The XMM-Newton Survey Science Centre identifdication (XID) programme

1
The XMM-Newton Survey Science Centre
identifdication (XID) programme

• Xavier Barcons
• Instituto de Física de Cantabria (CSIC-UC)
• Santander, Spain

2
on behalf of the SSCentre XID working group

• Astrophysikalisches Institut Potsdam (Germany)
  Y. Hashimoto, G. Lamer, G. Szokoly, A. Schwope
• Centre d'Etude Spatiale des Rayonnements
  (France) N. Webb
• Institute of Astronomy, Cambridge (UK) R.G.
  McMahon, W. Yuan, A.C. Fabian, C.S. Crawford
• Instituto de Astrofísica de Canarias,
  Tenerife (Spain)I. Pérez-Fournon
• Instituto de Física de Cantabria, Santander
  (Spain) X. Barcons, F.J. Carrera, M.T. Ceballos,
  S. Mateos
• Subaru Telescope K. Sekiguchi
• Max-Planck-Institut fuer extraterrestriche
  Physik (Germany) T. Boller, G. Hasinger, W.
  Pietsch
• Mullard Space Science Laboratory, UCL (UK)
  M.S. Cropper, K.O. Mason, M.J. Page, S. R. Rosen
• Observatoire Astr de Strasbourg (France) C.
  Motch, P. Guillout, L. Mirioni, I. Negueruela, M.
  Pakull
• Osservatorio Astronomico di Brera, Milano
  (Italy) T. Maccacaro, R. Della Ceca, P.
  Severgnini
• University of Bristol (UK) D.M. Worrall, M.
  Bremer, M. Birkinshaw
• University of Central Lancashire (UK) G.E.
  Bromage, B.J.M. Hassall
• University of Leicester, (UK) M.G. Watson,
  J.P. Pye, D. Baskill, G.C. Stewart, T.P. Roberts,
  J.P. Osborne, N. Schurch, P.J. Wheatley, M.J.
  Ward, R.S. Warwick, J.A. Tedds
• XMM Science Operations Centre, (Spain) N.
  Schartel
• Harvard Smithsonian Astrophysical
  Observatory M. Elvis

3
Index

• The XID programme goals and strategy
• The imaging programme
• The extragalactic core programme
• The faint sample (almost nothing to report)
• The medium sample
• The bright sample (talk by R. Della Ceca)
• The Galactic Plane sample (poster by C. Motch)
• Other activities
• Outlook

4
The XMM-Newton serendipitous sky survey

• Every new XMM-Newton pointing discovers 30-150
  serendipitous X-ray sources.
• About 50,000 new X-ray sources/year
• Overall goal build up a catalogue with all
  serendipitous X-ray sources and their likely
  identifications

5
The XID strategy statistical identifications
X-ray properties
Need a large training sample with
proper spectroscopic ids the core programme
6
XID programme details

• Core programme (1000 sources/sample)
• High b faint sample (10-15 erg cm-2 s-1)
• High b medium sample (10-14 erg cm-2 s-1)
• High b bright sample (10-13 erg cm-2 s-1)
• Galactic Plane Sample (7 10-15 erg cm-2 s-1)
• Imaging programme (u,g,r,i,Z,H) a large
  number of XMM-Newton observations

7
XID ground-based resources

• Optical/IR imaging
• INT 2.5m with WFC
• ESO 2.2m with WFI
• Subaru 8.3m with SuprimeCam FOCAS
• Optical spectroscopy
• WHT 4.2m with ISIS
• WHT 4.2m with WYFFOS/AUTOFIB2
• TNG 3.5m with DOLORES
• NOT 2.5m with ALFOSC
• Subaru 8.3m with FOCAS

8
XID observational strategy
9
AXIS An XMM-Newton International Survey

• International Time Project (ITP) approved by the
  Comité Científico Internacional for years 2000
  and 2001 total of 85 nights spread in 4
  telescopes
• Major boost to XID programme in
• Imaging programme
• High galactic latitude medium sample
• High galactic latitude bright sample
• Galactic Plane survey

10
Imaging programme
XMM-Newton imaged fields in various filters Last
Updated 28 October 2001
Optical INT2.5m/WFC ESO2.2m/WFI Near IR
INT2.5m/CIRSI
11
Depth of images
Galaxies
Stars
SDSS
12
Seeing distribution
13
Astrometric calibration

• 100-200 APM or USNO stars per CCD each of 4 CCD
  chips is fit independently
• Median rms 0.25 believed due to internal errors
  in external catalogue and proper motions

Chip-4
14
Automated Photometric calibration
The majority of the images have photometric
calibration error lt 0.1 mag Currently exploring
systematics due to variations in zero-point and
extinction constants
15
Public release of XID optical images

• Fully-reduced CCD mosaics covering almost entire
  EPIC FOV in various filters
• Astrometrically and photometrically calibrated
  images and optical source catalogues
• Release of optical images corresponding to public
  XMM-Newton data

Release by end of January 2002
16
Spectroscopic identifications
Search for candidate counterparts i-band sources
within either 5? (statistical) or 5 arcsec

• Bright Sample gt95 success with 1 single
  candidate
• Medium Sample 90 success, 3/4 with single
  candidate
• Galactic Plane
• b10-20º, 85 success, 1/2 with single
  candidate
• b0-10º, very large star density no unique
  candidate

17
High-b identifications
119 BLAGN 23 NELG 15 Galaxies 2 BLLAC 41 Stars
18
The high-b medium sample

• Flux limit 2?10-14 erg cm-2 s-1 (0.5-4.5 KeV)
• Source density 110 sources deg-2
• 30 fields in the North 498 X-ray sources
• 122 identifications (25)
• By March 2002, expect a sample of 15 fields (212
  X-ray sources) identified to 90
• a few of X-ray sources do not show optical
  counterpart within 22.5mag

19
Medium Sample preliminary results

• 2 fields (Mkn205 and G133-69 Pos_2), 29 X-ray
  sources over 0.26 deg-2
• 19 Broad Line AGN (incl 2 BAL QSOs)
• 6 Narrow-Line AGN
• 1 Abs line Galaxy (NGC 4291)
• 1 Active Coronal Star
• 2 Unidentified (1 unobserved, 1 very faint)

20
MS Hardness ratios
HR1 0.5-2.0 keV ? 2.0-4.5 keV HR2 2.0-4.5 keV ?
4.5-10 keV
Marginal evidence for NLAGN being absorbed
BLAGN BLAGN have ?2 at 0.5-4.5 keV and ?1.6 at
4.5-10 keV
21
MS The X-ray source population
22
The Galactic Plane sample
23
The Galactic plane at b0º
24
Ha flux versus X-ray flux for ROSAT and XMM Me
stars
Me Stars
Rosat Cygnus Region (Motch et al. 1997)
G21.5-09 Ridge 3
25
The Galactic Plane landscape

• Active coronae exhibit soft X-ray spectra (HR2 lt
  0)
• Most soft X-ray sources have active coronae
  counterparts
• The population of Me stars seen by XMM-Newtin is
  similar to that detected by ROSAT, just seen
  farther away.
• The Me to K-A star ratio is 30, similar to
  that of ROSAT
• No Cataclysmic Variable has been yet detected
  down to an estimated R magnitude of 19.

26
The Be accreting binary SS397
27
SS397 a BeNS/WD accreting binary?

• Too X-ray luminous to be an isolated Be0.5 star
  binary
• Hard X-ray spectrum (?1.5 or kT 9 keV)
• LX1032 erg s-1, very low for a NS accreting
  binary
• A very good candidate to BeWD binary

28
Other on-going or planned XID activities

• Pilot cluster survey
• Pilot hard X-ray source survey
• EPIC astrometry studies (poster by J. Tedds
  Mike Watson)
• X-ray spectral templates / X-ray colours of
  various populations
• Bi-variate flux distributions

29
Special thanks to...

• Mike Watson, Jonathan Tedds X-ray sources,
  overall managing
• Mat Page Fibre spectroscopy
• Francisco Carrera AXIS programme and much more
• Richard McMahon Imaging programme
• Christian Motch Galactic plane survey
• Axel Schwope Southern observations
• Tommaso Maccacaro, Roberto Della Ceca Bright
  sample