XMM-Newton Science Analysis System


esas (esas-0.10.5) [xmmsas_20190531_1155-18.0.0]

Description

This package consists of a collection of XMM-Newton Extended Source Analysis Software (XMM-ESAS) tasks originally developed by Snowden, et al. and released as a stand-alone package in 2008. This package follows the methods outlined in Snowden et al. (2008)[1] for the analysis of extended objects and the diffuse background using XMM-Newton EPIC MOS and pn observations.

Two separate features are incorporated into ESAS; the capability of creating model quiescent particle background spectra (Kuntz & Snowden 2008)[2] for user defined regions of the detectors and the capability of creating background subtracted and exposure corrected images. Also included in the XMM-ESAS package is software to mosaic multiple and not necessarily coaligned observations of regions on the sky.

SAS/ESAS Task Descriptions:

FORTRAN routines:

• adapt $-$ FORTRAN

  adapt is an adaptive filtering routine used to create smoothed background subtracted and exposure corrected images for individual exposures or exposures from a single observation combined by the task comb. For each unmasked pixel, the program will average neighboring pixels within a circle of increasing radius until a selected number of counts is reached. The original pixel is then given the average surface brightness for the pixels within the circle. Images can also be binned before smoothing.

• adapt_merge $-$ FORTRAN

  adapt_merge adaptively smooths background subtracted and exposure corrected mosaicked images using the output of merge_comp_xmm. For each unmasked pixel, the program will average neighboring pixels within a circle of increasing radius until a selected number of counts from the count image is reached. The original pixel is then given the average surface brightness for the pixels within the circle. The images can also be binned before smoothing.

• bin_image $-$ FORTRAN

  bin_image produces binned count rate and count-rate uncertainty images of single observations. It can use either individual exposures or the output of the program comb which can merge all of the exposures associated with a single ObsID. For each unmasked and binned pixel, the program will determine the average count rate and the count rate uncertainty. The assumption is that the uncertainty is dominated by the counting statistics and the the systematics of the background modeling. Integer binning, including by 1 for no binning, is supported.

• bin_image_merge $-$ FORTRAN

  bin_image_merge bins mosaicked images combined by the task merge_comp_xmm into count rate and count rate uncertainty images. For each unmasked and binned pixel, the program will determine the average count rate and the count rate uncertainty. The assumption is that the uncertainty is dominated by the counting statistics and the the systematics of the background modeling. Integer binning, including by 1 for no binning, is supported.

• clean $-$ PERL

  clean deletes a number of intermediate and unneeded files after the processing is complete.

• cheese $-$ PERL

  cheese does source detection and creates cheese masks for point-source masking during image processing. cheese allows the user to set a flux threshold over the field for the removal of the source contributions to the spectra as well as the images.

• cheese-bands $-$ PERL

  cheese-bands does source detection and creates cheese masks for point-source masking during image processing in three bands: soft, hard, and combined. cheese-bands allows the user to set a flux threshold over the field for the removal of the source contributions to the spectra as well as the images.

• comb $-$ FORTRAN

  comb combines co-aligned event, exposure, QPB, SP, and SWCX background images from different exposures and different instruments from the same ObsID.

• conv_reg $-$ FORTRAN

  conv_reg converts region information in celestial coordinates into region information in detector coordinates. It will do so for region fits files, ascii lists, or individual regions. Development in progress.

• conv-region $-$ PERL

  conv-region converts a region file in celestial coordinates into regions files in detector coordinates for all active detectors in all observations in a list of ObsIDs. Development in progress.

• make_mask $-$ FORTRAN

  make_mask is called by the task cheese to produce a cheese mask.

• make_mask_merge $-$ FORTRAN

  make_mask_merge produces cheese masks in the total band (cheese) or soft, hard, and combined bands (cheese-bands) using a merged source list produced by the task merge-source-list from the maximum likelihood source lists produced by cheese or cheese-bands.

• merge_comp_xmm $-$ FORTRAN

  merge_comp_xmm creates mosaicked count, exposure, QPB, SP, and SWCX background images for multiple observations and exposures.

• merge_source_list $-$ FORTRAN

  merge_source_list creates a master list of sources detected from a list of observations which have been processed to the point of a creating an emldetect source lists produced by cheese or cheese-bands. Sources are compared and those within 2" of each other have the one with the lower flux thrown out.

• mos_back $-$ FORTRAN

  mos_back takes the output of the perl script mos-spectra and creates quiescent particle background (QPB) spectra and images in detector coordinates, as selected, for EPIC MOS data.

• mos-filter $-$ PERL

  mos-filter filters and cleans the event files of SP contamination using the SAS task espfilt. Along with a filtered event file it produces a QDP plot file showing the observation light curves and indicates the accepted time intervals.

• mos-spectra $-$ PERL

  mos-spectra processes the filtered event files from the task mos-filter to produce a set of intermediate files for the production of QPB background spectra and images. mos-spectra also produces source spectra and the appropriate Redistribution Matrix Files, RMFs, and Ancillary Region Files, ARFs, for spectral analysis.

• pn_back $-$ FORTRAN

  pn_back takes the output of pn-spectra and creates QPB spectra and images in detector coordinates, as selected, for EPIC pn data.

• pn-filter $-$ PERL

  pn-filter is the initial processing script for pn data and it performs the same tasks as mos-filter for MOS data. Each exposure is processed in both normal and out-of-time (OOT) modes.

• pn-spectra $-$ PERL

  pn-spectra provides the same functions for pn data as mos-spectra provides for the MOS. However, it also creates spectra and images from the out-of-time processing.

• point_source $-$ FORTRAN

  point_source calculates the appropriate Xspec normalization for the extragalactic background given the user-selected point-source exclusion threshold.

• proton $-$ FORTRAN

  proton produces images in detector coordinates of the model residual soft proton (SP) contamination. To do so, it uses the fitted values of the SP component from Xspec and standard detector maps.

• proton_scale $-$ FORTRAN

  proton_scale extracts the appropriate scale factors for the solid angle and relative SP contributions to include in spectral fitting.

• rot_det_sky $-$ FORTRAN

  rot_det_sky is called by the rot-im-det-sky task. It does the heavy lifting of rotating the QPB images output from mos_back and pn_back, the SP images output from proton, and the SWCX output from swcx which are in detector coordinates, into images in sky coordinates.

• rot-im-det-sky $-$ PERL

  rot-im-det-sky rotates both the model QPB, SP, and SWCX background images from detector coordinates to sky coordinates.

• sp_partial $-$ FORTRAN

  sp_partial scales the SP spectral fit results from a limited region of the detector to the full field of view. This allows the user to fit for the SP contamination in regions of lower surface brightness (e.g., an outer annulus for a cluster of galaxies) which can significantly improve the accuracy of the fit.

• swcx $-$ FORTRAN

  swcx produces images in detector coordinates of the model residual SWCX contamination. To do so, it uses the fitted values of the SWCX component from Xspec and standard detector maps.