Supermassive and intermediate-mass black holes in nuclear star - PowerPoint PPT Presentation

Supermassive and intermediate-mass black holes in nuclear star clusters Alessandra Mastrobuono-Battisti (Lund Observatory) Nadine Neumayer, Anna Sippel, Sassa Tsatsi (MPIA) Hagai Perets (Technion) Glenn van de Ven (Vienna) Roberto Capuzzo-Dolcetta (Sapienza)

Nuclear Star Clusters (NSCs) are observed at the center of most galaxies 1.2kpc x 1.2kpc 1.2kpc x 1.2kpc Neumayer et al 2011, Carollo et al. 1998, Matthews et al. 1999, Böker et al. 2002, 2003, 2004, Böker 2010, Côte et al. 2006 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the center of most galaxies 1.2kpc x 1.2kpc 1.2kpc x 1.2kpc Neumayer et al 2011, Carollo et al. 1998, Matthews et al. 1999, Böker et al. 2002, 2003, 2004, Böker 2010, Côte et al. 2006 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the center of most galaxies NSC 1.2kpc x 1.2kpc 1.2kpc x 1.2kpc Neumayer et al 2011, Carollo et al. 1998, Matthews et al. 1999, Böker et al. 2002, 2003, 2004, Böker 2010, Côte et al. 2006 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the centre of most galaxies Very common: >77% late types lower >66% early types limits! (Böker+ 2002, Côté+ 2006, Georgiev+ 2014) Böker+ 2002, 2004; Carollo+ 2002; Coté+ 2006; Balcells+ 2007; Georgiev & Böker 2014; den Brok+ 2014 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the centre of most galaxies Very common: >77% late types lower >66% early types limits! (Böker+ 2002, Côté+ 2006, Georgiev+ 2014) Very compact: R eff ∼ 2 − 5 pc Very massive: M ∼ 10 6 − 10 7 M � Böker+ 2002, 2004; Carollo+ 2002; Coté+ 2006; Balcells+ 2007; Georgiev & Böker 2014; den Brok+ 2014 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the centre of most galaxies Very common: >77% late types lower >66% early types limits! (Böker+ 2002, Côté+ 2006, Georgiev+ 2014) Carson et al. 2016 Very compact: R eff ∼ 2 − 5 pc Very massive: M ∼ 10 6 − 10 7 M � Böker+ 2002, 2004; Carollo+ 2002; Coté+ 2006; Balcells+ 2007; Georgiev & Böker 2014; den Brok+ 2014 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

NSCs form through cluster infall and/or in-situ star formation Gas accretion and NSC in situ star formation (Loose+ 1982, Milosavljevic+ 2004, Pflamm-Altenburg+ 2009,...) Accretion & merger of NSC star clusters (Tremaine+ 1975, Capuzzo-Dolcetta 1993, Capuzzo-Dolcetta & Miocchi 2008; Antonini+ 2012, Antonini 2013, 2015, Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The Milky Way has a NSC hosting a central Massive Black Hole Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The Milky Way has a NSC hosting a central Massive Black Hole ( Schödel+ 2014) Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The Milky Way has a NSC hosting a central Massive Black Hole ( Schödel+ 2014) Sgr A* Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The Milky Way has a NSC hosting a central Massive Black Hole ( Schödel+ 2014) Sgr A* Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We modelled NSC formation from cluster infalls using N -body simulations Credit: Sassa Tsatsi Antonini, Capuzzo-Dolcetta, Mastrobuono-Battisti & Merritt, 2012 ApJ; Perets & Mastrobuono-Battisti , 2014, ApJ; Mastrobuono-Battisti , Perets & Loeb, 2014, ApJ; Tsatsi, Mastrobuono-Battisti et al., 2017, MNRAS. See also Hartmann et al., 2011. Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We modelled NSC formation from cluster infalls using N -body simulations Nuclear bulge 10 8 M � Supermassive Black Hole 0 6 M � 1 4 · (Milky Way-like) Credit: Sassa Tsatsi Antonini, Capuzzo-Dolcetta, Mastrobuono-Battisti & Merritt, 2012 ApJ; Perets & Mastrobuono-Battisti , 2014, ApJ; Mastrobuono-Battisti , Perets & Loeb, 2014, ApJ; Tsatsi, Mastrobuono-Battisti et al., 2017, MNRAS. See also Hartmann et al., 2011. Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We modelled NSC formation from cluster infalls using N -body simulations Nuclear bulge 12 GCs with 10 8 M � random orientations Supermassive 1 . 1 · 10 6 M � Black Hole 0 6 M � 1 4 · (Milky Way-like) Credit: Sassa Tsatsi Antonini, Capuzzo-Dolcetta, Mastrobuono-Battisti & Merritt, 2012 ApJ; Perets & Mastrobuono-Battisti , 2014, ApJ; Mastrobuono-Battisti , Perets & Loeb, 2014, ApJ; Tsatsi, Mastrobuono-Battisti et al., 2017, MNRAS. See also Hartmann et al., 2011. Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We modelled NSC formation from cluster infalls using N -body simulations r a e c l u N Nuclear bulge 12 GCs with r e s t u C l a r t S 10 8 M � random orientations ~12 Gyr Supermassive 1 . 1 · 10 6 M � Black Hole 1 . 5 · 10 7 M � 0 6 M � 1 4 · (Milky Way-like) Credit: Sassa Tsatsi Antonini, Capuzzo-Dolcetta, Mastrobuono-Battisti & Merritt, 2012 ApJ; Perets & Mastrobuono-Battisti , 2014, ApJ; Mastrobuono-Battisti , Perets & Loeb, 2014, ApJ; Tsatsi, Mastrobuono-Battisti et al., 2017, MNRAS. See also Hartmann et al., 2011. Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The simulated NSC is very similar to the MW one r e a l u c N e r t u s l C r a S t ~12 Gyr Supermassive Black Hole similar to MW NSC mass ∼ 2 · 10 7 M � (Schödel+ 2014) similar BH mass ∼ 4 · 10 6 M � (Ghez+ 2008) similar flattening q~0.7 (Schödel+ 2014) similar density profile (Schödel+ 2014) similar tangential anisotropy β ~ -0.1 (Meritt+ 2010) Antonini et al. 2012; Tsatsi, Mastrobuono-Battisti et al., 2017 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The simulated NSC rotates as much as the observed one Tsatsi, Mastrobuono-Battisti et al., 2017; Feldmeier et al. 2014 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The simulated NSC rotates as much as the observed one Tsatsi, Mastrobuono-Battisti et al., 2017; Feldmeier et al. 2014 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Simulation I Simulation II I I n o i t a l u Simulation III m i S Tsatsi, Mastrobuono-Battisti et al., 2017 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Simulation I Simulation II I I n o i t a l u Simulation III m i S Tsatsi, Mastrobuono-Battisti et al., 2017 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Simulation I The Milky Way NSC Simulation II I I n o i t a l u Simulation III m i S ISAAC VLT Feldmeier + 2014 Tsatsi, Mastrobuono-Battisti et al., 2017 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Simulation I The Milky Way NSC Simulation II I I n o i t a l u Simulation III m i S ISAAC VLT Feldmeier + 2014 Tsatsi, Mastrobuono-Battisti et al., 2017 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Simulation I Simulation II I I n o i t a l u Simulation III m i S Tsatsi, Mastrobuono-Battisti et al., 2017 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Simulation I Simulation II I I n o i t a l u Simulation III m i S Tsatsi, Mastrobuono-Battisti et al., 2017 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Simulation I Simulation II I I n o i t a l u Simulation III m i S Tsatsi, Mastrobuono-Battisti et al., 2017 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Simulation I Simulation II I I n o i t a l u Simulation III m i S Tsatsi, Mastrobuono-Battisti et al., 2017 Alessandra Mastrobuono-Battisti MPIA, Heidelberg

If globular clusters contribute to the formation of nuclear clusters, they could bring IMBHs to the Galactic Centre x Credit: Sassa Tsatsi Antonini, Capuzzo-Dolcetta, Mastrobuono-Battisti & Merritt, 2012 ApJ; Perets & Mastrobuono-Battisti , 2014, ApJ; Mastrobuono-Battisti , Perets & Loeb, 2016, ApJ; Tsatsi, Mastrobuono-Battisti et al., 2016, MNRAS See also Hartmann+ 2011, Massive clusters may host an IMBH (Silk & Arons 1975) Alessandra Mastrobuono-Battisti MPIA, Heidelberg

If globular clusters contribute to the formation of nuclear clusters, they could bring IMBHs to the Galactic Centre Nuclear bulge 10 8 M � x Massive Black Hole 0 6 M � 1 4 · (Milky Way-like) Credit: Sassa Tsatsi Antonini, Capuzzo-Dolcetta, Mastrobuono-Battisti & Merritt, 2012 ApJ; Perets & Mastrobuono-Battisti , 2014, ApJ; Mastrobuono-Battisti , Perets & Loeb, 2016, ApJ; Tsatsi, Mastrobuono-Battisti et al., 2016, MNRAS See also Hartmann+ 2011, Massive clusters may host an IMBH (Silk & Arons 1975) Alessandra Mastrobuono-Battisti MPIA, Heidelberg

If globular clusters contribute to the formation of nuclear clusters, they could bring IMBHs to the Galactic Centre Nuclear bulge 12 GCs with 10 8 M � random orientations x Massive 1 . 1 · 10 6 M � Black Hole 0 6 M � 1 4 · (Milky Way-like) Credit: Sassa Tsatsi Antonini, Capuzzo-Dolcetta, Mastrobuono-Battisti & Merritt, 2012 ApJ; Perets & Mastrobuono-Battisti , 2014, ApJ; Mastrobuono-Battisti , Perets & Loeb, 2016, ApJ; Tsatsi, Mastrobuono-Battisti et al., 2016, MNRAS See also Hartmann+ 2011, Massive clusters may host an IMBH (Silk & Arons 1975) Alessandra Mastrobuono-Battisti MPIA, Heidelberg