Orientation Effects on Spectral Emission Features of Quasars - - PowerPoint PPT Presentation

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Orientation Effects on Spectral Emission Features of Quasars - - PowerPoint PPT Presentation

Feb 27, 2024 45 likes •275 views

Orientation Effects on Spectral Emission Features of Quasars Susanna Bisogni Harvard Smithsonian Center for Astrophysics INAF Osservatorio Astrofisico di Arcetri In collaboration with: Alessandro Marconi, Guido Risaliti

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SLIDE 1

Orientation Effects on Spectral Emission Features

  • f Quasars

Susanna Bisogni

Harvard – Smithsonian Center for Astrophysics INAF – Osservatorio Astrofisico di Arcetri In collaboration with: Alessandro Marconi, Guido Risaliti and Elisabeta Lusso

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SLIDE 2

EW[OIII]: orientation in quasars

: - no contamination from non-AGN processes (Kauffmann et al. 2003)

  • ISOTROPIC (Mulchaey et al. 1994)

if compared to disk and BLR emissions

(di Serego Alighieri et al. 1997)

  • disk

NLR

ϑ

L[OIII] Ldoss = Ldint cos ϑ

EW[OIII] ∝ f(ϑ)

Risaliti, Salvati, Marconi 2011

AGN STORM meeting - Susanna Bisogni

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SLIDE 3

AGN STORM meeting - Susanna Bisogni

EW[OIII]: intrinsic distribution

N EW[OIII]

intrinsic EW[OIII] distribution

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SLIDE 4

AGN STORM meeting - Susanna Bisogni

EW[OIII]: observed distribution

N

FLUX-LIMITED sample

EW[OIII]

intrinsic EW[OIII] distribution

  • bserved EW[OIII]

distribution

dN d(EWoss) ∝ EW −3.5

  • ss
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SLIDE 5

AGN STORM meeting - Susanna Bisogni

EW[OIII]: observed distribution

FLUX-LIMITED sample Bisogni, Marconi, Risaliti 2017

dN d(EWoss) ∝ EW −3.5

  • ss

~ 12000 blue objects SDSS DR7

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SLIDE 6

50 100 150 200 EW(Hβ) ( ˚ A) 1 10 100 N

AGN STORM meeting - Susanna Bisogni

V

ϑ

LBLRobs = LBLRint cos ϑ

Γ = −3.5 Γ = −6.9

Bisogni, Marconi, Risaliti 2017

EW[OIII] vs Broad Lines EWs

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SLIDE 7

AGN STORM meeting - Susanna Bisogni

EW[OIII]: a missing torus?

N EW[OIII]

intrinsic EW[OIII] distribution

ϑmax

EW −3.5

  • ss

ϑmax

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SLIDE 8

10 100 EW([O III]) ( ˚ A) 1 10 100 N

AGN STORM meeting - Susanna Bisogni

EW[OIII]: a missing torus?

ϑmax

Bisogni, Marconi, Risaliti 2017

Γ = −3.5

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SLIDE 9

10 100 EW([O III]) ( ˚ A) 1 10 100 N

AGN STORM meeting - Susanna Bisogni

EW[OIII]: a missing torus?

Bisogni, Marconi, Risaliti 2017

Γ = −3.5

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SLIDE 10

AGN STORM meeting - Susanna Bisogni

EW[OIII]: method

~ 12000 blue objects SDSS DR7

NO RED SPECTRA!

Bisogni, Marconi, Risaliti 2017

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SLIDE 11

AGN STORM meeting - Susanna Bisogni

EW[OIII]: results for Narrow Lines

voss = vout cos ϑ

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SLIDE 12

AGN STORM meeting - Susanna Bisogni

EW[OIII]: results for Narrow Lines

voss = vout cos ϑ

low EW[OIII]

5007

high EW[OIII]

Bisogni, Marconi, Risaliti 2017

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SLIDE 13

AGN STORM meeting - Susanna Bisogni

EW[OIII]: results for Narrow Lines

voss = vout cos ϑ

[OIII] blue component velocity

Bisogni, Marconi, Risaliti 2017

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SLIDE 14

AGN STORM meeting - Susanna Bisogni

EW[OIII]: results for Broad Lines

vint voss

ϑ

voss = vrot sin ϑ

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SLIDE 15

AGN STORM meeting - Susanna Bisogni

EW[OIII]: results for Broad Lines

voss = vrot sin ϑ

high EW[OIII] low EW[OIII]

Bisogni, Marconi, Risaliti 2017

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SLIDE 16

AGN STORM meeting - Susanna Bisogni

EW[OIII]: results for Broad Lines

voss = vrot sin ϑ

FWHM Hβ

Same results for MgII and Hα!!

Bisogni, Marconi, Risaliti 2017

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SLIDE 17

AGN STORM meeting - Susanna Bisogni

EW[OIII]: eigenvector 1

H-[OIII] EW[OIII] = (1-6) EW[OIII] = (12-25) EW[OIII] = (100-250)

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SLIDE 18

1014 1015

ν[H]]

1

νLν [Hrg s−1]

15 μ 15 μ 15 μ 15 μ 15 μ 15 μ

(1 − 6)Å (6 − 12)Å (12 − 25)Å (25 − 50)Å (50 − 100)Å (100 − 250)Å

AGN STORM meeting - Susanna Bisogni

EW[OIII]: results for the torus

~ 12000 blue objects SDSS DR7

  • GALEX FUV, NUV
  • SDSS ugriz
  • 2MASS J, H, K
  • WISE 3.4, 4.6, 12,

22 m Bisogni, Marconi, Lusso, Risaliti 2017b, in preparation Spectral Energy Distrubution

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SLIDE 19

1014 1015

ν[H]]

1

νLν [Hrg s−1]

15 μ 15 μ 15 μ 15 μ 15 μ 15 μ

(1 − 6)Å (6 − 12)Å (12 − 25)Å (25 − 50)Å (50 − 100)Å (100 − 250)Å

AGN STORM meeting - Susanna Bisogni

EW[OIII]: results for the torus

~ 12000 blue objects SDSS DR7

  • GALEX FUV, NUV
  • SDSS ugriz
  • 2MASS J, H, K
  • WISE 3.4, 4.6, 12,

22 m Bisogni, Marconi, Lusso, Risaliti 2017b, in preparation Spectral Energy Distrubution

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SLIDE 20

AGN STORM meeting - Susanna Bisogni

101 4 × 100 6 × 100 2 × 101

λ[μm]

100 6 × 10−1

λfλ [erg cm−2 s−1]

15 μ 15 μ 15 μ 15 μ 15 μ 15 μ (1 − 6)Å (6 − 12)Å (12 − 25)Å (25 − 50)Å (50 − 100)Å (100 − 250)Å

1 0.6 4 20 10 6

Bisogni, Marconi, Lusso, Risaliti 2017b, in preparation

EW[OIII]: results for the torus

high EW[OIII] low EW[OIII]

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SLIDE 21

AGN STORM meeting - Susanna Bisogni

101 4 × 100 6 × 100 2 × 101

λ[μm]

100 6 × 10−1

λfλ [erg cm−2 s−1]

15 μ 15 μ 15 μ 15 μ 15 μ 15 μ (1 − 6)Å (6 − 12)Å (12 − 25)Å (25 − 50)Å (50 − 100)Å (100 − 250)Å

1 0.6 4 20 10 6

Bisogni, Marconi, Lusso, Risaliti 2017b, in preparation

EW[OIII]: results for the torus

Nenkova et al.(2008)

high EW[OIII] low EW[OIII]

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SLIDE 22

AGN STORM meeting - Susanna Bisogni

EW[OIII]: summary

Both Broad and Narrow Lines behaviours confirm EW[OIII] is a good

  • rientation indicator:
  • BLR is disk-shaped
  • outflows in the NLR

Analysis of the IR SED confirms the torus is co-axial with the disk and the BLR and probably clumpy

Correcting virial mass estimates Better understanding of geometry and kinematics of the inner components

Perspectives

Looking for Changing Look Quasars as a function of EW[OIII]