M87 Avery E. Broderick Sheperd Doeleman (MIT Haystack) Avi Loeb - - PowerPoint PPT Presentation

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M87 Avery E. Broderick Sheperd Doeleman (MIT Haystack) Avi Loeb - - PowerPoint PPT Presentation

Apr 15, 2023 129 likes •564 views

VLBI observations of jets in M87 Avery E. Broderick Sheperd Doeleman (MIT Haystack) Avi Loeb (Harvard) Vincent Fish (MIT Haystack) Ramesh Narayan (Harvard) Alan Rogers (MIT Haystack) Mark Reid (Smithsonian) Dimitrios Psaltis (Arizona)

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SLIDE 1

VLBI

  • bservations of jets in

M87

Avery E. Broderick

Sheperd Doeleman (MIT Haystack) Vincent Fish (MIT Haystack) Alan Rogers (MIT Haystack) Dimitrios Psaltis (Arizona) Tim Johannsen (Arizona/UW-PI-CITA) Avi Loeb (Harvard) Ramesh Narayan (Harvard) Mark Reid (Smithsonian) Mareki Honma (NAOJ)

Fermi Bubbles Workshop 12.4.2013

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SLIDE 2

mm-VLBI

  • bservations of jets in

M87

Avery E. Broderick

Sheperd Doeleman (MIT Haystack) Vincent Fish (MIT Haystack) Alan Rogers (MIT Haystack) Dimitrios Psaltis (Arizona) Tim Johannsen (Arizona/UW-PI-CITA) Avi Loeb (Harvard) Ramesh Narayan (Harvard) Mark Reid (Smithsonian) Mareki Honma (NAOJ)

Fermi Bubbles Workshop 12.4.2013

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SLIDE 3

mm-VLBI

  • bservations of jets in

M87 & Sgr A*

Avery E. Broderick

Sheperd Doeleman (MIT Haystack) Vincent Fish (MIT Haystack) Alan Rogers (MIT Haystack) Dimitrios Psaltis (Arizona) Tim Johannsen (Arizona/UW-PI-CITA) Avi Loeb (Harvard) Ramesh Narayan (Harvard) Mark Reid (Smithsonian) Mareki Honma (NAOJ)

Fermi Bubbles Workshop 12.4.2013

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SLIDE 4

SGR A* & M87 ARE THE SAME!

  • Very sub-Eddington: 𝑴/𝑴𝑭𝒆𝒆~𝟐𝟏−𝟘 & 𝟐𝟏−𝟕 ≪ 𝟏. 𝟏𝟐
  • Flat radio spectrum with spectral break at ~1mm
  • Similar 𝒐𝒇, 𝑪~𝟐𝟏𝟏 G

Fermi Bubbles Workshop 12.4.2013

Sgr A*

(Zhao & Goss, 1998)

M87

VLA (NRAO)

What ingredient in jet production is missing in Sgr A*? (Is an ingredient missing?)

SGR A* & M87 ARE DIFFERENT!

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SLIDE 5

Fermi Bubbles Workshop 12.4.2013

SMA, JCMT ARO-SMT CARMA APEX, ASTE, ALMA Plateau de Bure IRAM 30m SPT LMT

  • Earth-sized mm/sub-mm VLBI array
  • Existing and Planned telescopes.
  • Accesses resolutions of ~10 mas,

 Sufficient to resolve horizons of M87 & Sgr A*

Haystack APEX, ASTE, ALMA SPT

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SLIDE 6

Fermi Bubbles Workshop 12.4.2013

SMA, JCMT SMT CARMA

Data already exists on Hawaii-CARMA-SMT

  • Doeleman et al., Nature, 455, 78 (2008)

𝐸~37 ± 14 𝜈𝑏𝑡~0.7 𝐸𝐼

  • Fish et al., ApJ, 727, 36 (2011)
  • Doeleman et al., Science, 338, 355 (2012)

FIRST DATA!

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SLIDE 7

SMA, JCMT ARO-SMT CARMA APEX, ASTE, ALMA Plateau de Bure IRAM 30m SPT LMT Haystack APEX, ASTE, ALMA SPT

7 8 9 10 11 12 13 Courtesy of Vincent Fish

Fermi Bubbles Workshop 12.4.2013

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SLIDE 8

M87

  • Sgr A*

M87

THE STATE OF EHT DATA TODAY

Fermi Bubbles Workshop 12.4.2013

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SLIDE 9

PHYSICAL MODELS FOR LOW-LUMINOSITY AGN

Modeling Priors Empirical Priors

SPIN OF SGR A*

Fermi Bubbles Workshop 12.4.2013

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SLIDE 10

PHYSICAL MODELS FOR LOW-LUMINOSITY AGN

Modeling Priors Empirical Priors

Low Spin High Spin SPIN OF SGR A*

Fermi Bubbles Workshop 12.4.2013

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SLIDE 11

GETTING AT SGR A*’S SPIN

a~0+0.64+0.86 q=68+5+8

  • 20-28 deg.

x=-52+17+33

  • 15-24 deg.

Inclination Spin Magnitude

Our accretion model is wrong!

Observations are easy to fit Non-accretion physics is important!

Fermi Bubbles Workshop 12.4.2013

SPIN OF SGR A*

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SLIDE 12

Fermi Bubbles Workshop 12.4.2013

SPIN OF SGR A*

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SLIDE 13

Fermi Bubbles Workshop 12.4.2013

SPIN OF SGR A*

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SLIDE 14

Fermi Bubbles Workshop 12.4.2013

SPIN OF SGR A*

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SLIDE 15

𝜘, 𝜒 , Θ, Φ0 , ro, a, dir

SPIN/INCLINATION FROM DISK LENSE-THIRRING PRECESSION

Fermi Bubbles Workshop 12.4.2013

SPIN OF SGR A*

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SLIDE 16

𝜘, 𝜒 , Θ, Φ0 , ro, a, dir

SPIN/INCLINATION FROM DISK LENSE-THIRRING PRECESSION

Fermi Bubbles Workshop 12.4.2013

SPIN OF SGR A*

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SLIDE 17

SGR A*’S NATURAL PRECESSION RATE

𝑈

𝑞𝑠𝑓𝑑~ 𝑀𝑒𝑗𝑡𝑙

𝜐𝑀𝑈 ~ 𝐻𝑁 𝑑3 𝑠

𝑗 1/2𝑠 𝑝5/2

10 𝑏 sin Θ ~ 2 𝑏 𝑠

𝑝

103

5/2

yr

SPIN OF SGR A*

S2 periapse ~3 × 103 𝐻𝑁/𝑑2

 Comparable to timescales already probed by the EHT!

Fermi Bubbles Workshop 12.4.2013

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SLIDE 18

SPIN-DISK SIZE POSTERIOR PROBABILITY

Fermi Bubbles Workshop 12.4.2013

SPIN OF SGR A*

Sgr A*: Low spin (if at all)!

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SLIDE 19

MODELING M87: GRMHD JETS

  • Blanford-Znajek/Blandford-Payne:

Electromagnetic extraction of black hole spin/disk angular momentum.

  • Large-scale ordered magnetic fields
  • Canonical Structure:
  • MHD Disk
  • Magnetically dominated wind
  • Force-free, roughly parabolic jet

McKinney & Blandford (2009)

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

𝐸 = 40 ± 2 𝜈𝑏𝑡

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SLIDE 20

MODELING M87: GRMHD JETS

  • Blanford-Znajek/Blandford-Payne:

Electromagnetic extraction of black hole spin/disk angular momentum.

  • Large-scale ordered magnetic fields
  • Canonical Structure:
  • MHD Disk
  • Magnetically dominated wind
  • Force-free, roughly parabolic jet

McKinney & Blandford (2009)

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

M87 Jet Widths

𝐸 = 40 ± 2 𝜈𝑏𝑡

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SLIDE 21

MODELING M87: GRMHD JETS

  • Blanford-Znajek/Blandford-Payne:

Electromagnetic extraction of black hole spin/disk angular momentum.

  • Large-scale ordered magnetic fields
  • Canonical Structure:
  • MHD Disk
  • Magnetically dominated wind
  • Force-free, roughly parabolic jet

McKinney & Blandford (2009)

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

M87 Jet Widths

𝐸 = 40 ± 2 𝜈𝑏𝑡

Hada et al. (2011)

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SLIDE 22

SPIN OF M87: ROUGH CUT

Give non-spinning black holes best chance:

  • Jets are disk driven
  • Jets turn on (nearly)

immediately  Jets start out slow (𝚫~𝟐 − 𝟑), emission scale ~ ISCO

SPIN OF M87 Chris Fach

Fermi Bubbles Workshop 12.4.2013

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SLIDE 23

SPIN OF M87: ROUGH CUT

Give non-spinning black holes best chance:

  • Jets are disk driven
  • Jets turn on (nearly)

immediately  Jets start out slow (𝚫~𝟐 − 𝟑), emission scale ~ ISCO

SPIN OF M87 Chris Fach EHT size limit

Fermi Bubbles Workshop 12.4.2013

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SLIDE 24

MODELING M87: GRMHD JETS

  • Blanford-Znajek/Blandford-Payne:

Electromagnetic extraction of black hole spin/disk angular momentum.

  • Large-scale ordered magnetic fields
  • Canonical Structure:
  • MHD Disk
  • Magnetically dominated wind
  • Force-free, roughly parabolic jet

McKinney & Blandford (2009)

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 25

“SIMPLE” JET MODELS

  • Axisymmetric & Stationary (+poloidal struc)
  • Particle inertia irrelevant:
  • + Boundary conditions at disk/black hole!

𝑮𝑀 = 𝜍𝑭 + 𝒌 × 𝑪 = 0

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 26

“SIMPLE” JET MODELS

  • Axisymmetric & Stationary (+poloidal struc)
  • Particle inertia irrelevant:
  • + Boundary conditions at disk/black hole!

𝑮𝑀 = 𝜍𝑭 + 𝒌 × 𝑪 = 0

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

low RΩ

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SLIDE 27

“SIMPLE” JET MODELS

  • Axisymmetric & Stationary (+poloidal struc)
  • Particle inertia irrelevant:
  • + Boundary conditions at disk/black hole!

𝑮𝑀 = 𝜍𝑭 + 𝒌 × 𝑪 = 0

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

intermediate RΩ

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SLIDE 28

“SIMPLE” JET MODELS

  • Axisymmetric & Stationary (+poloidal struc)
  • Particle inertia irrelevant:
  • + Boundary conditions at disk/black hole!

𝜄

Choosing BCs = choosing Ω(r) & Γ∞

𝑮𝑀 = 𝜍𝑭 + 𝒌 × 𝑪 = 0

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

tan 𝜄 ~ 𝑤𝐵 𝑆Ω ~ 𝐶𝑄 𝐶𝜚 ~𝛾∞

−1

large RΩ

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SLIDE 29

“SIMPLE” JET MODELS

  • Axisymmetric & Stationary (+poloidal struc)
  • Particle inertia irrelevant:
  • + Boundary conditions at disk/black hole!

Choosing BCs = choosing Ω(r) & Γ∞

𝑮𝑀 = 𝜍𝑭 + 𝒌 × 𝑪 = 0

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

tan 𝜄 ~ 𝑤𝐵 𝑆Ω ~ 𝐶𝑄 𝐶𝜚 ~𝛾∞

−1

large RΩ

𝜄 Ω 𝑠

High spin low spin

Disk Friendly!

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SLIDE 30

FULL MHD VS. SIMPLE FORCE FREE

Disk Wind Jet

Fermi Bubbles Workshop 12.4.2013

SPIN OF M87

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SLIDE 31

FROM STRUCTURE TO EMISSION

Particle acceleration in the jet!

AEB & Loeb (2009) Dexter, McKinney & Agol (2012)

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 32

RESOLUTION, COOLING TIMES & PARAMETERIZING IGNORANCE

Cooling length from injection at 100 G Lensed Horizon size

  • Particle acceleration

smoothed over jet on EHT scales!

  • Places lower limit on

density of nonthermal electrons

  • Parameterize by typical

load radius, and conserve thereafter.

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 33

EMPIRICAL PRIORS

  • Optical super-luminal motion of

“knots” (6c at >1”, Γ∞~𝟔)

  • Radio super-luminal motion of

“knots” (~2.3c at few mas)

  • Orientation of large-scale jet (E-W)
  • Core Dominance
  • Spectra?

Courtesy of Craig Walker

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 34

EMPIRICAL PRIORS: SPECTRA OF WHAT?

>1” 0.1”-1” 1 mas-0.1” <1 mas SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 35

EMPIRICAL PRIORS: SPECTRA OF WHAT?

Strong non-VLBI constraint on jet models! >1” 0.1”-1” 1 mas-0.1” <1 mas SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 36

A MODEL FAMILY FOR M87

Load radius

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 37

A MODEL FAMILY FOR M87

Load radius Black hole spin

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 38

FIRST FITS: EXISTENCE

20 2 10

𝜓2

97 102

min 𝜓^2/DOF ~ 97/180! (cf. Gaussian ~ 130/184!)

Loading Radius in 𝐻𝑁/𝑑2 Black hole spin

Fermi Bubbles Workshop 12.4.2013

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SLIDE 39

FIRST FITS: SOME CHECKS

Loading radius Jet position angle (E of N), from mm-VLBI alone! 𝑄 𝑆, 𝜊 𝑄 ~70∘!

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 40

FIRST FITS: SOME CHECKS

Fermi Bubbles Workshop 12.4.2013

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SLIDE 41

FIRST FITS: THE SPIN OF M87

M87: (Very) high spin!

Caution: spin calibration not good near a~1

SPIN OF M87

Fermi Bubbles Workshop 12.4.2013

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SLIDE 42

A TALE OF TWO BLACK HOLES SGR A*

  • Low accretion rate  RIAF
  • Flat radio spectra

+ break at 1mm

  • 𝐶~102 G
  • Well fit by physically

motivated models

  • No prominent jet
  • Low spin!

M87

Fermi Bubbles Workshop 12.4.2013

  • Low accretion rate  RIAF
  • Flat radio spectra

+ break at 1mm

  • 𝐶~102 G
  • Well fit by (surprisingly simple)

physically motivated models

  • Prominent jet
  • High spin!

First empirical evidence that black hole spin is important in AGN jets!