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Astronomical Data Analysis Software and Systems VII
ASP Conference Series, Vol. 145, 1998
Editors: R. Albrecht, R. N. Hook and H. A. Bushouse

ASC Coordinate Transformation -- The Pixlib Library, II

H. He, J. McDowell and M. Conroy
Harvard-Smithsonian Center for Astrophysics
60 Garden Street, MS 81
Cambridge, MA 02138, Email:hhe@cfa.harvard.edu

 

Abstract:

Pixlib, an AXAF Science Center (ASC) coordinate library, has been developed as the continuing effort of (He 1997). Its expansion includes, handling of the High Resolution Mirror Assembly (HRMA) X-ray Detection System (HXDS) stage dither and the five-axis mount (FAM) attachment point movements, correction of misalignments of the mirror mount relative to X-ray calibration facility (XRCF) and to the default FAM axes, as well as solution of sky aspect offsets of flight, etc. In this paper, we will discuss the design and the configuration of the pixlib system, and show, as an example, how to integrate the library into ASC data analysis at XRCF.

             

1. Introduction

The work of He (1997) established a preliminary framework for the pixlib system, including the parameter-interface data I/O structure, matrix calculation algorithm, and coordinate transformation threading baselines. Since then, the library has undergone thorough re-organization and expansion to meet the AXAF on-going requirements of both ground calibration and flight observation. At the time of writing, the library is about 95% completed with approximate 6000 source lines of codes. It was successfully integrated and built during the XRCF calibration phase.

In this paper, we will highlight the system design and architecture of the library, complementary to the early work, and describe the system configuration in terms of user application. The complexities of coordinate transformation at XRCF and the resolutions will be discussed.

2. Architecture of the ASC Coordinate Library

The building blocks of the Pixlib library are three sub-systems, core, auxiliary, and application interface (API), and the foundation of the library is built with the parameter-interface structure. Figure 1 sketchs the architecture of the library.

 

Figure 1: Pixlib library architecture, constructed on three sub-systems which are layered on the parameter-file structure.

As discussed in He (1997), the design of pixlib is modular to allow system expandibility, easy maintenance and simple ways to incorporate new scientific knowledge. The core sub-system, which includes 8 modules (see Figure 2 for details), builds the ASC coordinate frameworks of grating, FAM motion, sky aspect offsets, telemetry (raw) reads, detector-chip tiling, and coordinate transformation among chip pixels and celestial angles. Because of the common needs of generic data sources, handy utilities, module-to-module communication, etc., the library is supported with a 4-module auxiliary sub-system, as shown below.

      pix_errstatus.c    -- error handling 
      pix_utils.c        -- utility functions 
      pix_common.c       -- common data sources to all modules 
      pixlib_hiden.c     -- internal configuration, bookkeeping

The upper-level interface of the library is implemented in the module pixlib.c, which distributes functions between the lower-level modules. pixlib.c, in large part, provides setup functions for system configuration, and other API functions are implemented locally without the need for cross-module function calls. All the API functions are identified by the ``pix_'' prefix.

The data in-stream of the parameter-interface approach simplifies system configuration and data readability. The number and organization of those data files have remained almost same as described in He (1997) with few updates. pix_pixel_plane.par, substituting the original pix_size_cnter.par, groups 2-D pixel system parameters of focal plane, tiled detector, grating dispersion together; pix_grating.par is added to define dispersion period and angle of grating arms.

 

Figure 2: Pixlib data flow and system configuration. Each smaller box above represents a module. For example, the ``raw'' and ``cpc2stf'' boxes denote the modules of pix_raw.c and pix_cp2stf.c, respectively. 

3. System Configuration

Prior to application program execution, the library needs to be configured properly. The system configuration is optionally either static or dynamic, as illustrated in Figure 2. A set-parameter-value to a parameter file, pix_coords.par, handles the static configuration and the user can set values for the following parameters.

  flength = Telescope focal length in mm 
 aimpnt   = Name of aim point  of detector 
    fpsys = Focal Plane pixel system 
  tdetsys = Tile Detector pixel system 
   gdpsys = Grating Dispersion pixel system
  grating = Grating arm
    align = FAM    misalignment angle in degrees(pitch, yaw, roll)
   mirror = mirror misalignment angle in degrees(pitch, yaw, roll)

In the course of the system initiation, executed through pix_init_pixlib(), internal functions lookup the parameter table to parse the information down to relevant modules, which are then configured accordingly.

An alternative way to configure the system is to make function, ``pix_set_*", calls in application program following the initiation. pix_set_flength(int), for instance, is equivalent to the pset ``flength'' for pix_coords.par, and

pix_set_fpsys(int) to the pset ``fpsys'', to name a few. The consequence of those calls is to override the static configuration which is the system defaults.

4. Coordinate Transformation at XRCF

Coordinate transformations at XRCF need to be carefully handled when the FAM feet move and the HXDS stage dithers. In the default, boresight configuration the FAM axes are parallel to the XRCF (and Local Science Instrument, LSI) axes, but they may undergo some movements in addition to the HXDS stage dithering and possible mirror mount movement. Therefore, those effects, as listed below, must be accounted for before coordinate transformations between focal plane and LSI system are made:

• misalignments of the default FAM axes from the mirror due to FAM attachment point motion,
• motion of the HXDS stage from the default FAM reference point,
• possible misalignments of the mirror mount relative to the XRCF prescribed by pitch-yaw angles,
• misalignments of the FAM axes from the default due to FAM feet motion.

The following two functions, in addition to other generic configurations, effectively supply the system configuration for coordinate transformation at XRCF. The routine

   pix_set_mirror (double hpy[2],       /* in degrees */
                   double stage[3],     /* in mm      */
                   double stage_ang[3]) /* in degrees */

corrects misalignment from the mirror axis by measuring its displacement from the boresight configuration of the default FAM frame (stage_ang) for a given mirror position (hpy) in mirror nodal coordinate system. The hpy is measured in HRMA pitch and yaw axes, and the HXDS stage position (stage) monitored relative to the default FAM reference point. The routine

   pix_set_align(
       double mir_align[3], /* (yaw, pitch, roll), in degrees */
       double stg_align[3]) /* (yaw, pitch, roll), in degrees */

serves to assess

• misalignments of mirror mount (mir_align) relative to XRCF axes are measured in the given yaw-pitch-roll Euler angles in the mirror nodal coordinate, and
• misalignments of the default FAM (stg_align) relative to XRCF axes are corrected in terms of yaw-pitch-roll Euler angles in the default FAM frame.

The system configuration above was successfully applied to and integrated into ASC data analysis during the X-ray calibration.

Acknowledgments:

We gratefully acknowledge many fruitful discussions with ASC members. This project is supported from the AXAF Science Center (NAS8-39073).

References:

McDowell, J., ASC Coordinates, Revision 4.1, 1997, SAO/ASCDS.

He, H., McDowell, J., & Conroy, M., 1997, in Astronomical Data Analysis Software and Systems VI, ASP Conf. Ser., Vol. 125, eds. Gareth Hunt and H. E. Payne (San Francisco, ASP), 473.

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