The X-ray source population The X-ray source population studies in nearby galaxies studies in nearby galaxies

Wolfgang PietschMax Planck Institut für extraterrestrische Physik

OutlineOutline

• 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

Introduction: X-ray sources in nearby Introduction: X-ray sources in nearby galaxy fieldsgalaxy 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

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

Bauer et al. 2007

Simbol-X:

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

408 X–ray 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

XMM-Newton survey of the Local GroupXMM-Newton survey of the Local Group galaxy M 33 galaxy M 33 W. Pietsch, Z. Misanovic, F. Haberl,

D. Hatzidimitriou, M. Ehle, G. Trinchieri 2004, A&A 426, 11

Hardness ratio plots of M 33 sourcesHardness ratio plots of M 33 sourcesHRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B1: 0.2-0.5 keV

B2: 0.5-1.0 keV B3: 1.0-2.0 keV B4: 2.0-4.5 keV B5: 4.5- 12 keV

fg-starAGN

SSSSNRXRB

Hardness ratio plots of M 33 sourcesHardness ratio plots of M 33 sourcesHRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B1: 0.2-0.5 keV

B2: 0.5-1.0 keV B3: 1.0-2.0 keV B4: 2.0-4.5 keV B5: 4.5- 12 keV

fg-starAGN

SSSSNRXRB

Hardness ratio plots of M 33 sourcesHardness ratio plots of M 33 sourcesHRi = (Bi+1 – Bi)/ (Bi+1 + Bi) B1: 0.2-0.5 keV

B2: 0.5-1.0 keV B3: 1.0-2.0 keV B4: 2.0-4.5 keV B5: 4.5- 12 keV

fg-starAGN

SSSSNRXRB

X-ray sources in M 33 field: X-ray sources in M 33 field: identification and classificationidentification and classification

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

Using X-ray hardness ratio criteria, optical correlation with USNO-B1, catalogues at different wavelengths, SIMBAD, NED

M 33 zoom in

M33 X-7

[PMH2004] 47

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

Eclipsing X-ray binary M33 X-7Eclipsing X-ray binary M33 X-7

On state Eclipse On state

XMM-Newton EPIC Chandra ACIS I

0.5-4.5 keV images

Eclipsing X-ray binary M33 X-7Eclipsing X-ray binary M33 X-7Pietsch et al. 2004, A&A 413,

879

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

Eclipsing X-ray binary M33 X-7Eclipsing X-ray binary M33 X-7Pietsch et al. 2004

XMM-Newton EPIC + Chandra ACIS-I

Optical V and B-V light curve

re-analysis of DIRECT data by

B. Mochejskafolded modulo 3.45d period Dubus et al. 1999

Improved binary ephemeris

Eclipsing X-ray binary M33 X-7Eclipsing X-ray binary M33 X-7Pietsch et al. 2004, A&A 413, 879

Best fitting spectral models:Absorbed bremsstrahlung or disk blackbody

Eclipsing X-ray binary M33 X-7Eclipsing X-ray binary M33 X-7

First eclipsing black hole (high mass) X-ray binary ?

ChASeM33 lightcurve of X-7ChASeM33 lightcurve of X-7 Pietsch et al. 2006, ApJ 646, 420

Gemini North radial velocity curve: > 6.9 Msun black holeOrosz et al. 2007, ATel 977

ChASeM33 light curve of ChASeM33 light curve of [PMH2004] 47[PMH2004] 47

Pietsch et al. 2006, ATel 905

2nd eclipsingHMXB in M33

Orbital period1.73245 d

Similar to LMC X-4 orHer X-1

The Andromeda The Andromeda Galaxy M 31Galaxy M 31W. Pietsch, M. Freyberg, F. Haberl et.al. 2004, A&A 434, 483

• Similar analysis to M 33 based on archival data

• 856 sources in fields

• Hardness ratio and time variability

• classification and identification

M 31 centreM 31 centreAll 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

H. Stiele, W. Pietsch et al. 2007, in preparation

• Determine time variability between M 31 center pointings half a year apart

• Check classification of SNRs

• Classify new XRB candidate by time variability

Time variability of X-ray sources in the Time variability of X-ray sources in the M 31 centre fieldM 31 centre field

1035 1036 1037 1038 erg/s

Variable X-ray sources in the M 31 centre

W. Pietsch & F. Haberl 2005, A&A 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

XMM-Newton detection of type I XMM-Newton detection of type I X-ray bursts in M 31X-ray bursts in M 31

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

Observation c4 Jan 7, 2002

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

Rise time < 10 s Total 50 ctsMaximum duration < 20 s Max. rate 1.4±0.4ct/s Decay to backgr. ~150 s corresponds to 3.8 1038erg/sQuiescent luminosity ~5 1036erg/s (Eddington limit for H-poor matter)

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

– Sources within galaxy (all approximately at same distance)• X-ray binaries (XRBs) <hard>

– 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) <hard>

• Nuclear source • Ultraluminous X-ray sources• Diffuse emission in disk and halo

– Foreground stars– Galaxies, galaxy clusters and AGN in background <hard>

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

– Sources within galaxy (all approximately at same distance)• X-ray binaries (XRBs) <hard>

– 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) <hard>

• Nuclear source • Ultraluminous X-ray sources• Diffuse emission in disk and halo

– Foreground stars– Galaxies, galaxy clusters and AGN in background <hard>

Important Simbol-X parameters for nearby galaxy investigations:

Big field of view high resolution

Unexplored energy band!!! Discovery space for the unpredicted !!!