Jets in (nearby) radio loud AGN

Elisabetta Liuzzo

INAF-IRA BolognaItalian Node of the ALMA Regional Center

with the contribution of H. Nagai, G. Giovannini, A. Mignano, R. Falomo, V. Casasola, ARC and many

other people

High power

● FRII – Cygnus A

Low power

● FRI – 3C 31

viewing angles + intrinsic relativistic speeds

Unified view of Radio Loud AGNKpc scale

● BL Lac –Mkr 501● FSRQ - 1641+399

* Extended* Compact (projection effect,young RS, other?)

Unified view of Radio Loud AGN????????

● Evolution- LEG/HEG evolve in LEG/HEG (Kunert-Bajraszewska et al. 2010)- Models for FRI from FRII: interaction with ISM (Kaiser & Best 2007);- Hybrid sources (Gawroński et al. 2006);- fainding sources (Alexander et al. 2000, Giroletti et al. 2005);- short lived C sources and intermediate activity ~104 yrs (Czerny et al. 2009)

New FR0 radio-galaxies(Baldi, R et al. 2015)

HYMORS(Gopal-Krishna & Wiita 2002)FR I on one side, FRII on the other: ambient medium differences?

Parsec -scale jets

One sided morphology dominant (Fig.1). Compactnuclei also at the center of very low power radio coresources (Fig.2) -> ONGOINGONGOING

Environment effects in Low power compact radiogalaxies (Fig.3) and Brightest Cluster Galaxies(Fig.4)-> FUTURE?FUTURE?

Gamma-ray/radio emission not clear --> work also onfaint BL Lacs -> ONGOINGONGOING

AGN jet model: external medium influence,transverse stratification, role of B.

Aim: parsec scale study of statistical propertiesin different class of sources defining a samplefree from selection effects due to orientation

Facilities: with VLBI

Sample: Bologna Complete Sample of 94 nearby(z<0.1) radiosources selected from low frequencycatalogs

RESULTS

References: Liuzzo et al. 2009A,b; 2010, 2013a,b; 2015 in preparation

Fig.2: Recent 18 cm EVN and 6 cm VLBA maps of 3 of the very faintBCS sources.

Fig. 3: Diagnostic Diagrams for Low power compact BCS sources

Fig.1: Aligned structure of 4C 29.30 at different angular resolution.

Fig.4: Z-shaped structure of the BCG 4C 26.42 at different angular resolution.

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ONGOINGONGOINGONGOINGONGOING

ONGOINGONGOING

Why study with ALMA? ALMA sensitivity significantly increases the detection of Fermi sources-> Giroletti et al.

● First detailed morphological studies -> see also Orienti et al.

Why at mm-band?

Radio cm-band highly self-absorbed

The variability in mm band is close in time with the variability athigh energies -> Marti-Vidal et al. 2013 Orienti et al.2013

PKS 1510-089

Opacity effects in mm are less important than in cm.

Frequency(GHz)

rms in 1min(mJy/beam)

angularresolution

(mas)86 0.10 50

230 0.13 15

345 0.20 10

480 0.8 8

650 2.0 5For continuum emission, Cycle 2 capabilities

Why study Fermi sources at mm-band? Origin of the gamma-ray emission

ALMA jet studiesONGOINGONGOING

ONGOINGONGOING

PI: Nagai et al. (Hada, Liuzzo, Giroletti, Orienti, Giovannini...)

mm/submm continuum spectrum of blazars in the close vicinity of their centralengine.

Not the radio core:● Core shift(e.g.M87,Hada);● flat spectrum

Using archivalALMA and SMA calibrators data: ν

SSA ~ 100 GHz

In which frequency can we observe the true jet base?

One zone model is not valid? Stratified jetmodel is needed

Spectral index between B6/B3 and B7/B3

consistent with optically thin spectrum.

B3~ 90GHz, B6 ~ 240 GHz, B7 ~ 300 GHz

Jet modelssynchrotron self-absorbed conical jet plusrelativistic shocks (Blandford-Königl jet)

stratified (MHD) jet with moving hot spots/shocks or filamentary patterns

models

observations

M87 – VLBA 43 GHz

Still unclear: stratification on < 10 R_s scales?

Liuzzo, Falomo, Nagai, Giovannini, Mignano, Treves et al. In prep

Morphology: hotspot (and jet) detected at least up to 320 GHz

SED: consistent with expectation: jet knots and hotspot dominated bysynchrotron component, while in the nucleus a IC component is present athigh energy

To do: spectral index map analysis + compared with Orienti ALMA results on study of hot spots in powerful radio sources.

RESULTS

PKS 0521-365: ALMA results

Preliminary!!

BL Lac objects with multi-ν resolved jets

ALMA Band 6

SED

VLA 15 GHz

ALMA Band 6

Waiting to use Long Baseline Campaign data (?)

B6 image from archival data

Liuzzo, Falomo, Nagai, Giovannini, Mignano, Treves et al. In prep

Fumagalli et al. 2012

CO(1-0) line luminosity vs z in different AGN types Molecular gas contentin different AGN types

L(CO) < 2.9 103 K km s-1 pc-2 : assuming α=4MΘ

K km

s-1 pc-2, M(H2) <1.1 106 MΘ

Low molecular gas content in BL Lacs comparedto quasars? similar to low-z RG (see M87)

ALMA Band 3 contains the CO(1-0) line frequency(rest frame ~ 109,2 GHz)

Free-line continuum rms ~ 1.7 mJy/(100km/s)

OBSERVATIONSRESULTS

VHE sources

PKS 0521-365

PKS 0521-365

Preliminary!!

BL Lacs with multi-ν resolved jetsPKS 0521-365: Search of CO emission line

Dark: detectionsLight: Upper Limits

FSRQs with multi-ν resolved jetsNagai, Liuzzo, Giovanni, et al.

OBSERVATIONS Archival ALMA data in bands 3, 6, 7, 9

Angular resolution: 2-0.2 arcsec

Period :over 2012, ~2min/each obs

Some simultaneously multi-band data(e.g. 2/06/2012 )

Preliminary!!

RESULTS

Colour: Band 6 ~ 230 GHzContours: Band 3 ~ 90 GHzf.c.=3mJy/b, peak=4Jy/b

Chandra ALMA

3C273: ALMA results

Uchiyama et al. 2006

At least up to 230 GHz well resolved jet with knots

Spectrum at 2 June 2012 seems to indicate optically thin/thick transition ~ 100 GHz

H1 SED seems consistent with single-synchrotron model (as Uchiyama et al. 2006 )

Comparison with BL Lac objects results

H1

Misaligned (Fermi) sources in ALMA database

ALMA Continuum Spectrum of the M87 Nucleus

Doi et al. 2013 (...Hada...)

Quasi-simultaneous ALMA data in bands 3, 6, 7,and 9

ALMA angular resolution: 2 – 0.2 arcsec

VLA archival data in 8,4-43 GHz after 2006

OBSERVATIONS ALMA band 3 image show similar structure of

VLA map: nucleus + kpc jet

HST-1 contamination negligible in ALMA band

VLA/ALMA flat spectrum

Spectral break ~ 200 GHz: implicationsin Doi et al. in preparation

RESULTS

Misaligned (Fermi) sources in ALMA database

ALMA CO emission in the nucleus of M 87

Liuzzo, Mignano et al.

OBSERVATIONS Available ALMA data could improve SMA results

(Tan et al. 2006) ?

ALMA band 6, CO(2-1) at 230.54 GHz

In 10s, rms = 6mJy/(100km/s)

Band 6 ~ 230 GHz

Preliminary!! Shifted at ~ 1280 km/sFWHM~ 200km/s

Tentative detection as same as SMA data: total mass gas ~4.3 x 106 M

sun (Tan et al. 2006)

Atomic gas disk revealed by Marchetto et al. 1997

Discriminator of different accretion models

RESULTS

.......ALMA cannot go further than 5 mas!!

Perspectives:

mm-VLBI with ALMA

Why mm-VLBI?Opacity effects and high angular resolution

Credits of Krichbaum

Why not only continuum but also polarization?B-field jet structure

Credits of Krichbaum

Current mm-VLBI at 86 GHz

Credits of Krichbaum

Example of GMVA results

See also 3C 345 (Orienti et al. ), M87 (Hada et al.)

Credits of Krichbaum

mm-VLBI at 230-345 GHz

Credits of Krichbaum

Results of EHT

Credits of Krichbaum

Why mm-VLBI with ALMA? with ALMA sensitivity at least 10 times better

2015: initial ALMA phasing tests are expected.

White papers: 1) Fish et al. 2013 2013arXiv1309.3519F ;

2) A. Zensus, A. Baudry, M. Bremer,Sept. 2013 presented at ESAC.

Credits of Krichbaum

Conclusions

➢ ALMA sensitivity allow an unprecedented study of mm emission of jets in nearby radio sources➢ ALMA operating wavelength are ideal to access regions were gamma rays are most likely

produced in AGNs, increasing the number of Fermi sources studied at mm.➢ As an element of a mm-VLBI array, ALMA will allow us to directly image the SMBH vicinity and

jet launching region.➢ Do not forget the importance of polarization studies at mm band to understand the role and

structure of B in jets