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XMM­Newton
Routine Calibration Plan
Version 2.9
Edited by: M.G.F. Kirsch
10.01.2008
Revision history
Revision number Date Revision author Comments
Version 2.9 10.01.2008 M. Kirsch Update: EPIC closed
Version 2.8 20.11.2007 M. Kirsch Update: OM f.fields/dark frames, EPIC calclosed
Version 2.7 10.11.2006 M. Ehle Update: New RGS target & logs
Version 2.6 15.06.2006 M. Ehle Update: RGS calibration, plans & logs
Version 2.5 06.07.2005 M. Ehle Update: RGS targets & strategy
Version 2.4 04.05.2005 M. Ehle Update: OM sections
Version 2.3 20.04.2005 M. Ehle Update: full text & logs; drop of visibility annex
Version 2.2 27.01.2003 M. Ehle Update: skeleton plans & log of perf. obs.
Version 2.1 01.02.2002 M. Ehle Several updates & extension up to rev. 760
Version 2.0 22.05.2001 M. Ehle Several updates & extension up to rev. 600
Version 1.0 15.03.2001 M. Ehle Includes several target updates
Draft 0.2 24.07.2000 M. Ehle Includes comments from calibration scientists
Draft 0.1 12.07.2000 M. Ehle First Draft
i

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Contents
1 Purpose and Scope 1
2 XMM­Newton Routine Calibration Program 1
2.1 List of Targets and Calibration Budget . . . . . . . . . . . . . . . . . . . . . . . . 1
2.1.1 EPIC Routine Calibration Monitoring . . . . . . . . . . . . . . . . . . . . 2
2.1.1.1 CTI, Gain, Noise and Bright Pixel Monitoring . . . . . . . . . . 2
2.1.1.2 E#ective Area, Gain/O#set Monitoring . . . . . . . . . . . . . . 3
2.1.1.3 Stability of the Boresight . . . . . . . . . . . . . . . . . . . . . . 3
2.1.1.4 Monitoring of Spectral Capabilities and Contamination . . . . . 3
2.1.1.5 Detector Response and Redistribution Monitoring . . . . . . . . 4
2.1.1.6 Monitoring of Relative and Absolute Timing Capabilities . . . . 4
2.1.2 RGS Routine Calibration Monitoring . . . . . . . . . . . . . . . . . . . . . 4
2.1.2.1 Confirmation of the Wavelength Scale . . . . . . . . . . . . . . . 4
2.1.2.2 Long­wavelength Calibration . . . . . . . . . . . . . . . . . . . . 4
2.1.2.3 Monitoring of E#ective Area . . . . . . . . . . . . . . . . . . . . 4
2.1.2.4 Gain and CTI Monitoring . . . . . . . . . . . . . . . . . . . . . . 5
2.1.3 OM Routine Calibration Monitoring . . . . . . . . . . . . . . . . . . . . . 5
2.1.3.1 Monitoring the Grisms Absolute Flux Calibration . . . . . . . . 5
2.1.3.2 Monitoring of the Visual and UV Grisms Wavelength Calibration 5
2.1.3.3 Monitoring the Photometric Calibration . . . . . . . . . . . . . . 5
2.1.3.4 Engineering Mode Observations . . . . . . . . . . . . . . . . . . 5
2.1.3.5 Flat fields and dark frames . . . . . . . . . . . . . . . . . . . . . 6
2.1.4 XMM­Newton Cross Calibration . . . . . . . . . . . . . . . . . . . . . . . 6
2.1.5 XMM­Newton Long­Wavelength Response . . . . . . . . . . . . . . . . . . 7
3 Annexes 7
3.1 Term Planning Skeleton . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7
3.1.1 Planning skeleton for remaining part of year 2000 . . . . . . . . . . . . . . 8
3.1.2 Routine calibration plan for Jan ­ Mar 2001 . . . . . . . . . . . . . . . . . 8
3.1.3 Routine calibration plan for Apr ­ Jun 2001 . . . . . . . . . . . . . . . . . 8
3.1.4 Routine calibration plan for Jul ­ Dec 2001 . . . . . . . . . . . . . . . . . 9
3.1.5 Routine calibration plan for Feb ­ Jun 2002 . . . . . . . . . . . . . . . . . 9
3.1.6 Routine calibration plan for Jul ­ Dec 2002 . . . . . . . . . . . . . . . . . 10
3.2 Performed calibration observations . . . . . . . . . . . . . . . . . . . . . . . . . . 11

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1 Purpose and Scope
This document describes the global planning strategy for XMM­Newton calibration observations
in the routine phase of the project.
2 XMM­Newton Routine Calibration Program
It has been agreed with the calibration scientists and instrument teams of XMM­Newton that the
targets listed in Sect. 2.1 will be used for regular routine calibration observations. These targets
are flagged as sources reserved for calibration observations and included in the XMM­Newton
Observation Lokator (http://xmm.esac.esa.int/external/xmm sched/obs lokator/index.php).
2.1 List of Targets and Calibration Budget
Figure 1 lists possible calibration targets that should be monitored at a regular time scale and the
needed calibration time budget for that. Note that some targets that were originally part of the
routine calibration monitoring have been dropped in the meantime and replaced by other/better
targets. Some of these former targets (for example OMC2/3, MS1229.2+6430, H1426+428 or
Sco X­1) might be re­visited on request and as non­routine calibration observations.
Target obs/year time/obs time slews overhead Purpose
CLOSED 12 10 120 0 12 quiescent particle BG monitoring
1E0102­72 2 30 60 2 2 EPIC eff. Area, gain , offset
N132D 1 30 30 1 1 EPIC eff. Area, gain , offset
Vela SNR 1 60 60 1 1 EPIC spectral cap. & contamination
Tycho SNR 1 30 30 1 1 EPIC spectral cap. & contamination
Crab 2 15 30 6 6 EPIC relative and absolute timing
AB Dor 1 50 50 1 1 RGS wavelength scale
PSR B0833­45 1 100 100 1 1 RGS long­wavelength scale
Mkn 421 2 60 120 4 10 RGS effective area/ CTI
Mkn 421 offset 0.5 20 10 0.5 0.5 RGS effective area/ CTI
GD153 1 15 15 1 0
HZ2 1 15 15 1 0
HD 13499 1 15 15 1 0 OM visual & UV grisms wavelength scale
BPM 16274 2 15 30 2 0 OM phorometric calibration
SA95­42 1 35 35 1 0 OM phorometric calibration
PKS2155­304 1 60 60 1 1 Cross Calibration
Cross Calibration
Cross Calibration
zeta Puppis 1 60 60 1 1 low energy cross response
RXJ1856.6­3754 2 70 140 2 2 cross response monitoring
SUM obs/year time slews over ead all [ks]
EPIC 19 330 11 23 438.1 1.83 1.62
RGS 4.5 280 6.5 12.5 316.15 1.32 1.20
OM 6 110 6 0 137.6 0.58 0.46
Cross cal 5 320 5 5 355.5 1.49 1.39
SUM ALL 1247.35 5.22 4.67
Available scince time 182.5 rev * 131 ks 23907.50
OM grisms absolute flux
OM visual grism wavelength scale
1 60 60 1 1
Capella or
3C273
all [%]
all [%]
wit out
slew
Figure 1: List of calibration targets and the time budget spend. Note that the used overheads
are 2.5 ks (EPIC) and 0.5 ks (RGS). Quoted times for OM include operational overheads. A
slew has been assumed as 4.6 ks.
Note that, as several routine calibration observations in the plan are marked as `to be scheduled
on request' and as non­routine calibration observations might be necessary, the time actually
spent on calibration might be higher. The routine calibration planning skeletons (see Section
3.1) are always aiming at keeping the time for routine calibrations below the 5% margin (cf
XMM­Newton Policies and Procedures document) to allow for additional NRCOs.

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2.1.1 EPIC Routine Calibration Monitoring
It is assumed, unless otherwise stated, that both RGS will operate in the standard spectroscopy
mode with all CCDs read during the EPIC calibration observations.
2.1.1.1 CTI, Gain, Noise and Bright Pixel Monitoring
Routine closed/calclosed observations of short duration (from 1 to 3 hours) are scheduled for
MOS and pn (pn only if available time # 6 ks) at the start and end of each revolution. The
pointing direction is irrelevant, but it is advantageous to schedule the closed/calclosed exposures
at the start or end of a revolution with the same position as the adjacent science observations
to avoid one extra slew. With this setup it is possible to extend closed/calclosed observations
up to the time when the radiation is low enough to start full science observations.
In the past, longer (at least 15 ks) closed/calclosed observations for MOS and pn were performed
every two weeks to one month. Such exposures were scheduled as far as possible parasitically with
RGS and OM routine calibration observations. If gaps between such calibration observations
were too large, dedicated closed/calclosed observations had to be requested.
Due to the decreasing flux of the EPIC internal calibration source, longer calclosed exposures
are needed to obtain high enough statistics for the gain and CTI monitoring.
In April 2005 it has been confirmed that MOS full frame calclosed data collected during slews
between adjacent targets can be used for CTI and gain monitoring. For pn, the new request
is that instead of several rather frequent 15 ks observations only long observations should be
scheduled parasitically to RGS and OM prime calibration observations. No additional dedicated
closed/calclosed routine calibration observations are requested. The frequency of calclosed ob­
servations hence has been reduced to one observation approximately every 2 ­ 3 months.
The distribution of specific EPIC calclosed exposure times between di#erent readout modes and
filter combinations should roughly be
. for pn:
calclosed full­frame : calclosed extended full­frame = 3 : 1
. for MOS:
alwawys calclosed full­frame
Additionaly monthly Closed exposures of 10 ks are needed to track the state of variations in the
quiescent particle background.
. for pn:
closed full­frame
. for MOS:
closed full­frame
Diagnostics and Noise mode exposures:
MOS diagnostic images should be taken twice per year parasitically to OM routine calibration
observations for 10 ­ 15 ks. The filter and readout modes are:
. scheme 1 (# 15 ks): all CCDs Full Frame, 3 exposures per CCD

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. scheme 2 (# 7+7 ks):
10 exposures Small Window CCD1 + 1 exposure Full Frame all peripheral CCDs
5 exposures Large Window CCD1 + 1 exposure Full Frame all peripheral CCDs
Pn should be scheduled twice per year in full­frame noise mode, possibly in parallel with the
MOS diagnostic mode observations (details are defined in the half year skeleton plans).
Time budget: 120 ks + overheads for the CLOSED for quiescent particle background monitor­
ing. The rest of the observations are performed during slews and calibration observations where
EPIC is not prime, so there is no impact on the time available for science.
2.1.1.2 E#ective Area, Gain/O#set Monitoring
The two targets for the EPIC e#ective area and gain/o#set monitoring are the SNRs 1ES0102­72
and N132D in the Magellanic Clouds.
1ES0102­72 should be scheduled twice per year for 30 ks each: once at a position o#set from
the MOS patch, once on the patch position. MOS cameras will be in large­window mode with
the thin filter in place, pn in small­window mode alternating between thin and medium filter
exposures.
N132D should be scheduled with thin filter, pn in small­window and MOSs in large­window
mode once per year for 30 ks.
For both these SNRs the pointing coordinates might need to be adjusted (depending on the
position angle) to re­center the slightly extended sources in the pn small­window field of view.
The observations of 1ES0102­72, in particular, and N132D are also of importance to RGS for
monitoring purposes provided the pointing direction is properly constrained.
Note that for the SNRs listed above (and in § 2.1.1.4 below), the same spacecraft position angle
should be kept for repeating observations (i.e. they should always be observed at roughly the
same time of the year).
2.1.1.3 Stability of the Boresight
In the past a test to check the stability of the boresight was scheduled once after every eclipse
seasons and once per year after two years of XMM­Newton operations with targets NGC 2516
or OMC2/3. This has been dropped from the routine calibration plan and should be requested
(if needed) as a non routine calibration observation (NRCO).
2.1.1.4 Monitoring of Spectral Capabilities and Contamination
The best suited target in the past for the check of spectral capabilities seemed to be MS1229.2+6430
which was planned to be scheduled on request. Otherwise, the XMM­Newton cross­calibration
target 3C 273 was used.
The pn team has proposed as replacement target Vela SNR to routinely monitor the low energy
part across the face of the detector. This target should be scheduled once per year for 60 ks
with EPIC cameras in full­frame mode and the thin filter in place.
In addition, the Tycho SNR should also be monitored once per year for 30 ks with EPIC cameras
in full­frame mode and the medium filter in place.

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Note that for the SNRs listed here (and in § 2.1.1.2 above), the same spacecraft position angle
should be kept for repeating observations (i.e. they should always be observed at roughly the
same time of the year).
2.1.1.5 Detector Response and Redistribution Monitoring
To monitor the EPIC energy redistribution, the isolated neutron star RXJ1856.6­3754 should
be observed twice per year with small­window thin filter exposures. As also RGS is using this
target for monitoring purposes, the observing time was increased to 70 ks and will be counted
half and half for EPIC and RGS, respectively.
The routine calibration target zeta Puppis (§ 2.1.5), will also be used for this monitoring task.
2.1.1.6 Monitoring of Relative and Absolute Timing Capabilities
The Crab pulsar should be scheduled twice per year for 15 ks each to monitor the EPIC timing
capabilities. Both of the 15 ks total time visits should be split into three 5 ks pointings: pn in
burst, timing and another burst mode observation with the thick filter in place. Ideally, these
three pointings should be scheduled at di#erent phases of a single orbit to cover di#erent time
delays and ground station data links.
For RGS the the following setting is used
. RGS 1: 1 exposure CCDs: ­ ­ 3 4 5 ­ ­ ­ ­
. RGS 2: 1 exposure CCDs: ­ ­ 3 ­ 5 6 ­ ­ ­
2.1.2 RGS Routine Calibration Monitoring
It is assumed, unless otherwise stated, that during the RGS calibration observations all EPICs
will operate the first 10 ks with filters followed by calclosed/closed observations (details are
defined in the half year skeleton plans).
2.1.2.1 Confirmation of the Wavelength Scale
This should regularly be checked by routine observations of AB Dor. (Long EPIC closed/calclosed
exposures (see § 2.1.1.1) will be performed in parallel). The XMM­Newton cross calibration tar­
get Capella (see § 2.1.4) originally was also listed here and still is used for this RGS monitoring
task.
AB Dor is always visible and should be scheduled once per year for 50 ks.
2.1.2.2 Long­wavelength Calibration
A single annual 100 ks observation of PSR B0833­45 should be executed to monitor the RGS
long­wavelength calibration.
2.1.2.3 Monitoring of E#ective Area
The e#ective area should be monitored by two 60 ks observations of Mkn 421 per year. These
Mkn 421 observations should be executed varying the pointing direction in steps along the
dispersion axis in order to mitigate the e#ects of bad pixels and other instrumental features.
The steps are: ­30'', ­15'', 0'', +10'', +20''

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The XMM­Newton cross­calibration targets PKS2155­304 and 3C 273 (see § 2.1.4) can also help
in this monitoring task: Based on present analysis, PKS2155­304 is the better suited target
and should be observed once per year in the framework of the XMM­Newton cross­calibration
activities. PKS2155­304 is much more stable than 3C 273 which is known to be variable, both
in intensity and spectral shape.
2.1.2.4 Gain and CTI Monitoring
For CTI purposes, Mkn 421 should be observed once every two years for 20 ks at large cross­
dispersion o#sets.
Sco X­1 (one CCD at a time to cope with high telemetry rate) should be observed only if required
(on­axis, 2 ks per CCD) e.g. after major solar flares. When necessary, specific observations on
Sco X­1 with o#­axis pointing positions in the cross­dispersion will be requested.
Sco X­1 only if requested & to be handled as NRCO.
2.1.3 OM Routine Calibration Monitoring
Quoted times for OM include operational overheads.
It is assumed, unless otherwise stated, that all EPICs will operate in calclosed/closed (details are
defined in the half year skeleton plans) and both RGS will operate in the standard spectroscopy
mode with all CCDs read during the OM calibration observations. Note that if OM is operated
in high BG condition the RGS should not take data.
2.1.3.1 Monitoring the Grisms Absolute Flux Calibration
Once per year the two spectrophotometric standard targets GD153 and HZ2 should be scheduled
for 15 ks each. The observation of HZ2 is also used to monitor the wavelength scale of the visible
grism. Since the observations are performed with all filters and grisms, they are also used for
photometric performance monitoring of the filters.
2.1.3.2 Monitoring of the Visual and UV Grisms Wavelength Calibration
As mentioned above, HZ2 is used for wavelength scale monitoring of the Visible grism. In
addition a F type star, HD 13499 will be observed once per year. Eventually, the star will be
o#set to monitor wavelength variations across the field of view. This observation will use 15 ks,
eventually split in two to allow for the pointing o#set.
2.1.3.3 Monitoring the Photometric Calibration
Two targets will be used for this purpose: BPM 16274 with two observations per year for 15 ks
each, and the standard field SA95­42 only once per year with 35 ks.
2.1.3.4 Engineering Mode Observations
These type of exposures should be performed whenever the OM does not allow any filter ob­
servations but needs to be blocked because of bright optical sources. A recipe on how to chose
engineering mode sequences based on the time available was provided by the OM calibration
scientist. Currently the following version applies:

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Obs. OM Sequence of Engineering Modes
Length Length
[ks] [s]
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­
5 ­ 10 3675 Flat low
10 ­ 15 8908 E6, Flat low, Dark low
15 ­ 20 13736 E6, Flat high
20 ­ 25 17411 E6, Dark low, Flat high
25 ­ 30 24360 Flat high, Full Frame High Res.
30 ­ 35 29593 E6, Flat high, Full Frame High Res., Flat low
35 ­ 40 33268 E6, Flat low, Dark low, Full Frame High Res., Flat high
40 ­ 45 38096 E6, Flat high, Flat high, Full Frame High Res.
45 ­ 50 41771 E6, Flat high, Flat high, Full Frame High Res., Flat low
50 ­ 55 48720 Flat high, Flat high, Full Frame High Res.,
Full Frame High Res.
55 ­ 60 53953 E6, Flat high, Flat high, Full Frame High Res.,
Full Frame High Res., Flat low
60 ­ 65 57628 E6, Flat high, Flat high, Full Frame High Res.,
Full Frame High Res., Flat low, Dark low
65 ­ 70 64014 E6, Flat high, Flat high, Flat high, Full Frame High Res.,
Full Frame High Res., E6
these observations do not reduce the time available for science.
2.1.3.5 Flat fields and dark frames
Independently of the Engineering observations described in Section 2.1.3.4, flat fields and dark
frames should be obtained more or less periodically at time intervals around 10 days. The ODB
activities ''FLAT LOW'' and ''DARK LOW'' shall be used respectivelly. These observations
should be scheduled parasitically with EPIC CalClose observations, at the end of the revolution.
The default duration of DARK LOW is 4109 s (1500 s exptime + 2609 s overhead), and of FLAT
LOW 4140 s (1500 s exptime + 2640 s overhead). Therefore, depending on the available time
both activities will be scheduled in the same revolution (if more than 8.5 ks available) or only
one of them, in which case the other one should be put in the next revolution. The exposure
time can be edited and reduced to 1000 s if necessary to accomodate one or the two activities
in a given revolution.
2.1.4 XMM­Newton Cross Calibration
In 2003, a major cross­calibration campaign started at the XMM­Newton SOC in collabora­
tion with the Instrument Principle Investigator teams. After reaching a good status for the
calibration of the individual instruments, the project decided to put significant e#orts both
into the internal agreement of the XMM­Newton detectors and the cross­calibration with other
observatories, especially with the Chandra X­ray satellite.
The main cross­calibration target with Chandra/Suzaku is currently PKS2155­304 and is ob­
served once per year in spring.
For internal cross calibration 3C273 is used that may occasionally be replaced by Capella on
request

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Setup for the targets:
PKS2155­304:
. EPIC­pn: small­window, medium filter
. EPIC­MOS: small­window, medium filter
. RGS: spectroscopy
3C273:
. EPIC­pn: small­window, medium filter
. EPIC­MOS: small­window, medium filter
. RGS: spectroscopy
Capella:
. EPIC­pn: small­window, thick filter
. EPIC­MOS: small­window, thick filter
. RGS: spectroscopy
2.1.5 XMM­Newton Long­Wavelength Response
This routine calibration task will be addressed by one annual 60 ks observation of zeta Puppis.
EPIC will normally be scheduled with small­window thick filter exposures, see § 2.1.1.5.
3 Annexes
3.1 Term Planning Skeleton
Routine calibration monitoring formally has started after the revolutions a#ected by the Cluster
launch (i.e. after rev. 113).
Every 3 and now every 6 months a planning skeleton of the upcoming routine calibration obser­
vations is defined in agreement with the calibration scientists and instrument teams. This plan
is included in the general advanced plan for allXMM­Newton observations that is available from
the WWW at http://xmm.esac.esa.int/external/xmm sched/advance plan.shtml.
As mission planning constraints can cause a scheduling di#erent from that in the routine cal­
ibration planning skeleton, the XMM­Newton Observation Log Browser should be checked for
info on the actual scheduling and success of a specific routine calibration observation (see URL
http://xmm.esac.esa.int/external/xmm obs info/obs view frame.shtml).
See also Section 3.2 for a log of the calibration observations that have been performed up to
now.

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3.1.1 Planning skeleton for remaining part of year 2000
Planning of XMM­Newton routine calibration monitoring after rev. 113 for the year 2000.
Revolutions 122 ­ 125: affected by Cluster launch
Revolution 121: OY Car, OM fast mode test
Revolution 122 or 123 (if possible): pn CTI check (20 h)
prior to Rev. 125: PG0136+251, EPIC contamination
October, after eclipses: NGC 2516, EPIC metrology
3.1.2 Routine calibration plan for Jan ­ Mar 2001
Planning for the routine calibration observations in Jan­Mar 2001 (i.e. revolutions from 196 to
239).
Rev. Target Visib. Time Objectives
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­
>= 196 AB Dor 196­239 50ks RGS wavelength
>= 196 N132D 196­236 25ks EPIC eff area, gain, offset
>= 208 HR1099 208­223 40ks RGS wavelength
>= 219 Sco X­1 219­230 ~20ks RGS CTI, EPIC burst, RFS, ff­> PSF wings
~= 220 EXO0748 196­239 ~50ks OM contam & calib (replaces LBB227)
>= 225 Capella 225­239 30ks RGS wavelength
>= 238 RXJ0720 238­239 55ks EPIC contamination
~= 239 AB Dor 196­239 50ks RGS wavelength
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­
Assuming an average of 2ks for instrument set­up overheads and 6ks for slews
(closed+open), the total amount of time to be spent for routine calibrations
in these three months is ~380 ks.
Comments: N132D analysis of previous failure still pending ­ was replaced by an observation of
NGC 2516. RXJ0720 probably needs major updates of SAS and DB to allow correct analysis
of earlier observation ­ on hold. The last AB Dor observation was dropped as Capella was late
and as the next AB Dor observation is planned for rev 250 already.
3.1.3 Routine calibration plan for Apr ­ Jun 2001
Planning for the routine calibration observations in Apr­Jun 2001 (i.e. revolutions from 240 to
286).
Rev. Target Visib. Time Objectives
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­
=> 240 1ES0102 240­276 30ks EPIC gain/offset & eff. area
~= 250 AB Dor 240­286 50ks RGS wavelength
=> 256 Mkn421 256­271 50ks RGS eff. area
~= 260 EXO0748 240­286 35ks OM photomometry (last done in 212 TBC)
~= 265 AB Dor 240­286 50ks RGS wavelength
=> 277 3C273 277­286 100ks RGS eff. area (not visib. 284, should be
coordinated with SAX(?)/Chandra) &
OM contamination
~= 280 AB Dor 240­286 50ks RGS wavelength
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­

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Assuming an average of 2ks for instrument set­up overheads and 6ks for slews
(closed+open), the total amount of time to be spent for routine calibrations
in these three months is ~440 ks (~ 7% of available time).
3.1.4 Routine calibration plan for Jul ­ Dec 2001
Planning for the routine calibration observations in Jul­Dec 2001 (i.e. revolutions from 287 to
378).
Rev. Target Visib. Time Objectives
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­
=>291 G153 291­312 30ks OM photometry
~=310 HR1099 301­316 40ks RGS wavelength scale
~=325 N132D 287­378 25ks EPIC gain/offset & eff. area
~=340 AB Dor 287­378 50ks RGS wavelength scale
>344? NGC2516 287­378 20ks EPIC stability of boresight (after eclipse)
~=351 EXO0748 287­378 40ks OM photometry (raster)
~=370 N132D 287­378 25ks EPIC gain/offset & eff. area
~=370 AB Dor 287­378 50ks RGS wavelength scale
<=380 3C273 368­381 100ks RGS eff area (coord), OM photometry,
EPIC (parasitically) spectr. capab. & contam.
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­
Note: 3C273 might be replaced by PKS2155.
Assuming an average of 2ks for instrument set­up overheads and 6ks for slews
(closed+open), the total amount of time to be spent for routine calibrations
in these six months is ~452 ks. If one assumes 10432ks available time the
percentage of time for routine calibration will be ~4.3%.
As the OM team suggested, there might be some more time needed for OM NRCOs.
3.1.5 Routine calibration plan for Feb ­ Jun 2002
Planning for the routine calibration observations in Feb­Jun 2002 (i.e. revolutions from 394 to
468). Note that in Jan 2002 no routine calibrations were performed due to mission planning
constraints.
Rev. Target Visib. Time Objectives
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­
>=396 LBB227 396­409 15ks OM photometry
~=402 N132D always 25ks EPIC gain/offset & eff. area
~=410 GD71 410­425 35ks OM spectrophotometric Grism
~=415 Capella 408­423 30ks RGS wavelength scale
~=432 1ES0102 423­459 25ks EPIC gain/offset & eff. area
>=436 NGC2516 always 20ks EPIC stability of boresight (after eclipse)
~=439 EXO0748 always 50ks OM photometry
>=444 BPM16274 444­464 15ks OM photometry
~=450 PKS2155 438­451 100ks RGS eff area (coord), OM, EPIC (parasitically)
spectr. capab. & contam.
~=460 AB Dor always 50ks RGS wavelength scale
~=460 GD153 460­468 35ks OM spectrophotometric Grism
~=462 N132D always 25ks EPIC gain/offset & eff. area
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­

XMM­Newton SOC
Document No.: XMM­SOC­CAL­PL­0001
Issue/Rev.: Version 2.9
Date: 10.01.2008
Page: 10
Assuming an average of 2ks for instrument set­up overheads and 6ks for slews
(closed+open), the total amount of time to be spent for routine calibrations
in these five months is ~425+(12*8)=521ks. If one assumes 140ks available
time per revolution, the period covered here (75 revolutions) is 10500ks
and hence the percentage of time for routine calibration will be ~5%.
Comments: LBB227 has been replaced by a NRCO: OM photometric zeropoints (target Feig 16
o#set, 25 ks). GD71 was finally removed from the plan and replaced by target SA 95. NGC2516
was dropped in this term.
3.1.6 Routine calibration plan for Jul ­ Dec 2002
Rev. Target Visib. Time Objectives
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­
469 N132D always 25ks EPIC gain/offset & eff. area
470 GD 153 460­474, 15ks OM spectrophotometry, EPIC (CAL)CLOSED
552­566
480 HD8867 465­480 28ks OM grism wavelength (5x4ks raster)
480 HD13499 470­487 16ks OM grism wavelength (3x4ks raster)
480 ? n.a. 23ks EPIC (CAL)CLOSED (dedicated)
489 Hz 4 486­501 4ks OM UV flux (not 499)
489 GD50 484­499 4ks OM UV flux
489 BD+33 2642 478­499 4ks OM UV flux
490 HR1099 484­499 40ks RGS wavelength scale, EPIC (CAL)CLOSED
501 Hz 2 492­496, 15ks OM grism flux, EPIC (CAL)CLOSED
501­506
515 Capella 501­517 30ks RGS wavelength scale, EPIC (CAL)CLOSED
(after eclipse, coord. with Chandra!)
517 1ES0102 517­551 30ks EPIC gain/offset & eff. area
525 ? n.a. 23ks EPIC (CAL)CLOSED (dedicated)
535 PKS2155 531­544 100ks RGS eff area, OM & EPIC parasitically
(coord. with Chandra!),EPIC (CAL)CLOSED
541 NGC7293 534,535, 15ks OM grism flux (ONLY IF NO AO­2 TARGET!)
538­546 EPIC (CAL)CLOSED
542 G93­48 533­535, 4ks OM UV flux
538­546
542 BD+284211 541­557 4ks OM UV flux
547 1ES0102 517­551 30ks EPIC gain/offset & eff. area
550 AB Dor always 50ks RGS wavelength scale, EPIC (CAL)CLOSED
552 BPM 16274 537­556 15ks OM spectrophotometry, EPIC (CAL)CLOSED
­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­­
Assuming an average of 2ks for instrument set­up overheads and 6ks for slews
(closed+open), the total amount of time to be spent for routine calibrations
in these six months is ~124ks+{11 targets*(2ks(overhead)+6ks(slew)}=212ks.
If one assumes 135ks available time per revolution, the period covered here
(93 revolutions) is 12555ks and hence the percentage of time for routine
calibration will be ~5%.
Comments: HD8867 was finally removed from the plan. For HD13499 a 3 â 8 ks raster was
performed. Dedicated EPIC (cal)closed observations in revs. 480 and 525 were dropped as
several such observations could be performed parasitically to non EPIC routine cal. and non­
routine cal. observations.

XMM­Newton SOC
Document No.: XMM­SOC­CAL­PL­0001
Issue/Rev.: Version 2.9
Date: 10.01.2008
Page: 11
All further detailed implementation plans of calibration can be found on the EPIC internal web
page at:
http://xmm.esac.esa.int/ xmmdoc/internal/int cal instr supp/epic/idt.php
3.2 Performed calibration observations
A log of actually performed routine and non­routine calibration observations can
be found at:
http://xmm.esac.esa.int/ xmmdoc/internal/int cal instr supp/epic/index.php