1. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 1 XMM-Newton SOC, ESAC Hot gaseous Halos & their Dependence on Activity in the underlying galactic Disks Matthias Ehle European Space Astronomy Centre (ESAC), Madrid, Spain XMM-Newton Science Operations Centre European Space Agency (ESA), Research and Scientific Support Department, Science Operations and Data Systems Division Michael Dahlem CSIRO/ATNF - Paul Wild Observatory, Narrabri, Australia

2. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 2 XMM-Newton SOC, ESAC Intro: Co-Investigators List of (some) collaborators: A. M. Read (Uni. Leicester), T. J. Ponman (Uni. Birmingham) D. Breitschwerdt (Inst. f. Astron., Uni. of Vienna) S. Ryder (AAO) U. Lisenfeld (Inst. Astrof. Andalucia) T. Heckman, D. K. Strickland (Johns Hopkins Uni.) K. Weaver (NASA/GSFC) F. Walter (NRAO)

3. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 3 XMM-Newton SOC, ESAC Intro: Motivation We want to know… –How is the IGM fed with metals? –Do star formation-driven galactic outflows play a significant role? –How do SF-driven outflows work? –How are gaseous halos energised? –Is there a direct link between galactic disk activity and halo (existence and properties)? –How much energy is required to initiate disk-halo interactions?

4. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 4 XMM-Newton SOC, ESAC Intro: Main Goals Build galaxy sample of sufficient size to study dependence of halo properties on… –total SFR –SFR per unit surface area (or take into account volume filling factor of HII regions); energy input rate: Ė A tot  Ė / A SF proportional to L FIR / A SF Study interdependence of different components of halo ISM: –spatial correlation? –energy budget / equilibrium? Caveats: –interaction partners –galaxy’s size, i.e. shape of its gravitational potential –nuclear activity

5. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 5 XMM-Newton SOC, ESAC Intro: Status 2004 Halos break off further inwards than underlying disks. Ė a tot can quantify Norman & Ikeuchi’s “breakout condition” for the creation of chimneys. Same rules apply for archetypical starburst galaxies and systems with widespread SF. Many more gaseous halos detected over past decade: –In H , radio continuum and/or X-ray emission (Rossa, Dettmar, Rand, Irwin, Strickland + others) –Progress on X-ray imaging (XMM-Newton, Chandra; Strickland, Read, Bregman, Pietsch, Vogler + others) –First detections of HI in galaxy halos (Swaters, Irwin, Fraternali + others) –New results presented at this (and Dwingeloo June ’04) conference…

6. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 6 XMM-Newton SOC, ESAC Method: Multi-wavelength Observations multi-wavelength study: –Tracers of SF in galactic disk: FIR continuum (selection criteria) H   warm ionized gas, SF regions thermal radio continuum ( < a few cm) –Tracers of galactic halos: H  : spurs & filaments non-thermal radio continuum ( : cm – dm)  cosmic rays & B-fields radio lines: HI, CO  cold, neutral gas: dynamics, inclination, outflow? X-rays –last (but not least) X-rays …

7. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 7 XMM-Newton SOC, ESAC Method: X-rays X-rays: –Imaging  disc & halo emission, existence & distribution of extra-planar hot gas –Timing  variability of emission (source identification) –Spectroscopy  origin of emission: individual sources and/or hot gas nuclear or extended starburst, AGN? temperature, metallicity of hot gas –(chemical) evolution of a galaxy –potential impact on enrichment of IGM Strengths of XMM-Newton –a lot of photons –High resolution soft X-ray spectroscopy: not-so-bright objects Will show three beasts from the (X-ray) zoo... –NGC 1511 (news from the radio), NGC 4666, NGC 3628 –NGC 1511 (X-ray halo detected) Dahlem, Ehle et al., A&A 403, 547 (2003) –NGC 1808 (nuclear starburst/AGN) Jimenez Bailon et al., astro-ph/0301109, A&A in prep. –NGC 7090 observed May 2004

8. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 8 XMM-Newton SOC, ESAC NGC 1511: The quest for hot gas in the halo Comparison with radio continuum data : ATCA: 13 cm ATCA: 13 cm (Dahlem et al. 2001, 2004 (subm., improved)) EPIC 0.5-1.3 keV A&A 403, 547 (2003)

9. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 9 XMM-Newton SOC, ESAC NGC 1511: The quest for hot gas in the halo X-ray spectroscopy with XMM-Newton: (bright source excluded) simple models do not fit:  complex emission composition best fit: (others are possible) phabs fg (mekal 1 + phabs (mekal 2 + powerl))  0.19 keV (12 % of total flux) 0.59 keV (11 %) photon index 1.4 (77 %)  L X(0.2-12 keV) = 1.11  10 40 erg s -1 log(L FIR /L X ) = 3.62 typical for starburst galaxies  L X,diffuse = 2.55  10 39 erg s -1 log(L FIR /L X,diffuse ) = 4.25 relatively low amount of diffuse emission (see Read & Ponman 2001)

10. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 10 XMM-Newton SOC, ESAC NGC 1511: The quest for hot gas in the halo Comparison with HI: ATCA: ATCA: (Dahlem et al. 2004, subm.)

11. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 11 XMM-Newton SOC, ESAC NGC 1511: The quest for hot gas in the halo Summary: XMM-Newton revealed previously unknown extended hot gas, partly extending out of disk plane, extra-planar emission also in radio continuum spectral analysis: complex emission composition X-ray properties characterise NGC 1511 as starburst galaxy not an ideal candidateUV, H , NIR, esp. HI suggest: NGC 1511 heavily disturbed (by two small companions)  not an ideal candidate to test halo properties depending on star formation in underlying disk...

12. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 12 XMM-Newton SOC, ESAC NGC 4666: X-rays from a “Superwind” galaxy State of knowledge before XMM-Newton: FIR luminosity higher than for actively star-forming galaxies NGC 253 and NGC 4631  high global SFR in NGC 4666 log (L FIR /L B ) = 0.48 & FIR colour f 60 /f 100 = 0.45  NGC 4666 is a typical FIR-selected galaxy (Lehnert & Heckman `95)  good candidate for multi wavelength search for halo emission Dahlem et al. `97First evidence for existence of starburst driven galactic superwind in NGC 4666 reported in Dahlem et al. `97: –optical emission line imagery: filaments –optical line diagnostics: shocks as main heating source –radio continuum maps: halo detected –radio polarization data: B-fields follow flow or allow it (?) –X-rays: ROSAT PSPC: soft extended extra-planar emission paper on X-ray results: Ehle et al. A&A (in prep.)

13. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 13 XMM-Newton SOC, ESAC X-ray imaging results: ROSAT versus XMM-Newton ROSAT PSPC ROSAT PSPC (Dahlem et al. `98) 0.25 keV, 48” FWHMXMM-EPIC 0.2-0.5 keV, smoothed to 10” FWHM NGC 4666: X-rays from a “Superwind” galaxy

14. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 14 XMM-Newton SOC, ESAC NGC 4666: X-rays from a “Superwind” galaxy XMM-Newton energy bands

15. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 15 XMM-Newton SOC, ESAC Radio continuum & H  Radio continuum & H  (Dahlem et al. `97): clear detection of radio halo (6, 20 cm) spectral steepening away from disk outflow cone from central starburst (radial diameter 6.5 kpc), traced by optical filaments up to 7.5 kpc above disk polarized radio spurs: outer wall of outflow cone? vertical B-fields: pushed out by superwind, or poloidal dynamo field? NGC 4666: X-rays from a “Superwind” galaxy Multi-wavelength (qualitative) comparison: Radio continuum, B-fields, H  HI observations XMM-EPIC: 0.5-0.9 keV

16. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 16 XMM-Newton SOC, ESAC NGC 4666: Spectral analysis of EPIC-pn data Disk: 0.18 & 0.54 keV fit model: phabs fg (mekal 1 + phabs (mekal 2 + powerl)) lower Halo: cf. Disk upper Halo: no strong need for 2 nd mekal: single Temp. Fit: 0.23 keV halo fit improves with free Z...(~ 0.1-0.3 Z solar ), seems unphysical (starburst enriches out-flowing material) –wrong CIE assumption (Breitschwerdt 2003), TBC bulk of soft emission due to hot gas: mekal contribution –0.3-0.9 keV flux: 72% (disk), 69% (lower), 92% (upper halo) mekal 2 (high T2) contribution decreases in upper halo: –fluxT1/fluxT2: 1.12 (disk), 0.72 (lower), 6.07 (upper halo) in disk & lower halo higher contribution due to powerl: unresolved point-like sources, XRBs –0.3-12 keV flux: 81% (disk), 80% (lower), 56% (upper halo)

17. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 17 XMM-Newton SOC, ESAC Summary: Characteristics of diffuse emission components NGC 4666: Spectral analysis of EPIC-pn data L X =  (T)  n e n H dV   (T) n e 2  V geom In general: energy density of B-field predominant: channelling the outflow?In general: energy density of B-field predominant: channelling the outflow? Lower halo: higher thermal energy density  outflow possible…Lower halo: higher thermal energy density  outflow possible…

18. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 18 XMM-Newton SOC, ESAC NGC 4666: a “Superwind” galaxy Summary: XMM-Newton observations reveal huge, structured hot gas halo, on both sides of disk; southern soft emission absorbed due to inclined disk X-ray properties confirm: superwind exists in NGC 4666 HI shows: starburst probably triggered due to tidal interactions interesting correlation of X-ray, H , polarization filaments: outflow cone & walls? comparison of energy densities: B-fields important plasma  1 spectral analysis shows complex emission composition: fit with mekal (CIE) model NOT unambiguous: NIE-model currently under testing

19. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 19 XMM-Newton SOC, ESAC NGC 3628: outflow & a very bright source NGC 3628 is interacting member of Leo Triplet collimated outflow from starburst nucleus detected by Einstein (Fabbiano et al `90) and X-ray ‘halo’ confirmed by ROSAT (Dahlem et al. `96) strange central X-ray source (unresolved with ROSAT): strong variability (faded by factor >27 between 1991 - 1994) variable obscuration of AGN or HXRB (>75 M sun black hole)? Chandra (52 ksec, Strickland et al. 2001 ): luminous source visible again, but 20” offset from nucleus XMM-Newton (~50 ksec):XMM-Newton (~50 ksec): analysis started, some preliminary results... Ehle, Read et al., A&A (in prep.)

20. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 20 XMM-Newton SOC, ESAC NGC 3628: outflow & halo emission ROSAT PSPC (Dahlem et al. `96) 0.75 keV, 48” FWHM XMM-EPIC (plus DSS contours) 0.3-0.5, 0.5-0.9, 0.9-2 keV, 10” FWHM XMM-EPIC (plus DSS contours) 0.3-0.5, 0.5-0.9, 0.9-2 keV, 10” FWHM Overlay with VLT-FORS2:

21. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 21 XMM-Newton SOC, ESAC NGC 3628: central emission Chandra () Chandra (Strickland et al. 2001) 0.3-8 keV, 1” FWHM XMM-EPIC 0.3-8 keV slightly smoothed Preliminary spectral fit to IXO:

22. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 22 XMM-Newton SOC, ESAC Summary & Outlook high f 60 /f 100 FIR colour (> 0.4): successful criterion for halo candidates (shown for radio halos, X-ray sample still small, but promising…), main targets: M82, NGC 3175, NGC 4666, NGC 4700, NGC 7090, NGC 7462 galaxies with highest Ė A tot  Ė / A SF show ‘most prominent’ radio halos; X-ray halos, too (details still to be quantified) High spatial resolution & sensitivity of XMM-Newton is important: –disentangle starburst/AGN/point-like sources/diffuse/disk/halo emission –detailed spatial comparison with optical/radio/B-field filaments (originating in strongest SF regions) –spectral sensitivity allows detailed study of hot gas (CIE vs. NIE, T, Z, n e,…)  energy budget of different ISM components Search for other extra-planar phases of the ISM, e.g. HI (Dahlem, Ehle et al., A&A, subm.) Investigate influence of more parameters, such as galaxy mass, on halo properties. Many thanks for your attention…

23. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 23 XMM-Newton SOC, ESAC NGC 4666 NGC 4668 (undet. ROSAT) companion companion NGC 4666: a “Superwind” galaxy HI (VLA) map & 0.5-0.9 keV XMM-Newton EPIC HI (VLA) map (Walter et al., ‘04) & 0.5-0.9 keV XMM-Newton EPIC Prominent tidal arms Interacting with NGC 4668 prev. unknown dwarf companions  Starburst activity probably caused by interaction

24. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 24 XMM-Newton SOC, ESAC NGC 3628: ejection associated with Quasars? XMM-EPIC 0.5-0.9 keV over VLT-FORS2 No connection between X-ray filament & QSOs  Arp et al., 2002XMM-EPIC 0.5-0.9 keV over H  (Rossa & Dettmar ’03) Correlation of X-ray filament & H  plume?

25. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 25 XMM-Newton SOC, ESAC NGC 3628: fit to the luminous source Chandra () Chandra (Strickland et al. 2001) XMM-Newton pn best fit model: wabs  powerl N H  F X,0.3-8keV F X,0.3-2keV F X,2-8keV Chandra: 8.0 +1.2 -1.1 10 21 1.82 +0.21 -0.20 9.40 10 -13 4.75 10 -13 4.65 10 -13 XMM-pn: 6.6 +0.8 -0.6 10 21 1.74 +0.10 -0.09 8.49 10 -13 4.00 10 -13 4.49 10 -13

26. Matthias Ehle The Environments of Galaxies Crete, 9-13 August 2004 26 XMM-Newton SOC, ESAC NGC 4666: X-rays from a “Superwind” galaxy Multi-wavelength (qualitative) comparison: CO(1  0) Multi-wavelength (qualitative) comparison: CO(1  0) (Walter et al. 2004) … and a rather hard X-ray source: –another ultra-luminous source (ULX)? –powl fit; 9 10 39 ergs/s –Pakull ‘04: ULX often surrounded by large ionized nebulae with bubble-like morphology An expanding molecular supershell... –near foot point of H  spur –diameter ~ 1.3 kpc –powered by star formation at centre?