VLBA 7 mm/43 GHz Stacked Image (BU Blazar Group) Kazu...

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Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30 The Global “Radio’’ Structure of the Archetypical Quasar 3C 273 Kazu Akiyama ( MIT Haystack Observatory / JSPS Fellow ) VLBA 7 mm/43 GHz Stacked Image (BU Blazar Group) Keiichi Asada, Masanori Nakamura (ASIAA) Kazuhiro Hada, Hiroshi Nagai (NAOJ) Vincent L. Fish, Colin Lonsdale (MIT Haystack) Shep Doeleman (MIT Haystack/CfA) et al.

Transcript of VLBA 7 mm/43 GHz Stacked Image (BU Blazar Group) Kazu...

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

The Global “Radio’’ Structure of the Archetypical Quasar 3C 273

Kazu Akiyama( MIT Haystack Observatory / JSPS Fellow )

VLBA 7 mm/43 GHz Stacked Image (BU Blazar Group)

Keiichi Asada, Masanori Nakamura (ASIAA) Kazuhiro Hada, Hiroshi Nagai (NAOJ)Vincent L. Fish, Colin Lonsdale (MIT Haystack) Shep Doeleman (MIT Haystack/CfA) et al.

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

Jet Collimation: Central questions

106 Rs

Cygnus A at 5 GHz- Highly collimated outflowOpening Angle: ~ few degree

How? Where?

- Theoretical Paradigm:

Hoop Stress(assist collimation)

Coulomb Force (AGAINST collimation)

Self Collimation by Magnetic Hoop Stress(Blandford & Payne 82, Sakurai 85, …. )

Not sufficient for relativistic jets

External confinementby the circum-jet medium(e.g. Nakamura+06, Komissarov+07, Tchekhovskoy+10, Toma & Takahara 13)

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

Lessons from Nearby Low Luminosity Radio Galaxies

Bond

i rad

iusISCO

VLBA at 43 GHzVLBA at 15 GHzEVN at 1.6 GHz MERLIN at 1.6 GHzVLBA core at 43 GHzVLBA core at 86 GHzEHT core at 230 GHz

(Asada & Nakamura 12; Doeleman+12, Nakamura & Asada 13; Hada+13, 16)

Parabolic stream

(z ∝ width

1.7 )

Conical S

tream

(z ∝ w

idth1.0 )

B.H.

CircumNuclearMedium (Giant RIAF?)

R.C.S105 Rs

107 Rs

103 Rs

1 Rs

Collimation inside Bondi radii (~105 Rs)

M 87 (Asada+, Hada+) 3C 84 (Nagai+14) Cyg A (Boccardi+14)

M 87

de-projected distance from the core (rs)

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

The Stream Line in Blazars (particularly Quasars)

Historically the conical jet has been assumed for modeling emission(e.g. Blandford & Konigl 1979; Marcher & Gear 1985; many papers in literature)

Visible region in the jet could be different to LLRGs (Spine vs Sheath) (e.g. Ghisellini et al. 2005; Tavecchio & Ghisellini 2014; Sikora et al. 2016)

The geometry of the accretion flow would be different for quasars LLAGN: Giant RIAF? (Narayan &Fabian 11; Hot quasi-spherical flow) — pressure can be balanced with the jet pressure (M87; Hada+2016) Quasars: Thin or Slim Disk — The disk can not confine the jet. Need winds?

The jet power is also different for quasars

Many intriguing questions but NO measurements

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

3C 273: the Archetypical Quasar

- Hosts a very massive black hole (6.6x109 Msolar ;Paltani & Turler 2005)

- One of the First Quasars (Schmidt 1963)- One of the nearest radio-loud quasars (z = 0.158)

(Bahcall et al. 1995)

- Linear scales (1 mas=2.7 pc=4.8x103 Rs)

- One of the brightest sources in radio regimes- Resolved transverse structure on wide ranges of spatial scales

(MOJAVE; stacked)(BU Blazar group; stacked)

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

Observational Data

MERLIN 1.6 GHz

kilo pc (z ~108-109 Rs)

100 pc (z ~106-107 Rs)VLBA 1.6 GHz (8 epochs from 2008, 2009, 2011)

10 pc (z ~105-106 Rs)

VLBA 15 GHz (MOJAVE: 65 epochs during 2007-2014)

1 pc (z ~104-105 Rs)VLBA 43 GHz (BU Blazar; 76 epochs during 2007-2014)

VLA 22 GHz

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

Results: Collimation Profile

Conical S

tream

(z ∝ w

idth1.0

4 )

Parabolic stream

(z ∝ width

1.98 )

kpc Lobe

Bending

Preliminary

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

Discussion: Comparison to M87

BH

CircumNuclearMedium (Giant RIAF?)

R.C.S

105 Rs

107 Rs

103 Rs

1 Rs

M 87

105 Rs

107 Rs

103 Rs

1 Rs

3C 273

Preliminary

3C 273

M 87

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

Discussion: Comparison to classical BP & BZ jets

EHT

BP82 (a=0.5-0.998)

(Accr

etion-flow D

riven

)

GMVA+ALMA

Preliminary

BZ77 (a=0.5-0.998)

(BH-spin Driven)

BZ & BP solutions: Outermost streamline foranalytic force-free solutionsCourtesy of Masa Nakamura

3C 273

M 87

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

Summary

• We measure the stream line of the global jet in 3C 273 from sub-pc to kpc scales, for the first time among the high-powered quasar sources.

• The global structure of the 3C 273 jet has a break in its stream line very similar to much lower-powered M87

~5 mas - 10 arcsec (>105-106 Rs): Conical

< ~5 mas (<105-106 Rs): Parabolic

• The quasar jets are also collimating at the inner jet as well as LLAGN’s jets

• EHT+ALMA and GMVA+ALMA observations will be extremely important to survey the active collimation region of the quasar jets.

How to collimate the jets from thin/slim disks? Detailed comparison to (GR)RMHD simulations will be important

Kazu Akiyama, Blazars through Sharp Multi-Wavelength Eyes, Malaga, Spain, 2016/05/30

Stream-line AnalysisSTEP 1: Circularly slice the image

STEP 2: Measure the position angle profile

STEP 3: Measure the FWHM size of the linear slice