WHAT HAVE WE LEARNED FROM THE XMM- NEWTON … · The XMM-Newton survey of the SMC ... Maggi et al....
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Transcript of WHAT HAVE WE LEARNED FROM THE XMM- NEWTON … · The XMM-Newton survey of the SMC ... Maggi et al....
![Page 1: WHAT HAVE WE LEARNED FROM THE XMM- NEWTON … · The XMM-Newton survey of the SMC ... Maggi et al. 2014 J0528-6727 (DEM L205) Maggi et al. 2012 (Fe): ... Questions for the next decade:](https://reader034.fdocuments.in/reader034/viewer/2022051206/5b0862987f8b9a56408e71a6/html5/thumbnails/1.jpg)
WHAT HAVE WE LEARNED FROM THE XMM-NEWTON SURVEYS OF LOCAL GROUP GALAXIES?
Max-Planck-Institut für extraterrestrische Physik
ESAC, Madrid, 2016 May 11
Frank Haberl
XMM-Newton: The Next Decade
• Accretion onto compact objects
• Supernova remnants
• The hot interstellar medium
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• The Small Magellanic CloudA unique population of high-mass X-ray binaries
• The Large Magellanic CloudSupernova remnants
• The Andromeda galaxy (M31)Classical Novae as supersoft X-ray sources
• The Triangulum galaxy (M33)Supernova remnants
• The Milky WayGalactic centre scan
XMM-Newton Surveys of Local Group Galaxies
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The XMM-Newton survey of the SMC
30 survey fields (May 2009 – Mar. 2010)1 Ms+ archival observations5.5 square degrees (60% >10 ks exposure)flux limit 10-14 erg cm-2 s-1 (5⋅1033 erg s-1)
0.2-1.0 keV1.0-2.0 keV2.0-4.5 keV
EPIC pn and MOSdetector-background subtractedvignetting corrected
Haberl et al. 2012, Sturm et al. 2013
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High mass X-ray binaries in the SMC
40 new HMXB candidates(15-20 chance coincidences)147 (candidate) HMXBs in literature120 reliable Be/X-ray binaries63 pulsarspulsars/‘non-pulsars’ ≈ 1
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High mass X-ray binaries in the SMC
63 pulsars
• Knigge et al. 2011: Two different types of SNe1) Capture of electrons by a Ne/Mg nuclei in a lower-mass O/Ne/Mg core: short spin-periods, short orbital periods, low eccentricities2) Iron-core collapse of high-mass star
• Cheng et al. 2014: Two different accretion modes1) disc accretion during type-II outbursts 2) advection dominated/quasi-spherical accretion in case of normal (type I) outbursts
• Variability distribution for pulsars and ‘non-pulsars are consistent
• Long periods expected for non-pulsars• Alignment of rotation / magnetic axes?
Haberl & Sturm 2016
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0.2-1.0 keV1.0-2.0 keV2.0-4.5 keV
XMM-Newton Survey of the Large Magellanic Cloud
70 survey fields2 Ms(Dec. 2011 – Mar. 2014)+ archival observations10 square degrees
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Supernova remnants in the LMC
SNRs in the LMC survey
J0508-6902 (Fe)Bozzetto et al. 2014
J0508-6830 (Fe)J0511-6759 (Fe)J0514-6840J0517-6759
Maggi et al. 2014J0528-6727 (DEM L205)
Maggi et al. 2012(Fe):X-ray spectra dominated by Fe L-shell linesThermonuclear origin (Ia)
Faint/X-ray soft SNRs cannot be observed in the Galaxy
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New LMC supernova remnants
Kavanagh et al. 2016 Kavanagh et al. 2015
• Now 59 confirmed SNRs, 51 covered by XMM-Newton• 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• NCC/NIa = 1.35 (+0.11/-0.24), lower than derived from local SNe and galaxy cluster abundances
missing CC SNe in superbubbles? More likely consequence of SFH of the LMC
Bozzetto et al. 2014
DEM L205
Maggi et al. 2012
MCSNR J0514-6840 MCSNR J0517-6759
Maggi et al. 2014:
0.3-0.7 keV0.7-1.1 keV1.1-4.2 keV
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The evolution of type Ia SNRs in the LMC
Maggi et al. 2016
Borkowski et al. 2006
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Diffuse emission from the hot ISM in the SMC
0.2-1.0 keV
Hα
H I
PhD thesis R. Sturm
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Ponti +15
Hot plasma filling the GC Radio Lobe?
Ponti et al. 2015
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➜ Imaging with exquisite detail the center of a quiescent galaxy
Su et al. 2010
FERMI BUBBLES
A connection to the Fermi bubbles?
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XMM-Newton Observations of the Local Group
Extended our knowledge on the X-ray source populations
Different source classes dominate depending of SFHHelp to understand the unresolved X-ray emission from more distant galaxies
Prepare for future missions like Athena
Questions for the next decade:
HMXBs in SMC
• Intrinsic ratio of pulsars / non-pulsars (∢ rotation and magnetic axis)?
• Bimodal spin period distribution, maximum spin period ?
→ Extended monitoring, long observations (+EPIC FoV)
SNRs in the LMC
• Evolutionary sequence of type Ia SNRs
• More SNRs in supergiant shells ?
→ Larger coverage, deep observations of faint SNRs (+EPIC FoV, soft sensitivity)
Hot gas and outflows
• SMC, Galactic Centre – other?
→ Larger, deeper coverage (+EPIC FoV, soft sensitivity)
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THANKS TO
SMC-survey:
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
LMC-survey:
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
Galactic Centre:
G. Ponti, M.R. Morris, R. Terrier, R. Sturm, M. Clavel, S. Soldi, A. Goldwurm, P. Predehl, K. Nandra, G. Belanger, R.S. Warwick, V. Tatischeff