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a new era of x - ray astronomy has begun with the launch of the @xmath0 @xmath21-@xmath22 @xmath23 on 1999 july 23 , thanks to its very high sensitivity , broad energy range and high angular resolution ( weisskopf et al . 2002 ) . the two deepest x - ray surveys ever conducted , 2 ms @xmath0 deep field north ( brandt et al . 2003 , alexander et al . 2003 ) and 1 ms @xmath0 deep field south ( giacconi et al . 2002 ; rosati et al . 2001 ) , were obtained using the advanced ccd imaging spectrometer detector ( acis ; garmire et al . 2003 ) on @xmath0 @xmath21-@xmath22 @xmath23 . these two surveys are @xmath14 50 times more sensitive than the deepest pre-@xmath0 observations in the soft x - ray band ( 0.5  2.0 kev , e.g. , hasinger et al . 1998 ) and greater than 100 times more sensitive than those deepest pre-@xmath0 observations in the hard x - ray band ( 2.0  10.0 kev , e.g. , ueda et al . 1999 ; fiore et al . 1999 ) . with these surveys , the `` diffuse '' x - ray background discovered four decades ago ( giacconi et al . 1962 ) has been almost entirely resolved into discrete sources ( i.e. @xmath20 90% in the soft band , and @xmath14 80% in the hard band ) . many other deep x - ray blank - sky surveys from @xmath0 ( stern et al . 2002a ; yang et al . 2003 ; mushotzky et al . 2000 ; manners et al . 2003 ) and xmm ( hasinger et al . 2001 ) were also performed in the past few years . along with multi - band observations of the detected x - ray sources , these deep surveys have brought us many interesting results and more important science issues to be addressed . these include the large scale structures from 2d ( yang et al . 2003 ) and 3d ( gilli et al . 2003 ; barger et al . 2002 ) analyses , type 2 qsos ( norman et al . 2002 ; stern et al . 2002b ) , very high redshift x - ray selected active galactic nuclei ( agn , e.g. , barger et al . 2003 ) , and much more .    here we present a new deep ( 172 ks ) @xmath0 acis exposure , obtained originally for the follow - up of ly@xmath24 sources from the large area lyman alpha ( lala ) survey s botes field . the large area lyman alpha ( lala ) survey ( rhoads et al . 2000 , 2003 ; rhoads & malhotra 2001 , malhotra & rhoads 2002 ) was designed to search for lyman @xmath24 emitters at high redshifts through narrowband imaging . the survey comprises two primary fields , 36@xmath136   in size each , located in botes ( at 14:25:57 + 35:32 j2000.0 ) and in cetus ( at 02:05:20 -04:55 j2000.0 ) . both fields were chosen to be inside the large areas of the noao deep wide - field survey ( ndwfs ) , which is a deep optical and ir ( @xmath25 ) imaging survey of 18 @xmath26 of the sky with the primary goal of studying the evolution of large - scale structure from @xmath27 ( jannuzi and dey 1999 ; brown et al . 2003 ; jannuzi et al . 2004 , in preparation ) . five broadband optical images ( @xmath9 , @xmath7 , @xmath11 from ndwfs , and @xmath10 , @xmath12 as part of lala ) and eight narrowband images are used to search for lyman-@xmath24 emitters at z @xmath14 4.5 , 5.7 , and 6.5 respectively . the x - ray image presented here was originally obtained to investigate the x - ray properties of the detected high redshift ly@xmath24 emitters . this study was presented by malhotra et al . ( 2003 ) , where we placed stringent upper limits on the typical x - ray flux of ly@xmath24 sources and conclude that agn ( obscured or otherwise ) can not constitute a dominant portion of the ly@xmath24 source population . this @xmath0 exposure ( 172 ks ) is among the deepest yet obtained by @xmath0 of the extragalactic sky ; only the cdf - n and cdf - s are substantially deeper . in this paper we present a full catalog of the detected x - ray sources , along with an analysis of the x - ray source counts , and the @xmath7-band magnitudes ( or 3@xmath8 upper limits ) for their optical counterparts . to study the nature of these sources , spectroscopic follow - up observations for these sources are under way . the present paper is structured as follows : we present the x - ray observations and data reduction in section 2 , source detection and catalog in section 3 , logn - logs in section 4 , and optical identifications in section 5 . our conclusions and summary are presented in section 6 . an 178 kilo - second exposure , composed of two individual observations , was obtained using the advanced ccd imaging spectrometer ( acis ) on the _ chandra x - ray observatory _ in the very faint ( vfaint ) mode . the first observation , with 120 ks exposure , was taken on 2002 april 16 - 17 ( _ chandra _ obs i d 3130 ) . the second observation , with 58 ks exposure , was taken on 2002 june 9 ( obs i d 3482 ) . all four acis - i chips and acis - s2 , acis - s3 chips were used , with the telescope aimpoint centered on the acis - i3 chip for each exposure . the aimpoint of obs i d 3130 is 14:25:37.791 + 35:36:00.20 ( j2000.0 ) , and the aimpoint of obs i d 3482 is 14:25:37.564 + 35:35:44.32 , 16@xmath28 away from that of obs i d 3130 . the galactic column density n@xmath29 towards our field is 1.15 @xmath1 10@xmath30 @xmath4 ( hartmann et al . due to their large off - axis angle during the observations , the acis - s chips have worse spatial resolution and lower effective area relative to the acis - i chips . in this paper , data from any acis - s ccd were therefore ignored . the data were reduced and analyzed using the @xmath0 interactive analysis of observations ( ciao ) software ( version 2.2.1 , see http://asc.harvard.edu/ciao ) . the data were reprocessed to clean the acis particle background for very faint mode observations , and then filtered to include only the standard event grades 0,2,3,4,6sec : grades ] . all bad pixels and columns were also removed , not only from the photon events files , but also when calculating the effective exposure maps . the high background time intervals were manually removed by checking the total event rates . the total net exposure time is 172 ks ( 120 ks from obs i d 3130 , and 52 ks from obs i d 3482 ) . the offset between the astrometry of the two observations was obtained by registering the x - ray sources showing up in both exposures . the two event files were merged after correcting the small offset ( 0.3 ) , and the combined data have the same coordinate system as obs i d 3130 . we present the color composite x - ray image of the combined exposure in fig . [ color ] . three images were extracted from the combined event file for source detection : a soft image ( 0.5  2.0 kev ) , a hard image ( 2.0  7.0 kev ) and a total image ( 0.5  7.0 kev ) . the hard and total bands were cut at 7 kev since the effective area of @xmath0 decreases above this energy , and the instrumental background rises , giving a very inefficient detection of sky and source photons . the wavdetect program ( freeman et al . 2002 ) , which is included with the ciao software package , was run on the extracted images . a probability threshold of 1 @xmath1 10@xmath31 ( corresponding to 0.5 false sources expected per image ) , and wavelet scales of 1,2,4,8,16 pixels ( 1 pixel = 0.492 ) were used . a total of 168 x - ray sources were detected : 160 in the total band ( 0.5  7.0 kev ) , 132 in the soft band ( 0.5  2.0 kev ) , and 111 in the hard band ( 2.0  7.0 kev ) . we present the catalog of the detected sources in table 1 . note that the number of total detected x - ray sources will be increased to 196 if we use a probability threshold of wavdetect ( 1 @xmath1 10@xmath32 ) , however , considering the increased number of possible false detections ( @xmath14 5 expected per image ) , we prefer to publish a conservative catalog with fewer false detections . we also tried to search for x - ray sources with scales much larger than the psf by running wavdetect with wavelet scales of 32,64,128 pixels on the images . however , we did nt detect any new source beyond those in the catalog . below we give explanations to the columns in table 1 . column(1)-(4 ) : the source i d , iau name , right ascension and declination respectively . the iau name for the sources is cxolala1 jhhmmss.s+ddmmss . the positions were determined by wavdetect . whenever possible , we use positions derived in the soft band , which has the best spatial resolution among the three bands . for sources which are not detected in the soft band , we use total band positions instead if available , and hard band positions were quoted for those sources detected only in the hard band . column(5 ) : 3 @xmath8 uncertainties of the centroid positions directly given by wavdetect . column(6)-(8 ) : the net counts in the soft , hard and total bands . the counts were calculated using circular aperture photometry . for each source , we defined a source region which is a circle centered at the position given in column ( 3 ) and ( 4 ) , with radius r@xmath33 set to the 95% encircled - energy radius of @xmath0 acis psf at the source position . r@xmath33 varies in the range of 2@xmath28 to 15@xmath28 from the center to the edge of the field . source photons were then extracted from the regions , and the local background was extracted from an annulus with outer radius of 2.4 @xmath1 r@xmath33 and inner radius of 1.2 @xmath1 r@xmath33 , after masking out nearby sources . the aperture correction ( @xmath1 1/0.95 ) was applied to the source counts . the derived net counts and 1 @xmath8 poisson uncertainties ( e.g. , gehrels 1986 ) are given for each source in each band . column(9 ) : indication of source detection . we mark the source with `` t '' , `` s '' and `` h '' for source detected in total , soft and hard band respectively . multiple letters are used for sources detected in more than one band . for example , `` ts '' means detections in both the total band and the soft band , but non - detected in the hard band . column(10 ) : hardness ratio defined as @xmath34 = ( h - s)/(h+s ) , where h and s are the vignetting - corrected net counts in the hard and soft band respectively . the hardness ratios vs 0.5  10.0 kev band x - ray fluxes for the detected x - ray sources are plotted in fig . [ hr ] . assuming a power - law spectrum with the galactic hi column density ( 1.15 @xmath1 10@xmath30 @xmath4 ) , the observed hardness ratio can be converted to the photon index @xmath35 of the spectrum , which is also presented in the figure . as presented in earlier surveys , harder sources are seen at fainter fluxes , most of which are believed to be obscured agns . column(11)-(13 ) : x - ray fluxes ( galactic absorption corrected ) of three bands in the unit of 10@xmath3 ergs @xmath4 s@xmath5 . a power - law spectrum with the galactic column density was assumed to calculate the conversion factors from net counts to x - ray fluxes . the photon index of the power - law was chosen at @xmath35 = 1.4 , which was also used in giacconi et al . ( 2002 ) and stern et al . ( 2002a ) . three band net count rates were calculated by dividing the net counts in column 6 - 8 by the effective exposure time at each source position in each band , and then converted into x - ray fluxes of 0.5  10.0 kev , 0.5  2.0 kev , and 2.0  10.0 kev respectively . these settings make our results directly comparable with those from other surveys . the conversion factors used were 1.25 @xmath1 10@xmath36 ergs @xmath4 count@xmath5 from the 0.5  7.0 kev band observed count rates to the galactic absorption corrected x - ray fluxes in the band 0.5  10.0 kev , 4.67 @xmath1 10@xmath37 ergs @xmath4 count@xmath5 from the 0.5  2.0 kev band count rates to the 0.5  2.0 kev band fluxes , and 2.96 @xmath1 10@xmath36 ergs @xmath4 count@xmath5 from the 2.0  7.0 kev band count rates to the 2.0  10.0 kev band fluxes . note the total band ( 0.5  10.0 kev ) flux is not equal to the sum of the soft and hard band fluxes if the actual photon index differs from 1.4 . to calculate the fluxes assuming a power - law spectrum with different photon index @xmath35 , the conversion factors f@xmath38/f@xmath39 for different bands are needed ( fig . we can see from the figure that the soft band ( 0.5  2.0 kev ) flux is not sensitive to the photon index @xmath35 , while the hard ( 2.0  10.0 kev ) and total ( 0.5  10.0 kev ) band fluxes correlate with it strongly . one thus has to be careful while using these fluxes . column(14)-(16 ) : the offsets of the detected optical counterparts from the x - ray source positions ( @xmath40 = ra@xmath41 - ra@xmath42 , @xmath43 = dec@xmath41 - dec@xmath42 ) , and the @xmath7-band auto magnitudes ( kron - like elliptical aperture magnitudes , bertin & arnouts 1996 ) with 1 @xmath8 uncertainties - band zeropoint . ] . for sources which are not detected in @xmath7-band , 3@xmath8 upper limits of the magnitudes are given when available . see section 5 for details . column(17 ) : the fwhm ( full - width half - maximum ) of the optical counterparts in ndwfs @xmath7-band image ( see section 5 ) . in order to calculate the cumulative source counts , n(@xmath20s ) , one need count the number of sources with fluxes @xmath20s , and also compute the summed sky in the field where these sources can be detected ( the sky coverage ) . in fig . [ cutoff ] , we present the soft and hard band net counts vs off - axis angle for faint sources ( with net counts @xmath18 50 ) . detected and non - detected sources ( detected in other bands but having net counts from x - ray photometry ) are displayed with different symbols . it s clear from the figure that the x - ray sources with larger off - axis angles need more net counts to be detected because of the larger psf size . this indicates that the detection limits of net counts vary with the psf sizes . two dashed lines ( net counts = a + b @xmath1 psf@xmath44 respectively ) are added to fig . [ cutoff ] , with the parameters a and b chosen for both bands by visual inspection to exclude all non - detected sources and include maximum number of detected sources . we can see that although some detected sources are located below the threshold dashed lines , they are mixed up with these non - detected sources , i.e. , the detection is incomplete below the lines , and the sky coverage for these sources is thus not available . in this paper , we use only these sources with net counts c @xmath20 a + b @xmath1 psf@xmath44 to calculate logn - logs . using the above cutoffs , the sky coverages are derived and presented in fig . the derived logn - logs for both soft and hard band are presented in fig . [ lognlogs ] . a maximum - likelihood power - law was used to fit the slope of the logn - logs in each band . for the 0.5  2.0 kev band we find @xmath45 and for the 2.0  10.0 kev band , we find : @xmath46    the above procedures of calculating logn - logs were also run on the 1 ms cdf - n data ( brandt at al . 2001 ) , 1 ms cdf - s data ( rosati et al . 2002 ) , and 184.7 ks lynx data ( stern et al . the independently derived logn - logs from the above three fields match the published ones to within 1@xmath8 , and are plotted in fig . [ lognlogs ] for comparison . the source densities ( n@xmath20s ) and 1@xmath8 uncertainties at the faint end ( 2.0 @xmath1 10@xmath2 ergs @xmath4 s@xmath5  in 0.5  2.0 kev band , and 2.0 @xmath1 10@xmath3 ergs @xmath4 s@xmath5  in the 2.0  10.0 kev band ) are plotted in the inserts . in the soft band , there is no significant difference among the source counts from the four deep surveys . in the hard band , obvious fluctuations of the source counts are seen at the faint end : lala botes field has the highest source density at 2.0 @xmath1 10@xmath3 ergs @xmath4 s@xmath5 which is 33% higher than that of cdf - s , while cdf - n is 23% higher than cdf - s and lynx field is 14% lower . note that similar field - to - field variances of the hard band source counts have been reported previously ( see tozzi 2001a , cowie et al . this is believed to be due to the clustering of the x - ray sources . the non - detection of field - to - field variance in the soft band is also consistent with the results from previous studies ( yang et al . 2003 ; tozzi et al . 2001a ) , indicating that the soft x - ray sources are less correlated than the hard x - ray sources . what fraction of the hard x - ray background is resolved by our deep 172 ks @xmath0 imaging ? in the range of 1.7 - 100 @xmath1 10@xmath3 ergs @xmath4 s@xmath5 , the integrated hard x - ray flux density in the 2.0  10.0 kev band is 1.2 @xmath1 10@xmath36 ergs @xmath4 s@xmath5  deg@xmath47 . note for sources bright than 10@xmath48 ergs @xmath4 s@xmath5 , the integrated hard x - ray flux density from our survey is 0.4 @xmath1 10@xmath36 ergs @xmath4 s@xmath5  deg@xmath47 , consistent with the value derived by della ceca et al . ( 1999 ) from a wider area asca survey . the total integrated hard x - ray flux density we obtained is 1.6 @xmath1 10@xmath36 ergs @xmath4 s@xmath5  deg@xmath47 , down to 1.7 @xmath1 10@xmath3 ergs @xmath4 s@xmath5  in 2.0  10.0 kev band . this is equal to the high energy astronomy observatory 1 ( heao 1 ) value ( marshall et al . 1980 ) , but 10%-30% lower than the more recent determinations from asca and @xmath49 ( e.g. , ueda et al . 1999 ; vecchi et al . we conclude that our 172 @xmath0 deep imaging resolves @xmath6 70% of the 2.0  10.0 kev x - ray background , and the main uncertainty comes from the value of total x - ray background itself . our deep chandra pointing is within the ndwfs botes subfield ndwfs j1426 + 3531 ( which is 35@xmath135  in size ) centered at ra 14:26:00.8 , dec + 35:31:32.0 ( j2000 ) . five broadband optical images ( @xmath9 , @xmath10 , @xmath7 , @xmath11 , and @xmath12 ) are available to search for the optical counterparts of the x - ray sources . three of these ( @xmath9 , @xmath7 , and @xmath11 ) and @xmath11 band images are available from the noao science archive ( http://www.archive.noao.edu/ndwfs/ ) . the @xmath7-band image , which is deeper than the currently released version , will be available from the noao science archive within 12 months . ] are from the noao deep wide field survey ( ndwfs ; jannuzi & dey 1999 ) , while the remaining two ( @xmath10 and @xmath12 ) were obtained as part of lala . the limiting kron - cousins system magnitudes ( 3@xmath8 , 4  diameter aperture ) of the ndwfs images are @xmath50 , @xmath51 , and @xmath52 . the corresponding limits in the lala broadband data are @xmath53 and @xmath54 ( where the @xmath12 limit is on the ab system ) . our primary optical image for identifications in this paper is the @xmath7-band image from ndwfs , which is substantially deeper than the others . all the optical images were obtained using the kitt peak national observatory mayall 4 m telescope and the mosaic-1 camera ( muller et al . 1998 ; jannuzi et al . 2004 , in preparation ) . these images were produced following the procedures described in version 7.01 of `` the noao deep wide - field survey mosaic data reductions '' . a general description of the software used is provided by valdes ( 2002 ) and the complete details of the ndwfs data reduction will be provided by jannuzi et al . ( 2004 ) . sextractor package ( bertin & arnouts 1996 ) v2.1.0 was run on the ndwfs deep @xmath7-band image to generate the @xmath7-band source catalog . the registration of the x - ray to optical coordinates was done by cross - correlating the x - ray and the above @xmath7-band catalogs ( e.g. , see giacconi et al . 2002 , stern et al . average shifts in ( ra@xmath41 - ra@xmath42 , dec@xmath41 - dec@xmath42 ) of ( 0.1 , -0.2 ) were found from the ndwfs @xmath7-band to x - ray imaging , but no obvious rotation or plate - scale effects were discovered . after correcting the average shifts , we matched the optical and x - ray source catalogs using a 1.5  radius aperture for host identifications , which was generally used by other @xmath0 surveys ( giacconi et al . 2002 , stern et al . the 3@xmath8 x - ray positional uncertainties in table 1 are used if larger than 1.5 . optical counterparts for 144 of the 168 x - ray sources were detected in the @xmath7-band image down to 3@xmath8 . one of them ( no . 122 ) has multiple possible optical counterparts . calculations show that the possibility of having one optical source down to 3@xmath8 in a 1.5  circle by chance is 10% . this means that at least 90% of the optical counterparts we found should correspond to the x - ray sources , and at worst we might have @xmath14 14 false matches . we present the offsets from the x - ray source positions ( @xmath40 = ra@xmath41 - ra@xmath42 , @xmath43 = dec@xmath41 - dec@xmath42 ) , the derived @xmath7-band auto magnitudes ( kron - like elliptical aperture magnitudes , bertin & arnouts 1996 ) for all optical counterparts in table 1 , and the optical cutouts in fig . [ cutout ] . iraf package `` radprof '' was used to measure the radial profiles of these counterparts in ndwfs @xmath7 image , and we present the measured fwhm ( full - width half - maximum ) in table 1 . these sources which have fwhm larger than the average seeing of the ndwfs @xmath7 image ( fwhm = 1.16 ) were examined visually . we conclude that it is safe to consider all the bright sources ( @xmath7 @xmath18 23 ) with fwhm @xmath55 1.3  as optically resolved . the only exception is source no . 144 , which is too close to another bright source , thus we can not tell if it is resolved or not . the total number of optically resolved sources is 15 . the search for optical counterparts was extended to @xmath9 , @xmath11 , @xmath10 and @xmath12 band for the 24 x - ray sources without @xmath7-band optical counterparts , which brought us optical counterparts for 8 more x - ray sources . the positions of these counterparts are also given in table 1 ( by listing ra - ra@xmath42 , dec - dec@xmath42 ) . the limiting magnitude of the @xmath7-band image was given as upper limits for 22 of the x - ray sources . note source no . 37 and 160 are overlapped by bleeding trails in the ndwfs @xmath7 image , and the upper limits of their @xmath7-band magnitudes are not available .    the first survey ( faint images of the radio sky at twenty - cm , becker , white , & helfand 1995 ) detection limit in our field is 0.96 mjy / beam . radio counterparts for 4 of our x - ray sources were found , which are source no . 1 , 66 , 91 and 141 , with integrated flux density ( mjy ) of 6.02 , 1.24 , 2.17 and 8.30 respectively . the first 3 of the 4 radio sources are resolved r@xmath1821 red galaxies , which are some of the brightest optical counterparts to x - ray sources in our catalog . the remaining source is an r - band non - detection more than 10 " from any r@xmath1821 galaxies and is presumably at z@xmath201 .      in fig . [ xr ] we plot the x - ray - to - optical flux ratio of our x - ray sources ( in soft and hard band respectively ) , and in fig . [ xrhr ] we plot the log(@xmath15/@xmath16 ) in the hard band vs the hardness ratio of x - ray emission . for the 22 x - ray sources without @xmath7-band counterparts detected , the lower limits of log(@xmath15/@xmath16 ) were plotted , which shows a consistent distribution with that of the optically faint ( @xmath7 @xmath20 24 ) sources . from the figures we can see that the majority ( @xmath14 76% ) of the x - ray sources fall within log(@xmath56/@xmath16 ) = 0.0@xmath171 , which is typical of agns .    there is a significant population ( @xmath14 10% ) of x - ray faint / optically bright sources ( log(@xmath56/@xmath16 ) @xmath18 -1.0 ) , most of which are extended in the @xmath7 band optical image and x - ray soft ( see fig . [ xrhr ] ) . these sources should be nearby , bright normal galaxies ( see tozzi et al . 2001b ; barger et al . 2001 ; hornschemeier at al . 2001 ) . other optically extended sources falling within log(@xmath56/@xmath16 ) = 0.0@xmath171 or x - ray hard are most likely to be low redshift seyfert galaxies , or low luminosity agns . in addition , we also have a population of sources which are x - ray @xmath19 for their optical magnitudes ( log(@xmath56/@xmath16 ) @xmath20 1.0 ) , especially in the hard band , including most of the 22 @xmath7-band nondetected x - ray sources . we plot in fig . [ hist ] the histogram distribution of the hardness ratios of the optically faint x - ray bright sources ( log(@xmath57/@xmath16 ) @xmath20 1.0 ) , comparing with these sources with lower x - ray - to - optical flux ratio ( 1.0 @xmath20 log(@xmath57/@xmath16 ) @xmath20 0.0 ) . the optically faint x - ray bright sources are obviously harder in x - ray , suggesting that most of them are obscured agns , for which high column density absorption shields both the optical and the soft x - ray emission . there are 22 x - ray sources which are not detected in the @xmath7-band down to @xmath7 = 25.7 ; 5 of them are detected in redder bands ( @xmath11,@xmath12 ) ; and 3 of them in bluer bands ( @xmath9 , @xmath10 ) ; 14 x - ray sources have no optical counterparts found in any band , which corresponds to a sky surface density of 145 deg@xmath47 . the integrated hard x - ray ( 2.0  10.0 kev ) flux density from these 22 sources is 0.14 @xmath1 10@xmath36 ergs @xmath4 s@xmath5  deg@xmath47 , down to a flux limit of 1.7 @xmath1 10@xmath3 ergs @xmath4 s@xmath5 . this contributes 6@xmath149% of the total 2.0  10.0 kev band x - ray background . the 19 @xmath7-band nondetected sources , which are not detected in bluer bands ( @xmath9 , @xmath10 ) , are possible candidates for @xmath58 @xmath20 5 quasars , because of the absorption from the lyman transitions of hydrogen along our line of sight . however , our calculations indicate that even for a compton thick agn ( with intrinsic photon power - law index @xmath35 = 2.0 and absorption column density n@xmath29 = 10@xmath59 @xmath4 ) , the hardness ratio hr is expected to be @xmath18 0 at @xmath58 @xmath20 5 . thus 8 of them with harder x - ray spectra ( hr @xmath20 0 ) can not be at @xmath58 @xmath20 5 . in fig . [ xrhr ] , we also marked the 5 x - ray sources without @xmath7-band counterparts , but showing up in redder bands ( @xmath11,@xmath12 ) . preliminary results from photometric redshift analyses show that the two softest ones of the 5 are at photo - z @xmath14 4.3 , and the other 3 which have harder x - ray spectra at photo - z @xmath14 1 - 2 . this agrees well with the above argument that high redshift objects should be soft in x - ray . excluding these sources with hr @xmath20 0 , there are 11 @xmath7-band nondetections left , which can be possibly at @xmath58 @xmath20 5 .    assuming a constant agn density up to @xmath58 = 10 , gilli , salvati & hasinger ( 2001 ) predicted a @xmath58 @xmath20 5 agn density of 500 deg@xmath47 for a limiting flux of 2.3 @xmath1 10@xmath3 ergs @xmath4 s@xmath5  in the 0.5  2.0 kev band . this model predicts @xmath14 50 @xmath13 5 sources in our field , which is clearly too high . assuming the agn density above @xmath58 = 2.7 decreases by a factor of 2.7 per unit redshift as found for optical quasars ( schmidt , schneider , & gunn 1995 ) , gilli et al . predicted a much lower source density of @xmath58 @xmath20 5 agns ( 25 deg@xmath47 ) for the same limiting flux . it corresponds to @xmath142 @xmath58 @xmath20 5 objects in our field , which is very plausible with the current data , considering that those 11 sources are unlikely to be all at @xmath58 @xmath20 5 . actually , several optically faint @xmath0 sources from other surveys have already been confirmed to be at @xmath58 @xmath18 5 by spectroscopic observations ( e.g. , see alexander et al . we present a deep , 172 ks @xmath0 acis exposure of the lala botes field . this paper describes the details of the observations , data reduction , source detection , logn - logs analysis , and presents the x - ray source catalog along with @xmath7-band magnitudes of their optical counterparts . a total of 168 x - ray sources were detected , 160 in the total band ( 0.5  7.0 kev ) , 132 in the soft band ( 0.5  2.0 kev ) , and 111 in the hard band ( 2.0  7.0 kev ) . near the aim point , the detection is down to a flux limit of 1.5 @xmath1 10@xmath2 ergs @xmath4 s@xmath5  in soft ( 0.5  2.0 kev ) band , and 1.0 @xmath1 10@xmath3 ergs @xmath4 s@xmath5  in hard ( 2.0  10.0 kev ) band . logn - logs was compared with those from other deep surveys , and we find obvious field - to - field fluctuations of the hard band source counts . these fluctuations are believed to be due to the large scale clustering of the detected x - ray sources . calculations show that our deep imaging resolves @xmath6 70% of the x - ray background in 2.0  10.0 kev band . optical counterparts for 90% of the x - ray sources were found from deep optical images . among the @xmath7-band non - detected sources , 11 of them can be possibly at @xmath13 5 , based on the hardness ratios of their x - ray emission and the fact that they are not detected in bluer bands ( @xmath9,@xmath10 ) . spectroscopic follow - up observations of these counterparts are being undertaken and will be present in future paper . this work was supported by the cxc grant go2 - 3152x and the national optical astronomy observatory which is operated by the association of universities for research in astronomy ( aura ) , inc . under a cooperative agreement with the national science foundation . we would like to thank the ndwfs team , and in particular melissa miller ( noao ) , who assisted in the reduction of the @xmath7-band image used extensively in this paper . we would like to thank n. brandt for providing the cdf - n logn - logs . we also thank the referee for a prompt and helpful report . alexander , d. m. , brandt , w. n. , hornschemeier , a. e. , garmire , g. p. , schneider , d. p. , bauer , f. e. , & griffiths , r. e 2001 , aj , 122 , 2156 alexander , d. m. , et al . 2003 , aj , in press , astro - ph/0304392 barger , a. j. , cowie , l. l. , mushotzky , r. f. , & richards , e. a. 2001 , aj , 121 , 662 barger , a. j. , cowie , l. l. , brandt , w. n. , capak , p. , garmire , g. p. , hornschemeier , a. e. , steffen , a. t. , & wehner , e. h. 2002 , aj , 124 , 1839 barger , a. j. , cowie , l. l. , capak , p. , alexander , d. m. , bauer , f. e. , brandt , w. n. , garmire , g. p. , & hornschemeier , a. e. 2003 , apj , 584 , 61 becker , r. h. , white , r. l. , & helfand , d. j. 1995 , apj , 450 , 559 bertin , e. and arnouts , s. 1996 ,  117,393 brandt , w. n. , et al . 2001 , 122 , 2810 brandt , w. n. , et al . 2003 , head , 35 , 3601b brown , m , dey , a , jannuzi , b. t. , lauer , t. r. , tiede , g. p. , & mikles , v. j. 2003 , apj , in press , astro - ph0306128 cowie , l. l. , garmire , g. p. , bautz , m. w. , barger , a. j. , brandt , w. n. , & hornschemeier , a. e. 2002 , apj , 566 , l5 della ceca , r. , castelli , g. , braito , v. , cagnoni , i. , & maccacaro , t. 1999 , apj , 524 , 674 fiore , f. , la franca , f. , giommi , p. , elvis , m. , matt , g. , comastri , a. , molendi , s. , & gioia , i. 1999 , mnras , 306 , l55 freeman , p.e . , kashyap , v. , rosner , r. , & lamb , d. q. 2002 , apjs , 138 , 185 garmire , g. p. , bautz , m. w. , ford , p. g. , nousek , j. a. , & ricker , g. r. 2003 , proc . spie , 4851 , 28 gehrels , n. 1986 , apj , 303 , 336 giacconi , r. , gurksy , h. , paolini , f.r . , & rossi , b.b . 1962 , phys . , 9 , 439 giacconi , r. , et al . 2002 , apjs , 139 , 369 gilli , r. , salvati , m. , & hasinger , g. 2001 , a&a , 366 , 407 gilli , r. et al . 2003 , apj letter accepted hornschemeier , a. e. et al . 2001 , apj , 554 , 742 hartmann , d , kalberla , p. m. w. , burton , w. b. , & mebold , u. 1999 , a&as , 119 , 115 hasinger , g. , burg , r. , giacconi , r. , schmidt , m. , trumper , j. , & zamorani , g. 1998 , a&a , 329 , 482 hasinger , g. et al . 2001 , a&a , 365 , l45 jannuzi , b. t. , & dey , a. 1999 , in asp conf . 191 , photometric redshifts and high - redshift galaxies , ed . r. j. weymann , l. j. storrie - lombardi , m. sawicki , & r. j. brunner ( san francisco : asp ) , 111 malhotra , s. & rhoads , j. e. 2002 , apj , 565 , l71 malhotra , s. , wang , j. x. , rhoads , j. e. , heckman , t. m. , & norman , c. a. 2003 , apj , 585 , l25 manners , j. c. , et al . 2003 , mnras , 343 , 293 muller , g. p. , reed , r. , armandroff , t. , boroson , t. a. , & jacoby , g. h. 1998 , proc . spie , 3355 , 577 mushotzky , r. f. , cowie , l. l. , barger , a. j. , & arnaud , k. a. 2000 , @xmath60 , 404 , 459 norman , c , et al . 2002 , apj , 571 , 218 rhoads , j.  e. , malhotra , s. , dey , a. , stern , d. , spinrad , h. , & jannuzi , b.  t.  2000 , , 545 , l85 rhoads , j.  e. , & malhotra , s. 2001 , apj , 563 , l5 rhoads , j.  e. , et al . 2003 , aj , 125 , 1006 rosati , p. , et al . 2002 , apj , 566 , 667 schmidt , m. , schneider , d. p. , & gunn , j. e. 1995 , aj , 110 , 68 stern , d. , et al . 2002a , apjs , 123 , 2223 stern , d. , et al . 2002b , apj , 568 , 71 tozzi , p. 2001a , in proc . marseille 2001 conf . where s the matter l. tresse & m. treyer , astro - ph/0111036 tozzi , p. et al . 2001b , apj , 562 , 42 ueda , y. , et al . 1999 , apj , 518 , 656 valdes , f. g. 2002 , in automated data analysis in astronomy , eds . ranjan gupta , harinder p. singh , and coryn a. l. bailer - jones , ( new delhi : narosa publishing house ) , 309 . vecchi , a. , molendi , s. , guainazzi , m. , fiore , f. , & parmar , a. n. 1999 , a&a , 349 , l73 weisskopf , m. c. , brinkman , b. , canizares , c. , garmire , g. , murray , s. , & van speybroeck , l. p. 2002 , pasp , 114 , 1 yang , y. , mushotzky , r. f. , barger , a. j. , cowie , l. l. , sanders , d. b. , & steffen , a. t. 2003 , apj , 585 , l85      1 & j142620.3 + 35370814:26:20.3635:37:08.7 & 0.2 & @xmath61 & @xmath62 & @xmath63 & tsh & -0.52@xmath64 & @xmath65 & @xmath66 & @xmath67 & 0.3 & -0.1 & @xmath68 & 1.3 + 2 & j142555.5 + 35352814:25:55.5035:35:28.5 & 0.5 & @xmath69 & @xmath70 & @xmath71 & tsh & 0.07@xmath72 & @xmath73 & @xmath74 & @xmath75 & 0.6 & -0.0 & @xmath76 & 1.1 + 3 & j142547.2 + 35362714:25:47.2535:36:27.6 & 0.4 & @xmath77 & @xmath78 & @xmath79 & tsh & -0.27@xmath80 & @xmath81 & @xmath82 & @xmath83 & 0.4 & -0.1 & @xmath84 & 1.2 + 4 & j142547.1 + 35395414:25:47.1035:39:54.9 & 0.2 & @xmath85 & @xmath86 & @xmath87 & tsh & -0.81@xmath88 & @xmath89 & @xmath90 & @xmath91 & 0.2 & -0.1 & @xmath92 & 1.1 + 5 & j142546.4 + 35352214:25:46.4835:35:22.3 & 0.4 & @xmath93 & @xmath94 & @xmath95 & tsh & -0.08@xmath96 & @xmath97 & @xmath98 & @xmath99 & 0.3 & -0.1 & @xmath100 & 1.4 + 6 & j142545.3 + 35344914:25:45.3335:34:49.7 & 0.3 & @xmath101 & @xmath102 & @xmath103 & tsh & -0.19@xmath104 & @xmath105 & @xmath106 & @xmath107 & 0.3 & -0.2 & @xmath108 & 1.0 + 7 & j142543.3 + 35354814:25:43.3135:35:48.1 & 0.4 & @xmath109 & @xmath110 & @xmath111 & tsh & -0.15@xmath112 & @xmath113 & @xmath114 & @xmath113 & -0.1 & -0.4 & @xmath115 & 0.8 + 8 & j142542.5 + 35335814:25:42.5335:33:58.2 & 0.4 & @xmath116 & @xmath117 & @xmath118 & tsh & -0.37@xmath80 & @xmath119 & @xmath120 & @xmath121 & 0.4 & -0.3 & @xmath122 & 0.9 + 9 & j142539.5 + 35335714:25:39.5535:33:57.9 & 0.4 & @xmath123 & @xmath124 & @xmath125 & tsh & -0.43@xmath126 & @xmath127 & @xmath74 & @xmath128 & 0.2 & 0.2 & @xmath2025.7 & ... + 10 & j142538.7 + 35361814:25:38.7235:36:18.0 & 0.4 & @xmath129 & @xmath130 & @xmath131 & ts & -0.32@xmath132 & @xmath133 & @xmath134 & @xmath135 & -0.0 & -0.0 & @xmath136 & 1.1 + 11 & j142537.9 + 35361214:25:37.9435:36:12.0 & 0.3 & @xmath137 & @xmath138 & @xmath139 & ts & -0.47@xmath140 & @xmath141 & @xmath142 & @xmath143 & 0.4 & -0.3 & @xmath144 & 1.3 + 12 & j142536.3 + 35363414:25:36.3235:36:34.2 & 0.3 & @xmath145 & @xmath146 & @xmath147 & tsh & 0.06@xmath148 & @xmath149 & @xmath150 & @xmath151 & -0.6 & -0.0 & @xmath152 & 1.2 + 13 & j142534.7 + 35340714:25:34.7635:34:07.8 & 0.3 & @xmath153 & @xmath154 & @xmath155 & tsh & 0.26@xmath156 & @xmath157 & @xmath158 & @xmath159 & 0.0 & -0.1 & @xmath160 & 1.0 + 14 & j142533.5 + 35384514:25:33.5135:38:45.6 & 0.3 & @xmath161 & @xmath162 & @xmath163 & tsh & -0.32@xmath164 & @xmath165 & @xmath166 & @xmath167 & -0.1 & -0.5 & @xmath168 & 1.1 + 15 & j142530.7 + 35391114:25:30.7135:39:11.3 & 0.3 & @xmath169 & @xmath170 & @xmath171 & tsh & 0.12@xmath164 & @xmath172 & @xmath173 & @xmath174 & ... & ... & @xmath2025.7 & ... + 16 & j142529.2 + 35341214:25:29.2435:34:12.2 & 0.4 & @xmath175 & @xmath176 & @xmath177 & ts & -0.66@xmath178 & @xmath179 & @xmath180 & @xmath181 & -0.1 & -0.0 & @xmath182 & 1.1 + 17 & j142525.4 + 35362214:25:25.4035:36:22.8 & 0.5 & @xmath183 & @xmath184 & @xmath185 & tsh & 0.11@xmath186 & @xmath187 & @xmath188 & @xmath189 & 0.2 & -0.1 & @xmath190 & 1.1 + 18 & j142520.7 + 35331114:25:20.7535:33:11.7 & 0.3 & @xmath191 & @xmath192 & @xmath193 & tsh & -0.46@xmath194 & @xmath195 & @xmath196 & @xmath197 & 0.4 & -0.3 & @xmath198 & 1.0 + 19 & j142614.2 + 35363114:26:14.2935:36:31.5 & 1.0 & @xmath199 & @xmath200 & @xmath201 & tsh & -0.55@xmath202 & @xmath203 & @xmath204 & @xmath187 & -0.5 & -0.1 & @xmath205 & 1.1 + 20 & j142614.2 + 35383314:26:14.2135:38:33.1 & 0.6 & @xmath206 & @xmath207 & @xmath208 & tsh & -0.47@xmath209 & @xmath210 & @xmath211 & @xmath212 & 0.5 & -0.0 & @xmath213 & 1.0 + 21 & j142609.5 + 35321314:26:09.5635:32:13.8 & 0.7 & @xmath214 & @xmath215 & @xmath216 & tsh & -0.39@xmath217 & @xmath218 & @xmath219 & @xmath220 & 0.0 & -0.1 & @xmath152 & 1.0 + 22 & j142607.6 + 35335114:26:07.6635:33:51.4 & 0.6 & @xmath221 & @xmath222 & @xmath223 & tsh & 0.82@xmath209 & @xmath224 & @xmath225 & @xmath226 & 0.6 & 0.1 & @xmath227 & ... + 23 & j142605.8 + 35350814:26:05.8335:35:08.7 & 0.4 & @xmath228 & @xmath229 & @xmath230 & tsh & -0.25@xmath217 & @xmath231 & @xmath232 & @xmath233 & 0.1 & -0.1 & @xmath234 & 1.0 + 24 & j142602.4 + 35360514:26:02.4235:36:05.6 & 0.6 & @xmath235 & @xmath236 & @xmath237 & tsh & -0.50@xmath238 & @xmath239 & @xmath240 & @xmath241 & -0.1 & -0.0 & @xmath242 & 1.1 + 25 & j142601.1 + 35415114:26:01.1835:41:51.1 & 0.7 & @xmath243 & @xmath244 & @xmath245 & tsh & -0.26@xmath246 & @xmath247 & @xmath248 & @xmath249 & 0.5 & -0.7 & @xmath250 & 1.1 + 26 & j142557.6 + 35344514:25:57.6535:34:45.9 & 0.4 & @xmath251 & @xmath252 & @xmath103 & tsh & -0.23@xmath253 & @xmath75 & @xmath143 & @xmath254 & 0.0 & 0.1 & @xmath255 & 1.0 + 27 & j142557.7 + 35351214:25:57.7035:35:12.4 & 0.9 & @xmath256 & @xmath257 & @xmath258 & th & 0.60@xmath259 & @xmath260 & @xmath261 & @xmath127 & 0.6 & -0.5 & @xmath262 & 1.1 + 28 & j142556.9 + 35384514:25:56.9435:38:45.1 & 0.5 & @xmath263 & @xmath264 & @xmath265 & tsh & -0.33@xmath238 & @xmath266 & @xmath267 & @xmath268 & 0.2 & -0.3 & @xmath269 & 1.0 + 29 & j142556.3 + 35401814:25:56.3435:40:18.4 & 0.5 & @xmath270 & @xmath271 & @xmath272 & tsh & -0.51@xmath273 & @xmath274 & @xmath275 & @xmath276 & -0.0 & -0.2 & @xmath277 & 1.0 + 30 & j142555.9 + 35324014:25:55.9535:32:40.6 & 0.5 & @xmath278 & @xmath279 & @xmath280 & tsh & -0.23@xmath238 & @xmath281 & @xmath282 & @xmath283 & 0.1 & 0.2 & @xmath284 & 1.0 + 31 & j142555.4 + 35365014:25:55.4035:36:50.4 & 0.7 & @xmath285 & @xmath286 & @xmath287 & ts & -0.56@xmath288 & @xmath289 & @xmath290 & @xmath291 & 0.4 & -0.4 & @xmath2025.7 & ... + 32 & j142554.1 + 35323714:25:54.1135:32:37.1 & 0.5 & @xmath292 & @xmath293 & @xmath294 & tsh & -0.08@xmath164 & @xmath295 & @xmath296 & @xmath297 & -0.1 & -0.4 & @xmath298 & 0.9 + 33 & j142553.8 + 35382614:25:53.8035:38:26.0 & 0.6 & @xmath299 & @xmath300 & @xmath301 & tsh & -0.25@xmath302 & @xmath303 & @xmath304 & @xmath305 & -0.5 & -0.5 & @xmath306 & 0.8 + 34 & j142553.6 + 35331414:25:53.6835:33:14.9 & 0.3 & @xmath307 & @xmath308 & @xmath309 & tsh & -0.60@xmath310 & @xmath311 & @xmath312 & @xmath313 & -0.0 & -0.2 & @xmath314 & 1.0 + 35 & j142552.7 + 35344814:25:52.7235:34:48.2 & 0.7 & @xmath315 & @xmath316 & @xmath317 & ts & -0.54@xmath318 & @xmath319 & @xmath134 & @xmath320 & -0.3 & 0.2 & @xmath321 & 1.1 + 36 & j142552.4 + 35373014:25:52.4535:37:30.3 & 0.5 & @xmath322 & @xmath258 & @xmath323 & ts & -0.39@xmath324 & @xmath181 & @xmath325 & @xmath326 & -1.1 & -0.6 & @xmath327 & 1.3 + 37 & j142552.2 + 35382314:25:52.2735:38:23.7 & 0.4 & @xmath328 & @xmath329 & @xmath330 & th & 0.72@xmath331 & @xmath332 & @xmath134 & @xmath333 & ... & ... & ... @xmath334 & ... + 38 & j142551.3 + 35340414:25:51.3835:34:04.4 & 0.4 & @xmath335 & @xmath336 & @xmath337 & ts & -0.70@xmath178 & @xmath338 & @xmath180 & @xmath339 & 0.1 & -0.1 & @xmath340 & 1.3 + 39 & j142551.0 + 35330714:25:51.0035:33:07.2 & 0.8 & @xmath341 & @xmath342 & @xmath343 & ts & -0.39@xmath302 & @xmath344 & @xmath345 & @xmath99 & 0.0 & -0.6 & @xmath346 & 1.0 + 40 & j142550.8 + 35303314:25:50.8135:30:33.6 & 1.0 & @xmath347 & @xmath348 & @xmath349 & tsh & -0.66@xmath350 & @xmath351 & @xmath352 & @xmath353 & 0.2 & -0.2 & @xmath354 & 1.0 + 41 & j142550.6 + 35374314:25:50.6735:37:43.1 & 0.5 & @xmath355 & @xmath356 & @xmath323 & ts & -0.50@xmath357 & @xmath358 & @xmath359 & @xmath360 & 0.1 & -0.0 & @xmath361 & 1.0 + 42 & j142550.4 + 35324714:25:50.4935:32:47.9 & 0.8 & @xmath362 & @xmath363 & @xmath364 & ts & -0.53@xmath365 & @xmath121 & @xmath366 & @xmath367 & 0.0 & -0.1 & @xmath368 & 1.0 + 43 & j142549.9 + 35320314:25:49.9035:32:03.8 & 0.5 & @xmath369 & @xmath370 & @xmath371 & tsh & -0.41@xmath372 & @xmath373 & @xmath374 & @xmath375 & 0.1 & -0.1 & @xmath376 & 1.1 + 44 & j142549.8 + 35361914:25:49.8135:36:19.0 & 0.6 & @xmath377 & @xmath378 & @xmath110 & th & 0.93@xmath379 & @xmath74 & @xmath380 & @xmath381 & 0.6 & -0.4 & @xmath382 & 1.1 + 45 & j142549.2 + 35361514:25:49.2635:36:15.3 & 0.6 & @xmath383 & @xmath384 & @xmath385 & ts & -0.44@xmath386 & @xmath387 & @xmath388 & @xmath389 & 0.3 & 0.1 & @xmath2025.7 & ... + 46 & j142548.5 + 35350714:25:48.5835:35:07.8 & 0.4 & @xmath390 & @xmath391 & @xmath300 & tsh & 0.02@xmath392 & @xmath393 & @xmath389 & @xmath394 & -0.1 & -0.4 & @xmath395 & 1.4 + 47 & j142548.2 + 35304114:25:48.2135:30:41.1 & 0.4 & @xmath396 & @xmath397 & @xmath398 & tsh & -0.27@xmath273 & @xmath399 & @xmath400 & @xmath401 & 0.2 & 0.1 & @xmath402 & 0.7 + 48 & j142547.6 + 35304314:25:47.6735:30:43.0 & 0.7 & @xmath403 & @xmath404 & @xmath405 & th & 0.43@xmath406 & @xmath393 & @xmath407 & @xmath408 & 0.3 & -0.4 & @xmath409 & 1.1 + 49 & j142547.2 + 35372814:25:47.2535:37:28.0 & 0.9 & @xmath410 & @xmath131 & @xmath411 & t & -0.04@xmath412 & @xmath188 & @xmath413 & @xmath414 & ... & ... & @xmath2025.7 & ... + 50 & j142546.9 + 35324014:25:46.9535:32:40.3 & 0.5 & @xmath415 & @xmath416 & @xmath417 & tsh & -0.59@xmath418 & @xmath419 & @xmath99 & @xmath420 & -0.0 & -0.4 & @xmath421 & 2.0 + 51 & j142546.3 + 35334914:25:46.3335:33:49.4 & 0.8 & @xmath422 & @xmath423 & @xmath424 & t & 0.56@xmath425 & @xmath426 & @xmath427 & @xmath428 & ... & ... & @xmath2025.7 & ... + 52 & j142546.1 + 35335414:25:46.1335:33:54.9 & 0.4 & @xmath429 & @xmath430 & @xmath316 & tsh & -0.12@xmath431 & @xmath432 & @xmath433 & @xmath434 & 0.1 & -0.6 & @xmath2025.7 & ... + 53 & j142546.0 + 35382614:25:46.0235:38:26.3 & 0.5 & @xmath435 & @xmath430 & @xmath436 & tsh & 0.20@xmath437 & @xmath438 & @xmath325 & @xmath439 & 0.3 & -0.8 & @xmath440 & 0.9 + 54 & j142545.8 + 35384914:25:45.8535:38:49.2 & 0.4 & @xmath441 & @xmath138 & @xmath442 & tsh & -0.30@xmath443 & @xmath444 & @xmath445 & @xmath446 & 0.6 & -0.3 & @xmath447 & 1.4 + 55 & j142545.7 + 35322814:25:45.7835:32:28.4 & 0.7 & @xmath448 & @xmath449 & @xmath450 & ts & -1.00@xmath451 & @xmath452 & @xmath291 & @xmath453 & 0.1 & -0.2 & @xmath454 & 1.0 + 56 & j142545.6 + 35315214:25:45.6935:31:52.9 & 0.4 & @xmath455 & @xmath456 & @xmath457 & tsh & -0.38@xmath238 & @xmath149 & @xmath458 & @xmath459 & -0.1 & -0.0 & @xmath460 & 1.0 + 57 & j142545.1 + 35361614:25:45.1735:36:16.3 & 0.8 & @xmath130 & @xmath461 & @xmath462 & t & 0.34@xmath463 & @xmath387 & @xmath464 & @xmath465 & 0.2 & -0.5 & @xmath466 & 1.2 + 58 & j142544.7 + 35395414:25:44.7035:39:54.1 & 0.8 & @xmath467 & @xmath468 & @xmath469 & tsh & -0.19@xmath470 & @xmath471 & @xmath359 & @xmath472 & 0.0 & -0.2 & @xmath473 & 1.0 + 59 & j142541.6 + 35410714:25:41.6635:41:07.2 & 0.7 & @xmath474 & @xmath475 & @xmath476 & ts & -0.38@xmath477 & @xmath119 & @xmath478 & @xmath420 & 0.4 & 0.5 & @xmath479 & 1.1 + 60 & j142538.7 + 35334214:25:38.7335:33:42.1 & 0.4 & @xmath480 & @xmath481 & @xmath482 & tsh & -0.01@xmath483 & @xmath484 & @xmath134 & @xmath485 & -0.0 & -0.3 & @xmath486 & 1.1 + 61 & j142538.5 + 35342914:25:38.5135:34:29.9 & 0.4 & @xmath487 & @xmath488 & @xmath489 & th & 0.57@xmath490 & @xmath491 & @xmath492 & @xmath187 & 0.2 & -0.4 & @xmath493 & 1.0 + 62 & j142538.2 + 35343814:25:38.2935:34:38.0 & 0.4 & @xmath494 & @xmath495 & @xmath496 & tsh & -0.36@xmath497 & @xmath472 & @xmath304 & @xmath498 & 0.2 & -0.2 & @xmath499 & 1.1 + 63 & j142537.1 + 35430914:25:37.1535:43:09.8 & 1.3 & @xmath500 & @xmath501 & @xmath502 & ts & -0.56@xmath503 & @xmath504 & @xmath505 & @xmath240 & 0.5 & -0.4 & @xmath506 & 1.1 + 64 & j142536.9 + 35320914:25:36.9935:32:09.3 & 0.4 & @xmath507 & @xmath170 & @xmath508 & tsh & -0.41@xmath202 & @xmath509 & @xmath498 & @xmath510 & 0.4 & -0.3 & @xmath511 & 1.1 + 65 & j142535.9 + 35410714:25:35.9935:41:07.1 & 0.3 & @xmath512 & @xmath513 & @xmath514 & tsh & -0.40@xmath194 & @xmath515 & @xmath516 & @xmath517 & 0.2 & -0.2 & @xmath100 & 1.0 + 66 & j142534.5 + 35355114:25:34.5235:35:51.3 & 0.4 & @xmath518 & @xmath130 & @xmath519 & ts & -0.54@xmath520 & @xmath326 & @xmath521 & @xmath304 & 0.1 & 0.1 & @xmath522 & 1.2 + 67 & j142533.8 + 35413814:25:33.8035:41:38.1 & 0.7 & @xmath523 & @xmath524 & @xmath525 & tsh & -0.46@xmath372 & @xmath333 & @xmath526 & @xmath527 & -0.1 & -0.3 & @xmath528 & 1.0 + 68 & j142533.0 + 35364814:25:33.0935:36:48.5 & 0.5 & @xmath529 & @xmath530 & @xmath531 & tsh & -0.45@xmath532 & @xmath533 & @xmath366 & @xmath534 & 0.2 & -0.0 & @xmath535 & 0.8 + 69 & j142531.1 + 35392114:25:31.1735:39:21.6 & 0.6 & @xmath536 & @xmath537 & @xmath538 & th & 0.73@xmath539 & @xmath540 & @xmath541 & @xmath542 & ... & ... & @xmath2025.7 & ... + 70 & j142530.6 + 35342014:25:30.6335:34:20.3 & 0.3 & @xmath543 & @xmath544 & @xmath356 & tsh & -0.42@xmath545 & @xmath157 & @xmath546 & @xmath547 & ... & ... & @xmath2025.7 & ... + 71 & j142529.9 + 35364014:25:29.9135:36:40.0 & 0.4 & @xmath548 & @xmath549 & @xmath550 & ts & -0.53@xmath551 & @xmath150 & @xmath552 & @xmath553 & 0.1 & -0.5 & @xmath554 & 0.8 + 72 & j142529.2 + 35324814:25:29.2235:32:48.4 & 0.4 & @xmath555 & @xmath556 & @xmath258 & tsh & -0.47@xmath557 & @xmath558 & @xmath559 & @xmath560 & ... & ... & @xmath2025.7 & ... + 73 & j142526.6 + 35314014:25:26.6835:31:40.8 & 0.8 & @xmath561 & @xmath562 & @xmath563 & tsh & -0.13@xmath564 & @xmath565 & @xmath553 & @xmath566 & ... & ... & @xmath2025.7 & ... + 74 & j142525.7 + 35384114:25:25.7235:38:41.5 & 0.4 & @xmath87 & @xmath110 & @xmath567 & tsh & 0.72@xmath568 & @xmath569 & @xmath114 & @xmath570 & 0.6 & -0.5 & @xmath571 & 1.9 + 75 & j142524.7 + 35303714:25:24.7035:30:37.1 & 0.5 & @xmath572 & @xmath573 & @xmath574 & tsh & -0.54@xmath575 & @xmath576 & @xmath408 & @xmath577 & 0.7 & 0.1 & @xmath578 & 1.1 + 76 & j142523.6 + 35282414:25:23.6935:28:24.5 & 0.7 & @xmath579 & @xmath580 & @xmath581 & tsh & 0.62@xmath194 & @xmath582 & @xmath583 & @xmath584 & 0.2 & -0.1 & @xmath585 & 1.1 + 77 & j142521.8 + 35340714:25:21.8735:34:07.8 & 0.5 & @xmath586 & @xmath363 & @xmath322 & tsh & -0.14@xmath72 & @xmath587 & @xmath588 & @xmath587 & 0.1 & -0.4 & @xmath589 & 1.0 + 78 & j142521.3 + 35302914:25:21.3835:30:29.5 & 0.9 & @xmath590 & @xmath591 & @xmath592 & tsh & 0.42@xmath593 & @xmath594 & @xmath345 & @xmath595 & -0.4 & -0.2 & @xmath596 & 1.1 + 79 & j142517.7 + 35382214:25:17.7035:38:22.2 & 0.7 & @xmath597 & @xmath598 & @xmath109 & tsh & -0.19@xmath564 & @xmath599 & @xmath600 & @xmath601 & 0.5 & -0.3 & @xmath602 & 1.8 + 80 & j142514.3 + 35391814:25:14.3735:39:18.2 & 0.6 & @xmath603 & @xmath604 & @xmath605 & tsh & -0.21@xmath606 & @xmath607 & @xmath608 & @xmath609 & 0.5 & -0.9 & @xmath610 & 1.2 + 81 & j142514.3 + 35361814:25:14.3435:36:18.8 & 0.4 & @xmath611 & @xmath612 & @xmath613 & tsh & -0.59@xmath310 & @xmath311 & @xmath614 & @xmath615 & 0.1 & -0.2 & @xmath255 & 1.2 + 82 & j142513.1 + 35332314:25:13.1835:33:23.4 & 0.6 & @xmath616 & @xmath617 & @xmath618 & tsh & -0.50@xmath372 & @xmath619 & @xmath620 & @xmath621 & 0.4 & -0.3 & @xmath585 & 1.4 + 83 & j142512.0 + 35312414:25:12.0035:31:24.3 & 0.7 & @xmath622 & @xmath623 & @xmath624 & tsh & -0.53@xmath625 & @xmath626 & @xmath627 & @xmath628 & 0.6 & 0.1 & @xmath629 & 1.0 + 84 & j142511.3 + 35385714:25:11.3235:38:57.8 & 0.6 & @xmath630 & @xmath631 & @xmath632 & tsh & -0.47@xmath310 & @xmath633 & @xmath634 & @xmath635 & -0.2 & 0.2 & @xmath636 & 1.5 + 85 & j142509.3 + 35435614:25:09.3935:43:56.1 & 1.1 & @xmath637 & @xmath638 & @xmath639 & tsh & -0.52@xmath194 & @xmath640 & @xmath641 & @xmath642 & 0.2 & -0.6 & @xmath643 & 1.2 + 86 & j142504.5 + 35410714:25:04.5835:41:07.9 & 0.6 & @xmath644 & @xmath645 & @xmath646 & tsh & -0.42@xmath647 & @xmath648 & @xmath649 & @xmath650 & 0.6 & 0.3 & @xmath651 & 1.1 + 87 & j142457.1 + 35351814:24:57.1635:35:18.8 & 0.9 & @xmath652 & @xmath653 & @xmath654 & tsh & -0.53@xmath246 & @xmath655 & @xmath165 & @xmath656 & 0.5 & -0.7 & @xmath657 & 1.0 + 88 & j142618.8 + 35421814:26:18.8435:42:18.4 & 1.5 & @xmath658 & @xmath659 & @xmath660 & tsh & -0.37@xmath217 & @xmath661 & @xmath662 & @xmath663 & 0.9 & 0.1 & @xmath664 & 1.1 + 89 & j142618.6 + 35375414:26:18.6035:37:54.2 & 2.2 & @xmath665 & @xmath666 & @xmath667 & th & 0.55@xmath668 & @xmath669 & @xmath670 & @xmath671 & -0.3 & -0.7 & @xmath672 & 1.2 + 90 & j142611.9 + 35423014:26:11.9235:42:30.5 & 1.7 & @xmath673 & @xmath674 & @xmath675 & ts & -0.56@xmath253 & @xmath676 & @xmath677 & @xmath678 & 0.6 & -0.0 & @xmath242 & 1.0 + 91 & j142610.8 + 35420214:26:10.8935:42:02.5 & 1.5 & @xmath679 & @xmath680 & @xmath681 & tsh & 0.41@xmath682 & @xmath683 & @xmath684 & @xmath685 & 1.1 & -0.2 & @xmath686 & 1.3 + 92 & j142606.7 + 35315114:26:06.7235:31:51.3 & 1.5 & @xmath687 & @xmath688 & @xmath689 & ts & -0.44@xmath690 & @xmath691 & @xmath484 & @xmath634 & -0.3 & 0.3 & @xmath692 & 1.1 + 93 & j142604.7 + 35301514:26:04.7835:30:15.3 & 1.7 & @xmath693 & @xmath694 & @xmath695 & tsh & 0.10@xmath104 & @xmath696 & @xmath697 & @xmath698 & 1.1 & -0.2 & @xmath699 & 1.2 + 94 & j142603.7 + 35324614:26:03.7335:32:46.2 & 1.6 & @xmath700 & @xmath364 & @xmath701 & t & 0.21@xmath702 & @xmath703 & @xmath704 & @xmath303 & -0.4 & 0.1 & @xmath705 & 1.3 + 95 & j142600.2 + 35344214:26:00.2435:34:42.4 & 0.8 & @xmath706 & @xmath707 & @xmath708 & th & 1.00@xmath709 & @xmath358 & @xmath710 & @xmath711 & 0.3 & -0.6 & @xmath712 & 1.1 + 96 & j142558.1 + 35321614:25:58.1335:32:16.1 & 1.5 & @xmath713 & @xmath714 & @xmath715 & ts & -0.33@xmath716 & @xmath717 & @xmath359 & @xmath697 & ... & ... & @xmath2025.7 & ... + 97 & j142552.4 + 35272414:25:52.4735:27:24.1 & 1.8 & @xmath718 & @xmath719 & @xmath720 & tsh & -0.14@xmath721 & @xmath722 & @xmath526 & @xmath723 & -0.6 & -0.5 & @xmath724 & 1.0 + 98 & j142551.4 + 35343314:25:51.4335:34:33.1 & 0.7 & @xmath118 & @xmath707 & @xmath125 & th & 1.00@xmath725 & @xmath225 & @xmath726 & @xmath727 & 0.1 & -0.1 & @xmath728 & 1.3 + 99 & j142551.1 + 35301514:25:51.1635:30:15.7 & 1.5 & @xmath729 & @xmath730 & @xmath731 & ts & -0.56@xmath732 & @xmath733 & @xmath734 & @xmath133 & 0.1 & 0.2 & @xmath735 & 0.9 + 100 & j142547.4 + 35272014:25:47.4335:27:20.2 & 1.4 & @xmath736 & @xmath737 & @xmath738 & tsh & -0.41@xmath739 & @xmath740 & @xmath741 & @xmath742 & 0.4 & -0.3 & @xmath743 & 1.0 + 101 & j142545.5 + 35300314:25:45.5335:30:03.6 & 1.3 & @xmath744 & @xmath745 & @xmath746 & ts & -0.03@xmath747 & @xmath141 & @xmath748 & @xmath749 & 0.7 & 0.6 & @xmath750 & 1.0 + 102 & j142544.7 + 35404614:25:44.7735:40:46.6 & 1.1 & @xmath448 & @xmath111 & @xmath751 & th & 0.38@xmath752 & @xmath472 & @xmath704 & @xmath187 & 0.1 & -0.7 & @xmath753 & 1.2 + 103 & j142544.2 + 35401814:25:44.2035:40:18.4 & 0.9 & @xmath754 & @xmath755 & @xmath756 & th & 0.86@xmath757 & @xmath727 & @xmath758 & @xmath241 & ... & ... & @xmath2025.7 & ... + 104 & j142541.8 + 35424914:25:41.8035:42:49.7 & 1.3 & @xmath759 & @xmath562 & @xmath760 & tsh & -0.13@xmath564 & @xmath761 & @xmath326 & @xmath615 & -0.9 & 0.6 & @xmath762 & 1.2 + 105 & j142539.6 + 35394214:25:39.6535:39:42.6 & 0.8 & @xmath708 & @xmath763 & @xmath764 & ts & -0.24@xmath765 & @xmath260 & @xmath766 & @xmath498 & 0.4 & -0.5 & @xmath767 & 1.1 + 106 & j142536.8 + 35314714:25:36.8135:31:47.2 & 1.0 & @xmath768 & @xmath769 & @xmath770 & th & 0.63@xmath771 & @xmath772 & @xmath773 & @xmath774 & 0.2 & -0.2 & @xmath775 & 2.0 + 107 & j142533.3 + 35313014:25:33.3335:31:30.6 & 0.8 & @xmath776 & @xmath777 & @xmath778 & th & 0.49@xmath779 & @xmath780 & @xmath781 & @xmath587 & 0.5 & -0.2 & @xmath782 & 1.0 + 108 & j142532.6 + 35283814:25:32.6635:28:38.8 & 1.4 & @xmath783 & @xmath784 & @xmath785 & ts & -0.66@xmath786 & @xmath787 & @xmath788 & @xmath485 & 0.9 & 0.9 & @xmath789 & 1.4 + 109 & j142531.4 + 35445214:25:31.4135:44:52.5 & 2.1 & @xmath790 & @xmath791 & @xmath792 & tsh & 0.35@xmath793 & @xmath794 & @xmath135 & @xmath795 & -0.0 & 1.4 & @xmath796 & 1.2 + 110 & j142530.8 + 35320814:25:30.8235:32:08.6 & 1.1 & @xmath797 & @xmath531 & @xmath798 & t & 0.03@xmath799 & @xmath800 & @xmath114 & @xmath282 & -0.1 & -0.4 & @xmath801 & 1.2 + 111 & j142528.2 + 35395814:25:28.2435:39:58.4 & 0.9 & @xmath802 & @xmath803 & @xmath804 & th & 0.64@xmath805 & @xmath282 & @xmath806 & @xmath807 & 0.5 & -0.3 & @xmath168 & 1.0 + 112 & j142527.5 + 35401214:25:27.5935:40:12.1 & 0.8 & @xmath808 & @xmath809 & @xmath810 & tsh & 0.10@xmath811 & @xmath812 & @xmath766 & @xmath813 & ... & ... & @xmath2025.7 & ... + 113 & j142527.4 + 35310114:25:27.4935:31:01.0 & 1.2 & @xmath814 & @xmath815 & @xmath816 & ts & -0.34@xmath817 & @xmath505 & @xmath818 & @xmath819 & 0.4 & -0.1 & @xmath820 & 1.3 + 114 & j142526.6 + 35332714:25:26.6635:33:27.2 & 0.7 & @xmath821 & @xmath822 & @xmath823 & ts & -0.53@xmath824 & @xmath559 & @xmath114 & @xmath825 & -1.0 & -0.1 & @xmath826 & 1.2 + 115 & j142524.2 + 35292814:25:24.2235:29:28.6 & 1.4 & @xmath827 & @xmath828 & @xmath829 & tsh & -0.14@xmath830 & @xmath691 & @xmath831 & @xmath832 & ... & ... & @xmath2025.7 & ... + 116 & j142523.8 + 35412214:25:23.8035:41:22.4 & 0.8 & @xmath833 & @xmath834 & @xmath835 & ts & -0.59@xmath836 & @xmath594 & @xmath837 & @xmath838 & 0.0 & 0.2 & @xmath839 & 1.0 + 117 & j142523.6 + 35321614:25:23.6935:32:16.7 & 1.1 & @xmath840 & @xmath841 & @xmath436 & tsh & 0.14@xmath842 & @xmath121 & @xmath290 & @xmath843 & 0.6 & -0.5 & @xmath844 & 0.8 + 118 & j142523.0 + 35431314:25:23.0035:43:13.4 & 1.1 & @xmath845 & @xmath846 & @xmath847 & tsh & -0.28@xmath238 & @xmath848 & @xmath849 & @xmath850 & 0.3 & 0.8 & @xmath851 & 1.0 + 119 & j142522.8 + 35311614:25:22.8235:31:16.8 & 1.0 & @xmath852 & @xmath323 & @xmath853 & th & 0.68@xmath854 & @xmath855 & @xmath781 & @xmath856 & 0.7 & -0.2 & @xmath857 & 1.1 + 120 & j142522.4 + 35351714:25:22.4035:35:17.2 & 0.6 & @xmath858 & @xmath859 & @xmath329 & t & 0.40@xmath860 & @xmath819 & @xmath413 & @xmath861 & ... & ... & @xmath2025.7 & ... + 121 & j142521.1 + 35334014:25:21.1035:33:40.0 & 0.7 & @xmath862 & @xmath863 & @xmath317 & ts & -0.73@xmath864 & @xmath780 & @xmath142 & @xmath158 & 0.0 & -0.6 & @xmath865 & 1.1 + 122 & j142517.6 + 35345314:25:17.6135:34:53.0 & 0.5 & @xmath866 & @xmath867 & @xmath868 & ts & -0.20@xmath765 & @xmath434 & @xmath290 & @xmath358 & 0.7 & 0.3 & @xmath869 & 1.0 + & & & & & & & & & & & -0.2 & -1.3 & @xmath870 & 1.3 + 123 & j142516.6 + 35412914:25:16.6735:41:29.6 & 1.3 & @xmath871 & @xmath872 & @xmath873 & ts & -0.44@xmath690 & @xmath504 & @xmath874 & @xmath614 & 0.2 & 0.1 & @xmath875 & 1.2 + 124 & j142516.4 + 35294014:25:16.4335:29:40.7 & 1.2 & @xmath876 & @xmath877 & @xmath878 & tsh & -0.33@xmath879 & @xmath880 & @xmath452 & @xmath881 & 0.2 & 0.8 & @xmath882 & 1.2 + 125 & j142516.0 + 35314214:25:16.0035:31:42.3 & 1.1 & @xmath883 & @xmath884 & @xmath885 & t & -0.22@xmath886 & @xmath465 & @xmath521 & @xmath887 & -0.1 & -0.8 & @xmath888 & 1.0 + 126 & j142514.9 + 35400414:25:14.9035:40:04.1 & 0.9 & @xmath889 & @xmath890 & @xmath891 & tsh & -0.30@xmath690 & @xmath241 & @xmath892 & @xmath400 & 1.0 & 0.2 & @xmath893 & 1.2 + 127 & j142510.9 + 35360214:25:10.9435:36:02.8 & 1.0 & @xmath894 & @xmath895 & @xmath341 & tsh & 0.18@xmath896 & @xmath897 & @xmath734 & @xmath898 & -0.9 & 0.3 & @xmath899 & 1.0 + 128 & j142510.1 + 35341114:25:10.1935:34:11.4 & 0.9 & @xmath900 & @xmath901 & @xmath902 & tsh & -0.23@xmath903 & @xmath73 & @xmath772 & @xmath904 & -0.6 & 0.1 & @xmath905 & 1.2 + 129 & j142509.5 + 35424414:25:09.5135:42:44.9 & 2.1 & @xmath906 & @xmath907 & @xmath908 & th & 0.58@xmath909 & @xmath910 & @xmath366 & @xmath911 & -0.8 & 2.0 & @xmath912 & 1.4 + 130 & j142509.5 + 35374714:25:09.5035:37:47.5 & 0.6 & @xmath913 & @xmath914 & @xmath915 & tsh & 0.42@xmath916 & @xmath917 & @xmath918 & @xmath919 & 0.5 & -0.1 & @xmath920 & 1.2 + 131 & j142509.2 + 35352714:25:09.2335:35:27.5 & 0.8 & @xmath921 & @xmath922 & @xmath923 & tsh & 0.74@xmath924 & @xmath925 & @xmath818 & @xmath926 & -0.3 & -0.0 & @xmath927 & 1.0 + 132 & j142505.1 + 35405414:25:05.1635:40:54.9 & 0.8 & @xmath928 & @xmath929 & @xmath930 & tsh & -0.27@xmath575 & @xmath931 & @xmath419 & @xmath932 & -0.5 & 0.6 & @xmath933 & 1.0 + 133 & j142504.4 + 35351414:25:04.4735:35:14.6 & 1.5 & @xmath934 & @xmath935 & @xmath201 & ts & -0.33@xmath80 & @xmath936 & @xmath937 & @xmath938 & 0.3 & -0.7 & @xmath939 & 1.0 + 134 & j142503.9 + 35334514:25:03.9035:33:45.7 & 1.5 & @xmath940 & @xmath810 & @xmath941 & tsh & 0.37@xmath942 & @xmath943 & @xmath944 & @xmath945 & -0.9 & -0.2 & @xmath946 & 1.0 + 135 & j142503.1 + 35342114:25:03.1635:34:21.2 & 1.2 & @xmath947 & @xmath948 & @xmath949 & tsh & 0.56@xmath950 & @xmath951 & @xmath304 & @xmath952 & 1.1 & 0.5 & @xmath2025.7 & ... + 136 & j142502.9 + 35351214:25:02.9435:35:12.8 & 1.0 & @xmath953 & @xmath954 & @xmath955 & tsh & -0.24@xmath164 & @xmath956 & @xmath957 & @xmath958 & -0.6 & -0.2 & @xmath959 & 1.1 + 137 & j142501.2 + 35362214:25:01.2035:36:22.0 & 1.2 & @xmath960 & @xmath961 & @xmath962 & tsh & -0.42@xmath238 & @xmath373 & @xmath963 & @xmath964 & 0.5 & 0.0 & @xmath965 & 1.0 + 138 & j142457.3 + 35362714:24:57.3335:36:27.5 & 1.2 & @xmath966 & @xmath967 & @xmath968 & tsh & 0.04@xmath969 & @xmath970 & @xmath971 & @xmath972 & 0.5 & 0.2 & @xmath2025.7 & ... + 139 & j142454.8 + 35343114:24:54.8035:34:31.9 & 0.9 & @xmath973 & @xmath974 & @xmath975 & tsh & -0.25@xmath217 & @xmath976 & @xmath977 & @xmath978 & 0.2 & -0.7 & @xmath979 & 1.1 + 140 & j142616.9 + 35372914:26:16.9435:37:29.4 & 1.9 & @xmath980 & @xmath981 & @xmath982 & tsh & 0.35@xmath950 & @xmath983 & @xmath478 & @xmath984 & 0.9 & 0.7 & @xmath985 & 1.5 + 141 & j142613.9 + 35344514:26:13.9735:34:45.5 & 1.6 & @xmath986 & @xmath987 & @xmath988 & ts & -0.50@xmath989 & @xmath990 & @xmath360 & @xmath991 & ... & ... & @xmath2025.7 & ... + 142 & j142601.7 + 35403714:26:01.7235:40:37.5 & 1.3 & @xmath992 & @xmath993 & @xmath994 & ts & -0.28@xmath995 & @xmath141 & @xmath188 & @xmath996 & 0.2 & -0.8 & @xmath997 & 1.0 + 143 & j142601.7 + 35280214:26:01.7135:28:02.8 & 2.7 & @xmath998 & @xmath999 & @xmath1000 & t & 0.17@xmath1001 & @xmath393 & @xmath290 & @xmath1002 & 0.8 & 0.3 & @xmath985 & 1.8 + 144 & j142530.9 + 35275614:25:30.9535:27:56.8 & 2.4 & @xmath1003 & @xmath1004 & @xmath1005 & ts & -0.64@xmath1006 & @xmath1007 & @xmath282 & @xmath1008 & 0.6 & -0.9 & @xmath1009 & 1.3 + 145 & j142527.5 + 35265614:25:27.5335:26:56.2 & 3.1 & @xmath1010 & @xmath1011 & @xmath1012 & ts & -0.67@xmath551 & @xmath1013 & @xmath458 & @xmath1014 & -0.3 & 0.9 & @xmath1015 & 1.1 + 146 & j142524.4 + 35254214:25:24.4035:25:42.1 & 2.5 & @xmath1016 & @xmath1017 & @xmath1018 & ts & -0.27@xmath879 & @xmath1019 & @xmath1020 & @xmath1021 & -0.7 & -0.4 & @xmath1022 & 1.0 + 147 & j142519.7 + 35443214:25:19.7935:44:32.2 & 2.1 & @xmath660 & @xmath1023 & @xmath1024 & ts & -0.43@xmath879 & @xmath1025 & @xmath420 & @xmath1026 & -0.5 & 0.4 & @xmath1027 & 1.0 + 148 & j142517.7 + 35375414:25:17.7135:37:54.3 & 1.1 & @xmath841 & @xmath1028 & @xmath1029 & t & 0.79@xmath1030 & @xmath534 & @xmath758 & @xmath1031 & 0.7 & -0.6 & @xmath1032 & 1.3 + 149 & j142516.0 + 35432514:25:16.0235:43:25.8 & 2.3 & @xmath1033 & @xmath1034 & @xmath1035 & ts & -1.00@xmath1036 & @xmath1037 & @xmath1038 & @xmath1039 & ... & ... & @xmath2025.7 & ... + 150 & j142505.2 + 35372914:25:05.2535:37:29.5 & 1.6 & @xmath1040 & @xmath1041 & @xmath1042 & ts & -0.78@xmath1043 & @xmath352 & @xmath366 & @xmath1044 & 0.2 & -0.2 & @xmath2025.7 & ... + 151 & j142503.5 + 35385914:25:03.5735:38:59.2 & 1.7 & @xmath1045 & @xmath1046 & @xmath700 & ts & -0.20@xmath1047 & @xmath1048 & @xmath553 & @xmath1049 & -0.6 & -0.2 & @xmath1050 & 1.2 + 152 & j142501.5 + 35400014:25:01.5835:40:00.3 & 1.9 & @xmath1051 & @xmath1052 & @xmath1053 & ts & -0.34@xmath690 & @xmath594 & @xmath1054 & @xmath1055 & 1.0 & -1.6 & @xmath1056 & 1.0 + 153 & j142501.2 + 35305714:25:01.2835:30:57.4 & 2.2 & @xmath1057 & @xmath1058 & @xmath1059 & tsh & 0.18@xmath437 & @xmath1060 & @xmath1061 & @xmath1062 & -1.7 & 0.1 & @xmath1063 & 1.0 + 154 & j142459.2 + 35375114:24:59.2435:37:51.4 & 1.8 & @xmath1064 & @xmath1065 & @xmath1066 & ts & -0.21@xmath1067 & @xmath1068 & @xmath135 & @xmath1069 & -0.6 & -0.4 & @xmath1070 & 1.2 + 155 & j142611.8 + 35330114:26:11.8535:33:01.9 & 1.7 & @xmath1071 & @xmath1072 & @xmath1073 & t & 0.83@xmath1074 & @xmath991 & @xmath758 & @xmath904 & -0.4 & 0.6 & @xmath1075 & 1.1 + 156 & j142540.2 + 35462314:25:40.2135:46:23.0 & 3.8 & @xmath1076 & @xmath1077 & @xmath1078 & t & 0.57@xmath1079 & @xmath1080 & @xmath1061 & @xmath1081 & -0.7 & 1.1 & @xmath1082 & 1.6 + 157 & j142539.8 + 35443814:25:39.8735:44:38.6 & 2.4 & @xmath1083 & @xmath1084 & @xmath1085 & t & 0.23@xmath1086 & @xmath394 & @xmath552 & @xmath1087 & -1.3 & 0.4 & @xmath1088 & 1.2 + 158 & j142531.6 + 35265914:25:31.6035:26:59.0 & 3.5 & @xmath1089 & @xmath1090 & @xmath1091 & th & 0.69@xmath1092 & @xmath1093 & @xmath944 & @xmath1094 & 2.1 & 2.0 & @xmath1095 & 1.0 + 159 & j142448.4 + 35322714:24:48.4835:32:27.4 & 2.8 & @xmath1096 & @xmath1097 & @xmath1098 & t & -0.29@xmath1099 & @xmath1100 & @xmath432 & @xmath1101 & -0.6 & 1.0 & @xmath1102 & 1.1 + 160 & j142447.8 + 35313814:24:47.8035:31:38.8 & 3.3 & @xmath1103 & @xmath1104 & @xmath1105 & t & -0.22@xmath1106 & @xmath1107 & @xmath225 & @xmath990 & ... & ... & ... @xmath334 & ... + 161 & j142528.8 + 35334214:25:28.8035:33:42.0 & 0.6 & @xmath1108 & @xmath1109 & @xmath1110 & s & -0.50@xmath1111 & @xmath82 & @xmath1112 & @xmath290 & 0.6 & -0.1 & @xmath1113 & 1.3 + 162 & j142558.2 + 35314414:25:58.2935:31:44.4 & 1.6 & @xmath1114 & @xmath364 & @xmath1115 & s & 0.04@xmath1116 & @xmath465 & @xmath1117 & @xmath1118 & 0.5 & -0.2 & @xmath1119 & 1.3 + 163 & j142458.1 + 35391914:24:58.1435:39:19.4 & 2.5 & @xmath1120 & @xmath1121 & @xmath1122 & s & -0.32@xmath1123 & @xmath127 & @xmath1038 & @xmath121 & 0.8 & 0.1 & @xmath321 & 0.9 + 164 & j142535.9 + 35310214:25:35.9635:31:02.8 & 1.1 & @xmath1124 & @xmath1125 & @xmath1126 & h & 1.00@xmath1127 & @xmath181 & @xmath1128 & @xmath587 & -0.2 & -0.4 & @xmath1129 & 1.5 + 165 & j142527.4 + 35325714:25:27.4635:32:57.9 & 0.6 & @xmath1130 & @xmath707 & @xmath125 & h & 1.00@xmath1131 & @xmath135 & @xmath710 & @xmath1132 & 0.8 & -0.6 & @xmath1133 & 1.3 + 166 & j142545.4 + 35271114:25:45.4435:27:11.8 & 2.5 & @xmath1134 & @xmath1135 & @xmath1136 & h & 0.89@xmath1137 & @xmath1138 & @xmath427 & @xmath1139 & -1.9 & -0.0 & @xmath1140 & 1.2 + 167 & j142523.4 + 35351214:25:23.4935:35:12.4 & 0.7 & @xmath715 & @xmath1125 & @xmath1141 & h & 1.00@xmath1142 & @xmath158 & @xmath1128 & @xmath1118 & 0.1 & -0.4 & @xmath1143 & 1.3 + 168 & j142621.6 + 35393114:26:21.6335:39:31.1 & 3.2 & @xmath1144 & @xmath1145 & @xmath1146 & h & 0.87@xmath1147 & @xmath439 & @xmath427 & @xmath1148 & 1.4 & -2.1 & @xmath2025.7 & ... +
we present an analysis of a deep , 172 ks @xmath0 observation of the large area lyman alpha survey ( lala ) botes field , obtained with the advanced ccd imaging spectrometer ( acis - i ) on the @xmath0 x - ray observatory . 
 this is one of the deepest @xmath0 images of the extragalactic sky ; only the 2 ms cdf - n and 1 ms cdf - s are substantially deeper . in this paper 
 we present the x - ray source catalog obtained from this image , along with an analysis of source counts , and optical identifications . 
 the x - ray image is composed of two individual observations obtained in 2002 , and reaches 0.5  2.0 and 2.0  10.0 kev flux limits of 1.5 @xmath1 10@xmath2 and 1.0 @xmath1 10@xmath3 ergs @xmath4 s@xmath5 , respectively , for point sources near the aim point . 
 a total of 168 x - ray sources were detected : 160 in the 0.5  7.0 kev band , 132 in the 0.5  2.0 kev band , and 111 in the 2.0  7.0 kev band . the x - ray source counts were derived and compared with those from other @xmath0 deep surveys ; the hard x - ray source density of the lala botes field is 33% higher than that of cdf - s at the flux level of 2.0 @xmath1 10@xmath3 ergs @xmath4 s@xmath5 , confirming the field - to - field variances of the hard band source counts reported by previous studies . 
 the deep exposure resolves @xmath6 72% of the 2.0  10.0 kev x - ray background . 
 our primary optical data are @xmath7-band imaging from noao deep wide - field survey ( ndwfs ) , with limiting magnitude of @xmath7 = 25.7 ( vega , 3@xmath8 , 4  diameter aperture ) . 
 we have found optical counterparts for 152 of the 168 @xmath0 sources ( 90% ) ; 144 of these are detected on the @xmath7-band image , and 8 have optical counterparts in other bands ( either @xmath9,@xmath10,@xmath11,@xmath12 ) . among the @xmath7-band non - detected sources , 
 not more than 11 of them can possibly be at @xmath13 5 , based on the hardness ratios of their x - ray emission and nondetections in bluer bands ( @xmath9,@xmath10 ) . 
 the majority ( @xmath14 76% ) of the x - ray sources are found to have log(@xmath15/@xmath16 ) within 0.0@xmath171 , which are believed to be agns . 
 most of the x - ray faint / optically bright sources ( log(@xmath15/@xmath16 ) @xmath18 -1.0 ) are optically extended , which are low - z normal galaxies or low luminosity agns . 
 there is also a population of sources which are x - ray @xmath19 for their optical magnitudes ( log(@xmath15/@xmath16 ) @xmath20 1.0 ) , which are harder in x - ray and are probably obscured agns .