HST imaging of the globular clusters in the Fornax cluster: NGC 1379

AbstractThe Fornax Deep Survey (FDS) is a multi-band imaging survey of the Fornax cluster of galaxies, executed with the ESO VLT Survey Telescope (VST). The survey is designed to reach unprecedented surface brightness and point-source magnitude depth over one virial radius of the cluster. The scientific objectives of the survey are numerous: the study of the galaxy luminosity function, derivation of galaxy scaling relations, determination of the properties of compact stellar systems, an accurate determination of distances and 3-D geometry of the Fornax cluster, analysis of diffuse stellar light and galaxy interactions, etc.In this contribute we give an overview on the interest of the survey on globular clusters (GC) populations, and present a report the status of the study of GCs also providing some preliminary results of our analysis, with particular regard to the two-dimensional distribution of GC candidates over ∼20 sq. degree area of Fornax centered on NGC 1399.

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HST imaging of the globular clusters in the Fornax cluster: NGC 1399 and NGC 1404

Monthly Notices of the Royal Astronomical Society ◽

10.1046/j.1365-8711.1998.01202.x ◽

1998 ◽

Vol 293 (3) ◽

pp. 325-336 ◽

Cited By ~ 45

Author(s):

D. A. Forbes ◽

C. J. Grillmair ◽

G. M. Williger ◽

R. A. W. Elson ◽

J. P. Brodie

Keyword(s):

Globular Clusters ◽

Fornax Cluster

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An Update on the ACS Virgo and Fornax Cluster Surveys

Proceedings of the International Astronomical Union ◽

10.1017/s1743921308016013 ◽

2007 ◽

Vol 3 (S246) ◽

pp. 377-386 ◽

Cited By ~ 2

Author(s):

Patrick Côté ◽

Laura Ferrarese ◽

Andrés Jordán ◽

John P. Blakeslee ◽

Chin-Wei Chen ◽

...

Keyword(s):

Globular Clusters ◽

Milky Way ◽

Dwarf Galaxies ◽

Hubble Space Telescope ◽

Structural Parameters ◽

Star Clusters ◽

Early Type ◽

Space Telescope ◽

Fornax Cluster ◽

Selection Of

AbstractWe present a brief update on the ACS Virgo and Fornax Cluster Surveys —Hubble Space Telescopeprograms to obtainACSimaging for 143 early-type galaxies in the two galaxy clusters nearest to the Milky Way. We summarize a selection of science highlights from the surveys as including new results on the central structure of early-type galaxies, the apparent continuity of photometric and structural parameters between dwarf and giant galaxies, and the properties of globular clusters, diffuse star clusters and ultra-compact dwarf galaxies.

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Ultra compact objects in the Fornax cluster of galaxies: Globular clusters or dwarf galaxies?

Astronomy and Astrophysics ◽

10.1051/0004-6361:20011833 ◽

2002 ◽

Vol 383 (3) ◽

pp. 823-837 ◽

Cited By ~ 93

Author(s):

S. Mieske ◽

M. Hilker ◽

L. Infante

Keyword(s):

Globular Clusters ◽

Dwarf Galaxies ◽

Compact Objects ◽

Cluster Of Galaxies ◽

Fornax Cluster

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The Fornax Deep Survey with the VST

Astronomy and Astrophysics ◽

10.1051/0004-6361/201833741 ◽

2019 ◽

Vol 623 ◽

pp. A1 ◽

Cited By ~ 16

Author(s):

E. Iodice ◽

M. Spavone ◽

M. Capaccioli ◽

R. F. Peletier ◽

G. van de Ven ◽

...

Keyword(s):

Globular Clusters ◽

Surface Brightness ◽

Major Axis ◽

Position Angle ◽

Early Type ◽

Semi Major Axis ◽

Cluster Galaxies ◽

The Galaxy ◽

Deep Survey ◽

Fornax Cluster

Context. This paper is based on the multi-band (ugri) Fornax Deep Survey (FDS) with the VLT Survey Telescope (VST). We study bright early-type galaxies (mB ≤ 15 mag) in the 9 square degrees around the core of the Fornax cluster, which covers the virial radius (Rvir ∼ 0.7 Mpc). Aims. The main goal of the present work is to provide an analysis of the light distribution for all galaxies out to unprecedented limits (in radius and surface brightness) and to release the main products resulting from this analysis in all FDS bands. We give an initial comprehensive view of the galaxy structure and evolution as a function of the cluster environment. Methods. From the isophote fit, we derived the azimuthally averaged surface brightness profiles, the position angle, and ellipticity profiles as a function of the semi-major axis. In each band, we derived the total magnitudes, effective radii, integrated colours, and stellar mass-to-light ratios. Results. The long integration times, the arcsec-level angular resolution of OmegaCam at VST, and the large covered area of FDS allow us to map the light and colour distributions out to large galactocentric distances (up to about 10−15 Re) and surface brightness levels beyond μr = 27 mag arcsec−2 (μB ≥ 28 mag arcsec−2). Therefore, the new FDS data allow us to explore in great detail the morphology and structure of cluster galaxies out to the region of the stellar halo. The analysis presented in this paper allows us to study how the structure of galaxies and the stellar population content vary with the distance from the cluster centre. In addition to the intra-cluster features detected in previous FDS works, we found a new faint filament between FCC 143 and FCC 147, suggesting an ongoing interaction. Conclusions. The observations suggest that the Fornax cluster is not completely relaxed inside the virial radius. The bulk of the gravitational interactions between galaxies happens in the W-NW core region of the cluster, where most of the bright early-type galaxies are located and where the intra-cluster baryons (diffuse light and globular clusters) are found. We suggest that the W-NW sub-clump of galaxies results from an infalling group onto the cluster, which has modified the structure of the galaxy outskirts (making asymmetric stellar halos) and has produced the intra-cluster baryons (ICL and GCs), concentrated in this region of the cluster.

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The Fornax 3D project: Globular clusters tracing kinematics and metallicities

Astronomy and Astrophysics ◽

10.1051/0004-6361/202037685 ◽

2020 ◽

Vol 637 ◽

pp. A26 ◽

Cited By ~ 8

Author(s):

K. Fahrion ◽

M. Lyubenova ◽

M. Hilker ◽

G. van de Ven ◽

J. Falcón-Barroso ◽

...

Keyword(s):

Galaxy Evolution ◽

Globular Clusters ◽

Spectroscopic Studies ◽

Host Galaxy ◽

Massive Galaxies ◽

The Galaxy ◽

Stellar Body ◽

Galaxy Assembly ◽

Fossil Records ◽

Fornax Cluster

Globular clusters (GCs) are found ubiquitously in massive galaxies and due to their old ages, they are regarded as fossil records of galaxy evolution. Spectroscopic studies of GC systems are often limited to the outskirts of galaxies, where GCs stand out against the galaxy background and serve as bright tracers of galaxy assembly. In this work, we use the capabilities of the Multi Unit Explorer Spectrograph (MUSE) to extract a spectroscopic sample of 722 GCs in the inner regions (≲3 Reff) of 32 galaxies in the Fornax cluster. These galaxies were observed as part of the Fornax 3D project, a MUSE survey that targets early and late-type galaxies within the virial radius of Fornax. After accounting for the galaxy background in the GC spectra, we extracted line-of-sight velocities and determined metallicities of a sub-sample of 238 GCs. We found signatures of rotation within GC systems, and comparing the GC kinematics and that of the stellar body shows that the GCs trace the spheroid of the galaxies. While the red GCs prove to closely follow the metallicity profile of the host galaxy, the blue GCs show a large spread of metallicities but they are generally more metal-poor than the host.

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Resolving Globular Clusters in the Fornax Cluster and Beyond

Symposium - International Astronomical Union ◽

10.1017/s0074180900223978 ◽

2002 ◽

Vol 207 ◽

pp. 327-329

Author(s):

Carl J. Grillmair ◽

Jon Holtzman ◽

Rebecca Elson

Keyword(s):

Globular Clusters ◽

Structural Parameters ◽

Stellar Clusters ◽

Early Type ◽

Minimization Method ◽

Luminosity Functions ◽

Fornax Cluster ◽

Structure Spectrum

We describe an ongoing program to measure structural parameters for globular clusters with a range of ages in early-type galaxies. Using deep, optimally-dithered HST WFPC2 observations of NGC 3597, NGC 1316, and NGC 1399, we apply a χ2 minimization method to the determination of cluster sizes. The goals include studying the structure spectrum of stellar clusters at birth, and determining the rate at which tidal and evaporative destruction mechanisms operate to alter luminosity functions and specific frequencies to what we see in ellipticals today.

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