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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/28884
Title: The Next Generation Virgo Cluster Survey. XXIII. Fundamentals of Nuclear Star Clusters over Seven Decades in Galaxy Mass
Authors: Sánchez-Janssen, Rubén
Côté, Patrick
Ferrarese, Laura
Peng, Eric W.
Roediger, Joel
Blakeslee, John P.
Emsellem, Eric
Puzia, Thomas H.
Spengler, Chelsea
Taylor, James
Álamo-Martínez, Karla A.
Boselli, Alessandro
CANTIELLO, Michele 
Cuillandre, Jean-Charles
Duc, Pierre-Alain
Durrell, Patrick
Gwyn, Stephen
MacArthur, Lauren A.
Lançon, Ariane
Lim, Sungsoon
Liu, Chengze
Mei, Simona
Miller, Bryan
Muñoz, Roberto
Mihos, J. Christopher
Paudel, Sanjaya
Powalka, Mathieu
Toloba, Elisa
Issue Date: 2019
Journal: THE ASTROPHYSICAL JOURNAL 
Number: 878
Issue: 1
First Page: 18
Abstract: Using deep, high-resolution optical imaging from the Next Generation Virgo Cluster Survey, we study the properties of nuclear star clusters (NSCs) in a sample of nearly 400 quiescent galaxies in the core of Virgo with stellar masses 10<SUP>5</SUP> ≲ {\text{}}{M}<SUB>* </SUB>/{\text{}}{M}<SUB>☉ </SUB> ≲ 10<SUP>12</SUP>. The nucleation fraction reaches a peak value f <SUB>n</SUB> ≈ 90% for {\text{}}{M}<SUB>* </SUB> ≈ 10<SUP>9</SUP> {\text{}}{M}<SUB>☉ </SUB> galaxies and declines for both higher and lower masses, but nuclei populate galaxies as small as {\text{}}{M}<SUB>* </SUB> ≈ 5 × 10<SUP>5</SUP> {\text{}}{M}<SUB>☉ </SUB>. Comparison with literature data for nearby groups and clusters shows that at the low-mass end nucleation is more frequent in denser environments. The NSC mass function peaks at M <SUB>NSC</SUB> ≈ 7 × 10<SUP>5</SUP> {\text{}}{M}<SUB>☉ </SUB>, a factor 3-4 times larger than the turnover mass for globular clusters (GCs). We find a nonlinear relation between the stellar masses of NSCs and those of their host galaxies, with a mean nucleus-to-galaxy mass ratio that drops to M <SUB>NSC</SUB>/M <SUB>⋆</SUB> ≈ 3.6 × 10<SUP>-3</SUP> for {\text{}}{M}<SUB>* </SUB> ≈ 5 × 10<SUP>9</SUP> {\text{}}{M}<SUB>☉ </SUB> galaxies. Nuclei in both more and less massive galaxies are much more prominent: {M}<SUB>NSC</SUB>}\propto {M}<SUB>* </SUB><SUP>0.46</SUP> at the low-mass end, where nuclei are nearly 50% as massive as their hosts. We measure an intrinsic scatter in NSC masses at a fixed galaxy stellar mass of 0.4 dex, which we interpret as evidence that the process of NSC growth is significantly stochastic. At low galaxy masses we find a close connection between NSCs and GC systems, including very similar occupation distributions and comparable total masses. We discuss these results in the context of current dissipative and dissipationless models of NSC formation.
URI: http://hdl.handle.net/20.500.12386/28884
URL: https://iopscience.iop.org/article/10.3847/1538-4357/aaf4fd
ISSN: 0004-637X
DOI: 10.3847/1538-4357/aaf4fd
Bibcode ADS: 2019ApJ...878...18S
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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