Mass Outflow in the Seyfert 1 Galaxy NGC 4151 - PowerPoint PPT Presentation

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Mass Outflow in the Seyfert 1 Galaxy NGC 4151

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Jack Gabel (University of Colorado) NGC 4151. Mass Outflows from AGN in. Emission and Absorption ... IUE: black pluses. HUT: red diamonds. FOS: green triangles ... – PowerPoint PPT presentation

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Title: Mass Outflow in the Seyfert 1 Galaxy NGC 4151


1
Mass Outflows from AGN in Emission and Absorption
Mike Crenshaw (Georgia State University) Steve
Kraemer (Catholic University of America) Jack
Gabel (University of Colorado)
2
UV/X-ray Observations of NGC 4151
NGC 4151 O III Image
3
History of UV Continuum Variations (21 Years)
IUE black pluses HUT red diamonds FOS green
triangles STIS blue xs
4
Absorption Components in STIS and FUSE Spectra
  • A, C, DE, E? are intrinsic B is Galactic F, F?
    are host galaxy.
  • DE (vr -500 km s-1) responsible for bulk of UV
    and X-ray absorption.

5
Variability in C IV Region
(Kraemer et al. 2006, in preparation)
  • DE varies strongly in the low-ionization lines
    (e.g., Si II)
  • DE in 2002 is much weaker than expected from
    ionization changes

6
Variability of DE Absorption (1999 - 2002)
  • EW of low-ionization lines generally
    anti-correlated with continuum
    ? ionization changes (high-ionization lines
    are saturated)
  • Low EW in last observation indicates change in
    column density. ? transverse motion vT
    1250 km s-1

7
Emission-Line Profiles at Low Flux Levels
He II
  • He II profile has two components (broad component
    not detected)
  • narrow 260 km s-1 FWHM, intermediate
    1150 km s-1 FWHM

8
Emission-Line Profiles at Low Flux Levels
C IV
  • Fit to C IV profile using He II components (plus
    broad-line profile)
  • DE absorbs intermediate component ? self
    absorption? (P-Cygni like) ?
    likely the absorber in emission

9
Photoionization Models 2002 STIS, FUSE, CXO
Observations
  • DEb responsible for most of the metastable C
    III. ? distance 0.1pc
  • DEa is responsible for high-ionization UV lines
    and most of the X-ray absorption, and must screen
    DEb ? distance 0.1pc
  • DEc needed for low Clos of P V, etc.
    (distance unknown)

10
Conclusions
  • The outflowing UV absorbers in NGC 4151 vary as a
    result of both changing ionization and motion
    across the line of sight.
  • Component DE is responsible for the bulk of the
    UV and X-ray absorption, and has several physical
    subcomponents (a-c).
  • Most of DE is only 0.1 pc from the central
    source (compared to tens of pcs for many UV/X-ray
    absorbers).
  • DE (at vr 500 km s-1) has a transverse
    velocity 1250 km s-1, similar to the rotation
    velocity at 0.1 pc (720 km s-1).
  • We have detected DE in emission, which yields a
    global covering factor of 0.35 - 0.8.
  • This component provides the best case for a
    rotating accretion disk wind in a Seyfert galaxy.
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