2.1   HEADAS

Before starting the Suzaku analysis, you need to install the latest version of the HEADAS package from lheasoft.

2.2   CALDB

Many Suzaku FTOOLS cannot run without accessing CALDB files.

Go to 2.1 CALDB.

3.1   Make sure the last information

Users should check important events and processing version.

Go to 4.1 Important Events and Processing Version.

Also, users should check any updates.

Go to 4.2 Checking for Updates.

3.2   Obtain the desired data set of your observation

Go to 3.1.1 Retrieving the data

For example, when your OBS_ID is 101005040, you can download whole directory tree with the wget command as follows:

unix% wget -rL -nH --cut-dirs=4 ftp://darts.isas.jaxa.jp/pub/suzaku/ver2.1/101005040

4.1   Download NXB data

Go to 7.5.1 PIN Non X-Ray Background.

4.2   Spectral Analysis

Go to 7.5.6 hxdpinxbpi.

4.3   Timing Analysis

Go to 7.8.1 hxdpinxblc

4.4   Noise Check (if needed)

Go to Caution on the PIN noise increase.

5.1   Download NXB data

You should check New GSO Gain Annouce Page to get appropriate background files.

5.2   Check if reprocess is needed

You should check New GSO Gain Annouce Page to see if you need reprocess your data.

When you need to reprocess the data, then

Go to 5.4.1 Reprocessing and Screening : Aepipeline.

5.3   Spectral Analysis

Go to 7.7.2 hxdgsoxbpi.

5.4   Timing Analysis

Go to 7.9.1 hxdgsoxblc.

6.1   HXD Perl scprits do not work on Mac, why?

HXD Perl scripts refer to 7.5.6 hxdpinxbpi and 7.8.1 hxdpinxblc or 7.7.2 hxdgsoxbpi. and 7.9.1 hxdgsoxblc and also you need 5.4.1 Reprocessing and Screening : Aepipeline for reprocessing your data. All of them are written in Perl scripts, so you should set the following enironmental variable

export LHEAPERL=/usr/bin/perl

for bash users:

setenv LHEAPERL /usr/bin/perl

for tcsh users.

If you do so, then these scripts should work.

6.2   Cross Normalization

Go to 5.7.2 Flux Cross Calibration: XIS and HXD.

Generally, crossnormarization among the three detectors should be as follows.

As for crossnormalization amond the XISs,

Go to 5.7.1 Flux Cross Calibration: XIS0,1,3.

6.3   Systematic Uncertainties on NXB

If you would like to examine the systematic error of the background model for your object, the best way is to extract the NXB spectrum by use of the earth-occulted period and compare it with the model. Please note that there is not always earth-occultation.

You can estimate the duration with the EHK file:

unix% fplot auxil/ae101005040.ehk.gz TIME ELV - /XW pltcmd=" "

(In this example, there is no earth-occultation because this is a very

short observation, actually, the step-point for the large maneuver.)

When the elevation of the source (ELV) is less than -5 degree, the FOV of the detector is occulted by the earth and hence the spectrum during this period can be treated as same as the NXB component. Thus, what you should do is to change ELV>5 into ELV<-5 when extracting data. The procedure can be easily done as follows.

1. Go to 7.3 HXD Reprocessing and Screening: General Remarks and download pin_mkf.sel ( Note that gso_mkf.sel is the same as pin_mkf.sel).
2. Chenge ELV>5 into ELV<-5 in pin_mkf.sel.
3. Run aepipeline with specifying hxd_pin_expr= @pin_mkf.sel hxd_gso_expr= @pin_mkf.sel hxd_pse_expr= @pin_mkf.sel.
4. To compare the earth with the NXB data, go to 7.5.6 hxdpinxbpi and 7.8.1 hxdpinxblc or 7.7.2 hxdgsoxbpi. and 7.9.1 hxdgsoxblc.