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Mike Crenshaw (Georgia State University) Steve Kraemer (Catholic University of America)

NGC 4151. Mass Outflows from AGN in Emission and Absorption. Mike Crenshaw (Georgia State University) Steve Kraemer (Catholic University of America) Jack Gabel (University of Colorado).

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Mike Crenshaw (Georgia State University) Steve Kraemer (Catholic University of America)

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  1. NGC 4151 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. Six HST/STIS echelle observations (0.2'' x 0.2'’) of central emission-line knot (including nucleus): 1999 July - 2002 May • Simultaneous HST, FUSE, and CXO observations in 2002 May (see Kraemer et al. 2005, ApJ, 633, 693 for more on X-ray observations) UV/X-ray Observations of NGC 4151 NGC 4151 [O III] Image

  3. STIS observations taken at moderate to low flux levels History of UV Continuum Variations (~21 Years) IUE: black pluses HUT: red diamonds FOS: green triangles STIS: blue x’s

  4. Absorption Components in STIS and FUSE Spectra • A, C, D+E, E are intrinsic; B is Galactic; F, F are host galaxy. • D+E (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) • D+E varies strongly in the low-ionization lines (e.g., Si II) • D+E in 2002 is much weaker than expected from ionization changes

  6. Variability of D+E 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. blue - narrow green - intermediate 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. blue - narrow green - intermediate red - broad Emission-Line Profiles at Low Flux Levels C IV • Fit to C IV profile using He II components (plus broad-line profile) • D+E absorbs intermediate component  self absorption? (P-Cygni like)  likely the absorber in emission

  9. Photoionization Models: 2002 STIS, FUSE, CXO Observations • D+Eb responsible for most of the metastable C III.  distance ≈ 0.1pc • D+Ea is responsible for high-ionization UV lines and most of the X-ray absorption, and must screen D+Eb  distance ≤ 0.1pc • D+Ec 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 D+E is responsible for the bulk of the UV and X-ray absorption, and has several physical subcomponents (a-c). • Most of D+E is only ~0.1 pc from the central source (compared to tens of pcs for many UV/X-ray absorbers). • D+E (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 D+E 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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