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The Chandra view of Mrk 279. Elisa Costantini SRON, National Institute for Space Research Astronomical Institute Utrecht. Outline. Mrk 279 Chandra-LETGS observation Emission spectrum Broad lines UV– X-rays modeling Absorption components Warm absorber Redshift zero absorption

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the chandra view of mrk 279

The Chandra view of Mrk 279

Elisa Costantini

SRON, National Institute for Space Research

Astronomical Institute Utrecht

outline
Outline

Mrk 279 Chandra-LETGS observation

Emission spectrum

  • Broad lines
  • UV– X-rays modeling

Absorption components

  • Warm absorber
  • Redshift zero absorption

Conclusions

Warsaw warm absorber workshop

mrk 279 previous study
Mrk 279 previous study
  • z = 0.0306
  • 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

Warsaw warm absorber workshop

letgs observation of mrk 279
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, 2005
    • Gabel et al. 2005

Warsaw warm absorber workshop

the first fit
The first fit
  • Complex oxygen region:
    • Narrow emission lines

(OVII f, OVIII Ly α)

    • Absorption lines  OI-OVIII
    • Broad emission features OVII, OVIII

Warsaw warm absorber workshop

x rays broad lines in sy 1
X-rays broad lines in Sy 1

NGC 5548

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)

Warsaw warm absorber workshop

x rays broad lines in sy 11
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

Warsaw warm absorber workshop

uv broad lines
UV broad lines

Gabel et al. 2005

FWHM=11000 km/s

Warsaw warm absorber workshop

the loc method
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)

Warsaw warm absorber workshop

the loc method 2

Reflected

Transmitted

The LOC method (2)

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

Warsaw warm absorber workshop

slide11
FUSE+HST best fit:

 = 0.89

  • = 0.97

X-ray line luminosity !

Warsaw warm absorber workshop

where are the lines produced
Where are the lines produced?

BLR size: 6-17 ldays

(Santos-Lleo et al. 2001)

Warsaw warm absorber workshop

slide13

No strong evidence of :

  • highly ionized skin of the BLR
  • relativistically broadened profile of OVIII

Warsaw warm absorber workshop

warm absorber the models
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 NH and ξ, gi ven a SED

relies on XSTAR or Cloudy

Parameters: NH, ξ, outflow velocity, line broadening

    • WARM: a continuos distribution of XABS

Parameters: outflow velocity, sigma, ξlowξhigh

Warsaw warm absorber workshop

warm absorber variability
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)

Yes ngc 4051 (Krongold et al. 2005)

0 days 10

Warsaw warm absorber workshop

warm absorber variability1
warm absorber variability

Logξ

2.5

0.46

NH

  • Large error bars
  • Large scatter in the ionization parameter

Warsaw warm absorber workshop

the warm absorber 2
The warm absorber (2)

3 ionized warm absorbers intrinsic to Mrk 279

2 absorbers in the Milky Way

Warsaw warm absorber workshop

the nature of the wa in mrk 279
The nature of the wa in mrk 279

No pressure equilibrium  continuous distribution ?

Warsaw warm absorber workshop

continuous vs clumpy wa
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

Warsaw warm absorber workshop

the milky way ionized absorber
The Milky way ionized absorber

Blue wing

v= - 87 km/s

σ = 80 km/s

(Kaastra et al in prep.)

Warsaw warm absorber workshop

z 0 absorber interpretation
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

Warsaw warm absorber workshop

conclusions
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

Warsaw warm absorber workshop