The Fornax Cluster VLT Spectroscopic Survey – I. VIMOS spectroscopy of compact stellar systems in the Fornax core region

Pota, Vincenzo; Napolitano, N. R.; Hilker, M.; Spavone, M.; Schulz, Christine; Cantiello, M.; Tortora, C.; Iodice, E.; Paolillo, M.; D’Abrusco, R.; Capaccioli, M.; Puzia, Thomas H.; Peletier, Reynier F.; Romanowsky, Aaron J.; Ven, Glenn van de; Spiniello, C.; Norris, Mark A.; Lisker, Thorsten; Muñoz, Roberto P.; Schipani, P.; Eigenthaler, Paul; Taylor, Matthew A.; Sánchéz-Janssen, R.; Órdenes-Briceño, Yasna

doi:10.1093/mnras/sty2149

Cited by 45 publications

(91 citation statements)

References 58 publications

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“…This is important because of the need to remove interloping point sources from our final GCC catalogue, which include foreground stars and unresolved background galaxies. However, we point out that both interloping populations are partially degenerate in colour space with the actual GCs (see also Pota et al 2018) and these sources must be accounted for using spatial information (see §3.6). This colour selection was accomplished by first crossmatching our point sources from the four FDS frames with a compilation of spectroscopically confirmed Fornax compact objects (Schuberth et al 2010;Wittmann et al 2016;Pota et al 2018).…”

Section: Colour Selectionmentioning

confidence: 99%

Halo mass estimates from the globular cluster populations of 175 low surface brightness galaxies in the Fornax cluster

Prole

Hilker

Burg

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The halo masses M halo of low surface brightness (LSB) galaxies are critical measurements for understanding their formation processes. One promising method to estimate a galaxy's M halo is to exploit the empirical scaling relation between M halo and the number of associated globular clusters (N GC ). We use a Bayesian mixture model approach to measure N GC for 175 LSB (23 ≤ µ e,r [mag arcsec −2 ] ≤ 28) galaxies in the Fornax cluster using the Fornax Deep Survey (FDS) data; this is the largest sample of low mass galaxies so-far analysed for this kind of study. The proximity of the Fornax cluster means that we can measure galaxies with much smaller physical sizes (0.3 ≤ r e,r [kpc] ≤ 9.5) compared to previous studies of the GC systems of LSB galaxies, probing stellar masses down to M * ∼ 10 5 M . The sample also includes 12 ultra-diffuse galaxies (UDGs), with projected r-band half-light radii greater than 1.5 kpc. Our results are consistent with an extrapolation of the M * − M halo relation predicted from abundance matching. In particular, our UDG measurements are consistent with dwarf sized halos, having typical masses between 10 10 and 10 11 M . Overall, our UDG sample is statistically indistinguishable from smaller LSB galaxies in the same magnitude range. We do not find any candidates likely to be as rich as some of those found in the Coma cluster. We suggest that environment might play a role in producing GC-rich LSB galaxies.

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Section: Colour Selectionmentioning

confidence: 99%

Halo mass estimates from the globular cluster populations of 175 low surface brightness galaxies in the Fornax cluster

Prole

Hilker

Burg

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…All of this suggests that there are interactions between Fornax cluster members (Iodice et al 2017b) and among galaxies with the overall cluster potential (Spiniello et al 2018;Pota et al 2018). This "stripe" along the west-north-west direction of NGC 1399, otherwise called as a west-north-west sub-clump, may have resulted from the accretion of a galaxy-group during the build-up of the cluster, hence creating what has been perceived to be an asymmetry (Iodice et al 2019a).…”

Section: Evolution Of Ltgs Inside the Virial Radius Of The Fornax Clumentioning

confidence: 99%

“…Fornax is dynamically more evolved than Virgo, as most of its bright (m B < 15 mag) cluster members (Ferguson 1989) are ETGs which are mainly located in its core (Grillmair et al 1994;Jordán et al 2007). However, the mass assembly of the Fornax cluster is still ongoing (Scharf et al 2005) and the intra-cluster light (ICL) in its core indicates interactions between cluster members (Iodice et al 2017a;Pota et al 2018;Spiniello et al 2018). Iodice et al (2017a) found that this ICL is the counterpart in the diffuse light of the overdensity in the blue intra-cluster globular clusters (D'Abrusco et al 2016;Cantiello et al 2018) and a fraction of the ICL population are low-mass dwarf galaxies (Venhola et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The Fornax Deep Survey with the VST

Raj

Iodice

Napolitano

et al. 2019

A&A

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Context. We present the study of a magnitude limited sample (mB ≤ 16.6 mag) of 13 late type galaxies (LTGs), observed inside the virial radius, Rvir ∼ 0.7 Mpc, of the Fornax cluster within the Fornax Deep Survey (FDS). Aims. The main objective is to use surface brightness profiles and g − i colour maps to obtain information on the internal structure of these galaxies and find signatures of the mechanisms that drive their evolution in high-density environments inside the virial radius of the cluster. Methods. By modelling galaxy isophotes, we extract the azimuthally averaged surface brightness profiles in four optical bands. We also derive g − i colour profiles, and relevant structural parameters like total magnitude and effective radius. For ten of the galaxies in this sample, we observe a clear discontinuity in their typical exponential surface brightness profiles, derive their “break radius”, and classify their disc-breaks into Type II (down-bending) or Type III (up-bending). Results. We find that Type II galaxies have bluer average (g − i) colour in their outer discs while Type III galaxies are redder. The break radius increases with stellar mass and molecular gas mass while it decreases with molecular gas-fractions. The inner and outer scale-lengths increase monotonically with absolute magnitude, as found in other works. For galaxies with CO(1-0) measurements, there is no detected cold gas beyond the break radius (within the uncertainties). In the context of morphological segregation of LTGs in clusters, we also find that, in Fornax, galaxies with morphological type 5 < T ≤ 9 (∼60% of the sample) are located beyond the high-density, ETG-dominated regions, however there is no correlation between T and the disc-break type. We do not find any correlation between the average (g − i) colours and cluster-centric distance, but the colour-magnitude relation holds true. Conclusions. The main results of this work suggest that the disc-breaks of LTGs inside the virial radius of the Fornax cluster seem to have arisen through a variety of mechanisms (e.g. ram-pressure stripping, tidal disruption), which is evident in their outer-disc colours and the absence of molecular gas beyond their break radius in some cases. This can result in a variety of stellar populations inside and outside the break radii.

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“…The high concentration of galaxies in the center of the Fornax cluster (Ferguson 1989) and the observed mass segregation of the galaxies (Drinkwater et al 2001) are both signs that the galaxies in the center have spent several Gyr in the cluster environment corresponding to a few crossing times 1 . This long standing interaction of galaxies with the cluster potential is possibly the main mechanism that has produced a significant intracluster population of stars, as the one recently traced by globular clusters (Pota et al 2018) and planetary nebulae (Spiniello et al 2018) in the core of the Fornax cluster. This population shows a velocity dispersion which is consistent with the one of the galaxy population in the same area, hence supporting the picture of a cluster core being dynamically evolved.…”

Section: Introductionmentioning

confidence: 99%

The Fornax Deep Survey with the VST

Venhola

Peletier

Laurikainen

et al. 2018

A&A

129

309

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Context. The Fornax Deep Survey (FDS), an imaging survey in the u , g , r , and i -bands, has a supreme resolution and image depth compared to the previous spatially complete Fornax Cluster Catalog (FCC). Our new data allows us to study the galaxies down to r -band magnitude m r ≈ 21 mag (M r ≈ −10.5 mag), which opens a new parameter regime to investigate the evolution of dwarf galaxies in the cluster environment. After the Virgo cluster, Fornax is the second nearest galaxy cluster to us, and with its different mass and evolutionary state, it provides a valuable comparison that makes it possible to understand the various evolutionary effects on galaxies and galaxy clusters. These data provide an important legacy dataset to study the Fornax cluster. Aims. We aim to present the Fornax Deep Survey (FDS) dwarf galaxy catalog, focusing on explaining the data reduction and calibrations, assessing the quality of the data, and describing the methods used for defining the cluster memberships and first order morphological classifications for the catalog objects. We also describe the main scientific questions that will be addressed based on the catalog. This catalog will also be invaluable for future follow-up studies of the Fornax cluster dwarf galaxies. Methods. As a first step we used the SExtractor fine-tuned for dwarf galaxy detection, to find galaxies from the FDS data, covering a 26 deg 2 area of the main cluster up to its virial radius, and the area around the Fornax A substructure. We made 2D-decompositions of the identified galaxies using GALFIT, measure the aperture colors, and the basic morphological parameters like concentration and residual flux fraction. We used color-magnitude, luminosity-radius and luminosity-concentration relations to separate the cluster galaxies from the background galaxies. We then divided the cluster galaxies into early-and late-type galaxies according to their morphology and gave first order morphological classifications using a combination of visual and parametric classifications. Results. Our final catalog includes 14 095 galaxies. We classify 590 galaxies as being likely Fornax cluster galaxies, of which 564 are dwarfs (M r > −18.5 mag) consisting our Fornax dwarf catalog. Of the cluster dwarfs we classify 470 as early-types, and 94 as late-type galaxies. Our final catalog reaches its 50% completeness limit at magnitude M r = −10.5 mag and surface brightness µ e,r = 26 mag arcsec −2 , which is approximately three magnitudes deeper than the FCC. Based on previous works and comparison with a spectroscopically confirmed subsample, we estimate that our final Fornax dwarf galaxy catalog has 10% contamination from the background objects.The catalogs are only at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/620/A165Article published by EDP Sciences A165, page 1 of 31 A&A 620, A165 (2018)

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The Fornax Cluster VLT Spectroscopic Survey – I. VIMOS spectroscopy of compact stellar systems in the Fornax core region

Cited by 45 publications

References 58 publications

Halo mass estimates from the globular cluster populations of 175 low surface brightness galaxies in the Fornax cluster

Halo mass estimates from the globular cluster populations of 175 low surface brightness galaxies in the Fornax cluster

The Fornax Deep Survey with the VST

The Fornax Deep Survey with the VST

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