The Fornax3D project: Tracing the assembly history of the cluster from the kinematic and line-strength maps

Iodice, E.; Sarzi, Marc; Bittner, A.; Coccato, L.; Costantin, Luca; Corsini, E. M.; Ven, Glenn van de; Zeeuw, P. T. de; Falcón-Barroso, J.; Gadotti, Dimitri A.; Lyubenova, M.; Martín-Navarro, Ignacio; McDermid, Richard M.; Nedelchev, B.; Pinna, Francesca; Pizzella, A.; Spavone, M.; Viaene, S.

doi:10.1051/0004-6361/201935721

Cited by 74 publications

(207 citation statements)

References 137 publications

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“…The data reduction of the F3D data is described in detail in Sarzi et al (2018) and Iodice et al (2019a), and was performed with the MUSE pipeline 2.2 (Weilbacher et al 2012(Weilbacher et al , 2016. It includes bias and flat-field correction, astrometric calibration, sky subtraction using dedicated sky observations, wavelength and flux calibration.…”

Section: Muse Datamentioning

confidence: 99%

“…Maps of the LOS velocities were presented in Iodice et al (2019a) and in this work, we further used metallicity maps that were derived from the same line-strength measurements for a comparison to the GCs. More detailed maps of the stellar population properties will be subject of future work.…”

Section: Muse Datamentioning

confidence: 99%

“…While background galaxies, bright foreground stars and line-emission objects such as HII regions can be easily found by visual inspection of the spectrum, the GC sample was finally cleaned after measuring the LOS velocity to confirm membership to the Fornax cluster (500 < v LOS < 2500 km s −1 ). This range was based on the observed radial velocities of the F3D galaxies (Iodice et al 2019a), but the final sample only contains GCs with 800 < v LOS < 2300 km s −1 . The sources shown by blue circles in the right panel of Fig.…”

Section: Detection Of Gcs In the Muse Datamentioning

confidence: 99%

“…The galaxies are ordered by their FCC number. Masses are from Iodice et al (2019a); Liu et al (2019). (1) Galaxy name from Ferguson (1989) and (2) alternative name.…”

Section: Sample Of Globular Clustersmentioning

confidence: 99%

“…GC metallicities relative to the central pixel of the host are shown as a function of GC projected galactocentric distance relative to the host's effective radius for comparison between galaxies. The symbols are colour coded by the host's stellar mass from Iodice et al (2019a) and Liu et al (2019). There is one additional GC of FCC 170 with R/R eff ∼ 5 that is not shown in this figure.…”

Section: Globular Cluster System Rotationmentioning

confidence: 99%

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

Fahrion

Lyubenova

Hilker

et al. 2020

A&A

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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 ( 3R eff ) 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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Section: Muse Datamentioning

confidence: 99%

Section: Muse Datamentioning

confidence: 99%

Section: Detection Of Gcs In the Muse Datamentioning

confidence: 99%

“…The galaxies are ordered by their FCC number. Masses are from Iodice et al (2019a); Liu et al (2019). (1) Galaxy name from Ferguson (1989) and (2) alternative name.…”

Section: Sample Of Globular Clustersmentioning

confidence: 99%

Section: Globular Cluster System Rotationmentioning

confidence: 99%

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

Fahrion

Lyubenova

Hilker

et al. 2020

A&A

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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 GIST pipeline: A multi-purpose tool for the analysis and visualisation of (integral-field) spectroscopic data

Bittner

Falcón-Barroso

Nedelchev

et al. 2019

A&A

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We present a convenient, all-in-one framework for the scientific analysis of fully reduced, (integral-field) spectroscopic data. The GIST pipeline (Galaxy IFU Spectroscopy Tool) is entirely written in Python 3 and conducts all steps from the preparation of input data, over the scientific analysis to the production of publication-quality plots. In its basic setup, it extracts stellar kinematics, performs an emission-line analysis and derives stellar population properties from full spectral fitting as well as via the measurement of absorption line-strength indices by exploiting the well-known pPXF and GandALF routines, where the latter has now been implemented in Python. The pipeline is not specific to any instrument or analysis technique and provides easy means of modification and further development, as of its modular code architecture. An elaborate, Python-native parallelisation is implemented and tested on various machines. The software further features a dedicated visualization routine with a sophisticated graphical user interface. This allows an easy, fullyinteractive plotting of all measurements, spectra, fits, and residuals, as well as star formation histories and the weight distribution of the models. The pipeline has successfully been applied to both low and high-redshift data from MUSE, PPAK (CALIFA), and SINFONI, as well as to simulated data for HARMONI@ELT and WEAVE and is currently being used by the TIMER, Fornax3D, and PHANGS collaborations. We demonstrate its capabilities by applying it to MUSE TIMER observations of NGC 1433.

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The Fornax3D project: Tracing the assembly history of the cluster from the kinematic and line-strength maps

Cited by 74 publications

References 137 publications

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

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

The Fornax Deep Survey with the VST

The GIST pipeline: A multi-purpose tool for the analysis and visualisation of (integral-field) spectroscopic data

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