List of Figures

• 2.1. The 96 minute Suzaku orbit.
• 2.2. [Left] Schematic picture of the bottom of the Suzaku satellite. [Right] A side view of the instrument and telescopes on Suzaku.
• 2.3. XIS Effective area of one XRT + XIS system, for both the FI and BI chips.
• 2.4. The Encircled Energy Function (EEF) showing the fractional energy within a given radius for one quadrant of the XRT-I telescopes on Suzaku at 4.5 and 8.0 keV.
• 2.5. Total effective area of the HXD detectors, PIN and GSO, as a function of energy.
• 5.1. Layout of the XRTs on the Suzaku spacecraft.
• 5.2. A Suzaku X-Ray Telescope
• 5.3. A thermal shield.
• . Images and PSFs are shown in the upper, middle, and lower panels for the XRT-I0 through XRT-I3 from left to right. In each image drawn are ten contours in logarithmic spacing with the outermost contour being 1% surface brightness of the peak. The position of the maximum surface brightness is written as a caption in each panel in a unit of arcmin. Its typical error is $\pm 0.\!'1$. Each PSF is normalized by the number of total photons collected over the entire XIS aperture.
• 5.5. Focal positions at the XISs when the satellite points MCG$-$6$-$30-15 at the XIS aimpoint.
• . Optical axis directions of the XIS-S0 through S3. The optical axis of the XRT-I0 (XIS-S0), for example, locates at $(1.\!'0,\;-0.\!'2)$, which implies that the maximum throughput is achieved for XRT-I0 when the satellite points at the XIS aimpoint.
• 5.7. Vignetting curves of XRT-I at three different energies of 1.5, 4.5 and 8.0 keV. The three solid lines in the plots correspond to a parameter of ray-tracing program while the crosses are the preliminary XRT-I effective area "inferred" from the Crab pointings with some assumptions. The XRT-I effective area shown here does not includes either the quantum efficiency of the detector or transmissivity of the thermal shield and the optical blocking filter.
• 5.8. left: A $-20'$-off image of the Crab nebula taken with XIS3. middle: A simulated image of a point source at $-20'$ off with the pre-collimator. right: The same as the middle panel but without the pre-collimator. The pre-collimator properly works in orbit.
• 5.9. Angular responses of the XRT-I at 1.5 (left) and 4.5 keV (right) up to 2 degrees. The effective area is normalized at on-axis. The integration area is corresponding to the detector size of XIS ( $17'.8\times 17'.8$). The three solid lines in the plots correspond to different parameters of ray-tracing program while the crosses are the normalized effective area using the Crab pointings.
• 6.1. The four XIS detectors before installation onto Suzaku.
• 6.2. One XIS instrument. Each XIS consists of a single CCD chip with $1024 \times 1024$ X-ray sensitive cells, each 24 $\mu$m square. Suzaku contains four CCD sensors (XIS-S0 to S3), two AE/TCUs (AE/TCE01 and AE/TCE23), two PPUs (PPU01 and PPU23), and one MPU. AE/TCU01 and PPU01 service XIS-S0 and XIS-S1, while AE/TCE23 and PPU23 service XIS-S2 and XIS-S3. Three of the XIS CCDs are front-illuminated (FI) and one (XIS-S1) is back-illuminated (BI).
• 6.3. Time sequence of the exposure, frame-store transfer, CCD readout, and data transfer to the pixel RAM in PPU is shown (1) in normal mode without options, (2) in normal mode with Burst option, and (3) in normal mode with Window option. In this example, the 1/4 Window option is assumed.
• 6.4. Information sent to the telemetry is shown for $5 \times 5$, $3 \times 3$, and $2 \times 2$ modes. 1-bit information means whether or not the PH of the pixel exceeds the outer split threshold. In $2 \times 2$ mode, the central 4 pixels are selected to include the second and the third (or fourth) highest pixels among the 5 pixels in a cross centered at the event center.
• 6.5. Definition of the grades in the P-Sum/timing mode. Total pulse height and the grade of the event are output to the telemetry. Note that the grades are defined referring to the direction of the serial transfer, so the central pixel of a grade 1 event has the larger RAWX value, while the opposite is true for a grade 2 event.
• 6.6. The XIS background rate for each of the four XIS detectors, with prominent fluorescent lines marked. These spectra are based on $\sim 110-160$ksec of observations towards the dark Earth.
• 6.7. The XIS background rate for each of the four XIS detectors, showing only energies between 0.1-2.0 keV. Below 0.3 keV the background rate for the FI chips cannot be determined due to their low effective area.
• 7.1. The Hard X-ray Detector before installation.
• 7.2. Schematic picture of the HXD instrument, which consists of two types of detectors: the PIN diodes located in the front of the GSO scintillator, and the scintillator itself.
• 7.3. Example of the observed HXD background on orbit. Plots normalized both with effective (solid) and geometric (dashed) area are presented.
• 7.4. [Left] The sensitivity of the HXD to continuum emission, taking into account the expected background. [Right] Same, for line emission.