Properties of the NLR from Properties of the NLR from Spatially Resolved Spatially Resolved Spectroscopy Spectroscopy Nicola Bennert Nicola Bennert University of California Riverside University of California Riverside Collaborators: Bruno Jungwiert, Stefanie Komossa, Martin Haas, Collaborators: Bruno Jungwiert, Stefanie Komossa, Martin Haas, Rolf Chini Rolf Chini
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Properties of the NLR from Spatially Resolved Spectroscopy
Properties of the NLR from Spatially Resolved Spectroscopy. Nicola Bennert University of California Riverside Collaborators: Bruno Jungwiert, Stefanie Komossa, Martin Haas, Rolf Chini. Extended enough to be directly accessible Affected by ionizing source, presence of torus, jets, … - PowerPoint PPT Presentation
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Properties of the NLR from Properties of the NLR from Spatially Resolved SpectroscopySpatially Resolved Spectroscopy
Nicola BennertNicola Bennert
University of California RiversideUniversity of California Riverside
Collaborators: Bruno Jungwiert, Stefanie Komossa, Martin Haas, Rolf ChiniCollaborators: Bruno Jungwiert, Stefanie Komossa, Martin Haas, Rolf Chini
The Narrow-Line Region of Active GalaxiesThe Narrow-Line Region of Active Galaxies
Extended enough to be directly accessibleExtended enough to be directly accessibleAffected by ionizing source, presence of torus, jets, … Affected by ionizing source, presence of torus, jets, … Forbidden lines for diagnostics Forbidden lines for diagnostics
[OIII] narrow-band imaging commonly used[OIII] narrow-band imaging commonly used(e.g. Mulchaey et al. 1996, Schmitt et al. 2003)(e.g. Mulchaey et al. 1996, Schmitt et al. 2003)
⇒⇒ Disappearing NLR (Netzer et al. 2004)?Disappearing NLR (Netzer et al. 2004)?
The Narrow-Line Region of Active GalaxiesThe Narrow-Line Region of Active Galaxies
Extended enough to be directly accessibleExtended enough to be directly accessibleAffected by ionizing source, presence of torus, jets, … Affected by ionizing source, presence of torus, jets, … Forbidden lines for diagnostics Forbidden lines for diagnostics
[OIII] narrow-band imaging commonly used [OIII] narrow-band imaging commonly used (e.g. Mulchaey et al. 1996, Schmitt et al. 2003)(e.g. Mulchaey et al. 1996, Schmitt et al. 2003)
But: dependency on sensitivityBut: dependency on sensitivityMulchaey et al. 1996 vs. Schmitt et al. 2003: Mulchaey et al. 1996 vs. Schmitt et al. 2003: 6 times larger NLRs!6 times larger NLRs!
And: emission contaminated by contributions And: emission contaminated by contributions from e.g. star formation/shock-ionized gasfrom e.g. star formation/shock-ionized gas
Answers from SpectroscopyAnswers from Spectroscopy
Correction of stellar contribution: galaxy itself at 18‘‘ distanceCorrection of stellar contribution: galaxy itself at 18‘‘ distance
⇒ ⇒ NLR size free of stellar contamination:NLR size free of stellar contamination:r ~ 6‘‘ (here) vs. r ~ 3‘‘ (Schmitt et al. 2003) vs. r ~ 12‘‘ (Fraquelli et al. 2003)r ~ 6‘‘ (here) vs. r ~ 3‘‘ (Schmitt et al. 2003) vs. r ~ 12‘‘ (Fraquelli et al. 2003)
Separation NLR/HII region (2Sy1s, 2Sy2s), confirmed by CLOUDY modelingSeparation NLR/HII region (2Sy1s, 2Sy2s), confirmed by CLOUDY modeling
Electron density and ionization parameterElectron density and ionization parameter
⇒ ⇒ excitation of the NLR due to photoionizationexcitation of the NLR due to photoionization
⇒⇒ No Strömgren behaviour No Strömgren behaviour
Both radially decreasing (1/r) Both radially decreasing (1/r)
Stellar and gaseous kinematicsStellar and gaseous kinematics
curves similar, signs of rotational motion, no difference in HII regioncurves similar, signs of rotational motion, no difference in HII region
⇒ ⇒ torus axis not aligned with galaxy axis, ionization cone lies in disk?torus axis not aligned with galaxy axis, ionization cone lies in disk?
Central AGN and galaxy randomly orientated? (e.g. Kinney et al. Central AGN and galaxy randomly orientated? (e.g. Kinney et al. 2000)2000)
⇒⇒ NLR gas distributed in a disk rather than a sphereNLR gas distributed in a disk rather than a sphere
The Narrow-Line Region of Active GalaxiesThe Narrow-Line Region of Active Galaxies
NLR size free of stellar NLR size free of stellar contaminationcontamination
NLR photoionizedNLR photoionized
NLR gas in a diskNLR gas in a diskTorus axis in galaxy disk?Torus axis in galaxy disk?
Unified model supportedUnified model supported
BLR size from literature („reverberation mapping“; Kaspi et al. 2000)BLR size from literature („reverberation mapping“; Kaspi et al. 2000)
Modeling: NLR size and luminosityModeling: NLR size and luminosity
⇒ ⇒ Different slopes for type 1/2Different slopes for type 1/2
flatter thanflatter than
Unified model (Antonucci 1993)Unified model (Antonucci 1993) & „receding“ torus (Lawrence & „receding“ torus (Lawrence 1991)1991)
)cos(][
.
150
UVOIII
UV
LLLh
50.UVLh
determined fromdetermined from
HHαα/H/Hββ continuum slope continuum slope
ReddeningReddening
⇒ ⇒ locally varying amount of dust intrinsic to the NLR? (true for all objects)locally varying amount of dust intrinsic to the NLR? (true for all objects)
Comparison of type-1 and type-2Comparison of type-1 and type-2
Reddening of nuclear spectrum Reddening of nuclear spectrum higher higher
Electron densities comparableElectron densities comparable (decrease faster in Sy1s)(decrease faster in Sy1s)
In agreement with statistics:In agreement with statistics:high-ionization lines & high-critical-density lines stronger in Sy1shigh-ionization lines & high-critical-density lines stronger in Sy1s
⇒⇒ Highly-ionized gas clouds are located close to nucleus and can be hiddenHighly-ionized gas clouds are located close to nucleus and can be hidden by torus (e.g. Nagao et al. 2000)by torus (e.g. Nagao et al. 2000)
Solid line 1: ionization parameter (log Solid line 1: ionization parameter (log U U = -4.0 … -1.5 steps of 0.5, from bottom to top; = -4.0 … -1.5 steps of 0.5, from bottom to top; n n = 800, 400, 200 cm= 800, 400, 200 cm-3-3; ; r r = 50, 100, 250 pc, from right to left)= 50, 100, 250 pc, from right to left)
Dotted lines 2&3: metal abundances (Z = 3…0.05 solar, from right to left; log U = -2.8 Dotted lines 2&3: metal abundances (Z = 3…0.05 solar, from right to left; log U = -2.8 for line 2; log U = -3.7 for line 3)for line 2; log U = -3.7 for line 3)
Dash-dotted lines 4&5: N & S abundances (Dash-dotted lines 4&5: N & S abundances (ZZ, , UU dito 2&3) dito 2&3)
Dashed line 6: high density (Dashed line 6: high density (n n = 1000000 cm= 1000000 cm-3-3; ; U U dito 1)dito 1)
CLOUDY modelingCLOUDY modeling
⇒ ⇒ transition in first and transition in first and third diagnostic diagram: third diagnostic diagram: decreasing ionization decreasing ionization parameter & metallicityparameter & metallicity
But not for second But not for second diagnostic diagramdiagnostic diagram