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

The Chandra view of Mrk 279

Elisa CostantiniSRON, National Institute for Space Research

Astronomical Institute Utrecht

5-7/10/2005 Warsaw warm absorber workshop 2

Outline Mrk 279 Chandra-LETGS observation

Emission spectrum • Broad lines• UV– X-rays modeling

Absorption components• Warm absorber• Redshift zero absorption

Conclusions

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Mrk 279 previous studyz = 0.0306ASCA (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

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LETGS observation of Mrk 279- 10-20th May 2003- 7 shots (30-100 ks)- Total exposure: 355 ks

- FUSE (91 ks) + HST (41.3 ks)Arav et al. 2004, 2005Gabel et al. 2005

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The first fit

Complex oxygen region:– Narrow emission lines (OVII f, OVIII Ly α)– Absorption lines OI-OVIII– Broad emission features OVII, OVIII

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X-rays broad lines in Sy 1 Broad emission lines

Iron K α 6.4 keV (Tanaka 1995)

OVII triplet (21.5-22.09 Å)(ngc5548 Steenbrugge et al. 2005)

OVIII Ly α (18.96 Å) (ngc4051 Ogle et al. 2004, Fenovcik et al. 2005)

NGC 5548

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X-rays broad lines in Sy 1 Broad emission lines

Iron K α 6.4 keV (Tanaka 1995)

OVII triplet (21.5-22.09 Å)(ngc5548 Steenbrugge et al. 2005)

OVIII Ly α (18.96 Å) (ngc4051 Ogle et al. 2004, Fenovcik et al. 2005)

Relativistic broadening

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UV broad linesGabel et al. 2005

FWHM=11000 km/s

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The LOC methodOne 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)

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The LOC method (2)

Transmitted

Reflected

Ingredients for the BLR:Log NH=23 cm-2

Cf =0.5

Log n = 8-12.5 cm-3

Log r = 15.2-17.5 cm

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FUSE+HST best fit:0.89

X-ray line luminosity !

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Where are the lines produced?BLR size: 6-17 ldays(Santos-Lleo et al. 2001)

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No strong evidence of :• highly ionized skin of the BLR• relativistically broadened profile of OVIII

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Warm absorber: the modelsSPEX (Kaastra 2001)

– SLAB: transmission from a thin layer. Parameters: ionic column densities, outflow velocity, line broadening

– XABS: fit with a pre-calculated grid of NH and ξ, gi ven a SED

relies on XSTAR or CloudyParameters: NH, ξ, outflow velocity, line broadening

– WARM: a continuos distribution of XABS

Parameters: outflow velocity, sigma, ξlow ξhigh

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Warm absorber: variabilityDifficult 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)

Yes ngc 4051 (Krongold et al. 2005)

0 days 10

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warm absorber variability

NH

Log ξ

Large error bars Large scatter in the ionization parameter

2.5

0.46

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The warm absorber (2)3 ionized warm absorbers intrinsic to Mrk 2792 absorbers in the Milky Way

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The nature of the wa in mrk 279

No pressure equilibrium continuous distribution ?

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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

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The Milky way ionized absorber

Blue wingv= - 87 km/sσ = 80 km/s

(Kaastra et al in prep.)

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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/ssolar metallicity

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ConclusionsBroad 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 BLRNo strong evidence of relativistic profilesWarm absorbers:3 main components, not variable, possibly in a continuous outflowz=0 absorption: most likely in the Milky Way