# Presentation: 268675

## Status of the XIS Orbital Calibration and Softwares

**K. Hayashida****, N. Tawa, M. Nagai, H. Nakajima, M. Uchino, **
**N. Anabuki, S. Katsuda, H. Uchida, H. Tsunemi (Osaka Univ.), **
**H. Matsumoto****, H. Mori, H. Uchiyama, M. Ozawa, T. G. Tsuru, Y. Hyodo, M. Nobukawa, K. Koyama (Kyoto Univ.), **
**T. Dotani, H. Murakami, A. Bamba, M. Ozaki, T.Anada (JAXA),**
**D. Takei, S. Kitamoto (Rikkyo Univ.), **
**T. Kato, S. Maeno, K. Mori (Miyazaki Univ),**
**Y. Ishisaki (TMU), T. Kohmura (Kohgakuinn Univ.),**
**E. Miller, B. LaMarr, S. E. Kissel, ****M. W. Bautz**** (MIT), **
**and the Suzaku Team**

**Notes:**
We are going to report our activity on the XIS calibration in orbit. The work are done by many people, including graduates students.  

## Current Status of the XIS  

- No significant change in the XIS hardware since the last Users’ Meeting 2007May
- SCI-ON for all the observations

- 2%/yr

- 0.4-0.8%/yr

## Ver. 2 Processing & HEASOFT6.4

- Ver. 2 processing started.
- Full processing of the SCI-ON data
- HEASOFT v6.4
- Updates + New software xisnxbgen is introudced
- CALDB updated (as always)

**Processing FTOOLS**

**CALDB for Processing**

**CALDB for Users’ Analysis**

**Analysis FTOOLS**

**Updating Parameters**

**Accuracy Check**

**Data Products for Users **

**Raw Data**

**Science Results **

- Quality of the CCD Data (accuracy of the energy scale etc) is significantly affected by the processing

## Contamination on the XIS OBF until 2007Apr evaluated from E0102 obs. (ver.1.x products) 

- Shown in the 2007May Users Meeting
- & Displayed on the Web in the Technical Description Page

- Previous trend model used in CALDB2006
- Current trend model used in CALDB2007Oct

- Ver.2

- CALDB will be updated at the end of this Dec.

**green = XIS0 2006-10-22**
**black = XIS0 2007-10-25**
**blue = XIS3 2006-10-22**
**red  = XIS3 2007-10-25**

- XIS0,XIS3 spectra of E0102

- Almost Similar

## RXJ1856 observed on 2007Oct

**XIS0**

**XIS3**

- Current
- contami-model
- under-estimate

- Current
- contami-model
- over-estimate

- Observed Spectra of XIS0 and XIS3 agree well.
- No apparent difference in the absorber properties, except for the time evolution.

- XIS1(BI)

- RJX1856

## Contamination N_O vs N_C

- O/C=1/10; offset_N_C=0

- O/C=1/6; offset_N_C=1.27

- *)Error bars are 90% error for 2parameters confidence,i.e., delta 2=4.61

- XIS0(2005)

- XIS1(2005)

- XIS2(2006)

- XIS3(2005)

- XIS2(2005)

- XIS1(2006)

- XIS0(2006)

- XIS3(2006)

## Factor of 2 underestimate below 0.3keV

- Unable to improve the fit only with C & O
- Absorption by Heavier Element
- Absorption by H (or He)    but too much ~1021cm^2
- Constant Factor (Grading Problem at low energy?)

**Tune C and**** ****O absorption only**

**Include absorption by H **

- No apparent edge found

## PKS2155 2007Apr

- Power * Abs
- Index  and NH free & common
- Normalization free &vary independently

**Users may encounter this level of inconsistency among sensors**

## Atmospheric Fluorescence Line    

- When the telescope is looking at the shining Earth or its atmosphere, fluorescence lines of the Earth atmosphere (N-K, O-K) by Solar X-rays are contaminated in the observed spectra.
- Intensity and line ratio depends on the elevation angle from the Earth rim and the Solar activity.

- DAY EARTH
- 0 < DYE_ELV < 5
- 5 < DYE_ELV < 10
- 10 < DYE_ELV < 20
- 20 < DYE_ELV < 30

**N-K**
**(0.39keV)**

**O-K**
**(0.52keV)**

## Detected Intensity of N-K linecan be used to measure the contamination thickness 

## Radial Profile of Contamination from Atmospheric N-K, O-K

- 2005/11/28

- 2006/5/25

- 2007/2/15

- 2007/8/1

**XIS1**

- Model Profile impemented in the current CALDB for xissimarfgen

## Radial Profile of Contamination from Atmospheric O-K for FI-CCD

**2007/8/6**

**2007/1/17**

**2005/11/2**

**2006/4/7**

**XIS0**

- Under investigation

## Cut-Off-Rigidity Dependence of the XIS NXB

- 5.0-14.9keV

- 0.1-5.0keV

- Count rate

- COR

- XIS0 XIS1XIS2 XIS3

- The COR dependence of the NXB can be used to model the XIS NXB.
-  Sort the NXB spectra from the Night Earth Database into each COR bin.
-  Calculate the appropriate weights of each COR bin for a given source observation.
-  Make the NXB spectrum for the given source observation by summing the sorted spectra with appropriate weights.
- Other parameters, such as PINUD of the HXD, can be used instead of the COR.

## 5-12keV NXB (integrated for 5ks) 

**Raw**

**Residual from COR2-Model**

- XIS0

- XIS2

**with “Orbit filter” -2005/9**

- Frequency

**Residual from PINUD-Model**

**Residual from PINUD-Model**

- Tawa et al., 2008
- PASJ in press

## Reproducibility 5-12keV XIS NXB

- 2005Oct-2006Jun (Cut 2005Sep)
- Applying “Orbit Filter”
- 5ks integration
- Duration>>5ks

| Parameter | COR | COR2 | PINUD |
| --- | --- | --- | --- |
| XIS0 | 4.4±0.5% | 3.5±0.7% | 2.8±0.9% |
| XIS1 | 6.6±0.1% | 6.9±0.1% | 4.4±0.1% |
| XIS2 | 5.7±0.4% | 5.7±0.4% | 4.0±0.6% |
| XIS3 | 3.3±0.9% | 2.4±1.2% | 3.8±0.8% |

- We introduced a new COR database

- Tawa et al., 2008

- % of the NXB

## Case Study

- Target is (excess) diffuse emission over XIS FOV with comparable surface density as the average CXB
- Exposure 100ks
- For 5-12keV band integrated counts for the whole area of an FI-CCD
- CXB: 9.7x10-3c/s
- Target Diffuse Emission: 9.7x10-3c/s (assumed)
- NXB: 52 x10-3c/s

- Statistical Error                                ΔIstat =  0.84x10-3 c/s
- Fluctuation of the CXB (estimated) ΔICXB = 1.5x10-3 c/s
- NXB reproducibility (PINUD)           ΔINXB = 1.8 x 10-3 c/s

- Tawa et al., 2008
- PASJ in press

- Comparable

- *) CXB fluctuation dominates when we take 1-7keV band.

## xisnxbgen is introduced HEASOFT6.4to make an appropriate NXB spectra for a given source observation

- 1.  Create an estimated NXB file 'xis1_nxb.pi'
-     in the DET coordinates region 'ds9.reg‘
-     % xisnxbgen xis1_nxb.pi xis1_src.pi DETREG ds9.reg suzaku.orb none
- Create an estimated NXB file 'xis1_nxb.pi‘
-     in the SKY coordinates region 'ds9.reg'
-     including the calibration source area,
-     and an image in the energy range of 274 <= PI <= 548 (1-2 keV).
-     % xisnxbgen xis1_nxb.pi xis1_src.pi SKYREG ds9.reg
-       suzaku.orb suzaku.att pixq_and=0 pi_min=274 pi_max=548

- We (XIS team) had been providing perl scripts and the NXB database independent to the HEASOFT/CALDB.
- The new ftool xisnxbgen is simper to use, and the _NXB data base_ is now included in the CALDB.

- See Detail by fhelp

- We have to update every half a year at least