# Presentation: 070369

## HXD Status/performance and Calibration plan

*Y.Terada *
*on behalf of the Suzaku-HXD team*

## Hard X-ray Detector

- 16 well-type phoswich (GSO) : 40-600 keV

- Wide-band All-sky Monitor (WAM) as a GRB detector

- 64 PIN-Si diodes : 10-70 keV, dE~4keV(FWHM)

## In-orbit Operation (2007)~1.1 PIN HV operation~

- Flare-like event on 28 Jul, 2007

- Low energy noise around LD
- HV (W1) 400V  0V
- 		        300V  400V
- Now it is quiet

- flare

- Noisy&quiet

- One day

## 	Date	    W0/   W1/   W2/  W3

- 	Date	    W0/   W1/   W2/  W3
- 2005/08/17  500V/500V/500V/500V
- 2006/05/25  400V/500V/500V/500V
- 2006/10/03  400V/400V/500V/500V
- Now 		  400V/400V/500V/500V

- Please check
- 	http://www.astro.isas.jaxa.jp/suzaku/log/hxd/

## In-orbit Operation (2007)~1.2 GSO UD operation~

- In-orbit Operation (2007)~1.2 GSO UD operation~

- Sensor

- HXD-AE
- (analog elec.)

- HXD-DE
- (digital elec.)

- AE-DE transfer limitation
- 1k events x 4 line

- Telemetry limitation
- 32/16kbps
- (Data Rate-H/M)

- dead time increase

- data gap / skip

- If saturated,

- HXD sub system

- Spacecraft

- In condition of sun angle, temperature of cold plate of the HXD, charging the battery, etc...

## In-orbit Operation (2007)~1.2 GSO UD operation~

- W3 AD-DE data transfer rate

- UD level
-  changed

- Saruration

- Average rate decreased by ~15%
-  as estimated.
- AE-DE rate saturate at low COR
-  regions even after the UD operation
-  (excluded from the cleaned event).
- In the low COR region, lower energy events than GSO UD dominate the rate.
- No further operations are planned.
-  (Final setting of HXD-AE)

- To avoid the saturation between AE-DE, we checked the setting parameters of the HXD-AE;  on 11/Aug/2007, we changed the upper discrimination level of GSO (>1000 keV  ~800 keV)

- Successfully made the margin of the saturation of the data transfer between the HXD-AE and HXD-DE

## In-orbit Operation (2007)~1.3 WAM gain changed~

- We check the PMT gain of WAM 20 units, every day using annihilation line feature after the SAA passage.

-  Change AMP gain at 10 April 2007,
-   after the mode check on 10 Feb ’07.
-  No impacts on PIN/GSO spectra

## 2. Software Updates (V1.x  V2.x)

- _2.1 Format Changed_
-  Format of WEL event fits file was changed.
-  HXD ftools in HEADAS 6.3-6.4;  **no** backward compatibility to V1.x format files.
-  If you need to analyze ver 1.x products, please use format conversion script
-       provided via
-  		http://suzaku.gsfc.nasa.gov/docs/suzaku/analysis/v2soft.html,
-       and use new ftools.
-  The HXD team strongly suggest to use the ver2.x products with new ftools
-   and CALDB.
- _2.2 GTI Changed_
-  v1.x  GTI includes the time when HXD-AE to –DE transfer is saturated
-  v2.0  The epochs when AE to DE transfer is saturated are excluded in the
- 	      GTI to make cleaned event list.
-  If you want to ignore AE-DE saturation, please make a GTI file by yourself with *hxdgtigen* in fifo_full=no mode, and make cleaned events with the GTI from UFF.

## 2.3 PIN (Software) Threshold changed 

- 2005.08.19 -- 2005.12.30
- 2006.01.04 -- 2006.05.31
- 2006.06.04 -- 2006.10.31
- 2006.11.02 -- 2007.03.31

- 4 sets of ae_hxd_pinthr_YYYYMMDD.fits in CALDB.
-        epoch 1) 2005-08-17 11:00
-        epoch 2) 2006-05-25 13:25
-        epoch 3) 2006-10-03 23:35
-        eopch 4) 2007-07-28 02:00

- discarded by *hxdgrade* with ae_hxd_pinthr.fits
- in making cleaned file

- automatically selected by *hxdpi*.

- Ch

- 10 keV

- 8 keV

## 2.4 GSO gain history

- Energy scale calibration with the annihilation line, activation lines, intrinsic lines.

**(V1.x) GSO Gain History File:**
-     ae_hxd_gsoghf_YYYYMMDD.fits
- 	- list of PHA channel of lines
- 	- one column per 1 day
- 	- sometimes pipe-line proc failed.
- 	- no maintenance now
**(V2.x) GSO Gain History Table:**
-     ae_hxd_gsoght_YYYYMMDD.fits
- 	- products from gsoghf, stable
- 	- list of parameters of gain trend
- 	- drifts by the temperature, short
-           term trend after HV_OFF/ON at
-           SAA passage, are also included
- 	- smaller file size

**We changed the GSO gain history file **
** ****in CALDB after ver 2.0.**

## 	 Please reprocess gso events file by yourself.

- Black: v1.x
- Red :  v2.0 (HEADAS 6.3)
- Green: v2.x (HEADAS 6.4)

- No difference between v1 and v2 products
- Bug in hxdpi for v2.0,v2.1,v2.2 products (which is fixed in the latest release, 6.4)

- Important notes:
- Gain determined in the pipe line process is a tentative value.
- Final gain values will appear  in CALDB area, (every month).
- 	 Please reprocess gso events file by yourself.
- There’s a known bug in *hxdpi* in HEADAS 6.3.x, which is fixed
-   in the latest release HEADAS 6.4 last week (Dec 2007)

## 3. Calibration Updates (2007)

- http://www.astro.isas.jaxa.jp/suzaku/process/caveats/

- _3.1 Current status_

## 3.2 PIN HV=400V data

- In version 2, we can analyze all the PIN data including HV=400V datasets.

- - Response files for epochs
- 	ae_hxd_pinxinome1_20070914.rsp
- 	ae_hxd_pinxinome2_20070914.rsp
- 	ae_hxd_pinxinome3_20070914.rsp
- 	ae_hxd_pinxinome4_20070914.rsp
- - NXB models
-         estimation for selected WEL units (v1.x)  each Unit and HV settings (v2.x)

- 2005/8/17 – 2006/5/25 (e1)

- 2006/5/25 – 2006/10/3(e2)

- 2006/10/3 – now (e3,e4)

**500V**

**400 V**

**400 V**

**500V**

**500V**

- Ver1.x

- Ver2.x

**You can analyze all the data**

## Crab spectra

- Epoch 1. 2005.8.17 -- 2006.5.13
- Epoch 2. 2006.5.13 -- 2006.10.2
- Epoch 3. 2006.10.2 -- 2007.7.28
- Epoch 4. 2007.7.28 -- **

- Epoch	Nominal	gamma		norm (@ 1 keV)		chi2/dof	constant factor%
- 1	XIS	2.11 (±0.01)	11.6 (+0.2,-0.3)	79.6/89		1.16 (±0.01)
- 1	HXD	2.09 (±0.01)	10.9 (+0.3,-0.2)	63.6/83		1.15 (±0.01)
- 2	XIS	2.11 (±0.01)	11.4 (±0.2)	99.3/94		1.15 (±0.01)
- 3	HXD	2.11 (±0.01)	11.0 (+0.2,-0.3)	95.1/81		1.11 (±0.01)
- 4	#

- _Crab spectra_

## 3.3 Energy response of PIN & GSO

- 2005/09/15 XIS nominal Crab

- Black: v1.x products
- Red : v2.x  products (new hxdpi, with GSO arf)

- _3.3 Energy response of PIN & GSO_

- No difference between the v1 and v2 response matrix.
- Please use the v2 rsp for the v2 products.

## 3.4 GSO response

**2007/03/20 HXD nominal, Crab Spectra**

**Nominal GSO response (v2.x)  **

- - Cross normalization PIN : GSO = 1: 0.80
-  Residual ±10% in GSO band
- 			χ2/dof ~ 2.5
-  We need further studies on GSO response

-  We prepared fudge GSO arf file, which is just adjusted to
-    the Crab spectra
- 				χ2/dof ~ 1.5
-  Cross normalization
- PIN :GSO = 1: 1.00 for the dataset of 15 Sep 2005
- PIN :GSO = 1: 0.96 for 20 March 2007 Crab
- 	(caused by the angular response, roll angle)
- - Need more checks on this fudge factor!! Please be careful

**With fudge arf file of GSO  (v2.x)**

****** ****For convenience to use GSO data**

## Another photon index (1)  Crab Pulse On-Off spectrum

- Counts/sec/keV

- ~33 msec

- HXD-PIN

- HXD-GSO

- Crab On-Off spectra which can be fitted with a single power law
- (Γ=1.5,
-   cross normalization PIN:GSO = 1:1)

- Epoch3 HXDnominal 20 ksec

- Pulsed component of Crab

## HXD-PIN

- Counts/sec/keV

- ~151 msec

- HXD-GSO

- Epoch4 XISnominal 39 ksec

- Pulsed component spectra of PSR1509-58

**HXD-PIN**

**HXD-GSO**

- On         Off

- PSR1509-58 On-Off spectra which can be fitted with a single power law (Γ=1.92,
-   cross normalization PIN:GSO = 1:1)

- _Another photon index (2)  PSR B1509-58 Pulse On-Off spectrum_

## cross normalization (XIS: PIN = 1 : 1.12~1.15) the same as v1.x 

- _3.5 cross normalization between the XIS and the HXD_

- cross normalization (XIS: PIN = 1 : 1.12~1.15) the same as v1.x

- 2007/03/20 HXD nomina, Crabl

- χ^2/dof ~ 1.2

**XIS0: PIN: GSO = 1 : 1.12 : 1.07**

- ※ PIN: GSO = 1: 0.96 for this dataset

- NH = 0.33x1022
-  = 2.10
- Norm = 9.54

- ※ Same results on NGC2110
-      (XIS nominal), XIS:PIN=1:1.13

- Ver 2 products

## 3.6 PIN NXB model, updated

- Typical NXB spectrum and LC of a long “Earth” observation (MCG-6-30-15)

**data**
**vs.**
**model**

**SAA passage**

**data**
**vs.**
**model**

- 80 ksec exposure

- _3.6 PIN NXB model, updated_

- Tuned up several parameters on PIN NXB model
- Provided via WWW (ISAS & GOF), as an archive data.
- 		http://www.astro.isas.jaxa.jp/suzaku/analysis/hxd/pinnxb/
- 		ftp://legacy.gsfc.nasa.gov/suzaku/data/background/pinnxb_ver2.0/

**good agreement in 12-70 keV**
**NXBs in SAA path and non-SAA path are well modeled**

**Suzakumemo-2007-09**

## We checked the reproducibility of all available earth data.

**2005/09 ~ 2007/09**

-  **No long-term trend**
** ****s=3.8%, s****stat****=2.0% ********   s****sys****= ****3.2%**** (15-40keV, 10ks exposure each)**

**Suzakumemo-2007-09**

## Comment:  reproducibility after renormalization

- Renormalization of the spectrum using a higher band is proposed for a better NXB estimation. (**suzakumemo-2007-10**)
- The improvement could be canceled by statistical errors in high energy band.
-    check using earth observation with long exposure.

**No significant improvement****. **
** ****(probably due to statistical error)**
**peak-to-peak of the residual is ****~5%****   **
** ****for earth obs. with exposures >40 ks. **

## 3.7 GSO background 

- Background level is almost saturated, as expected

## GSO background for ver 2.x products 

- The model is obtained by fitting the light curve of BGD, by an appropriate formula indicated by the properties of the BGD. (This technique is also available for the PIN background, and a part of released PIN BGD is prepared by this model. ) The model parameters are determined for each 32 energy band. From 1.2 to 2.0, some minor improvement will be done.
**	****- after the PMT gain is determined. ******** normally takes 1.5 months**
**	****- delayed by the bug in hxdpi         ******** please wait for a moment**

- Earth Data

- BGD model

**residual**

**±3%**

- Time bin  10000sec

- Soon, it is available! (End of December 2007)

- Now checking in the HXD team

## 3.8 Timing capability of the HXD

- Pulse profiles

- History of Period of Crab pulsar

- P and P_dot (~4.12×1013 s s-1)
-      consistent with Radio results

- Period (msec)

- Difference (nsec)

-  No problem at 33msec – 103 sec

- Y.Terada etal 2008 PASJ in press

## Simultaneous observation of Crab pulsar (20 March 2007)

- 360±150μsec or
- 270±130μsec (in condition)

- Consistent within
- 100μsec

- Y.Terada+ 2008
- PASJ in press

## 4. WAM status

- Calibration with Crab spectra by the Earth Occultation technique

- Cross calibration with Konus/Wind, RHESSI, Swift BAT
- using GRB events and Solar flares

**Please visit the WAM WWW page (http://www.astro.isas.ac.jp/suzaku/research/HXD-WAM/WAM-GRB/)**

- *** Summary (2005 Ag. -- 2007 Oct.) ***
- confirmed GRB 		317 (194)
- possible  GRB 		223 (97)
- SGR            		68 (6)
- Solar flare    		166 (28)

## 5. Future prospects

- _PIN low energy spectra (<13 keV ____ <10 keV)_

- _PIN effective area_

- _GSO response (without fudge factor)_

- _Reproducibility of NXB model(s)_

- Due to thermal noise around LD channel (heat pipe problem)
- Try to “model” the time variable noise shape (looking for coincidence parameters)

- PIN-XIS cross normalization ~13%
- Tune up parameters in making response matrix via Geant4 Mass Model
- Ground experiments with fright spare PIN diodes

- Energy scale: re-calibration of electronics of HXD-AE
- Tune up parameters in Geant4 Mass Model

- - Many efforts on modeling empirically
- - Study the origin of NXB events by the full simulations
-    of activation events with MGGPOD

## Comments: analyses for diffuse sources 

- Angular response of PIN

- Position from the optical axis (deg)

- diffuse arf(PI) = Σ (arf(PI) x model) / Σ model

- βmodel distribution

- HXD arf:  correction factor to the HXD nominal rsp
- Produced by ***hxdarfgen***
- Not support an image input  Please add arfs by yourself

- Or wait for the next release

## Summary