The X-ray source population studies in nearby galaxies

1
The X-ray source population studies in nearby
galaxies

• Wolfgang Pietsch
• Max Planck Institut für extraterrestrische Physik

2
Outline

• Introduction to X-ray source population in galaxy
  fields
• X-ray source population of M 33 field
• X-ray source population of the Andromeda galaxy M
  31 field
• Advancements with Simbol-X observations

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Introduction X-ray sources in nearby galaxy
fields

• Sources within galaxy (all approximately at same
  distance)
• X-ray binaries (XRBs)
• Low mass XRBs (?dips with orbital period, bursts,
  ...)
• High mass XRBs (?eclipses with orb. period,
  pulsations, optical id,...)
• Bright transients
• Supersoft X-ray sources
• Classical SSS as known from Magellanic Clouds
• Optical novae (dominant class of SSS in M 31)
• Supernova remnants
• Thermal remnants
• Plerions (PWN)
• Nuclear source
• Ultraluminous X-ray sources
• Diffuse emission in disk and halo
• Foreground stars
• Galaxies, galaxy clusters and AGN in background

4
XMM-Newton EPIC view of the diffuse emission of
the starburst galaxy NGC 253

• Simbol-X
• ULX sources
• undetected AGN???
• Hard X-ray halo???

• Bauer et al. 2007

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XMM-Newton survey of the Local Group galaxy M
33
W. Pietsch, Z. Misanovic, F. Haberl, D.
Hatzidimitriou, M. Ehle, G. Trinchieri
2004, AA 426, 11
408 Xray sources X-ray properties Correlation
with catalogues from other wavelength Optical
identification Identify foreground and background
sources Characterization of X-ray source
population of M 33
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Hardness ratio plots of M 33 sources
HRi (Bi1 Bi)/ (Bi1 Bi)
B1 0.2-0.5 keVB2 0.5-1.0 keV B3 1.0-2.0 keV
B4 2.0-4.5 keV B5 4.5- 12 keV
fg-star AGN SSS SNR XRB
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Hardness ratio plots of M 33 sources
HRi (Bi1 Bi)/ (Bi1 Bi)
B1 0.2-0.5 keVB2 0.5-1.0 keV B3 1.0-2.0 keV
B4 2.0-4.5 keV B5 4.5- 12 keV
fg-star AGN SSS SNR XRB
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Hardness ratio plots of M 33 sources
HRi (Bi1 Bi)/ (Bi1 Bi)
B1 0.2-0.5 keVB2 0.5-1.0 keV B3 1.0-2.0 keV
B4 2.0-4.5 keV B5 4.5- 12 keV
fg-star AGN SSS SNR XRB
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X-ray sources in M 33 field identification and
classification
Using X-ray hardness ratio criteria, optical
correlation with USNO-B1, catalogues at
different wavelengths, SIMBAD, NED

• identified classified
• foreground stars 5 30
• AGN 12
• Galaxies 1 1
• SSS 5
• SNR 21 (2) 23 (-2)
  (Ghavamian et al. 2005, AJ 130, 539)
• XRB 2
• Hard 267

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M 33 zoom in
M33 X-7
PMH2004 47
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Eclipsing X-ray binary M33 X-7
Einstein ROSAT observations 3.45 d
period 0.31 s pulsation? Peres et al. 1989, ApJ
336, 140 Dubus et al. 1999, MNRAS 302, 731
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Eclipsing X-ray binary M33 X-7
Pietsch et al. 2004, AA 413, 879
On state Eclipse On
state XMM-Newton EPIC
Chandra ACIS I 0.5-4.5 keV images
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Eclipsing X-ray binary M33 X-7
Pietsch et al. 2004
Optical identification Star with V 18.9 mag with
3.45 d variability DIRECT image by B.
Mochejska Green circle ROSAT error box Haberl
Pietsch 2001 Yellow circle Chandra error
box Insert HST image 10 x 10 Pietsch et al.
2006, ApJ 646, 420
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Eclipsing X-ray binary M33 X-7
Pietsch et al. 2004, AA 413, 879
XMM-Newton EPIC Chandra ACIS-I Optical V and
B-V light curvere-analysis of DIRECT data by B.
Mochejska folded modulo 3.45d period Dubus et al.
1999 Improved binary ephemeris
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Eclipsing X-ray binary M33 X-7
Best fitting spectral modelsAbsorbed
bremsstrahlung or disk blackbody
First eclipsing black hole (high mass) X-ray
binary ?
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ChASeM33 lightcurve of X-7
Pietsch et al. 2006, ApJ 646, 420
Gemini North radial velocity curve
gt 6.9 Msun black hole Orosz et al. 2007,
ATel 977
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ChASeM33 light curve of PMH2004 47
2nd eclipsing HMXB in M33 Orbital period 1.73245
d Similar to LMC X-4 or Her X-1
Pietsch et al. 2006, ATel 905
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The Andromeda Galaxy M 31
W. Pietsch, M. Freyberg, F. Haberl et.al. 2004,
AA 434, 483

• Similar analysis to M 33 based on archival
  data
• 856 sources in fields
• Hardness ratio and time variability
• classification and identification

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M 31 centre

• All EPIC mosaic (100 ks)
• SNRs, SSSs
• foreground stars
• diffuse emission
• Many LMXBs
• Galaxtic center sources not fully resolved
• Movie of centre area by blinking four
  observationswith separation of half a year plus
  one 2.5 year later

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Time variability of X-ray sources in the M 31
centre field
H. Stiele, W. Pietsch et al. 2007, in preparation
1035 1036 1037
1038 erg/s

• Determine time variability between M 31
  center pointings half a year apart
• Check classification of SNRs
• Classify new XRB candidate by time
  variability

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Variable X-ray sources in the M 31 centre
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Summary catalogue

• HR2-HR1 diagram important to select SSS, thermal
  SNRs and foreground stars
• fx/fopt separate SNRs and foreground stars
• Hard X-ray spectra very important for
  classification should separate
• XRBs
• Active nuclei
• Plerions
• Individual papers on bright sources (Osborne et
  al, Barnard et al., Trudolyubov et al., Mangano
  et al.)
• Time variability studies to identify XRBs

Simbol-X
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XMM-Newton detection of type I X-ray bursts in M
31
W. Pietsch F. Haberl 2005, AA 430, L45

• search for X-ray bursts in GC candidates from
  catalogue paper
• 37 sources in fields
• most GC sources in center field that got
  longest exposure
• two burst sources detected in X-ray faint
  GCs, neutron star LMXBs

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X-ray burster PFH2005 253 in the GC WSB85 S5
15

• Observation c4 Jan 7, 2002

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Optical novae the major class of supersoft X-ray
sources in M 31
Pietsch, Fliri, Freyberg, Greiner, Haberl,
Riffeser, Sala 2005,

AA 442, 879

• search for optical nova correlations in XMM-
  Newton, Chandra and ROSAT catalogs and
  archival observations
• 21 X-ray counterparts in M 31 and 2 in M 33
• novae dominant class of supersoft X-ray
  sources in M 31 center
• determine masses of ejecta and burned mass
  from lightcurve

10 arcmin
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X-ray burster PFH2005 253 in the GC WSB85 S5
15

• Rise time lt 10 s Total 50 cts
• Maximum duration lt 20 s Max.
  rate 1.40.4ct/s
• Decay to backgr. 150 s
  corresponds to 3.8 1038erg/s
• Quiescent luminosity 5 1036erg/s
  (Eddington limit for H-poor matter)

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Chandra HRC nova detections 2004/5 Pietsch et
al. 2007, AA 465, 375
Nova SSS light curves (lt250 d)
More than 30 of optical novae show SSS state
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Simbol-X contributions X-ray sources in nearby
galaxy fields

• Sources within galaxy (all approximately at same
  distance)
• X-ray binaries (XRBs)
  lthardgt
• Low mass XRBs (?dips with orbital period, bursts,
  ...)
• High mass XRBs (?eclipses with orb. period,
  pulsations, optical id,...)
• Bright transients
• Supersoft X-ray sources
• Classical SSS as known from Magellanic Clouds
• Optical novae
• Supernova remnants
• Thermal remnants
• Plerions (PWN)
  lthardgt
• Nuclear source
• Ultraluminous X-ray sources
• Diffuse emission in disk and halo
• Foreground stars
• Galaxies, galaxy clusters and AGN in background
  lthardgt

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Simbol-X contributions X-ray sources in nearby
galaxy fields

• Sources within galaxy (all approximately at same
  distance)
• X-ray binaries (XRBs)
  lthardgt
• Low mass XRBs (?dips with orbital period, bursts,
  ...)
• High mass XRBs (?eclipses with orb. period,
  pulsations, optical id,...)
• Bright transients
• Supersoft X-ray sources
• Classical SSS as known from Magellanic Clouds
• Optical novae
• Supernova remnants
• Thermal remnants
• Plerions (PWN)
  lthardgt
• Nuclear source
• Ultraluminous X-ray sources
• Diffuse emission in disk and halo
• Foreground stars
• Galaxies, galaxy clusters and AGN in background
  lthardgt

Important Simbol-X parameters for nearby galaxy
investigations Big field of view
high resolutionUnexplored energy band !!!
Discovery space for the unpredicted !!!