scholarly journals UPDATED MASS SCALING RELATIONS FOR NUCLEAR STAR CLUSTERS AND A COMPARISON TO SUPERMASSIVE BLACK HOLES

2013 ◽  
Vol 763 (2) ◽  
pp. 76 ◽  
Author(s):  
Nicholas Scott ◽  
Alister W. Graham
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Supermassive Black Holes ◽  
Scaling Relations ◽  
Mass Scaling

scholarly journals Black hole and nuclear cluster scaling relations: Mbh ∝ Mnc2.7±0.7

2014 ◽  
Vol 10 (S312) ◽  
pp. 269-273 ◽  
Author(s):  
Alister W. Graham
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Star Clusters ◽  
Compact Object ◽  
Scaling Relations ◽  
Black Hole Mass ◽  
Massive Black Holes ◽  
Mass Scaling ◽  
Nuclear Cluster ◽  
Evolutionary Growth

AbstractThere is a growing array of supermassive black hole and nuclear star cluster scaling relations with their host spheroid, including a bent (black hole mass)–(host spheroid mass) Mbh–Msph relation and a different (massive compact object mass)–(host spheroid velocity dispersion) Mmco–σ relations for black holes and nuclear star clusters. By combining the observed Mbh ∝ σ5.5 relation with the observed Mnc ∝ σ1.6–2.7 relation, we derive the expression Mbh ∝ Mnc2–3.4, which should hold until the nuclear star clusters are eventually destroyed in the larger core-Sérsic spheroids. This new mass scaling relation helps better quantify the rapid evolutionary growth of massive black holes in dense star clusters, and the relation is consistently recovered when coupling the observed Mnc ∝ Msph0.6–1.0 relation with the recently observed quadratic relation Mbh ∝ Msph2 for Sérsic spheroids.

scholarly journals Nuclear star clusters

2009 ◽  
Vol 5 (S266) ◽  
pp. 58-63 ◽  
Author(s):  
Torsten Böker
Keyword(s):  
Black Holes ◽  
Structural Properties ◽  
Galaxy Evolution ◽  
Globular Clusters ◽  
Star Clusters ◽  
Supermassive Black Holes ◽  
Subsequent Growth ◽  
Local Universe ◽  
Fundamental Plane ◽  
Evolutionary Connection

AbstractThe centers of most galaxies in the local Universe are occupied by compact, barely resolved sources. Based on their structural properties, position in the Fundamental Plane, and integrated spectra, these sources clearly have a stellar origin. They are therefore called ‘nuclear star clusters’ (NCs) or ‘stellar nuclei’. NCs are found in galaxies of all Hubble types, suggesting that their formation is intricately linked to galaxy evolution. Here, I review some recent studies of NCs, describe ideas for their formation and subsequent growth, and touch on their possible evolutionary connection with both supermassive black holes and globular clusters.

scholarly journals The X-Ray Halo Scaling Relations of Supermassive Black Holes

2019 ◽  
Vol 884 (2) ◽  
pp. 169 ◽  
Author(s):  
M. Gaspari ◽  
D. Eckert ◽  
S. Ettori ◽  
P. Tozzi ◽  
L. Bassini ◽  
...  
Keyword(s):  
Black Holes ◽  
Supermassive Black Holes ◽  
Scaling Relations ◽  
X Ray

scholarly journals Nuclear Star Clusters (Nuclei) in Spirals and Connection to Supermassive Black Holes

2006 ◽  
Vol 2 (S241) ◽  
Author(s):  
Roeland P. van der Marel ◽  
Joern Rossa ◽  
Carl Jakob Walcher ◽  
Torsten Boeker ◽  
Luis C. Ho ◽  
...  
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Supermassive Black Holes

scholarly journals Coevolution (or not) of supermassive black holes and host galaxies: Black hole scaling relations are not biased by selection effects

2019 ◽  
Vol 14 (S353) ◽  
pp. 186-198
Author(s):  
John Kormendy
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Velocity Dispersion ◽  
Stellar Mass ◽  
Supermassive Black Holes ◽  
Scaling Relations ◽  
Selection Effects ◽  
Host Galaxies ◽  
Scatter Plots ◽  
Host Properties

AbstractThe oral version of this paper summarized Kormendy & Ho 2013, ARA&A, 51, 511. However, earlier speakers at this Symposium worried that selection effects bias the derivation of black hole scaling relations. I therefore added – and this proceedings paper emphasizes – a discussion of why we can be confident that selection effects do not bias the observed correlations between BH mass M• and the luminosity, stellar mass, and velocity dispersion of host ellipticals and classical bulges. These are the only galaxy components that show tight BH-host correlations. The scatter plots of M• with host properties for pseudobulges and disks are upper envelopes of scatter that does extend to lower BH masses. BH correlations are most consistent with a picture in which BHs coevolve only with classical bulges and ellipticals. Four physical regimes of coevolution (or not) are suggested by Kormendy & Ho 2013 and are summarized here.

scholarly journals Masses and scaling relations for nuclear star clusters, and their co-existence with central black holes

2016 ◽  
Vol 457 (2) ◽  
pp. 2122-2138 ◽  
Author(s):  
Iskren Y. Georgiev ◽  
Torsten Böker ◽  
Nathan Leigh ◽  
Nora Lützgendorf ◽  
Nadine Neumayer
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Scaling Relations
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