English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
Add to Basket
  Local TagsRelease HistoryDetailsSummary

Released
Conference Paper

Measuring Masses and Densities of Nuclear Star Clusters in the Nearest Galaxies

MPS-Authors

Pechetti,  Renuka
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Seth,  Anil
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Neumayer,  Nadine
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Georgiev,  Iskren
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kacharov,  Nikolay
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2019AAS...23324908P
(Any fulltext)

Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Pechetti, R., Seth, A., Neumayer, N., Georgiev, I., & Kacharov, N. (2019). Measuring Masses and Densities of Nuclear Star Clusters in the Nearest Galaxies. In American Astronomical Society Meeting Abstracts #233.


Cite as: https://hdl.handle.net/21.11116/0000-0005-D01E-F
Abstract
Galaxy nuclei contain both black holes (BHs) and nuclear star clusters (NSCs). Low-mass galaxies are typically dominated by NSCs. Measurements of NSC mass density suggest a scaling relation exists between them and their host galaxy mass, but very few NSC masses are dynamically estimated. We will present density profiles and dynamical masses for 29 nearby galaxies within 10 Mpc based on HST imaging and accompanying infrared spectroscopy from GNIRS and XSHOOTER. We quantify the NSC profiles by determining the effective radius and Sersic index. These profiles are then combined with their central velocity dispersions, derived using CO bandheads, to get dynamical mass density estimates for the NSCs and upper limits on any BHs. These measurements increase the number of dynamical measurements of NSCs by a factor of 3. The resulting scaling relations can be used to disentangle the formation scenarios of the NSCs. In addition, the measurement of central densities will help determine the expected rate of tidal disruption events by central BHs in galactic nuclei.