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From: audard@astro.columbia.edu
Subject: EPIC CTI correction for timing mode
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4 replies: 1 2 3 4
2 followups: 1 2

Private message: yes  no

Notes:

Notification:


Date: Fri, 13 Jun 2003 00:13:19 GMT
From: audard@astro.columbia.edu
To: xmmhelp@xmm.vilspa.esa.es
CC: audard@astro.columbia.edu
Subject: EPIC CTI correction for timing mode
Full_Name: Marc Audard
Submission from: (NULL) (128.59.171.220)


Hi-

I noticed that the CTI correction at high energies is not good enough for
timing mode spectra. The data are shifted to smaller energies compared to
the model spectrum. In particular, the Fe Kalpha complex seems to peak at
6.63keV instead of 6.69keV.

Regards

Marc

PS: Data processed with SAS 5.4.1, EPN_CTI CCF #11, gainctiaccuracy=2.


Reply 1

Resend
From: Michel G. Breitfellner <xmmhelp@xmm.vilspa.esa.es>
To: audard@astro.columbia.edu
Subject: Re: EPIC CTI correction for timing mode (PR#8730)
Date: Fri Jun 13 14:44:06 2003
Dear Marc,

Your question was forwarded to our experts.
We will come back to you as soon as possible.

With best regards,
Michel G. Breitfellner
XMM-Newton User Support Group


Reply 2

Resend
From: Michel G. Breitfellner <xmmhelp@xmm.vilspa.esa.es>
To: audard@astro.columbia.edu
Subject: Re: EPIC CTI correction for timing mode (PR#8730)
Date: Fri Jun 13 15:47:53 2003
Dear Marc,

I assume we are talking about the PN.
Normally the relative energy calibration of the pn is better than
0.3 % over the complete energy range.

Here we see something like 1 %.
Some questions:
1. when was the observation performed. If it is very recently,
   it could be evidence for a not perfect long term CTI correction?
2. What is the source
4. What is the count rate of the source
5. Was the same source already observed in FF

With best regards,
Michel G. Breitfellner
XMM-Newton User Support Group


Followup 1

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Date: Fri, 13 Jun 2003 12:25:25 -0400
From: Marc Audard <audard@astro.columbia.edu>
To: "Michel G. Breitfellner" <xmmhelp@xmm.vilspa.esa.es>
Subject: Re: EPIC CTI correction for timing mode (PR#8730)
This is a multi-part message in MIME format.
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Content-Transfer-Encoding: 7bit

Hi Michel

Michel G. Breitfellner wrote:
> Dear Marc,
> 
> I assume we are talking about the PN.

Yes, sorry.

> Normally the relative energy calibration of the pn is better than
> 0.3 % over the complete energy range.
> 
> Here we see something like 1 %.
> Some questions:
> 1. when was the observation performed. If it is very recently,
>    it could be evidence for a not perfect long term CTI correction?

rev 316 shows it best. But the same mode and target was observed in rev
0404, and seems to again show a similar shift.

> 2. What is the source

Sigma2 CrB

> 4. What is the count rate of the source

52 ct/s (bkg subtracted; 61 c/s not subtracted)

> 5. Was the same source already observed in FF

Only in MOS2.

I need to add that the shift "seems" a bit less important now that I use APEC
1.3
(I used the default APEC 1.1, which does not have all innershell excitation Fe
lines,
thus shifting the apparent Fe Kalpha complex to higher E than it should).
However, I still
seem to see a shift. I attach a plot of the best-fit around 6-7 keV.

Regards

		Marc

PS: One additional comment: arfgen should take into account the # of RAWX
selected to
correct for energy encircled loss. I know it is in development, but would be
nice for
a future release.



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Followup 2

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Date: Fri, 13 Jun 2003 17:06:42 -0400
From: Marc Audard <audard@astro.columbia.edu>
To: "Michel G. Breitfellner" <xmmhelp@xmm.vilspa.esa.es>
Subject: Re: EPIC CTI correction for timing mode (PR#8730)
This is a multi-part message in MIME format.
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I retract my previous claim that there was a similar shift
for rev 404. The shift is only present in rev 316. I fitted
the rev 404 correctly (see attachment).

Marc

PS: Could you explain to me how there can be PATTERN>0 for
timing modes in MOS and pn?


-- 
___________________________________________________________________________

Marc Audard                           E-mail: audard@astro.columbia.edu
   Columbia Astrophysics Laboratory
   Mail code 5247                      Tel: (212) 854-8125
   550 West 120th Street               Fax: (212) 854-4648
   New York, NY 10027                  http://www.astro.columbia.edu/~audard
___________________________________________________________________________

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Reply 3

Resend
From: Michel G. Breitfellner <xmmhelp@xmm.vilspa.esa.es>
To: audard@astro.columbia.edu
Subject: Re: EPIC CTI correction for timing mode (PR#8730)
Date: Tue Jun 17 10:03:50 2003
Dear Marc,

I cannot open your attachments in our Helpdesk email
system. Can you please send your last two emails again
to my privat email account

mbreitfe@xmm.vilspa.esa.es

Many thanks and sorry for the inconvenience.

Best regards,
Michel G. Breitfellner
XMM-Newton User Support Group


Reply 4

Resend
From: Michel G. Breitfellner <xmmhelp@xmm.vilspa.esa.es>
To: audard@astro.columbia.edu
Subject: Re: EPIC CTI correction for timing mode (PR#8730)
Date: Thu Jul  3 14:18:57 2003
Dear Marc,

Please find enclosed the answer from our expert:
______________________________________________________________

The observation in Rev 316 was affected by radiation.
Have you done a flare screening like we explain in the
data analysis threads for EPIC
http://xmm.vilspa.esa.es/external/xmm_sw_cal/sas_frame.shtml


In the timing mode, imaging is made only in one dimension,
along the column (RAWX) axis.
Along the row direction (RAWY axis), data from a
predefined area on one CCD chip are collapsed into a
one-dimensional row to be read out at high speed.

The following pattern in "normal" pixels will create a double
in the macro pixels

0000001000
0100000000

----->
1
1
______________________________________________________________

Best regards,
Michel G. Breitfellner
XMM-Newton User Support Group

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