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

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

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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

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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)

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the center of most galaxies

Neumayer et al 2011, Carollo et al. 1998, Matthews et al. 1999, Böker et al. 2002, 2003, 2004, Böker 2010, Côte et al. 2006 1.2kpc x 1.2kpc 1.2kpc x 1.2kpc

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the center of most galaxies

Neumayer et al 2011, Carollo et al. 1998, Matthews et al. 1999, Böker et al. 2002, 2003, 2004, Böker 2010, Côte et al. 2006 1.2kpc x 1.2kpc 1.2kpc x 1.2kpc

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the center of most galaxies

Neumayer et al 2011, Carollo et al. 1998, Matthews et al. 1999, Böker et al. 2002, 2003, 2004, Böker 2010, Côte et al. 2006 1.2kpc x 1.2kpc

NSC

1.2kpc x 1.2kpc

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the centre of most galaxies

Böker+ 2002, 2004; Carollo+ 2002; Coté+ 2006; Balcells+ 2007; Georgiev & Böker 2014; den Brok+ 2014

Very common: >77% late types >66% early types lower limits!

(Böker+ 2002, Côté+ 2006, Georgiev+ 2014)

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the centre of most galaxies

Böker+ 2002, 2004; Carollo+ 2002; Coté+ 2006; Balcells+ 2007; Georgiev & Böker 2014; den Brok+ 2014

Very common: >77% late types >66% early types lower limits!

(Böker+ 2002, Côté+ 2006, Georgiev+ 2014)

Very compact:

Reff ∼ 2 − 5pc

Very massive:

M ∼ 106 − 107M

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SLIDE 7

Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Nuclear Star Clusters (NSCs) are observed at the centre of most galaxies

Böker+ 2002, 2004; Carollo+ 2002; Coté+ 2006; Balcells+ 2007; Georgiev & Böker 2014; den Brok+ 2014

Very common: >77% late types >66% early types lower limits!

(Böker+ 2002, Côté+ 2006, Georgiev+ 2014)

Very compact:

Reff ∼ 2 − 5pc

Very massive:

M ∼ 106 − 107M

Carson et al. 2016

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

NSCs form through cluster infall and/or in-situ star formation

(Loose+ 1982, Milosavljevic+ 2004, Pflamm-Altenburg+ 2009,...)

Gas accretion and in situ star formation

NSC

Accretion & merger of star clusters

(Tremaine+ 1975, Capuzzo-Dolcetta 1993, Capuzzo-Dolcetta & Miocchi 2008; Antonini+ 2012, Antonini 2013, 2015,

NSC

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The Milky Way has a NSC hosting a central Massive Black Hole

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The Milky Way has a NSC hosting a central Massive Black Hole

( Schödel+ 2014)

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The Milky Way has a NSC hosting a central Massive Black Hole

( Schödel+ 2014)

Sgr A*

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The Milky Way has a NSC hosting a central Massive Black Hole

( Schödel+ 2014)

Sgr A*

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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.
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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We modelled NSC formation from cluster infalls using N-body simulations

4 · 1 06 M

108M

Nuclear bulge (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.

Supermassive Black Hole

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We modelled NSC formation from cluster infalls using N-body simulations

4 · 1 06 M

108M

Nuclear bulge (Milky Way-like)

12 GCs with random

  • rientations

1.1 · 106M

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.

Supermassive Black Hole

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We modelled NSC formation from cluster infalls using N-body simulations

4 · 1 06 M

108M

Nuclear bulge (Milky Way-like)

12 GCs with random

  • rientations

1.1 · 106M

N u c l e a r S t a r C l u s t e r

1.5 · 107M

~12 Gyr

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.

Supermassive Black Hole

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The simulated NSC is very similar to the MW one

similar flattening q~0.7 (Schödel+ 2014) similar tangential anisotropy β~ -0.1 (Meritt+ 2010) similar density profile

(Schödel+ 2014)

similar BH mass

(Ghez+ 2008)

∼ 4 · 106M

similar to MW NSC mass ∼ 2 · 107M (Schödel+ 2014)

Antonini et al. 2012; Tsatsi, Mastrobuono-Battisti et al., 2017

Supermassive Black Hole

N u c l e a r S t a r C l u s t e r

~12 Gyr

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The simulated NSC rotates as much as the

  • bserved one

Tsatsi, Mastrobuono-Battisti et al., 2017; Feldmeier et al. 2014

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The simulated NSC rotates as much as the

  • bserved one

Tsatsi, Mastrobuono-Battisti et al., 2017; Feldmeier et al. 2014

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg S i m u l a t i

  • n

I I

Simulation I Simulation II Simulation III

Tsatsi, Mastrobuono-Battisti et al., 2017

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg S i m u l a t i

  • n

I I

Simulation I Simulation II Simulation III

Tsatsi, Mastrobuono-Battisti et al., 2017

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg S i m u l a t i

  • n

I I

Simulation I Simulation II Simulation III

Tsatsi, Mastrobuono-Battisti et al., 2017

ISAAC VLT Feldmeier + 2014

The Milky Way NSC

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg S i m u l a t i

  • n

I I

Simulation I Simulation II Simulation III

Tsatsi, Mastrobuono-Battisti et al., 2017

ISAAC VLT Feldmeier + 2014

The Milky Way NSC

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Tsatsi, Mastrobuono-Battisti et al., 2017

S i m u l a t i

  • n

I I

Simulation I Simulation II Simulation III

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Tsatsi, Mastrobuono-Battisti et al., 2017

S i m u l a t i

  • n

I I

Simulation I Simulation II Simulation III

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Tsatsi, Mastrobuono-Battisti et al., 2017

S i m u l a t i

  • n

I I

Simulation I Simulation II Simulation III

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Tsatsi, Mastrobuono-Battisti et al., 2017

S i m u l a t i

  • n

I I

Simulation I Simulation II Simulation III

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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)

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

If globular clusters contribute to the formation of nuclear clusters, they could bring IMBHs to the Galactic Centre

x

4 · 1 06 M

108M

Nuclear bulge

Massive Black Hole

(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)

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

If globular clusters contribute to the formation of nuclear clusters, they could bring IMBHs to the Galactic Centre

x

4 · 1 06 M

108M

Nuclear bulge

Massive Black Hole

(Milky Way-like)

12 GCs with random

  • rientations

1.1 · 106M

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)

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SLIDE 31

Alessandra Mastrobuono-Battisti MPIA, Heidelberg

If globular clusters contribute to the formation of nuclear clusters, they could bring IMBHs to the Galactic Centre

x

4 · 1 06 M

108M

Nuclear bulge

Massive Black Hole

(Milky Way-like)

12 GCs with random

  • rientations

1.1 · 106M

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)

IMBHs

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

If globular clusters contribute to the formation of nuclear clusters, they could bring IMBHs to the Galactic Centre

x

4 · 1 06 M

108M

Nuclear bulge

Massive Black Hole

(Milky Way-like)

12 GCs with random

  • rientations

1.1 · 106M

N u c l e a r S t a r C l u s t e r

1.5 · 107M

~ 1 2 G y r

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)

IMBHs

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

IMBHs may be present in dense clusters and decay with them

Mastrobuono-Battisti et al., 2014

Massive clusters may host an IMBH (Silk & Arons 1975)

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

IMBHs may be present in dense clusters and decay with them

Mastrobuono-Battisti et al., 2014

Massive clusters may host an IMBH (Silk & Arons 1975)

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The presence of IMBHs causes the NSC to have a steep cusp and to be strongly mass segregated

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

without IMBHs

Mastrobuono-Battisti et al., 2014

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

The presence of IMBHs causes the NSC to have a steep cusp and to be strongly mass segregated

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

Mastrobuono-Battisti et al., 2014

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We can estimate the tidal disruption events rate

Image credit: NASA/CXC/ M.Weiss

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

Mastrobuono-Battisti et al., 2014

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SLIDE 38

Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We can estimate the tidal disruption events rate

Image credit: NASA/CXC/ M.Weiss

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

Mastrobuono-Battisti et al., 2014

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SLIDE 39

Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We can estimate the tidal disruption events rate

Image credit: NASA/CXC/ M.Weiss

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

Mastrobuono-Battisti et al., 2014

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We can estimate the tidal disruption events rate

Image credit: NASA/CXC/ M.Weiss

Komossa 2012; Khabibullin & Sazonov 2014

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

Mastrobuono-Battisti et al., 2014

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SLIDE 41

Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We can estimate the tidal disruption events rate

Image credit: NASA/CXC/ M.Weiss

Komossa 2012; Khabibullin & Sazonov 2014

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

Mastrobuono-Battisti et al., 2014

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SLIDE 42

Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We can estimate the tidal disruption events rate

Image credit: NASA/CXC/ M.Weiss

Komossa 2012; Khabibullin & Sazonov 2014

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

Mastrobuono-Battisti et al., 2014

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We can estimate the tidal disruption events rate

Image credit: NASA/CXC/ M.Weiss

Komossa 2012; Khabibullin & Sazonov 2014

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

Mastrobuono-Battisti et al., 2014

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

We can estimate the tidal disruption events rate

Image credit: NASA/CXC/ M.Weiss

No IMBHs in NSCs?

Komossa 2012; Khabibullin & Sazonov 2014

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

Mastrobuono-Battisti et al., 2014

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Alessandra Mastrobuono-Battisti MPIA, Heidelberg

Take-home messages

  • NSCs can form through the infall and

merger of massive and dense globular clusters, however we need to combine dynamics and chemistry of stars to disentangle the Galactic NSC history.

  • NSCs are very common and can co-exist

with a central supermassive black hole.

10−1 100 101 102

r (pc)

101 102 103 104 105 106

ρ (M/pc3)

with IMBHs without IMBHs

  • The expected TDE rate excludes

the presence of multiple IMBHs at the Galactic centre.