Which detectors can I use to analyze this flare?

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Nugget
Number: 23?
1st Author: Brian Dennis
2nd Author: Kim Tolbert
Published: September, 2014
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Introduction

This is the most common question we get asked by many people trying to analyze RHESSI imaging and/or spectroscopy data. The answer is not always easy and it is becoming more and more difficult as the individual detectors respond differently to radiation damage and to the four anneals that have now been completed. However, we now have new front-segment spectral plots available in Browser for all identified contiguous flares that can help answer this question. These plots show both the count flux spectrum and the corresponding "semi-calibrated" photon spectrum for each of the nine detector front segments. The plots cover a one minute interval centered on the peak times of all identified contiguous events in the RHESSI flare catalog. They can be obtained for any given flare by selecting "Detector spectra" under "Flare Quicklook" in Browser.

Example 1 in A0 Attenuator State

Figure 1: Total count and photon flux spectra for individual detector front segments during a flare on 02 May 2014 at 00:54:36 UT.

An example of these plots is shown in Figure 1 for a one minute interval centered on the peak of a small flare in the A0 attenuator state. The nine total count-flux spectra in units of counts~ Failed to parse (PNG conversion failed; check for correct installation of latex, dvips, gs, and convert): $s^{-1}~cm^{-2}~keV^{-1}$ , one for each front segment, are each fully corrected for decimation and live time and use 0.3 keV energy bins below 10 keV increasing logarithmically up to 100 keV. The photon flux spectra are computed from the corresponding count flux spectra by multiplying by the diagonal elements of the detector response matrix [2] applicable for that time of the flare. This has traditionally been called a "semi-calibrated photon spectrum." Since no background was subtracted, it is equivalent to assuming that all the counts were from solar photons and that the off-diagonal elements are negligible. Photon spectra determined in this way approximate the actual solar spectrum only in the energy range where the solar counts are significantly above background and the off-diagonal elements are small. For the case shown in Figure 1, this would be below ~20 keV. Even in that case, they serve only to show the relative sensitivity of the nine detector front segments and how well the detector response matrices correct for the known sensitivities of the different detectors. Since, at the time of the plot, the instrument was in attenuator state A0, i.e. no attenuators were in place above the detectors, an estimate of the photon spectrum can be made down to ~3 keV, the approximate energy of the electronic lower threshold level for each detector and the effective cutoff from the absorption of material in front of the detectors including the thermal blankets, both inside the cryostat and above the top grids, and the beryllium windows on the cryostat. Counts recorded below ~3 keV are electronic noise and cannot be used in the determination of the photon spectrum, hence the hatched areas in the plots.

From this plot you can already begin to decide which detectors are OK to use for specific applications such as light curves, spectroscopy, and imaging. The count flux plots show immediately which detectors have recorded an increase in count rate from the flare. The solar signal is the peak at around 7 keV that falls off at lower energies down to 3 keV and extends up to about 25 keV before merging with the background spectrum at higher energies. Here is a breakdown of what you can determine about each of the nine detectors from these two plots:

Example 2 in A3 Attenuator State

Another example from earlier in the mission on 20 January 2005 is shown in Figure 2.

Figure 1: Similar to Figure 1 during an X-class flare on 20 January 2005 at 06:50:40 UT.

This is for a much more intense flare in the A3 attenuator state, i.e. with both the thick and thin attenuators in place above the detectors. Thus, we see the solar count flux spectrum peaking just below 20 keV and extending above background to >100 keV. In the A3 state the strong attenuation at low energies is such that almost all counts below 5 or 6 keV are from K-escape events (photons above the germanium K-edge at 11 keV that have photoelectric interactions that result in the escape of the K-shell photon from the detector). Hence, counts below this energy should not be used as indicated by the hatched areas on the plots. The close alignment of the photon spectra for all detectors indicates that they can all be used above ~6 keV although there are still small differences between detectors as indicated below.

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