Probing the efficiency of the AGN feedback in young radio sources: - - PowerPoint PPT Presentation

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Probing the efficiency of the AGN feedback in young radio sources: - - PowerPoint PPT Presentation

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Probing the efficiency of the AGN feedback in young radio sources: the case of PKS1934-63 Francesco Santoro Raffaella Morganti PhD student Clive Tadhunter santoro@astro.rug.nl Marvin Rose Francesco Santoro - santoro@astro.rug.nl Malta - The

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

Probing the efficiency of the AGN feedback in young radio sources:

the case of PKS1934-63

Raffaella Morganti Clive Tadhunter Marvin Rose

Francesco Santoro PhD student santoro@astro.rug.nl

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

Rupke & Veilleux Mc Namara QUASAR mode RADIO Mode

Mrk 231 Galaxy cluster MS 0735

Probing the efficiency of the

AGN feedback

in young radio sources:

the case of PKS1934-63

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

Probing the efficiency of the

AGN feedback

in young radio sources:

the case of PKS1934-63

Models require efficiencies ~5-10% AGN feedback & Star Formation Quenching

Silk,J.+2012

Fabian 1999; di Matteo et al. 2005; Springel et al. 2005

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

  • High Radio Power P1.4GHz >1025 W/Hz
  • Early evolutionary stages YOUNG age 102-105 yr
  • Found in gas rich ETGs / merging systems
  • Hosting atomic, ionised, molecular gas extreme outflows

OUR SAMPLE

PKS0023-26 , PKS0252-71 PKS1814-63 , PKS2135-209 , 3C 459

PKS1934-63

X-Shooter

Probing the efficiency of the AGN feedback in young radio sources:

the case of PKS1934-63

slit spectroscopy UVB + VIS + NIR

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

z=0.1824 Radio age~1.6 x103 yr Very Compact Dradio~130 pc Very Powerful P1.4GHz = 1027.2 W/Hz Merging

Roche+2016

Ramos Almeida+2011

Tziomis+2002

Probing the efficiency of the AGN feedback in young radio sources:

the case of PKS1934-63

X-Shooter

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

PKS1934-63

X-Shooter

[OIII] line

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

[OIII]5007Å

[OIII] line

4 KINEMATICAL COMPONENTS 2 Narrow 1 Broad 1 Very Broad component

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

[OIII]5007Å OUTFLOWING GAS

[OIII] line

4 KINEMATICAL COMPONENTS 2 Narrow 1 Broad

1 Very Broad

component

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

[OIII]5007Å

[OIII] line

Main Goal

mass outflow rate kinetic power efficiency OUTFLOWING GAS 4 KINEMATICAL COMPONENTS 2 Narrow 1 Broad

1 Very Broad

component

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

mass outflow rate kinetic power efficiency

M

  • E
  • E / Lbol
  • Models require efficiencies ~5-10% for

Silk,J.+2012

Fabian 1999; di Matteo et al. 2005; Springel et al. 2005

AGN feedback & Star Formation Quenching

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

mass outflow rate L(H𝛾) vout Ne Rout

  • Outflow Velocity

Gas electron density Outflow Radius

M

  • H𝛾 Luminosity
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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

L(H𝛾) Ne Rout

  • n density

Outflow Radius Luminosity

vout Outflow Velocity

vout= -325 km/s FWHM= 2090 km/s vmax= -2500 km/s from the kinematical model

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

vout

Rout Outflow Radius

Outflow V Tziomis+2002

Rout < 1Kpc Rout > 65 pc

from radio lobes separation

The outflow is COMPACT spatially unresolved

L(H𝛾) Luminosity Ne

  • n density
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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

Ne Gas electron density

High density ISM Blended lines

Compact Sources outflows

L(H𝛾) Rout Outflow Radius Luminosity vout Outflow V

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

Trans-auroral lines method (Holt et al. (2011)

Ne Gas electron density

L(H𝛾) Rout Outflow Radius Luminosity vout Outflow V

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

Ne Gas electron density

Fit of the lines with the [OIII]5007Å model

L(H𝛾) Rout Outflow Radius Luminosity vout Outflow V

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

Ne Gas electron density

AGN photoionization models

FIX spectral index and photoionisation parameter

L(H𝛾) Rout Outflow Radius Luminosity vout Outflow V

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

Ne Gas electron density

Ne E(B-V)

L(H𝛾) Rout Outflow Radius Luminosity vout Outflow V

AGN photoionization models

FIX spectral index and photoionisation parameter VARY density and reddening

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

Ne Gas electron density

Narrow components Ne~103 cm-3 Broad component Ne~104.5 cm-3 Ne~105.5 cm-3 Very broad component

L(H𝛾) Rout Outflow Radius Luminosity vout Outflow V

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

mass outflow rate L(H𝛾) vout Ne Rout

  • Outflow Velocity

Gas electron density Outflow Radius

M

  • H𝛾 Luminosity

Very broad component

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

mass outflow rates kinetic power efficiency

E

  • M
  • (vout2

Lbol~1.5 x1045 erg/s

from L[OIII]

E / Lbol

  • M
  • +FWHM2)
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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

M

  • E
  • <

< 0.02 M⦿/yr < < 0.19 M⦿/yr

5.5x1040 erg/s < < 5.1x1041 erg/s

3.5x10-5 3.3x10-4 E / Lbol

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

5-10% for classical models Are we missing outflowing gas? Is it a ?

3.5x10-5 3.3x10-4 E / Lbol

  • ~0.5% ’multi-staged’ outflows (e.g. Hopkins & Elvis 2010)

< <

PKS1934 PKS1733 3C459 PKS0023 PKS0252 PKS1151 PKS1306 PKS2135 PKS1549 PKS1345

multiphase outflow

10-4<E / Lbol<1.5

  • 0.01<M<3 M⦿/yr
  • similar results:

Rose et al.2017, Villar-Martín et al 2016

10−5 -10−4 - Kurosawa et al. (2009)

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

multiphase outflow

NIR - H2 warm ionised gas

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

multiphase outflow

compact outflow

Ionised gas atomic & warm molecular gas

no evident sign of

  • utflow

Is PKS 1934-63 too young ?

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

… a possible scenario … AGN - ISM interaction ionise the gas Cold gas forms in post-shock cooling regions

multiphase outflow

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

multiphase outflow

… a possible scenario … AGN - ISM interaction ionise the gas Cold gas forms in post-shock cooling regions

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

multiphase outflow

COMPACT RADIO SOURCES (ages 102-5 yr) can be used to test the scenario SIMULATION

H2 and CO start to form ~105 yr after the start of the AGN-ISM interaction (Richings & Faucher-Giguere 2017)

… a possible scenario …

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

multiphase outflow

COMPACT RADIO SOURCES (ages 102-5 yr) can be used to test the scenario COMPACT RADIO SOURCES (ages 102-5 yr) can be used to test the scenario

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

multiphase outflow

COMPACT RADIO SOURCES (ages 102-5 yr) can be used to test the scenario PKS 1934-63 might be too young to have a cold gas outflow COMPACT RADIO SOURCES (ages 102-5 yr) can be used to test the scenario

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Francesco Santoro - santoro@astro.rug.nl Malta - The role of gas in Galaxy Dynamics - Oct 2017

Take home messages

Density is a crucial parameters to characterise outflows Observed outflow efficiencies are far from the 5 -10% required by classical models Compact radio sources can test if time is the main driver to explain the multiphase outflow properties More results from the rest of the sample