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Contents:
17 Feb 2011 - ACIS peaks and sigmas
24 Mar 2011 - ACIS line fluxes
04 May 2011 - XIS peaks versus COR
04 May 2011 - IACHEC plots: ACIS & XIS peaks, FWHMs & line fluxes
21 Jun 2011 - Is line centroid a good proxy for CTI?
17 Oct 2011 - Figures for paper?
31 Oct 2011 - Trailing charge
31 Oct 2011 - Figures for paper
21 Nov 2011 - OLD Schematic figures for paper
02 Dec 2011 - CTI change at -120C and -90C on ACIS
20 Dec 2011 - Schematic figures for paper
02 Feb 2012 - XIS Perseus analysis for non-CTI changes
09 Feb 2012 - XIS Perseus analysis for non-CTI changes, part II
05 Sep 2012 - ACIS fits with Gehrels weighting
05 Sep 2012 - cal source plots
14 Sep 2012 - XIS fits with Gehrels weighting
14 Sep 2012 - XIS background trend from night Earth data
24 Sep 2012 - new cal source plots
25 Sep 2012 - perseus intercepts
31 Oct 2012 - XIS BG trend from night Earth data, updated
31 Oct 2012 - XIS + ACIS background spectra with lines ID'd
17 Jan 2014 - XIS + ACIS calibration source spectra overplotted
17 Jan 2014 - XIS + ACIS background spectra with lines ID'd, version 2
13 Mar 2014 - new cal source plots

SPENVIS work has its own page: spenvis

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17 Feb 2011 - Catherine's attempt to duplicate Bev's monthly XIS plots for ACIS I3 (FI) and S3 (BI). Each data point is a fit to 0.1 years worth of cold ACIS calibration source data, filtered to include only the upper corner regions like XIS and grades G02346. After some testing as to which fitting procedures were less sensitive to background variations (important for ACIS probably not as much for XIS), and robust against low signal-to-noise data, I chose to use a Gaussian plus a linear background component (mpfitfun.pro Anchoranchor1anchor117 Feb 2011 - Catherine's attempt to duplicate Bev's monthly XIS plots for ACIS I3 (FI) and S3 (BI). Each data point is a fit to 0.1 years worth of cold ACIS calibration source data, filtered to include only the upper corner regions like XIS and grades G02346. After some testing as to which fitting procedures were less sensitive to background variations (important for ACIS probably not as much for XIS), and robust against low signal-to-noise data, I chose to use a Gaussian plus a linear background component (mpfitfun.pro with some limits to prevent non-physical fits).

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calibration source plots. I fit the peak in adu for each quad separately, then re-processed using the main fe55 peak as the gain, then plotted quads A&D combined. I normalized by dividing by the total number of counts in the spectrum from 0 to 10 keV but only plotted 1 to 10. g02346 events only.

both side by side
both stacked
acis only
xis only

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the gain, then plotted quads A&D combined. I normalized by dividing by the total number of counts in the spectrum from 0 to 10 keV but only plotted 1 to 10. g02346 events only.

both side by side
both stacked
acis only
xis only

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Sep 14, 2012 - Catherine

Figures 5 (xis peaks vs time), 8 (xis fwhm vs time), 12 (xis peak vs cor) and 13 (xis fwhm vs for) using Gehrels weighting in the fits and showing the error bars. The Gehrels results are similar to what's in the paper except for fwhm vs time which increasing more slowly in the Gehrels fits.

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Sep 14, 2012 - Eric

Trend of the XIS NXB from night Earth data, extracting a 512x512 box from the chip center, using only COR2>6 data with normal SCI on (XIS1 at 2 keV level). XIS1 has a clear downward slope of -0.003 cts/s/yr +/- 20%, or about 3% per year. XIS0,3 are consistent with no change. Perhaps this is actually a gain issue with XIS1.

Look at the PDF also.

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Update post-meeting: Now including all COR2, 5-15 keV (to reduce gain effects around 7 keV). XIS1 still changes by 4% +/- 1% per year, though with lots of scatter. +/-1-sigma limits for FIs: +0%/-1% (XIS0), +0.5%/-0.5% (XIS3).

Look at the PDF also.

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XIS NXB spectra from Tawa et al 2008 (Fig 1):

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Sep 24, 2012 - Bev

New version of cal source plots.

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eps version for .tex.

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Sep 25, 2012 - Bev

I took the intercept of peak vs row for the main iron line in the perseus data
and fit it versus time. The summary is that the intercept is dropping less than half a percent per year for the higher CI levels and less than 1 percent per year for the original, lower, BI level.

CCD

quad

CI

 

adu/year

error (edu/year)

XIS1

c0

higher CI

3 SRs

-5.39

21.81

XIS1

c0

original CI

12 SRs

-15.24

1.56

XIS1

c1

higher CI

3 SRs

1.63

3.59

XIS1

c1

original CI

12 SRs

-8.94

0.47

XIS1

c2

higher CI

3 SRs

-2.42

4.03

XIS1

c2

original CI

12 SRs

-11.25

0.48

XIS1

c3

higher CI

3 SRs

6.52

10.35

XIS1

c3

original CI

12 SRs

-11.54

1.59

XIS3

c0

FI CI

13 SRs

-5.41

0.95

XIS3

c1

FI CI

13 SRs

-3.66

0.32

XIS3

c2

FI CI

13 SRs

-3.54

0.26

XIS3

c3

FI CI

12 SRs

-5.07

0.82

ps of plots. individual eps files available on request.

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Oct 31, 2012 - Eric

Trend of the XIS NXB from night Earth data, extracting all but the cal source regions and bad regions of each chip, using all COR2 data with normal SCI on (XIS1 at 2 keV level). See previous post.

Here it is in 4 week bins, with the XIS1 y errorbars corresponding to the counting statistics. First using FTOOL lcurve:

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Second doing this by hand in xselect by and-ing a 4 week time range with the GTIs:

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I don't understand the scatter; each bin contains about 50 ksec of data, 1000's of counts, and should span a similar distribution of COR2, yet there is an intrinsic ~ 25% scatter, far higher than the < 5% quoted by Tawa. Restricting COR2>=10 does not change this, nor do larger time bins. Perhaps something is wrong with the GTIs and thus the effective exposure time calculation.

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Oct 31, 2012 - Eric

Background spectra for XIS and ACIS with lines ID's a lo Tawa:

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Also the EPS for the paper.

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Jan 17, 2014 - Bev

Calibration source spectra for XIS and ACIS:

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Also the EPS for the paper.

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Jan 17, 2014 - Eric

Background spectra for XIS and ACIS with lines ID's a la Tawa,
now with "FI CCD" and "BI CCD" identified.

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Also the EPS for the paper.

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Mar 12, 2014 - Bev

Calibration source spectra for XIS and ACIS:

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Also the EPS for the paper.

Figures 5 (xis peaks vs time), 8 (xis fwhm vs time), 12 (xis peak vs cor) and 13 (xis fwhm vs for) using Gehrels weighting in the fits and showing the error bars. The Gehrels results are similar to what's in the paper except for fwhm vs time which increasing more slowly in the Gehrels fits.

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Trend of the XIS NXB from night Earth data, extracting a 512x512 box from the chip center, using only COR2>6 data with normal SCI on (XIS1 at 2 keV level). XIS1 has a clear downward slope of -0.003 cts/s/yr +/- 20%, or about 3% per year. XIS0,3 are consistent with no change. Perhaps this is actually a gain issue with XIS1.

Look at the PDF also.

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Update post-meeting: Now including all COR2, 5-15 keV (to reduce gain effects around 7 keV). XIS1 still changes by 4% +/- 1% per year, though with lots of scatter. +/-1-sigma limits for FIs: +0%/-1% (XIS0), +0.5%/-0.5% (XIS3).

Look at the PDF also.

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