xmm-newton 1 matthias ehle - rssd xmm-newton observations of nearby edge-on starburst galaxies...

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XMM-Newton 3 Matthias Ehle - RSSD 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 / A SF proportional L FIR / A SF –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

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XMM-Newton 1 Matthias Ehle - RSSD 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) XMM-Newton 2 Matthias Ehle - RSSD 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) XMM-Newton 3 Matthias Ehle - RSSD 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: / A SF proportional L FIR / A SF interaction partners, nuclear activity galaxys 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 lets go and visit the X-ray zoo... NGC 1511, NGC 1808, NGC 4666, NGC 3628 XMM-Newton 4 Matthias Ehle - RSSD 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: keV hard: keV background source? XMM-Newton 5 Matthias Ehle - RSSD 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 mekal+phabs (mekal+powl) 0.19 keV (12 % of total flux) 0.59 keV (11 %) photon index 1.4 (77 %) L X( keV) = 1.11 erg s -1 log(L FIR /L X ) = 3.62 typical for starburst galaxies L X,diffuse = 2.55 erg s -1 log(L FIR /L X,diffuse ) = 4.25 relatively low amount of diffuse emission (see Read & Ponman 2001) XMM-Newton 6 Matthias Ehle - RSSD NGC 1511: The quest for hot gas in the halo XMM-Newtons Optical monitor: 2 FWHM; 17x17 FOV; V, B, U, and 3 UV filters ( nm), two Grisms (V, UV, nm resolution) UVM2 (centred at 230 nm) UVM2 plus EPIC keV absorption due to dust lane XMM-Newton 7 Matthias Ehle - RSSD NGC 1511: The quest for hot gas in the halo Comparison with radio continuum data: (Dahlem et al. 2001) ATCA: 13 cm EPIC keV XMM-Newton 8 Matthias Ehle - RSSD 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... XMM-Newton 9 Matthias Ehle - RSSD NGC 1808: Combined starburst/AGN activity High star-forming activity: HII regions in 1 kpc circumnuclear region (Forbes `92) Age SFR ~ 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 (Jimenez Bailon et al., astro-ph/ ; A&A, in prep.) XMM-Newton 10 Matthias Ehle - RSSD 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 HHHH X-ray: EPIC, 36 ks X-ray: Chandra X-ray: pn UVW1UVW2 XMM-Newton 11 Matthias Ehle - RSSD NGC 1808: Spatial analysis of X-ray emission Energy bands (pn): non-nuclear sources detected at lower energies nucleus visible in all energy range keV soft band: emission associated with star-formation activity XMM-Newton 12 Matthias Ehle - RSSD = 0.86 0.07 N H,mekal = cm -2 kT = keV [Ne] = [Mg] = [Si] = [Fe] = 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: L keV =1.6 0.3 erg s -1 XMM-Newton 13 Matthias Ehle - RSSD XMM-Newton RGS ( 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 NGC 1808: Spectral analysis of RGS data XMM-Newton 14 Matthias Ehle - RSSD NGC 4666: a Superwind galaxy 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 (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 (Ehle, Dahlem et al., A&A, in prep.) XMM-Newton 15 Matthias Ehle - RSSD X-ray imaging results: ROSAT versus XMM-Newton ROSAT PSPC (Dahlem et al. `98) 0.25 keV, 48 FWHM XMM-EPIC, ~55 ks keV, smoothed to 10 FWHM NGC 4666: a Superwind galaxy XMM-Newton 16 Matthias Ehle - RSSD NGC 4666: a Superwind galaxy X-ray imaging results: XMM-Newton energy bands XMM-Newton 17 Matthias Ehle - RSSD NGC 4666: a Superwind galaxy Multi-wavelength (qualitative) comparison: 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? HI observations HI observations (ongoing) XMM-EPIC: keV XMM-Newton 18 Matthias Ehle - RSSD 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 Z solar ), 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 keV flux in disk higher contribution due to powerl: unresolved point-like sources, XRBs powerl contributes 87% (disk) and 59% (halo) to total keV flux higher gas temperature in the disk: 0.29 0.01 keV (disk) 0.21 0.01 keV (halo) disk halo XMM-Newton 19 Matthias Ehle - RSSD 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...... XMM-Newton 20 Matthias Ehle - RSSD 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 ) variable obscuration of AGN or HXRB (>75 M sol 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.) XMM-Newton 21 Matthias Ehle - RSSD NGC 3628: outflow & halo emission ROSAT PSPC (Dahlem et al. `96) 0.75 keV, 48 FWHM XMM-EPIC (plus DSS contours) , , keV, 10 FWHM XMM-EPIC (plus DSS contours) , , keV, 10 FWHM XMM-Newton 22 Matthias Ehle - RSSD NGC 3628: central emission Chandra () Chandra (Strickland et al. 2001) keV, 1 FWHM XMM-EPIC keV slightly smoothed Preliminary spectral fit to IXO: XMM-Newton 23 Matthias Ehle - RSSD The Search for Galactic Halos: Comments high f 60 /f 100 FIR colour (> 0.4): successful criterion for halo candidates (shown to work for radio halos, X-ray sample still small) galaxies with highest / A SF 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 (D 25 20 kpc), even with f 60 / f 100 < 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 XMM-Newton 24 Matthias Ehle - RSSD NGC 4666 NGC 4668 (undet. ROSAT) companion companion NGC 4666: a Superwind galaxy HI (VLA) map & keV XMM-Newton EPIC HI (VLA) map (Walter et al., ApJ subm.) & keV XMM-Newton EPIC XMM-Newton 25 Matthias Ehle - RSSD NGC 3628: fit to the luminous source Chandra () Chandra (Strickland et al. 2001) XMM-Newton pn best fit model: wabs powl N H F X,0.3-8keV F X,0.3-2keV F X,2-8keV Chandra: XMM-pn: