1. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) The interplay between radio jets and ISM in sub-kpc radio sources evolution of jets interacting with their environment as seen in small and intermediate scale objects Raffaella Morganti ASTRON, Dwingeloo Kapteyn Inst. Groningen Clive Tadhunter, Tom Oosterloo, Joanna Holt, Bjorn Emonts

2. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Characteristics and effects of jet-ISM interaction: why important? Effect of the ISM on the radio jet: doesn’t care? momentarily disrupt? frustrated? destroyed? Effects of the jets on the surrounding ISM: gas outflow clearing the circum-nuclear regions? Interaction radio jets/ISM is one of the possible mechanisms for triggering outflows (together with radiation pressure and starburst winds) important for the evolution of the host galaxy

3. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Following a hierarchical scenario: evolution of AGN vs host galaxy Start of merger -1 billion yr Advanced merger: gas driven towards nucleus; starburst -0.5 billion yr Quasar and jet activity drives gas out of galaxy Now Relaxed E-galaxy +1 billion yr from Clive Tadhunter onset of radio activity related to accretion or merger -> but variety of conditions in the merger

4. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Initial phase of AGN can be crucial in the evolution of the host galaxy in radio-loud objects we know which one are YOUNG AGN (e.g. CSS/GPS) thus we can study their effect on the medium

5. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) We use the (kinematics of the) gas to trace what is happening in the central regions of active galaxies Atomic neutral hydrogen Ionised gas Molecular gas (talk Patrick Ogle) complementary information

6. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Gas in (the centre of) early-type (field) galaxies: important and very common component In general (not only AGN selected early-type): Ionised gas -> ~70% detected, complex kinematics, kinematical decoupled cores etc. -> external origin of the gas in many cases (but not all!) Neutral hydrogen emission (on large scale) absorption (for radio-loud): can explore the small scales comparison compact/extended

7. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) HI in EMISSION: 70% detection rate for deep observations (down to few x 10 6 M sun ) HI in early-type galaxies 200 kpc ATCA data HI total intensity + optical Serra et al. 2005 (van Langevelde et al. 2000) NGC 4261 HI in ABSORPTION: detected in ~30% of radio loud

8. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) How about sub-kpc (CSS/GPS) radio sources: is gas (ionised/neutral) present? and how compares to what found in large radio galaxies? are they (CSS/GPS) really moving through a dense medium? kinematics of the gas?

9. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) - Typical optical depth for radio galaxies:  ~0.01 – 0.05 - High optical depth  0.1-0.2 detected in Seyferts and small/young sources. - High detection rate of HI in CSS/GPS ( e.g. Vermeulen et al. 2005 ) (not so clear for HFP Orienti et al. 2006 ) upper limits optical depth  Gallimore et al. Vermeulen et al. Morganti et al. Typical HI column densities: 10 19 - few times 10 20 cm -2 for T spin =100 K BUT T spin can be up to few 1000 K Atomic neutral hydrogen in large vs compact radio sources Narrow (100-200 km/s) absorption component, associated with settled gas (e.g. circum-nuclear disks, halo, clouds e.g. see 4C12.50) BUT NOT THE FULL STORY!

10. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) radio jet The nuclear regions probed by the HI extra-gas surrounding the AGN, e.g. left over from the merger that triggered the AGN HI absorption from the torus or from circumnuclear disks Cygnus A Conway & Blanco 1995 ~150 km/s fast HI outflows 1400 km/s WSRT Morganti et al. 2003 shocks

11. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) WSRT observations of broad HI absorption Up to 2000 km/s width, optical depth <<1% Column density few times 10 21 cm -2 (for T spin = 1000 K) Mostly blueshifted HI outflows - Morganti, Oosterloo, Tadhunter A&A 2005  ~0.003 ~1500 km/s  ~0.004  ~0.0023  ~0.0005  ~0.006  ~0.002 ~1400 km/s~1000 km/s ~800 km/s ~2000 km/s ~600 km/s

12. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Radio sources with detected fast HI outflows are either mainly compact/young or large with steep-spectrum cores (considered to be objects with restarted radio activity: 3C293 and 3C236) All with rich ISM (CO, farIR....) Outflows detected in off-nuclear regions: jet-ISM interaction Outflows detected (with similar characteristics) both in ionised AND neutral gas!

13. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) The case of 3C305 WSRT VLA core 500 km/s VLA HI The broad HI absorption is found off-nucleus at the location of the radio lobe (about 1.6kpc from the nucleus) column density 2x10 21 cm -2 (for T spin =1000K) Mass outflowing gas ~10 6 M sun Morganti, Oosterloo, Tadhunter, van Moorsel & Emonts 2005 A&A 1 kpc

14. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Jet-driven outflows can have an impact on the evolution of a galaxy comparable to starburst-driven superwinds Bulk kinetic energy: ~ few x 10 57 erg (over a lifetime of a radio jet) Rupke, Veilleux, Sanders 2002, 2005 Radio Galaxies Mass outflow rate between a few and ~50 M sun /yr comparable (lower end) to that found in Ultraluminous IR galaxies Relevant impact in the evolution of the galaxy?

15. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Comparison between young (compact) and extended radio sources 14 powerful CSS/GPS from 3C/4C-2Jy samples 11/14 show evidence for fast outflows –systemic to broadest component –different distributions: K-S test significance: 99.9% size is important Histograms: systemic-broadest Number of sources Extended radio sources (Taylor 2004) Compact radio sources (Holt 2005) Shift (km s -1 ) GPS CSS Other Holt (2005) PhD work of Joanna Holt Ionised gas

16. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) General results on ionized and neutral hydrogen in compact sources Indication of a rich medium around these objects? Broader & blueshifted optical emission lines are associated with compact radio sources: fast outflow of ionised gas very common Higher HI column density and fast HI outflows detected (produced by the interaction between the radio jet and the surrounding dense medium)

17. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Detailed study of two objects and the connection atomic neutral - ionised gas

18. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) -450 km/s -2000 km/s [OIII] Profiles WHT+ISIS Holt et al. 2002 HST [OIII]VLBI Compact and powerful radio galaxy (P 5GHz = 10 26 W Hz-1) Far-IR bright, L IR ~2x10 12 L sun Large amount of CO, ~ 10 10 M sun Very rich ISM 4C12.50 and its unfriendly medium

19. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) AGN feedback: outflows Extended [O II]3727 emission Deep HI 21cm absorption (Mirabel 89, Morganti et al 03) [O III] emission in the nucleus broad narrow intermediate blueshift ~ 400 km s -1 blueshift ~ 2000 km s -1 (Holt et al 03a,b)

20. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) AGN feedback: outflows Extended [O II]3727 emission Deep HI 21cm absorption (Mirabel 89, Morganti et al 03) [O III] emission in the nucleus (Morganti et al 03) (Holt et al 03a,b)

21. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Observer’s L.O.S. quiescent halo emitting narrow component narrow component broad component intermediate component obscured quasar bi-polar radio jets The broadest components are the most highly reddened & higher density (> 5000 cm -3 ) Bow shock Jet HI clouds [OIII] clouds Shocked clouds [OII]-emitting cocoon Far side of galaxy, completely obscured from view Stratified outflow Upper limit for the total mass of line emitting gas (kinematically disturbed component combined) < 10 6 M sun - too low for frustrating, confining the source

22. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) radio jet high density cloud 2D simulations Bicknell et al. 2003 4C12.50 Core black=WSRT red = VLBI Integrated HI profile Mass of the HI cloud ~10 5-6 M sun High column density (N H ~10 22 cm -2 ) HI absorption Global VLBI Morganti, Oosterloo, Vermeulen et al. 2004 HI at the systemic tracing a clumpy medium Case of 4C12.50: the jet is “fighting” its way out of a rich medium? ~50pc

23. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) PKS 1549-79: an example of a radio source in the early-stage of its evolution Recent major merger: tidal tails in optical, young stellar population (50-250 Myr) Core-jet radio structure: close to the line- of-sight HI absorption surprisingly present No broad permitted (optical) lines but Pa  in NIR Broad blueshifted (outflowing) component e.g. [OIII]5007 VLT+FORS1: Gunn r (Batcheldor et al. 2007) (King 1996) 2.3 GHz Broad [OIII] (FWHM~1350km/s) blueshift ~ 680 km s -1 Narrow H  (FWHM<400km/s) HI centre NTT+EMMI & VLT+FORS2 VLBI

24. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) PKS 1549-79: in a stage where the nucleus is still hidden (in the optical) by the gas/dust coming from the merger that triggered the radio source Observer’s L.O.S. [O II]- emitting disk/cocoon young, small scale radio jets expanding through dense cocoon sweep aside gas and dust AGN driven outflow will eventually remove the gas PKS1549-79 AAT/IRIS2 K-band FWHM = 1950 ± 40 km/s

25. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) core Tzioumis et al. 1.2GHz [OII] ~200 pc Not enough sensitivity to detect broad HI, but the HI at the systemic velocity represents the cocoon around the radio source

26. Raffaella Morganti Extragalactic jets, Girdwood (May 2007). mass outflow rate: 0.12 < M < 12 M ๏ yr -1 mass of ionised gas in the outflow : 1.9x10 4 < M ๏ < 1.9x10 6. energy flux: 5.1x10 40 < E < 5.1x10 42 erg s -1 Main problem: relatively modest warm gas outflow the warm-gas outflow is not large! more in cold/hot gas? not as large as expected in the quasars feedback model it will not be able to clear all gas amount of ionised gas: not large to stop the jet 1.5x10 -6 < E/L edd < 1.5x10 -4 Only small fraction of accretion power.

27. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Results from the study of single objects Interaction important - many effects seen complex, stratified structure of the ionised gas outflow the gas masses do not seem to be large enough to frustrate the source but likely slowing down the evolution of the jets. mass outflow not enough as expected in feedback models ?

28. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) For nearby (z < 0.04) lower luminosity, compact sources the situation could be different (see also talk Giroletti) not all GPS/CSS become large galaxies? but not necessarily because of the interaction? different evolution? large amount of HI in emission around nearby CSS: connected to their origin? BUT we don’t see large sources with such large HI disks.

29. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) HI-rich compact radio sources do not grow into extended sources (either because frustrated by the ISM in the central region of the galaxy or because the fuel stops before the source expands) Remarkable trend: radio galaxies with large amounts (M HI >10 9 M sun ) of extended (many tens of kpc up to 200 kpc!) HI disks all have a compact radio source Emonts et al. 2006, astro-ph/0701438 Nearby (z<0.04) compact radio sources ~1kpc Giroletti et al. 2004 Morganti et al. 2006 NGC 3894

30. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Results Powerful compact sources Interaction important - many effects seen complex, stratified structure of the ionised gas outflow the masse of the gas involved does not seem to be large enough to frustrate the source but likely slowing down the evolution of the jets. Nearby low-luminosity compact sources different evolution? some of them just fade away? do not grow to large size

31. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) X

32. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) looks promising BUT can the fragmented clouds be accelerated to such high velocities? Evolution of clouds in radio galaxy cocoons: shock runs over a cloudcompression phase (overpressured cocoon) fragmentation & cooling formation of dense, cool & fragmented structures Cool gas can be produced in jet/cloud interaction Simulations show that cooled fragmented clouds (likely to collapse and form stars) do form as result of the interaction Mellema et al. 2002, Fragile et al. 2003 Fragile et al. 2003 Cloud + Denser and warmer subclouds

33. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) [OIII]4959,5007 fit with 3 components "Deep" Absorption  only 1%, N H ~2x10 20 cm -2 for T SPIN =100K Broad HI absorption: full width of ~2000 km/s mostly blueshifted (already known from Mirabel 1989) Ionized and neutral gas Broad absorption

34. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) The location of the HI outflows: the case of the radio-loud Seyfert IC 5063 ATCA – 17 GHz radio core H  +[NII] ~4 arcsec circa 1.3kpc ATCA & NTT radio core Vel Morganti, Holt et al. submitted Outflow located at the radio lobe (0.5 kpc from the nucleus): jet-induced outflow 0.5 kpc

35. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) AGN feedback: outflows Extended [O II]3727 emission Deep HI 21cm absorption (Mirabel 89, Morganti et al 03) (Holt et al 03a,b)

36. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Outflows in young radio sources 11/14 show evidence for fast outflows –systemic to broadest component –different distributions: K-S test significance: 99.9% size is important orientation may be important Holt (2005) Ionised gas

37. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Emonts et al. (from Spitzer archival data PI. Armus)

38. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) 4C12.50 and its unfriendly medium VLT image (Batcheldor et al. 2007) Stanghellini et al. ~300 pc

39. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Integral field spectrograph SAURON Integral field spectrograph OASIS Kinematical decoupled cores The kinematics changes in the very inner parts McDermid et al. using Sauron and OASIS integral field spectrographs Examples of gas in the centre of nearby early-type galaxies linear scale, between 50 and 100 pc/arcsec

40. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Gas in (the centre of) early-type galaxies: important and very common component In general (not only AGN selected early-type): Ionised gas -> ~70% detected, complex kinematics, KDC etc. -> external origin of the gas in many cases (but not all!) Neutral hydrogen emission (on large scale) absorption (for radio-loud): can explore the small scales comparison compact/extended

41. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Case of the compact radio source OQ208  known to have fast outflow in the broad emission lines (Marziani et al.)  particularly rich medium from X-ray absorption: radio jets possibly piercing their way through a Compton-thick medium pervading the nuclear environment (Guainazzi et al. 2004) ~10 pc Stanghellini et al. 1993 Optical depth of the peak absorption  ~0.005 WSRT 1500 km/s

42. Raffaella Morganti Extragalactic jets, Girdwood (May 2007) Radio sources with detected fast HI outflows are mainly compact/young or large with steep-spectrum cores (considered to be objects with restarted radio activity: 3C293 and 3C236) All sources with rich ISM (CO, farIR....)