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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.
)
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