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usually , astronomers deal with catalogues of _ point _ sources . however , if the source is _ extended _
( i.e. its size is comparable or even bigger than the point spread function of the instrument ) , more sophisticated method of scientific data visualisation is needed . the most common method of such visualisation is building _ sky maps _
 specially processed series of 2-dimensional images in different energy bands .
an example of such map for x - ray astronomy is all - sky map in 0.1 - 2.4  kev band made by rosat x - ray satellite  @xcite observations .
this all - sky map also exists as interactive web - tool  @xcite .
after the end of rosat mission , several missions in kev range have been operating .
these missions have covered a minor part of the sky ( not more than several % ) but with much better sensitivity and wider energy range compared with rosat . in this paper , we present the interactive maps in 2 - 5 and 5 - 10  kev range . for these maps
, we use publicly available observations by mos cameras  @xcite of _ xmm - newton
_  @xcite x - ray mission .
special attention was paid to handle with most important background components , including soft proton flares and quiescent particle background , see  @xcite for detailed properties of _ xmm - newton _  background . the obtained map is included to website of virtual roentgen and gamma observatory in ukraine  .
.general properties of mos observations used in our analysis .
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for constructing sky map , we first downloaded all publically available ( on july  1 , 2013 ) observation data files for mos  @xcite cameras of _ xmm - newton _  x - ray observatory  @xcite available on the heasarc data archive  @xcite .
these data files were processed using _ extended sources analysis software _ ( esas ) package  @xcite specially developed for analysis of extended sources at the nasa / gsfc _ xmm - newton _  guest observer facility  @xcite in cooperation with the _ xmm - newton _  science operation centre  @xcite and the _ xmm - newton _  background working group  @xcite .
it is publically available as part of _ xmm - newton _  science analysis system ( sas ) v.13.5.0 .
the methodology of esas software is based on detailed modeling and/or subtraction of various background components ( see  @xcite for complete list ) experienced by mos and pn cameras on - board _ xmm - newton _  cosmic mission using the `` first principles '' as much as possible . to model instrumental background ,
esas software relies on filter - wheel - closed data and the data from the unexposed corners of archived observations , rather than `` blank sky '' data ( contaminated by unknown level by different variable background components ) used by a number of other methods .
this is essential for analysis of very faint sky regions ( e.g. galaxy cluster outskirts ) dominated by the background ( rather than the source ) emission .
the obtained data products  filtered event  mev ) cosmic rays thus significantly reducing the amount of data telemetry . ]
lists , images , lightcurves and spectra  are produced in fits  @xcite format for user - defined regions within _ xmm - newton _  field - of - view .
our data reduction is started from production of filtered event lists using esas script ` mos - filter ` .
this script effectively removes time intervals affected by highly variable background component 
soft proton flares , see  @xcite .
we used the standard filters and cuts provided by esas software .
for example , we selected single , double , triple and quadruple events ( described by event ` pattern ` @xmath2 ) of highest quality ( described by ` flag ` @xmath3 ) for high - quality spectral analysis . ] .
main parameters for obtained event lists are shown in table  [ tab : obs - properties ] .
the leftover mos event lists were processed by esas scripts ` mos - spectra ` and ` mos_back ` giving observed and modelled quiscent particle background spectra , exposure maps , count images for selected energy ranges and modelled particle background count images .
the resulting images and exposure maps of individual observations are then combined by esas scripts ` merge_comp_xmm ` and ` bin_image_merge ` into count - rate images of sky regions with size @xmath4 and minimal pixel size @xmath5 .
point sources are not excluded , although very bright point sources observed with timing mode ( such as by  cam , see fig .  [
fig : bycam-2 - 5 - 200x200 ] ) havent been processed by esas and therefore do not appear in our map . for the sky map , we chose two energy ranges  2 - 5kev and 5 - 10kev  motivated by their    * negligible contamination by remaining solar wind charge exchange background component , see  @xcite for details ; * complementarity to existing rosat all - sky map  @xcite in 0.1 - 2.4  kev .    for sky map visualisation
, we used the standard nasa ` skyview.jar ` tool  @xcite .
this tool selects appropriate images overlapping with given sky region and samples them to the given pixel size .
the sutherland - hodgman clipping algorithm was used to resample images .
this method treats the output pixel grid as a window over the input images grid and integrates the flux within each output pixel exactly .
the output image can be produced in given sky coordinates and projection .
the obtained images in ` fits `  @xcite format are available for quick look and can be directly downloaded from  http://skyview.virgoua.org .
we constructed sky maps in 2 - 5kev and 5 - 10kev bands using @xmath64000 publically available observations of mos cameras on - board _ xmm - newton _  x - ray cosmic mission .
positions of given observations and their basic properties are shown in fig .
[ fig : obs - positions ] and table  [ tab : obs - properties ] , respectively .
the produced maps are cleaned from variable soft proton component and instrumental background with the help of standard analysis for extended sources 
esas software  @xcite  and included to web - interface of virtual roentgen and gamma - ray observatory in ukraine , http://skyview.virgoua.org , see figs  [ fig : gc-2 - 5 - 200x200 ] and  [ fig : perseus-5 - 10 - 200x200 ] as examples .
the obtained maps cover about 1% of all sky , see fig .
[ fig : obs - positions ] for details .
they are complementary to existing rosat all - sky map in soft x - rays ( 0.1 - 2.4  kev ) as well as usual x - ray catalogues of point sources .
we thank yuri izotov , vladimir savchenko , igor telezhinsky , ievgen vovk and the anonymous referee for their comments and suggestions . this work was supported by part by the program of cosmic research of the national academy of sciences of ukraine , the state programme of implementation of grid technology in ukraine and the grant of president of ukraine for young scientists .
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sky maps are powerful visualisation tools for quicklook analysis of extended sources . 
 the latest sky map in soft x - rays ( 0.1 - 2.4  kev ) has been created in 90ies using rosat data . by analyzing publically available data from _ xmm - newton _   x - ray mission we constructed new sky maps in two energy bands  2 - 5kev and 5 - 10kev , complementary to rosat data , covering about 1% of all sky , and included them to our web - based tool http://skyview.virgoua.org . 
 + * key words : x - rays : general , virtual observatory tools *    @xmath0bogolyubov institute of theoretical physics , metrologichna str . 
 14-b , 03680 , kyiv , ukraine + @xmath1national university `` kyiv - mohyla academy '' , skovorody str . 2 , 04070 , kyiv , ukraine + dsavchenko@bitp.kiev.ua