Each Suzaku proposal must include at a minimum the source coordinates, exposure time, instrument configuration and expected count rates, and any observing constraints within the four page limit. The review panels will base their decision primarily upon the justification of the proposed science to be done with the data. This chapter describes how to prepare a strong proposal, including the various software tools available to assist the proposer.
One of the first tasks in preparing a proposal is determining when and for how long a target can be observed as there is very little use to simulate a source that cannot be observed. This can be easily done with Viewing, a simple webbased interactive tool (see Appendix B) that can determine visibility for many different satellites. To use Viewing, simply enter the target name or coordinates, and select the satellite. Viewing will return all the available dates when that target is observable.
Another initial check to be performed before starting sophisticated
simulations is to ensure that the target has not yet been extensively
observed by Suzaku, e.g., using Browse. Users should also check
the observations log located at
http://heasarc.gsfc.nasa.gov/docs/suzaku/docs/suzaku/aehp_time_miss.html
as some of the targets (category C) may have been accepted but not
observed.
While it is conceivable that one would wish to study a previously unknown Xray source with Suzaku, a more likely scenario would involve a spectroscopic study of an object with known Xray flux. A viable proposal should state the scientific objective of the observation and show that Suzaku can achieve this objective. Observations that require one or more of Suzaku's unique capabilities would be especially strong candidates.
Every Suzaku proposal must have an estimate of the expected source count rates from the proposed target for all detectors. This rate is used both by the reviewers to evaluate the viability of the proposal and the operations team to evaluate any safety concerns. The simplest tool to use in estimating the expected XIS or HXD count rate is PIMMS. This tool is freely available as a standalone tool or on the web as WebPIMMS (see Appendix B). The next level of detail is provided via simulations using XSPEC, and such simulations should provide significant insight into the expected spectrum obtained from a proposed observation. A brief guide to XSPEC simulations is given in section 5.4. In many cases, this should be sufficient for a point source. There are also tools available to simulate imaging data, which may be useful for an extended source or a particularly bright source. In particular, the most powerful tool is xissim, which can use a FITS format image with an assumed spectral shape of the source to estimate the distribution of events in all elements of the XIS detectors.
PIMMS is an interactive, menudriven program, which has an extensive HELP facility. It is also available as the webbased tool WebPIMMS. In either case, users specify the flux and spectral model with its parameters, and PIMMS/WebPIMMS returns the predicted count rate. PIMMS/WebPIMMS can be used for a variety of other instruments, so if, for instance, the count rate and spectrum of a given source observed with the ROSAT PSPC is known, PIMMS/WebPIMMS can estimate the expected count rates for Suzaku's instruments. The limitations of the input source must be considered carefully. For example, ROSAT had no significant response to Xrays above keV, and so is not useful when estimating the HXD GSO count rate.
Perhaps the easiest tool for simulating Xray spectra is the XSPEC program (a part of the XANADU software package), which is designed to run on a variety of computer platforms and operating systems and is freely distributed on the NASA GSFC HEASARC website (see Appendix B). The simulation of an XIS observation requires the current instrument redistribution matrix (the socalled RMF file) and the energydependent effective area of the instrument (the socalled ARF file), while the simulation of an HXD observation requires the current instrument response (the socalled RSP file). These files are available on the Web or via anonymous FTP (see Appendix B).
The procedure for simulations is relatively simple: if the XSPEC program is installed, one should start XSPEC, making sure that the proper RMF, ARF, and RSP files are accessible. Within XSPEC, one should specify the spectral model, such as hot thermal plasma or the like (via the model command). Specifying the model will drive XSPEC to query for the model parameters (such as the temperature and abundances for an APEC collisional plasma model), as well as its normalization. The key command to create a simulated spectrum is the fakeit command, which will query for the RMF and ARF files, when simulating XIS, or for an RSP file, in the HXD case. The fakeit command will also request the data filename and the length of the observation to be simulated. One can then use the resulting spectrum within XSPEC to determine the sensitivity of the simulated data file to changes in the model parameters. Users should adjust the normalization of their input models to reflect the actual count rate or flux (absorbed or unabsorbed) of their source.
Some of the features of XSPEC are also available as a webbased tool on the HEASARC website (see Appendix B). WebSPEC calls XSPEC behind the scenes, so the description above applies here as well.
After selecting the instrument, WebSPEC allows the user to choose the spectral model, such as an absorbed collisional plasma or a powerlaw spectrum with an absorption component. The next page will then query for the model parameters (such as the temperature and abundances for an APEC collisional plasma model), as well as its normalization. In addition, it queries for the simulation parameters, i.e., the exposure, upper and lower energies, and the number of bins to use in the spectral plot. WebSPEC will then create a simulated spectrum after clicking the ``Show me the Spectrum'' button, using the fakeit command. This folds the specified model through the instrument response and effective area, calculating the observed count rate and fluxes as well. WebSPEC will then allow one to download the postscript file of the spectrum, change the model parameters, or replot the data.
In order to show how to estimate the proper exposure, we include some simple examples of XIS and HXD observations that illustrate the process.
The Local Hot Bubble is the proposed origin for at least some of the 1/4keV emission seen in the ROSAT AllSky Survey at all latitudes. Although Suzaku has some sensitivity at 1/4keV, a more profitable approach to finding this emission is to detect the OVII emission that should accompany it. In this case we need to calculate the expected count rate from the OVII and compare it to the expected background.
We first need the expected flux, based on published papers or the PI's model. In this case, we expect the surface brightness to be 0.34ph/cm/s/sr, based on a number of papers. Since the XIS field of view is , this value corresponds to a total surface brightness in one XIS of ph/cm/s. The next question is the effective area of the XIS instruments at the line energy. OVII is in fact a complex of lines, centered around 0.57keV. Examining the effective area plots for the XIS in Chapter 3, we see that the effective area at 0.57 keV in the BI CCD is cm; for the FI CCDs it is cm. The curves shown on Fig. 3.3 do not include the contamination effect. The computation below is only given as an example. Please note that the more current effective area curves for the FI and BI CCDs can also be found by loading their responses into XSPEC and using the plot efficiency command. Warning: The XIS RMF response matrices are not normalized, and thus must be combined with the ARF files to determine the total effective area. With the expected flux and the effective area, we can now determine the expected count rate in the BI and FI CCDs to be 1.3 and 0.87counts/ks. This is obviously a extremely low count rate and so the expected background is very important. The resolution of the XIS is quite good, as shown in Chapter 7, at 0.57keV a bin of width 60eV will contain most of the emission. The XIS background rate (see section 7.3.4 at this energy is only 0.05counts/s/keV in both the FI and BI detectors, so we can expect a background of 3counts/ks. In both the FI and BI detectors the line will be below the background, but this does not intrinsically hinder detection. As will be seen below, in the HXD this is the norm rather than the exception. One aid for this observation is that the OVII line is relatively isolated in this energy range, with the exception of the nearby OVIII line. Assume we wish to detect the OVII feature with significance. The total count rate in the XISS1 (the BI CCD) in our energy band will be 4.3counts/ks, with 3counts/ks of background. In an Nks observation, we will measure the signal to be . To achieve a result, then, we need , or ks.
Another common observation will be to search for faint hard Xray tails from sources such as Xray binaries. We describe here how to simulate such an observation, including the allimportant HXD background systematics, which will dominate all such observations.
The first step is to download the latest versions of the background template files and the response files from the website listed in Appendix B. The HXD website will also describe the current best value for the systematic error in background estimation. For this AO, proposers should carefully read Chapter 8 and evaluate the systematic errors for the PIN and the GSO backgrounds in the energy band of interest, and at the exposure level chosen. For example, for a 100ks exposure, the value for the PIN in the 1540keV band and the GSO in the 50100keV band can be estimated to be 3% and 1.5%, respectively. Since the energy bands are important in this case, the associated errors should first be estimated and then used in the procedure described below. In addition, the proposer should also check if contaminating sources exist in the FOV of the HXD, using existing hard Xray source catalogs from satellites such as RXTEASM, INTEGRAL, and Swift, before beginning this process.
We set up XSPEC for simulating by reading the background template files as both data and background along with the response files:
XSPEC12>data ae_hxd_pinbkg_20101012.pha ae_hxd_gsobkg_20101012.pha 2 spectra in use Spectral Data File: ae_hxd_pinbkg_20101012.pha Spectrum 1 Net count rate (cts/s) for Spectrum:1 4.735e01 +/ 3.973e04 Assigned to Data Group 1 and Plot Group 1 Noticed Channels: 1256 Telescope: SUZAKU Instrument: HXD Channel Type: PI_PIN Exposure Time: 3e+06 sec Using fit statistic: chi No response loaded. Spectral Data File: ae_hxd_gsobkg_20101012.pha Spectrum 2 Net count rate (cts/s) for Spectrum:2 4.397e+01 +/ 3.829e03 Assigned to Data Group 1 and Plot Group 2 Noticed Channels: 1512 Telescope: SUZAKU Instrument: HXD Channel Type: PI_SLOW Exposure Time: 3e+06 sec Using fit statistic: chi No response loaded. ***Warning! One or more spectra are missing responses, and are not suitable for fit. XSPEC12>back ae_hxd_pinbkg_20101012.pha ae_hxd_gsobkg_20101012.pha Net count rate (cts/s) for Spectrum:1 0.000e+00 +/ 5.619e04 (0.0 % total) Net count rate (cts/s) for Spectrum:2 0.000e+00 +/ 5.414e03 (0.0 % total) ***Warning! One or more spectra are missing responses, and are not suitable for fit. XSPEC12>resp ae_hxd_pinxinome9_20100731.rsp ae_hxd_gsoxinom_20100524.rsp Response successfully loaded. Response successfully loaded.
We first create background spectra with the correct statistics, by simulating an observation with no source flux using the fakeit command. In the case of the PIN the simulated background exposure is a factor 10 higher than the exposure of the source observation to be simulated (here 10s), following the prescription for PIN data analysis. In the case of the GSO the simulated background exposure is equal to the exposure of the source observation (here 10s).
XSPEC12>model powerlaw Input parameter value, delta, min, bot, top, and max values for ... 1 0.01( 0.01) 3 2 9 10 1:powerlaw:PhoIndex>1 1 0.01( 0.01) 0 0 1e+24 1e+24 2:powerlaw:norm>0 ======================================================================== Model powerlaw<1> Source No.: 1 Active/On Model Model Component Parameter Unit Value par comp 1 1 powerlaw PhoIndex 1.00000 +/ 0.0 2 1 powerlaw norm 0.0 +/ 0.0 ________________________________________________________________________ ChiSquared = 0.0 using 768 PHA bins. Reduced chisquared = 0.0 for 766 degrees of freedom Null hypothesis probability = 1.000000e+00 ***Warning: Chisquare may not be valid due to bins with zero variance in spectrum number(s): 1 2 Current data and model not fit yet. XSPEC12>fakeit Use counting statistics in creating fake data? (y): Input optional fake file prefix: Fake data file name (ae_hxd_pinbkg_20101012.fak): pin_10mCrab_1Ms.bkg Exposure time, correction norm, bkg exposure time (3.00000e+06, 1.00000, 3.00000e+06): 1000000 Fake data file name (ae_hxd_gsobkg_20101012.fak): gso_10mCrab_100ks.bkg Exposure time, correction norm, bkg exposure time (3.00000e+06, 1.00000, 3.00000e+06): 100000 No ARF will be applied to fake spectrum #1 source #1 No ARF will be applied to fake spectrum #2 source #1 2 spectra in use ChiSquared = 637.77 using 768 PHA bins. Reduced chisquared = 0.83260 for 766 degrees of freedom Null hypothesis probability = 9.997317e01 ***Warning: Chisquare may not be valid due to bins with zero variance in spectrum number(s): 1 2 Current data and model not fit yet.
Now we assume a spectrum for our source; here, we use a Crablike spectrum (Toor & Seward 1974 AJ, 79, 995) with a photon index of 2.1, a hydrogen column density N of 310cm, and 10mCrab flux. This can be set up in XSPEC via the following commands (note that while the response files are still present from the previous step, the simulated background files from the previous step should be loaded as background files, and the data files do not matter):
XSPEC12>back pin_10mCrab_1Ms.bkg gso_10mCrab_100ks.bkg Net count rate (cts/s) for Spectrum:1 2.101e17 +/ 9.723e04 (0.0 % total) Net count rate (cts/s) for Spectrum:2 3.640e15 +/ 2.965e02 (0.0 % total) ChiSquared = 3e26 using 768 PHA bins. Reduced chisquared = 4e29 for 766 degrees of freedom Null hypothesis probability = 1.000000e+00 ***Warning: Chisquare may not be valid due to bins with zero variance in spectrum number(s): 1 2 Current data and model not fit yet. XSPEC12>model phabs*powerlaw Input parameter value, delta, min, bot, top, and max values for ... 1 0.001( 0.01) 0 0 100000 1e+06 1:phabs:nH>0.3 1 0.01( 0.01) 3 2 9 10 2:powerlaw:PhoIndex>2.1 1 0.01( 0.01) 0 0 1e+24 1e+24 3:powerlaw:norm>0.097 ======================================================================== Model phabs<1>*powerlaw<2> Source No.: 1 Active/On Model Model Component Parameter Unit Value par comp 1 1 phabs nH 10^22 0.300000 +/ 0.0 2 2 powerlaw PhoIndex 2.10000 +/ 0.0 3 2 powerlaw norm 9.70000E02 +/ 0.0 ________________________________________________________________________ ChiSquared = 184046.2 using 768 PHA bins. Reduced chisquared = 240.5832 for 765 degrees of freedom Null hypothesis probability = 0.000000e+00 ***Warning: Chisquare may not be valid due to bins with zero variance in spectrum number(s): 1 2 Current data and model not fit yet.
Now we can create fake PIN and GSO data for the planned observation using the fakeit command. The result will be simulated spectral files which include the instrumental background, effective area, and resolution:
XSPEC12>fakeit Use counting statistics in creating fake data? (y): Input optional fake file prefix: Fake data file name (pin_10mCrab_1Ms.fak): pin_10mCrab_100ks.fak Exposure time, correction norm, bkg exposure time (1.00000e+06, 1.00000, 1.00000e+06): 100000 Fake data file name (gso_10mCrab_100ks.fak): gso_10mCrab_100ks.fak Exposure time, correction norm, bkg exposure time (100000., 1.00000, 100000.): 100000 No ARF will be applied to fake spectrum #1 source #1 No ARF will be applied to fake spectrum #2 source #1 2 spectra in use ChiSquared = 660.11 using 768 PHA bins. Reduced chisquared = 0.86289 for 765 degrees of freedom Null hypothesis probability = 9.974261e01 ***Warning: Chisquare may not be valid due to bins with zero variance in spectrum number(s): 1 2 Current data and model not fit yet.
At this point we have created simulated spectral files for an
observation of a 10mCrab XRB, pin_10mCrab_100ks.fak and gso_10mCrab_100ks.fak. In order to achieve the statistics of an
actual observations, these files have to be rebinned to the spectral
binning of the regularly created GSO background files. A grouping file
which can be used with the FTOOL grppha is available
from
http://heasarc.gsfc.nasa.gov/docs/suzaku/analysis/gsobgd64bins.dat:
grppha gso_10mCrab_100ks.fak gso_10mCrab_100ks_bin.fak  MANDATORY KEYWORDS/VALUES    EXTNAME  SPECTRUM Name of this BINTABLE TELESCOP  SUZAKU Mission/Satellite name INSTRUME  HXD Instrument/Detector FILTER  Instrument filter in use EXPOSURE  1.00000E+05 Integration time (in secs) of PHA data AREASCAL  1.0000 Area scaling factor BACKSCAL  1.0000 Background scaling factor BACKFILE  gso_10mCrab_100ks_bkg.fak CORRSCAL  1.0000 Correlation scaling factor CORRFILE  NONE Associated correlation file RESPFILE  ae_hxd_gsoxinom_20100524.rsp ANCRFILE  NONE Associated ancillary response file POISSERR  TRUE Whether Poissonian errors apply CHANTYPE  PI_SLOW Whether channels have been corrected TLMIN1  0 First legal Detector channel DETCHANS  512 No. of legal detector channels NCHAN  512 No. of detector channels in dataset PHAVERSN  1.1.0 OGIP FITS version number STAT_ERR  FALSE Statistical Error SYS_ERR  FALSE Fractional Systematic Error QUALITY  TRUE Quality Flag GROUPING  TRUE Grouping Flag   GRPPHA[] group gsobgd64bins.dat GRPPHA[] exit ... written the PHA data Extension ...... exiting, changes written to file : gso_10mCrab_100ks_bin.fak ** grppha 3.0.1 completed successfully
The same grouping has to be applied to the GSO background spectrum:
grppha gso_10mCrab_100ks.bkg gso_10mCrab_100ks_bin.bkg  MANDATORY KEYWORDS/VALUES    EXTNAME  SPECTRUM Name of this BINTABLE TELESCOP  SUZAKU Mission/Satellite name INSTRUME  HXD Instrument/Detector FILTER  Instrument filter in use EXPOSURE  1.00000E+05 Integration time (in secs) of PHA data AREASCAL  1.0000 Area scaling factor BACKSCAL  1.0000 Background scaling factor BACKFILE  gso_10mCrab_100ks_bkg.bkg CORRSCAL  1.0000 Correlation scaling factor CORRFILE  NONE Associated correlation file RESPFILE  ae_hxd_gsoxinom_20100524.rsp ANCRFILE  NONE Associated ancillary response file POISSERR  TRUE Whether Poissonian errors apply CHANTYPE  PI_SLOW Whether channels have been corrected TLMIN1  0 First legal Detector channel DETCHANS  512 No. of legal detector channels NCHAN  512 No. of detector channels in dataset PHAVERSN  1.1.0 OGIP FITS version number STAT_ERR  FALSE Statistical Error SYS_ERR  FALSE Fractional Systematic Error QUALITY  TRUE Quality Flag GROUPING  TRUE Grouping Flag   GRPPHA[group gsobgd64bins.dat] group gsobgd64bins.dat GRPPHA[exit] exit ... written the PHA data Extension ...... exiting, changes written to file : gso_10mCrab_100ks_bin.bkg ** grppha 3.0.1 completed successfully
In the next step we fit these datasets with the Crablike model defined above. We will use three different background assumptions  low, medium, and high  which vary by as much as 3% and 1.5% for the PIN and the GSO, respectively. This takes into account the fact that the ``true'' background will likely vary within these limits. We load the simulated source files (rebinned for the GSO). The simulated background files from the first fakeit step (rebinned for the GSO)  pin_10mCrab_1Ms.bkg and gso_10mCrab_100ks_bin.bkg , are loaded as background files as well as as correction files (``corfiles''), the latter allowing for an easy way to vary the total background within XSPEC.
XSPEC12>data pin_10mCrab_100ks.fak gso_10mCrab_100ks_bin.fak Spectrum #: 1 replaced Spectrum #: 2 replaced 2 spectra in use Spectral Data File: pin_10mCrab_100ks.fak Spectrum 1 Net count rate (cts/s) for Spectrum:1 3.803e01 +/ 3.000e03 (44.6 % total) Assigned to Data Group 1 and Plot Group 1 Noticed Channels: 1256 Telescope: SUZAKU Instrument: HXD Channel Type: PI_PIN Exposure Time: 1e+05 sec Using fit statistic: chi Using Background File pin_10mCrab_100ks_bkg.fak Background Exposure Time: 1e+06 sec Using Response (RMF) File ae_hxd_pinxinome9_20100731.rsp for Source 1 Spectral Data File: gso_10mCrab_100ks_bin.fak Spectrum 2 Net count rate (cts/s) for Spectrum:2 3.287e01 +/ 2.970e02 (0.7 % total) Assigned to Data Group 1 and Plot Group 2 Noticed Channels: 164 Telescope: SUZAKU Instrument: HXD Channel Type: PI_SLOW Exposure Time: 1e+05 sec Using fit statistic: chi Using Background File gso_10mCrab_100ks_bkg.fak Background Exposure Time: 1e+05 sec Using Response (RMF) File ae_hxd_gsoxinom_20100524.rsp for Source 1 ChiSquared = 318.41 using 320 PHA bins. Reduced chisquared = 1.0044 for 317 degrees of freedom Null hypothesis probability = 4.672303e01 ***Warning: Chisquare may not be valid due to bins with zero variance in spectrum number(s): 1 2 Current data and model not fit yet. XSPEC12>back pin_10mCrab_1Ms.bkg gso_10mCrab_100ks_bin.bkg Net count rate (cts/s) for Spectrum:1 3.802e01 +/ 3.000e03 (44.6 % total) Net count rate (cts/s) for Spectrum:2 3.261e01 +/ 2.970e02 (0.7 % total) ChiSquared = 305.87 using 320 PHA bins. Reduced chisquared = 0.96490 for 317 degrees of freedom Null hypothesis probability = 6.629651e01 ***Warning: Chisquare may not be valid due to bins with zero variance in spectrum number(s): 1 2 Current data and model not fit yet. XSPEC12>corfile pin_10mCrab_1Ms.bkg gso_10mCrab_100ks_bin.bkg Net count rate (cts/s) for Spectrum:1 8.529e01 +/ 3.000e03 (64.3 % total) After correction of 4.727e01 (using cornorm 1.000) Net correction flux: 0.472657 Net count rate (cts/s) for Spectrum:2 4.427e+01 +/ 2.970e02 (50.2 % total) After correction of 4.395e+01 (using cornorm 1.000) Net correction flux: 43.9467 ChiSquared = 2.212409e+06 using 320 PHA bins. Reduced chisquared = 6979.207 for 317 degrees of freedom Null hypothesis probability = 0.000000e+00 ***Warning: Chisquare may not be valid due to bins with zero variance in spectrum number(s): 1 2 Current data and model not fit yet. XSPEC12>model phabs*powerlaw Input parameter value, delta, min, bot, top, and max values for ... 1 0.001( 0.01) 0 0 100000 1e+06 1:phabs:nH>0.3 1 0.01( 0.01) 3 2 9 10 2:powerlaw:PhoIndex>2.1 1 0.01( 0.01) 0 0 1e+24 1e+24 3:powerlaw:norm>0.097 ======================================================================== Model phabs<1>*powerlaw<2> Source No.: 1 Active/On Model Model Component Parameter Unit Value par comp 1 1 phabs nH 10^22 0.300000 +/ 0.0 2 2 powerlaw PhoIndex 2.10000 +/ 0.0 3 2 powerlaw norm 9.70000E02 +/ 0.0 ________________________________________________________________________ ChiSquared = 2.212409e+06 using 320 PHA bins. Reduced chisquared = 6979.207 for 317 degrees of freedom Null hypothesis probability = 0.000000e+00 ***Warning: Chisquare may not be valid due to bins with zero variance in spectrum number(s): 1 2 Current data and model not fit yet.
We now experiment with different background levels, set by the value of ``cornorm''. A value of 0 gives the ``normal'' background, for example, 0.03 increases it by 3%, and 0.015 decreases it by 1.5%.
XSPEC12>cornorm 12 0.0 Spectrum 1 correction norm set to 0 Spectrum 2 correction norm set to 0 ChiSquared = 305.87 using 320 PHA bins. Reduced chisquared = 0.96490 for 317 degrees of freedom Null hypothesis probability = 6.629651e01 ***Warning: Chisquare may not be valid due to bins with zero variance in spectrum number(s): 1 2 Current data and model not fit yet. XSPEC12>ignore 1:**15. 70.** 2:**50. 600.** 40 channels (140) ignored in spectrum # 1 70 channels (187256) ignored in spectrum # 1 1 channels (1) ignored in spectrum # 2 12 channels (5364) ignored in spectrum # 2 ChiSquared = 152.83 using 197 PHA bins. Reduced chisquared = 0.78780 for 194 degrees of freedom Null hypothesis probability = 9.869519e01 Current data and model not fit yet. XSPEC12>fit Parameters ChiSquared Lvl 1:nH 2:PhoIndex 3:norm 152.172 3 0.986583 2.11789 0.101826 152.107 4 5.56204 2.13807 0.109058 152.035 5 6.34881 2.14176 0.110693 152.035 6 6.39060 2.14198 0.110787 ======================================== Variances and Principal Axes 1 2 3 8.9577E07 0.0002 0.3165 0.9486 3.3044E+02 1.0000 0.0035 0.0014 1.3350E03 0.0037 0.9486 0.3165  ==================================== Covariance Matrix 1 2 3 3.304e+02 1.145e+00 4.517e01 1.145e+00 5.168e03 1.966e03 4.517e01 1.966e03 7.519e04  ======================================================================== Model phabs<1>*powerlaw<2> Source No.: 1 Active/On Model Model Component Parameter Unit Value par comp 1 1 phabs nH 10^22 6.39060 +/ 18.1780 2 2 powerlaw PhoIndex 2.14198 +/ 7.18907E02 3 2 powerlaw norm 0.110787 +/ 2.74216E02 ________________________________________________________________________ ChiSquared = 152.04 using 197 PHA bins. Reduced chisquared = 0.78369 for 194 degrees of freedom Null hypothesis probability = 9.884693e01 XSPEC12>cpd /xs XSPEC12>setplot energy XSPEC12>plot ldata res
This result is shown in Fig. 5.1.

Now we check whether the same source signal would be detectable with a high background, i.e., a 3% and 1.5% higher background for the PIN and the GSO, respectively.
XSPEC12>cornorm 1 0.03 2 0.015 Spectrum 1 correction norm set to 0.03 Spectrum 2 correction norm set to 0.015 ChiSquared = 581.25 using 197 PHA bins. Reduced chisquared = 2.9961 for 194 degrees of freedom Null hypothesis probability = 2.754551e40 Current data and model not fit yet. XSPEC12>fit Parameters ChiSquared Lvl 1:nH 2:PhoIndex 3:norm 543.041 2 2.65270 2.21924 0.127136 514.453 2 4.29908 2.27391 0.153596 502.112 2 15.5709 2.31955 0.180934 <more trials here> 440.297 3 154.374 2.94577 1.56829 440.269 3 155.874 2.95280 1.60683 440.268 4 159.101 2.96827 1.69155 ======================================== Variances and Principal Axes 1 2 3 9.4350E06 0.0006 0.9792 0.2030 7.0331E+02 0.9997 0.0042 0.0232 5.0198E02 0.0236 0.2030 0.9789  ==================================== Covariance Matrix 1 2 3 7.029e+02 2.946e+00 1.632e+01 2.946e+00 1.443e02 7.840e02 1.632e+01 7.840e02 4.273e01  ======================================================================== Model phabs<1>*powerlaw<2> Source No.: 1 Active/On Model Model Component Parameter Unit Value par comp 1 1 phabs nH 10^22 159.101 +/ 26.5125 2 2 powerlaw PhoIndex 2.96827 +/ 0.120104 3 2 powerlaw norm 1.69155 +/ 0.653656 ________________________________________________________________________ ChiSquared = 440.27 using 197 PHA bins. Reduced chisquared = 2.2694 for 194 degrees of freedom Null hypothesis probability = 3.505307e21 XSPEC12>plot ldata res
This result is shown in Fig.5.2, and it clear from the figure that in this case the signal is undetectable in the GSO band.
Finally, we check the source signal using low backgrounds.
XSPEC12>cornorm 1 0.03 2 0.015 Spectrum 1 correction norm set to 0.03 Spectrum 2 correction norm set to 0.015 ChiSquared = 911.15 using 197 PHA bins. Reduced chisquared = 4.6967 for 194 degrees of freedom Null hypothesis probability = 2.974284e93 Current data and model not fit yet. XSPEC12>fit Parameters ChiSquared Lvl 1:nH 2:PhoIndex 3:norm 808.384 2 181.269 2.90266 1.54819 791.667 2 174.773 2.84250 1.27043 772.645 2 163.596 2.78155 1.03599 <more trials here> 434.587 0 0.00136529 1.83006 0.0445789 434.575 0 0.000110466 1.83001 0.0445767 434.575 6 0.000111649 1.83001 0.0445767 ======================================== Variances and Principal Axes 1 2 3 1.4396E07 0.0000 0.1354 0.9908 1.4928E+02 1.0000 0.0006 0.0001 7.6104E04 0.0006 0.9908 0.1354  ==================================== Covariance Matrix 1 2 3 1.493e+02 8.576e02 1.659e02 8.576e02 7.964e04 1.116e04 1.659e02 1.116e04 1.593e05  ======================================================================== Model phabs<1>*powerlaw<2> Source No.: 1 Active/On Model Model Component Parameter Unit Value par comp 1 1 phabs nH 10^22 1.11649E04 +/ 12.2180 2 2 powerlaw PhoIndex 1.83001 +/ 2.82200E02 3 2 powerlaw norm 4.45767E02 +/ 3.99093E03 ________________________________________________________________________ ChiSquared = 434.58 using 197 PHA bins. Reduced chisquared = 2.2401 for 194 degrees of freedom Null hypothesis probability = 1.748499e20 XSPEC12>plot ldata res
The result is shown in 5.3 where now the GSO spectrum is largely above to model.
By comparing the different fit results from these different runs, the overall uncertainties expected for the slope and normalization can be estimated.
Xissim is a Suzaku XIS event simulator, based on the tool xrssim. It reads a FITS format photon list file, traces photon paths in the telescope (via raytracing), and outputs a simulated XIS event file. The XRT thermal shield transmission and the XIS detection efficiency are taken into account if requested. Each record of the photon list file describes the celestial positions, arrival time, and energy of the input photon. The mkphlist FTOOL can create such photon list files from FITS images (e.g., ROSAT HRI or Chandra images) and spectral models (which may be created in XSPEC). The xissim output event file may be analyzed just like observational data, using standard analysis tools such as xselect. xissim is part of the latest version of the FTOOLS.
Maki is another webbased interactive tool (see Appendix B) that can determine the orientation of the XIS CCDs on the sky as a function of the observation epoch within the visibility window of the target. For Suzaku, the orientation of the solar panels with respect to the spacecraft is fixed, and at the same time, the range of the angles between the vector normal to the solar panels and the vector pointing to the Sun is restricted, which in turn restricts the roll angle of the spacecraft.
When using the tool, general instructions are available via the ``Help'' button. In order to check the visibility and available roll angles for a target, load a FITS image or by enter the RA and DEC of the source and click the ``New Graph'' button. This creates an image on which the Suzaku XIS field of view (FOV) will be shown.
The ``Mission and Roll Selector'' (in the upper right of the display) allows different instruments from different missions to be selected. Then the FOV will appear on your image. This can be rotated using the ``Roll angle'' slider bar.
Unfortunately, the current version of Maki does not work on
64bit machines. We therefore provide a simpler, textonly, perl
script, RollRange, as an alternative to Maki. The
RollRange package can be downloaded
from:
ftp://heasarc.gsfc.nasa.gov/suzaku/nra_info/tools/rollrange.tar.gz.
For
setup instructions, see:
http://heasarc.gsfc.nasa.gov/docs/suzaku/prop_tools/rollrange.html.
RollRange.pl
takes three arguments: the right ascension and declination of the
pointing direction in decimal degrees, and the MJD of interest (which
can be calculated using the HEASARC xTime tool).
At a roll angle of 0.0, the spacecraft's Y axis is pointing North; at 90.0, it points East (i.e., counterclockwise rotation looking up at the sky). One can subtract the roll angle from 90.0 to obtain the 3rd Euler angle.
Note that both Maki and RollRange consider only the Sun angle. Additional constraints often exist, due to the availability (or not) of suitable stars in the startracker fieldofview. For accepted observations, the mission scheduling team will provide the definitive range of allowed roll angles to the PI.
The Remote Proposal Submission (RPS) tool must be used to enter the basic proposal data into the ISAS/JAXA, HEASARC, or ESA database. Proposers should make sure they use the appropriate RPS, since there are multiple reviews. See Appendix B for the list of RPS websites and addresses. Two versions of RPS are available: a characteroriented version, where the user submits all the required information via email, or a weboriented version.
One aspect of RPS that is not immediately obvious is how to specify timeconstrained observations. For instance, a need for such an observation may arise for a study of a spectrum of a binary system at a particular orbital phase. If some particular aspect of the observation cannot be clearly specified in the RPS form, the user should detail it in the ``comments'' field of the RPS form and/or contact either the Suzaku team at ISAS/JAXA or the NASA Suzaku GOF before submitting.
A successful Suzaku proposal, from a technical point of view, must include the following elements:
While two default aim points were offered from AO1 to AO6  the XIS nominal and the HXD nominal positions (the HXD aim point is at (DETX,DETY)=(3.5, 0) on the XIS image); the reduction in effective area for the nonselected instrument is %)  support for the HXD nominal position will be dropped in AO7. This is done to mitigate effects due to the increased attitude jitter of Suzaku since the end of 2009. No observations with nonstandard readout clocks (Psum/Timing mode and Window/Burst options) will be carried out at the HXD nominal position. While the operation team does not prohibit observations at the HXD nominal point with a standard XIS mode response matrices will not be provided for such observations.
Note that Guest Observers are welcome to propose for targets already approved for in previous AOs (see the Announcement of Opportunity). However, in the interest of maximizing the scientific return from Suzaku, the proposal must explain why the alreadyapproved observation(s) does/do not meet their scientific objectives. Valid reasons include a much longer exposure time, incompatible time constraints, or different positions within an extended source.
We also note that the XISs are subject to count rate limitations, because of possible multiple events in an XIS pixel within one frame. This is much less of a problem than with the ACIS aboard Chandra, as Chandra's mirror focuses the Xray flux onto a CCD area that is orders of magnitude smaller. The rule of thumb is that the XIS can tolerate a point source with a count rate up to cps per CCD with essentially no loss of counts or resolution. For brighter sources, these limitations can be reduced via a variety of XIS modes, such as the use of a subarray of the XIS, as discussed in section 7.2.2.1.
Finally, it is important to remember that because the HXD is a nonimaging detector, contaminating sources in the field of view can significantly affect your results. The HXD field of view is defined by a collimator with a square opening. The FWHM of the field of view is 34.4 34.4 below keV and above keV. Considering that twice the FWHM value is required to completely eliminate the contamination in a collimatortype detector, and the source may happen to be located at the diagonal of the square, nearby bright sources within a radius of 50 and from the aim point can contaminate the data in the energy band below and above keV, respectively. If you specify the rollangle to avoid the source, the limit will be reduced to 35 and , respectively. It is the proposer's responsibility to show that any source with a flux level comparable to or brighter than that of the target of interest does not exist within these ranges. The proposer can, e.g., check this by using the hard Xray source catalogs from such satellites as RXTEASM, INTEGRAL, and Swift, among others.
There are two additional NASAspecific proposal rules that must be followed by USbased proposers: