XMM EPIC-pn Spatial CTI Correction using Cu K? and Mn K?

Detailed procedures for spatial CTI correction using Cu K? and Mn K? in XMM EPIC-pn detectors, including applying long-term CTI corrections, stacking event lists, extracting spectra, fitting Cu K line, and deriving spatial offsets. Examples show improvements in velocity space after corrections. Validation involves applying Cu-derived offsets to Mn K line and checking results at lower energies for validation.

• XMM EPIC-pn
• Spatial CTI correction
• Cu K?
• Mn K?
• Detectors

tre_h Follow

Uploaded on Oct 03, 2024 | 0 Views

Download Presentation

Please find below an Image/Link to download the presentation.

The content on the website is provided AS IS for your information and personal use only. It may not be sold, licensed, or shared on other websites without obtaining consent from the author.If you encounter any issues during the download, it is possible that the publisher has removed the file from their server.

You are allowed to download the files provided on this website for personal or commercial use, subject to the condition that they are used lawfully. All files are the property of their respective owners.

The content on the website is provided AS IS for your information and personal use only. It may not be sold, licensed, or shared on other websites without obtaining consent from the author.

Presentation Transcript

1. XMM EPIC-pn: spatial CTI correction using Cu K? ? and Mn K? ? (update from IACHEC 22) Ivan Valtchanov, XMM SOC IACHEC, Pelham, Germany, 24-27 Apr 2023 IACHEC 23, Detectors and Background Working Group session 1

2. Spatial CTI offsets Following Sanders, Dennerl et al. (2020), used in Gatuzz et al, (2022a, 2022b): 1. Apply the derived per-CCD long-term CTI correction for Cu K @8 keV 2. Stack event lists in bins of 500 revolutions, with step 250 (overlap) 3. For each stacked table, extract spectra for each CCD (12), read-out column RAWX (64) and bin by 20 pixels on RAWY (9). 4. Fit the Cu K line and derive the residual the spatial offsets as function of epoch, CCDNR, RAWX, RAWY. Spatial offset table dimensions: mode(2),epoch(8),CCDNR(12),RAWX(64),RAWY(200) IACHEC 23, Detectors and Background Working Group session 2

3. Example for modelling the LTC, CCD02 Q(t) = Eobs/8.04 keV Cyan curve: [(1-TCOEF(t))/(1-a)]^{190} Using <RAWY> for all observations 3

4. Cu K before and after Offsets in eV applied at event list level IACHEC 23, Detectors and Background Working Group session 4

5. Example, correction Procedure: 1. Apply derived offsets to the stacked event list 2. PI PI_CORR for all events 3. Fit Cu Ka using PI_CORR Overall: going down from ~30 eV to ~3 eV Taking the rms as redshift and then c*z Improvement in velocity space: ~1120 km/s (30 eV) to ~112 km/s (3 eV) IACHEC 23, Detectors and Background Working Group session 5

6. Full Frame Mode CU for Cu K Before, st.dev. After, st.dev. IACHEC 23, Detectors and Background Working Group session 6

7. Extended Full Frame Mode CU Before After Significant improvement in this quandrant! IACHEC 23, Detectors and Background Working Group session 7

8. Applying the spatial offsets to other energies? In Sanders et al. (2020) the derived offsets are applied to energies down to ~ 6 keV, i.e. for the iron complex at ~6.5 keV (galaxy clusters) To validate, we apply the Cu-derived offsets to the Mn K line at ~6 keV, internal calibration source Source is faint after rev. 2000 no results in most of the spatial bins Check at rev. < 2000 for validation IACHEC 23, Detectors and Background Working Group session 8

9. Mn K before and after CU correction IACHEC 23, Detectors and Background Working Group session 9

10. Marginal improvement IACHEC 23, Detectors and Background Working Group session 10

11. Mn K before and after MN correction IACHEC 23, Detectors and Background Working Group session 11

12. Mn K before and after CU and MN corrections Only FF mode IACHEC 23, Detectors and Background Working Group session 12

13. Energy scale in [6,9] keV IACHEC 23, Detectors and Background Working Group session 13

14. 6-lines model examples, full CCD areas Rev in [500,999] Rev in [2500,2999] IACHEC 23, Detectors and Background Working Group session 14

15. IACHEC 23, Detectors and Background Working Group session 15

16. Energy dependence of the long-term CTI Al K Cu K Mn K IACHEC 23, Detectors and Background Working Group session 16

17. Summary Spatial residuals derived using the fluorescent Cu K line at 8 keV Spatial residuals derived using the cal source Mn K line at 6 keV Both incorporated in EPN_SPATIALCTI_0001.CCF (Both with caveats) XMM-SAS task epspatialcti modified to use the new CCF with option SD20mode=yes (set as default) One can choose either to apply the Cu K or Mn K with element=CU or element=MN Inconclusive analysis of the energy scale compression in 6 to 9 keV not implemented. Release note: https://xmmweb.esac.esa.int/docs/documents/CAL-SRN-0391-1-3.pdf IACHEC 23, Detectors and Background Working Group session 17

18. The end IACHEC 23, Detectors and Background Working Group session 18