92
Detected in a 1155.2 day outburst from MJD=53137.5.
IGR J06421-5305 100.603 -53.081 4.86 1.40.6 2.0 ? Y 5.1 177
Detected in a 40.9 day outburst from MJD=55362.6. Flags: WARN
Mrk 6 103.051 74.427 1.84 2.50.2 2.60.3 AGN, Sy1.5 15.1 831
Detected as a persistent source in the 18-60 keV band.
IGR J06552-1146 103.792 -11.77 4.78 0.3 0.6 ? Y 5.2 1378
Detected in a 1611.4 day outburst from MJD=52875.4.
3A 0656-072 104.57 -7.21 0.74 3.30.2 1.10.3 HMXB, XP, Be, T Y 46.0 1422
Detected in a 3.3 day outburst from MJD=54414.2.
IGR J07072-1227 106.801 -12.427 4.86 0.50.1 0.80.3 ? 5.1 1523
Detected as a persistent source in the 18-60 keV band.
SWIFT J0709.3-1527 107.287 -15.509 4.32 0.90.2 0.6 AGN 5.8 1380
     PKS0706-15 Detected as a persistent source in the 18-60 keV band.
IGR J07096-7150 107.624 -71.858 4.06 0.3 0.5 ? Y 6.2 1589
Detected in a 157.4 day outburst from MJD=55341.2.
IGR J07202+0009 110.063 0.127 4.25 0.4 0.7 ? Y 5.9 829
Detected in a 1.3 day outburst from MJD=55321.7. Flags: WARN
IGR J07225-3810 110.621 -38.168 5.20 1.50.3 1.0 AGN, Blazar 4.7 430
Detected as a persistent source in the 17-30 keV band.
PKS 0723-008 111.492 -0.955 3.74 0.60.2 1.20.4 AGN, BL Lac 6.8 863
     SWIFT J0725.7-0055 Detected as a persistent source in the 30-60 keV band.
3A 0726-260 112.209 -26.099 4.39 1.20.3 0.9 HMXB, XP 5.7 542
Detected as a persistent source in the 17-30 keV band.
IGR J07304-7212 112.641 -72.233 3.89 0.60.2 0.5 ? Y 6.5 1269
Detected in a 43.9 day outburst from MJD=55357.0.
SWIFT J0732.5-1331 113.156 -13.518 2.66 1.50.2 0.80.3 CV, IP 9.9 1377
     V667 Pup Detected as a persistent source in the 18-60 keV band.
IGR J07361-4537 114.034 -45.618 5.45 0.3 0.5 ? YY 4.5 1485
Detected in a 10.1 day outburst from MJD=53359.9. Flags: WARN
Mrk 79 115.769 49.812 4.21 3.10.8 2.7 AGN, Sy1.2 6.0 74
     SWIFT J0742.5+4948 Detected as a persistent source in the 18-60 keV band.
IGR J07437-5137 115.921 -51.617 4.32 0.70.2 0.5 ? 5.8 1589
Detected as a persistent source in the 18-60 keV band.
SWIFT J0746.3-1608 116.597 -16.228 4.25 1.10.2 0.7 CV, IP? 5.9 1013
Detected as a persistent source in the 20-40 keV band.
IGR J07480-8329 117.049 -83.496 5.41 1.20.3 0.9 ? Y 4.5 546
Detected in a 12.2 day outburst from MJD=52648.2. Flags: WARN
EXO 0748-676 117.141 -67.753 0.42 14.90.2 12.80.3 LMXB, B, D, T Y 108.7 935
Detected in a 1683.9 day outburst from MJD=52641.4.
IGR J07506-1547 117.646 -15.788 4.69 0.4 0.80.4 ? Y 5.3 914
Detected in a 449.7 day outburst from MJD=52714.2.
IGR J07541-3500 118.547 -35.008 5.23 0.60.2 0.6 ? 4.7 916
Detected as a persistent source in the 18-60 keV band. Flags: WARN
IGR J07565-4139 119.082 -41.628 3.19 0.80.1 0.80.2 AGN, Sy2 Y 8.1 2133
Detected in a 808.7 day outburst from MJD=52893.1.
IGR J07597-3842 119.924 -38.733 1.36 2.60.1 1.90.2 AGN, Sy1.2 21.4 1820
Detected as a persistent source in the 18-60 keV band.
SWIFT J0800.7-4309 120.092 -43.166 4.86 0.50.1 0.4 ? 5.1 2445
Detected as a persistent source in the 18-60 keV band.
1RXS J080114.6-462324 120.284 -46.379 3.26 0.40.1 0.60.2 CV, IP Y 7.9 2679
Detected in a 2.8 day outburst from MJD=53687.1.
ESO 209-G12 120.49 -49.778 1.99 1.20.1 1.50.2 AGN, Sy1.5 13.8 2568
Detected as a persistent source in the 20-100 keV band.
IGR J08030-6853 120.765 -68.892 4.25 0.4 1.00.4 ? Y 5.9 776
Detected in a 4.9 day outburst from MJD=55353.9. Flags: WARN
Mrk 1210 121.021 5.153 3.55 2.90.6 4.01.0 AGN, Sy2 7.2 142
     SWIFT J0804.2+0506 Detected as a persistent source in the 20-100 keV band.
IGR J08062+4159 121.566 41.99 4.46 3.30.7 2.3 ? Y 5.6 56
Detected in a 4.4 day outburst from MJD=53500.6. Flags: WARN
PG 0804+761 122.744 76.045 4.06 1.00.2 0.80.3 AGN, Sy1 6.2 1158
Detected as a persistent source in the 20-40 keV band.
IGR J08190-3835 124.759 -38.583 3.55 0.70.1 0.60.2 AGN, Sy2 7.2 2720
Detected as a persistent source in the 20-100 keV band.
IGR J08262+4051 126.556 40.855 4.86 1.20.5 1.7 ? Y 5.1 100
Detected in a 2.3 day outburst from MJD=53500.6.
IGR J08262-3736 126.558 -37.62 4.01 0.60.1 0.70.2 HMXB, Sg 6.3 2719
Detected as a persistent source in the 20-100 keV band.
Vela Pulsar 128.836 -45.176 0.44 6.80.1 7.40.1 PWN, PSR 99.7 3880
Detected as a persistent source in the 18-60 keV band.
4U 0836-429 129.348 -42.901 0.23 13.40.1 12.00.1 LMXB, B, T Y 428.2 3814
     GS 0836-429 Detected in a 188.5 day outburst from MJD=52955.4.
FRL 1146 129.628 -35.993 2.09 1.30.1 1.40.2 AGN, Sy1.5 13.0 2480
Detected as a persistent source in the 18-60 keV band.
IGR J08390-4833 129.704 -48.524 2.93 0.60.1 0.3 CV, IP 8.9 3847
Detected as a persistent source in the 18-60 keV band.
IGR J08408-4503 130.196 -45.059 3.26 0.2 0.3 HMXB, SFXT Y 7.9 4031
Detected in a 0.6 day outburst from MJD=52821.7.
QSO B0836+710 130.352 70.895 1.39 2.30.2 4.10.3 AGN, QSO, Blazar 20.9 1398
Detected as a persistent source in the 20-100 keV band.
SWIFT J0845.0-3531 131.31 -35.495 4.61 0.60.1 0.70.2 AGN, Sy1.2 5.4 2247
     1RXS J084521.7-353048 Detected as a persistent source in the 18-60 keV band.
IGR J08447+6610 131.356 66.144 4.95 0.40.2 0.90.3 ? 5.0 1257
Detected as a persistent source in the 20-100 keV band.
IGR J08507+1503 132.669 15.054 5.04 1.80.4 1.5 ? 4.9 176
Detected as a persistent source in the 20-40 keV band.
IGR J08517-1827 132.931 -18.452 4.25 2.30.6 2.0 ? Y 5.9 118
Detected in a 2.8 day outburst from MJD=53496.7. Flags: WARN
IGR J08557+6420 133.942 64.349 4.42 0.80.2 0.90.3 AGN, Sy2? 5.7 1139
Detected as a persistent source in the 18-60 keV band.
IGR J08558+0814 133.957 8.248 5.14 2.60.5 1.9 AGN, Sy1 4.8 121
Detected as a persistent source in the 17-30 keV band.
Mrk 18 135.416 60.15 4.01 1.10.3 1.90.4 AGN, Sy2 6.3 707
     SWIFT J0902.0+6007 Detected as a persistent source in the 18-60 keV band.
Vela X-1 135.529 -40.555 0.17 223.20.1 55.00.2 HMXB, XP 2401.3 3727
Detected as a persistent source in the 20-40 keV band.
IGR J09026-4812 135.656 -48.226 1.67 1.20.1 1.10.1 AGN, Sy1 16.8 3885
Detected as a persistent source in the 18-60 keV band.
IGR J09025-6814 135.664 -68.227 4.69 0.70.2 1.40.4 AGN, XBONG Y 5.3 806
Detected in a 225.9 day outburst from MJD=52955.6.
IGR J09034+5329 135.833 53.506 4.89 1.70.6 2.1 ? 5.1 123
     1RXS J090320.0+53302 Detected as a persistent source in the 17-30 keV band.
1RXS J090431.1-382920 136.128 -38.49 3.79 0.60.1 0.50.2 AGN, Sy1 6.7 2855
Detected as a persistent source in the 20-100 keV band.
IGR J09058+7747 136.48 77.813 3.59 0.4 0.7 ? Y 7.1 1083
Detected in a 0.7 day outburst from MJD=55134.5.
SWIFT J0917.2-6221 139.039 -62.325 2.53 1.40.1 0.80.2 AGN, Sy1 10.5 1817
Detected as a persistent source in the 18-60 keV band.
IGR J09189-4418 139.744 -44.31 5.24 0.20.1 0.40.2 AGN Y 4.7 3548
Detected in a 1140.5 day outburst from MJD=52758.5.
MCG-01-24-012 140.193 -8.056 4.32 1.70.4 3.00.8 AGN, Sy2 5.8 166
Detected as a persistent source in the 20-100 keV band.
4U 0918-549 140.217 -55.216 0.89 4.00.1 3.10.2 LMXB, B 36.5 2882
Detected as a persistent source in the 18-60 keV band.
SWIFT J0924.2-3141 140.969 -31.706 4.32 1.00.2 1.60.4 ? 5.8 732
     CXO J092418.2-314217 Detected as a persistent source in the 20-100 keV band. Flags: BLEND
Mrk 110 141.304 52.286 4.19 3.70.7 3.01.1 AGN, NLS1 6.0 85
Detected as a persistent source in the 18-60 keV band.
IGR J09253+6929 141.448 69.464 4.30 0.70.2 0.60.3 AGN, Sy1.5 5.8 1369
Detected as a persistent source in the 17-30 keV band.
SWIFT J0929.7+6232 142.428 62.522 3.38 1.10.2 1.30.4 AGN, Sy2 7.6 955
Detected as a persistent source in the 18-60 keV band.
IGR J09446-2636 146.152 -26.565 5.45 0.6 1.1 AGN, Sy1.5 Y 4.5 346
Detected in a 0.6 day outburst from MJD=53496.8.
IGR J09453-2600 146.327 -26.049 4.95 0.6 1.1 ? Y 5.0 358
Detected in a 5.4 day outburst from MJD=53493.5.
NGC 2992 146.425 -14.326 1.96 3.50.3 4.40.5 AGN, Sy2 14.0 279
Detected as a persistent source in the 18-60 keV band.
MCG-05-23-16 146.917 -30.948 0.92 8.60.3 8.60.5 AGN, Sy2 34.5 400
Detected as a persistent source in the 18-60 keV band.
4C 73.08 147.505 73.257 4.69 0.80.2 0.6 AGN, Sy2 5.3 1292
     SWIFT J0950.5+7318 Detected as a persistent source in the 20-40 keV band.
IGR J09523-6231 148.085 -62.543 2.93 0.80.1 0.60.2 AGN, Sy1.9 8.9 2264
Detected as a persistent source in the 18-60 keV band.
M81 148.951 69.06 4.69 0.60.2 0.70.3 AGN, Sy1.8, Liner 5.3 1287
Detected as a persistent source in the 18-60 keV band.
SWIFT J0958.0-4208 149.461 -42.144 3.84 0.90.2 0.5 CV, IP? 6.6 1456
Detected as a persistent source in the 20-40 keV band.
NGC 3081 149.873 -22.826 2.06 3.20.3 4.10.5 AGN, Sy2 13.2 354
Detected as a persistent source in the 18-60 keV band.
SWIFT J0959.7-3112 149.958 -31.223 4.19 1.30.3 1.30.5 AGN, Sy1 6.0 385
     1RXS J095942.1-311300 Detected as a persistent source in the 18-60 keV band.
NGC 3079 150.449 55.747 4.46 1.80.4 2.50.8 AGN, Sy2 5.6 254
     SWIFT J1001.7+5543 Detected as a persistent source in the 18-60 keV band.
GRO J1008-57 152.442 -58.292 0.42 4.80.1 2.30.2 HMXB, XP, Be, T Y 105.9 2775
Detected in a 11.9 day outburst from MJD=54913.2.
SWIFT J1009.3-4250 152.451 -42.812 2.49 1.60.2 1.70.3 AGN, Sy2 10.7 1221
     ESO 263-G013 Detected as a persistent source in the 18-60 keV band.
IGR J10101-5654 152.549 -56.926 2.20 0.90.1 0.50.2 HMXB, Be Y 12.3 2711
Detected in a 220.6 day outburst from MJD=52937.2.
IGR J10109-5746 152.762 -57.804 1.97 1.20.1 0.50.2 CV, Symb 13.9 2822
     V648 Cor Detected as a persistent source in the 18-60 keV band.
IGR J10147-6354 153.563 -63.864 5.35 0.2 0.40.2 AGN, Sy1.2 Y 4.6 2572
Detected in a 837.7 day outburst from MJD=52692.4.
IGR J10163-5028 154.071 -50.481 5.24 0.3 0.4 ? Y 4.7 2067
Detected in a 14.3 day outburst from MJD=53742.8. Flags: WARN
IGR J10200-1436 155.007 -14.611 4.94 1.90.4 1.4 ? 5.0 173
Detected as a persistent source in the 20-40 keV band.
NGC 3227 155.878 19.865 1.73 6.30.5 6.30.8 AGN, Sy1.5 16.2 122
Detected as a persistent source in the 18-60 keV band.
IGR J10252-6829 156.252 -68.458 5.45 0.3 0.80.2 ? Y 4.5 1682
Detected in a 0.6 day outburst from MJD=54143.1.
NGC 3281 157.967 -34.854 2.31 3.20.3 3.20.6 AGN, Sy2 11.6 263
Detected as a persistent source in the 18-60 keV band.
IGR J10344+1401 158.604 14.017 4.39 2.00.8 2.7 ? Y 5.7 51
Detected in a 634.2 day outburst from MJD=52806.3.
4U 1036-56 159.391 -56.799 1.17 1.20.1 0.3 HMXB, Be, T Y 25.8 2853
Detected in a 33.3 day outburst from MJD=54113.2.
SWIFT J1038.8-4942 159.688 -49.782 3.09 0.80.1 1.40.2 AGN, Sy1.5 8.4 1673
Detected as a persistent source in the 20-100 keV band.
IGR J10404-4625 160.093 -46.424 2.51 1.70.2 2.40.3 AGN, Sy2 10.6 1004
Detected as a persistent source in the 20-100 keV band.
IGR J10432-6300 160.802 -63.013 5.45 0.2 0.3 ? Y 4.5 2980
Detected in a 5.6 day outburst from MJD=53529.7. Flags: WARN
IGR J10432-4446 160.805 -44.779 4.46 0.5 1.00.4 ? Y 5.6 696
Detected in a 22.3 day outburst from MJD=52805.4. Flags: WARN
IGR J10447-6027 161.15 -60.431 3.34 0.70.1 0.90.2 ? 7.7 3097
Detected as a persistent source in the 18-60 keV band.
Eta Carinae 161.196 -59.755 3.89 0.30.1 0.60.2 XB 6.5 3090
     4U 1053-58 Detected as a persistent source in the 18-60 keV band.
MCG+04-26-006 161.722 25.903 5.04 0.90.3 1.90.6 AGN, Liner 4.9 274
Detected as a persistent source in the 20-100 keV band.
IGR J11014-6103 165.443 -61.022 4.46 0.20.1 0.70.2 PWN, PSR 5.6 3237
Detected as a persistent source in the 20-100 keV band.
Mrk 421 166.114 38.209 0.35 17.50.2 12.10.3 AGN, BL Lac Y 149.0 670
Detected in a 48.0 day outburst from MJD=53870.1.
NGC 3516 166.698 72.569 1.40 3.50.2 4.40.3 AGN, Sy1.5 20.8 972
Detected as a persistent source in the 20-100 keV band.
IGR J11098-6457 167.36 -65.04 4.25 0.50.1 0.60.2 CV, Symb 5.9 2995
Detected as a persistent source in the 20-100 keV band.
IGR J11187-5438 169.588 -54.626 3.46 0.60.1 0.80.2 LMXB? 7.4 2731
Detected as a persistent source in the 20-100 keV band.
1A 1118-615 170.238 -61.916 0.36 3.40.1 1.60.2 HMXB, XP, Be, T Y 139.2 3307
Detected in a 34.9 day outburst from MJD=54864.6.
Cen X-3 170.316 -60.623 0.20 55.80.1 5.80.2 HMXB, XP 751.1 3397
Detected as a persistent source in the 17-30 keV band.
IGR J11215-5952 170.445 -59.863 1.46 0.30.1 0.3 HMXB, SFXT Y 19.7 3313
Detected in a 0.5 day outburst from MJD=52823.6.
1RXS J112955.1-655542 172.487 -65.906 4.54 0.50.1 0.60.2 AGN? 5.5 3089
Detected as a persistent source in the 17-30 keV band.
IGR J11305-6256 172.779 -62.947 0.92 2.60.1 1.30.2 HMXB Y 34.9 3415
Detected in a 447.9 day outburst from MJD=53098.6.
IGR J11321-5311 173.067 -53.195 3.55 0.2 0.4 AXP? YY 7.2 2416
Detected in a 0.5 day outburst from MJD=53548.9.
IGR J11366-6002 174.175 -60.052 3.59 0.70.1 0.50.2 AGN, Sy2, Liner 7.1 3374
Detected as a persistent source in the 20-100 keV band.
NGC 3783 174.757 -37.739 2.96 8.61.1 5.51.8 AGN, Sy1.5 8.8 46
Detected as a persistent source in the 18-60 keV band.
GT Mus 174.873 -65.398 1.39 0.60.1 0.3 RSCVn Y 20.9 3208
     IGR J11395-6520 Detected in a 0.8 day outburst from MJD=52824.2.
IGR J11435-6109 176.001 -61.127 0.68 3.20.1 2.10.2 HMXB, XP, Be, T Y 51.9 3453
Detected in a 9.7 day outburst from MJD=53537.8.
SWIFT J1143.7+7942 176.306 79.626 4.69 1.30.3 1.30.5 AGN, Sy1.2 5.3 556
Detected as a persistent source in the 18-60 keV band.
H 1143-182 176.419 -18.454 4.19 4.00.7 3.61.2 AGN, Sy1.5 6.0 94
Detected as a persistent source in the 20-40 keV band.
PKS 1143-696 176.449 -69.894 3.46 0.80.1 1.10.2 AGN, Sy1.2 7.4 2126
Detected as a persistent source in the 20-100 keV band.
GRB080723B 176.795 -60.231 2.49 0.2 0.3 GRB YY 10.7 3316
     IGR J11470-6015 Detected in a 0.5 day outburst from MJD=54670.0.
1E 1145.1-6141 176.869 -61.954 0.29 20.50.1 12.10.2 HMXB, XP, T 225.6 3454
Detected as a persistent source in the 18-60 keV band.
B2 1144+35B 176.885 35.108 3.95 0.60.1 0.80.3 AGN, Sy2 Y 6.4 1163
Detected in a 1321.5 day outburst from MJD=54122.4.
2E 1145.5-6155 177.0 -62.207 0.88 2.10.1 1.40.2 HMXB, XP, T Y 36.7 3492
     H 1145-619 Detected in a 1.9 day outburst from MJD=52789.1.
IGR J11486-0505 177.16 -5.098 4.58 1.20.2 0.7 ? 5.4 829
Detected as a persistent source in the 20-40 keV band. Flags: WARN
IGR J11502-5427 177.542 -54.463 5.24 0.2 0.4 ? YY 4.7 2606
Detected in a 1.1 day outburst from MJD=53165.3. Flags: WARN
IGR J11592+1437 179.809 14.621 4.86 0.3 0.5 ? Y 5.1 1705
Detected in a 1.0 day outburst from MJD=53560.6. Flags: WARN
IGR J11597-6324 179.92 -63.408 4.01 0.2 0.3 ? Y 6.3 3348
Detected in a 1.1 day outburst from MJD=54294.7.
SWIFT J1200.8+0650 180.241 6.806 2.74 0.90.1 1.20.2 AGN, Sy2 9.6 2477
Detected as a persistent source in the 18-60 keV band.
IGR J12026-5349 180.698 -53.835 1.32 2.40.1 2.20.2 AGN, Sy2 22.3 2307
Detected as a persistent source in the 18-60 keV band.
NGC 4051 180.79 44.531 1.82 2.00.1 1.40.3 AGN, NLS1 15.3 1232
Detected as a persistent source in the 20-40 keV band.
NGC 4074 181.136 20.249 3.20 1.10.2 1.10.3 AGN, Sy2 8.1 1341
Detected as a persistent source in the 18-60 keV band.
IGR J12077-6547 181.925 -65.789 4.54 0.2 0.3 ? Y 5.5 3349
Detected in a 16.8 day outburst from MJD=54114.5. Flags: WARN
Mrk 198 182.292 47.107 5.00 0.70.2 0.6 AGN, Sy2 5.0 949
     SWIFT J1209.5+4702 Detected as a persistent source in the 18-60 keV band.
NGC 4138 182.374 43.685 2.46 0.90.1 1.50.2 AGN, Sy1.9 10.8 1240
Detected as a persistent source in the 18-60 keV band.
NGC 4151 182.636 39.405 0.29 23.10.1 27.40.2 AGN, Sy1.5 216.9 1311
Detected as a persistent source in the 18-60 keV band.
IGR J12107+0525 182.677 5.416 4.19 0.50.1 0.60.2 ? Y 6.0 3057
Detected in a 0.5 day outburst from MJD=52644.6.
IGR J12107+3822 182.681 38.381 4.76 0.50.1 0.50.2 AGN, Sy1.5 Y 5.2 1307
Detected in a 1321.5 day outburst from MJD=53725.9.
IGR J12123-5802 183.108 -58.006 4.05 0.50.1 0.3 CV, IP 6.2 3056
Detected as a persistent source in the 17-30 keV band.
IGR J12131+0700 183.207 6.996 3.84 0.50.1 0.90.2 AGN, Sy1.5-Sy1.8 Y 6.6 3190
Detected in a 2417.3 day outburst from MJD=52765.4.
EXMS B1210-645 183.272 -64.897 2.51 1.00.1 0.60.2 HMXB, Be, T 10.6 3422
Detected as a persistent source in the 17-30 keV band.
IGR J12134-6015 183.35 -60.254 4.01 0.50.1 0.40.2 ? Y 6.3 3408
Detected in a 1605.1 day outburst from MJD=53292.6.
NGC 4235 184.288 7.159 2.08 1.00.1 1.00.2 AGN, Sy1.2 13.1 3387
Detected as a persistent source in the 18-60 keV band.
Mrk 766 184.611 29.813 2.93 1.20.1 0.90.2 AGN, NLS1 8.9 1360
Detected as a persistent source in the 20-100 keV band.
NGC 4258 184.74 47.304 3.79 1.00.2 1.10.3 AGN, Sy2 6.7 881
Detected as a persistent source in the 20-40 keV band.
PKS 1217+02 185.083 2.057 3.50 0.60.1 0.60.2 AGN, Sy1.2 7.3 3291
     1RXS J122011.9+020342 Detected as a persistent source in the 18-60 keV band.
IGR J12207+1517 185.193 15.287 4.01 0.2 1.00.2 ? Y 6.3 2448
Detected in a 1398.9 day outburst from MJD=53623.8.
PG 1218+305 185.343 30.136 3.46 0.60.1 0.50.2 AGN, BL Lac Y 7.4 1387
     SWIFT J1221.3+3012 Detected in a 368.8 day outburst from MJD=54439.1.
4C 04.42 185.594 4.221 2.20 0.80.1 1.60.2 AGN, QSO, Blazar 12.3 3573
Detected as a persistent source in the 20-100 keV band.
Mrk 50 185.851 2.679 2.79 0.90.1 0.60.2 AGN, Sy1 9.4 3472
Detected as a persistent source in the 18-60 keV band.
PG 1222+216 186.226 21.366 3.38 0.80.1 1.10.2 AGN, QSO, Blazar 7.6 1807
     SWIFT J1224.9+2122 Detected as a persistent source in the 20-100 keV band.
NGC 4388 186.446 12.662 0.38 10.00.1 12.50.2 AGN, Sy2 125.9 2967
Detected as a persistent source in the 18-60 keV band.
NGC 4395 186.454 33.547 2.49 1.00.1 1.30.2 AGN, Sy2 10.7 1468
Detected as a persistent source in the 18-60 keV band.
GX 301-2 186.657 -62.771 0.18 192.30.1 20.60.2 HMXB, XP, T 2074.5 3702
Detected as a persistent source in the 17-30 keV band.
XSS J12270-4859 187.008 -48.893 2.30 1.60.2 1.50.3 LMXB, MSP 11.7 1313
     1RX J122758.8-485348 Detected as a persistent source in the 18-60 keV band.
3C 273 187.278 2.052 0.32 13.20.1 17.00.2 AGN, Sy1, QSO 173.8 3589
Detected as a persistent source in the 18-60 keV band.
IGR J12319-0749 187.977 -7.816 3.97 0.80.1 0.4 AGN, QSO, Blazar 6.4 2004
Detected as a persistent source in the 18-60 keV band.
Mrk 771 188.039 20.125 4.01 0.60.1 0.4 AGN, Sy1 Y 6.3 2072
     SWIFT J1232.1+2009 Detected in a 468.4 day outburst from MJD=55010.4.
XSS J12303-4232 188.054 -42.295 4.86 0.80.2 0.8 AGN, Sy1.5 5.1 756
     SWIFT J1232.0-4219 Detected as a persistent source in the 18-60 keV band.
IGR J12341-6143 188.467 -61.796 3.98 0.2 0.3 ? Y 6.3 3470
Detected in a 0.9 day outburst from MJD=54649.9.
RT Cru 188.728 -64.566 0.76 4.10.1 2.50.2 XB, Symb 44.3 3395
     IGR J12349-6434 Detected as a persistent source in the 18-60 keV band.
NGC 4507 188.902 -39.909 0.80 7.80.2 10.40.4 AGN, Sy2 41.8 682
Detected as a persistent source in the 18-60 keV band.
SWIFT J1238.6+0928 189.642 9.488 4.54 0.40.1 0.3 AGN, Sy2 5.5 3387
     2MASX J12384342+0927362 Detected as a persistent source in the 18-60 keV band.
ESO 506-G27 189.727 -27.308 2.84 4.00.5 5.30.9 AGN, Sy2 9.2 159
Detected as a persistent source in the 20-100 keV band.
LEDA 170194 189.776 -16.18 2.46 1.70.2 2.20.4 AGN, Sy2 10.8 666
Detected as a persistent source in the 18-60 keV band.
NGC 4593 189.914 -5.344 0.81 3.70.1 4.30.2 AGN, Sy1 40.8 2561
Detected as a persistent source in the 18-60 keV band.
IGR J12415-5750 190.356 -57.834 1.83 1.40.1 1.40.2 AGN, Sy1.5 15.2 2979
Detected as a persistent source in the 18-60 keV band.
1H 1249-637 190.709 -63.059 3.46 0.60.1 0.3 HMXB, Be 7.4 3374
Detected as a persistent source in the 17-30 keV band.
IGR J12482-5828 191.991 -58.5 3.23 0.60.1 0.80.2 AGN, Sy1.9 Y 8.0 3214
Detected in a 1602.9 day outburst from MJD=52650.6.
IGR J12489-6243 192.223 -62.718 4.86 0.2 0.3 ? Y 5.1 3415
Detected in a 774.0 day outburst from MJD=52650.6.
4U 1246-588 192.415 -59.087 0.82 3.40.1 3.00.2 LMXB, T 40.0 3251
Detected as a persistent source in the 18-60 keV band.
NGC 4748 193.05 -13.43 4.95 0.60.2 0.70.3 AGN, NLS1 5.0 1094
Detected as a persistent source in the 18-60 keV band.
EX Hya 193.071 -29.296 4.54 1.40.3 1.1 CV, IP, DQ? 5.5 349
     4U 1228-29 Detected as a persistent source in the 18-60 keV band.
ESO 323-G32 193.335 -41.637 3.69 0.80.2 0.90.3 AGN, Sy2 6.9 1148
Detected as a persistent source in the 18-60 keV band.
3C 279 194.047 -5.789 2.90 0.90.1 1.40.2 AGN, QSO, Blazar 9.0 2093
Detected as a persistent source in the 20-100 keV band.
IGR J12562+2554 194.051 25.905 4.71 0.50.1 0.60.2 Cluster? 5.3 1848
Detected as a persistent source in the 18-60 keV band.
1H 1254-690 194.405 -69.289 1.01 2.50.1 0.4 LMXB, B, D 30.7 2673
Detected as a persistent source in the 17-30 keV band.
IGR J12579-0633 194.519 -6.521 4.13 0.3 0.5 ? YY 6.1 1935
Detected in a 21.1 day outburst from MJD=55000.7.
IGR J12585-6045 194.634 -60.765 5.24 0.2 0.3 ? Y 4.7 3501
Detected in a 24.2 day outburst from MJD=54103.7. Flags: WARN
Coma Cluster 194.953 27.981 1.87 1.40.1 0.4 Cluster 14.8 1849
Detected as a persistent source in the 17-30 keV band.
GX 304-1 195.322 -61.602 1.33 1.60.1 0.70.2 HMXB, XP, T Y 22.1 3564
Detected in a 1335.8 day outburst from MJD=53652.5.
IGR J13020-6359 195.497 -63.968 1.46 1.80.1 1.30.2 HMXB, XP, Be 19.8 3463
Detected as a persistent source in the 18-60 keV band. Flags: BLEND
Mrk 783 195.745 16.408 3.09 0.90.1 1.30.2 AGN, NLS1 8.4 2131
Detected as a persistent source in the 20-100 keV band.
PSR B1259-63 195.75 -63.833 2.69 0.90.1 1.20.2 PSR, Be 9.8 3518
Detected as a persistent source in the 20-100 keV band. Flags: BLEND
IGR J13038+5348 195.951 53.798 4.61 1.10.3 2.30.5 AGN, Sy1.2 5.4 299
Detected as a persistent source in the 20-100 keV band.
NGC 4941 196.055 -5.552 4.18 0.60.1 0.70.2 AGN, Sy2 6.0 1785
Detected as a persistent source in the 18-60 keV band.
IGR J13042-1020 196.06 -10.34 3.50 0.90.2 1.40.3 AGN, Sy2 7.3 1254
     NGC 4939 Detected as a persistent source in the 20-100 keV band.
IGR J13045-5630 196.131 -56.515 3.64 0.80.1 0.40.2 ? 7.0 3076
Detected as a persistent source in the 20-40 keV band.
NGC 4945 196.359 -49.471 0.42 11.30.1 17.00.2 AGN, Sy2 109.1 2021
Detected as a persistent source in the 20-100 keV band.
ESO 323-G77 196.611 -40.414 2.04 1.80.1 1.30.3 AGN, Sy1.2 13.4 1330
Detected as a persistent source in the 18-60 keV band.
IGR J13091+1137 197.273 11.634 1.73 1.60.1 2.60.2 AGN, XBONG 16.2 2165
Detected as a persistent source in the 20-100 keV band.
IGR J13107-5626 197.655 -56.449 3.64 0.60.1 0.60.2 AGN, RG Y 7.0 3078
Detected in a 883.6 day outburst from MJD=53799.3.
IGR J13109-5552 197.68 -55.87 1.90 1.20.1 1.90.2 AGN, Sy1 14.5 3056
Detected as a persistent source in the 20-100 keV band.
IGR J13133-1109 198.321 -11.143 5.12 0.90.2 0.7 AGN, Sy1 4.8 920
     1RXS J131305.9-110731 Detected as a persistent source in the 20-40 keV band.
IGR J13149+4422 198.822 44.407 4.39 1.00.2 0.70.4 AGN, Sy2, Liner 5.7 815
Detected as a persistent source in the 18-60 keV band.
IGR J13166+2340 199.132 23.66 4.60 0.70.1 0.5 ? 5.4 1720
Detected as a persistent source in the 20-40 keV band.
IGR J13168-7157 199.226 -71.923 3.69 0.60.1 0.90.2 AGN, Sy1.5 6.9 1924
Detected as a persistent source in the 18-60 keV band.
IGR J13186-6257 199.605 -62.971 3.26 0.60.1 0.3 HMXB?, Be? 7.9 3526
Detected as a persistent source in the 18-60 keV band.
IGR J13191+2307 199.787 23.119 4.69 0.60.1 0.5 ? Y 5.3 1685
Detected in a 2283.9 day outburst from MJD=53239.7.
NGC 5100 200.219 8.915 4.06 0.70.1 0.90.3 AGN, Liner 6.2 1916
Detected as a persistent source in the 18-60 keV band.
IGR J13216-5947 200.447 -59.766 4.39 0.40.1 0.3 ? 5.7 3496
Detected as a persistent source in the 18-60 keV band.
MCG-03-34-064 200.602 -16.729 4.34 1.60.3 1.40.5 AGN, Sy2 5.8 434
     IGR J13225-1645 Detected as a persistent source in the 20-40 keV band.
SAX J1324.3-6313 201.161 -63.228 4.25 0.30.1 0.40.2 LMXB, B, T Y 5.9 3501
Detected in a 57.4 day outburst from MJD=52667.8.
CEN A 201.365 -43.019 0.23 44.30.1 54.60.2 AGN, Sy2 408.3 1780
Detected as a persistent source in the 18-60 keV band.
4U 1323-62 201.65 -62.136 0.41 9.00.1 6.70.2 LMXB, B, D 110.3 3581
Detected as a persistent source in the 18-60 keV band.
IGR J13290-6323 202.267 -63.392 3.89 0.30.1 0.30.2 ? Y 6.5 3544
Detected in a 3.1 day outburst from MJD=52836.4.
IGR J13307-6038 202.671 -60.633 4.39 0.2 0.3 ? Y 5.7 3565
Detected in a 9.3 day outburst from MJD=53085.7. Flags: WARN
ESO 383-G18 203.36 -34.016 3.84 0.90.2 0.70.3 AGN, Sy2 6.6 1153
Detected as a persistent source in the 18-60 keV band.
BH CVn 203.699 37.182 4.19 0.70.2 0.7 RSCVn Y 6.0 810
     1RX J133447.5+37110 Detected in a 11.5 day outburst from MJD=52773.9.
MCG-6-30-15 203.974 -34.296 1.31 3.10.1 2.10.3 AGN, Sy1.2 22.5 1192
Detected as a persistent source in the 18-60 keV band.
NGC 5252 204.567 4.542 0.84 4.90.2 6.10.3 AGN, Sy1.9 38.8 1470
Detected as a persistent source in the 18-60 keV band.
IGR J13396-3306 204.892 -33.101 5.14 0.3 0.6 ? Y 4.8 1056
Detected in a 1550.4 day outburst from MJD=52650.8.
IGR J13402-6428 205.05 -64.48 3.64 0.40.1 0.3 ? Y 7.0 3521
Detected in a 613.6 day outburst from MJD=52926.8.
IGR J13408-6836 205.191 -68.615 5.14 0.2 0.4 ? YY 4.8 2889
Detected in a 41.9 day outburst from MJD=53802.2. Flags: WARN
IGR J13415+3033 205.296 30.378 2.84 1.20.2 1.20.3 AGN, Sy2 9.2 1158
     Mrk 268 Detected as a persistent source in the 18-60 keV band.
SWIFT J1344.7+1934 206.139 19.596 4.69 0.50.2 1.70.3 AGN, Sy2, Liner 5.3 1146
Detected as a persistent source in the 20-100 keV band.
IGR J13466+1921 206.619 19.386 5.09 0.80.2 0.7 AGN, Sy1.2 Y 4.8 1091
Detected in a 1903.3 day outburst from MJD=53144.6.
CEN B 206.704 -60.391 2.17 1.10.1 1.50.2 AGN, RG/Type, 2 12.5 3576
Detected as a persistent source in the 20-100 keV band. Flags: BLEND
4U 1344-60 206.883 -60.61 0.66 4.50.1 4.70.2 AGN, Sy1.5 54.5 3577
Detected as a persistent source in the 18-60 keV band.
IGR J13477-4210 206.998 -42.185 5.15 0.60.1 0.4 AGN, Sy2 4.8 2101
Detected as a persistent source in the 20-40 keV band.
IC 4329A 207.33 -30.31 0.52 11.40.2 12.80.3 AGN, Sy1.2 75.7 792
Detected as a persistent source in the 18-60 keV band.
IGR J13499-4832 207.468 -48.543 4.69 0.2 0.4 ? YY 5.3 2485
Detected in a 1.2 day outburst from MJD=54472.6. Flags: WARN
1AXG J135417-3746 208.564 -37.776 3.26 0.90.1 0.70.2 AGN, Sy1.9 7.9 1812
     Tol 1351-375 Detected as a persistent source in the 18-60 keV band.
IGR J13550-7218 208.805 -72.32 4.46 0.50.1 0.80.2 AGN, Sy2 Y 5.6 1945
Detected in a 909.5 day outburst from MJD=53287.3.
PKS 1355-416 209.719 -41.827 4.78 0.50.1 0.4 AGN, Sy1 Y 5.2 2275
     1RXS J135859.0-415259 Detected in a 1.1 day outburst from MJD=52871.6.
IGR J13595-3454 209.912 -34.904 4.69 0.40.1 0.5 ? Y 5.3 1509
Detected in a 0.8 day outburst from MJD=54882.3. Flags: WARN
IGR J14003-6326 210.19 -63.429 2.64 0.80.1 0.90.2 SNR, PSR, PWN 10.0 3381
Detected as a persistent source in the 20-100 keV band.
IGR J14018-4051 210.526 -40.831 4.95 0.2 0.4 ? Y 5.0 2243
Detected in a 40.4 day outburst from MJD=54103.6. Flags: WARN
IGR J14043-6148 211.123 -61.789 3.42 0.60.1 0.70.2 ? 7.5 3513
Detected as a persistent source in the 20-100 keV band.
IGR J14059-6116 211.485 -61.275 4.13 0.40.1 0.50.2 ? Y 6.1 3548
Detected in a 2198.6 day outburst from MJD=52980.4.
IGR J14080-3023 212.027 -30.398 4.13 0.70.2 0.80.3 AGN, Sy1.5 6.1 1029
Detected as a persistent source in the 18-60 keV band.
V834 Cen 212.281 -45.288 4.27 0.80.1 0.4 CV, P 5.9 2544
     1E 1405-45 Detected as a persistent source in the 17-30 keV band.
IGR J14102+0722 212.549 7.377 4.95 0.3 0.6 ? YY 5.0 1343
Detected in a 0.6 day outburst from MJD=54487.1. Flags: WARN
SWIFT J1410.9-4229 212.665 -42.498 4.86 0.60.1 0.60.2 AGN, Sy2 5.1 2477
Detected as a persistent source in the 20-40 keV band.
Circinus Galaxy 213.287 -65.341 0.35 13.50.1 10.90.2 AGN, Sy2 151.7 3274
Detected as a persistent source in the 18-60 keV band.
NGC 5506 213.312 -3.207 0.63 10.80.2 9.60.4 AGN, Sy2 57.4 777
Detected as a persistent source in the 18-60 keV band.
IGR J14175-4641 214.266 -46.694 2.44 1.10.1 1.20.2 AGN, Sy2 10.9 2628
Detected as a persistent source in the 18-60 keV band.
SWIFT J1417.7+2539 214.476 25.679 4.78 1.50.3 1.1 AGN, BL Lac 5.2 390
     1RXS J141756.8+254329 Detected as a persistent source in the 20-40 keV band.
NGC 5548 214.499 25.137 2.39 2.50.3 2.60.5 AGN, Sy1.5 11.2 399
Detected as a persistent source in the 18-60 keV band.
IGR J14193-6048 214.821 -60.801 4.54 0.40.1 0.40.2 PSR, PWN 5.5 3498
Detected as a persistent source in the 18-60 keV band.
ESO 511-G030 214.842 -26.645 2.55 2.00.2 2.40.4 AGN, Sy1 10.4 758
Detected as a persistent source in the 18-60 keV band.
H 1417-624 215.303 -62.698 1.40 0.70.1 0.40.2 HMXB, XP, Be?, T Y 20.8 3438
Detected in a 11.1 day outburst from MJD=54651.4.
H 1419+480 215.373 47.791 5.40 1.10.3 0.9 AGN, Sy1.5 4.5 394
     QSO B1419+480 Detected as a persistent source in the 18-60 keV band.
IGR J14227-2931 215.683 -29.519 4.61 0.70.2 0.6 ? Y 5.4 1183
Detected in a 1246.6 day outburst from MJD=52650.8.
IGR J14229-3347 215.728 -33.792 3.95 0.3 0.5 ? Y 6.4 1809
Detected in a 2.1 day outburst from MJD=54154.6.
IGR J14235-1547 215.87 -15.779 4.13 1.20.3 1.90.6 ? 6.1 371
Detected as a persistent source in the 18-60 keV band.
IGR J14257-6117 216.282 -61.316 4.85 0.40.1 0.40.2 CV, IP? 5.1 3490
Detected as a persistent source in the 20-100 keV band.
H 1426+428 217.136 42.675 5.04 1.00.3 1.20.5 AGN, BL Lac 4.9 372
Detected as a persistent source in the 18-60 keV band.
IGR J14297-5623 217.415 -56.396 4.01 0.2 0.3 ? YY 6.3 3521
Detected in a 1.5 day outburst from MJD=53431.6.
IGR J14298-6715 217.498 -67.245 2.76 0.90.1 0.60.2 LMXB 9.5 2896
Detected as a persistent source in the 18-60 keV band.
IGR J14300-2558 217.509 -25.982 4.86 0.80.2 0.8 ? 5.1 799
Detected as a persistent source in the 20-40 keV band.
IGR J14301-4158 217.518 -41.979 4.25 0.50.1 0.4 AGN, Sy2 Y 5.9 2548
Detected in a 1526.7 day outburst from MJD=52879.8.
IGR J14315-7046 217.878 -70.773 4.06 0.3 0.4 ? YY 6.2 2233
Detected in a 2.6 day outburst from MJD=52831.8.
IGR J14319-3315 217.988 -33.245 3.95 0.30.1 0.90.2 ? Y 6.4 1849
Detected in a 1035.3 day outburst from MJD=52702.5.
NGC 5643 218.172 -44.173 3.64 0.70.1 0.70.2 AGN, Sy2 7.0 2609
Detected as a persistent source in the 18-60 keV band.
IGR J14331-6112 218.285 -61.261 3.46 0.60.1 0.3 HMXB, Be 7.4 3533
Detected as a persistent source in the 18-60 keV band.
NGC 5674 218.453 5.473 4.01 0.90.2 1.20.3 AGN, Sy2 6.3 1041
     SWIFT J1433.9+0528 Detected as a persistent source in the 20-100 keV band.
SWIFT J1436.8-1615 219.183 -16.114 3.84 1.40.3 1.0 AGN, QSO 6.6 522
Detected as a persistent source in the 20-40 keV band.
IGR J14385+8553 219.616 85.883 5.04 0.7 1.30.6 ? Y 4.9 254
Detected in a 164.3 day outburst from MJD=53175.3.
IGR J14388-0724 219.732 -7.413 4.12 0.4 0.90.4 ? YY 6.1 736
Detected in a 0.7 day outburst from MJD=55214.1.
NGC 5728 220.597 -17.281 1.82 3.20.3 3.40.5 AGN, Sy2 15.3 537
Detected as a persistent source in the 18-60 keV band.
IGR J14437-1653 220.938 -16.894 4.54 0.70.3 1.90.5 ? 5.5 558
Detected as a persistent source in the 20-100 keV band.
IGR J14443-2750 221.072 -27.827 3.99 0.40.2 0.6 ? Y 6.3 1080
Detected in a 9.1 day outburst from MJD=55227.2.
IGR J14471-6414 221.618 -64.273 3.64 0.60.1 0.60.2 AGN, Sy1.2 7.0 3090
Detected as a persistent source in the 18-60 keV band.
IGR J14466-3352 221.656 -33.875 4.54 0.30.1 0.60.2 AGN?, Blazar? Y 5.5 1960
Detected in a 416.1 day outburst from MJD=53774.0.
IGR J14471-6319 221.811 -63.289 3.50 0.60.1 0.70.2 AGN, Sy2 7.3 3263
Detected as a persistent source in the 20-100 keV band.
IGR J14488-5942 222.205 -59.701 3.19 0.60.1 0.3 HMXB, Be Y 8.1 3584
Detected in a 883.6 day outburst from MJD=54108.5.
IGR J14488-4008 222.212 -40.146 4.54 0.50.1 0.4 AGN, Sy1.2 5.5 2495
Detected as a persistent source in the 18-60 keV band.
IGR J14492-5535 222.303 -55.606 2.05 0.90.1 1.20.2 AGN 13.3 3720
     LEDA 3085605 Detected as a persistent source in the 18-60 keV band.
IGR J14515-5542 222.888 -55.677 1.94 1.10.1 1.40.2 AGN, Sy2 14.2 3725
Detected as a persistent source in the 18-60 keV band.
IGR J14532-6356 223.312 -63.927 5.45 0.2 0.4 ? YY 4.5 3143
Detected in a 33.2 day outburst from MJD=52667.3. Flags: WARN
IGR J14536-5522 223.424 -55.362 1.93 1.00.1 0.40.2 CV, IP Y 14.3 3780
     1RX J145341.1-552146 Detected in a 883.6 day outburst from MJD=52915.8.
PKS 1451-375 223.591 -37.774 4.69 0.30.1 0.80.2 AGN, Sy1.2 5.3 2354
     1RXS J145427.2-374738 Detected as a persistent source in the 20-100 keV band.
IGR J14552-5133 223.825 -51.57 2.51 1.00.1 0.90.2 AGN, NLS1 10.6 3556
Detected as a persistent source in the 18-60 keV band.
IGR J14557-5448 223.862 -54.786 4.61 0.50.1 0.50.2 ? 5.4 3762
Detected as a persistent source in the 18-60 keV band.
IGR J14561-3738 224.034 -37.648 2.64 0.90.1 1.10.2 AGN, Sy2 10.0 2338
Detected as a persistent source in the 18-60 keV band.
IC 4518A 224.422 -43.132 1.91 1.40.1 0.80.2 AGN, Sy2 14.4 2751
Detected as a persistent source in the 18-60 keV band.
1RXS J145959.4+120124 224.991 12.003 4.39 0.70.3 1.10.5 ? Y 5.7 553
Detected in a 48.7 day outburst from MJD=54640.7. Flags: WARN
1RXS J150101.7+223812 225.285 22.624 5.14 0.90.4 3.20.7 AGN, BL Lac 4.8 228
     RBS 1452 Detected as a persistent source in the 20-100 keV band.
IGR J15038-6021 225.941 -60.357 3.95 0.50.1 0.40.2 ? 6.4 3531
Detected as a persistent source in the 18-60 keV band.
Mrk 841 226.005 10.438 3.46 1.50.3 2.00.5 AGN, Sy1.5 7.4 532
Detected as a persistent source in the 18-60 keV band.
IGR J15077+0906 226.932 9.109 4.78 0.6 1.0 ? Y 5.2 498
Detected in a 899.8 day outburst from MJD=53755.7.
SWIFT J1508.6-4953 227.154 -49.874 3.19 0.40.1 0.70.2 AGN, Blazar Y 8.1 3651
     PMN J1508-4953 Detected in a 1957.4 day outburst from MJD=53433.7.
IGR J15094-6649 227.383 -66.816 1.78 1.60.1 1.00.2 CV, IP 15.7 2553
Detected as a persistent source in the 18-60 keV band.
IGR J15107-5414 227.67 -54.241 4.06 0.2 0.3 ? YY 6.2 4064
Detected in a 1.9 day outburst from MJD=54307.0.
IRAS 15091-2107 227.975 -21.356 3.50 1.60.2 0.8 AGN, NLS1 7.3 632
Detected as a persistent source in the 20-40 keV band.
PKS 1510-089 228.211 -9.1 2.17 1.60.2 2.80.3 AGN, QSO, Blazar 12.5 972
     SWIFT J1512.8-0906 Detected as a persistent source in the 20-100 keV band.
PSR B1509-58 228.477 -59.138 0.42 8.70.1 11.00.2 PSR, PWN 107.3 3639
Detected as a persistent source in the 18-60 keV band.
SWIFT J1513.8-8125 228.676 -81.394 3.84 1.00.2 1.80.4 AGN, Sy1.2 6.6 709
Detected as a persistent source in the 20-100 keV band.
ESO 328-36 228.696 -40.359 4.54 0.50.1 0.50.2 AGN, Sy1 5.5 2804
     1RXS J151447.8-402157 Detected as a persistent source in the 20-40 keV band.
Cir X-1 230.17 -57.167 0.42 5.40.1 0.40.2 LMXB, B, A, T Y 106.3 3881
     4U 1516-569 Detected in a 180.4 day outburst from MJD=52659.7.
IGR J15219-0935 230.545 -9.647 4.06 0.4 0.6 ? YY 6.2 1026
Detected in a 0.6 day outburst from MJD=55233.2.
IGR J15293-5609 232.316 -56.163 4.69 0.2 0.30.2 XB, Symb Y 5.3 4112
Detected in a 4.8 day outburst from MJD=53771.2. Flags: WARN
IGR J15301-3840 232.54 -38.675 4.25 0.40.1 0.50.2 AGN? 5.9 2706
Detected as a persistent source in the 18-60 keV band.
IGR J15311-3737 232.767 -37.625 3.55 0.50.1 0.90.2 AGN, Sy1 7.2 2493
Detected as a persistent source in the 30-60 keV band.
MCG-01-40-001 233.329 -8.672 3.15 1.10.2 1.00.3 AGN, Sy2 8.2 1062
     SWIFT J1533.2-0836 Detected as a persistent source in the 20-100 keV band.
IGR J15359-5750 234.012 -57.814 2.06 1.10.1 1.30.2 AGN 13.2 3957
Detected as a persistent source in the 18-60 keV band.
IGR J15368-5102 234.197 -51.045 4.06 0.40.1 0.30.2 ? Y 6.2 4461
Detected in a 1641.0 day outburst from MJD=52650.8.
IGR J15390-6226 234.8 -62.467 1.19 0.60.1 0.70.2 LMXB?, BHC?, T Y 25.3 2877
     SWIFT J1539.2-6227 Detected in a 142.7 day outburst from MJD=54770.3.
IGR J15391-5307 234.82 -53.138 4.25 0.40.1 0.3 ? Y 5.9 4558
Detected in a 1969.1 day outburst from MJD=52650.9.
IGR J15407-1206 235.177 -12.109 4.06 0.4 0.5 ? YY 6.2 1058
Detected in a 1.1 day outburst from MJD=55410.3.
IGR J15409-4057 235.259 -40.968 4.13 0.30.1 0.4 ? Y 6.1 3012
Detected in a 4.8 day outburst from MJD=53056.8.
IGR J15415-5029 235.369 -50.491 3.46 0.50.1 0.70.1 AGN, Sy2? 7.4 4572
     WKK 5204 Detected as a persistent source in the 18-60 keV band.
4U 1538-522 235.597 -52.386 0.28 21.00.1 3.50.1 HMXB, XP 237.2 4679
Detected as a persistent source in the 17-30 keV band.
XTE J1543-568 236.008 -56.712 1.32 0.60.1 0.60.2 HMXB, XP, Be, T Y 22.3 4122
Detected in a 8.3 day outburst from MJD=52667.3.
4U 1543-624 236.978 -62.568 0.96 3.00.1 0.80.2 LMXB, NS? 32.8 2715
Detected as a persistent source in the 17-30 keV band.
IGR J15479-4529 237.061 -45.478 0.62 5.20.1 3.40.2 CV, IP 59.2 3930
Detected as a persistent source in the 18-60 keV band.
NGC 5995 237.104 -13.758 1.90 1.80.2 1.80.2 AGN, Sy1.9 14.5 1101
Detected as a persistent source in the 20-100 keV band.
AX J1550.8-5418 237.724 -54.306 1.03 1.00.1 1.80.1 PSR, RM Y 30.1 4594
Detected in a 88.8 day outburst from MJD=54843.2.
XTE J1550-564 237.745 -56.477 0.19 15.90.1 25.80.2 LMXB, BH, M, T Y 897.2 4212
Detected in a 20.6 day outburst from MJD=52721.3.
IGR J15529-5029 238.195 -50.498 3.95 0.40.1 0.3 CV, IP Y 6.4 4746
Detected in a 949.7 day outburst from MJD=52650.8.
IGR J15539-6142 238.397 -61.682 2.71 0.80.1 1.20.2 AGN, Sy2 9.7 2846
Detected as a persistent source in the 18-60 keV band.
IGR J15541-5613 238.527 -56.216 4.32 0.2 0.80.2 ? Y 5.8 4302
Detected in a 949.5 day outburst from MJD=52651.2.
IGR J15549-3740 238.721 -37.67 3.19 1.00.1 1.10.2 AGN, Sy2 8.1 2230
Detected as a persistent source in the 18-60 keV band.
IGR J15550-4034 238.771 -40.582 4.39 0.60.1 0.40.2 ? 5.7 2959
Detected as a persistent source in the 18-60 keV band.
H 1553-542 239.452 -54.435 2.21 0.20.1 0.3 HMXB, XP, Be? Y 12.2 4645
Detected in a 24.8 day outburst from MJD=54494.8.
SWIFT J1559.5+2553 239.818 25.878 3.39 4.30.7 4.21.1 XB, Symb 7.6 138
Detected as a persistent source in the 18-60 keV band.
1H 1556-605 240.26 -60.738 2.11 1.00.1 0.4 LMXB 12.9 3020
Detected as a persistent source in the 17-30 keV band.
IGR J16016-3431 240.408 -34.528 4.86 0.60.2 0.5 ? Y 5.1 1622
Detected in a 456.2 day outburst from MJD=53677.4.
IGR J16024-6107 240.452 -61.148 3.74 0.70.1 1.00.2 AGN, Sy2 6.8 2884
Detected as a persistent source in the 20-100 keV band.
IGR J16056-6110 241.464 -61.195 3.88 0.70.1 1.10.2 AGN, Sy1.5 6.5 2839
Detected as a persistent source in the 20-100 keV band.
IGR J16058-7253 241.47 -72.9 3.59 1.10.2 0.70.3 AGN, pair, Sy2, Sy2? 7.1 1242
Detected as a persistent source in the 18-60 keV band.
IGR J16078-2521 242.009 -25.364 4.11 0.4 0.5 ? YY 6.1 811
Detected in a 2.3 day outburst from MJD=55412.7.
IGR J16119-6036 242.964 -60.631 1.89 1.50.1 1.50.2 AGN, Sy1.5 14.6 2942
Detected as a persistent source in the 20-100 keV band.
IGR J16120-3543 242.974 -35.754 4.69 0.40.2 0.60.3 ? Y 5.3 1565
Detected in a 127.3 day outburst from MJD=52911.9.
4U 1608-522 243.179 -52.423 0.27 18.20.1 13.20.1 LMXB, B, A, T Y 266.8 4640
Detected in a 1969.1 day outburst from MJD=53438.6.
Abell 2163 243.965 -6.12 3.79 0.90.2 0.5 Cluster 6.7 1021
Detected as a persistent source in the 18-60 keV band.
IGR J16167-4957 244.157 -49.979 1.23 2.10.1 1.00.1 CV, IP 24.3 4798
Detected as a persistent source in the 17-30 keV band.
IGR J16173-5023 244.314 -50.386 2.71 0.80.1 0.70.1 CV? 9.7 4818
Detected as a persistent source in the 20-40 keV band.
PSR J1617-5055 244.372 -50.92 2.49 0.80.1 1.20.1 PSR 10.7 4746
Detected as a persistent source in the 20-100 keV band.
IGR J16181-5407 244.533 -54.103 4.61 0.50.1 0.40.1 ? 5.4 4379
Detected as a persistent source in the 18-60 keV band.
IGR J16185-5928 244.61 -59.479 2.87 0.70.1 1.10.2 AGN, NLS1 9.1 3150
Detected as a persistent source in the 18-60 keV band.
AX J161929-4945 244.884 -49.742 1.19 2.00.1 1.40.1 HMXB?, SFXT? 25.2 4828
     IGR J16195-4945 Detected as a persistent source in the 18-60 keV band.
IGR J16194-2810 244.889 -28.128 2.25 1.90.2 1.30.3 LMXB, Symb 12.0 1027
Detected as a persistent source in the 20-100 keV band.
Sco X-1 244.979 -15.64 0.16 712.80.1 22.60.2 LMXB, Z, M 8052.6 1776
     4U 1617-15 Detected as a persistent source in the 20-40 keV band.
IGR J16207-5129 245.193 -51.502 0.80 3.20.1 2.30.1 HMXB, Sg 41.8 4579
Detected as a persistent source in the 18-60 keV band.
IGR J16226-2759 245.641 -27.995 4.54 0.4 0.5 ? YY 5.5 1095
Detected in a 3.3 day outburst from MJD=53772.7. Flags: WARN
IGR J16246-4556 246.091 -45.923 4.61 0.40.1 0.3 ? Y 5.4 4713
Detected in a 1969.2 day outburst from MJD=53044.7.
SWIFT J1626.6-5156 246.651 -51.943 1.62 0.40.1 0.50.1 HMXB, Be, T Y 17.5 4488
Detected in a 127.8 day outburst from MJD=53660.6.
4U1624-490 247.012 -49.199 0.54 3.90.1 0.50.1 LMXB, D 72.1 4860
Detected as a persistent source in the 17-30 keV band.
IGR J16283-4838 247.045 -48.649 1.32 1.00.1 0.60.1 HMXB, Sg Y 22.3 4711
Detected in a 14.3 day outburst from MJD=54154.9.
Mrk 1498 247.053 51.749 5.14 2.00.6 3.81.1 AGN, Sy1.9 4.8 160
     SWIFT J1628.1+5145 Detected as a persistent source in the 20-100 keV band.
IGR J16287-5021 247.112 -50.378 2.62 0.60.1 0.50.1 LMXB 10.1 4591
Detected as a persistent source in the 17-30 keV band.
IGR J16293-4603 247.304 -46.047 4.39 0.30.1 0.40.1 LMXB, Symb Y 5.7 4792
Detected in a 4.8 day outburst from MJD=53433.1.
SWIFT J1630.5+3925 247.663 39.38 4.39 1.10.2 0.8 AGN, Sy2 5.7 761
Detected as a persistent source in the 20-40 keV band.
IGR J16316-4028 247.9 -40.467 4.46 0.30.1 0.60.2 ? Y 5.6 4025
Detected in a 1141.8 day outburst from MJD=54363.4.
IGR J16318-4848 247.952 -48.817 0.25 26.40.1 13.80.1 HMXB, Be, Sg 326.0 4617
Detected as a persistent source in the 18-60 keV band.
AX J1631.9-4752 248.008 -47.874 0.29 19.40.1 6.60.1 HMXB, XP, Sg 227.4 4543
     IGR J16320-4751 Detected as a persistent source in the 20-40 keV band.
4U 1626-67 248.07 -67.462 0.37 20.30.2 2.80.3 LMXB, XP 133.0 1440
Detected as a persistent source in the 17-30 keV band.
IGR J16328-4726 248.158 -47.395 1.24 1.70.1 1.20.1 HMXB, SFXT 23.9 4541
Detected as a persistent source in the 18-60 keV band.
IGR J16327-4940 248.172 -49.666 5.04 0.2 0.60.1 ? Y 4.9 4824
Detected in a 0.9 day outburst from MJD=53435.3.
4U 1630-47 248.502 -47.394 0.22 20.60.1 19.10.1 LMXB, BHC, D, T Y 476.3 4520
Detected in a 61.6 day outburst from MJD=52848.1.
IGR J16351-5806 248.805 -58.08 2.17 1.30.1 1.50.2 AGN, Sy2 12.5 3335
Detected as a persistent source in the 20-100 keV band.
IGR J16358-4726 248.974 -47.428 0.76 1.00.1 0.90.1 LMXB, Symb, T Y 44.5 4471
Detected in a 10.0 day outburst from MJD=52716.8.
IGR J16363-2243 249.108 -22.797 4.90 0.40.2 0.4 ? Y 5.1 1684
Detected in a 1616.7 day outburst from MJD=53829.9.
IGR J16374-5043 249.306 -50.725 2.39 0.40.1 0.50.1 HMXB?, SFXT? Y 11.2 4562
Detected in a 0.5 day outburst from MJD=55430.0.
IGR J16377-6423 249.576 -64.352 2.49 1.40.2 0.50.3 Cluster 10.7 1717
Detected as a persistent source in the 17-30 keV band.
IGR J16385-2057 249.63 -20.924 3.84 0.80.1 0.70.2 AGN, NLS1 6.6 1820
Detected as a persistent source in the 20-100 keV band.
IGR J16388+3557 249.708 35.959 4.95 0.40.2 0.7 ? Y 5.0 881
Detected in a 0.6 day outburst from MJD=53574.6.
AX J163904-4642 249.773 -46.704 0.52 5.90.1 0.80.1 HMXB, XP 77.2 4896
     IGR J16393-4643 Detected as a persistent source in the 17-30 keV band.
4U 1636-536 250.231 -53.751 0.26 25.40.1 14.10.2 LMXB, B, A, T 298.3 4108
Detected as a persistent source in the 18-60 keV band.
IGR J16413-4046 250.331 -40.794 2.87 0.80.1 0.90.2 AGN? 9.1 4927
Detected as a persistent source in the 20-100 keV band.
IGR J16418-4532 250.462 -45.541 0.66 4.80.1 1.30.1 HMXB, XP, SFXT? 54.5 4734
Detected as a persistent source in the 20-40 keV band.
IGR J16426+6536 250.767 65.548 5.14 0.3 0.5 AGN, NLS1 Y 4.8 1618
Detected in a 0.7 day outburst from MJD=53178.1.
IGR J16447-5138 251.178 -51.649 4.95 0.20.1 0.40.1 ? Y 5.0 4092
Detected in a 35.7 day outburst from MJD=54141.5.
GX 340+0 251.449 -45.611 0.22 30.20.1 1.80.1 LMXB, Z 521.5 4835
Detected as a persistent source in the 17-30 keV band.
IGR J16460+0849 251.488 8.818 4.78 0.6 1.0 ? YY 5.2 451
Detected in a 356.6 day outburst from MJD=52919.6.
IGR J16465-4507 251.648 -45.118 1.59 1.50.1 0.90.1 HMXB, XP, SFXT 17.9 4869
Detected as a persistent source in the 17-30 keV band.
IGR J16476-3135 251.889 -31.557 3.56 0.2 0.70.2 ? 7.2 4238
Detected as a persistent source in the 30-60 keV band.
IGR J16479-4514 252.027 -45.202 0.71 4.00.1 2.10.1 HMXB, SFXT 48.8 4871
Detected as a persistent source in the 18-60 keV band.
IGR J16482-3036 252.062 -30.585 1.30 1.90.1 2.30.2 AGN, Sy1 22.6 3931
Detected as a persistent source in the 20-100 keV band.
IGR J16482-2959 252.145 -30.019 4.25 0.30.1 0.60.2 ? Y 5.9 3860
Detected in a 263.9 day outburst from MJD=54344.1.
IGR J16493-4348 252.362 -43.819 1.12 2.30.1 1.50.1 HMXB, Sg 27.2 5048
Detected as a persistent source in the 18-60 keV band.
IGR J16500-3307 252.483 -33.117 1.65 1.70.1 0.70.2 CV, IP 17.1 4593
     RX J164955.1-330713 Detected as a persistent source in the 18-60 keV band.
SWIFT J1650.5+0434 252.647 4.595 4.78 1.10.2 0.9 AGN, Sy2 5.2 588
     NGC 6230 Detected as a persistent source in the 20-100 keV band.
ESO 138-1 252.833 -59.234 2.33 1.40.1 1.50.2 AGN, Sy2 11.5 2527
     ESO 138-G001 Detected as a persistent source in the 18-60 keV band. Flags: BLEND
IGR J16523-3854 253.07 -38.924 4.32 0.2 0.3 ? Y 5.8 5732
Detected in a 4.8 day outburst from MJD=55089.2. Flags: WARN
XTE J1652-453 253.085 -45.344 0.52 1.50.1 1.00.1 LMXB, BHC?, T YY 76.0 4869
Detected in a 24.6 day outburst from MJD=55082.4.
IGR J16524-2352 253.122 -23.875 3.84 0.30.1 0.80.2 ? 6.6 3276
Detected as a persistent source in the 30-60 keV band.
NGC 6221 253.194 -59.216 2.33 1.40.1 1.50.2 AGN, Sy2 11.5 2527
Detected as a persistent source in the 18-60 keV band. Flags: BLEND
NGC 6240 253.246 2.4 1.76 3.00.2 3.90.4 AGN, Sy2, Liner 15.9 664
Detected as a persistent source in the 20-100 keV band.
Mrk 501 253.468 39.76 1.49 2.90.2 2.20.3 AGN, BL Lac Y 19.3 870
Detected in a 1902.4 day outburst from MJD=53322.2.
GRO J1655-40 253.501 -39.846 0.25 8.30.1 10.50.1 LMXB, BH, M, T Y 324.3 5728
Detected in a 8.3 day outburst from MJD=53434.3.
IGR J16547-1916 253.682 -19.275 2.44 1.20.1 0.50.2 CV, IP 10.9 3259
     RXS J165443.5-191620 Detected as a persistent source in the 18-60 keV band.
IGR J16560-4958 253.989 -49.967 3.59 0.70.1 0.60.1 AGN? 7.1 4295
Detected as a persistent source in the 17-30 keV band.
IGR J16558-5203 254.024 -52.061 1.40 1.70.1 1.90.2 AGN, Sy1.2 20.7 3605
Detected as a persistent source in the 18-60 keV band.
SWIFT J1656.3-3302 254.07 -33.037 1.34 0.90.1 1.90.1 AGN, QSO, Blazar Y 21.8 5422
Detected in a 1960.9 day outburst from MJD=53158.5.
IGR J16565-1607 254.117 -16.12 3.46 0.60.2 1.20.2 ? 7.4 2521
Detected as a persistent source in the 30-60 keV band.
Her X-1 254.458 35.342 0.20 119.40.2 21.80.3 LMXB, XP 693.9 947
     4U 1656+35 Detected as a persistent source in the 20-40 keV band.
MAXI J1659-152 254.761 -15.256 0.25 10.00.1 7.40.2 LMXB, BHC, T Y 317.9 2475
Detected in a 29.3 day outburst from MJD=55463.8.
AX J1700.2-4220 255.075 -42.34 1.24 2.10.1 1.70.1 HMXB 24.0 4734
Detected as a persistent source in the 18-60 keV band.
OAO 1657-415 255.204 -41.656 0.20 70.80.1 38.30.1 HMXB, XP 823.5 5253
Detected as a persistent source in the 18-60 keV band.
IGR J17008-6425 255.204 -64.425 5.14 0.4 1.10.3 ? Y 4.8 1503
Detected in a 11.9 day outburst from MJD=53222.9. Flags: WARN
XTE J1701-462 255.244 -46.186 0.37 3.00.1 0.90.1 LMXB, B, T Y 137.9 4327
Detected in a 455.2 day outburst from MJD=53760.6.
IGR J17009+3559 255.264 36.002 3.84 1.10.2 0.6 AGN, XBONG 6.6 868
Detected as a persistent source in the 17-30 keV band.
IGR J17014-4306 255.337 -43.092 2.90 0.80.1 0.60.1 CV, IP? 9.0 4798
Detected as a persistent source in the 17-30 keV band.
XTE J1701-407 255.435 -40.858 0.54 3.10.1 3.00.2 LMXB Y 71.4 4338
Detected in a 788.0 day outburst from MJD=54638.4.
GX 339-4 255.706 -48.79 0.19 69.70.1 78.00.2 LMXB, BH, M, T Y 1255.1 4063
     4U 1659-48 Detected in a 73.5 day outburst from MJD=55230.3.
4U 1700-377 255.987 -37.844 0.17 203.70.1 122.70.1 HMXB, Sg 2517.3 7499
Detected as a persistent source in the 18-60 keV band.
IGR J17044-1844 256.089 -18.735 3.71 0.70.1 0.70.2 ? 6.9 3995
Detected as a persistent source in the 30-60 keV band.
GX 349+2 256.435 -36.423 0.20 44.00.1 1.00.1 LMXB, Z 827.7 7188
     4U 1702-36 Detected as a persistent source in the 17-30 keV band.
IGR J17063-7338 256.493 -73.607 5.24<