TheThe ChandraChandra 3C3C SnapshotSnapshot Survey:Survey: TheThe StoryStory SoSo FarFar AlessandroAlessandro PaggiPaggi1,2

F. Massaro1,2,3,4, D. Axon5,6, B. Balmaverde1, S. A. Baum7,8, S. Bianchi9, A. Bonafede10,11,12, G. Brunetti10, A. Capetti1, C. C. Cheung13, M. Chiaberge14,15, G. Cusumano16, C. J. Donzelli17,18, W. R. Forman19, R. Gilli20, G. Giovannini10,11, P. Grandi20, M. J. Hardcastle21, D. E. Harris19, P. Kharb22, R. P. Kraft19, J. Kuraszkiewicz19, V. La Parola16, E. Liuzzo10, L. Lovisari19, F. D. Macchetto14, K.-H. Mack10, J. P. Madrid23, A. Maselli16, V. Missaglia1,19,24, R. Morganti25,26, C. P. O’Dea7,27, M. Orienti10, R. Paladino10, M. A. Prieto28,29, F. Ricci30, G. Risaliti31,32, A. Rodríguez-Ardila33,34, M. Schirmer35,36, A. Siemiginowska19, W. Sparks14, C. Stuardi10,11, E. Torresi20, G. R. Tremblay19 & B. J. Wilkes19

1INAF-Osservatorio Astrofisico di Torino – Italy; 2Istituto Nazionale di Fisica Nucleare, Sezione di Torino – Italy; 3Dipartimento di Fisica, Università degli Studi di Torino – Italy; 4Consorzio Interuniversitario per la Fisica Spaziale (CIFS) – Italy; 5Department of Physics, Rochester Institute of Technology, Carlson Center for Imaging Science – USA; 6School of Physics and Astronomy, Rochester Institute of Technology – USA; 7Department of Physics and Astronomy, University of Manitoba – Canada; 8Chester F. Carlson Center for Imaging Science, Rochester Institute of Technology – USA; 9Dipartimento di Fisica, Università degli Studi Roma Tre – Italy; 10Istituto di Radioastronomia - INAF Bologna – Italy; 11Department of Physics and Astronomy, University of Bologna – Italy; 12Hamburger Sternwarte, Universitat Hamburg – Germany; 13Space Science Division, Naval Research Laboratory – USA; 14Space Telescope Science Institute – USA; 15Center for Astrophysical Sciences, Johns Hopkins University – USA; 16INAF-IASF Palermo – Italy; 17Instituto de Astronomía Teórica y Experimental IATE, CONICET - Observatorio Astronómico, Universidad Nacional de Córdoba – Argentina; 18Observatorio Astronomico, Universidad Nacional de Córdoba – Argentina; 19Center for Astrophysics, Harvard & Smithsonian – USA; 20INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna- Italy; 21Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire – UK; 22National Centre for Radio Astrophysics - Tata Institute of Fundamental Research – India; 23Australia Telescope National Facility, CSIRO Astronomy and Space Science – Australia; 24Dipartimento di Fisica “Ettore Pancini”, Università di Napoli Federico II – Italy; 25ASTRON, The Netherlands Institute for Radio Astronomy - The Netherlands; 26Kapteyn Astronomical Institute, University of Groningen - The Netherlands; 27School of Physics & Astronomy, Rochester Institute of Technology – USA; 28Instituto de Astrofísica de Canarias (IAC) – Spain; 29Universidad de La Laguna (ULL), Dpto. Astrofísica – Spain; 30Instituto de Astrofísica and Centro de Astroingeniería, Facultad de Física, Pontificia Universidad Católica de Chile – Chile; 31Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze – Italy; 32INAF - Osservatorio Astrofisico di Arcetri – Italy; 33Laboratório Nacional de Astrofísica/MCTIC – Brazil; 34Divisao deAstrofísica, Instituto Nacional de Pesquisas Espaciais – Brazil; 35Gemini Observatory, Southern Operations Center – Chile; 36Max-Planck-Institut für Astronomie - Germany ASTROPHYSICSASTROPHYSICS OFOF HOTHOT PLASMAPLASMA ININ EXTENDEDEXTENDED X-RAYX-RAY SOURCESSOURCES 6/12-14/20196/12-14/2019

X-Rays from Radio Galaxies

X-ray emission associated with radio sources ~ 100s kpc scale (e.g., Fabian et al. 2003; Scharf et al. 2003; Erlund et al. 2006)

● SSC (Kataoka & Stawarz 2005) dominates in radio hot spots (Hardcastle et al. 2004) ● IC/CMB (Harris, & Grindlay 1979; 3C 274.1 (Ineson et al. 2013) Schwartz et al. 2000), X-ray structures 3C 6.1 (Hardcastle et al. 2004) generally aligned with radio axis (Celotti & Fabian 2004; Ghisellini et al. 2015; Wu et al. 2017) ● IC form far-IR photons from galactic starburst on ~100-200 kpc scale (Smail et al. 2009, 2012) ● Thermal emission from the hot gas of the IGM (Ineson et al. 2013, 2015; Worrall 2002; Crawford & Fabian 2003).

3C 432 (Erlund et al. 2006)

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 3CR Catalog The last revised version of the Third Cambridge Catalog (3CR) of extragalactic radio sources (Spinrad et al. 1985) is one of the best-studied samples of radio-loud AGNs

● 178 MHz radio flux-limited sample ● 9 Jy cutoff ● 0.0005quasars, 2 Seyferts, 2 BL Lacs, 20 unidentified, and 20 unclassified)

Unbiased with respect to viewing angle, X-ray properties of the sources. It spans a wide range of redshift and radio power It has a vast multifrequency database of ground and spaced-based observations (radio: NRAO VLA, NVAS, MERLIN; infrared: Spitzer, Dicken et al. 2014; Ramírez et al. 2014; Ghaffari et al. 2017; optical: HST; Privon et al. 2008; Tremblay et al. 2009) It is an ideal sample to investigate the properties of active galaxies.

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 Chandra Snapshot Program Before 2007, only ~ 60% of 3CR extragalactic sources were observed by Chandra and ~ 35% by XMM-Newton. To extend the wavelength coverage of the 3CR catalog, we started an X- ray snapshot survey with Chandra → angular resolution comparable to optical and radio frequencies. Main goals: ● Study the X-ray emission arising from jet knots, hotspots, and nuclei of radio sources ● Search for observational evidence of AGN interactions with the hot gas in galaxies, groups, and clusters of galaxies (feedback) (Fabian 2012; Kraft et al. 2012) ● Search for galaxy clusters via the presence of extended X-ray emission unrelated to the radio structures (Belsole et al. 2007; Ineson et al. 2013; Mannering et al. 2013)

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 The Story So Far...

During Chandra AO9, AO12, AO13, AO15, AO17 data acquired for 113 sources (z<1.5) with at least a snapshot (<20 ks exposure) Chandra observation:

● Flux maps in three energy bands (0.5-1 keV, 1-2 keV, and 2-7 keV) ● Basic parameters (net counts, extension ratios, fluxes, and luminosity) for the nuclei and other radio structures detected (i.e., knots, hotspots, lobes) ● X-ray spectral analysis of the brightest nuclei

(Massaro et al. 2010, 2012, 2013, 2018; Stuardi et al. 2018) A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 Extended Emission Extended X-ray emission found in 18 sources

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 Hotspots 24 hotspots

3C 105

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 Lobe Emission 13 lobes

3C 105

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 The Power of the Snapshot 3C 459 (Maselli et al. 2018)

● Proprietary rights are immediately waived: legacy program for the whole astronomical community ● X–ray extended emission 3C 89 (Dasadia et al. 2016) around other nuclei (Balmaverde et al. 2012) ● Statistical analyses of extragalactic jets (Massaro et 3C 305 (Hardcastle et al. 2010) al. 2011) ● Follow-up observations (3C 171, 3C 305, 3C 89, 3C 459)

3C 171 (Hardcastle et al. 2010)

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 3C 17 Knots

IC/CMB (Massaro et al. 2009). Gemini data: 3C 17 is part of a galaxy cluster at a redshift of z=0.220 with 12 members (Madrid et al. 2018) .

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 3C 305

CSS with X-ray radiation associated with the [O iii] emission: radio jet interactions with the circumnuclear environment (collisional ionization) or by emission from photoionized gas (Massaro et al. 2009).

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 3C 196.1

Inner cavity: past merger event (sloshing). Outer cavity: buoyantly rising bubble originating from AGN outburst (Ricci et al. 2018).

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 3C 196.1

XMM-Newton AO 18 ~ 100 ks

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 3C 187

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 3C 187

Extended cross-cone emission, lobe emission compatible with IC/CMB (but low statistic, Paggi et al. in prep).

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 Main Results

● During AO9, AO12, AO13, AO15, AO17 (and AO20) the 3CR Chandra snapshot survey allowed us to observe 113 targets (z<1.5) ● Flux maps, net counts, fluxes, and luminosity for nuclei and other radio structures, X-ray spectral analysis of the brightest nuclei ● X–ray emission has been detected for all but two radio nuclei (3C 153 and 3C 319) ● We found extended X-ray emission in 18 sources, 11 jet knots, 13 lobes, 24 hotspots (marginal detections for other 9) ● Follow-up observations, detailed analysis for most interesting sources

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 Chandra Catalog Cool Target

Cool-attitude targets for the Chandra mission: Bologna Sky Survey (B2CAT) at 408 MHz.

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019 Unidentified 3CR Sources

● 25 unidentified source ● SWIFT XRT and UVOT 5 ks observations ● X-ray counterpart for 11 ● WISE counterparts for 9, with colors consistent with quasars ● No optical/UV counterpart (Maselli et al. 2016)

➔ High redshift quasars ➔ Highly obscured radio- loud active galaxies

A. PAGGI ASTROPHYSICS OF HOT PLASMA IN EXTENDED X-RAY SOURCES 6/12-14/2019