Thaisa  Storchi  Bergmann                                                                                                                                                        Instituto  de  Física,  UFRGS,  Porto  Alegre,  RS,  Brazil  

 The LLAMA Project Evaluation Workshop, FAPESP, São Paulo, August 8-9, 2011

Rogemar  A.  Riffel  Peter  McGregor  Fausto  Barbosa  Claudia  Winge  Allan  Schnorr  Muller  David  Sanmartin  Guilherme  Couto  Rodrigo  Nemmen  Tiberio  Borges  Vale      

¡ AGN  (Active  Galactic  Nuclei)  structure  ¡ HST  images:  AGN  feeding  ¡ Gemini  NIFS  data  ¡ Nuclear  source:  dusty/molecular  torus  ¡ Gas  kinematics:  inflows  ¡ Need  for  ALMA/LLAMA  data  

Supported by broad lines seen in polarized (scattered) light in NGC1068: Antonucci & Miller 1985, Antonucci 1993; other Seyfert 2: Tran, Kay (1990’s, early 2000’s)

Dusty/molecular torus: inner portion of feeding flow to the Supermassive Black Hole Size (dust sublimation radius): 0.01 – 1 pc -> 0.15 – 15 mas for ~15 Mpc (Virgo) Accretion disk: 0.05 mas Event horizon: ~10-4 mas (MW ~ 0.1 mas)

Elitzur 2007; Nenkova 2008: toroidal, clumpy obscuration region 1-10 pc; Maybe stars in it (Wada 2009, fig. from Zier & Bierman 2002)

Fig. by Schartmann et al. 2008

Netzer & Laor 1993: BLR outer boundary set by dust sublimation Rd; Rd: inner boundary of the torus; Both BLR and torus originating from an accretion disk wind (Elitzur & Ho 2009; Risaliti & Elvis 2010)

Fig. from Gaskell et al. 2007

Simões-­‐Lopes  et  al.  2007:  

§  Structure  maps:  HST  F606W  early-­‐type  AGN  vs.  non-­‐AGN  

§   Dusty  nuclear  spirals  in  ~100%  AGN;    

§   But  in  ~  25%  of  non-­‐AGN;  

èChannels  to  feed  the  SMBH  ?  

AGN Non-AGN AGN Non-AGN

Optical:  GMOS    §  FOV:  3.5”x5”  or  5”x7”  §  Sampling  0.2”  ,  Res.  0.6”    §  R~3000  

Near-­‐IR:  NIFS  +ALTAIR  Superb  instrument!  ¡  FOV:  3” x 3”  ¡  Sampling:  0.04”×0.1”  ¡  Res.  0.1”  ¡  R~5500,  Z,  J,  H  &  K-­‐band        

§   GMOS  IFU:  3  fields  5”x7”=15”x7”(1.2x0.6  kpc)  §   Measured  gas  kinematics  (Hα  +[NII])  §   Fit  and  subtract  a  circular  rotating  disk  model  §   Look  for  residuals  in  association  with  nuclear  spirals    

§  Fit and subtraction of circular rotation model to the velocity field;

§  Residuals of up to 50 km/s along nuclear spirals;

§  Mass inflow rate of ionized gas: ~10-3 Msun yr-1

§  Davies et al. 2009: flow in warm molecular gas (Davies et al. 2009) §  Another case: NGC6951 (Storchi-Bergmann et al. 2007)

§  In many cases kinematics is too disturbed to fit circular model

§   GMOS  IFU:  3  fields  5”x7”=15”x7”(255x120  pc2)  

§   Measured  stellar  and  gas  kinematics  (Hα  +[NII])  

§   Subtract  stellar  from  gaseous  kinematics  

§   Look  for  residuals  in  association  with  nuclear  spirals    

Gas kinematics Stellar kinematics

§ Stellar kinematics: major axis along y; rotation axis along x;

§ Gas kinematics distinct: “rotation axis” perpendicular to stellar

§ Relation between velocity, velocity dispersion and structure map: shocks in the plane;

§ If gas is in the plane, blueshifts in the far side èinflows

PC3: rotating disk being fed along minor axis

PC4: bi-polar outflow related to radio jet (arrow)

PC5: more of the disk

§ 3”x 4”(135x180pc)

§  0.1”= 4.5 pc

§ Unresolved K-band source

§  Torus R≤2.3 pc

H2 channel maps

§  Nuclear spiral arms within inner ~ 50 pc down to inner 2.3 pc; blueshifts in far side, redshifts in near side. If gas is in the plane è inflow

§  Mass inflow rate ~1/100 mass accretion rate è only “hot skin” of molecular gas flow §  Cold molecular gas: ≥ 105 larger (Dale et al. 2005) è Mass inflow rate ≥1 Msun yr-1

§ 0.1”= 6.5 pc

§  [FeII]: along ionization cone; 100 pc

§ H2: “toroidal” flux distribution; 50 pc § Coronal lines: barely resolved

Within 4 pc from nucleus: black body with temperature T=1340K è dusty torus

§  0.1”= 6.5 pc §  Unresolved nuclear K-

band source §  Torus R≤3.3 pc

Channel maps: distinct kinematics between ionized and molecular gas: §  [Fe II]: (a) highest velocities along axis of ionization cone; (b) correlation with radio at zero velocities; (c) outflows at 2 Msun yr-1

§  H2: low velocities: rotation in the plane

   Riffel,  R.  A.  &  Storchi-­‐Bergmann  2010):  

§   0.1”=  23.3  pc    §   3”x3”  (700x700  pc2)  

§   Unresolved  nuclear  source          

Spectral synthesis using STARLIGHT (Cid Fernandes): §  Old population (109-10 yr) within 0.5” of nucleus);

§  Unresolved (within ~11 pc) black-body at the nucleus (~1000K)

§  Intermediate age (3-7 x 108 yr) stellar population at low-σ ring è such rings as signatures of post-starburst population

H2 channel maps: inflows in warm molecular gas

FAR

NEAR

HST Optical structure map

                                                     § Centroid  velocity  map  and  σ map for H2(warm  molecular  gas):  compact  rotating  disk  (100  pc)  with  low  low  σ fed  by  spiral  arms  è

§ Model  by  Maciejewski  (2009,  with  Davies):    spiral  arms  as  shocks  in  the  gas  driving  inflows  è    

¡  Inflows  along  nuclear  “tongue”  in  warm  molecular  gas  (Mueller  Sanchez  et  al.  2009);  

¡  Other  similar  works  on  other  objects  by    Richard  Davies  group  at  MPE  

§  Inflows  on  scales  of  10  -­‐  100  pc  mapped  in  ionized  (HII)  and  molecular  gas;    

§  Structure:  nuclear  spiral  arms  or  nuclear  disks;    

§  Mass  inflow  rates:  ~  10-­‐3  M¤  yr-­‐1  in  ionized  gas  and  even  smaller  in  warm  molecular  gas;    

 

§  Total  inflow  rate  larger,  in  cold  molecular  gas;  Dale  et  al.  (2005):  cold/warm  molecular  gas  ratio:  106è  inflow  rate    ~  few    M¤  yr-­‐1      

§  Martini  et  al.  (2011):  Spitzer  dust  masses  of  nuclear  spirals  ~  105  M¤;  Mgas  ~  107  M¤;  if  activity  lasts  107  yr,  inflow  rate  ~  1  M¤  yr-­‐1  

§  Next  step:  flux  distribution  and  kinematics  in  cold  molecular  gas:  ALMA,  LLAMA  

 

 

NGC1097, Nobeyama MM Array, Kohno et al. 2003 §  Strong HCN at the nucleus, but

beam 4.4”x 10”; cannot resolve distribution nor kinematics

§  Need ALMA/LLAMA observations to obtain actual inflow rate

§  How does it compare with the “extrapolated” ~1 M¤ yr-1?

NGC1365, Sub-mm Array (SMA), Hawaii, Sakamoto et al. 2007

NGC3227, PdBI, Sani et al. 2011, HCN at nucleus: higher density gas