Marx 5.0.0

 

Marx 5 Highlights

 

Marx 5 is a major new release. This page is devoted to the new features.

Contents

Subpixel Randomization
New Dither Model
Calibration Updates
Marx Parameter File Updates

Subpixel Randomization


The EDSER subpixel algorithm was incorporated into CIAO 4.3. When computing Sky coordinates, acis_process_events first converts the integer-valued chip coordinate to a floating point value. There are several ways in which this may be done. One way is to simply cast the integer to a float, e.g,, the integer 2 becomes 2.0. The problem with this approach is that it can cause aliasing artifacts in the resulting Sky image. For this reason, the default up until CIAO 4.3 was to simply add a uniform random deviate from -0.5 to 0.5 to the integer value so that 2 would become a random real number in the semi-open interval [1.5, 2.5). The default was changed in CIAO 4.3 to use a discrete probability distribution based upon flight grade and energy, known as the EDSER method.

The marx 5 version of marx2fits introduces a --pixadj command line parameter that allows the user to select one of several pixel randomization methods. Simply running marx2fits without any command line arguments will display its usage message:

marx2fits v5.0.0:
Usage: marx2fits [options] marxdir outfile
Options:
  --pileup             Process a marxpileup simulation
  --pixadj=EDSER       Use a subpixel algorithm (default)
  --pixadj=RANDOMIZE   Randomize within a detector pixel
  --pixadj=NONE        Do not randomize within a detector pixel
  --pixadj=EXACT       Use exact chip coordinates

The effect of these randomization methods may be seen in the following plot, which shows that the EDSER distribution approaches the exact limit.

Image of PSF with different pixadj values

If using SAOTrace rays with marx, see the important caveat regarding the use of the EDSER method with such rays.


New Dither Model


The EDSER subpixel algorithm necessitated numerous changes to the marx aspect code. In particular, aspect reconstruction blur had to be cleanly separated into its independently contributing pieces, namely the telescope pointing uncertainty, the blur introduced by pixel quantization/truncation, and the blur associated with pixel randomization. Previous versions of marx incorporated these blurs under the guise of a single parameter, DitherBlur, whose value was the RSS sum of the contributing blurs. This was the source of a lot of confusion among users resulting in numerous help desk inquiries about how this value was obtained and why it was so large. For these reasons, the DitherBlur parameter was removed from marx and replaced by one called AspectBlur whose value represents just the telescope pointing uncertainty, 0.07 arc-seconds. One consequence of this change is that marx 4.x parameter files cannot be used with marx 5.0.

It was also necessary to remove the blur parameters from marxasp, which computes an aspect solution file for use in reprocessing a marx2fits generated event file. Hence any scripts that pass blur parameter values to marxasp will need to be modified.


Calibration Updates


As mentioned above, the DitherBlur parameter's value reflected more that just that associated with the aspect uncertainty. It was also tweaked to get the marx PSF to better match Chandra grating line profiles. With this parameter gone, the marx HRMA blur parameters had to be re-calibrated to get the widths of the marx simulated grating line profiles to match those in the Chandra CALDB.

There was a long standing issue of a relative rotation between the LETG and the ACIS detector. The root of this problem was tracked down (with the help of marx) to a rotation offset between the aspect coordinate system and the focal plane detector system. This offset was masked by compensating rotations of the detectors from astrometric analysis, and manifested itself as a small rotation of the LEG dispersion arm on the ACIS detector. Changes were added to CIAO 4.3 that effectively adds an additional rotation to the LETG when used with ACIS. The corresponding change in marx 5.0 is implemented via a new parameter called LETG_ACIS_dTheta.

The marx calibration data have been brought up to date with the Chandra CALDB 4.4.7.


Marx Parameter File Updates


The parameter files for earlier versions of marx (e.g., the marx.par file for version 4.5) cannot be used with marx 5.0. The recalibrations that were necessary for subpixel support resulted in changes to all of the HRMA blur parameters, as well as the introduction of the new AspectBlur parameter discussed above.

The following marx.par parameter values have changed since marx 4.5:

 P1Blur: 0.18129215 --> 0.303427
 H1Blur: 0.13995037 --> 0.0051428
 P3Blur: 0.11527828 --> 0.0951899
 H3Blur: 0.16360829 --> 0.0713614
 P4Blur: 0.1289134 --> 0.178899
 H4Blur: 0.098093014 --> 0.0101367
 P6Blur: 0.076202759 --> 0.151085
 H6Blur: 0.079767401 --> 0.0239287
 MEGRowlandDiameter: 8632.65 --> 8632.48
 HEGRowlandDiameter: 8632.65 --> 8632.48
 HETG_Shell1_Period: 0.400141 --> 0.400195
 HETG_Shell3_Period: 0.400141 --> 0.400195
 LETG_Shell1_Theta: -0.07 --> 0.07
 LETG_Shell3_Theta: -0.07 --> 0.07
 LETG_Shell4_Theta: -0.07 --> 0.07
 LETG_Shell6_Theta: -0.07 --> 0.07
 legCoarseNumOrders: 11 --> 121
The following parameters have been removed:
 DitherBlur
The following parameters have been added:
 AspectBlur: 0.07
 LETG_ACIS_dTheta: -0.0867
 Use_This_Order: 0
 DetExtendFlag: no
The latter two parameters were added for the purposes of calibration.

This page was last updated Jan 25, 2012 by John E. Davis.
Technical questions should be addressed to marx-help at space mit edu.
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