XMM-Newton: Status Of The Project

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XMM-Newton Status Of The Project

• Talk for the The X-ray Universe 2008 symposium
• 27th to 30th of May 2008, Granada, Spain
• Norbert Schartel
• (XMM-Newton Project Scientist)

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Contents

• Status of spacecraft, its instruments and
  calibration
• Status of the observing program
• XMM-Newton users, oversubscription and requests
• Scientific highlights
• Publications and citations
• Public outreach
• Conferences and their proceedings
• Next Call for observing time new chances
• Conclusions performance key points

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Status of the Spacecraft

• Spacecraft status is very good
• In May 2007 Mission Extended Operations Review
  concluded that XMM-Newton can operate at least up
  to 2018
• All systems are running on their primary unit,
  i.e. full redundancy still available
• At end of 2008 April, 87 kg of fuel remain with
  usage of around 6 kg per year
• The solar array is generating around 1950 W and
  between 800-1200 W are used.
• All other consumable are fine, too
• On November 2007, the SPC approved operations
  until end of 2012. Further extensions will be
  reviewed in 2 years time

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Status of the Optical Monitor

• primary components in use, i.e. full redundancy
  still available

• Sensitivity loss in 2015
• U, B, V 20
• UV 20 40

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Status of the Reflection Grating Spectrometers

• 2 CCDs were lost early in the mission (full
  wavelength coverage due to redundancy between
  RGS1 and RGS2)
• RGS 2 single readout mode since August 2007 to
  avoid ADC errors (no impacts for large majority
  of sources)
• Reduction in EPIC MOS and RGS operating T in 2002
  resulted in far fewer hot pixels

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Status of the Reflection Grating Spectrometers
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Status of the EPIC Cameras

• The Nov 2002 reduction in EPIC MOS (and RGS)
  operating T resulted in far fewer hot pixels, and
  decreased energy resolution degradation rates.
• 4 micrometeoroid impact events in 7 yrs have
  resulted in the loss of 1 in 14 of the MOS CCDs
  a 5 reduction in the EPIC area.
• No effects of contamination visible

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Status of the EPIC Cameras
CAMERA FWHM _at_ MN AFTER LAUNCH FWHM _at_ MN AFTER COOLING FWHM _at_ MN IN 2015 FWHM _at_ AL AFTER LAUNCH FWHM _at_ AL AFTER COOLING FWHM _at_ AL IN 2015
MOS1 135 140 156 75 75 86
MOS2 135 135 148 77 77 82
pn 155 NA 185 120 NA 141
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Calibration
Representative examples 1H1219301
Line rich source 1ES0102-7219
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Calibration
XMM-Newton versus Suzaku
XMM-Newton vs. Chandra ACIS/LETG
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Status of the Observing Program

• Statistics up to REV 1532 (5.5.2007)?
• A1 to A5 Program and GT
  finished
• Open Time Program A6
• Number of allocated targets (A and B)
  413
• Allocated cumulative exposure time
  12910 ks
• Number of successfully observed targets
  401 (97.1)?
• Successfully observed cumulative exposure time
  12591 ks (97.5)?
• AO7 started on May 1, 2008
• Statistics of C-priority observations
• AO3 observed cumulative exposure time
  1200 ks ( 9.2 )?
• AO4 observed cumulative exposure time
  1367 ks (31.0)?
• AO5 observed cumulative exposure time
  2232 ks (26.5)
• AO6 observed cumulative exposure time
  2459 ks (31.8)

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Users

• Observatory type mission
• Annual call for observing time proposals
• Peer review process (OTAC)
• Support for users from definition of observation
  details, enhancement, scheduling/coordination,
  TOO request evaluation and TOO implementation
  help-desk, analysisto (SAS) calibration
  archiving SAS workshops, documentation,
  conferences and public outreach
• Users
• Large Community 1500 - 2000 scientists
• All scientific topics are addressed
• from comets and planets up to the most distant
  quasars
• Most of the users are external to the
  XMM-Newton project, e.g. they do not belong to
  instrument institutes nor the Survey Science
  Center)

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Requests and Users

• Announcement of Opportunity AO7
• 586 valid proposals were submitted
• Oversubscription 7.8
• 424 different principal investigators from 23
  countries
• 1560 individual scientists
• 8 proposals joint XMM/Chandra
• 11 proposals joint XMM/VLT
• Observing Time Allocation Committee OTAC
• 13 panels
• 66 scientists (rotation every 2 AOs)

• Archive XSA
• 2400 external registered uses
• 110 external users per month (typical value)
• 2500 data sets (ODF and PPS) per month (typical
  value)
• Analysis Software SAS
• Version 7.1 (from July 2007)
• 1240 downloads
• 2200 scientists have access to SAS 7.1

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XMM-Newton Extended Survey Of The Taurus
Molecular Cloud

• Taurus molecular cloud is the nearest star
  formation region
• Detection of almost all young stars embedded in
  the cloud as X-ray sources, including many brown
  dwarfs and protostars
• Identification of unusual physical processes not
  known before in forming stars
• Gas streams falling down onto the forming and
  young star
• Ejection of jets

• AA special feature 15 papers, 2007,
  AA 468 Guedel et al., 2007, AA 468,
  353

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Million-Degree Plasma Pervading the Extended
Orion Nebula

• The Orion nebula is illuminated by a small group
  of massive stars (the Trapezium).
• ? XMM-Newton observations reveal a hot plasma
  with a temperature of 1.7-2.1 106 K pervading the
  southwest extension of the Orion nebula.
• ? The plasma flows into the adjacent interstellar
  medium.
• ? This X-ray outflow phenomenon must be
  widespread throughout our Galaxy.
• M. Guedel et al., 2008, Science 319, 309

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New Class Of Type 1 SN

• DEM L238 DEM L249
• Thermal spectrum dominated by Fe L-shell lines
• Fe over-abundance ? Thermo-nuclear Type Ia
  explosions
• K.J. Borkowski et al. 2007, ApJ 652, 1259

• Explosions with energies of 3 1050 ergs
• New class of SN Ia, more massive and young (100
  Myr old) progenitors

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Broad Relativistic Iron Line From Serpens X-1

• Neutron star low-mass X-ray binary (LMXB) Serpens
  X-1
• Previously known broad iron Ka emission line
• Asymmetric shape of the line supports an inner
  accretion disk origin
• ? First strong evidence of a relativistic line in
  a neutron star LMX
• Bhattacharyya Strohmayer, 2007, ApJ 664, L103

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First Black Hole In Globular Star Clusters

• GCs contain 103-106 old stars packed within tens
  of light years
• Formation of 103 solar mass BH ?
• Interaction will eject BHs ?
• T.J. Maccarone et al., 2007, Nature 445, 183

NGC 4472

• X-ray source in GC associated with NGC 4472 (in
  the Virgo cluster)
• X-ray luminosity 4x1039 erg s-1
• Variability excludes composition by several
  objects
• ? Black hole (15-30 or 400 solar masses)

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Compact, Conical, Accretion-Disk Warm Absorber Of
The Seyfert 1 Galaxy NGC4051

• Absorber consists of two different ionization
  components, with a difference of 100 in
  ionization parameter and 5 in column density
• Distances 0.5-1.0 lt-days (2200RS-4400RS) and
  lt3.5 lt-days (lt15,800 RS) from the continuum
  source

• Suggests strongly accretion-disk origin for the
  warm absorber wind
• ? Mass outflow rate from wind is 2-5 of the
  mass accretion rate
• Krongold et al., 2007, ApJ 659, 1022

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Origin Of Elements In Galaxy Clusters

• Sersic 159-03 2A 0335096

N. Werner, et al. , 2006, AA 446, 475 J. de
Plaa, et al. 2006, AA 452, 397 2007, AA 465,
345

• Abundances ?
• 30 of the supernovae in these clusters were
  exploding white dwarfs (Type Ia)
• 70 were collapsing stars at the end of their
  lives (core collapse)

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XMMXCS J2215.9-1738

• Massive galaxy cluster at z1.45
• The redshift of XMMXCS J2215.9-1738 is the
  highest currently known for a spectroscopically
  confirmed cluster of galaxies
• Stanford et al., 2006 ApJ 646, L13

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Dark Matter Maps Reveal Cosmic Scaffolding
COSMOS Field 1.637 degree2 1000 h (HST)
400 h (XMM)
Matter 1/6 baryonic
(hot and cold) 5/6 dark
Gravitational lensing total amount of matter
(hot and cold) Optical infrared cold baryonic
matter

• Maps of the large-scale distribution of dark
  matter, resolved in both angle and depth.
• Loose network of filaments, growing over time,
  which intersect in massive structures at the
  locations of clusters of galaxies
• Consistent with predictions of gravitationally
  induced structure formation

R. Massey et al., 2007, Nature 445, 286
XMM-Newton hot matter (red in picture)
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Detection of hot gas in the filament connecting
two clusters of galaxies

• about 50 of the baryons in the local Universe
  are expected to resides in filaments connecting
  clusters of galaxies in form of low density gas
  with temperatures of 105ltTlt107 K.

• filament connecting the clusters of galaxies A
  222 and A 223 (z 0.21) has been previously
  detected using weak lensing data
• ?detection of the filament in the soft-band
  X-rays with a 5s with . kT
  0.91 0.25 keV
• ?baryon over-density of ?/lt?Cgt 150, which is
  consistent with expectations . for the densest
  and hottest parts of the warm-hot intergalactic
  medium
• . Werner et al., 2008, AA 482, 29

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XMM-Newton Serendipitous Source Catalogue 2XMM

• 246897 source detections corresponding to 191870
  unique sources
• 360 square degrees
• Source products spectra, light curves
• Well-defined samples of various object types
  AGN, clusters of galaxies, interacting compact
  binaries, active stellar coronae
• Largest X-ray source catalogue ever produced
• Released in August 2007

• M. Watson et al. 2008, in preparation

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Publications
2007 330 publications 2008 (May) 115 in
refereed journals directly based on XMM-Newton
data
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Citations
31.4 citations / paper
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Public Outreach 2007
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Public Outreach 2007
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Public Outreach 2007
http//xmm.esac.esa.int/external/xmm_news/latest_n
ews.shtml
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Public Outreach 2008
http//xmm.esac.esa.int/external/xmm_news/
latest_news.shtml
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Conferences and
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and their Proceedings
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Next Call of Proposals AO8

• Planned key milestones
• Announcement 26 August 2008
• Due date for proposals 10 October 2008 (1200
  UT)?
• Final approved program late December 2008
• Second phase submission 12 January 6 February
  2009
• Start of observations May 2009
• 6 Scientific categories / 13 Panels in total / 66
  scientists
• OTAC chairpersons selected
• Panel member search underway

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AO8 New Modes

• New Mosaic mode for observation of large areas
  with short exposure time
• Since AO7 pn modified timing for observation of
  very bright sources
• Since AO7 RGS multi-pointing mode for very
  homogenously exposed spectra

courtesy of Pedro Rodríguez-Pascual
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AO8 Large and Very Large Programs
courtesy of Pedro Rodríguez-Pascual

• Very Large Programs can ask for observations to
  be performed over two AOs with observation of up
  to 1.5 Ms in the following AO
• Maximum size of Very Large Programs will be
  defined reflecting the total time available for
  Large and Very Large Programs as well as the
  actual visibility of the proposed target

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Conclusion Performance Key Points

• XMM-Newton is unique at
• Large field of view (d30)
• Large collecting area (gt2000 cm2 for all EPIC)
• Largest collecting area at 6.4 keV
• High time resolution
• High spectral resolution (RGS, best for extended
  sources)
• Long observations (130 ks)
• XMM-Newton can operate at least up to 2018
• ? No other telescope with similar or better
  overall performances available for the next 10
  years or more