THE XMM-NEWTON SURVEYS OF THE LARGE (AND SMALL) MAGELLANIC CLOUD

Max-Planck-Institut für extraterrestrische Physik

Dublin, 17 June 2014

Frank Haberl

The XMM-Newton LMC-survey collaboration: P. Maggi, G. Vasilopoulos, A. Becker, D. Bomans, L. Bozzetto, Y.-H. Chu, J. Dickel, M. Ehle, M. Filipovic, D. Hatzidimitriou, P. Kavanagh, J. Ott, W. Pietsch, S. Points, M. Sasaki, S. Snowden, R. Sturm, R. Williams and the XMM-Newton SMC-survey collaboration: R. Sturm, J. Ballet, D. Bomans, D.A.H. Buckley, M.J. Coe, R. Corbet, M. Ehle, M.D. Filipovic, M. Gilfanov, D. Hatzidimitriou, N. La Palombara, S. Mereghetti, W. Pietsch, S. Snowden, A. Tiengo

The X-ray Universe 2014

• Einstein – 1st X-ray survey with imaging instruments ~100 discrete sources and large scale diffuse emission in the LMC (Long et al. 1981, Wang et al. 1991)

70 sources in the SMC (Wang & Wu 1992)

• ROSAT

All-sky survey (13x13 deg2 LMC field: Pietsch & Kahabka 1993)

Pointed observations with PSPC and HRI (LMC: Sasaki et al. 2000a, Haberl & Pietsch 1999; SMC: Sasaki et al. 2000b, Haberl et al. 1999, Kahabka et al. 1999) Also hot gas in SMC (Sasaki et al. 2002)

• ASCA SMC survey

High mass X-ray binary population (Yokogawa et al. 2003)

X-ray Surveys of the Magellanic CloudsXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

The MCs as seen by ROSAT

18 deg2

including southern pointings (Kahabka et al. 1999, Haberl et al. 2000)

59 deg2

750 sources (Haberl et al. 1999)

0.1-2.4 keV

PSPC pointings LMC SMC

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

MCELS (Winkler et al. 2005) Hα [SII] [OIII]

The XMM-Newton survey of the SMCXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

XMM-Newton 0.2-1.0 keV 1.0-2.0 keV 2.0-4.5 keV

The Small Magellanic CloudXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

XMM-Newton 0.2-1.0 keV 1.0-2.0 keV 2.0-4.5 keV

The Small Magellanic CloudXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

MCELS (Winkler et al. 2005) Hα [SII] [OIII]

The Large Magellanic CloudXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

XMM-Newton 0.2-1.0 keV 1.0-2.0 keV 2.0-4.5 keV

The Large Magellanic CloudXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

XMM-Newton 0.2-1.0 keV 1.0-2.0 keV 2.0-4.5 keV

The Large Magellanic CloudXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

Diffuse emission from the hot ISM (SMC)

XMM-Newton EPIC

0.2-0.5 keV 0.5-1.0 keV 1.0-2.0 keV

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

Diffuse emission from the hot ISM (SMC)

ROSAT PSPC

0.1-0.4 keV 0.5-0.9 keV 0.9-2.0 keV

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

Sasaki et al. 2002

XMM-Newton 0.2-1.0 keV 1.0-2.0 keV 2.0-4.5 keV

Analysis of the diffuse emission

SMC Detector X-ray Fore-/Background Soft-proton flares

12

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

XMM-Newton 0.2-1.0 keV 1.0-2.0 keV 2.0-4.5 keV

Analysis of the diffuse emission

SMC Detector X-ray Fore-/Background Soft-proton flares

13

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

Diffuse emission from the hot ISM (SMC)Temperature Luminosity

Surface brightness Column density

kT ≈ 0.2 keV Higher absorption in the SW Total luminosity: 7.1 x 1036 erg s-1

absorption corrected: 4.0 x 1037 erg s-1

(a factor of ~4 higher than from ROSAT due to higher absorption)

keV 1030 erg s-1 arcsec-2

10-18 erg cm-2 s-1 arcsec-2 1022 cm-2

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

Diffuse emission from the hot ISM (SMC)0.2-1.0 keV

Hα

H I

PhD thesis of Richard Sturm Sturm et al. in preparation

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

Supernova remnants - SMCSynoptic study of 13 known SNRs (van der Heyden et al. 2004,A&A 421, 1031)

X-ray morphology, spectra improved images pn and MOS out-of-time events subtracted (pn) detector background subtracted vignetting corrected a number of SNRs show larger extent (than in Badenes et al. 2010, MNRAS 407, 1301)

new candidates with low surface brightness and large extent complete sample down to a few 10-14 erg cm-2 s arcmin-2 Thermonuclear SN origin: Fe-rich: IKT 5, IKT 25, DEM S128, IKT 4? irregular morphology, small X-ray extent no SNR at position of IKT 7 (BeXRB) no detection of DEM S130, NS21, N83C Haberl et al. 2012, A&A 545, A128

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

Supernova remnants - LMCSNRs in the LMC survey J0508-6902 (Fe)

Bozzetto et al. 2014 J0508-6830 (Fe) J0511-6759 (Fe) J0514-6840 J0517-6759

Maggi et al. 2014 J0528-6727 (DEM L205)

Maggi et al. 2012 (Fe): X-ray spectra dominated by Fe L-shell lines Thermonuclear origin (Ia)

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

New LMC supernova remnants

E. Whelan et al. (poster D06) E. Whelan et al. (poster D06)

• Now more than 60 SNRs • Multi-λ studies → density, temperature, abundance, age… • XMM-Newton sensitive to the faint end of the population • LMC provides a variety of different ISM environments

Bozzetto et al. 2014

DEM L205

Maggi et al. 2012

MCSNR J0514-6840 MCSNR J0517-6759 Maggi et al. 2014:

0.3-0.7 keV 0.7-1.1 keV 1.1-4.2 keV

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

Fe-rich LMC supernova remnants

in preparation in preparation

Maggi et al. 2014, A&A 561, A76

vapec model: kT ≈ 0.7 keV Large Fe abundance

empty

empty XMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

X-ray spectra dominated by Fe-L emission lines Thermonuclear SN (Ia)

The evolution of type Ia SNRs in the LMC

Pierre Maggi

Borkowski et al. 2006

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

High mass X-ray binaries - SMC

63 pulsars

Knigge et al. 2011: Core collapse and electron capture supernovae Cheng et al. 2014: Two different accretion modes (disc accretion during type-II outburst and advection dominated)

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

𝒊 Energy band

1 (0.2 – 0.5) keV

2 (0.5 – 1.0) keV

3 (1.0 – 2.0) keV

4 (2.0 – 4.5) keV

5 (4.5 – 12.0) keV

Hardness ratios:

𝐻𝐻𝑖 =𝐻𝑖+1 − 𝐻𝑖𝐻𝑖+1 + 𝐻𝑖

⇒ 2711 hard sources ⇒ 945 very hard sources

Sturm et al. 2013, A&A, 558, 3

HMXBs – X-ray spectral classificationXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

𝒊 Energy band

1 (0.2 – 0.5) keV

2 (0.5 – 1.0) keV

3 (1.0 – 2.0) keV

4 (2.0 – 4.5) keV

5 (4.5 – 12.0) keV

Hardness ratios:

𝐻𝐻𝑖 =𝐻𝑖+1 − 𝐻𝑖𝐻𝑖+1 + 𝐻𝑖

⇒ 2711 hard sources ⇒ 945 very hard sources

Sturm et al. 2013, A&A, 558, 3

HMXBs – X-ray spectral classificationXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

⇒ 16 605 Be-star candidates in the XMM field Sturm et al. 2013, A&A, 558, 3

HMXBs - Optical counterpart , CMDXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

HMXBs – SMC luminosity function

𝒅𝒅𝒅𝒅

= �𝒅𝟏𝒅−𝜶𝟏 if 𝒅 ≤ 𝒅𝒃𝒅𝟐𝒅−𝜶𝟐 if 𝒅 > 𝒅𝒃

25

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

Sturm et al. 2013, A&A, 558, 3

High mass X-ray binaries - LMC

15 pulsars (11 Be)

8.04 s: Vasilopoulos et al. 2014 28.8 s: Vasilopoulos et al. 2013 168.8 s: Maggi et al. 2013

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

LXP 169: The first eclipsing BeXRBTwo XMM-Newton observations Spin period 169 s Powerlaw X-ray spectrum (photon index 0.84, 1.1) Optical counterpart: early type star

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

LXP 169: The first eclipsing BeXRBAn X-ray pulsar transiting in front of its Be companion star Transit every 24.33 days Transit profile varies with λ and time OGLE I-band Swift/UVOT uvw1-filter GROND g’,r’,i’,z’,J,H,K Be star eclipsed by NS + surrounding matter

Maggi et al. 2013, A&A 554, A1

XMM Surveys of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169

• Magellanic Clouds ideally suited for population studies (distance, foreground absorption)

• Flux limit of XMM-Newton surveys ̴10-14 erg cm-2 s-1 (5·1033 erg s-1) Very sensitive to soft extended emission

• SNR population studies High sensitivity for faint SNRs with soft spectra New faint remnants (10-14 erg cm-2 s-1 arcmin-2) Extended evolutionary sequence of SNRs with type Ia (thermonuclear) SN origin

• HMXBs Large population in the SMC Discovery of unique objects

SummaryXMM Surveys

of the MCs

Frank Haberl

X-ray Surveys

Summary

ROSAT

SNRs

LMC survey

Properties

SMC census

XMM-Newton

New SNRs

The hot ISM X-ray Images

Fe-rich

Morphology

Evolution of Ia

HMXBs Identification SMC logN–logS LMC LXP 169