Title-Page Axion Luminosity From AGN Phenomenology-2010 Pankaj - - PowerPoint PPT Presentation

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Title-Page Axion Luminosity From AGN Phenomenology-2010 Pankaj Jain Subhayan Mandal IFPA, University of Liege-Belgium May 10, 2010 S. Mandal - (IFPA@ULg) -Luminosity@AGN/pheno-10 May 10, 2010 1 / 16 Overview Features Of AGN 1 B.M.

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SLIDE 1

Title-Page Axion Luminosity From AGN

Phenomenology-2010 Pankaj Jain Subhayan Mandal∗

IFPA, University of Liege-Belgium

May 10, 2010

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 1 / 16

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SLIDE 2

Overview

Features Of AGN

1B.M. Peterson, An Introduction To Active Galactic Nuclei(CUP) 2Accretion power in astrophysics-J. Frank, A. R. King, Derek J. Raine (CUP)

  • 3D. Hutsem kers and H. Lamy, Astronomy and Astrophysics, 367, 381, (2001).
  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 2 / 16

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SLIDE 3

Overview

Features Of AGN Luminosity ∼ 1045 erg-cm 1

1B.M. Peterson, An Introduction To Active Galactic Nuclei(CUP) 2Accretion power in astrophysics-J. Frank, A. R. King, Derek J. Raine (CUP)

  • 3D. Hutsem kers and H. Lamy, Astronomy and Astrophysics, 367, 381, (2001).
  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 2 / 16

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SLIDE 4

Overview

Features Of AGN Luminosity ∼ 1045 erg-cm 1 Stability 2

1B.M. Peterson, An Introduction To Active Galactic Nuclei(CUP) 2Accretion power in astrophysics-J. Frank, A. R. King, Derek J. Raine (CUP)

  • 3D. Hutsem kers and H. Lamy, Astronomy and Astrophysics, 367, 381, (2001).
  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 2 / 16

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SLIDE 5

Overview

Features Of AGN Luminosity ∼ 1045 erg-cm 1 Stability 2 Accreting System

1B.M. Peterson, An Introduction To Active Galactic Nuclei(CUP) 2Accretion power in astrophysics-J. Frank, A. R. King, Derek J. Raine (CUP)

  • 3D. Hutsem kers and H. Lamy, Astronomy and Astrophysics, 367, 381, (2001).
  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 2 / 16

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SLIDE 6

Overview

Features Of AGN Luminosity ∼ 1045 erg-cm 1 Stability 2 Accreting System Polarization Properties 3

1B.M. Peterson, An Introduction To Active Galactic Nuclei(CUP) 2Accretion power in astrophysics-J. Frank, A. R. King, Derek J. Raine (CUP)

  • 3D. Hutsem kers and H. Lamy, Astronomy and Astrophysics, 367, 381, (2001).
  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 2 / 16

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SLIDE 7

Overview

Features Of AGN Luminosity ∼ 1045 erg-cm 1 Stability 2 Accreting System Polarization Properties 3 ‘Coherent Orientation Of The “Visible” Quasar Polarization On Cosmological Scale’

1B.M. Peterson, An Introduction To Active Galactic Nuclei(CUP) 2Accretion power in astrophysics-J. Frank, A. R. King, Derek J. Raine (CUP)

  • 3D. Hutsem kers and H. Lamy, Astronomy and Astrophysics, 367, 381, (2001).
  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 2 / 16

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SLIDE 8

Overview

Features Of AGN Luminosity ∼ 1045 erg-cm 1 Stability 2 Accreting System Polarization Properties 3 ‘Coherent Orientation Of The “Visible” Quasar Polarization On Cosmological Scale’ Different AGN’s

1B.M. Peterson, An Introduction To Active Galactic Nuclei(CUP) 2Accretion power in astrophysics-J. Frank, A. R. King, Derek J. Raine (CUP)

  • 3D. Hutsem kers and H. Lamy, Astronomy and Astrophysics, 367, 381, (2001).
  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 2 / 16

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SLIDE 9

Overview

Features Of AGN Luminosity ∼ 1045 erg-cm 1 Stability 2 Accreting System Polarization Properties 3 ‘Coherent Orientation Of The “Visible” Quasar Polarization On Cosmological Scale’ Different AGN’s

1 Quasar 2 QSO 3 Seyfert 4 Blazar 5 BL Lac

1B.M. Peterson, An Introduction To Active Galactic Nuclei(CUP) 2Accretion power in astrophysics-J. Frank, A. R. King, Derek J. Raine (CUP)

  • 3D. Hutsem kers and H. Lamy, Astronomy and Astrophysics, 367, 381, (2001).
  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 2 / 16

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SLIDE 10

Alignment Effect

4

  • 4D. Hutsem kers, R. Cabanac, H. Lamy and D. Sluse, Astronomy and Astrophysics,

441, 915, (2005)

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 3 / 16

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SLIDE 11

Explanation

This curious effect has given way to several theories - such as -

5arXiv:0910.3036

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 4 / 16

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SLIDE 12

Explanation

This curious effect has given way to several theories - such as -

1 Instrumental Artefact

5arXiv:0910.3036

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 4 / 16

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SLIDE 13

Explanation

This curious effect has given way to several theories - such as -

2 Contamination By Intersteller Polarization Inside Milky Way

5arXiv:0910.3036

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 4 / 16

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SLIDE 14

Explanation

This curious effect has given way to several theories - such as -

3 Extinction By Dust Grains Aligned ⊥ To Magnetic Field

5arXiv:0910.3036

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 4 / 16

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SLIDE 15

Explanation

This curious effect has given way to several theories - such as -

3 Extinction By Dust Grains Aligned ⊥ To Magnetic Field 4 Conversion Of γ to φ

5arXiv:0910.3036

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 4 / 16

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SLIDE 16

Explanation

This curious effect has given way to several theories - such as -

3 Extinction By Dust Grains Aligned ⊥ To Magnetic Field 4 Conversion Of γ to φ 5 Correlated Magnetic Fields

5arXiv:0910.3036

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 4 / 16

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SLIDE 17

Explanation

This curious effect has given way to several theories - such as -

3 Extinction By Dust Grains Aligned ⊥ To Magnetic Field 4 Conversion Of γ to φ 5 Correlated Magnetic Fields 6 Production Of φ In The Accretion Disk

5arXiv:0910.3036

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 4 / 16

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SLIDE 18

Explanation

This curious effect has given way to several theories - such as -

3 Extinction By Dust Grains Aligned ⊥ To Magnetic Field 4 Conversion Of γ to φ 5 Correlated Magnetic Fields 6 Production Of φ In The Accretion Disk 7 Mixing Of γ to φ & Dust Extinction 5

5arXiv:0910.3036

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 4 / 16

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SLIDE 19

AGN Morphology

The schematic diagram for an AGN -

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 5 / 16

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SLIDE 20

Production Of φ From γ Inside Accretion Disk

Axion can be produced inside the accretion disk by the following processes

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 6 / 16

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SLIDE 21

Production Of φ From γ Inside Accretion Disk

Axion can be produced inside the accretion disk by the following processes

  • Compton
  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 6 / 16

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SLIDE 22

Production Of φ From γ Inside Accretion Disk

Axion can be produced inside the accretion disk by the following processes

  • Compton

Bremsstrahlung

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 6 / 16

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SLIDE 23

Production Of φ From γ Inside Accretion Disk

Axion can be produced inside the accretion disk by the following processes

  • Compton

Bremsstrahlung Primakoff

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 6 / 16

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SLIDE 24

Luminosity From poduction Of φ

The integrated luminosity of the accretion disk for the previously mentioned cases are found to be - Lcomp = 9.7 × 1029 erg − s−1 (1) Lbrem =

  • ˙

ǫa(B) dM = 5.7 × 1036 erg − s−1 (2) LPrim = 2.84 × 1032 + 7.1 × 1031 erg − s−1 (3) Which is quite low compared to the γ luminosity6.

6Here the coupling values of gaee & gaγγ are used, which, in turn are consensus

parameters for axion.

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 7 / 16

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SLIDE 25

Conversion In AGN Surroundings

AGN surroundings consists of the disk, jets, BLR, NLR, dust tori & the radio lobes. The exact morphology is not yet known but we can assume a spherical domain (like the camel) of certain magnitude.What is more, it is not known what are the parameters there, or, how they change in different

  • regions. Still, we can go ahead with some representative numbers.

Parameters Object Magnetic Field Plasma density Cygnus A 4 × 10−4 G 10−4 cm−3

Table: The value of of parameters we take for the representative case

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 8 / 16

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SLIDE 26

Conversion Diagram

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 9 / 16

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SLIDE 27

Methodology

Extinction Here we shall use the standard 2×2 channel φ mixing with γ with extinction with intergalactic dust. Again the parameter space is a little flimsy but we can (as a first guess) use the value of the host galaxy gaxtinction found in high redshift (as the aligned quasars) supernovae.

  • ω2 + ∂2

z

A||(z) φ(z)

  • = M

A||(z) φ(z)

  • .

(4) M = ω2

p + iΓ(ω)

−gφBTω −gφBTω m2

φ

  • (5)

Where, Γ = 2ω2K z

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 10 / 16

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SLIDE 28

Solution

λ± = 1 2

  • Ω2

p + m2 φ ±

  • (Ω2

p + m2 φ)2 − 4(Ω2 pm2 φ − g2 φB2 Tω2)

  • (6)

where Ω2

p = ω2 p + iΓ. We assume the boundary condition, φ(0) = 0, and

find the final result A||(z) = 1 ad − bc

  • ad e(iz√

ω2−λ+) − bc e(iz√ ω2−λ−)

A||(0) φ(z) = bd ad − bc

  • e(iz√

ω2−λ+) − e(iz√ ω2−λ−)

A||(0) (7) where a = (λ+ − m2

φ)/√N+, b = −gφBTω/√N+, c = gφBTω/√N−,

d = (Ω2

p − λ−)/√N−. Here N+ and N− are normalization factors which

cancel out in the final expressions. The perpendicular component of the electromagnetic wave is given by, A⊥(z) = A⊥(0)eiz√

ω2−Ω2

p

(8)

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 11 / 16

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SLIDE 29

Plot

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 12 / 16

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SLIDE 30

Quasar Polarization Alignment

In AGN surroundings, the conversion of γ → φ dominates when extinction is assumed. The φ reconverts to γ upon entering our supercluster. The selective attenuation of a particular polarization induces some linear polarization - dichroism. The alignment towards local supercluster Virgo emboldens our claim

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 13 / 16

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SLIDE 31

Some Issues

The observed alignemnt may be consistently (qualitatively) understood by the following -

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 14 / 16

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SLIDE 32

Some Issues

The observed alignemnt may be consistently (qualitatively) understood by the following - Two Classes Of Quasars BAL/ RQ+O

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 14 / 16

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SLIDE 33

Some Issues

The observed alignemnt may be consistently (qualitatively) understood by the following - Two Classes Of Quasars BAL/ RQ+O The Latters’ Polarization Distribution Peaks At A Low Value

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 14 / 16

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SLIDE 34

Some Issues

The observed alignemnt may be consistently (qualitatively) understood by the following - Two Classes Of Quasars BAL/ RQ+O The Latters’ Polarization Distribution Peaks At A Low Value The Former’s Polarization Distribution Peaks At A High Value & Somewhat Broad Distribution

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 14 / 16

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SLIDE 35

Some Issues

The observed alignemnt may be consistently (qualitatively) understood by the following - Two Classes Of Quasars BAL/ RQ+O The Latters’ Polarization Distribution Peaks At A Low Value The Former’s Polarization Distribution Peaks At A High Value & Somewhat Broad Distribution

1 General Mixing In The Virgo Supercluster

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 14 / 16

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SLIDE 36

Some Issues

The observed alignemnt may be consistently (qualitatively) understood by the following - Two Classes Of Quasars BAL/ RQ+O The Latters’ Polarization Distribution Peaks At A Low Value The Former’s Polarization Distribution Peaks At A High Value & Somewhat Broad Distribution

1 General Mixing In The Virgo Supercluster 2 The Flux Of Pseudoscalars Photon Flux

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 14 / 16

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SLIDE 37

Some Issues

The observed alignemnt may be consistently (qualitatively) understood by the following - Two Classes Of Quasars BAL/ RQ+O The Latters’ Polarization Distribution Peaks At A Low Value The Former’s Polarization Distribution Peaks At A High Value & Somewhat Broad Distribution

1 General Mixing In The Virgo Supercluster 2 The Flux Of Pseudoscalars Photon Flux 3 The Ratio Of φ/γ Flux is Different In The AGN Classes

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 14 / 16

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SLIDE 38

Some Issues

The observed alignemnt may be consistently (qualitatively) understood by the following - Two Classes Of Quasars BAL/ RQ+O The Latters’ Polarization Distribution Peaks At A Low Value The Former’s Polarization Distribution Peaks At A High Value & Somewhat Broad Distribution

1 General Mixing In The Virgo Supercluster 2 The Flux Of Pseudoscalars Photon Flux 3 The Ratio Of φ/γ Flux is Different In The AGN Classes 4 It Explains The Effect!

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 14 / 16

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SLIDE 39

Some Issues

The observed alignemnt may be consistently (qualitatively) understood by the following - Two Classes Of Quasars BAL/ RQ+O The Latters’ Polarization Distribution Peaks At A Low Value The Former’s Polarization Distribution Peaks At A High Value & Somewhat Broad Distribution

1 General Mixing In The Virgo Supercluster 2 The Flux Of Pseudoscalars Photon Flux 3 The Ratio Of φ/γ Flux is Different In The AGN Classes 4 It Explains The Effect!

Future Scope → To Quantify The Claim.

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 14 / 16

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SLIDE 40

Conclusion

The standard processes yield a low luminosity of pseudoscalars inside AGN. However, the flux can be sizable at ultraviolet frequencies if we assume a fre- quency dependent dust extinction in the AGN atmosphere while calculating standard photon to pseudoscalar conversion mediated in a magnetic field. This may in turn be applied to the apparent problem of Quasar alignment.

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 15 / 16

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SLIDE 41

Thank You

Acknowledgement : I thank the following persons for their useful suggestions during the preparation of this presentation. Jean-Rene Cudell Alexandre Payez Davide Mancusi Igor Ivanov

  • S. Mandal - (IFPA@ULg)

φ-Luminosity@AGN/pheno-10 May 10, 2010 16 / 16