late Oct.,>20

Paris Center for Astrophysics Cambridge Cesena

Paris Center for Astrophysics Cambridge Cesena

Paris Center for Astrophysics Cambridge Cesena

Center for Astrophysics Cambridge Paris CEA Office 153 Cesena

..and now: Relativistic Jets Giulia Migliori - 15/03/2016 4C29.30 z=0.064 (Siemiginowska+12)

Jets in Active Galactic Nuclei radio lobe kpc jet narrow line clouds blazar region broad line clouds Giulia Migliori - 15/03/2016 disk SMBH molecular torus

Jets in Active Galactic Nuclei: motivational slide impact on the host galaxy/cluster: Cygnus A (Wilson+00) Cen A jet (0.8-3 kev) Worrall+08 Candidate sources of UHECRs: Fermi Bubbles: jet activity in the MW?

Jets in Active Galactic Nuclei: some questions What is their structure & composition? How do they form? How do they interact with their environment?

Radio Duty Cycle radio galaxy radio luminosity J1 J2 J3 NE2 NE1 J4 SW1 SW2 d) high power low power re-started giant dying radio galaxy size/age

Young Radio Sources NE2 NE1 10 pc SW1 SW2 Wu et al. (2013) d) z=0.0765 1.406 kpc/ linear size <1kpc; symmetric, two-sided radio morphology, dominated by minilobes/hotspots; estimated ages from the hot spots advance velocities: <10 3 yrs J1 J2 J3 J4 Excess of young sources in catalogs of radio sources: intermittent radio activity? dense medium preventing the expansion of the radio source?

Young Radio Sources in X-rays X-ray sample (16 sources, z<1.0): Probing the environment: 100 OQ208 0108 1607 NH(z) [10 22 cm 2 ] 10 1 0.1 2021 1843 0035 0710 1511 1946 1943 1031 1934 2352 1718 0.01 Siemiginowska+2016 all detected with snapshot observations 0 1000 2000 3000 Age [years] moderate column densities in the majority of the sources: no dense environment

Young Radio Sources in X-rays NE2 NE1 z=0.0765 1.406 kpc/ d) 10 pc SW1 SW2 J1 J2 J3 J4 Wu et al. (2013)

Young Radio Sources in X-rays Origin of the emission? NE2 NE1 z=0.0765 1.406 kpc/ d) I. Quasar 10 pc SW1 SW2 J1 J2 J3 J4 II. Jet Wu et al. (2013) UV -disk IR - dust III. Lobe 1kpc Stawarz+2008 jet model in Migliori+2012,2014

Young Radio Sources in gamma-rays The answer is in the gamma-rays: radio - IR - optical - UV - X-ray - γ-ray synch disk+ corona IC νf ν The jets/lobes can produce non-thermal gamma-ray emission detectable with Fermi-LAT ν

Young Radio Sources in gamma-rays PKS 1718-649 (z=0.014, ~100yrs): detection in gamma-rays with 7yrs Fermi-LAT observations Tingay, de Kool (2003), 22 GHz VLBI radio imaging 7 mas ~ 2 pc >200 MeV; 0.2 deg/pix 3FGL J1728.0-6446 7yrs best fit pos. (gtfindsrc) PKS 1718-649 radio pos. High-energy emission from the compact radio lobes? preliminary: Ljet,kin Ldisk Migliori+, in prep. Faint, non variable gamma-ray emission Sobolewska+, in prep.

Young Radio Sources in gamma-rays Testing the lobe scenario: ALMA NuSTAR CTA?

Jets in Active Galactic Nuclei: structure & energetics RGB J1512+020A (z=0.2) X-ray/gamma-ray blazar component 13 /45 kpc X-ray kpc jet radio lobe

Jets in Active Galactic Nuclei: tracing the jet emission ffiffi integrated jet power from the radio lobes X-ray kpc jet jet power through the linear scale γ-ray blazar component

Jets in Active Galactic Nuclei: tracing the jet power jet power from the radio luminosity @151MHz (Willott+99) Ljet,kin=3 10 21 f 3/2 L151 6/7 erg s -1 Ljet,kin~10 45 erg s -1 jet power from SED modeling of the γ-ray blazar component Ljet,kin~10 44-46 erg/s LogνFν [erg cm -2 s -1 ] r~10 16 cm<rblr (Rblob~10 15 cm) theta~4, Γbulk=12, B=2.1 G (UB/Ue=0.3) Logν [Hz] >10% of the initial jet power transported to kpc scales

Jets in Active Galactic Nuclei: pc νf ν accretion & ejection radio - IR - optical - UV - X-ray - γ-ray disk+ corona synch IC RGB J1512+020A (z=0.2) synchrotron Kitt Peak spectrum ν SDSS quasar template (Vanden Berk+ 01) host galaxy template (Mannucci+ 01) SDSS spectrum UVOT Galex

Jets in Active Galactic Nuclei: accretion & ejection Ljet,kin 10 44 erg s -1 disk luminosity: 10 44 erg s -1 Ljet,kin Ldisk: the mechanism responsible for the jet formation is maximally efficient in extracting the BH rotational energy (see also Ghisellini+ 11)

From Quasar to Microquasar: Cygnus A, z=0.056/600 Mly 1.032 kpc/arcsec 10 8-9 Msun, 10 6-7 yrs GRS1915+105, 11000 pc Mirabel+1994 10-18 Msun >60

XTE J1550-564 western jet Microquasar: Time lapse of a jet-ism interaction March 11 2002 June 19 2002 Sept 24 2002 June 28 2003 0.3-7.0 kev 0ct. 23 2003 Migliori et al. in prep.

XTE J1550-564 western jet Microquasar: Time lapse of a jet-ism interaction March 11 2002 June 19 2002 Sept 24 2002 June 28 2003 0.3-7.0 kev 0ct. 23 2003 Migliori et al. in prep.

Microquasar: Time lapse of a jet-ism interaction Jets dynamics: nism: 1 cm -3 ballistic expansion jet deceleration East Jet West Jet low density cavity dynamical models: Hao&Zhang+ 09;Steiner+ 12 West Jet dynamics: centroid vel. first to last obs.: vrel=0.07c tail vel. first to last obs.: vrel=-0.12c

Future Perspectives Observations at low radio frequencies (LOFAR) will tell us more on the radio duty cycle; High sensitivity radio observations will look for radio jets in radio quiet sources; Multi-wavelength all-sky survey (LOFAR/SKA, LSST, EROSITA/ SVOM, CTA) will monitor radio transients (blazars, microquasars, GRBs, SNs..);