Hostname: page-component-78c5997874-t5tsf Total loading time: 0 Render date: 2024-11-17T14:40:45.764Z Has data issue: false hasContentIssue false
  • English
  • Français

Using MUSE-AO observations to constrain the formation of the large nuclear star cluster in FCC 47

Published online by Cambridge University Press:  11 March 2020

Katja Fahrion Open the ORCID record for Katja Fahrion [Opens in a new window] ,
Mariya Lyubenova ,
Glenn van de Ven Open the ORCID record for Glenn van de Ven [Opens in a new window]  and
Michael Hilker Open the ORCID record for Michael Hilker [Opens in a new window]
Katja Fahrion
Affiliation:
European Southern Observatory, Karl-Scharzschild-Straße 2, 85748 Garching bei München, Germany email: kfahrion@eso.org
Mariya Lyubenova
Affiliation:
European Southern Observatory, Karl-Scharzschild-Straße 2, 85748 Garching bei München, Germany email: kfahrion@eso.org
Glenn van de Ven
Affiliation:
Department of Astrophysics, University of Vienna, Türkenschanzenstrasse 17, 1180 Wien, Austria
Michael Hilker
Affiliation:
European Southern Observatory, Karl-Scharzschild-Straße 2, 85748 Garching bei München, Germany email: kfahrion@eso.org
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Nuclear star clusters (NSCs) are found in at least 70% of all galaxies, but their formation path is still unclear. In the most common scenarios, NSCs form in-situ from the galaxy’s central gas reservoir, through merging of globular clusters (GCs), or through a combination of the two. As the scenarios pose different expectations for angular momentum and stellar population properties of the NSC in comparison to the host galaxy and the GC system, it is necessary to characterise the stellar light, NSC, and GCs simultaneously. Wide-field observations with modern integral field units such as the Multi Unit Spectroscopic Explorer (MUSE) allow to perform such studies. However, at large distances, NSCs usually are not resolved in MUSE observations. The particularly large NSC (Reff ∼ 66 pc) of the early-type galaxy FCC 47 at distance of ∼20 Mpc is an exception and is therefore an ideal laboratory to constrain NSC formation of external galaxies.

Keywords

galaxies: individual (NGC 1336)galaxies: star clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 108 - 111
Copyright
© International Astronomical Union 2020

References

Antonini, F. 2014, The Astrophysical Journal, 794, 106CrossRefGoogle Scholar
Antonini, F., Barausse, E., & Silk, J. 2015, ApJ, 812, 72CrossRefGoogle Scholar
Arca-Sedda, M. & Capuzzo-Dolcetta, R. 2014, ApJ, 785, 51CrossRefGoogle Scholar
Bekki, K., Couch, W. J., & Shioya, Y. 2006, ApJ, 642, L133CrossRefGoogle Scholar
Blakeslee, J. P., Jordán, A., Mei, S., et al. 2009, ApJ, 694, 556CrossRefGoogle Scholar
Böker, T., Laine, S., van der Marel, R. P., et al. 2002, AJ, 123, 1389CrossRefGoogle Scholar
Cappellari, M. 2017, MNRAS, 466, 798CrossRefGoogle Scholar
Cappellari, M. & Emsellem, E. 2004, PASP, 116, 138CrossRefGoogle Scholar
Fahrion, K., Georgiev, I., Hilker, M., et al. 2019, A&A, 625, A50Google Scholar
Fahrion, K., Lyubenova, M., van de Ven, G., et al. 2019, A&A, 628, 92Google Scholar
Feldmeier, A., Neumayer, N., Seth, A., et al. 2014, A&A, 570, A2Google Scholar
Georgiev, I. Y., Böker, T., Leigh, N., Lützgendorf, N., & Neumayer, N. 2016, MNRAS, 457, 2122CrossRefGoogle Scholar
Guillard, N., Emsellem, E., & Renaud, F. 2016, MNRAS, 461, 3620CrossRefGoogle Scholar
Hartmann, M., Debattista, V. P., Seth, A., Cappellari, M., & Quinn, T. R. 2011, MNRAS, 418, 2697CrossRefGoogle Scholar
Jordán, A., Peng, E. W., Blakeslee, J. P., et al. 2015, ApJS, 221, 13CrossRefGoogle Scholar
Liu, Y., Peng, E. W., Jordán, A., et al. 2019, ApJ, 875, 156CrossRefGoogle Scholar
Lyubenova, M. & Tsatsi, A. 2019, arXiv e-prints, arXiv:1903.10918Google Scholar
Neumayer, N., Walcher, C. J., Andersen, D., et al. 2011, MNRAS, 413, 1875CrossRefGoogle Scholar
Ordenes-Briceño, Y., Puzia, T. H., Eigenthaler, P., et al. 2018, ApJ, 860, 4CrossRefGoogle Scholar
Pinna, F., Falcón-Barroso, J., Martig, M., et al. 2019, A&A, 623, A19Google Scholar
Poci, A., McDermid, R. M., Zhu, L., et al. 2019, MNRAS, 487, 3776CrossRefGoogle Scholar
Rantala, A., Johansson, P. H., Naab, T., Thomas, J., & Frigo, M. 2019, ApJ, 872, L17CrossRefGoogle Scholar
Tremaine, S. D., Ostriker, J. P., & Spitzer, Jr., L. 1975, ApJ, 196, 407CrossRefGoogle Scholar
Tsatsi, A., Macciò, A. V., van de Ven, G., & Moster, B. P. 2015, ApJ, 802, L3CrossRefGoogle Scholar
Tsatsi, A., Mastrobuono-Battisti, A., van de Ven, G., et al. 2017, MNRAS, 464, 3720CrossRefGoogle Scholar
Vazdekis, A., Sánchez-Blázquez, P., Falcón-Barroso, J., et al. 2010, MNRAS, 404, 1639Google Scholar