The MIXR sample: Radio-loud AGN through the eyes of 3XMM, WISE, and - - PowerPoint PPT Presentation

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The MIXR sample: Radio-loud AGN through the eyes of 3XMM, WISE, and - - PowerPoint PPT Presentation

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The MIXR sample: Radio-loud AGN through the eyes of 3XMM, WISE, and FIRST/NVSS Beatriz Mingo University of Leicester ARCHES Scientific Workshop Collaborators: Paris, Nov 30 Dec 2 2015 Mike Watson, Gordon Stewart, Simon Rosen, Andrew

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Beatriz Mingo

University of Leicester Collaborators: Mike Watson, Gordon Stewart, Simon Rosen, Andrew Blain (Leicester), Martin Hardcastle (Hertfordshire),Angel Ruiz, Silvia Mateos, Francisco Carrera (IFCA)

The MIXR sample: Radio-loud AGN through the eyes

  • f 3XMM, WISE, and

FIRST/NVSS

ARCHES Scientific Workshop Paris, Nov 30 – Dec 2 2015

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Beatriz Mingo - Radio-loud AGN

Why radio-loud AGN?

  • How relevant are radio-loud AGN?

– RL ~10-20% of the total AGN population, but

(presumably) all AGN have been RL

– RL phase affects environment dramatically and

is fundamental to understand accretion

  • Many Seyferts with jets and lobes! (see e.g.

Croston + 2008, Mingo + 2011, 2012)

  • Advantages for AGN science:

– Select dimmer AGN than optical/X-ray/IR cuts – Low sky density, clean selection – Only selects very nearby starburst galaxies

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Beatriz Mingo - Radio-loud AGN

The (LM)XRB link

FRII RG rad efficient (HERG) FRI RG rad inefficient (ADAF/RIAF) (LERG) RQ rad efficient winds LERG/HERG =/= FRI/FRII same jets in LERG/HERG → jet can't be originated in classical accr. disk AGN can develop jets while in this region, XRB, pulsars, WD, etc cannot, as they can't get enough magnetic flux accretion rate (Tchekhovskoy+ 2011, Sikora & Begelman 2013)

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Beatriz Mingo - Radio-loud AGN

The Idea

  • 3XMM + WISE +

NVSS/FIRST

– What does the WISE

c/c plot look like?

  • Data quality criteria:

– S/N>5 in w1, w2,

S/N>3 in w3

– No X-ray extended – “good” radio

  • ARCHES X-matching

code (FX Pineau's talk)

Lake + 2012

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Beatriz Mingo - Radio-loud AGN

The goals

  • The MIXR sample: build the largest (to date)

uniform Mid-IR + X-ray + Radio catalogue of AGN + star-forming galaxies.

  • Establish diagnostics to quickly characterise

sources even when no z available

– Useful for big data (SKA/Athena/JWST/E-ELT...)

  • Address science questions

– Diagnose/disentangle SF & AGN activity? – Lbol vs Q: origin of the scatter? – How biased are MIR/X-ray selected samples?

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Beatriz Mingo - Radio-loud AGN

It's complicated...

1) Collapse FIRST sources within 30” (Magliocchetti et al. 1998) 2) USE FIRST flux unless NVSS larger by 5 sigma 3) Exclude extended X-ray sources 4) Xmatch

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Beatriz Mingo - Radio-loud AGN

All that work to get just ~1400 sources

1008 AGN (577 z) 145 Ellipticals (94 z) 222 Spirals (149 z) 174 Starburst (114 z)

W3 S/N>3 eliminates 45% of the sample SDSS z eliminates another 45% (still good result!)

Beware: populations overlap!

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Beatriz Mingo - Radio-loud AGN

Diagnostics: Flux/mag triage

Strong SF correlation, also tells us about “radio-shy” AGN Wide range of radio fluxes for given mid-IR magnitude → jet regulation? Need L to verify

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Beatriz Mingo - Radio-loud AGN

Diagnostics: Flux/mag triage

SF correlation, messier than IR/radio, but still reliable AGN correlation: many “radio-shy” AGN from the previous plot are X-ray bright LERG/LINER have systematically lower X-ray fluxes

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Beatriz Mingo - Radio-loud AGN

Get some z's

For each pop. The W3 rejected sources distrib. peaks at larger z → distance, not evolution

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Beatriz Mingo - Radio-loud AGN

Luminosity diagnostics (1)

Radio/IR correlation for SF looks wonderful! LERG clearly separated from the rest AGN: wide range of radio L for a given mid-IR L → Mingo+ 2014

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Beatriz Mingo - Radio-loud AGN

Luminosity diagnostics (2)

SF, LERG/LINER and AGN populations clearly separated Wide range of radio L for given X-ray L Several Spirals harbouring AGN!

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Beatriz Mingo - Radio-loud AGN

RL AGN, RQ AGN and LERG/LINER

RL AGN: 1.5 sigma above SF correlation in Lmid-IR/Lradio RQ AGN: Below 1.5 sigma in the SF correlation, but L2-10 keV >= 5x10^41 erg/s LERG/LINER: RL AGN with L2-10 keV < 5x10^41 erg/s

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Beatriz Mingo - Radio-loud AGN

Rawlings & Saunders 1991 = wrong?

...probably?

AGN CAUTION When plotting sources with unclear radio emission! Timescales probably introduce a lot of scatter in this correlation (more than we suspected in Mingo et al. 2014) LERG/LINER certainly don't follow the same trend!

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Beatriz Mingo - Radio-loud AGN

Beware of the bias!

  • Make sure to

compare like with like!

– Most MIR AGN

samples ignore Seyferts

– Many X-ray AGN

samples ignore RL sources

– More cat. = more

diagnostics, but also more bias!

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Beatriz Mingo - Radio-loud AGN

MIXR Conclusions

  • Diagnostic plots: useful when you don't have z!

– SF radio/IR correlation is tight and fairly reliable

  • Useful also to identify RQ AGN
  • Lbol/Q does have large scatter

– Still unclear why... if we can understand the

timescales involved we can also shed light on the AGN vs star formation conundrum.

  • Beware of the bias!

– w1-w2>0.5 leaves out lots of interesting AGN – X-ray samples biased against RL sources – More data, please! :)