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XMM-Newton Observations of nearby edge-on Starburst Galaxies

XMM-Newton Observations of nearby edge-on Starburst Galaxies. Matthias Ehle XMM-Newton Science Operations Centre VilSpa, Spain European Space Agency (ESA), Research and Scientific Support Department, Science Operations and Data Systems Division major input from: Michael Dahlem (ATNF),

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XMM-Newton Observations of nearby edge-on Starburst Galaxies

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  1. XMM-Newton Observations of nearby edge-on Starburst Galaxies Matthias Ehle XMM-Newton Science Operations Centre VilSpa, Spain European Space Agency (ESA), Research and Scientific Support Department, Science Operations and Data Systems Division major input from:Michael Dahlem(ATNF), Elena Jimenez Bailon& Maria Santos Lleo(ESA, XMM-Newton SOC) Matthias Ehle - RSSD

  2. The Search for Galactic Halos To investigate different phases of complex halo ISM, we are conducting multi-wavelength observations Other members of the gang: • A.M. Read (Uni Leicester), T.J. Ponman (Uni. Birmingham), • J.M. Mas Hesse (CSIC-INTA), • M. Guainazzi (ESA, XMM-Newton), • T. Heckman, D.K. Strickland (Johns Hopkins Uni.), • K. Weaver (NASA/GSFC) • R.F. Haynes (ATNF, Uni. Tas.), J.S. Lazendic (ATNF,CfA), • S. Ryder (AAO), • D. Breitschwerdt (MPE), • U. Lisenfeld (Inst. Astrof. Andalucia) Matthias Ehle - RSSD

  3. The Search for Galactic Halos Main Goals: • galaxy sample of sufficient size to study dependence of (multi-wavelengths) halo properties on… • total SFR, • SFR per unit surface area, energy input rate: Ė / ASF proportional LFIR / ASF • interaction partners, nuclear activity • galaxy’s size, i.e. shape of its gravitational potential • interdependence of different components of halo ISM? • investigate metallicity of hot halo gas (X-ray spectroscopy) • chemical evolution of a galaxy • potential impact on enrichment of IGM • now let’s go and visit the X-ray zoo... • NGC 1511, NGC 1808, NGC 4666, NGC 3628 Matthias Ehle - RSSD

  4. background source? NGC 1511: The quest for hot gas in the halo (Dahlem et al., A&A 403, 547 (2003)) X-ray imagery: XMM-Newton, ~ 30 ks EPIC pn+MOS soft: 0.5-1.3 keV hard: 2.0-7.5 keV Matthias Ehle - RSSD

  5. NGC 1511: The quest for hot gas in the halo X-ray spectroscopywithXMM-Newton: (bright source excluded) • simple models do not fit: •  complex emission composition • best fit: (others are possible) • phabsmekal+phabs(mekal+powl) •  0.19 keV (12 % of total flux) • 0.59 keV (11 %) • photon index 1.4 (77 %) •  LX(0.2-12 keV) = 1.111040 erg s-1 • log(LFIR/LX) = 3.62 • typical for starburst galaxies •  LX,diffuse = 2.551039 erg s-1 • log(LFIR/LX,diffuse) = 4.25 • relatively low amount of diffuse • emission(see Read & Ponman 2001) Matthias Ehle - RSSD

  6. NGC 1511: The quest for hot gas in the halo XMM-Newton’s Optical monitor: • 2” FWHM; 17’x17’ FOV; V, B, U, and 3 UV filters (160-600 nm), two Grisms (V, UV, 0.5-1 nm resolution) UVM2 (centred at 230 nm) UVM2 plus EPIC 0.5-1.3 keV absorption due to dust lane Matthias Ehle - RSSD

  7. ATCA: 13 cm NGC 1511: The quest for hot gas in the halo Comparison with radio continuum data: (Dahlem et al. 2001) EPIC 0.5-1.3 keV Matthias Ehle - RSSD

  8. NGC 1511: The quest for hot gas in the halo Summary: • XMM-Newton observations reveal presence of previously unknown extended hot gas, partly extending out of disk plane, extra-planar emission also seen in radio continuum • emission distribution is asymmetric: bright in eastern half, where also radio continuum suggests highest level of star formation • spectral analysis shows complex emission composition • X-ray properties characterise NGC 1511 as starburst galaxy • UV, H, NIR suggest that NGC 1511 is heavily disturbed (by two small companions?)  not an ideal candidate to test halo properties dependence on star formation in underlying disk... Matthias Ehle - RSSD

  9. NGC 1808: Combined starburst/AGN activity (Jimenez Bailon et al., astro-ph/0301109;A&A, in prep.) High star-forming activity: • HII regions in 1 kpc circumnuclear region (Forbes `92)AgeSFR ~ 8-17 Myr (Kotilainen`96) • SNR population detected in IR and radio (Saikia `90) • starburst activity (and peculiar morphology) due to a recent interaction with NGC 1792 (Dahlem `90; Koribalski `93) Nuclear activity: starburst and/or AGN? • Analysis of optical emission lines (Kotilainen `96) and polarised light (Scarrott `93) point out presence of Seyfert 2 nucleus together with intense SF activity • ISO: only 10% of nuclear emission is due to stellar activity (Siebenmorgen 2001) • ROSAT data (Dahlem `94; Junkes `95) and ASCA (Awaki `96) can be explained assuming a hot plasma and/or SNR; other possibilities can not be ruled out • Ginga observations (Awaki `93) suggest NGC 1808 has obscure nucleus • Nuclear emission remains unclear but shows high contributions of star forming activity Matthias Ehle - RSSD

  10. X-ray: Chandra X-ray: pn H X-ray: EPIC, 36 ks NGC 1808: Spatial analysis of X-ray emission Peak position: • X-ray (XMM-Newton,Chandra (Zezas et al.), UV (XMM-Newton) and R-optical images are consistent: location of maximun luminosity corresponds to an unresolved point-like source UVW1 UVW2 Matthias Ehle - RSSD

  11. NGC 1808: Spatial analysis of X-ray emission Energy bands (pn): • non-nuclear sources detected at lower energies • nucleus visible in all energy range • 0.5-2 keV soft band: emission associated with star-formation activity Matthias Ehle - RSSD

  12. NGC 1808: Spectral analysis of EPIC-pn data bulk of X-ray emission originates from nuclear region: EPIC-pn spectrum of central 850 pc: best fit: phabs (zpow + vmekal) thermal components (which account for the main part of the soft X-ray emission), plus power law required to explain hard energy tail:  = 0.86 ± 0.07 NH,mekal= 2.1+0.5-0.21021 cm-2 kT = 0.57+0.02-0.05 keV [Ne] = 1.5+0.9-0.6 [Mg] = 2.0+0.9-0.6 [Si] = 1.6+0.9-0.6 [Fe] = 0.6+0.2-0.1 L0.24-10keV=1.6 ± 0.31040 erg s-1 Matthias Ehle - RSSD

  13. NGC 1808: Spectral analysis of RGS data • XMM-Newton RGS (0.35-2.5 keV) spectrum: • no continuum emission larger than noise, but emission lines visible • emission lines at wavelenghts and with relative ratios similar to strongest features identified in RGS data from prototypical starburst galaxy M82 (Read & Stevens 2002) • weak lines seen in M82 but not detected in NGC 1808: M82 is brighter so its RGS spectrum has better S/N •  soft X-ray spectrum in NGC 1808 is dominated by thermal emission from a starburst Matthias Ehle - RSSD

  14. NGC 4666: a “Superwind” galaxy (Ehle, Dahlem et al., A&A, in prep.) • FIR luminosity higher than for actively star-forming galaxies NGC 253 and NGC 4631  high global SFR in NGC 4666 • log (LFIR/LB) = 0.48 & FIR colour f60/f100 = 0.45  NGC 4666 is a typical FIR-selected galaxy(Lehnert & Heckman `95) good candidate for multi wavelength search for halo emission (cf. Dahlem et al. `95) • First evidence for existence of starburst driven galactic superwind in NGC 4666 given 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 extraplanar emission Matthias Ehle - RSSD

  15. ROSAT PSPC (Dahlem et al. `98) 0.25 keV, 48” FWHM XMM-EPIC, ~55 ks 0.2-0.5 keV, smoothed to 10” FWHM NGC 4666: a “Superwind” galaxy X-ray imaging results: ROSAT versus XMM-Newton Matthias Ehle - RSSD

  16. NGC 4666: a “Superwind” galaxy X-ray imaging results: XMM-Newton energy bands Matthias Ehle - RSSD

  17. XMM-EPIC: 0.5-0.9 keV NGC 4666: a “Superwind” galaxy Multi-wavelength (qualitative) comparison: • 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? HI observations (ongoing) Matthias Ehle - RSSD

  18. disk halo NGC 4666: Spectral analysis of EPIC-pn data diffuse X-ray emission from disk and halo regions (preliminary results): • best (not perfect!) fit: phabs (mekal + powerl) • halo fit improves with free Z...(~ 0.1 Zsolar), seems unphysical (starburst enriches outflowing material), wrong CIE assumption (see Breitschwerdt `03) • bulk of soft emission due to hot gas: • mekal contributes 60% (disk), 74% (halo) to soft 0.3-0.9 keV flux • in disk higher contribution due to powerl: unresolved point-like sources, XRBs • powerl contributes 87% (disk) and 59% (halo) to total 0.3-12 keV flux • higher gas temperature in the disk: • 0.29  0.01 keV (disk) • 0.21  0.01 keV (halo) Matthias Ehle - RSSD

  19. 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 • spectral analysis shows complex emission composition: fit with mekal (CIE) model NOT ok: Breitschwerdt (NIE) model needed? • X-ray properties confirm: superwind exists in NGC 4666 • interesting correlation of X-ray, H, polarization filaments: outflow cone & walls: energy densities to be compared... • ... Matthias Ehle - RSSD

  20. NGC 3628: outflow & a strange 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 nuclear X-ray source (unresolved with ROSAT): strong variability (faded by factor >27 between 1991 - 1994) variable obscuration of AGN or HXRB (>75 Msol black hole)? • Chandra (52 ks, Strickland et al. 2001): luminous source visible again, but 20” offset from nucleus • XMM-Newton (~50 ks): analysis started, some preliminary results... (Ehle, Read et al., A&A, in prep.) Matthias Ehle - RSSD

  21. 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 NGC 3628: outflow & halo emission ROSAT PSPC (Dahlem et al. `96) 0.75 keV, 48” FWHM Matthias Ehle - RSSD

  22. NGC 3628: central emission Chandra (Strickland et al. 2001) 0.3-8 keV, 1” FWHM XMM-EPIC 0.3-8 keV slightly smoothed Preliminary spectral fit to IXO: Matthias Ehle - RSSD

  23. The Search for Galactic Halos: Comments • high f60/f100 FIR colour (> 0.4): successful criterion for halo candidates (shown to work for radio halos, X-ray sample still small) • galaxies with highest Ė / ASF show most prominent radio halos; TBC for X-ray halos • Contradiction to Irwin et al. `99 ?: no such connection between radio halo and SF level in disk - BUT: different object classes (Sy-2 nuclei, magellanic irregulars, interacting galaxies, unresolved emission) • add HI observations (VLA &ATCA, ongoing)  info on inclination angle, intrinsic absorbing gas distribution & kinematics, search for extraplanar HI (tracers of tidal interactions) • all physically small galaxies (D25  20 kpc), even with f60 / f100 < 0.4,have prominent (radio) halos; low total mass  CR electrons (and hot gas?) escape easier from disks • spatial resolution & sensitivity of XMM-Newton allows detailed comparisons with optical/radio filaments (originating in strongest SF regions);  energy budget of different ISM components • spectral sensitivity allows separation of starburst/AGN & detailed study of hot gas (CIE versus NIE) • Final goal: to create galaxy sample of sufficient size to study dependence of halo properties on several parameters Matthias Ehle - RSSD

  24. NGC 4666 companion companion NGC 4668 (undet. ROSAT) NGC 4666: a “Superwind” galaxy HI (VLA) map(Walter et al., ApJ subm.)& 0.5-0.9 keV XMM-Newton EPIC Matthias Ehle - RSSD

  25. Chandra (Strickland et al. 2001) XMM-Newton pn best fit model: wabs  powl NH  FX,0.3-8keV FX,0.3-2keV F X,2-8keV Chandra: 8.0+1.2-1.11021 1.82+0.21-0.20 9.40 10-13 4.75 10-13 4.65 10-13 XMM-pn: 6.6+0.8-0.61021 1.74+0.10-0.09 8.49 10-13 4.00 10-13 4.49 10-13 NGC 3628: fit to the luminous source Matthias Ehle - RSSD

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