Radio Galaxies as Viewed by Chandra: The 3C Snapshot Surveys and Other Aspects

Radio Galaxies as Viewed by Chandra: The 3C Snapshot Surveys and Other Aspects

D. E. Harris, SAO~~~~~~~Collaborators:

Massaro, F., Axon, D., Balmaverde, B., Baum, S. A., Bonafede, A., Capetti, A., Chiaberge, M., Gilli, R., Giovannini, G., Grandi, P., Kharb, P., Liuzzo, E., Macchetto, F. D., O,Dea,

C. P., Paggi, A., Risaliti, G., Sparks, W., Tremblay, G. R., Torresi, E.

Leiden - 2013 June 11

outline• Chandra Projects on Extragalactic Radio

Sources

• X-ray Contributions to Studies of RGs+Q: lobes, jets, hotspots, nuclei

• Open Issues


The Big 3: Actually some progress was made with the ROSAT HRI

FR I: M87 Jet The start of detailed Radio-Optical-Xray comparisons

FR II: Cygnus A Hotspots Cavities Feedback

Q: 3C 273 High power jets X-ray emission process

Radio Sources in the Chandra Archives

• 3C – about 200• 4C – about 20• PKS – about 46• Specific 3C Projects:


PI Chan AO # target Redshift Remarks

Birkinshaw 10 16 z<0.1 To complete; HST+SpitzerWilkes 9 24 1<z<2 Q: Radio lobe selectedKuraszkiewicz 14 23 z<1 Herschel for SEDsHarris 9,12 57 z<0.3 To complete; HSTMassaro 13 19 0.3<z<0.5 Working out to complete


Goal: Chandra Observations of All Extragalactic 3C Sources

• The effort to get all 3C out to z=0.3 was initiated by Bill Sparks, Marco Chiaberge and friends. Our (SAO) contribution was to alter strategy by proposing for ‘bite-sized’ segments, and later, to work out to higher redshifts.

• The 3 segments have been published: Massaro et al. 2010 ApJ (AO9); 2012 ApJS (AO12) and 2013 ApJS (AO13)

• Many thanks to our generous friends for sharing their radio maps: R. Morganti, C. C. Cheung, and M. Hardcastle. And to NRAO for the NVAS.


Interesting Sources from the Chandra 3C Snapshot Surveys: Cluster Sources

3C 89: TRG 3C 196.1: 3C 320: FRIIHigh density Hybrid, FRII Baby brotherGas between thwarted jet? Of Cygnus A

Tails; stripping?


Interesting Sources from the Chandra 3C Snapshot Surveys: CSS sources 3C171 &

3C305

• Thermal emission aligns with emission line regions.


Interesting Sources from the Chandra 3C Snapshot Surveys: Nuclei

• Unification: searching for an indicator of jet alignment with l.o.s.


Interesting Sources from the Chandra 3C Snapshot Surveys: Lobes

• X-ray emission aligned along the radio axis (c.f. high z RG)

• IC/CMB from steep spectra radio lobes?

• Will LOFAR detect this emission ?

• If so, we should get a better estimate of Beq

• Or is it thermal X-ray emission?


Interesting Sources from the Chandra 3C Snapshot Surveys: Hotspots

• SSC plus ? (Hardcastle et al. 2004)

• In 3C 105 S hotspot, the brightest X-ray region coincides with where the radio jet enters the hotspot region; is this an example of IC scattering off radio photons from the hotspots?


Interesting Sources from the Chandra 3C Snapshot Surveys: Jets

Two knots detected in the curved jet of 3C 17. The outer knot at the location of maximum curvature; perhaps at the point where the jet is coming towards us?


3C 17 – optical feature across jet


JETS: Offsets

At end of jet, note that there is no evidence for a UV counterpart to the anomalous X-ray feature


3C273 offsets


3C273: X, Opt, & Radio

Offsets and Progressions: XTwo sides of the Same coin. UV

R


The inner knot, HST-1, in the jet of M87

• 60 pc (in projection) from the nucleus• Giant flare: factor of 50 to 100: radio, UV,

and X-ray• Superluminal motions in the UV and radio• Beaming factor estimated at 4 to 5• Oscillations in rate of increase (X-rays)• Where do TeV flares originate?


Signatures of E2 Losses for HST-1

• If all frequencies decay together, expansion losses dominate or the beaming factor is changing (e.g. a ‘thrashing jet’).

• If E2 losses (synchrotron & IC) are important, we expect longer decay times for lower frequencies.


Superluminal Proper Motions• The inner (vlba) jet is

not known to be superluminal.

• HST-1 has =v⁄c≈4 for some components.


HST-1• 4 epochs shown

between 2005.0 and 2006.5

• New bits getting resolved and downstream bit moving


Annoyances: Clusters• We failed to find evidence of a cavity for 3C129. Is that

because FRI plumes are well mixed with the ICM or just because 3C129 is far enough away from the cluster centre that the ICM density is too low?

• We failed to find X-ray cluster emission for z=2 RG's. Is it the case that there are no deep potentials filled with hot gas for z>2?


Annoyances: Lobes• IC/CMB: Real progress will come when we get above

20keV. Then we won't have to worry about thermal contamination AND we will reduce significantly the extrapolation required for N(E) between radio data and X-ray data. LOFAR will lower E of electrons and >20keV will raise the γ=1000 for 2 keV.

• What are the effects of the (1+z)4 increase in E2 losses as we go to high z? Will jets and lobes have larger B field strengths? Will sources be smaller? We need to factor in also the ambient plasma densities; both near the SMBH and out in inter galactic space.


Annoyances: Hotspots3C 351:Is hotspot emission (sometimes) beamed? Or are these features 'misplaced' jet knots?

We need to build a testable model for the excess X-ray emission over and above the SSC predictions.


Annoyances: Jets• What caused the flare in M87/HST-1?• And the TeV flaring in M87?• What is the dominant X-ray emission process for

Q (and FRII) jets?• Are high power kpc scale jets still moving

relativisticaly with Γ of order 10 or more? • Does jet X-ray emission sample the electron

spectrum near γ~100 (IC/CMB) or at γ~107

(Synchrotron)?


FINIn addition to collaborators on the 3C snapshot surveys, I owe a lot to working with colleagues over the years....Henric KraczynskiTeddy CheungMartin HardcastleChris CarilliFrancesco MassaroJosh Grindlay and many others...• FOR JET AFICIONADOS: SAVE THE DATE: IAU

SYMPOSIUM 313 ”Extragalactic Jets from Every Angle” Puerto Ayora (Ecuador) / Sep 15-20, 2014


Appendix: Birkinshaw• Title: The multi-faceted X-ray activity of low-redshift active galaxies• Abstract: We propose ACIS-I observations of Chandra-unobserved

low-redshift 3CRR active galaxies and their environments. The data will complete Chandra observations of 3CRR at z < 0.1, making the sample useful for statistical studies. Only Chandra can resolve the multiple components of these sources, as is needed for an improved understanding of source physics and gas heating. The imaging and spectroscopy of cores, jets, hot spots, and atmospheres will be of permanent legacy value. We will use the data to investigate particle acceleration, interactions between radio plasma and the ISM and IGM, the emission mechanisms of hot spots, and AGN fueling. Comparison with our complete Spitzer coverage and HST images will aid interpretation. The dataset will be made public immediately


Appendix: Wilkes• Title: Orientation effects in the X-ray and multi-wavelength

properties of high-z, 3CRR quasars.• Abstract: We propose X-ray observations of 24 sources to complete

a subset of 38 radio-lobe-selected, 3CRR massive radio galaxies in the redshift range 1 < z < 2. We will measure the strength of the nuclear activity and study the relation of X-ray flux and spectral hardness to orientation, estimated from the radio core-dominance. In combination with the rich, multi-wavelength dataset for this inclination unbiased sample (to include Spitzer 3.6-70μm photometry), we will test AGN Unification at these redshifts. SED fitting will also provide constraints on models for the obscuring material, allow us to estimate the relative numbers of obscured and unobscured quasars and to quantify selection effects likely to be present in X-ray samples due to orientation.


Appendix: Kuraszkiewicz• Title: The Herschel Legacy of powerful 3C radio galaxies and

quasars II.• We propose X-ray observations of 23 sources from a well-defined

sample of 77, z < 1 3CR radio sources for which we were allocated Herschel observations (PI Haas). The inclusion of Chandra and Herschel data will complete their radio-X-ray spectral energy distributions allowing us to quantify the orientation-dependence of AGN radiation, investigate the interplay between accretion and star formation and understand the evolution of the black-hole/stellar-bulge relation. The X-ray data enable us to determine the strength of any nuclear activity, estimate the obscuration, study the orientation dependence of the X-ray properties, probe the nuclear geometry with full SED modeling and study evolution via comparison with our higher redshift/luminosity 3CR sources.


Or all together for a single view:


PKS 0637 – Quasar with Jet


Forward & Reverse Shock?


The River Analogy

Looking upstream from knot A in the M87 jet

• A jet is like a smoothly flowing river; observable emission arises only where there is white water.

• Even though HST-1 increased its emission by more than a factor of 50, the power so dissipated is less than one percent of the total power believed to be flowing down the jet.

• Hence HST-1 could be considered to be a very localized, but high efficiency converter of jet power.


Variability: 1980-2004

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Radio Galaxies as Viewed by Chandra: The 3C Snapshot Surveys and Other Aspects