Kinematical Modeling of the NLR of Seyfert Galaxies

1
Kinematical Modeling of the NLR of Seyfert
Galaxies

• By
• V. Das
• 2005 November 10

2
Contents

• Introduction
• Goals, Definitions Seyferts, NLR, etc,
• Data Analysis
• Obtaining, reducing data, etc
• Models
• Generation and fitting, etc
• Conclusion
• Work in progress
• What next

3
Introduction
http//www.astr.ua.edu/gifimages/ngc5548.html
--Definitions--

• Parts of a Seyfert
• SMBH accretion disk hot corona
• BLR - region 10 Ld from SMBH
• Torus 1 Pc?
• Scattering region - region of hot electrons
  outside the torus
• NLR - region lt 500 pc from SMBH
• Radio jet (weak) extends from 0 - 500 pc
• ENLR - region gt 500 pc (gas from the host)
• NLR
• The gases are in outflow (Crenshaw Kraemer,
  2000a,b)
• Resembles a biconical geometry (Evans et. al.,
  1993 Schmitt Kinney, 1996)

• Seyfert Galaxies
• Spirals with star-like cores ( 1 all spirals
  are Sey)
• Strong high-ionization emission lines
• Lower luminosity end of AGN distribution , nearby
  (lt100 Mpc)
• Seyfert 1
• Broad emission lines (FWHM gt 1000 km/s)
• Superposed with narrower emission lines
• Seyfert 2
• Only narrow emission lines seen (FWHM lt 500 km/s)
• Non-stellar continuum is weaker
• Goal
• Understand the kinematics of the Narrow-Line
  Region (NLR)
• Help us understand the forces at work in the
  central engine

Seyfert 1 NGC 5548
Normal Spiral NGC 3277
68 Mpc
4
Data AnalysisNGC 4151

• NGC 4151, Seyfert 1
• Five parallel long-slit data, 2000 July, by
  Hutchings et al.
• HSTs STIS, with grating G430M, which has
  9000
• G430M resolve velocities down to 30 km/s (0.5
  )
• Each slit contains 1064 spectra of the
  emission doublet
• ??4959, 5007!
• Each spectrum contains multiple components of
  ??4959, 5007 emission!

Black spectrum Green gaussian fit per
component Red sum of green (total fit) Blue
fit error (black red)
Red high flux Blue medium flux black low flux
WFPC2 ? 5007 image NLR of NGC 4151
5
Data AnalysisNGC 1068

• NGC 1068, Seyfert 2
• Seven slits covering the NLR, taken in, 1999
  2000 September, by Cecil et al. 2002
• Same instruments were used
• Same processing as previous

6
Biconical Outflow Models
2D Models

• Input parameters
• Inner outer opening angles
• Position angle of the bicone axis in the sky
• Inclination in the sky
• Maximum velocity of outflow
• Turnover point
• Size of bicone along z axis
• Velocity law of outflow (vdistance from SMBH
  seem to work best)
• Fill the bicone with radial velocity
• i.e. each point in the bicone is assigned a
  radial velocity

• 2D Projection Models
• Written by Mike Crenshaw
• Used on low resolution data on the same objects,
  NGC 4151, NGC 1068
• Crenshaw Kraemer 2000 a,b
• Or was it c, d, e, f, ???
• Disadvantages of..
• Long run time
• Difficult to visualize
• Bombs with certain input parameters
• Advantage
• Good resolution

• 3D Models
• Total rewrite from scratch
• Solve all the previous problems
• So far
• Disadvantage
• Memory allocation problem
• 3D Arrays are HUGE

Parameters used Outer ? 40 Inner ? 20 Inc. ?
5 P.A. ? 30 Max Vel. 2000 km s-1 Turn. Pt.
140 pc Height of cone 400 pc
Ruled out infall and rotation models
His model sucks!
Front
Back
It stinks!
Radial
7
Biconical Outflow Models
3D Models
Parameters used Outer ? 402 Inner ?
202 Inc. ? 52 P.A. ? 302 Max Vel.
200050 km s-1 Turn. Pt. 14010 pc Height of
cone 40030 pc
LOS
8
Biconical Outflow Models

• Slit extraction
• Width, placement, position angle, mimics STIS
  (aboard HST)

Position (arcsec)
velocity
blueshifts
redshifts
9
Fitting the model
Best fit Parameters (NGC 4151) Outer ?
332 Inner ? 152 Inc. ? -452 P.A. ?
522 Max Vel. 80030 km s-1 Turn. Pt. 9610
pc Height of cone 40030 pc

• Aim
• Model should be consistent
• across all slits
• at different slit position angles
• Model fits to data are chi by eye
• Parameters are tweaked
• Models are run
• Parameters are tweaked
• Models are re-run
• until we determine a best fit

Best fit Parameters (NGC 1068) Outer ?
402 Inner ? 202 Inc. ? 52 P.A. ?
302 Max Vel. 200050 km s-1 Turn. Pt. 14010
pc Height of cone 40030 pc
10
Work in Progress

• The radio jet problem
• Some authors claim that radio jet is accelerating
  the NLR clouds
• Radially (Whittle Wilson 2004)
• Laterally (Capetti et al. 1999, Axon et al.
  1998)
• We obtained radio maps from Mundell et al. 2003
  and Gallimore et al. 2004 to test these claims
• Both claims are not seen observationally

11
Conclusion

• Models are not a perfect match
• Meant to show general trend in Sey 1s and 2s
• Points outside of the bicone region suggest a
  patchy torus
• Radio jet does not seem to accelerate the clouds
  radially or laterally
• However it may cause some disturbance of the
  faint clouds
• Fits for both Seyfert types indicate a common
  acceleration/deceleration mechanism

12
What Next?

• Building a more dynamical model which will
  include
• Gravity from the SMBH, Nuclear star cluster,
  bulge mass,
• Radiation pressure
• Drag forces (possibly from diffuse X-ray gas)

13
Acknowledgement
(Mikes buddy ??)

• Steve Kraemer (Catholic Univ.)

• My Adviser
• Mike Crenshaw
• My Committee members
• Mike IM S. P. Crenshaw
• Dick IV B. N. Miller
• Paul IM S. S. Wiita
• Doug IM S. N. Gies
• ????? ???? From physics dept.

14
References