# Using Response Matrices with marx¶

The detector models within marx include analytic representations of the intrinsic spectral resolution of these instruments. For some users, a higher degree of accuracy may be necessary. marx allows users to supersede the built-in spectral response function using an external spectral response matrix file (RMF). In this section, we describe how to use the marxrsp tool in conjunction with these RMF files.

## What is a Response Matrix?¶

As commonly employed, the spectral response matrix or spectral redistribution function defines the mapping of input photon energy to detected pulse height for a given detector. In this sense, it includes the spectral resolving power of the detector but by definition does not include the quantum efficiency. Typically, these detector response matrices are stored as response matrix files (RMFs) in the form of FITS binary tables.

The format for an RMF has been defined by HEASARC and marxrsp has been designed to work with RMFs which adhere to this format. Specifically, the marxrsp tool checks the indicated RMF file for valid values of the HDUCLAS3 FITS keyword. HEASARC-allowed values for this keyword include REDIST, DETECTOR, or FULL. A value of REDIST indicates a bare redistribution matrix while DETECTOR and FULL indicate that a quantum efficiency or effective area have been included, respectively. The marxrsp tool requires a value of HDUCLAS3=REDIST. The --force option can be used to make marxrsp accept RMF files with other values of the HDUCLAS3 keyword. In such circumstances, the input marx simulation should be run with DetIdeal="yes".

Response matrices for the ACIS CCDs can be created using the CIAO tool mkrmf. More information and the necessary calibration data to create ACIS RMFs are available from the CIAO. There are currently no RMFs available for the HRC.

A simulated ACIS pulse height spectrum computed using a marx simulation, the marxrsp tool, and RMF files for a FI and BI CCD. The upper curve shows the PHA spectrum for the BI RMF while the lower curve represents a typical FI RMF near the ACIS-I aimpoint. The input spectrum was the same thermal plasma spectrum used in the examples in Simulating a user-defined CCD spectrum with ACIS.

## The marxrsp Tool¶

Like all post-processing tools in the marx suite, marxrsp operates on an existing simulation directory created using marx. The user specifies a simulation directory and an RMF to use in calculating the pulse height spectrum. For example, to fold the Raymond-Smith thermal plasma spectrum simulated in Simulating a user-defined CCD spectrum with ACIS through an ACIS RMF called acis7b_aim_pha_rmf.fits, we would use the syntax:

unix% marxrsp --rmf acis7b_aim_pha_rmf.fits --marx therm/


Here, the pre-existing simulation directory is called therm. Operationally, marxrsp will check the indicated RMF for a valid HDUCLAS3 keyword value. If HDUCLAS3=REDIST, marxrsp will read the energy.dat binary vector from the simulation directory and multiply it by the values in the RMF to determine the event pulse heights or PHA values. A new pha.dat binary vector will then be written back out to the marx simulation directory. The old pha.dat file, containing the pulse height spectrum calculated using marx’s internal redistribution function, will be renamed to pha.dat.BAK. Figure figrmf shows the pulse height spectra obtained from folding the thermal spectrum simulation from Simulating a user-defined CCD spectrum with ACIS through RMFs for an ACIS frontside and backside illuminated CCD.

By default, marxrsp will process all events in the specified simulation directory. Users may restrict which photons are folded through the RMF using the --chip parameter. For example, the command

unix% marxrsp --chip 7 --rmf acis7b_aim_pha_rmf.fits --marx therm/


would calculate pulse heights for only those events which landed on chip 7 (the aimpoint of the ACIS-S array) in the calculation of the pulse height spectrum. See marxrsp for a detailed description of all options.

Note, marxrsp cannot be used to process the output products of the marxpileup tool. marxrsp uses the binary output vector energy.dat to compute the new PHA value for an event. However, the events produced by the pileup tool are potentially the sum of multiple photons and therefore their true energies are unknown.

## Limitations of the marxrsp tool¶

Due to spatial variations in the gain across the ACIS CCDs, the detected PHA value of an event will vary even for monochromatic photons. This variation is illustrated in Figure Gain which shows the PHA spectra obtained for the S3 and I3 ACIS CCDs from a uniform illumination of 1.0 keV photons. During CXC Level 1 processing, the known calibration of the gain is used to correct the PHA values and produce a list of “pulse invariant” (PI) detector channels. These PI values are essentially uniformly binned energy values with bins of 14.6 eV. marx emulates this behavior in marx2fits by using the same ACIS gain map as the CXC Level 1 pipeline. However, processing a simulation with marxrsp is equivalent to replacing the actual spatially varying gains with whatever uniform value was used in the construction of the RMF. If a simulation which has been folded though an RMF file with marxrsp is subsequently written to a Level 1 FITS events with marx2fits, the PI values in the file event file will be incorrect. Consequently, if using marxrsp, users should perform all spectral extractions and data analysis in PHA space.

The PHA spectra obtained for simulations of the S3 and I3 ACIS CCDs from a uniform illumination of 1.0 keV photons. The upper curve shows the PHA spectrum for the S3 while the lower curve represents I3. Both spectra have been normalized to the same total number of counts.