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Troubleshooting Noisy Pixels in Data Reduction

Learn how to handle noisy pixels impacting data analysis processes. Understand the effects of hot and noisy pixels on data reduction methods and solutions for better flare screening. This comprehensive guide by Michael Smith from ESAC provides insights on addressing noisy pixels and optimizing data reduction workflows.

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Troubleshooting Noisy Pixels in Data Reduction

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  1. PN Monitoring Mallorca, October 2006 Michael Smith, ESAC

  2. Hot Pixels Michael Smith, ESAC

  3. FF 50-Iteration Offset Introduction Noisy Pixels Michael Smith, ESAC

  4. Noisy Pixels Michael Smith, ESAC

  5. Rev 156 Impact Noisy Pixels and Telemetry Load Fraction of counts due to Noisy Pixels Per Quadrant Michael Smith, ESAC

  6. Noisy Pixels and Telemetry Load CCD 11 Column 63 Fraction of counts due to Noisy Pixels Per CCD of Quadrant 3 Should we blank CCD 11 Column 63 (at least partially)??? Michael Smith, ESAC

  7. Hot + Noisy Pixels: Effects on Data Reduction Some very hot pixels are not flagged by standard use of epproc/ epchain: • epproc/epchain call badpixfind with default high energy threshold of 12 keV (parameter hienergythresh=12) Combination of noisy and very hot pixels (E > 12 keV) results in problems with flare screening GTI creation (at least when following the EPIC analysis threads): • b/g rate curve selection expression: #XMMEA_EP && (PATTERN==0) && (PI>10000) • so very hot pixels are “missed”, and if these happen to be noisy… Michael Smith, ESAC

  8. Hot + Noisy Pixels: Effects on Data Reduction Background Rate Curve for Flare Screening Michael Smith, ESAC

  9. Hot + Noisy Pixels: Effects on Data Reduction Hot & Noisy Pixel in CCD 11 Column 63 Offset Trend Frequency Trend Michael Smith, ESAC

  10. >10 keV and 10-12 keV rates are highly correlated Hot + Noisy Pixels: Effects on Data Reduction For flare screening the solution could be to create the b/g curve in 10 - 12 keV band: #XMMEA_EP && (PATTERN==0) && (PI>10000) && (PI<12000) with a suitably adapted threshold (0.4 counts/s) This is an incomplete solution: The bad pixels remain in the calibrated events file! Michael Smith, ESAC

  11. Offset Median Michael Smith, ESAC

  12. Eclipse Season Boundaries First Observations per Revolution Offset Variance Michael Smith, ESAC

  13. Offset Maps Normal Variance Excessive Variance Michael Smith, ESAC

  14. Mean Row Offset vs RAWY Normal Variance Michael Smith, ESAC

  15. Mean Row Offset vs RAWY Excessive Q0 & Q2 Variance Michael Smith, ESAC

  16. Mean Row Offset vs RAWY Excessive Q1 & Q3 Variance Michael Smith, ESAC

  17. CalClosed Line Widths vs Offset Map Variance Quadrant 0 Quadrant 1 Michael Smith, ESAC

  18. Energy Scale vs Time very good, esp. for FF mode. Slight over-correction for EFF mode. SW mode under-correction, esp. at Mn (Result of SAS 6.5 Processing) Michael Smith, ESAC M. Kirsch

  19. Line width trend is stable ~0.5 ADU/year increase at Mn (Result of SAS 6.5 Processing) Michael Smith, ESAC M. Kirsch

  20. MOS Monitoring Mallorca, October 2006 Michael Smith, ESAC

  21. MOS1 Bad Pixels MOS2 Michael Smith, ESAC

  22. Michael Smith, ESAC

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