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The Chandra view of Mrk 279

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The Chandra view of Mrk 279. Elisa Costantini. SRON, National Institute for Space Research ... Successfully applied to NGC 5548 (Korista & Goad 2000) 5-7/10/2005 ... – PowerPoint PPT presentation

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Title: The Chandra view of Mrk 279


1
The Chandra view of Mrk 279
  • Elisa Costantini
  • SRON, National Institute for Space Research
  • Astronomical Institute Utrecht

2
Outline
  • Mrk 279 Chandra-LETGS observation
  • Emission spectrum
  • Broad lines
  • UV X-rays modeling
  • Absorption components
  • Warm absorber
  • Redshift zero absorption
  • Conclusions

3
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 z0
    (Savage et al. 2003)
  • HTSFUSEChandra HETGS (Scott et al. 2004)
  • 4 absorption systems from the host galaxy
  • 1 warm absorber

4
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
5
The first fit
  • Complex oxygen region
  • Narrow emission lines
  • (OVII f, OVIII Ly a)
  • Absorption lines ? OI-OVIII
  • Broad emission features OVII, OVIII

6
X-rays broad lines in Sy 1
  • Broad emission lines ?
  • Iron K a 6.4 keV (Tanaka 1995)
  • OVII triplet (21.5-22.09 Å)
  • (ngc5548 Steenbrugge et al. 2005)
  • OVIII Ly a (18.96 Å)
  • (ngc4051 Ogle et al. 2004, Fenovcik et al. 2005)

NGC 5548
7
X-rays broad lines in Sy 1
  • Broad emission lines ?
  • Iron K a 6.4 keV (Tanaka 1995)
  • OVII triplet (21.5-22.09 Å)
  • (ngc5548 Steenbrugge et al. 2005)
  • OVIII Ly a (18.96 Å)
  • (ngc4051 Ogle et al. 2004, Fenovcik et al. 2005)

Relativistic broadening
8
UV broad lines
Gabel et al. 2005
FWHM11000 km/s
9
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)

10
The LOC method (2)
  • Ingredients for the BLR
  • Log NH23 cm-2
  • Cf 0.5
  • Log n 8-12.5 cm-3
  • Log r 15.2-17.5 cm

11
  • FUSEHST best fit
  • ? 0.89
  • 0.97

X-ray line luminosity !
12
Where are the lines produced?
BLR size 6-17 ldays (Santos-Lleo et al. 2001)
13
  • No strong evidence of
  • highly ionized skin of the BLR
  • relativistically broadened profile of OVIII

14
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 ?,
    gi ven a SED
  • relies on XSTAR or Cloudy
  • Parameters NH, ?, outflow velocity, line
    broadening
  • WARM a continuos distribution of XABS
  • Parameters outflow velocity, sigma, ?low ?high

15
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
16
warm absorber variability
Log ?
2.5
0.46
NH
  • Large error bars
  • Large scatter in the ionization parameter

17
The warm absorber (2)
3 ionized warm absorbers intrinsic to Mrk 279 2
absorbers in the Milky Way
18
The nature of the wa in mrk 279
No pressure equilibrium ? continuous
distribution ?
19
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
20
The Milky way ionized absorber
Blue wing v - 87 km/s s 80 km/s
(Kaastra et al in prep.)
21
Z0 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
22
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
  • z0 absorption most likely in the Milky Way
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