AGN10-dallorizzonte degli eventi allorizzonte cosmologico Roma 11/09/2012Eleonora SaniCo-Is: Davies, Sternberg, Gracia-Carpio, Hicks, Tacconi,Genzel, Engel, Vollmer, Schinnerer, Garcia-BurrilloUsero, Orban de XivryPhisical properties of dense molecular gas in centres of Seyfert galaxies

IntroductionTorus structureAGN-SF connectionStellar and molecular gas kinematics Motivation:Trace the dense molecular gasThe origin of huge velocity dispersion

Results:- PdBI data cubes and observables- DYSMAL- Can the torus form stars?

OutlineE. Sani AGN10 Roma 11/09/2012

Torus Properties molecular gas and dustoptically thick: it obscures the AGN if viewed edge oncompact: tens of parsecs of radial extensionvertically extended: several parsecs (provide collimation for ionized gas)Antonucci & Miller 1985E. Sani AGN10 Roma 11/09/2012

Torus structureNenkova+02, +08; Honig+06; Schartmann+08Stellar radiation pressure (Thompson+05; Ballantyne 2008)Supernovae explosions (Wada & Norman 2002)Stellar winds (Nayakshin & Cuadra 2007)External gas accretion (Vollmer+08)Nuclear star formation can play an important roleE. Sani AGN10 Roma 11/09/2012Pier & Krolik 1992; Granato & Danese 1994 Efstathiou & Rowan-Robinson 1995; Shartmann+05; Fritz+06Dust distribution:Smooth (continuous)Clumpy (discrete)

AGN-SF connectionSF happens in all types of AGN(Schweitzer+06, Veilleux+09)even in the nuclear region (R < 200 pc)(Cid Fernandes +04)Sani+10SF enhanced for MBH < 107 ML/Ledd > 0.5BH growth and SF happens simultaneouslyE. Sani AGN10 Roma 11/09/2012

AGN-SF with high spatial resolutionDavies+07

Recent (~40 Myr ago) but no longer starburst in the inner 100 pc (with spatial resolution ~10 pc)H2 fluxvelocityv. dispersionHicks+09H2 1-0(S1) traces warm molecular gasat centres v/ < 1 with gas~50-100 km/sdistribution must be vertically extended with gas & stars spatially mixedrandom bulk motions must account for gas in AGNE. Sani AGN10 Roma 11/09/2012

Molecular gas tracers1-0S(1) H2 traces hot component of the gas (~1000 K) at the edges of clouds1-0S(1) H2 accounts for 10-6-10-5 of the total gas massit is not straightforward to derive the vertical extent of the torus and the origin of the huge gas

E. Sani AGN10 Roma 11/09/2012

Kinematics of the dense gas~1 resolution from PdBI NGC 3227, 2273, 4051, 6951 (now also NGC 3079, 5033, 6764) Directly observable constraints: major & minor axis size Integrated line width FWHM~70-210 km/sSeparation + PA of the red/blue channels

Sani+12

Modelling the kinematicsUse DYSMAL (Cresci +09, Davies +11) -Gaussian distribution for the luminosity and mass profiles -Fixed parameters: and PA-Elliptical beam (beam smearing is a key aspect of dynamical modeling)-Free parameters: R, H, MR

Thin disk-Line width is only ~2/3 of that observed

Thick disk-Can reproduce all observed characteristics-Intrinsic dispersion is 25-50 km/s for HCN and HCO+ (about ~50% of H2 1-0S(1) reported by Hicks+09)-Dispersion is due to a combination of beam smearing of velocity gradients as well as V/~R/H~3-4

SF within the Torus?NGC 3227: nuclear (

The model: starburst & torus evolutionVollmer, Beckert, & Davies 08Phase I: short, massivegas infall generates a massive turbulent disk (Q~Qc) where SF occurs.

Thick diskQ > Qc

Conclusion & Future WorkWe observed 4 Seyfert galaxies with the PdBI tracing HCN and HCO+ molecular lines. The line emission is (marginally) resolved.

We measured morphological (dimension & position angle) and kinematical (channel separation & integrated line width) parameters. The most remarkable feature is the line width FWHM ~ 70-210 km/s

Observed parameters are well reproduced by a thick (R/H = V/) taking into account the beam smearing.

Increase the statistics: now available data for 3 more sources.

Add other AGN types to trace the torus structure in different environments and its evolution.

Use tracers at 1.3mm, e.g. HCN(3-2), to constrain the chemistry

Dynamical modelling of the data with DYSMAL Disk in vertical hydrostatic equilibrium: R/H = V/ inclined disk with a Gaussian mass distribution elliptical beam shape (crucial for modelling marginally resolved sources to account for beam smearing)

Free parameters are: R, H and a Mass scaling

Thin disk: linewidth and/or channel separation are NOT reproducedThick rapidly rotating diskSource 2R() 2H() Vrot(km/s) int(km/s) H2(km/s) NGC2273 1.38 0.43 83.1 44.8 NGC3227 0.54 0.14 104 60.4 95.0 NGC4051 0.86 0.18 54.4 24.7 55.0

Dense gas has a THICK distribution

The Toomre Q parameterQ = /(G), = 3 x (uniform disk)

= V/R = V x R/H (thick disk) = M/(R2) Md = (V2+32)R/G

Qc=0.68(thick Isothermaldisk)Dekel +09Q = 3 H 1 R (1+3xH2/R2) fgas

ruolo della sf nel determinare la dist del toro e cosa sappiamo daCome mai per capire sigma ho bisogno di traccianti di gas desoDiscussione

distribuzione omogenea del materiale porta a problemi di stabilita`.Toro deve essere clumpy O supportato da meccanismi che si combinano con la pressione termica. SF puo` giocare un ruolo importante nel mantenere la struttura verticale del toro attraverso pressione di radiazione, Esplosioni SN, venti stellari => forte connessione AGN-SF

distribuzione omogenea del materiale porta a problemi di stabilita`.Toro deve essere clumpy O supportato da meccanismi che si combinano con la pressione termica. SF puo` giocare un ruolo importante nel mantenere la struttura verticale del toro attraverso pressione di radiazione, Esplosioni SN, venti stellari => forte connessione AGN-SF

Ce` da capire se tale dispersione cosi` elevata e` dovuta alle proprieta` del tracciante o se e` effettivamente rappresentativo della fisica del gas (bulk gas properties)Cut a 45deg lungo lasse minore dellanelloMarginalmente risolti, HCN, HCO+ sempre consistentiFWHM elevataAnche se le sorgenti sono solo marginalmente risolte, possiamo misurare un gradiente in velocita` usando la spectroastrometry, la precisione dipende dallaccuratezza con cui puo` essere misurato il centroide (< 1/10 beam). I centroidi di tali mappe derivano dallo stesso dataset, quindi gli ofset dovuti alla calibrazione in fase sono trascurabili.Errori assoluti nella posizione del centroide (in generale): rms in fase e` nellintervallo 30-43 deg, che corrisponde ad un errore assoluto