XIS Non-X-ray BGD Database and Application to Detecting Faint Diffuse X-ray Emissions

1. Al-Ka Mn-Ka Ni-Ka Si-Ka Au-Ma Au-La Au-Lb Mn-Kb XIS0XIS2XIS1XIS3 Ni-Kb XIS2 XIS0 0.04 0.02 0 -0.02 Counts keV-1 5ks exposure no. in time order XIS0 0.04 0.02 ACTY 0 -0.02 5ks exposure no. in time order XIS0 0.04 XIS2 XIS0 0.02 0 -0.02 5ks exposure no. in time order DETY DETY Latitude. ≤ -23 (deg) & Altitude. ≥ 576.5 (km) and Latitude. ≥ 29 (deg) & Altitude. ≥ 577.5 (km) DETX DETX XIS0 XIS1XIS2XIS3 0.1-5.0keV 5.0-14.9keV Count rate COR Model : wabs * ( apec + powerlaw )+apec Galactic&local CXB (a) : 1.72Mpc : 1.37Mpc 0.1 Region → (a) (b) (c) (b) 10-2 DETY Normalized counts s-1 keV-1 10-3 (c) datamodelA3376CXBGalactic 10-4 DETX 10-5 0.5 1 2 5 Energy (keV) Energy (keV) A3376 Galactic&local Temperature (keV) Abundance Temperature (keV) (a) 3.91+/-0.13 0.24+/-0.07 0.259+/-0.012 (b) 3.5+/-0.3 0.18+/-0.16 〃 (c) 3.8+/-1.5 0.3+/-0.8 〃 Rev0.7 (Rev0.6) Total observation data 2005/09/01 ~ 2006/05/21 (2006/03/the last day) ＜Extraction＞ Night Earth observation data [ELV < -5°& DYE_ELV > 100°] （In Night Earth, neither ② nor ③ contribute.） NXB database Total exposure time : 799ks (786ks) N. Tawa, M. Nagai, K. Hayasida, H. Nakamoto, M. Namiki (Osaka-U), H. Yamaguchi (Kyoto-U), E. Miller (MIT), Y. Takei (ISAS/JAXA), T. Mizuno (Hiroshima-U), H. Katayama (JAXA) and the Suzaku Team Abstract One of the advantages the Suzaku XIS(X-ray Imaging Spectrometers) is their low background level. To maximize this advantage, we study the Non-X-ray Background (NXB) in XIS, using the night Earth data. Many fluorescent lines, Al, Si, Au, Ni are observed in the NXB spectra. Positional dependence of the NXB level with ACTY is found. Variations of factor larger than 2 is primarily correlates with the Cut-Off-Rigidity (COR) in the satellite orbit. The NXB database of about 800ks is open to observers. The database can be used as any kind of NXB modeling and subtraction, but we first employ the simplest model using the COR as a parameter. The reproducibility of this NXB model is examined with the same NXB database, dividing for each 5ks exposure chunk. We find large residual to this model in some occasions. Those deviation is removed by imposing a filter with latitude and altitude. The reproducibility of the current NXB model is 6.8-11.6% in 5-12keV band for 5ks exposure. Further improvement is expected. We also show the application of this NXB model to an analysis of cluster outskirt. XIS Non-X-ray BGD Database and Application to Detecting Faint Diffuse X-ray Emissions ３．NXB database reproducibility １．NXB characteristic NXB model with COR The NXB database is a simple event file and flexible use is encouraged. However, for the 1st step, the COR dependence is good to be considered. Thus we prepare a tool to 1) sort the NXB events by the COR value, 2) make the NXB spectra for each COR value, 3) and then make appropriate NXB spectra for a target observation by summing up the CPR sorted spectra with appropriate weights. Schematically the procedure is expressed with the follow equation, where the COR is sorted into n bins. Sw is a kind ofNXB models, for which we examine reproducibility. Low background level in XIS NXB spectra NXB spectra of XIS show fluorescece lines of various elements used in the camera body. Background (NXB+CXB in this plot) level of X-ray CCDs in various mission is compared in terms of the N/S ratio to diffuse emissions. Ti：exposure time of the target observation with ith COR bin Ttotal：total exposure time of target observation Si：spectrum made of the NXB database in the ith COR bin Sw： appropriately weighted NXB spectrum for this target ACTY dependence Reproducibility of the NXB model with COR If we apply the same procedure to a portion of the NXB database, the reproducibility of the NXB model (the simplest version) can be examined. Here we divide the database for each 5ks. Note that 5ks NXB data spans for typically one day or a few days’ duration. ACTY dependence Scattered Mn K in XIS0 (Left) Counting rate averaged for each 5ks (right) Residual to the NXB model described above The NXB level is higher at larger ACTY, for which time spent on the frame store region is longer. The scattered component of Mn K from calibration sources is not negligible in XIS0. c/s in 5-12 keV c/s in 5-12 keV 7.2-7.8keV (Ni-Ka)3.0-7.0keV (Continuum) 55Fe source area The (COR sort) NXB model reproduce the NXB level usually, but it is found that large deviations in some 5ks exposures. We examine various filters (filtering is done by each 32s not by each 5ks) using orbital parameters. It is found that filtering by the satellite latitude and altitude is effective. Excluding the data with the left condition (we here call “orbit filter”) makes the residual clean. Mn-Ka band(5.7-6.0keV) image Cut-off rigidity dependence Altitude(km) latitude The NXB level varies by factor of more than 2. The primary parameter is the Cut-Off-Rigidity (COR) in the satellite orbit. The total exposure of NXB database slightly decreases when orbit filter is applied(800ks→725ks). longitude latitude *) The values are relative fraction to average NXB level in the same band. Counting rate of the XIS1 during a blank sky observation on 2005 September 2nd. Count rate in 5-10keV （ XIS0,1,2,3 ） vs COR The NXB model with COR clearly reduce the reproducibility from ~20% to 8-12% (of the average NXB level in the same band). The orbital filter is effective not only to exclude extraordinary deviation but also to reduce the reproducibility (except for XIS2). The reproducibility of the NXB model with COR is evaluated to be 6.8-11.6% in 5-12keV for 5ks exposure data. For larger exposure, we get smaller systematic errors. The NXB model with COR is the simplest one, and should be improved further employing more parameters. Other Components in the sky XIS background The XIS sky background consists of the NXB, the extragalactic Cosmic X-ray Background (NXB), and local & galactic diffuse X-rays depending on the sky position. In addition, when the telescope FOV is close to the limb of the shining Earth, atmospheric fluorescence lines of N-K and O-K are heavily contaminated. ４．Application to Cluster outskirt Source : A3376_WEST_RELIC Sensor : XIS-0 + XIS-2 + XIS-3 ２．NXB database We made the 1st version of the NXB database consisting of 1) large screened event file for each sensor, 2) a EHK file that has orbital and other useful information as a function of time. The following data selection criteria was used. The data base with associated tools are accessible via Suzaku web page at ISAS/JAXA and GSFC/NASA. Distance from center of A3376: 1.02Mpc 0.5 1 2 5 0.5 1 2 5 Energy (keV)