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From: Igor Antokhin <igor@astro.gla.ac.uk>
Subject: XMM PSF
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9 followups: 1 2 3 4 5 6 7 8 9

Private message: yes  no

Notes:

Notification:


Date: Mon, 5 Aug 2002 17:15:38 +0100 (BST)
From: Igor Antokhin <igor@astro.gla.ac.uk>
To: xmmhelp@xmm.vilspa.esa.es
Subject: XMM PSF
Dear Sir/Madam,

for my current XMM data analysis I need to know the encircled energy 
or PSF for MOS1, MOS2 and PN at various off-axis angles. Please note that 
it is NOT about correcting for the out-of-the-aperture contribution. I 
need to know the numbers (the fraction of the total PSF within a 
particular set of circular apertures).

The xmmsas_20020605_1701/doc/arfgen/node21.html states that "For the
common case of a circular or annular region centred on the source, a 
tabulation of enclosed energy as a function of energy, off-axis
angle and box radius is used." I'd tried to find this table in the CCF 
directory but failed. Could you please point me to this file (if 
available) or to the way I can compute the numbers I need?

Thanks,
Igor Antokhin


Reply 1

Resend
From: Michel G. Breitfellner <xmmhelp@xmm.vilspa.esa.es>
To: igor@astro.gla.ac.uk
Subject: Re: XMM PSF (PR#5635)
Date: Wed Aug  7 11:11:15 2002
Dear Dr. Antokhin,

Please see the XMM-Newton Current Calibration File Release Note

http://xmm.vilspa.esa.es/ccf/releasenotes/

XMM-CCF-REL-69   Encircled Energy Function of the X-ray telescopes   3 Apr 2001

http://xmm.vilspa.esa.es/docs/documents/CAL-SRN-0069-1-0.ps.gz

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


Followup 1

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Date: Wed, 7 Aug 2002 14:31:41 +0100 (BST)
From: Igor Antokhin <igor@astro.gla.ac.uk>
To: "Michel G. Breitfellner" <xmmhelp@xmm.vilspa.esa.es>
Subject: Re: XMM PSF (PR#5635)
  This message is in MIME format.  The first part should be readable text,
  while the remaining parts are likely unreadable without MIME-aware tools.
  Send mail to mime@docserver.cac.washington.edu for more info.

---779972051-8496021-1028727101=:1763
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Dear Michel,

thanks for your answer. Still it did not provide me with the means to 
calculate the encircled fraction of the PSF. I cannot access the CAL 
routines directly and the CAL manual (version 2.1, see the relevant 
extract from it attached to this message) does not really 
explain the algorithm of the subroutine CAL_getEncircledEnergy (which I 
hoped it would so I could reproduce it myself). In fact, it is puzzling. 
E.g, the formula for Rarcsec seems to be irrelevant as it is not explained 
how this parameter is used in the algorithm.

In the files XRT[23]_XENCIREN_0003.CCF the parameters cor1 and cor2 are 
equal to zero. Does this mean that for MOS2 and PN no correction
can be made for any off-axis angles? Even if so, I would still like to 
be able to calculate the numbers for MOS1.

Thanks,
Igor Antokhin

On Wed, 7 Aug 2002, Michel G. Breitfellner wrote:

> Dear Dr. Antokhin,
> 
> Please see the XMM-Newton Current Calibration File Release Note
> 
> http://xmm.vilspa.esa.es/ccf/releasenotes/
> 
> XMM-CCF-REL-69   Encircled Energy Function of the X-ray telescopes   3 Apr
2001
> 
> http://xmm.vilspa.esa.es/docs/documents/CAL-SRN-0069-1-0.ps.gz
> 
> With best regards,
> Michel G. Breitfellner
> XMM-Newton User Support Group
> 
> 

--------------------------------------------
Igor Antokhin
Astronomy and Astrophysics Group
University of Glasgow
Kelvin Building, G12 8QQ
Glasgow, UK
E-mail: igor@astro.gla.ac.uk

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Reply 2

Resend
From: Michel G. Breitfellner <xmmhelp@xmm.vilspa.esa.es>
To: igor@astro.gla.ac.uk
Subject: Re: XMM PSF (PR#5635)
Date: Wed Aug  7 16:07:48 2002
Dear Dr. Antokhin,

Your question was forwarded to our PSF specialist. We will inform you 
as soon as possible.

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


Reply 3

Resend
From: Michel G. Breitfellner <xmmhelp@xmm.vilspa.esa.es>
To: igor@astro.gla.ac.uk
Subject: Re: XMM PSF (PR#5635)
Date: Mon Aug 12 12:47:18 2002
Dear Igor,

Please find enclosed the answer of our specialist.

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

--------------------------------------------

Dear Igor,

   the latest formulation of the encircled energy is contained in the
CCF files XRT1_XPSF_0005.CCF, XRT2_XPSF_0005.CCF and XRT3_XPSF_0004.CCF
for the MOS-1, MOS-2 and PN cameras respectively.
In these files you will find an extension called KING_PARAMS.
This contains the columns

   4  BINTABLE KING_PARAMS     8     16(3) 80                    0    1

      Column Name                Format     Dims       Units     TLMIN
      1 ENERGY                     E                   eV
      2 THETA                      E                   rad
      3 PARAMS                     2E

Where the PARAMS column contains the King function parameters
core radius (in arcseconds) and index (alpha). These parameters,
tabulated against photon energy and off-axis angle (THETA in radians)
can be converted to an encircled energy fraction using the formula
given in the attached postscript file.
In the SAS we interpolate in energy and theta using a spline but this
isn't critical and a linear interpolation should be adequate.

I hope this helps,

Richard
------------------------------------


Followup 2

Compose reply
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Date: Mon, 12 Aug 2002 14:10:04 +0100 (BST)
From: Igor Antokhin <igor@astro.gla.ac.uk>
To: "Michel G. Breitfellner" <xmmhelp@xmm.vilspa.esa.es>
Subject: Re: XMM PSF (PR#5635)
On Mon, 12 Aug 2002, Michel G. Breitfellner wrote:

> Dear Igor,
> 
> Please find enclosed the answer of our specialist.
...

> ... These parameters,
> tabulated against photon energy and off-axis angle (THETA in radians)
> can be converted to an encircled energy fraction using the formula
> given in the attached postscript file.

Thanks for the answer. Could you please send me the ps file which was NOT 
attached to your original message?

Thanks again,
Igor Antokhin



Followup 3

Compose reply
Download message
Date: Mon, 12 Aug 2002 16:33:43 +0200
From: "Michel G. Breitfellner" <mbreitfe@xmm.vilspa.esa.es>
To: igor@astro.gla.ac.uk
CC: xmmhelp@xmm.vilspa.esa.es
Subject: XMM Helpdesk request 5635: XMM PSF (PR#5635)
This is a multi-part message in MIME format.
--------------2E618022144926D997C8FD0C
Content-Type: text/plain; charset=us-ascii
Content-Transfer-Encoding: 7bit

Dear Igor,

Sorry, I forgot that our helpdesk system has difficulties handling
attachments. Therefore I send you the file from my personal email
account.

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

--------------------------------------------
Dear Igor,

   the latest formulation of the encircled energy is contained in the
CCF files XRT1_XPSF_0005.CCF, XRT2_XPSF_0005.CCF and XRT3_XPSF_0004.CCF
for the MOS-1, MOS-2 and PN cameras respectively.
In these files you will find an extension called KING_PARAMS.
This contains the columns

   4  BINTABLE KING_PARAMS     8     16(3) 80                    0    1

      Column Name                Format     Dims       Units     TLMIN
      1 ENERGY                     E                   eV
      2 THETA                      E                   rad
      3 PARAMS                     2E

Where the PARAMS column contains the King function parameters
core radius (in arcseconds) and index (alpha). These parameters,
tabulated against photon energy and off-axis angle (THETA in radians)
can be converted to an encircled energy fraction using the formula
given in the attached postscript file.
In the SAS we interpolate in energy and theta using a spline but this
isn't critical and a linear interpolation should be adequate.

I hope this helps,

Richard
------------------------------------
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Followup 4

Compose reply
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Date: Tue, 13 Aug 2002 18:09:11 +0100 (BST)
From: Igor Antokhin <igor@astro.gla.ac.uk>
To: "Michel G. Breitfellner" <mbreitfe@xmm.vilspa.esa.es>
cc: xmmhelp@xmm.vilspa.esa.es
Subject: Re: XMM Helpdesk request 5635: XMM PSF (PR#5635)
Dear Michel,

thanks for your response. Could you please clarify a couple of points so 
that I will not make any mistakes using the info you provided earlier?

1.In your message and in the postscipt description you say that the 
function used is the King function. In XRT1_XPSF_0005.CCF, the extention 
containing the parameters ENERGY, THETA and PARAMS is called 
GLE_GAUSS_PARAM (I could not find the KING_PARAMS extension). Is it still 
ok to use the formula provided in your postscript document (which I 
honestly doubt)? 

2.The size of PARAMS is 6E, not 2E so there are 6 parameters for every 
offset angle and energy, not just r_c and alpha. What is their meaning and 
how can I use them?

3.How about the XRT[23]_XENCIREN_0003.CCF files? I has been told before 
that it is these files which are being used to correct for the fraction of 
the PSF outside of one's aperture. Still, cor1 and cor2 from those files 
are equal to 0 for MOS2 anf PN. This is not directly related to my current 
question but I would like to know whether my psf is being corrected if I 
use e.g. a 30arcsec aperture within 5arcmin from the center of the FOV and 
use appropriate task switches to make the correction.

Thanks again,
Igor Antokhin
 
On Mon, 12 Aug 2002, Michel G. Breitfellner wrote:

> Dear Igor,
> 
> Sorry, I forgot that our helpdesk system has difficulties handling
> attachments. Therefore I send you the file from my personal email
> account.
> 
> Best regards,
> Michel G. Breitfellner
> XMM-Newton User Support Group
> 
> --------------------------------------------
> Dear Igor,
> 
>    the latest formulation of the encircled energy is contained in the
> CCF files XRT1_XPSF_0005.CCF, XRT2_XPSF_0005.CCF and XRT3_XPSF_0004.CCF
> for the MOS-1, MOS-2 and PN cameras respectively.
> In these files you will find an extension called KING_PARAMS.
> This contains the columns
> 
>    4  BINTABLE KING_PARAMS     8     16(3) 80                    0    1
> 
>       Column Name                Format     Dims       Units     TLMIN
>       1 ENERGY                     E                   eV
>       2 THETA                      E                   rad
>       3 PARAMS                     2E
> 
> Where the PARAMS column contains the King function parameters
> core radius (in arcseconds) and index (alpha). These parameters,
> tabulated against photon energy and off-axis angle (THETA in radians)
> can be converted to an encircled energy fraction using the formula
> given in the attached postscript file.
> In the SAS we interpolate in energy and theta using a spline but this
> isn't critical and a linear interpolation should be adequate.
> 
> I hope this helps,
> 
> Richard
> ------------------------------------

--------------------------------------------
Igor Antokhin
Astronomy and Astrophysics Group
University of Glasgow
Kelvin Building, G12 8QQ
Glasgow, UK
E-mail: igor@astro.gla.ac.uk



Reply 4

Resend
From: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
To: igor@astro.gla.ac.uk
Subject: Re: XMM PSF (PR#5635)
Date: Wed Aug 14 07:17:34 2002
Dear Igor,

(Michel is on leave for 4 weeks now but I hope that me too, I can help you
a bit with your questions on the PSF...)

you wrote:
> 1.In your message and in the postscipt description you say that the 
> function used is the King function. In XRT1_XPSF_0005.CCF, the extention 
> containing the parameters ENERGY, THETA and PARAMS is called 
> GLE_GAUSS_PARAM (I could not find the KING_PARAMS extension). Is it still 
> ok to use the formula provided in your postscript document (which I 
> honestly doubt)? 

hmmm, I just had a look at the XRT1_XPSF_0005.CCF file myself and I see
the extension called KING_PARAMS (and no GLE_GAUSS_PARAM extension)!
Please make sure you are looking at the correct file - you can download it from
ftp://xmm.vilspa.esa.es/pub/ccf/constituents

> 2.The size of PARAMS is 6E, not 2E so there are 6 parameters for every 
> offset angle and energy, not just r_c and alpha. What is their meaning and

> how can I use them?

in the correct XRT1_XPSF_0005.CCF file, the size is 2E in fact

> 3.How about the XRT[23]_XENCIREN_0003.CCF files? I has been told before 
> that it is these files which are being used to correct for the fraction of

> the PSF outside of one's aperture. Still, cor1 and cor2 from those files 
> are equal to 0 for MOS2 anf PN. This is not directly related to my current

> question but I would like to know whether my psf is being corrected if I 
> use e.g. a 30arcsec aperture within 5arcmin from the center of the FOV and

> use appropriate task switches to make the correction.

Please, have a look at the CCF release notes available at
http://xmm.vilspa.esa.es/ccf/releasenotes/ccfindex.html 
There you should find a reasonable description of what the different CCFs
are and gow they are related.

Please, let me know if still some info is needed here - in that case I will 
need to contact our CCF specialists.

Cheers,
Matthias.

Matthias Ehle 
XMM-Newton SOC 
User Support Group


Followup 5

Compose reply
Download message
Date: Wed, 14 Aug 2002 15:56:30 +0100 (BST)
From: Igor Antokhin <igor@astro.gla.ac.uk>
To: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
Subject: Re: XMM PSF (PR#5635)
On Wed, 14 Aug 2002, Matthias Ehle wrote:

> Dear Igor,
> 
> (Michel is on leave for 4 weeks now but I hope that me too, I can help you
> a bit with your questions on the PSF...)
> 
> you wrote:
> > 1.In your message and in the postscipt description you say that the 
> > function used is the King function. In XRT1_XPSF_0005.CCF, the
extention 
> > containing the parameters ENERGY, THETA and PARAMS is called 
> > GLE_GAUSS_PARAM (I could not find the KING_PARAMS extension). Is it
still 
> > ok to use the formula provided in your postscript document (which I 
> > honestly doubt)? 
> 
> hmmm, I just had a look at the XRT1_XPSF_0005.CCF file myself and I see
> the extension called KING_PARAMS (and no GLE_GAUSS_PARAM extension)!
> Please make sure you are looking at the correct file - you can download it
from
> ftp://xmm.vilspa.esa.es/pub/ccf/constituents

Hi Matthias,

I have just downloaded the file you had mentined. Attached is the main 
screen as seen by the "fv program" (XRT1_XPSF_0005_CCF_1.gif). No 
"KING_PARAMS" extention. The "GLE_GAUSS_PARAM" extention is shown in  
XRT1_XPSF_0005_CCF_1.gif from which it is seen that PARAMS have 6 
elements. I am lost. Do I look into the wrong place? Thank you for your 
help.

Igor Antokhin



Followup 6

Compose reply
Download message
Date: Fri, 16 Aug 2002 11:16:01 +0100 (BST)
From: Igor Antokhin <igor@astro.gla.ac.uk>
To: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
Subject: Re: XMM PSF (PR#5635)
  This message is in MIME format.  The first part should be readable text,
  while the remaining parts are likely unreadable without MIME-aware tools.
  Send mail to mime@docserver.cac.washington.edu for more info.

---779972051-132576782-1029492961=:6873
Content-Type: TEXT/PLAIN; charset=US-ASCII

Sorry Matthias, I forgot to attach the plots to my last message.

Best,
Igor


> On Wed, 14 Aug 2002, Matthias Ehle wrote:
> 
> > Dear Igor,
> > 
> > (Michel is on leave for 4 weeks now but I hope that me too, I can help
you
> > a bit with your questions on the PSF...)
> > 
> > you wrote:
> > > 1.In your message and in the postscipt description you say that
the 
> > > function used is the King function. In XRT1_XPSF_0005.CCF, the
extention 
> > > containing the parameters ENERGY, THETA and PARAMS is called 
> > > GLE_GAUSS_PARAM (I could not find the KING_PARAMS extension). Is
it still 
> > > ok to use the formula provided in your postscript document (which
I 
> > > honestly doubt)? 
> > 
> > hmmm, I just had a look at the XRT1_XPSF_0005.CCF file myself and I
see
> > the extension called KING_PARAMS (and no GLE_GAUSS_PARAM extension)!
> > Please make sure you are looking at the correct file - you can
download it from
> > ftp://xmm.vilspa.esa.es/pub/ccf/constituents
> 
> Hi Matthias,
> 
> I have just downloaded the file you had mentined. Attached is the main 
> screen as seen by the "fv program" (XRT1_XPSF_0005_CCF_1.gif). No 
> "KING_PARAMS" extention. The "GLE_GAUSS_PARAM" extention is shown in  
> XRT1_XPSF_0005_CCF_1.gif from which it is seen that PARAMS have 6 
> elements. I am lost. Do I look into the wrong place? Thank you for your 
> help.
> 
> Igor Antokhin

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Reply 5

Resend
From: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
To: igor@astro.gla.ac.uk
Subject: Re: XMM PSF (PR#5635)
Date: Fri Aug 16 10:46:00 2002
Dear Igor,

OK. now I see what's happening:

There are much more file extensions in XRT1_XPSF_0005.CCF then you show
in your plot! You need to use the scroll bar on the right hand side of fv
to display the other extension (in total there are 71).
Extension 70 is the one called KING_PARAMS.

BTW, the fv window sometimes does not display the complete extension names:
GLE_GAUSS_PARAM is indeed an extension called SINGLE_GAUSS_PARAMS
(you see the complete name if you display the extension header with fv,
the name is given in the EXTNAME keyword)

I am glad that we could solve this 'mystery'.

Cheers,
Matthias,


Followup 7

Compose reply
Download message
Date: Fri, 16 Aug 2002 11:57:45 +0100 (BST)
From: Igor Antokhin <igor@astro.gla.ac.uk>
To: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
Subject: Re: XMM PSF (PR#5635)
Dear Matthias,
thanks for your reply. Stupid of me to not check the rest of the list. It 
is because after a few first extenstions everything else seemed 
to be the PSF image examples so I thought they would just go till the end 
of the list. Stupid of me.

Thanks a lot,
Igor

On Fri, 16 Aug 2002, Matthias Ehle wrote:

> Dear Igor,
> 
> OK. now I see what's happening:
> 
> There are much more file extensions in XRT1_XPSF_0005.CCF then you show
> in your plot! You need to use the scroll bar on the right hand side of fv
> to display the other extension (in total there are 71).
> Extension 70 is the one called KING_PARAMS.
> 
> BTW, the fv window sometimes does not display the complete extension names:
> GLE_GAUSS_PARAM is indeed an extension called SINGLE_GAUSS_PARAMS
> (you see the complete name if you display the extension header with fv,
> the name is given in the EXTNAME keyword)
> 
> I am glad that we could solve this 'mystery'.
> 
> Cheers,
> Matthias,
> 

--------------------------------------------
Igor Antokhin
Astronomy and Astrophysics Group
University of Glasgow
Kelvin Building, G12 8QQ
Glasgow, UK
E-mail: igor@astro.gla.ac.uk



Followup 8

Compose reply
Download message
Date: Thu, 22 Aug 2002 11:03:59 +0100 (BST)
From: Igor Antokhin <igor@astro.gla.ac.uk>
To: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
Subject: Re: XMM PSF (PR#5635)
Dear Matthias,

I have successfully used the info on the encircled PSF energy you 
provided. Thanks. Just one more question: the King's formula from 
XMM-PS-GM-20 (2.2), p.16, has 5arcmin term in the divisor. It looks like I 
can use this formula up to 5arcmin off-axis angles only. I recall reading 
somewhere that XMM PSF is defined within this distance from the center of 
the FOV. Yet the CCFs (XRT1_XPSF_0005.CCF and others) provide the 
interpolated r_c and alpha up to ~15arcmin. Does this mean that I could 
use the King's formula beyond 5arcmin? One of my apertures is 
7armin off-axis.

Thank you for your help,
Igor

--------------------------------------------
Igor Antokhin
Astronomy and Astrophysics Group
University of Glasgow
Kelvin Building, G12 8QQ
Glasgow, UK
E-mail: igor@astro.gla.ac.uk



Reply 6

Resend
From: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
To: igor@astro.gla.ac.uk
Subject: Re: XMM PSF (PR#5635)
Date: Thu Aug 22 10:47:16 2002
Dear Igor,

I have forwarded your question to our XRT experts and will let you know
their reply asap. Please note, however, that due to the vacation season, 
I am not sure if I can get a quick answer...

Cheers,
Matthias.


Reply 7

Resend
From: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
To: igor@astro.gla.ac.uk
Subject: Re: XMM PSF (PR#5635)
Date: Tue Aug 27 15:42:54 2002
Dear Igor,

please find attached now the expert's reply to your question:

The cited formula including the 5arcmin term, is for the EEF. 5arcmin is not
the
off-axis angle of the source, but a normalization radius.

The EEF provides the enrcicled energy fraction enclosed within a radius
R. We decided to normalize it at 5 arcmin. In practise, we assume that all the 
energy of the source is enclosed within a radius of 5 arcmin from the source 
center (whatever its off-axis position is), or in other words, the EEF evaluates

the fraction of the energy within a radius of 5 arcmin.

This is an approximation, and a discussion on this point can be found in
the report XMM-SOC-CAL-TN-0022 (at the XMM vilspa page).

Hence, the formula can be used for any off-axis position of the source.
However, let me recall that the data allowed a good calibration only for 
low off-axis angles (say < about 4 arcmin). For larger off-axis angles only
low
energies are well calibrated (see the report for the "range of
application" of the PSF/EEF model)


I hope this info will help you with your further analysis.

Cheers,
Matthias.


Followup 9

Compose reply
Download message
Date: Wed, 28 Aug 2002 11:32:24 +0100 (BST)
From: Igor Antokhin <igor@astro.gla.ac.uk>
To: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
Subject: Re: XMM PSF (PR#5635)
Dear Matthias,

thanks for your reply which was very useful. Still, while answering 
my query, it raised other question... Could you please ask your 
expert to answer just one question regarding my particular case?

I have 4 XMM observations of a source (a WR star), in 2 of them (rev 
284,285) it is located in the center of the FOV, in two others (rev 
115,116) - 7arcmin off-axis. I understand that the 5arcmin term in 
the EEF formula is not an off-axis angle but a normalization radius. 
5armin appeared in my message, because I saw this value as the off-axis 
limit (where PSF was still defined), in some documentation. I actually 
just checked the latest release notes and learned that currently the EEF 
is at least 5% accurate at energies below 4.5keV within the central 
10armin.

Now, what I see is that the EPIC flux of my source at the 7armin 
off-axis position is about 15% HIGHER that the flux in the on-axis 
position, the difference is the same in two energy bands 0.5-2.4keV and 
2.4-10.0keV. In both cases, I used the extraction aperture R=1armin and 
did NOT correct the extracted spectra for the EEF. According to the 
XRT PSF CCF, the difference between the fluxes due to this correction 
would be less that 1 per cent. I computed the fluxes in xspec, 
accounting for the rmf and arf matrixes. I understand that at 
least for the soft band the difference exceeds possible EEF errors. 
However, you also mentioned that "...the data allowed a good 
calibration only for low off-axis angles (say < about 4 arcmin). For 
larger off-axis angles only low energies are well calibrated (see the 
report for the "range of application" of the PSF/EEF model)". So the 
question is: did you mean the above 4.5keV limit? Are there any other 
calibration uncertainties (maybe apart from the PSF/EEF issue) which 
could account for the 15% difference of fluxes? I would like to know 
whether the difference can be considered as real variations or not...

Thanks for your help,
Igor Antokhin

On Tue, 27 Aug 2002, Matthias Ehle wrote:

> Dear Igor,
> 
> please find attached now the expert's reply to your question:
> 
> The cited formula including the 5arcmin term, is for the EEF. 5arcmin is
not
> the off-axis angle of the source, but a normalization radius.
... 
> Hence, the formula can be used for any off-axis position of the source.
> However, let me recall that the data allowed a good calibration only for 
> low off-axis angles (say < about 4 arcmin). For larger off-axis angles
only low
> energies are well calibrated (see the report for the "range of
> application" of the PSF/EEF model)
... 
> Cheers,
> Matthias.



Reply 8

Resend
From: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
To: igor@astro.gla.ac.uk
Subject: Re: XMM PSF (PR#5635)
Date: Fri Sep 20 08:43:27 2002
Dear Igor,

sorry for my late reply on your PSF followup question.
Somehow the system failed informing me that there was a new question raised 
by you.

I have forwarded your report to our experts and will let you know their reply 
asap.

Cheers and sorry again for the 'hickup' in our helpdesk system.

Cheers,
Matthias.


Reply 9

Resend
From: Matthias Ehle <xmmhelp@xmm.vilspa.esa.es>
To: igor@astro.gla.ac.uk
Subject: Re: XMM PSF (PR#5635)
Date: Tue Sep 24 08:33:15 2002
Dear Igor,

please, find below an answer from our calibration experts on the
subject of flux differences between on- and off-axis source position:

you wrote:
> Are there any other
> calibration uncertainties (maybe apart from the PSF/EEF issue) which
> could account for the 15% difference of fluxes? I would like to know
> whether the difference can be considered as real variations or not...

This is almost certainly due to a calibration error in the vignetting.
An uncertainty in the position of the optical-axis used within the SAS is 
currently giving an error, which we estimate to be about

MOS-1  3%
MOS-2  10%
PN     8%

at 7 arcmins off-axis for an energy of 4.5 keV.

There is a small energy dependence on the above values with lower energies
being affected less. At the moment you should use these numbers
as a systematic error on the 7' off-axis fluxes. There is also a 2-4%
error introduced by the same effect on the on-axis measurements.
We are actively working on this problem and have just taken a set of
calibration measurements which should resolve the issue within the next
1-2 months.

This may not be enough to solve the full 15% difference that you see
and after the vignetting correction becomes available we may need to
revisit other sources of potential error to investigate the remaining
5% discrepancy.

It is very unlikely that uncertainties in the PSF are causing more
than 1% of this particular problem for such a large extraction radius.

Best regards,

Matthias.

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