nasa logo, link to nasa home page Goddard Space Flight Center
NASA
> GSFC > Astrophysics Science Division > IXO
   + Search NASA
+ Google Search IXO
+ Intranet + Fast Facts + FAQs + Contact Us + Site Map
+ Home + Science + Technology + People + News + Resources

Related sites

+ NASA
+ NASA GSFC
+ ESA
+ JAXA

 


print Print this page

You are here: Science»  IXO Simulation Tools»  IXO Simulator—Response Matrices

Response Matrices

  2010  ››    2008  ›› 

Important information for anyone using these files

The most recent Segmented Glass optics responses are given here. SPO responses generated by Tim O˘sterbroek are available from the ESA web site. If you have any questions concerning using these response files for IXO spectral simulations or requests for assistance with scenarios not represented here, feel free to contact the IXO team. Segmented Glass optics response files were generated by Andrew Ptak using a glass mirror effective areas derived by Paul Reid and the same detector efficiencies as used in the SPO response files.

As the IXO mission is still under development, the exact specifications of the IXO mirrors and detectors are subject to change at any time.

  • Response Matrices – 2010 lists the current best files. Previous versions are available from here.
  • In some cases, multiple files will be given for the same topic, indicating a study is underway comparing the different designs. Please do all simulations using as many different cases as practical.
  • All of the files on this page follow a fixed format, and contain the date of their creation.
  • The file names are constructed using the following key: telescope_instrument_filter_[area]_date.rsp, where telescope = ixo-glass (indicating that the response matrices refer to the Segmented Glass optics option).
  • Whenever you generate a simulation using one of these responses, make sure any results clearly indicate which responses were used.
  • IXO_Matrices_v2.0.pdf outlines the various input parameters for the generation of the IXO response matrices, you may use this information for your reference.

When downloading files, please 'shift-click' rather than simply 'clicking' on the file links.

top of page Top

Response Matrices – 2010


Memo

IXO_glass_responses.pdf – a memo describing the matrices, June 20, 2010

top of page Top

XMS response matrices

XMS Core (glass)

Current version: ixo-glass-xms-none-20100524.rsp, June 20, 2010

Notes

Constant Gaussian response with FWHM=2.5 eV with 0.5 eV bin channels. The calorimeter core array of 40 × 40 pixels maintains a 2.5 eV resolution (FWHM) at all energies.

Previous versions

Available from here.

XMS (SPO)

Available from the ESA web site  »

Previous versions

Available from here.

top of page Top

Wide-Field Imager response matrices

WFI (glass)

Current versions: June 20, 2010

Notes

The WFI is a DEPFET-type detector, with the significant advantage over earlier CCD-type detectors in that the charge in each pixel is read directly, rather than being transferred from row to row and read out. However, the overall resolution is still limited by the statistics of electron counting to be on order 100 eV. ixo-glass-wfi-alpp-20100625.rsp includes a thick optical blocking filter will be required for most observations to reduce optical loading.

WFI (SPO)

Available from the ESA web site  »

Previous versions

Available from here.

top of page Top

Hard X-ray Imager response matrices

Current version: TBA.

HXI (SPO)

Available from the ESA web site  »

Previous versions

Available from here.

top of page Top

X-ray Grating Spectrometer response matrices

XGS (glass)

Current version: ixo-glass-catxgs-none-20100524.rsp, June 20, 2010

Notes

Model calculations of the XGS response for the critical angle transmission (CAT) and off-plane (OP) grating designs. An OP-XGS glass response will be released in the future.

XGS (SPO)

Available from the ESA web site  »

Previous versions

Available from here.

High Timing Resolution Spectrometer response matrices

HTRS (glass)

Current versions: June 20, 2010

Notes

The HTRS is a non-imaging silicon detector capable of detecting extremely high count rates – up to 1 Million counts/s. Three different filter settings are included to allow estimates under different optical loading conditions.

HTRS (SPO)

Available from the ESA web site  »

Previous versions

Available from here.

top of page Top

X-ray Polarimeter response matrices

X-ray Polarimeter (glass)

Current version: ixo-glass-xpol-20100524.rsp, June 20, 2010

Notes

X-ray Polarimeter matrix using Glass optics FMA effective area.

X-ray Polarimeter (SPO)

Available from the ESA web site  »

Previous versions

Available from here.

top of page Top


Response Matrices – 2008


Calorimeter response matrices – 2008

Calorimeter Core (glass): ixo_ucal_0p5_081030.rsp

Version: October 30, 2008

Constant Gaussian response with FWHM=2.5 eV with 0.5 eV bin channels. The calorimeter core array of 40 × 40 pixels maintains a 2.5 eV resolution (FWHM) at all energies. The default response matrix uses bins 0.5 eV wide, which may not be ideal for all projects. If higher resolution is needed, the file ixo_ucal_0p2_081030.rsp uses 0.2 eV bins and should allow the best possible calculation of line centroids. Conversely, if resolution is less important and the 0.5 eV bin file is too big or slow, a much smaller file ixo_ucal_5p0_081030.rsp is available that uses 5 eV bins.

Calorimeter Core (Pore): IXO_CDF_tes_none_081117.rsp

Version: November 17, 2008

Matrix is from Tim Oôsterbroek; This was generated assuming a Carbon-overcoating and the loss in effective area due to the grating has been modeled and taken into account.

Calorimeter Outer (glass): ixo_ucal_outer_081105.rsp

Version: November 5, 2008

Constant Gaussian response with FWHM=10 eV with 1 eV bin channels. The outer calorimeter array uses larger pixels which use 4 separate absorbers for each transition-edge sensor (TES) pickup. This arrangement allows a larger FOV, but with a larger 10 eV resolution (FWHM) at all energies.

top of page Top

Wide-Field Imager response matrices – 2008

WFI: ixo_mdl_wfi_default_081030.rsp

Version: October 30, 2008

Sample matrix using Glass optics FMA effective area; from Tim Oosterbroek. The WFI is a DEPFET-type detector, with the significant advantage over earlier CCD-type detectors in that the charge in each pixel is read directly, rather than being transferred from row to row and read out. However, the overall resolution is still limited by the statistics of electron counting to be on order 100 eV.

WFI (pore): IXO_CDF_wfi_default.rsp

Version: December 10, 2008

WFI response using Pore optics with an Iridium (+ Carbon overcoat) coating; from Tim Oôsterbroek. The WFI is a DEPFET-type detector, with the significant advantage over earlier CCD-type detectors in that the charge in each pixel is read directly, rather than being transferred from row to row and read out. However, the overall resolution is still limited by the statistics of electron counting to be on order 100 eV.

WFI (pore with multi-layer): IXO_CDF_hard_wfi_default.rsp

Version: December 10, 2008

WFI response using multi-layer coating(r < 47cm) from Japanese group that increases hard X-ray response, primarily in the 10-15 keV region; from Tim Oôsterbroek. The WFI is a DEPFET-type detector, with the significant advantage over earlier CCD-type detectors in that the charge in each pixel is read directly, rather than being transferred from row to row and read out. However, the overall resolution is still limited by the statistics of electron counting to be on order 100 eV.

top of page Top

Hard X-ray Imager response matrices – 2008

Hard X-ray Imager (Con-X-type): conx-hxt-080215.rsp

Version: February 15, 2008

A placeholder matrix with the same area as presented by Paul Gorenstein at the Dec 2006 Con-X FST meeting for a dual HXT option, and a "NuStar"-type CZT energy resolution. The exact specifications of the HXT mirror is still in flux. The matrix given here is from the original Constellation-X design, and overestimates the current effective area by a factor of 1.67.

Hard X-ray Imager (pore): IXO_CDF_hard_cdte_none_081117.rsp

Version: November 17, 2008

Hard X-ray response using multi-layer coating (r < 47 cm) on the pore optics FMA.

X-ray Grating Spectrometer response matrices – 2008

XGS (requirement): xgs_081216.rsp

Version: December 16, 2008

This matrix is unphysical but effectively describes the minimum requirements (effective area of 0.1 m2, R=3000) for the IXO gratings. The energy range covers 0.3-1.0 keV.

top of page Top

High Timing Resolution Spectrometer response matrices – 2008

HTRS (glass): ixo_mdl_htrs_default_081030.rsp

Version: October 30, 2008

Sample matrix using Glass optics FMA effective area; from Tim Oôsterbroek. The HTRS is a non-imaging silicon detector capable of detecting extremely high count rates – up to 1 Million counts/s.

HTRS (pore): IXO_CDF_htrs_default_081117.rsp

Version: November 17, 2008

From Tim Oôsterbroek; This was generated assuming a Carbon-overcoating and the loss in effective area due to the grating has been modeled and taken into account. The HTRS is a non-imaging silicon detector capable of detecting extremely high count rates – up to 1 Million counts/s.

top of page Top

X-ray Polarimeter response matrices – 2008

X-ray Polarimeter (glass): ixo_mdl_xpol_default_081030.rsp

Version: October 30, 2008

X-ray Polarimeter matrix using Glass optics FMA effective area; from Tim Oôsterbroek.

X-ray Polarimeter (pore): IXO_CDF_xpol_default_081117.rsp

Version: November 17, 2008

X-ray Polarimeter matrix using Pore optics FMA effective area assuming a Carbon-overcoating and the loss in effective area due to the grating has been modeled and taken into account; from Tim Oôsterbroek.

top of page Top


 
esa jaxa nasa logos esa home page jaxa home page nasa home page