Simulating the mass assembly history of Nuclear Star Clusters · Simulating the mass assembly history of Nuclear Star Clusters The imprints of cluster inspirals Alessandra Mastrobuono-Battisti

Simulating the mass assembly history of Nuclear Star Clusters

The imprints of cluster inspirals

Alessandra Mastrobuono-Battisti

Sassa Tsatsi Hagai Perets

Nadine Neumayer Glenn vad de Ven

Ryan Leyman David Merritt

Roberto Capuzzo-Dolcetta Fabio Antonini

Avi LoebStellar Aggregates, Bad Honnef, 8-12-2016

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

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

1.2kpc x 1.2kpc

∼ 10” = 87pc

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

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

1.2kpc x 1.2kpc

∼ 10” = 87pc

NSC

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

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

• The in-situ star formation or gas model (Loose et al. 1982, Schinnerer et al. 2008, Milosavljevic 2004, Pflamm-Altenburg, Jan & Kroupa 2009), possibly in a disk like configuration.

• The cluster merger scenario (Tremaine et al. 1975, Ostriker 1988, Antonini, Capuzzo

Dolcetta, MB & Merritt 2012, Antonini 2013, Gnedin et al. 2013 and references therein).

Both processes can work in concert, and both could be important for the formation and evolution of NSCs.

• Initially: only the nuclear bulge of the galaxy;

• An MBH (4x106M⊙) is at the center of the galaxy;

• The NSC is build up by consecutive infalls;

• Collisional evolution of the NSC.

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

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






4 · 106M�

108M�



et al., 2016, MNRAS

Nuclear bulge

Massive Black Hole

(Milky Way-like)






4 · 106M�

108M�12 GCs with random orientations

1.1 · 106M�



et al., 2016, MNRAS

Nuclear bulge

Massive Black Hole

(Milky Way-like)






4 · 106M�

108M�12 GCs with random orientations

1.1 · 106M�

Nuclear Star Cluster

1.5 · 107M�

~12 Gyr



et al., 2016, MNRAS

Nuclear bulge

Massive Black Hole

(Milky Way-like)

GCs decay and merge, forming the NSC: models based on Milky Way data

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• 12 GCs, initially at 20pc • 1.1x106M⊙ each • ~800Myr between each infall

Antonini, Capuzzo-Dolcetta, Mastrobuono-Battisti &

Merritt (2012); Perets & Mastrobuono-Battisti (2014)

GCs decay and merge, forming the NSC: models based on Milky Way data

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• 12 GCs, initially at 20pc • 1.1x106M⊙ each • ~800Myr between each infall

Antonini, Capuzzo-Dolcetta, Mastrobuono-Battisti &

Merritt (2012); Perets & Mastrobuono-Battisti (2014)

GCs decay and merge, forming the NSC: snapshots

Antonini, Capuzzo-Dolcetta, Mastrobuono-Battisti & Merritt 2012,

1st 2nd 3rd 4th

7th6th4th 8th

9th 10th 11th 12th

The infall scenario forms an NSC with a large core-like structure

Antonini et al. 2012, Mastrobuono Battisti et al. 2014, Perets & MB 2014

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MNSC ~107M⊙

The Milky Way’s is the closest NSC

• It hosts a massive BH: Sgr A* MBH = 4.3×106M⊙

• Tangentially anisotropic, 0.1”-10”: (Merritt 2010).

• Flattened with q = 0.71±0.02 (Schödel et al. 2014).

Schödel (2010)

(Genzel et al. 2010; Ghez et al. 2008; Gillessen et al. 2009; Eisenhauer et al. 2005)

MNSC ~107M⊙






MNSC ~107M⊙






10Gyr

Simulations vs Observations: Direct comparison with the

Milky Way NSC

ν

Feldmeier + 2014

σ

What do we learn from observations?

arcsec arcsec

arcsec

arcs

ec

arcs

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We can get similar maps for the simulated cluster




The real and simulated NSC look similar

arcsec arcsec arcsec

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The real and simulated NSC look similar

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The similarity is apparent from radial plots

Feldmeier + 2014The similarity is apparent from radial plots

arcsec

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arcsec

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Feldmeier + 2014

Tsatsi, Mastrobuono-Battisti et al. 2017


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Which role has the bulge?

Which role has the bulge?

Kinematic profiles are still consistent

A&A 570, A2 (2014)

0.0 0.1 0.2 0.3 0.4 0.5 0.6COmag

3000

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f (K

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SupergiantGiant

F0 F2 G0 G2 G5 G8 K0 K1 K2 K3

K4 K5 K7 M0 M1 M2 M3 M4 M5 M6

Fig. 7. Relationship between e↵ective temperature Te↵ in K and the COindex COmag for giant (triangle symbol) and supergiant (square symbol)stars of the IRTF Spectral Library (Rayner et al. 2009). Di↵erent coloursdenote a di↵erent spectral type. The black horizontal line marks 4800 K,the black vertical line marks COmag = 0.09.

parameters, the kinematic position angle PAkin, and kinematicaxial ratio qkin (= 1 � ✏kin). By default qkin is constrained to theinterval [0.1, 1], while we let PAkin unconstrained.

The result of the kinemetric analysis of the velocity mapfrom the cleaned data cube (Fig. 5) is listed in Table 2, andthe upper panel of Fig. 8 shows the kinemetry model velocitymap. From the axial ratio one can distinguish three families ofellipses. The three innermost ellipses form the first family, thenext seven ellipses build the second family, and the outermostfive ellipses form the third family.

For the two outer families the kinematic position anglePAkin is 4�15� Galactic east of north, with a median valueof 9�. However, the photometric position angle PAphot was mea-sured by Schödel et al. (2014) using Spitzer data to ⇠0�. Thismeans that there is an o↵set between PAphot and PAkin. Totest whether this o↵set could be caused by extinction from the20 km s�1 cloud (M-0.13-0.08, e.g. García-Marín et al. 2011) inthe Galactic south-west, we flag all bins in the lower right cor-ner as bad pixels and repeat the analysis, but the position angleo↵set remains. We test the e↵ect of Voronoi binning by runningkinemetry on a velocity map with S/N = 80. While the valuesof qkin for the second family are by up to a a factor two higherwith this binning, the PAkin fit is rather robust. We obtain a me-dian value for PAkin of 12.6� beyond a semi-major axis distanceof r ⇠ 4000. We conclude that the e↵ect of the binning can varythe value of the PAkin, but the PA o↵set from the Galactic planeis robust to possible dust extinction and binning e↵ects. Also ourcleaning of bright stars and foreground stars may cause a bias inthe PAkin measurements. For comparison we run the kinemetryon the velocity map of the full data cube (Fig. 4). In this casethere is higher scattering in the kinemetric parameters, causedby shot noise. However, beyond 3500 semi-major axis distancethe median PAkin is at 6.1�, i.e. the PA o↵set is retained. Thissmaller value could come from the contribution of foregroundstars, which are aligned along the Galactic plane. It could alsomean that bright stars are not as misaligned to the photometricmajor axis as fainter stars are. Young stars tend to be brighter,thus the integrated light likely samples an older population thanthe individual stars. Analysis of the resolved stars in the colourinterval 1.5m H � K 3.5m and in the radial range of 5000

V model

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Fig. 8. Upper panel: kinemetric model velocity map of the cleaned datacube. Black dots denote the best fitting ellipses. The model goes only tor ⇠ 10000 along the Galactic plane and to ⇠6000 perpendicular to it. TheVoronoi bin with the highest uncertainty was excluded from the model.Lower panel: the velocity map as in Fig. 5 shown in grayscale, the binsthat show rotation perpendicular to the Galactic plane are overplotted incolour scale.

to 10000 shows an o↵set in the rotation from the Galactic planeby (2.7±3.8)�. As previous studies focused on the brightest starsof the cluster, the PA o↵set of the old, faint population remainedundetected.

In the innermost family there is one ellipse with a positionangle of �81.5�, i.e. PAkin is almost perpendicular to the photo-metric position angle PAphot ⇡ 0�. This is caused by a substruc-ture at ⇠2000 north and south of Sgr A*, that seems to rotate onan axis perpendicular to the Galactic major axis. This feature ishighlighted in the lower panel of Fig. 8. North of Sgr A* wefind bins with velocities of 20 to 60 km s�1, while in the Galacticsouth bins with negative velocities around �10 to �30 km s�1 arepresent. The feature expands over several Voronoi bins north andsouth of Sgr A*. It extends over ⇠3500 (1.4 pc) along the Galacticplane, and ⇠3000 (1.2 pc) perpendicular to it.

This substructure also causes the small axial ratio valuesof the second family of ellipses between 3000 and 7000 in ourkinemetry model. All semi-minor axis distances from Sgr A*are below 2000, i.e. at smaller distances to Sgr A* than the per-pendicular substructure. Only the third family of ellipses, whichhas semi-major axis values above 7000, skips over this substruc-ture and reaches higher values of qkin.

To check if the perpendicular rotating substructure is real, weapply Voronoi binning with a higher S/N of 80 instead of 60, andobtain again this almost symmetric north-south structure. Alsowith a lower S/N of 50, the substructure appears in both datacubes. We also check the influence of the cleaning from brightstars on this feature using the cleaned maps with Kcut = 11m andKcut = 12m. The substructure remains also in these data cubes,independent of the applied binning. The fact that this feature per-sists independent on the applied magnitude cut, or binning, and

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Can we predict kinematic substructures?

Feldmeier+2014

Tsatsi, Mastrobuono-Battisti et al., 2017


Feldmeier+2014

Kinemetry (Krajnovic’+2006)



Feldmeier+2014




Created by a polar merger

Feldmeier+2014





Feldmeier+2014





The effect of IMBHs on the formation and evolution of NSCs

IMBHs may be present in dense clusters and decay with them

Silk & Arons (1975): massive clusters may host an IMBH at their center:

• The merging model implies the presence of IMBHs in NSCs.

• We introduced an IMBH in each GC

Orbital radius of the last IMBH to fall in

The other 11 IMBHs

Mastrobuono-Battisti et al., 2014

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

without IMBHs

with IMBHs

Mastrobuono-Battisti et al., 2014

We can estimate the tidal disruption events rate

Image credit: NASA/CXC/M.Weiss







Komossa 2012; Khabibullin & Sazonov 2014












No IMBHs in NSCs?


Conclusions

• N-body simulations to study the merger scenario

Conclusions


Conclusions

• Direct comparison with the Milky Way NSC: mock observational maps


Conclusions


• The infall scenario reproduces most of the properties of the MW NSC, including its rotation


Conclusions



• We also find kinematic substructures similar to the observed one: the infall scenario is really plausible!


Conclusions




• No IMBHs in NSCss? more observations needed!


Conclusions



• Can we predict chemical properties? (Leaman, MB, work in prog.)


• No IMBHs in NSCss? more observations needed!

Thank you!

Simulating the mass assembly history of Nuclear Star Clusters · Simulating the mass assembly history of Nuclear Star Clusters The imprints of cluster inspirals Alessandra Mastrobuono-Battisti

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