3D Spectroscopy to Dissect Galaxies Down to Their Central Supermassive Black Holes Kambiz Fathi Stockholm University, Sweden
Towards a better understanding of the Hubble Diagram
Towards a better understanding of the Hubble Diagram How different substructures form and evolve?
Towards a better understanding of the Hubble Diagram How different substructures form and evolve? What is the connection between processes on galactic scales and local processes such as star-formation and/or nuclear activity?
Towards a better understanding of the Hubble Diagram How different substructures form and evolve? What is the connection between processes on galactic scales and local processes such as star-formation and/or nuclear activity? What can we learn from quantifying the role of secular evolution?
Size of a structure Resonance location Bar/Spiral strength Induced in/outflow Pattern speed
A galaxy s disk is a rapidly rotating thin structure which contains a substantial fraction of the interstellar gas Disks are primarily rotating but are often perturbed by gravitational instabilities Here we use two-dimensional spectroscopy to explore the kinematic observables of these processes
A galaxy s disk is a rapidly rotating thin structure which contains a substantial fraction of the interstellar gas Disks are primarily rotating but are often perturbed by gravitational instabilities Here we use two-dimensional spectroscopy to explore the kinematic observables of these processes
A galaxy s disk is a rapidly rotating thin structure which contains a substantial fraction of the interstellar gas Disks are primarily rotating but are often perturbed by gravitational instabilities Here we use two-dimensional spectroscopy to explore the kinematic observables of these processes
A galaxy s disk is a rapidly rotating thin structure which contains a substantial fraction of the interstellar gas Disks are primarily rotating but are often perturbed by gravitational instabilities Here we use two-dimensional spectroscopy to explore the kinematic observables of these processes
Two-dimensional Spectroscopy (an Integral Field Unit)
Two-dimensional Spectroscopy (an Integral Field Unit)
Fabry-Perot Interferometry
Two-dimensional Spectroscopy Total Flux Morphology, Photometry Absorption lines Stellar kinematics Line indices Emission lines Gas kinematics Gas distribution
Two-dimensional Spectroscopy Total Flux Morphology, Photometry Absorption lines Stellar kinematics Line indices Emission lines Gas kinematics Gas distribution
Two-dimensional Spectroscopy GHAFAS SAURON Telescope 4.2 m William Herschel 4.2 m William Herschel Sampling modes 512 x 512 (LR)1024 x 1024 (HR) 512 x 512 Pixel Size 0.396 x 0.396 arcsec (LR) 0.198 x 0.198 arcsec (HR) 0.94 x 0.94 arcsec Field of view 3.8 x 3.8 arcmin 33 x 41 arcsec Free spectral range ~ 300-1800 km/s 4800-5350 Å Spacing between channels ~ 0.11 Å = ~ 5 km/s 1.1 Å = ~50 km/s Instrumental dispersion ~ 7 km/s 108 km/s Commissioned 2 July 2007 Februaru 1999
A Velocity Field
A Velocity Field
A Velocity Field
Harmonic Decomposition of a Velocity Field Assuming differential rotation, one can section a velocity field into concentric rings and fit the disk centre, inclination, PA, systemic and rotational velocity iteratively e.g., Rots (1975), Begeman (1989), Schoenmakers, Franx & de Zeeuw (1997) Fathi et al. (2004; 2005; 2007; 2008, 2009), van de Ven & Fathi (2009)
Harmonic Decomposition of a Velocity Field Assuming differential rotation, one can section a velocity field into concentric rings and fit the disk centre, inclination, PA, systemic and rotational velocity iteratively e.g., Rots (1975), Begeman (1989), Schoenmakers, Franx & de Zeeuw (1997) Fathi et al. (2004; 2005; 2007; 2008, 2009), van de Ven & Fathi (2009)
Harmonic Decomposition of a Velocity Field Assuming differential rotation, one can section a velocity field into concentric rings and fit the disk centre, inclination, PA, systemic and rotational velocity iteratively e.g., Rots (1975), Begeman (1989), Schoenmakers, Franx & de Zeeuw (1997) Fathi et al. (2004; 2005; 2007; 2008, 2009), van de Ven & Fathi (2009)
Harmonic Decomposition of a Velocity Field Assuming differential rotation, one can section a velocity field into concentric rings and fit the disk centre, inclination, PA, systemic and rotational velocity iteratively e.g., Rots (1975), Begeman (1989), Schoenmakers, Franx & de Zeeuw (1997) Fathi et al. (2004; 2005; 2007; 2008, 2009), van de Ven & Fathi (2009)
Harmonic Decomposition of a Velocity Field Assuming differential rotation, one can section a velocity field into concentric rings and fit the disk centre, inclination, PA, systemic and rotational velocity iteratively e.g., Rots (1975), Begeman (1989), Schoenmakers, Franx & de Zeeuw (1997) Fathi et al. (2004; 2005; 2007; 2008, 2009), van de Ven & Fathi (2009)
Analytic Models Perturbed potential: Pitch angle logarithmic spiral: Wong et al. (2004), Fathi et al. (2004; 2005), van de Ven & Fathi (2009)
Combination with Predictions From Epicyclic Approximation
Combination with Predictions From Epicyclic Approximation
A SAURON Study of the Bar in NGC 5448 Fathi et al. (2005)
A SAURON Study of the Bar in NGC 5448 Fathi et al. (2005)
Emsellem, Fathi et al. (2006) A SAURON Study of NGC 1068
Size and Strength of the Spiral Arms in NGC 1068 Emsellem, Fathi et al. (2006)
Size and Strength of the Spiral Arms in NGC 1068 Mass model from rotation curve disk mass, halo mass, bulge mass, multiple comp. Emsellem, Fathi et al. (2006)
Size and Strength of the Spiral Arms in NGC 1068 Mass model from rotation curve disk mass, halo mass, bulge mass, multiple comp. Inflow due to the spiral arms arm size, arm contrast, pitch angle Emsellem, Fathi et al. (2006)
Fathi et al. (2008) The Nuclear Spirals in M83 with GHAFAS
Fathi et al. (2008) The Nuclear Spirals in M83 with GHAFAS
Fathi et al. (2008) The Nuclear Spirals in M83 with GHAFAS
Fathi et al. (2008) The Bar-driven Circumnuclear Starburst in M83
The Bar-driven Circumnuclear Starburst in M83 The data give the first high-resolution view over 2 kpc radius Fathi et al. (2008)
The Bar-driven Circumnuclear Starburst in M83 The data give the first high-resolution view over 2 kpc radius Fathi et al. (2008)
The Bar-driven Circumnuclear Starburst in M83 The data give the first high-resolution view over 2 kpc radius We have been able to kinematically follow the gas falling in from 10 kpc to within 300 light-years from the nucleus Fathi et al. (2008)
The Bar-driven Circumnuclear Starburst in M83 The data give the first high-resolution view over 2 kpc radius We have been able to kinematically follow the gas falling in from 10 kpc to within 300 light-years from the nucleus Fathi et al. (2008)
The Bar-driven Circumnuclear Starburst in M83 The data give the first high-resolution view over 2 kpc radius We have been able to kinematically follow the gas falling in from 10 kpc to within 300 light-years from the nucleus and unveiled the inner disk with 5% of the total ISM mass of the galaxy Fathi et al. (2008)
The Bar-driven Circumnuclear Starburst in M83 The data give the first high-resolution view over 2 kpc radius We have been able to kinematically follow the gas falling in from 10 kpc to within 300 light-years from the nucleus and unveiled the inner disk with 5% of the total ISM mass of the galaxy Fathi et al. (2008)
The Bar-driven Circumnuclear Starburst in M83 The data give the first high-resolution view over 2 kpc radius We have been able to kinematically follow the gas falling in from 10 kpc to within 300 light-years from the nucleus and unveiled the inner disk with 5% of the total ISM mass of the galaxy The infalling gas is driven by the bar and is responsible for forming the disk, as well as feeding the circumnuclear starburst in this galaxy. Fathi et al. (2008)
Fathi et al. (2006) The Nuclear Spiral Arms in NGC 1097
Fathi et al. (2006) The Nuclear Spiral Arms in NGC 1097
Fathi et al. (2006) The Nuclear Spiral Arms in NGC 1097
The Nuclear Spiral Arms in NGC 1097 Fathi et al. (2006) GMOS-IFU on Gemini-South; 3 x 30 min = 1.5 h on-source Spatial 0.1 arcsec; spectral 5600-7000 Å at 85 km/s FWHM
The Nuclear Spiral Arms in NGC 1097 Fathi et al. (2006), van de Ven & Fathi (2010)
The Nuclear Spiral Arms in NGC 1097 Fathi et al. (2006), van de Ven & Fathi (2010)
Active galaxy NGC 1097 located about 47 million light-years away. Ring structure around central region is expanded below. Artist s conception of NGC 1097 s inner ring structure which is about 4,500 light-years in diameter. This is the region where several thousand spectra were obtained with the Gemini Multi-object Spectrograph to understand the detailed motions of this gas. Full-resolution artwork available at: www.gemini.edu/ngc1097 Artist s conception of inner 2000 Astronomical Units-wide (about 11.5 light days) accretion disk surrounding supermassive black hole at the core of NGC 1097. All artwork courtesy of Gemini Observatory by Jon Lomberg Fathi et al. (2006), van de Ven & Fathi (2010)
Spiral Perturbation Model for NGC 1097 m=2 spiral perturbation potential m=2 spiral surface brightness m=3 (and 1) spiral line-of-sight velocity van de Ven & Fathi (2010)
Mass Inflow Rate from [SII] onto the SMBH in NGC 1097 inflow velocity spiral model gas (over)density [SII] doublet ~6700Å geometric area Toomre s Q=1 van de Ven & Fathi (2010)
Combination with CO studies Combining optical with CO kinematics is crucial to link the dynamics with the state of he ISM How much of the gas is being converted into stars at and/or inside the resonance points How much the cold gas is displaced with respect to its hot counterparts Do dynamical models correctly predict the location and strength of the shocks How much gas is funnelled all the way into an AGN? Can the inflow sustain nuclear starburst, AGN activity?
Piñol-Ferrer, Fathi et al. (2011) What Do the Molecules Teach Us?
Piñol-Ferrer, Fathi et al. (2011) What Do the Molecules Teach Us?
Feeding the Supermassive Black Hole in NGC 1097 Stellar velocity dispersion 196 km/s (Lewis & Eracleous 2006) Black hole mass 1.2 x 10 8 M sun (Tremaine et al. 2002) Eddington accretion rate (ε=0.1) (dm/dt) Edd = 2.7 M sun /yr Fitting spectral energy distribution (dm/dt) SED = 0.0064 (dm/dt) Edd (Nemmen et al. 2006) (dm/dt) 70pc = 4.2 x 10-3 (dm/dt) Edd = 0.011 M sun /yr van de Ven & Fathi (2010)
Feeding the Supermassive Black Hole in NGC 1097 Stellar velocity dispersion 196 km/s (Lewis & Eracleous 2006) Black hole mass 1.2 x 10 8 M sun (Tremaine et al. 2002) Eddington accretion rate (ε=0.1) (dm/dt) Edd = 2.7 M sun /yr Fitting spectral energy distribution (dm/dt) SED = 0.0064 (dm/dt) Edd (Nemmen et al. 2006) (dm/dt) 70pc = 4.2 x 10-3 (dm/dt) Edd = 0.011 M sun /yr van de Ven & Fathi (2010) (dm/dt) 70pc [CO data]= 0.11 M sun /yr
MODELLING BARS AND SPIRAL ARMS TOGETHER
MODELLING BARS AND SPIRAL ARMS TOGETHER Piñol-Ferrer, Lindblad, Fathi (2012) arxiv:1112.3658
MODELLING BARS AND SPIRAL ARMS TOGETHER Piñol-Ferrer, Lindblad, Fathi (2012) arxiv:1112.3658
MODELLING BARS AND SPIRAL ARMS TOGETHER Piñol-Ferrer, Lindblad, Fathi (2012) arxiv:1112.3658
In Summary: IFUs deliver a wealth of data to analyse, and our models are reaching a stage where we can make sense of the information in a semi-quantitative way. We cannot only aim for the next generation IFUs without exploring the already available data to its full extent...