The Chandra view of Mrk 279 Elisa Costantini SRON, National Institute for Space Research Astronomical Institute Utrecht

5-7/10/2005Warsaw warm absorber workshop2 Outline Mrk 279 Chandra-LETGS observation Emission spectrum Broad lines UV– X-rays modeling Absorption components Warm absorber Redshift zero absorption Conclusions

5-7/10/2005Warsaw warm absorber workshop3 Mrk 279 previous study z = ASCA (Weaver et al. 2001) –Variable iron line at 6.4 keV On the line of sight of ionized gas at z=0 (Savage et al. 2003) HTS+FUSE+Chandra HETGS (Scott et al. 2004) –4 absorption systems from the host galaxy –1 warm absorber

5-7/10/2005Warsaw warm absorber workshop4 LETGS observation of Mrk th May shots ( ks) - Total exposure: 355 ks - FUSE (91 ks) + HST (41.3 ks) Arav et al. 2004, 2005 Gabel et al. 2005

5-7/10/2005Warsaw warm absorber workshop5 The first fit Complex oxygen region: –Narrow emission lines (OVII f, OVIII Ly α) –Absorption lines  OI-OVIII –Broad emission features OVII, OVIII

5-7/10/2005Warsaw warm absorber workshop6 X-rays broad lines in Sy 1 Broad emission lines  Iron K α 6.4 keV (Tanaka 1995) OVII triplet ( Å) (ngc5548 Steenbrugge et al. 2005) OVIII Ly α (18.96 Å) (ngc4051 Ogle et al. 2004, Fenovcik et al. 2005) NGC 5548

5-7/10/2005Warsaw warm absorber workshop7 X-rays broad lines in Sy 1 Broad emission lines  Iron K α 6.4 keV (Tanaka 1995) OVII triplet ( Å) (ngc5548 Steenbrugge et al. 2005) OVIII Ly α (18.96 Å) (ngc4051 Ogle et al. 2004, Fenovcik et al. 2005) Relativistic broadening

5-7/10/2005Warsaw warm absorber workshop8 UV broad lines Gabel et al FWHM=11000 km/s

5-7/10/2005Warsaw warm absorber workshop9 The LOC method One component of ionized emitting gas is inadequate to describe emission.  BLR as a distribution of clouds with different density, distance, column density, and covering factor. (Baldwin et al. 1995, Ferland et al.) The Locally Optimally emitting Cloud (LOC)  Successfully applied to NGC 5548 (Korista & Goad 2000)

5-7/10/2005Warsaw warm absorber workshop10 The LOC method (2) Transmitted Reflected Ingredients for the BLR: Log N H =23 cm -2 C f =0.5 Log n = cm -3 Log r = cm

5-7/10/2005Warsaw warm absorber workshop11 FUSE+HST best fit:  0.89   X-ray line luminosity !

5-7/10/2005Warsaw warm absorber workshop12 Where are the lines produced? BLR size: 6-17 ldays (Santos-Lleo et al. 2001)

5-7/10/2005Warsaw warm absorber workshop13 No strong evidence of : highly ionized skin of the BLR relativistically broadened profile of OVIII

5-7/10/2005Warsaw warm absorber workshop14 Warm absorber: the models SPEX (Kaastra 2001) –SLAB: transmission from a thin layer. Parameters: ionic column densities, outflow velocity, line broadening –XABS: fit with a pre-calculated grid of N H and ξ, gi ven a SED relies on XSTAR or Cloudy Parameters: N H, ξ, outflow velocity, line broadening –WARM: a continuos distribution of XABS Parameters: outflow velocity, sigma, ξ low ξ high

5-7/10/2005Warsaw warm absorber workshop15 Warm absorber: variability Difficult issue because: –High S/N –High resolution –Sufficient flux amplitude variation Long time scale variation: e.g.ngc 3516 (Turner et al.2005) ngc 4151 (Kraemer et al. 2005) Short time scale variation: No ngc 5548 (Steenbrugge et al. 2005) ngc 3783 (Netzer et al. 2003) Yesngc 4051 (Krongold et al. 2005) 0 days 10

5-7/10/2005Warsaw warm absorber workshop16 warm absorber variability NHNH Log ξ Large error bars Large scatter in the ionization parameter

5-7/10/2005Warsaw warm absorber workshop17 The warm absorber (2) 3 ionized warm absorbers intrinsic to Mrk absorbers in the Milky Way

5-7/10/2005Warsaw warm absorber workshop18 The nature of the wa in mrk 279 No pressure equilibrium  continuous distribution ?

5-7/10/2005Warsaw warm absorber workshop19 Continuous vs clumpy wa Phases in pressure equilibrium –NGC 3783 (Netzer et al. 2003, –Krongold et al. 2003) Prompt reaction to flux variation Continuous distribution –NGC 4051 (Ogle et al. 2004) –NGC 5548 (Steenbrugge et al. 2005) NGC5548

5-7/10/2005Warsaw warm absorber workshop20 The Milky way ionized absorber Blue wing v= - 87 km/s σ = 80 km/s (Kaastra et al in prep.)

5-7/10/2005Warsaw warm absorber workshop21 Z=0 absorber: interpretation predicted EW(OVI)X =0.74 mÅ, consistent with non detection if OVII were connected with the narrow UV component  deep OVII edge which is not observed Global UV-X model: collisionally ionized absorber Winning interpretation: HVC complex C/K v= -(100-55) km/s solar metallicity

5-7/10/2005Warsaw warm absorber workshop22 Conclusions Broad lines: HST + FUSE  BLR lines in X-rays  independent constraints to the X-ray spectral fit. No strong evidence of a highly ionized skin of the BLR No strong evidence of relativistic profiles Warm absorbers: 3 main components, not variable, possibly in a continuous outflow z=0 absorption: most likely in the Milky Way