Mike Crenshaw (Georgia State University)

Steve Kraemer(Catholic University of America)

Jack Gabel(University of Colorado)

NGC 4151

Mass Outflows from AGN in Emission and Absorption

UV/X-ray Observations of NGC 4151

• 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)

NGC 4151 [O III] Image

History of UV Continuum Variations (~21 Years)

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IUE: black plusesHUT: red diamondsFOS: green trianglesSTIS: blue x’s

• STIS observations taken at moderate to low flux levels

Absorption Components in STIS and FUSE Spectra

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• 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.

(Kraemer et al. 2006, in preparation)

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• 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

Variability in C IV Region

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

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blue - narrowgreen - intermediate

Emission-Line Profiles at Low Flux Levels

• He II profile has two components (broad component not detected):

narrow: 260 km s-1 FWHM, intermediate: 1150 km s-1 FWHM

He II

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Emission-Line Profiles at Low Flux Levels

• 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

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blue - narrowgreen - intermediatered - broad

C IV

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)

D+Ea D+Eb D+Ec

Log U -0.26 -1.66 -1.08

Log NH 22.5 20.8 21.6

Log nH 6.75 7.65 ---

Clos ~1 0.8 0.5

Cglobal 0.81 0.38 0.35

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.