1.  MOLECULAR GAS IN THE CORES OF AGN Violette Impellizzeri (NRAO) Alan Roy (MPIfR), Christian Henkel (MPIfR)

2. The unified scheme of AGN  Diversity of AGN classes explained by a single unified scheme :  The nuclear activity is powered by a supermassive black hole ( ∼ 10 6 –10 10 M ⊙ ) and its accretion disk.  This central engine is surrounded by dusty clouds, which are individually optically thick, in a toroidal structure (Krolik & Begelman 1988). Populated by molecular clouds accreted from the galaxy.  Observed diversity is the result of viewing this axisymmetric geometry from different angles.

3. The unified scheme of AGN

4. The torus: size  To determine an actual size one must rely on the torus emission.  Pier & Krolik (1992) approximate the density distribution with a uniform one : outer radius R ∼ 5 pc – 10 pc.  Pier & Krolik (1993) : later speculated that compact structure might be embedded in a much larger, and more diffuse, torus with R ∼ 30 pc –100 pc.  Granato and Danese (1994) elaborate toroidal geometries, concluded that the torus must have an outer radius R ~ 300 pc – 1000 pc.  Granato et al (1997) settled on hundreds of pc. Subsequently, R > 100 pc became common lore.  High-resolution IR observations brought unambiguous evidence in support of compact torus dimensions. VLTI interferometry shows that the 10 μm flux comes from a hot (T > 800 K) central region of ∼ 1 pc and its cooler (T ∼ 320 K) surrounding within R ∼ 2 pc and 3 pc (for NGC 1068; Jaffe et. al 2004).

5. The dusty torus: MIR interferometry  T1 = 334 K  T2 = 298 K Tristram et al. 2007 T1

6. The dusty torus: MIR interferometry  T1 = 334 K  T2 = 298 K Tristram et al. 2007

7. The torus : molecular Sy1 Sy2 N H 10 22 cm -2 ; OH opacities << 1 N H 10 24 cm -2 ; OH opacities > 1 Molecular abundances in tori: N(OH)/N(HI) ≤ 10 -3 (Krolik & Lepp 1989) Dusty AGN torus is molecular gas rich

8. OH surveys Expect to observe molecular absorption against the compact, flat spectrum radio cores of NLRs. Not only confirm the existence of a torus, but also derive valuable physical and kinematical information. OH surveys at 1.6 GHz Schmelz et al. 1986, Staveley-Smith et al. 1992, Baan et al. 1992... (sensitivities of few percent) CO, HCN and HNC searches Drinkwater et al. 1997 Surprisingly few detections! OH abundance lower than predicted ? No torus ? Observed ~ 300 galaxies Low detection rates (absorption towards two Seyferts maser emission in five).

9. No CO absorption in Cygnus A  Of all AGN Cygnus A is expected to have a molecular torus  NLR  Large X-ray absorbing column (10 23.5 cm -2 )  Search for CO (1-0) absorption yielded non detection!  Search for OH (1.6 GHz) non detection H 2 CO non detection HI detected (Coway & Blanco 1995)

10. Radiative excitation I  Gas in a hot (5000 -10000 K) mainly atomic phase.  Radiative excitation of CO, OH and NH 3 due to the central radio source causes the non detection of molecular absorption (Maloney, Begelman & Rees 1994).

11. Radiative excitation I  Gas in a hot (5000 -10000 K) mainly atomic phase.  Radiative excitation of CO, OH and NH 3 due to the central radio source causes the non detection of molecular absorption (Maloney, Begelman & Rees 1994).

12. Radiative excitation effects  Maloney, Begelman, & Rees (1994) High T ex depletes lower rotational levels, decreasing optical depth  Maloney, Begelman, & Rees (1994) postulate that lack of CO absorption is due to radiative excitation by non-thermal radio source: High T ex depletes lower rotational levels, decreasing optical depth is OH, too, radiatively excited ? For torus located 10 pc from AGN: opacity in 1.6 GHz transition suppressed by factor 10 3 opacity in 6.0 GHz transition suppressed by factor 10 2 opacity in 13.4 GHz transition will increase slightly by factor 2. Black (1998) Thus, absorption will strongly depend on transition one chooses to observe. Have we been looking at the right transitions ?

13. A new survey for OH  Search for highly excited rotational states of OH at 6.035 GHz & 6.031 GHz, 4.750 GHz and 13.4 GHz. The sample:  31 Seyfert 2 galaxies  High X-ray absorbing columns (> 10 22 cm -2 )  Continuum flux density at 6 GHz > 50 mJy  HPBL Effelsberg observations: 3-10 hours per source at 4.7 GHz and 6.0 GHz, PSW Velocity coverage 2000 km/s (4 km/s per channel) Sensitivity 3.5 mJy (5 σ) = line opacity of 0.002 to 0.07

14. Effelsberg Spectra 6.0 GHz Best targets due to high X-ray columns and high background continuum at 6.0 GHz.

15. Effelsberg Spectra 6.0 GHz Too strong continuum - Large standing wave ripple! 5 new detections - detection rate 18 %

16. Effelsberg Spectra 6.0 GHz Lets look at NGC 3079 & NGC 5793.

17. NGC 3079 NGC 5793 Width ~ 800 km s -1 Line opacity τ ~ 0.055 4.7 GHz non-detection 1.6 GHz abs (Baan et al. 1995) T ex = 30 K N OH = 1.5 10 18 cm -2 N OH = 1.5 10 18 cm -2 from X-rays: N H = 1.0 10 25 cm -2 Width ~ up to 1000 km s -1 Line opacity τ ~ 0.036 4.7 GHz non-detection 1.6 GHz abs (Hagiwara et al. 2000) T ex = 67 K N OH = 2.2 10 17 cm -2 N OH = 2.2 10 17 cm -2

18. Conclusions from OH survey  A survey for 6.0 GHz and 4.7 GHz with Effelsberg found highly excited, broad absorption lines in 5 out of 28 sources, i.e. 18%.  Line widths are 100s-1000 km/s (close to nuclear region?).  Selection criteria improved detection rate c.f. other OH surveys (< 7%).  No new detections at 6.0 GHz were made where there was no previous OH absorption/emission at 1.6 GHz.  Results do not support radiative excitation models alone to explain the lack of detections.  Still some sources with high column density didn’t show absorption. But still the non detections must be explained !!

19. Some open questions  Bimodal distribution of absorptions –> very compact clouds ?  Broad lines in infall/outflow ? Not a simple rotating torus ?  X-ray absorber may be non-molecular in most galaxies ??

20. VLBI Observations  VLBA observations carried out with interferometric observations to detect OH at 13.4 GHz towards the core of NGC 1052 and Cygnus A. => 0.9 mas beam Observing time: NGC 1052 – 7 hours Cygnus A – 8 hours Bandwidth 16 MHz (256 channels) per IF. Velocity coverage ~ 560 km/s.

21. NGC 1052 Nearby radio galaxy classified as LINER (z=0.0049) Hosts well-defined double-sided radio jet w/ P.A. 65 0 Jet extends up to kpc scale, angle of jet axis is > 76 0.

22. NGC 1052

24. Nearby radio galaxy classified as LINER (z=0.0049). Hosts well-defined double-sided radio jet w/ P.A. 65 0. Jet extends up to kpc scale, angle of jet axis is > 76 0. Multi-frequency VLBI observations have revealed the presence of a dense circumnuclear structure. Plasma condensation covers 0.1 pc and 0.7 pc of approaching and receding jet (Kameno et al. 2001). X-ray column is 10 22 – 10 23 cm -2 (e.g. Kadler et al. 2004). H 2 O megamasers found towards the centre redshifted by 50-350 km/s wrt systemic (e.g. Braatz et al. 2003). Nearby radio galaxy classified as LINER (z=0.0049). Hosts well-defined double-sided radio jet w/ P.A. 65 0. Jet extends up to kpc scale, angle of jet axis is > 76 0. Multi-frequency VLBI observations have revealed the presence of a dense circumnuclear structure. Plasma condensation covers 0.1 pc and 0.7 pc of approaching and receding jet (Kameno et al. 2001). X-ray column is 10 22 – 10 23 cm -2 (e.g. Kadler et al. 2004). H 2 O megamasers found towards the centre redshifted by 50-350 km/s wrt systemic (e.g. Braatz et al. 2003).

25. NGC 1052 Sawada-Satoh et al. 2008  H 2 O detected where free-free opacity large. Other lines have been detected : HI, OH, HCO +, HCN and CO…

26. NGC 1052 Sawada-Satoh et al. 2008 Vermeulen et al. 2003

27. NCG 1052 – VLBA 13.4 GHZ Broad Width: FWHM ≈ 200 km/s Optical depth (counter jet) τ OH ≈ 0.264 Obscuration in the inner jet region (< o.3 pc), coincident with free-free absorption. Vsys 0.2 pc

28. NGC 1052 – where is absorption located? Optical depth map

29. NGC 1052 – where is absorption located? Optical depth map

30. NCG 1052 – VLBA 13.4 GHZ Receding jet Approaching jet

31. Are we seeing the torus in NGC 1052? Approaching jet Receding jet

32. Fitting into the picture Sawada-Satoh et al. 2008

33. Fitting into the picture Sawada-Satoh et al. 2008 OH

34. Cygnus A Continuum peak flux 453 mJy per beam Optical depth (core) τ OH ≈ 0.12 Absorbing gas is diffuse around the inner jets. Profile strongest over the entire continuum.

35. Cygnus A Continuum peak flux 453 mJy per beam Optical depth (core) τ OH ≈ 0.12 Absorbing gas is diffuse around the inner jets. Profile strongest over the entire continuum. Conway & Blanco 1995

36. Conclusions from VLBA observations  13.4 GHz OH was detected for the first time in the core of an AGN (NGC 1052 and Cygnus A).  Evidence for molecular gas in the region we would expect to see a torus.  In Cygnus A, if real the detection is consistent with radiative excitation models proposed for this source.  In NGC 1052, redshifted OH gas cloud detected toward the counterjet.  Part of rotating torus/infalling material ?  Detection consistent with previous H 2 O observations.

37. Future outlook  Detections will strongly depend on which transition one chooses to observe!  Future surveys for the molecular component of AGN should include the 13.441 GHz and 13.434 GHz lines of OH.  New instruments like the VLBI, EVLA, and ALMA (just around the corner) with their increased sensitivity will hugely contribute to a high resolution, sensitive study of the molecules in AGN: perhaps a new era also for the Torus?

38. Future outlook For a source at the distance of NGC 1052: VLBA resolution : 1mas at 13.0 GHz : 0.1 pc EVLA resolution : 4 arcsec at 5.0 GHz : 400 pc ALMA resolution: 18mas at 1mm : 2 pc (extended configuration 17 km) ALMA resolution : 0.5 arcsec at 1mm: 50 pc (early science)

39. ALMA

40. Spiral Galaxy in Ursa Major Distance: 15 Mpc (50 million light-years) Dimensions: The full image 4.9´( 21 kpc) Sy2 galaxy N h = 1.6 10 22 cm -2 FIR excess: L fir = 19 10 9 L sun CO (1-0) emission tracing disk ( N h = 1.4 10 24 cm -2 ) Most luminous H 2 O megamaser known