ACCEPTED FORPUBLICATION IN THE ASTROPHYSICALJOURNAL

THE 37-MONTH MAXI/GSC SOURCE CATALOG IN THE HIGH GALACTIC-LATITUDE SKY

KAZUO HIROI,1 YOSHIHIRO UEDA,1 MASAAKI HAYASHIDA ,1 MEGUMI SHIDATSU,1 RYOSUKE SATO,1 TAIKI KAWAMURO ,1 MUTSUMISUGIZAKI ,2 SATOSHI NAKAHIRA ,3 MOTOKO SERINO,2 NOBUYUKI KAWAI ,4 MASARU MATSUOKA,2,3 TATEHIRO M IHARA ,2 M IKIO

MORII,4 MOTOKI NAKAJIMA ,5 HITOSHI NEGORO,6 TAKANORI SAKAMOTO ,7 HIROSHI TOMIDA ,3 YOHKO TSUBOI,8 HIROSHITSUNEMI,9 SHIRO UENO,3 KAZUTAKA YAMAOKA ,10 ATSUMASA YOSHIDA,7 MASATO ASADA,6 SATOSHI EGUCHI,11 TAKANORIHANAYAMA ,12 MASAYA HIGA ,8 KAZUTO ISHIKAWA ,4 MASAKI ISHIKAWA ,13 NAOKI ISOBE,14 M ITSUHIRO KOHAMA ,15 MASASHI

K IMURA ,3 KUMIKO MORIHANA ,2 YUJIN E. NAKAGAWA ,14 YUKI NAKANO ,7 YASUNORI NISHIMURA ,12 YUJI OGAWA ,12 MASAYUKISASAKI ,9 JURI SUGIMOTO,2 TOSHIHIRO TAKAGI ,2 RYUICHI USUI,4 TAKAYUKI YAMAMOTO ,2 MAKOTO YAMAUCHI ,12 AND KOSHIRO

YOSHIDOME12

Accepted on August 17, 2012

ABSTRACTWe present the catalog of high Galactic-latitude (|b| > 10◦) X-ray sources detected in the first 37-month

data of Monitor of All-sky X-ray Image (MAXI) / Gas Slit Camera (GSC). To achieve the best sensitivity,we develop a background model of the GSC that well reproduces the data based on the detailed on-boardcalibration. Source detection is performed through image fit with the Poisson likelihood algorithm. The catalogcontains 500 objects detected in the 4–10 keV band with significance ofsD,4−10keV≥ 7. The limiting sensitivityis ≈ 7.5×10−12 ergs cm−2 s−1 (≈ 0.6 mCrab) in the 4–10 keV band for 50% of the survey area, which is thehighest ever achieved as an all-sky survey mission covering this energy band. We summarize the statisticalproperties of the catalog and results from cross matching with the Swift/BAT 70-month catalog, the meta-catalog of X-ray detected clusters of galaxies, and the MAXI/GSC 7-month catalog. Our catalog lists thesource name (2MAXI), position and its error, detection significances and fluxes in the 4–10 keV and 3–4 keVbands, their hardness ratio, and basic information of the likely counterpart available for 296 sources.

Subject headings:catalogs — surveys — galaxies: active — X-rays: galaxies

1. INTRODUCTION

Monitor of All-sky X-ray Image (MAXI: Matsuoka et al.2009) is the first astronomical mission performed on the Inter-national Space Station (ISS). The main instrument of MAXIis the Gas Slit Camera (GSC: Mihara et al. 2011; Sugizaki et

Electronic address: hiroi@kusastro.kyoto-u.ac.jp1 Department of Astronomy, Kyoto University, Oiwake-cho, Sakyo-ku,

Kyoto 606-85022 MAXI team, Institute of Physical and Chemical Research (RIKEN), 2-1

Hirosawa, Wako, Saitama 351-01983 ISS Science Project Office, Institute of Space and Astronautical Sci-

ence (ISAS), Japan Aerospace Exploration Agency (JAXA), 2-1-1 Sengen,Tsukuba, Ibaraki 305-8505

4 Department of Physics, Tokyo Institute of Technology, 2-12-1Ookayama, Meguro-ku, Tokyo 152-8551

5 School of Dentistry at Matsudo, Nihon University, 2-870-1 Sakaecho-nishi, Matsudo, Chiba 101-8308

6 Department of Physics, Nihon University, 1-8-14 Kanda-Surugadai,Chiyoda-ku, Tokyo 101-8308

7 Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo-ku, Sagamihara, Kanagawa 252-5258

8 Department of Physics, Chuo University, 1-13-27 Kasuga, Bunkyo-ku,Tokyo 112-8551

9 Department of Earth and Space Science, Osaka University, 1-1Machikaneyama, Toyonaka, Osaka 560-0043

10 Astro-H Project team, Institute of Space and Astronautical Science(ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshino-dai,Chuo-ku, Sagamihara, Kanagawa 252-5210

11 National Astronomical Observatory of Japan, 2-21-1, Osawa, MitakaCity, Tokyo 181-8588

12 Department of Applied Physics, University of Miyazaki, 1-1 GakuenKibanadai-nishi, Miyazaki, Miyazaki 889-2192

13 School of Physical Science, Space and Astronautical Science, The grad-uate University for Advanced Studies (Sokendai), Yoshinodai 3-1-1, Chuo-ku, Sagamihara, Kanagawa 252-5210

14 Institute of Space and Astronautical Science (ISAS), Japan AerospaceExploration Agency (JAXA), 3-1-1 Yoshino-dai, Chuo-ku, Sagamihara,Kanagawa 252-5210

15 Mitsubishi Space Software Co., Ltd., WTC Bldg.2-4-1 Hamamatsu-cho, Minato-ku, Tokyo 105-6132

al. 2011), which covers the 2–30 keV band. Since its first lighton 2009 August 15, MAXI/GSC has been monitoring nearlythe entire sky every 92 minute with two instantaneous field-of-views of 1.5◦ × 160◦ that rotate according to the orbitalmotion of the ISS. The survey with MAXI/GSC is expectedto achieve the best sensitivity so far as an all-sky monitor inthe 2–10 keV band, which is complementary to other all-skysurveys conducted below 2 keV (ROSAT: Voges et al. 1999,2000) and above 10 keV (INTEGRAL: Bird et al. 2007; Beck-mann et al. 2006, 2009; Krivonos et al. 2007; Bird et al. 2010,Swift: Tueller et al. 2008, 2010; Cusumano et al. 2010; Baum-gartner et al. 2010, 2012). This bandpass is the most suitableto survey X-ray populations with intrinsically soft X-ray spec-tra with little bias for obscuration.

Utilizing the first 7-month data of MAXI/GSC in the 4–10keV band, Hiroi et al. (2011) produced the first X-ray sourcecatalog in the high Galactic latitude sky (|b| > 10◦). It con-sists of 143 objects above the 7σ significance level with a lim-iting sensitivity of∼ 1.5×10−11 ergs cm−2 s−1 (1.2 mCrab) inthe 4–10 keV band. Though limited in sample size, the firstMAXI/GSC catalog has an advantage that the identificationcompleteness is very high (> 99%). Utilizing the AGN sam-ple of this catalog, Ueda et al. (2011) calculate a new AGN X-ray luminosity function in the local universe and solve the dis-crepancy of the AGN space density previously reported fromdifferent missions.

In this paper, we present the second MAXI/GSC source cat-alog at|b| > 10◦, constructed from the data in the 4–10 keVband observed for 37 months between 2009 September and2012 October. The significantly increased photon statisticsenables us to achieve much better sensitivities than those ofthe 7-month catalog. We also analyze the data in the 3–4 keVband to derive the hardness ratio of the detected sources. Sec-tion 2 describes the data reduction and filtering. In section 3,we report the analysis procedures to detect source candidatesand determine their fluxes and positions. Section 4 presents

2 K. Hiroi

the source catalog, its basic properties, the results from cross-matching with other X-ray source catalogs, and the logN-logSrelation. We summarize our conclusion in section 5.

2. DATA REDUCTION

The second MAXI/GSC catalog is based on the 37-monthdata obtained from 2009 September 23 to 2012 October 15.The data reduction procedure is essentially the same as usedto produce the MAXI/GSC 7-month catalog in Hiroi et al.(2011). We start from processed event files provided by theMAXI team, which have columns of the photon arrival time(TIME), energy (Pulse-height Invariant = PI), and sky posi-tion (R.A. and Decl.). In the processing, two pulse-height val-ues read out from both ends of a carbon-anode wire were con-verted into the PI and an one-dimensional detector positionalong the anode wire on the basis of the ground and in-flightcalibration (Mihara et al. 2011; Sugizaki et al. 2011). The skyposition of the incident X-ray photon is then calculated by re-ferring to the ISS attitude at the photon arrival time. For thedata reduction, we use HEAsoft (version 6.12) and MXSOFT,an original MAXI software package developed by the MAXIteam.

To detect sources, the data in the 4–10 keV band are utilizedfor consistency with our previous work (Hiroi et al. 2011),where high signal-to-noise ratio is achievable due to the highquantum efficiency and low background rate of the detector(Mihara et al. 2011). We basically use all available data of alltwelve GSC counters operated with high voltage levels of both1650 V and 1550 V, except for those taken with GSC_3 after2010 June 22, in which the background-veto counters werenot available. Unlike Hiroi et al. (2011), the photon events ofanode #1 and #2 are also available in this study, thanks to theimprovement of the instrument response calibration. We dis-card the data acquired in unusual conditions where the back-ground reproducibility of the GSC is found to be poor: (1) theinitial operation phase from 2009 September 1 to 22, (2) thephase from 2012 October 16 to 31 when the Dragon space-craft was attached to the ISS, (3) those during the docking orundocking operation of the Soyuz spacecraft, (4) those soonafter the reboot of the electrical system of MAXI, (5) thoseduring large solar flares16, and (6) those when the telemetrydata were missed due to the network trouble between the ISSand the ground base station.

The following data selection criteria are applied in event se-lection. To exclude data of the GSC with high particle back-ground, we select the events when the latitude of the ISS isbetween−40◦ and 40◦ and those detected in an inner regionof each camera with the incident angle|ϕ| ≤ 38◦ (for defini-tion of ϕ, see Mihara et al. 2011). In our new analysis for the37-month catalog, we also properly take into account the ef-fects of the occultation of the GSC field-of-views by the spaceshuttle and the solar paddles of the ISS in a time dependentmanner; the occulted regions in the detector coordinate de-fined byϕ at a given time, if any, are excluded with a marginof 5◦ on the basis of monitoring information of the relativegeometry between MAXI and the ISS.

The left panel of figure 1 displays the effective exposuremap for the 37-month MAXI/GSC data in the Galactic co-ordinates projected with the Hammer-Aitoff algorithm. Theeffective-exposure distribution is shown in the right panel.

16 From the light curves with 16-sec bin size in the 4–10 keV band, wefilter out time regions when the count rates exceeded 25, 35, 40, and 30 cnts/sfor GSC_3, GSC_8, GSC_B, and the other cameras, respectively, with mar-gins of 32 sec each before and after these periods.

The map is produced by the latest version of the MAXI sim-ulator maxisim (Eguchi et al. 2009) for uniformly extendedemission, where theϕ dependence of the slit area, the colli-mator field-of-view, and the detector efficiency as a functionof an incident X-ray energy (see Mihara et al. 2011; Sugizakiet al. 2011) are correctly taken into account. Referring to theorbit and attitude of the ISS,maxisim is able to generate sim-ulated photon events from any input X-ray sources by reflect-ing the latest responses of the GSC. The stripe patterns foundin the map are caused by an incident-angle dependence of theeffective area of the GSC aimed at each pointing direction, thedifferent duty cycle among the twelve GSC counters, and theprecession of scanning motion of the field-of-views coupledwith that of the ISS orbit. The two darkest, annular-like struc-tures at the top-left and bottom-right of the map correspondto the regions with the longest exposure near the poles aroundthe rotation axis of the ISS orbit.

3. ANALYSIS

3.1. Background Reproduction

For source detection, we perform image analysis of the pro-jected sky image from the whole MAXI/GSC data, as detailedin section 3.2. Basically, we search for excess signals overthe profile of the background, which consists of the non-X-raybackground (NXB) and the cosmic X-ray background (CXB).Thus, to achieve the best sensitivity, it is critical to modelthe background image with the least systematic errors thatenables us to detect even the faintest sources as statisticallysignificant signals. The NXB of the GSC shows complex be-haviors (Sugizaki et al. 2011). The rate of the NXB is highlyvariable, depending on the environment such as conditions ofother spacecrafts attached to the ISS, the orbital position andattitude of the ISS.

We thus construct a background model of MAXI/GSCbased on the detailed calibration of the on-board data as de-scribed below. Here we do not distinguish the NXB from theCXB, only treating their sum, since it is not easy to separatethe two components from the observed data. This is mainlydue to the fact that the MAXI/GSC field-of-views always lookat the sky and seldom look at the earth. For this purpose, weanalyze the on-board data that can be regarded as blank sky,by excluding regions around the 70 brightest sources at highGalactic latitudes listed in the 7-month MAXI/GSC catalog17

(Hiroi et al. 2011) and that of the Galactic-center region with|l |< 50◦ and|b|< 10◦. The same screening described in sec-tion 2 is adopted for event extraction. To avoid complexity inexposure correction, we discard any data taken when a partof the field-of-view was occulted by the space shuttle and thesolar paddles of the ISS in each camera.

We first investigate the long-term variability of the back-ground rate. The top panel of figure 2 displays a one-dayaveraged background rate as a function of time, derived fromthe data in the 4–10 keV band taken with the GSC_4 counter.It is clearly seen that the MAXI/GSC background rate hastwo separate levels of 3–4 cnts/s and 2–2.5 cnts/s in this cam-era. We find that this long-term variability of the backgroundis strongly correlated with whether the Soyuz spacecraft wasdocked or undocked to the ISS. Since Soyuz has an altimetercontaining a radioactive source, the MAXI/GSC backgroundrate is largely increased when it is attached to the nearest ISS

17 We confirm that when our new 37-month catalog is used to exclude evenfainter sources in this process, the resultant background profile in the detectorcoordinate is little (< 1%) changed.

The 37-Month MAXI/GSC Source Catalog in the High Galactic-Latitude Sky 3

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FIG. 1.— (Left) Effective exposure map for the 37-month MAXI/GSC data in the Galactic coordinates projected with the Hammer-Aitoff algorithm. The unitsare cm2 s. The entire sky is divided into 12288 pixels with a size of 1.83◦×1.83◦. (Right) Histogram of the effective exposure presented in the left panel.

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FIG. 2.— (Top) History of the background rate in the 4–10 keV band ob-served with GSC_4 in a one-day bin (real data). The attached error is 1σ.The dot-dashed lines indicate the boundaries of the phases. The dock/undockstatus of the Soyuz spacecraft causes the drastic change of the daily back-ground rate. (Middle) Same as the top panel but produced from simulations.(Bottom) The ratio of the real background rate to the simulated one. Thesimulated background data are well consistent with the real ones with an rmsscatter of∼1%.

port to MAXI, and vice versa. Furthermore, it is found thatan increment of the background rate depends on the individ-ual Soyuz spacecraft docked at that time. The difference ofhigh-voltage level between 1650 V and 1550 V also affectsthe background rate. Thus, we divide the 37-month periodinto 9 different phases according to the existence of Soyuzand the high-voltage level of the GSC, and create the back-ground model separately in each phase.

Next, the short-term variability of the NXB on a time scaleless than one day is examined. In the previous study (Hi-roi et al. 2011), we considered the dependence of the back-ground rate on the cut-off rigidity (COR) parameter, which isdetermined solely by the orbital position of the ISS. The cor-relation of the NXB with COR is known to be not so good,however. Alternatively, we have found that the instantaneousbackground rate is well estimated from the so-called “VC”count, representing the rate of events simultaneously detectedby the carbon-anode cells and the tungsten-anode cells forparticle veto, available as a monitor count in the house keep-ing data of the GSC (Mihara et al. 2011; Sugizaki et al. 2011).The reason why the VC works as a good monitor of the NXBis that high energy particles hitting the GSC counter shouldbe detected by both the inner (carbon) and outer (veto) cells,unlike X-ray events. Figure 3 plots examples of the correla-tion between the VC and background rates in the 4–10 keVband for GSC_4 in two different phases. The blue circles and

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FIG. 3.— Correlation between the 4–10 keV background rate and the VCcount rate for GSC_4. The red squares (for visuality, slightly shifted) andsolid curve represent the data points and the best-fit model of a third-orderpolynomial, respectively, when Soyuz was undocked, while the blue circlesand dotted curve show them when it was docked from 2009 December 22 to2010 May 11 (MJD = 55187–55327).

red squares correspond to the data obtained when Soyuz wasdocked to the ISS port and undocked, respectively. The errorbars represent 1σ standard deviation in the background rateincluding the statistical fluctuation. A tight correlation is con-firmed in each phase. The blue-dotted and red-solid lines rep-resent the best-fit models of a third-order polynomial to thesecorrelations.

We develop a background-event generator of the GSC,which makes use of the framework of the MAXI simulatormaxisim. By using the correlation between the VC and back-ground rates determined for each camera and phase, it gen-erates simulated background events in time series with theinstantaneous rate calculated from the light curve of the VCcounts. Their energies and positions on the detector are ran-domly assigned according to their distributions derived fromthe real background data, which also depend on the VC count.We produce ten times more events than the real data to reducethe statistical error in the model. The simulated backgrounddata are then processed in the same way as for the observeddata. The middle panel of figure 2 plots the same as thatshown in the top panel of figure 2 but based on the simulatedbackground data. We confirm that the background light curveis well reproduced by our model with an rms scatter of∼1%,as shown in the bottom panel of figure 2.

3.2. Image Analysis

In this section, we describe the details of our image analy-sis method to produce the X-ray catalog from the MAXI/GSC

4 K. Hiroi

data. The procedure consists of two major stages: a detec-tion of source candidates from smoothed images, and a mea-surement of fluxes and positions for the source candidates bymaximum-likelihood image fitting. For the image analysis,we use display45 version 2.04, which is a command-driven,interactive histogram-browsing program based on CERN li-braries.

(1) MAKING PARTED IMAGES

Both for the real and simulated background data, we cre-ate images from the event lists after applying the selectioncriteria described in section 2. Like a standard image analy-sis, we produce a tangentially-projected image within a smallregion in the sky coordinates (X, Y) defined by three param-eters: the reference point in right ascension (R.A.) and decli-nation (Decl.) corresponding to the center of the image andthe position angle of the+Y-axis to the north, which is set tobe zero in our analysis. The images are simply stored in unitsof counts without exposure correction.

The entire sky is divided into 768 square regions with asize of 7.3◦ × 7.3◦, whose centers are determined by usingthe HEALPix software package (Górski et al. 2005) so thateach region has the same solid angle. Using the central posi-tion of each region as the sky-reference point, we then make768 tangentially-projected images with a size of 14◦×14◦ byreferring to the columns of sky position (R.A., Decl.) in theevent lists. In order not to miss any sources located near theboundaries, the images have overlapping area of> 3◦ on bothsides with neighboring ones. The bin size is set to 0.1◦, whichis sufficiently finer than the typical size of the point spreadfunction (PSF) of MAXI/GSC (FWHM∼ 1.5◦).

(2) SEARCHING FOR SOURCE CANDIDATES

To pick up source candidates from each image, we create asignificance map in the following manner. Firstly, we makenet-source maps by subtracting the simulated backgroundfrom the real data. Then, both the real data and net-sourcemap are smoothed with a circle ofr = 1◦ with a constantweight of unity (i.e., simple integration). We finally calculatethe significance of excess signals as “net-source/

√real data”

at each point, yielding the significance map.In this step, a correct estimate of the background level is es-

sential. Although the reproductivity of the background modeldescribed in section 3.1 is fairly good for blank sky, we findthat it is sometimes better to re-normalize the absolute levelof the background map from the observed data themselves,in particular when additional diffuse background other thanthe CXB such as Galactic diffuse emission exists in the im-age. Thus, the background level used to make a final source-candidate list is determined by iteration in the following way.At first, assuming a conservative background level higher thanthe nominal value by a factor of 1.1, we create a tentativesignificance map. We then search for the peak showing thehighest significance in the map if it is larger than 15σ. Next,after masking out the circular region around the peak of thebright source with a radius ofr = 3◦, the whole size of thePSF, we compare the averaged counts in the real and the sim-ulated background maps, whose ratio determines an improvedbackground level. By repeating these procedures of findingand masking out brightest sources until the significance of anewly detected peak becomes< 15σ, we finally derive themost reasonable background level in each image. The correc-tion from the nominal level is typically less than 3%, and thus

possible systematic errors in the positional dependence of thebackground do not affect the flux measurements of sources.

Once the background level is determined, we make the mostreliable significance map, from which peaks above 5σ arepicked up as source candidates. Those located near the bound-aries of the image (|X| > 5.5◦ or |Y| > 5.5◦) are discardedbecause they are located closer to the center of a neighboringimage that can detect them with better conditions. The issueof source confusion that two nearby sources may be detectedas a single source candidate will be overcome in a later pro-cedure (the 6th step).

(3) MERGING SOURCE-CANDIDATE LIST

Merging the source-candidate lists obtained from the wholesky yields 1308 sources in total above 5σ at |b| > 10◦. Thislist includes duplicate sources detected in multiple images,however, which are located at the overlapping regions nearthe boundaries. We treat any pair of sources whose positionsare within 1◦ as a single object; we adopt a source detected ata closer position to the image center and discard the other. Itis confirmed that the detection significances of the paired can-didates are consistent with each other within expected levels.Thus, we finally obtain a unique source-candidate list consist-ing of 615 objects above 5σ at |b|> 10◦.

(4) CONSTRUCTING MODELS OF POINT SPREADFUNCTION

For image analysis, we need to construct a model of the PSFfor each source candidate. Since the MAXI/GSC data usedin this study compose of multiple observations with differentconditions, it is difficult to model the PSF shape analytically.Hence, we utilize the MAXI simulatormaxisim (Eguchi etal. 2009) to produce the PSF model by inputting a point-likesource at the detected position. The simulation is performedwith exactly the same observational conditions (such as thetotal exposure) as for the real data, and hence the resultantPSF contains the expected number of counts from that sourcewith a given flux by fully taking into account the instrumentalresponses. The Crab Nebula-like spectrum18, a power law of aphoton index of 2.1 absorbed with a hydrogen column densityof NH = 2.6×1021 cm−2, and no flux variability are assumedfor simplicity. We confirm that the choice of the spectrum forthe PSF model does not affect the determination of the flux bythe image fitting because the energy dependence of the PSF isnot very large in the energy band of interest. To suppress thestatistical fluctuation in the PSF model, we generate a suffi-ciently large number of photons for each source candidate byassuming a flux of 50 mCrab. The simulated events of thePSF data are processed in the same way as for the real data,and are converted into images in the sky coordinates.

(5) DETERMINING FLUXES AND POSITIONS WITHIMAGE FIT

To determine the fluxes and positions of the source candi-dates, we perform image fitting to the real data with a modelconsisting of the background and PSF models, both producedby the simulations as described above. Here the fits to allof the source candidates and the background are performedsimultaneously in each image. The best-fit parameters aredetermined with the Poisson likelihood algorithm where the

18 The spectral parameters are adopted from the INTEGRAL General Ref-erence Catalog (ver. 35). http://www.isdc.unige.ch/integral/science/catalogue

The 37-Month MAXI/GSC Source Catalog in the High Galactic-Latitude Sky 5

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FIG. 4.— (Left) Example of a smoothed image of the real data. The image size is 14◦×14◦, whose center is located at (R.A., Decl.) = (253.125◦, 41.810◦).The best-fit background model obtained from image fitting is subtracted. The four cyan crosses represent the locations of detected sources withsD,4−10keV ≥ 7.(Right) Significance map of the same region. The contours display the significance levels of 5 (black), 7 (red), 10 (green), 20 (blue), 40 (yellow), 70(magenta),and 90(cyan), from outer to inner.

so-calledC statistics (Cash 1979) is minimized, defined as

C≡ 2∑i, j

{M(i, j) − D(i, j) lnM(i, j)}, (1)

whereD(i, j) andM(i, j) represent the data and model at theimage pixel (i, j), respectively. The parameter that gives aCvalue larger by unity than that of the best-fit with the otherfree parameters allowed to float corresponds to its 1σ error.The MINUIT package is utilized in the minimization. In thefitting, we change the bin width of an image from 0.1◦ to 0.2◦

for the fit to converge faster, and only treat the inner 11◦×11◦

region of the image for the calculation to ignore the influenceby sources located just outside the whole image with a size of14◦×14◦. For the PSF models of source candidates located inthe inner 11◦×11◦ region of the image, their normalizationsand positions are set to be free, as well as the overall back-ground level. The PSF normalization of each source gives itsflux corrected for exposure and the instrumental response inunits of “Crab” because we basically measure its total countsrelative to that would be observed from the Crab Nebula onwhich the PSF simulation is based. Since it is difficult to accu-rately determine the position of a source outside the 11◦×11◦

region whose PSF is distributed beyond the image boundary,we fix it at the location originally detected in the significancemap. It is found that in a few images containing very brightsources such as Sco X-1 and Cyg X-2, the background levelcannot be properly determined due to the incomplete repro-duction of the PSF shape. In such cases, we fix the back-ground level to the value obtained in the second step.

After the fitting, we calculate the detection significance inthe 4–10 keV (sD,4−10keV) for each source candidate, definedas

sD,4−10keV≡ (best-fit 4-10 keV flux)/(its 1σ statistical error).(2)

Here we use the MINOS negative error in the MINUIT pack-age as the flux error, although the positive and negative er-rors are consistent with each other in almost all cases becausethe number of source counts is always sufficiently high thatsymmetric errors are a reasonable approximation. We adoptsD,4−10keV ≥ 7 for the criterion of source detection, consider-ing the number of fake sources caused by the fluctuation ofbackground level (see section 4.2).

(6) ITERATION OF SOURCE SEARCH AND IMAGE FIT

Due to source confusion, multiple close sources can be de-tected as a single object. To salvage such sources located ina source crowded region as much as possible, we again per-form the source search in the second step but by adopting thebest-fit total model consisting of PSFs and the backgroundobtained in the previous step as a new background. Herewe adopt a more conservative detection criterion of 5.5σ thanin the first round to reduce the probability of fake detectionsaround the existing sources. This procedure gives us an addi-tional source-candidate list containing 135 objects above 5.5σat |b| > 10◦. The first and second source-candidate lists aremerged into one list. We then repeat the image fitting usingthe revised source-candidate list, and obtain the final list ofsources detected withsD,4−10keV≥ 7 in the 4–10 keV band.

(7) MEASUREMENT OF 3–4 KEV FLUX

To obtain spectral information, we also determine the 3–4keV fluxes of all sources in the final list created above. Theimages of real data, background model, and PSF models inthe 3–4 keV band are produced in the same way as for thosein the 4–10 keV band. We then perform image fitting to the3–4 keV band image using the source-candidate list obtainedin the 6th step. The source positions are fixed at those deter-mined by the image fit in the 4–10 keV band. Thus, we finallyderive the 3–4 keV fluxes and their errors for all the sourcesdetected in the 4–10 keV band. Using the 4–10 keV and 3–4keV fluxes, which are independently determined from the im-ages of the two energy bands, we calculate the hardness ratio(HR) defined as

HR =H − SH + S

, (3)

whereH andSrepresent the observed fluxes in the 4–10 keVand 3–4 keV bands, respectively. The error of the HR is cal-culated by simple propagation of those inH andS, both canbe regarded as symmetric errors.

4. CATALOG

4.1. Basic Properties

In this section, we present the second MAXI/GSC X-raysource catalog in the high Galactic latitude sky obtained fromthe 37-month all-sky survey data in the 4–10 keV band.

6 K. Hiroi

hpixID134(RA0, DEC0) = (253.125, 41.810), (L0, B0) = (66.208, 39.272)

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FIG. 5.— Projected images onto theX-axis (left) andY-axis (right) of the same region as shown in figure 4. The black points represent the real data with 1σPoisson errors. The two color lines display the best-fit models (red-solid: total, blue-dashed: only background).

It consists of 500 sources detected with a significance ofsD,4−10keV ≥ 7 at |b| > 10◦. Table 1 gives the catalog withcolumns of (1) source identification number, (2) MAXI sourcename based on the best-fit position in the final image fit (witha prefix of “2MAXI”), (3)-(4) best-fit position in the equa-torial coordinates in units of degree, (5)σstat: 1σ statisticalposition error in units of degree (the squared sum of those inthe X- and Y-directions). (6)sD,4−10keV: 4–10 keV detectionsignificance, (7)f4−10keV: observed 4–10 keV flux and its 1σerror in units of 10−12 ergs cm−2 s−1, (8) sD,3−4keV: 3–4 keVdetection significance, (9)f3−4keV: observed 3–4 keV flux andits 1σ error in units of 10−12 ergs cm−2 s−1, (10) HR: hard-ness ratio and its 1σ error, (11) counterpart name, (12)-(13)position of the counterpart (14) redshift, (15) type, (16) cross-matching flag, and (17) note.

Taking into account the MAXI/GSC response, we calculatethe dependences of the hardness ratio HR on spectral parame-ters and those of the conversion factors from an area-correctedcount rate (defined as that relative to the Crab one) into an en-ergy flux in the same energy band,C4−10 andC3−4. In thetop-left panel of figure 6, the hardness ratio is plotted as afunction of photon index with an unabsorbed power-law spec-trum, whereas in the top-right panel it is given as a functionof column density of an absorbed power-law spectrum with aphoton index of 1.8 at redshift of 0. In the middle and bottompanels, we also display the dependences of the conversion fac-tors on the same spectral parameters in the 4–10 keV and 3–4keV bands, respectively. The expected values of HR and con-version factors are HR=0.0745,C4−10 = 1.24 [10−11 ergs cm−2

s−1]/[mCrab],C3−4 =0.401 [10−11 ergs cm−2 s−1]/[mCrab] fora photon index of 1.8 with no absorption, and HR=0.000,C4−10 =1.21 [10−11 ergs cm−2 s−1]/[mCrab],C3−4 =0.398 [10−11

ergs cm−2 s−1]/[mCrab] for the Crab Nebula-like spectrum(see section 3.2 for its spectral parameters). The energy fluxeslisted in the catalog are all calculated by assuming the CrabNebula-like spectrum.

The correlation between the flux and the detection signifi-cance in the 4–10 keV band are plotted in figure 7. The de-tection significance,sD, can be approximated asSt/

√St+ Bt,

whereS and B are the count rates of the source and back-ground, respectively, andt is exposure. Thus, in the high fluxrange (sD ∼

√St), the detection significance is expected to

be proportional to (flux)1/2. In contrast, it is proportional to(flux)1 in the low flux range (sD ∼ S

√t/B). These trends

are confirmed in the figure. The limiting sensitivity withsD,4−10keV ≥ 7 (that of the faintest source detected) corre-sponds to∼ 5× 10−12 ergs cm−2 s−1 (∼ 0.4 mCrab) in the4–10 keV band.

4.2. Number of Spurious Sources

Since we conservatively adopt the detection threshold ofsD ≥ 7, fake detections by statistical fluctuation in photoncounts are expected to be negligible. However, the catalogmay contain a small fraction of spurious sources caused byremaining systematic errors in the background model. Tosimply estimate the number of such sources, we search for“negative” signals from the smoothed net-source maps pro-duced in the second step of section 3.2. This gives a “neg-ative” source-candidate list consisting of 50 objects below -7σ from the entire sky. Performing image fitting by addingnegative PSFs to the model, we find that the number of fi-nal “negative” detections withsD ≤ −7 becomes only 18% ofthat of spurious source candidates. The reduction is expectedbecause the shape of residual signals due to improper mod-eling of the background profile is very different from that ofthe PSF. Thus, we estimate that our catalog would include∼ 9 spurious detections, which are less than 2% of the totalsources. Note that if we instead adoptsD ≥ 6 as the detectioncriterion for the catalog, we find that the fraction of spuriousones becomes∼5% of the total, which is too high to be ac-cepted.

4.3. Cross Matching with Other X-ray Catalogs

Identification of X-ray sources with counterparts in otherwavelengths is very important for further scientific studies us-ing an X-ray catalog. The most critical information for thistask is the position accuracy. Figure 8 plots the correlationbetween the flux and position error of the MAXI sources.As noticed,σstat is roughly proportional to (sD,4−10keV)−1, asexpected from a simple statistical argument on the accu-racy of the centroid determination of the PSF with limitedphoton counts. A typical 1σ error becomesσstat ∼ 0.2◦ atσD,4−10keV = 7.

Considering the large positional uncertainties of MAXI,it is difficult to directly match them with those in opti-cal/infrared catalogs with large number densities. However,since the MAXI sources represent brightest X-ray popula-tions, a significant fraction of them are expected to be in-cluded by other X-ray catalogs at similar flux levels covering

The 37-Month MAXI/GSC Source Catalog in the High Galactic-Latitude Sky 7

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s−1]/[mCrab]. (Bottom) The same as above but in the 3–4 keV band. (Left) The parameter is the photon index of a power law with no absorption. (Right) Theparameter is the absorption column density for a power law with a photon index of 1.8.

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a wide sky area. Hence, as the first step of identification work,we cross-match our sources with two major X-ray catalogs todetermine the most likely counterparts: the Swift/BAT hardX-ray (14–195 keV) all-sky survey 70-month catalog (here-after, BAT70; Baumgartner et al. 2012) and the Meta-Catalogof X-Ray Detected Clusters of Galaxies (hereafter, MCXC;Piffaretti et al. 2011). The latter is based on the ROSAT all-sky survey and ROSAT serendipitous surveys performed inthe energy bands below∼2 keV. While BAT70 provides an X-ray sample including heavily obscured objects, MCXC com-plements the identification of galaxy clusters, which are hardto be detected above 10 keV due to their soft spectra.

The cross-matching of the MAXI sources with these cata-logs is carried out in the following way. We firstly search for

counterparts from the BAT70 catalog. Then, for those withoutBAT counterparts, we use the MCXC. Finally, we also per-form cross-matching with the first MAXI/GSC source cata-log (hereafter, GSC7; Hiroi et al. 2011). Basically, we refer tothe positions of the optical/infrared counterparts in these cat-alogs instead of the X-ray positions, except for a few sourcesin the first MAXI/GSC catalog that do not have unique opti-cal counterparts. As the position errors of the MAXI sources,we consider both statistical error (σstat) and systematic error(σsys) related to the instrument calibration and attitude deter-mination of MAXI. Since the two errors are independent ofeach other, we define the total 1σ position error (σposi) as theroot sum squares:

σposi≡√σ2

stat+σ2sys. (4)

In the matching process, we set the 1σ systematic erroras σsys = 0.05◦ on the basis of the previous work (Hiroiet al. 2011), and use an error circle with a radius ofr =2.5σposi, which corresponds to 95% confidence level in the2-dimensional space giving a typical increment in theC valueby 6.0. The position errors in the reference catalogs are ig-nored, since they are much smaller than those of the MAXIsources.

The cross-matching results are listed in columns (11)–(15)of table 1 for each source. The locations of the MAXI sourcesin the Galactic coordinates are plotted in figure 9. The num-bers of matched MAXI sources in a single or two reference

8 K. Hiroi

FIG. 9.— Locations of all the MAXI sources in the Galactic coordinates. The center is at (l ,b) = (0◦, 0◦). The radii of the circles are proportional to thelogarithm of the fluxes. Different colors correspond to different types: unidentified X-ray sources in BAT70 (black); galaxies (cyan); galaxy clusters (green);Seyfert galaxies, blazars (purple); CVs/Stars (magenta); X-ray binaries (red); confused sources (orange); sources without counterparts in BAT70 or MCXC(gray).

TABLE 2NUMBER OF MATCHED MAXI SOURCES.

Catalog name BAT70 MCXC GSC7 One catalog onlya

BAT70 185 (187)b 23 84 92MCXC ..... 123 (130)b 37 78GSC7 ..... ..... 114 (114)b 8

NOTE.— Numbers of MAXI sources matched with both catalogs are listed.aNumbers of MAXI sources matched only with one catalog given in the first column.bNumbers in parentheses represent those of total matched counterparts in each catalog.

TABLE 3CATEGORIES OF CATALOGED SOURCES.

Category Number of sources

unidentified 5galaxies 8

galaxy clusters 114Seyfert galaxies 100

blazars 15CVs/Stars 30

X-ray binaries 20confused 4

unmatched 204

catalogs in any combination from the three reference catalogsare summarized in table 2. We also show the total numbers ofcounterparts in each reference catalog with parentheses; herewe count more than one objects in the same reference cata-log if they are located within the error radius of the MAXIsource. In such cases, we adopt the one with the smallest an-gular separation from the MAXI position as the most likelycounterpart used for the definition of source type. As a result,we find that 296 out of the 500 sources in the present cataloghave one or more counterparts. The numbers of each sourcetype are as shown in table 3: 2 unidentified X-ray sources inBAT70, 8 galaxies, 114 galaxy clusters, 100 Seyfert galaxies,15 blazars, 30 CVs/Stars, 20 X-ray (neutron/black-hole) bina-ries, 4 confused objects, and 204 sources without counterpartsin BAT70 or MCXC.

In the above procedure, some of the MAXI sources maybe matched to those in the BAT70 catalog and MCXC bychance. Here we estimate the number of such coincidentalmatch,NCM, calculated as

NCM = ρBAT70×SBAT70 +ρMCXC ×SMCXC, (5)

where ρBAT70(MCXC) and SBAT70(MCXC) represent the sourcenumber densities of BAT70 (MCXC) at|b|> 10◦ and the to-tal areas of the error circles of the MAXI sources used forthe cross-matching with those catalogs. Specifically, we usethe following values:ρBAT70 = 0.025 (deg−2), ρMCXC = 0.050(deg−2), SBAT70 = 236.8 (deg2), andSMCXC = 173.9 (deg2). Wethus estimateNCM = 10.3, which is∼3% of the total numberof the matched sources.

4.4. Position Accuracy

We here examine the actual positional error of MAXI as afunction of detection significance in the 4–10 keV band on thebasis of the cross matching result. We calculate the angularseparation between the MAXI position and that of the mostlikely counterpart for each object. Figure 10 shows the his-tograms of the angular separation for all the matched sourcesin different significance bins (left:sD,4−10keV = 7− 12, mid-dle: σD,4−10keV = 12− 80, and right: sD,4−10keV > 80). Fig-ure 11 plots 90% error radii as a function of 4–10 keV detec-tion significance that are directly obtained from the observedhistograms. The black crosses represent those in the bins ofsD,4−10keV =7-9, 9-12, 12-25, 25-80, and> 80, from left toright. We fit these data with the form of

σ90%posi =

√(A/sD,4−10keV)B +C2, (6)

whereA, B, andC are free parameters. The blue curve infigure 11 represents the best-fit withA = 2.93±0.47, B =1.80±0.22, andC=0.09±0.01. The slopeB is close to 2.0as expected from the theory. From this result, we estimate the90% systematic error to be≈0.09◦, which is consistent withthat derived in the previous study (Hiroi et al. 2011).

The 37-Month MAXI/GSC Source Catalog in the High Galactic-Latitude Sky 9

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FIG. 10.— Histograms of the angular separation between the positions of the MAXI sources and those of their most-likely counterparts in the referencecatalogs. The left, center, and right panel include the objects with the significance level ofsD,4−10keV = 7–12, 12–80, and>80, respectively.

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curve represents the best-fit model with the form of√

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FIG. 12.— Flux in the 4–10 keV band versus HR plot for the catalogedsources with different types: AGNs (blue squares), galaxy clusters (greencircles), Galactic/LMC/SMC objects (red triangles), and others (i.e., sourceswithout unique identification; gray diamonds). The typical errors of the HR atf4−10keV of 10−10 and 10−11 ergs cm−2 s−1 are∼0.01 and∼0.09, respectively.For visuality, two points with the largest fluxes off4−10keV > 10−9 cm−2 s−1,corresponding to Sco X-1 and Cyg X-2, are excluded from this figure.

4.5. Hardness Ratio Distribution

Figure 12 plots the diagram between the 4–10 keV flux andhardness ratio (HR) for the cataloged sources with differenttypes. The blue squares and green circles represent AGNsand galaxy clusters, respectively. The red triangles corre-spond to Galactic objects and large/small Magellanic cloud(LMC/SMC) objects. Sources without unique counterpartsbased on the catalog matching described above (i.e., thosewith no counterpart or multiple ones) are denoted as the graydiamonds. Figure 13 displays the histograms of HR for each

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type. TheHR distribution of galaxy clusters is located atlower values than that of AGNs. This is consistent with the ex-pectation that galaxy clusters have softer spectra than AGNsin the 3–10 keV range.

4.6. Log N-log S Relation

10 K. Hiroi

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We derive the source number counts (logN-log S relation)in the 4–10 keV band based on the MAXI/GSC 37-month cat-alog. For this calculation, we need the so-called area curve,which represents a survey area guaranteed for detection of asource given as a function of flux. In the same way as in Hiroiet al. (2011), we estimate the sensitivity at each sky positionon the basis of the background photon counts and “effective”exposure (i.e., exposure× detector area). Figure 14 displaysthe area curve in the 4–10 keV band for the detection signif-icance ofsD,4−10keV> 7. As noticed from the figure, the sen-sitivity at the deepest exposure reaches to∼0.4 mCrab (∼5×10−12 ergs cm−2 s−1 in the 4–10 keV band), which is consis-tent with the faintest flux level of the cataloged sources.

Dividing the flux distribution of the detected sources by thesurvey area, we obtain the logN-log S relation in the differ-ential form. Figure 15 shows the logN-log S relation of allthe MAXI sources in the integral form, where the total num-ber densityN(> S) for sources with fluxes aboveS is plotted.The results at fluxes above 1.5×10−11 ergs cm−2 s−1 perfectlymatch with those of Hiroi et al. (2011) derived from the 7-month data. In the faintest range below 7×10−12 ergs cm−2

s−1, however, the number density is slightly (by∼10%) largerthan that extrapolated from the brighter flux range. This ismost probably attributable to the effects by source confusion,which is unavoidable at faintest fluxes close to a confusionlimit determined by the PSF size. The effects may have tobe taken into account in future studies using this catalog, de-pending on the scientific goals.

5. CONCLUSION

We present the second MAXI/GSC source catalog in thehigh Galactic-latitude sky based on the 37-month data in the4–10 keV band observed from 2009 September to 2012 Oc-tober. The accuracy of the background model is significantlyimproved from our previous work (Hiroi et al. 2011) by con-sidering the dependence of the background rate on the “VC”monitor count sensitive to high energy particles. Through theimage fitting to tangentially-projected images with the Pois-son likelihood algorithm, we finally detect 500 X-ray sourcesat |b|> 10◦ with the detection significancesD,4−10keV≥ 7. Thelimiting sensitivity is∼ 0.6 mCrab, or 7.5×10−12 ergs cm−2

s−1 (4–10 keV) for 50% of the survey area, which is the high-est ever achieved among all-sky missions covering this energyband. Performing cross-matching with other X-ray sourcecatalogs, we find that 296 sources have one or more than onecounterparts. The identification work of a complete samplefrom this catalog is on-going, which will be reported in futurepapers.

This work makes use of the HEALPix (Górski et al. 2005)package. This work was partly supported by the Grant-in-Aidfor JSPS Fellows for young researchers (KH), Scientific Re-search 23540265 (YU), and by the grant-in-aid for the GlobalCOE Program “The Next Generation of Physics, Spun fromUniversality and Emergence” from the Ministry of Education,Culture, Sports, Science and Technology (MEXT) of Japan.

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(10)

(11)

(12)

(13)

(14)

(15)

(16)

(17)

MA

XI

Cou

nter

part

No.

Nam

eR

.A.

Dec

l.σ

stat

[a]

s D,4

−10k

eVf 4

−10k

eV[b

]s D

,3−4

keV

f 3−4

keV

[c]

HR

Nam

e[d]

R.A

.D

ecl.

zTy

pe[e

]F

lag[f

]N

ote[g

]

288

2MA

XIJ

1408

−508

212.

0-5

0.9

0.05

820

.722

.3±1.

118

.06.

3±0.

40.

07±

0.04

RX

CJ1

407.

8−510

0(8

2)21

1.96

9-5

1.00

90.

0966

Gal

axy

Clu

ster

MG

289

2MA

XIJ

1409

−428

212.

5-4

2.8

0.12

49.

913

.3±1.

39.

23.

5±0.

40.

11±

0.07

RX

CJ1

410.

4−424

621

2.61

9-4

2.77

70.

049

Gal

axy

Clu

ster

M29

02M

AX

IJ14

13−0

3021

3.3

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0.02

649

.660

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232

.112

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40.

22±

0.02

NG

C55

06(8

3)21

3.31

2-3

.208

0.00

62S

y1.9

BG

291

2MA

XIJ

1417

+25

321

4.4

25.3

0.06

319

.828

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520

.68.

1±0.

40.

08±

0.03

NG

C55

48(8

4)21

4.49

825

.137

0.01

72S

y1.5

BG

292

2MA

XIJ

1417

−128

214.

5-1

2.9

0.30

07.

26.

0±0.

83.

21.

0±0.

30.

31±

0.15

293

2MA

XIJ

1419

−265

214.

9-2

6.6

0.10

39.

210

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15.

61.

9±0.

30.

28±

0.10

ES

O51

1−G03

021

4.84

3-2

6.64

50.

0224

Sy1

B29

42M

AX

IJ14

20−7

7921

5.1

-78.

00.

071

8.1

6.8±

0.8

4.4

0.9±

0.2

0.41±

0.11

295

2MA

XIJ

1420

+48

321

5.2

48.3

0.18

68.

910

.8±1.

28.

93.

3±0.

40.

04±

0.08

296

2MA

XIJ

1420

−485

215.

2-4

8.6

0.19

59.

710

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17.

72.

8±0.

40.

11±

0.08

297

2MA

XIJ

1422

−380

215.

7-3

8.1

0.19

39.

311

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211

.84.

4±0.

4-0

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0.07

298

2MA

XIJ

1423

+37

921

5.9

37.9

0.16

39.

412

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311

.54.

6±0.

4-0

.05±

0.07

BV

H20

07N

S10

216.

269

37.9

710.

163

Gal

axy

Clu

ster

M29

92M

AX

IJ14

23+

250

216.

025

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179

7.7

11.2±

1.5

5.8

2.1±

0.4

0.27±

0.10

NG

C56

1021

6.09

524

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0.01

69S

y2B

300

2MA

XIJ

1428

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217.

1-7

3.0

0.06

29.

07.

0±0.

87.

51.

8±0.

20.

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301

2MA

XIJ

1429

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521

7.4

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315

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7±0.

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0.05

1ES

1426

+42

8(8

5)21

7.13

642

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9B

LLa

cB

MG

302

2MA

XIJ

1436

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219.

1-3

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612

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27.

22.

6±0.

40.

30±

0.07

303

2MA

XIJ

1437

+58

821

9.4

58.8

0.15

210

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6±1.

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52.

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30.

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Mrk

817

219.

092

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0314

Sy1

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304

2MA

XIJ

1441

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305

2MA

XIJ

1446

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222

1.6

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69.

811

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27.

82.

9±0.

40.

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306

2MA

XIJ

1454

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223.

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110

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6±0.

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307

2MA

XIJ

1455

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223.

9-3

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19.

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12.

5±0.

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RX

CJ1

456.

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00.

115

Gal

axy

Clu

ster

M30

82M

AX

IJ14

59+

217

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921

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160

9.2

10.4±

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2009

225.

085

21.3

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153

Gal

axy

Clu

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M30

92M

AX

IJ15

03−4

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5.8

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10.

099

12.4

15.0±

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21.2

8.4±

0.4

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6±0.

0431

02M

AX

IJ15

03+

108

225.

810

.90.

103

12.8

15.6±

1.2

9.6

3.5±

0.4

0.19±

0.06

311

2MA

XIJ

1503

−027

226.

0-2

.70.

090

12.4

14.5±

1.2

11.7

4.1±

0.4

0.07±

0.06

RX

CJ1

504.

1−024

822

6.03

2-2

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0.21

53G

alax

yC

lust

erM

312

2MA

XIJ

1510

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227.

7-8

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99.

07.

4±0.

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40.

9±0.

30.

47±

0.12

2MA

SX

J151

4421

7−812

3377

228.

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394

0.06

84S

y1.2

B31

32M

AX

IJ15

11+

059

227.

85.

90.

025

48.3

64.5±

1.3

42.8

18.7±

0.4

0.06±

0.02

314

2MA

XIJ

1512

−213

228.

0-2

1.4

0.12

79.

710

.3±1.

17.

72.

5±0.

30.

14±

0.08

2MA

SX

J151

1597

9−211

9015

227.

999

-21.

317

0.04

46S

y1/N

LB

315

2MA

XIJ

1513

+42

322

8.4

42.4

0.21

97.

48.

9±1.

25.

02.

0±0.

40.

19±

0.12

NG

C58

9922

8.76

342

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0.00

86S

y2B

316

2MA

XIJ

1521

+08

223

0.4

8.2

0.09

121

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120

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0±0.

4-0

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317

2MA

XIJ

1522

+27

823

0.6

27.9

0.07

017

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219

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3±0.

4-0

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0.04

RX

CJ1

522.

4+27

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8)23

0.61

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23G

alax

yC

lust

erM

G31

82M

AX

IJ15

23+

304

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119

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0631

92M

AX

IJ15

23−3

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1.0

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10.

314

8.2

8.6±

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1.7±

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0.11

320

2MA

XIJ

1535

+58

123

3.9

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Mrk

290

233.

968

57.9

030.

0296

Sy1

B32

12M

AX

IJ15

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4.8

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711

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30.

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RX

CJ1

540.

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823

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33G

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yC

lust

erM

322

2MA

XIJ

1539

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A21

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323

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1545

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324

2MA

XIJ

1546

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RX

CJ1

539.

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Gal

axy

Clu

ster

M32

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AX

IJ15

48−1

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NG

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B32

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AX

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50.

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327

2MA

XIJ

1552

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68.

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LED

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183

Sy1

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30.

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0.8

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S15

49−79

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234

0.15

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329

2MA

XIJ

1555

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73.

5±0.

40.

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330

2MA

XIJ

1558

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9.6

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130

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AB

ELL

2142

(90)

239.

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Gal

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Clu

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BM

G33

12M

AX

IJ15

59−1

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80.

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11.7±

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3.3±

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0.07

332

2MA

XIJ

1600

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333

2MA

XIJ

1601

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RX

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601.

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153

Gal

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Clu

ster

MG

334

2MA

XIJ

1602

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0.7

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328

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0.03

335

2MA

XIJ

1603

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240.

9-9

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217

8.3

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2.2±

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0.10

TA

BL

E1

—C

ON

TIN

UE

D

(1)

(2)

(3)

(4)

(5)

(6)

(7)

(8)

(9)

(10)

(11)

(12)

(13)

(14)

(15)

(16)

(17)

MA

XI

Cou

nter

part

No.

Nam

eR

.A.

Dec

l.σ

stat

[a]

s D,4

−10k

eVf 4

−10k

eV[b

]s D

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keV

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keV

[c]

HR

Nam

e[d]

R.A

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ecl.

zTy

pe[e

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lag[f

]N

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]

336

2MA

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1605

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6±0.

40.

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337

2MA

XIJ

1607

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241.

8-7

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76.

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20.

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2MA

SX

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3565

241.

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899

Gal

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B33

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AX

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CG

CG

367−0

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74S

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339

2MA

XIJ

1614

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Mrk

876

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129

Sy1

B34

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RX

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342

2MA

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343

2MA

XIJ

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344

2MA

XIJ

1619

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2MA

SS

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Sym

b/N

SB

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2MA

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348

2MA

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RX

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Gal

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MG

349

2MA

XIJ

1627

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1627

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SR

C/X

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Gal

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2MA

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352

2MA

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RX

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Gal

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353

2MA

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2MA

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Gal

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RX

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RX

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Gal

axy

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M35

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IJ16

47−2

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11.8

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358

2MA

XIJ

1653

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1800

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1842

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398

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XIJ

1854

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400

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1900

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614

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0.1−2

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1900

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88.

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402

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1912

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1915

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2MA

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1919

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405

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1919

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1921

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1921

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1922

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411

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1933

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313

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30.

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412

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XIJ

1936

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413

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1937

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414

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1941

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415

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1947

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RX

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217

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144

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417

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XIJ

1950

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77.

28.

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16.

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30.

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418

2MA

XIJ

1952

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419

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XIJ

1954

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XIJ

1959

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140

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148

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1959

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421

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2005

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422

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2006

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423

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2009

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111

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2012

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2MA

XIJ

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(6)

(7)

(8)

(9)

(10)

(11)

(12)

(13)

(14)

(15)

(16)

(17)

MA

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Cou

nter

part

No.

Nam

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stat

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432

2MA

XIJ

2042

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655

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433

2MA

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434

2MA

XIJ

2043

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2MA

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2044

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2MA

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(5)

(6)

(7)

(8)

(9)

(10)

(11)

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(14)

(15)

(16)

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MA

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part

No.

Nam

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stat

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480

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