The Hard X-ray Detector (HXD, see Figure 8.1) is a non-imaging, collimated hard X-ray scintillating instrument sensitive in the keV to keV band. It has been developed jointly by the University of Tokyo, Aoyama Gakuin University, Hiroshima University, ISAS/JAXA, Kanazawa University, Osaka University, Saitama University, SLAC, and RIKEN. Its main purpose is to extend the bandpass of the Suzaku observatory to the highest feasible energies, thus allowing broad-band studies of celestial objects.
This AO-7 document is based on the calibration of the PIN and the GSO detectors as of October 2010 (HEASOFT 6.9). The recommended procedure for feasibility simulations is basically unchanged from previuos AOs, the same response and background files as provided for AO-6 can be used for simulations. Note that the HXD aim point is not supported anymore (see chapter 2 and section 5.5.2).
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The HXD sensor (HXD-S) is a compound-eye detector instrument, consisting of 16 main detectors (arranged as a 4 4 array) and the surrounding 20 crystal scintillators for active shielding. Each unit actually consists of two types of detectors: a GSO/BGO phoswich counter, and 2mm-thick PIN silicon diodes located inside the well, but in front of the GSO scintillator. The PIN diodes are mainly sensitive below keV, while the GSO/BGO phoswich counter (scintillator) is sensitive above keV. The scintillator signals are read out by photomultiplier tubes (PMTs). A schematic drawing of the HXD is given in Fig. 8.2. The HXD features an effective area of cm at 20keV, and cm at 100keV (Fig. 3.5). The energy resolution 4.5keV (FWHM) for the PIN diodes, and % (FWHM) for the scintillators, where is energy in MeV. The HXD time resolution is 61s.
Each main detector unit is of a well-type design with active anti-coincidence shields. The shields and the coarse collimator itself are made of Bismuth Germanate (BGO, BiGeO) crystals, while the X-ray sensing material ``inside the well'' consists of Gadolinium Silicate (GSO, GdSiO(Ce)) crystals. The aspect ratio of the coarse collimators yields an acceptance angle for the GSO of 4.5 (FWHM). Each unit forms a 2 2 matrix, containing four 24mm 24mm, 5mm thick GSO crystals, each placed behind a PIN diode. BGO crystals are also placed underneath of the GSO sensors, and thus each well is a five-sided anti-coincidence system. The effective thickness of the BGO active shield is about 6cm for any direction from the PIN and GSO, except for the pointing direction.
The reason for the choice of the two different crystals for the sensor and the shield is dictated by the large stopping ability of both, yet the very different rise/decay times, of ns for BGO, and ns for GSO, at a working temperature of C. This allows for an easy discrimination of the shield vs. X-ray sensor signals, where a single PMT can discriminate between the two types of scintillators in which an event may have occurred. Any particle events or Compton events that are registered by both the BGO and GSO can be rejected by this phoswich technique, utilizing custom-made pulse-shaping LSI circuits.
In early 2010, a new GSO gain calibration with associated response files has been released. With this update, GSO data become usable down to 50keV. See the Suzaku web pages for more details 8.1. Note that proposers do not need to consider the details of the new responses, since the differences to the old ones are minor with respect to performing feasibility simulations (although not negligible in a real data analysis).
The low energy response of the HXD is provided by 2mm thick PIN silicon diodes, placed in front of each GSO crystal. The geometrical area of the diodes is 21.5 21.5mm, while the effective area is limited to 16.5 16.5mm by the guard ring structure. The temperature of the PIN diodes is controlled to be C to suppress electrical noise caused by the leakage current, and they are almost fully depleted by applying a bias voltage of 400500V 8.2. The PIN diodes absorb X-rays with energies below keV, but gradually become transparent at harder X-rays, which reach and are registered by the GSO detectors. The X-rays are photoelectrically absorbed in the PIN diodes, and the signal is amplified, converted to digital form, and read out by the associated electronics. The PIN diodes are of course also actively shielded from particle events by the BGO shields, as they are placed inside the deep BGO wells. In addition, in order to reduce contamination by the cosmic X-ray background, passive shields called ``fine collimators'' are inserted in the well-type BGO collimator above the PIN diodes. The fine collimator is made of 50m thick phosphor bronze sheets, arranged to form 8 8 square meshes, 3mm wide and 300mm long, each.
The lower threshold of the PIN diodes has gradually become higher due to the increase of leakage current by cosmic-ray damage. Updated response files are regularly provided by the HXD team, for well defined ``epochs'' in time. As of August 2011 calibration epoch 11 is the newest/current one.
The field of view of the HXD changes with incoming energy. Below keV the passive fine collimators define a FWHM square opening as shown in Figure 8.3. The narrow field of view compared to the Beppo-SAX-PDS and RXTE-HEXTE experiments is one of the key advantages of HXD observations. Above keV the fine collimators become transparent and the BGO active collimator defines a 4.5 4.5 FWHM square opening. In summary, the full PIN energy range and the lower quarter of the GSO range have a field of view of , while the GSO events above keV have a wider field of view, up to 4.5.
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Although the HXD is a non-imaging instrument, its instantaneous background can be reproduced through modeling, without requiring separate off-source observations. The HXD has been designed to achieve an extremely low in-orbit background (cps cm keV), based on a combination of novel techniques: (1) the five-sided tight BGO shielding as mentioned above, (2) the use of the 20 shielding counters made of thick BGO crystals which surround the 16 main GSO/BGO counters, (3) sophisticated on-board signal processing and on-board event selection, employing both high-speed parallel hardware circuits in the analog electronics, and CPU-based signal handling in the digital electronics, and (4) the careful choice of materials that do not become strongly activated under in-orbit particle bombardment. Finally, (5) the narrow field of view below keV defined by the fine collimator effectively reduces both the CXB contribution and the source confusion.
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The non X-ray background (NXB) of the PIN diodes, measured in orbit, is plotted in the left panel of Fig. 8.4. The average background count rate summed over the 64 PIN diodes is 0.6counts s, which is roughly equal to an intensity of 10mCrab. In addition, almost no long-term growth has been observed in the PIN-NXB during the first three years of Suzaku, thanks to the small activation effect of silicon. In contrast, as shown in the right panel of Fig. 8.4, a significant long-term increase caused by in-orbit activation has been observed for the GSO-NXB, especially during the early phase of the mission. The background spectrum of the GSO contains several activation peaks, with intensities exponentially increasing with their half-lives. Since the longest half-life is about one year, the GSO-NXB level will have almost saturated.
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Figure 8.5 illustrates the comparison between detector backgrounds of several hard X-ray missions. The lowest background level per effective area is achieved by the HXD in an energy range of 12-70 and 150-500keV. The in-orbit sensitivity of the experiment can be roughly estimated by comparing the background level with celestial source intensities indicated by dotted lines. Below 30keV, the level is smaller than 10mCrab, which means a sensitivity better than 0.3mCrab can be obtained, if an accuracy of 3% is achieved in the background modeling.
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Since the long-term variation of both PIN-NXB and GSO-NXB can be expected to be stable, the main uncertainties of the background come from temporal and spectral short-term variations. As shown in Fig. 8.6, the PIN-NXB displays significant short-term variability, with a peak-to-peak amplitude of a factor of 3, anti-correlated with the Cut-Off Rigidity (COR) over the orbit. Since the COR affects the flux of incoming primary cosmic-ray particles, most of the PIN-NXB is considered to originate in the secondary emission produced by interactions between cosmic-ray particles and materials surrounding the detector. When a selection criterion of COR6, a standard value used in the pipeline processing, is applied for the event extraction, the amplitude decreases to a factor of 2. During this temporal variation of the PIN-NXB, its spectral shape also changes slightly (larger deviations from the average are observed at a higher energy range, Kokubun et al. 2007). In case of the GSO-NXB the temporal variation differs for different energy bands, as shown in the right panel of Fig 8.6. In the lowest energy range a rapid decline after the SAA passage is clearly observed, in addition to a similar anti-correlation with the COR. All these temporal and spectral behaviors have to be properly handled in the background modeling.
As is the case for every non-imaging instrument (and in particular, for those sensitive in the hard X-ray range), the limiting factor for the sensitivity of the HXD is the reproducibility of the background estimation. Since this is the first space flight of an HXD-type detector, and the reproduction of the in-orbit background is not at all an easy task, the modeling accuracy evolves with the experience with in-orbit data. The latest status of the estimation procedures and their uncertainties will be regularly posted on the Suzaku web-sites listed in Appendix B. For proposal preparation, methods, limitations, and reproducibilities (as a function of time-scale and energy range) of the current background modeling are briefly described below. Note that this document is based on ``Suzaku-memo-2008-03'' (Mizuno et al. 2008) and ``Suzaku-memo-2008-01'' (Fukazawa et. al 2008), which can be found at http://www.astro.isas.jaxa.jp/suzaku/doc/suzakumemo, and on Fukazawa et. al (2010, PASJ 61, S17). We recommend that proposers properly take into account the expected uncertainties for their observation, based on the following information. Note that all uncertainties are reported at the 90% confidence level in this section.
Since there is a strong anti-correlation between the PIN-NXB and the COR, the background modeling of the PIN is primarily based on the count rate of high-energy charged particles, directly measured by the PIN diodes. Due to large energy deposits in the silicon, penetrations of cosmic-ray particles cause large signals in the corresponding PIN diodes. Hence they activate the Upper Discriminator (UD) in the analog electronics and are then recorded as PIN-UD monitor count in the HK data. The PIN-UD rate is considered to directly indicate the flux of primary cosmic-ray particles. The background count rate at any time can be generally estimated based on the corresponding PIN-UD rate.
In the actual modeling procedure of the so called ``tuned-bgd'', the PIN-NXB rate is described by adding the raw PIN-UD rate and the integrated PIN-UD rate with a fixed decay time constant, to take into account the small effect of activation during SAA passages. In addition, several parameters such as GSO count rate, Earth elevation angle and cut-off rigidity, are included as input parameters.
The spectral shape of the PIN-NXB is assumed to depend on the COR and the elapsed time after the SAA passage. For each estimated rate it is extracted from a database of PIN-NXB spectra, which has been compiled from Earth occultation data.
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We first selected observations with no strong X-ray emission above 7keV (less than 20% above the XIS-FI NXB in the entire XIS field-of-view) and compared the HXD-PIN data and the NXB model count rate (10ks exposure) in the 15-40keV band, as shown in Figure 8.7. The 90% confidence region (including a statistical uncertainty of %) of the residual is 5.8% of the mean NXB count rate, which is larger than that obtained from the Earth occultation data (% including 3.1% statistical uncertainty, see § 3.2 of ``Suzaku-memo-2008-03'').
Figure 8.8 shows the same comparison of sky data and the NXB model for E010272 observations (the same sky region is observed regularly for XIS calibration purposes). Some observations do not satisfy the selection criteria using XIS due to sources or diffuse emission in the XIS field-of-view, but we used all E010272 observations in order to compare sky data and the NXB model for as big a data set as possible. We also plot the data and the NXB model for Cygnus LOOP multi-pointing observations (regions within a radius of 1.5degrees were observed). We see a clear difference of the residual between the two sets of observations. Especially, the width of the residual for the E010272 data is much narrower than that seen in Fig. 8.7.
The 90% confidence region of the residual obtained from the E010272 observations is counts s, or of the mean NXB rate, including the statistical uncertainty of %. This is somewhat larger, but comparable to, the residual distribution of 3.8% (including the statistical uncertainty of 3.1%) obtained from Earth occultation data. After subtracting the statistical uncertainty, the residual systematic uncertainty of the E010272 observations is estimated to be 3.8%, for a typical 10ks exposure. As described above, the E010272 data might suffer from contamination from sources within the field-of-view, and thus this confidence region should be regarded as a conservative estimate. For longer exposures the systematic uncertainty is expected to become a bit smaller, though the lack of long-exposure sample observations makes it difficult to verify this effect at the moment.
In order to check the NXB reproducibility for a sample of observations, we also investigated the background subtraction for eight objects for which the source signal is expected to be negligible in the HXD-PIN. The spectra are summarized in Figure 8.9. The background-subtracted spectra and the CXB model of Boldt (1987) 8.3 are displayed as blue and green histograms, respectively. No systematic difference between them is seen up to 60keV.
From these arguments, it is clear that the current NXB model reproducibility at the 90% confidence level (excluding the statistical error) is better than 5%, and will be as good as 3% in most observations with exposures longer than 10ks. When analyzing HXD data, the user should carefully estimate the reproducibility depending on the given observational conditions. For simplicity, we suggest to employ 3% as nominal value of the 15-40keV PIN NXB reproducibility at the 90% confidence level for the preparation of proposals (see, e.g., section 5.5.2).
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The GSO background is higher than that of the PIN, and hence the background modeling accuracy is very important. The background model generation methods are similar to those applied for the PIN background.
We compared the NXB model with the on-source data of dark objects, for which the source signal is expected to be negligible in the HXD-GSO. Examples for the comparison of spectra for eight dark objects are summarized in Figure 8.10. Unlike for the PIN, the CXB is negligible in the GSO band. The overall spectral shape is similar between the data and the background model spectra, where the latter is solely based on a template derived from Earth occultation data. In most cases, the residuals amount to 1-1.5% of the data. For simplicity, we therefore suggest to employ 1.5% as nominal value of the GSO NXB reproducibility at the 90% confidence level for the preparation of proposals (see, e.g., section 5.5.2).
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As a reference, Fig. 8.11 presents the theoretical sensitivity calculation results, that is, expected sensitivities defined by a certain systematic uncertainty of the background modeling, and those solely determined by the statistical uncertainty for a given exposure. In the plot, background reproducibility uncertainties of 3% and 1.5% are assumed as an example, for the PIN and the GSO, respectively. Since the actual statistical and systematic uncertainties that are to be expected for a proposed observation differ from case to case, they should be carefully verified using the data-NXB residual distribution plots.
HXD data are accumulated on event by event basis. After on-board data selection, event data are further screened by the ground pipeline analysis process. By referring to the trigger and flag information (including the inter-unit anti-coincidence hit patterns), the pipeline assigns specific grades to the HXD events such as pure PIN events and pure GSO events. Detector responses and background files that match the particular (i.e., default) grade of events are provided by the HXD team. There are no user-specified parameters for the HXD.
Tight active shielding of HXD results in a large array of guard counters surrounding the main detector parts. These anti-coincidence counters, made of cm thick BGO crystals, have a large effective area for sub-MeV to MeV gamma-rays. With limited angular ( ) and energy (% at 662keV) resolution, they work as a Wide-band All-sky Monitor (WAM).
Analog signals from normally four counters on each side of an HXD
sensor are summed up and a pulse height histogram is recorded every
second. If a transient event such as a Gamma-Ray Burst (GRB) is
detected, light curves with finer (31.25ms) time resolution are also
recorded in four energy bands. The energy coverage of the WAM extends
from keV to MeV, and its effective area is cm at 100keV and 400cm at 1MeV. These data are
shared among the PI and the HXD team, i.e., the PI can use the full
WAM data set. Since such transient events, especially GRBs, require
immediate distribution to the community, the HXD team will make the
analysis products, such as light curves and spectra, public as soon as
possible at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB.