mike crenshaw (georgia state university) steve kraemer (catholic university of america)

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.