The collimation structure of the relativistic jet of 3C 273 revealed - - PowerPoint PPT Presentation

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The collimation structure of the relativistic jet of 3C 273 revealed - - PowerPoint PPT Presentation

Feb 06, 2024 301 likes •502 views

Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ The collimation structure of the relativistic jet of 3C 273 revealed by GMVA+ALMA Hiroki Okino (U.Tokyo / NAOJ) Collaborators Kazunori Akiyama (NRAO / MIT) Keiichi Asada (ASIAA)

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

The collimation structure of the relativistic jet of 3C 273 revealed by GMVA+ALMA

Hiroki Okino (U.Tokyo / NAOJ)

Collaborators Kazunori Akiyama (NRAO / MIT) Keiichi Asada (ASIAA) GMVA+ALMA 3C273 Collabolation Team

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Opened question for jets in Active Galactic Nuclei

  • Formation
  • Collimation

& Acceleration A key clue: Shape of the jets!

VLBA @5GHz Cygnus A

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Jet collimation of LLAGN : M87

Nakamura+ 2018

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Jet collimation of LLAGN : M87

Nakamura+ 2018

Transition at close to the Bondi radius rB~ 105 rg

z R ∝ e.g. NGC6251** Tseng+ 2016 NGC4261 Nakahara+ 2016 1H 0323+342 Hada+ 2018 3C84 Nagai+ 2014 Cygnus A Boccardi+ 2016

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Jet collimation of nearby LLAGN

Nakamura+ 2018

Transition at close to the Bondi radius rB~ 105 rg

z R ∝

Collimation profile is consistent with field lines from the black hole (Nakamura+ 2018)

e.g. NGC6251** Tseng+ 2016 NGC4261 Nakahara+ 2016 1H 0323+342 Hada+ 2018 3C84 Nagai+ 2014 Cygnus A Boccardi+ 2016

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Jet collimation of nearby LLAGN

Nakamura+ 2018

Transition at close to the Bondi radius rB~ 105 rg

z R ∝

Collimation profile is consistent with field lines from the black hole (Nakamura+ 2018)

e.g. NGC6251** Tseng+ 2016 NGC4261 Nakahara+ 2016 1H 0323+342 Hada+ 2018 3C84 Nagai+ 2014 Cygnus A Boccardi+ 2016 z R ∝

How about more powerful AGNs which have higher accretion rate ??

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Target source: Quasar 3C 273

  • One of the most well-known bright quasars (Schmidt 1963)
  • Redshift z=0.158
  • Black Hole Mass ~6.59

10 ✕

9 Msun (Paltani+ 2005)

  • The Largest angular diameter (1 mas= 2.7pc=4.8

10 ✕

3 Rs)

  • Bolometric luminosity ~10^47 [erg/sec] ~ 0.13 - 0.53 Ledd
  • It’s Jet have been studied in multi “scales” and

“wavelengths” in the last decades

Uchiyama+ 2016

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Previous works of 3C 273 jet collimation profile

Akiyama+ 2018 C

  • n

i c a l s t r e a m w i d t h Z ∝

1.17

Parabolic stream width Z ∝

0.47

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Previous works of 3C 273 jet collimation profile

Akiyama+ 2018 C

  • n

i c a l s t r e a m w i d t h Z ∝

1.17

Parabolic stream width Z ∝

0.47

? ?

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Global Millimeter VLBI Array Observations with ALMA

Credit of original map : Max-Planck-Institute for Radioastronomy

Yebes

@3mm/86GHz

Phased ALMA!!

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Global Millimeter VLBI Array Observations with ALMA

Credit of original map : Max-Planck-Institute for Radioastronomy

Yebes

Phased ALMA!!

@3mm/86GHz April 2017, First VLBI session with ALMA 3C 273 Observations (PI: Akiyama)

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

uv-coverages with ALMA

  • ALMA baselines gave us high SNR! (> ~ 100)

80μas 40μas

Baseline including ALMA

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

uv-coverages with ALMA

  • ALMA enabled us to observe with higher resolution in N-S direction!

Baseline including ALMA

80μas 40μas

(N-S) Δθ~70μas

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Preliminary full closure Image

50 50μas beam ✕ convolved image by smili

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

How to measure the jet width?

Jet streamline of 3C273 in this scale does not look straight….

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

How to measure the jet width?

STEP1: Circularly slice the image STEP2: Measure the position angle STEP3: Measure the jet width perpendicular to position angle

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Preliminary collimation profile 3C273

This work!!

Parabolic stream width Z ∝

0.47

C

  • n

i c a l s t r e a m w i d t h Z ∝

1.17

Conical stream Parabolic stream

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Comparison with LLAGN:M87

M87 3C273

  • The jet profile of quasar 3C273

also has a transition at ~105 Rs

  • M87
  • LLAGN, RIAF disk
  • 3C273
  • Quasar, Standard thin disk
  • Above two AGNs are different

physical state but very similar collimation profile

3C273 GMVA+ALMA 86GHz

Why? How the disks work with jet?

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Hiroki Okino, 2018.11.30 VLBI conference @Kumamoto univ

Summary

  • We measured the jet streamline of quasar 3C273 at the most

inner region 103-104 Rs with higher angular resolution of first GMVA+ALMA observation.

  • The results from preliminary imaging indicate that 3C273 jet

streamline have transition from conical to parabolic at ~105 Rs.

  • Jet streamline of archetypical quasar 3C273 is quite similar to

that of LLAGN:M87.

  • More careful imaging and theoretical study with GRMHD

simulation are important to understand properties of jets.