Fornax3D project: Assembly history of massive early-type galaxies in the Fornax cluster from deep imaging and integral field spectroscopy

Spavone, M.; Iodice, E.; D’Ago, G.; Ven, Glenn van de; Morelli, L.; Corsini, E. M.; Sarzi, Marc; Coccato, L.; Fahrion, Katja; Falcón-Barroso, J.; Gadotti, Dimitri A.; Lyubenova, M.; Martín-Navarro, Ignacio; McDermid, Richard M.; Pinna, Francesca; Pizzella, A.; Poci, Adriano; Zeeuw, P. T. de; Zhu, Ling

doi:10.1051/0004-6361/202243290

Cited by 6 publications

(4 citation statements)

References 77 publications

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“…Furthermore, the spatial distribution of luminous earlytype galaxies is highly asymmetrical: most of them are found in an elongated structure (just west of NGC 1399), which has not yet dispersed within the cluster. This is also the region hosting most of the intra-cluster light and most of the galaxies with low-surface-brightness features, asymmetric stellar halos, high fractions of accreted stellar mass and small metallicity gradients -all results which imply recent / on-going interactions (Iodice et al 2016(Iodice et al , 2017a(Iodice et al , 2019Spavone et al 2020Spavone et al , 2022. Finally, Fornax hosts a diverse population of recent infallers: first, bright gas-rich late-type galaxies with moderate H i-, H 2and star formation rate deficiency (Zabel et al 2019;Loni et al 2021;Morokuma-Matsui et al 2022), which show evidence of environment-induced distortions in both the stellar body (Raj et al 2019) and the ISM distribution (Lee-Waddell et al 2018;Zabel et al 2019); and second, star forming dwarf galaxies at the outskirts of the cluster covering a range of optical morphologies (Drinkwater et al 2001b).…”

Section: Meerkat Fornax Survey Background and Goalsmentioning

confidence: 94%

The MeerKAT Fornax Survey

Serra¹,

Maccagni²,

Kleiner³

et al. 2023

A&A

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The MeerKAT Fornax Survey maps the distribution and kinematics of atomic neutral hydrogen gas (H i) in the nearby Fornax galaxy cluster using the MeerKAT telescope. The 12 deg 2 survey footprint covers the central region of the cluster out to ∼ R vir and stretches out to ∼ 2R vir towards south west to include the NGC 1316 galaxy group. The H i column density sensitivity (3σ over 25 km s −1 ) ranges from 5 × 10 19 cm −2 at a resolution of ∼ 10 (∼ 1 kpc at the 20 Mpc distance of Fornax) down to ∼ 10 18 cm −2 at ∼ 1 (∼ 6 kpc), and slightly below this level at the lowest resolution of ∼ 100 (∼ 10 kpc). The H i mass sensitivity (3σ over 50 km s −1 ) is 6 × 10 5 M . The H i velocity resolution is 1.4 km s −1 . In this paper we describe the survey design and H i data processing, and we present a sample of six galaxies with long, one-sided, star-less H i tails (of which only one was previously known) radially oriented within the cluster and with measurable internal velocity gradients. We argue that the joint properties of the H i tails represent the first unambiguous evidence of ram pressure shaping the distribution of H i in the Fornax cluster. The disturbed optical morphology of all host galaxies supports the idea that the tails consist of H i initially pulled out of the galaxies' stellar body by tidal forces. Ram pressure was then able to further displace the weakly bound H i and give the tails their present direction, length and velocity gradient.

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Section: Meerkat Fornax Survey Background and Goalsmentioning

confidence: 94%

The MeerKAT Fornax Survey

Serra¹,

Maccagni²,

Kleiner³

et al. 2023

A&A

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“…The Fornax3D survey (Sarzi et al 2018) measured highquality age and metallicity maps covering at least the inner 2R e of 23 ETGs in the Fornax cluster. These galaxies show significant positive age gradients between R e and 2R e (Spavone et al 2022), while they have negative metallicity gradients, which are shallower than the control sample galaxies in the field. On the other hand, positive age gradients together with negative metallicity gradients are widely found in the dwarf galaxies of the Local Group (e.g., Koleva et al 2011;Kirby et al 2011;Zhuang et al 2021).…”

Section: Introductionmentioning

confidence: 71%

The Fornax3D project: Environmental effects on the assembly of dynamically cold disks in Fornax cluster galaxies

Ding

Zhu

Ven

et al. 2023

A&A

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We apply a population-orbit superposition metho1d to 16 galaxies in the Fornax cluster observed with MUSE/VLT in the context of the Fornax3D project. By fitting the luminosity distribution, stellar kinematics, and age and metallicity maps simultaneously, we obtained the internal stellar orbit distribution, as well as the age and metallicity distribution of stars on different orbits for each galaxy. Based on the model, we decompose each galaxy into a dynamically cold disk (orbital circularity λz ≥ 0.8) and a dynamically hot non-disk component (orbital circularity λz < 0.8), and obtain the surface-brightness, age, and metallicity radial profiles of each component. The galaxy infall time into the cluster is strongly correlated with galaxy cold-disk age with older cold disks in ancient infallers. We quantify the infall time tinfall of each galaxy with its cold-disk age using a correlation calibrated with TNG50 cosmological simulations. For galaxies in the Fornax cluster, we found that the luminosity fraction of cold disk in galaxies with tinfall > 8 Gyr are a factor of ∼4 lower than in more recent infallers while controlling for total stellar mass. Nine of the 16 galaxies have spatially extended cold disks, and most of them show positive or zero age gradients; stars in the inner disk are ∼2 − 5 Gyr younger than that in the outer disk, in contrast to the expectation of inside-out growth. Our results indicate that the assembly of cold disks in galaxies is strongly affected by their infall into clusters, by either removal of gas in outer regions or even tidally stripping or heating part of the pre-existing disks. Star formation in outer disks can stop quickly after the galaxy falls into the cluster, while star formation in the inner disks can last for a few Gyrs more, building the positive age gradient measured in cold disks.

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“…However, the cluster is still assembling, which is evident by the substructure in Fig. 8 and the un-settled giant early types, located in a region where many galaxies host asymmetric halos and low surface brightness features (Iodice et al 2016(Iodice et al , 2019Spavone et al 2020Spavone et al , 2022. Furthermore, there are different populations of recent infallers; massive late-types that are gas-rich and have disturbed stellar bodies, moderate atomic and molecular gas ratios and star formation rate deficiencies (Raj et al 2019;Zabel et al 2019;Loni et al 2021;Morokuma-Matsui et al 2022), and a range of star-forming dwarfs, located at the cluster outskirts (Drinkwater et al 2001).…”

Section: The Mechanisms and Timescale Of H I Removalmentioning

confidence: 99%

The MeerKAT Fornax Survey

Kleiner¹,

Serra²,

Maccagni³

et al. 2023

A&A

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We present MeerKAT Fornax Survey atomic hydrogen (H I) observations of the dwarf galaxies located in the central ∼2.5 × 4 deg2 of the Fornax galaxy cluster (Rvir ∼2°). The H I images presented in this work have a 3σ column density sensitivity between 2.7 and 50 × 1018 cm−2 over 25 km s−1 for spatial resolution between 4 and 1 kpc. We are able to detect an impressive MHI = 5 × 105 M⊙ 3σ point source with a line width of 50 km s−1 at a distance of 20 Mpc. We detected H I in 17 out of the 304 dwarfs in our field, with 14 out of the 36 late-type dwarfs (LTDs) and three out of the 268 early-type dwarfs (ETDs). The H I-detected LTDs have likely just joined the cluster and are on their first infall as they are located at large clustocentric radii, with comparable MHI and mean stellar surface brightness at fixed luminosity as blue, star-forming LTDs in the field. By contrast, the H I-detected ETDs have likely been in the cluster longer than the LTDs and acquired their H I through a recent merger or accretion from nearby H I. Eight of the H I-detected LTDs host irregular or asymmetric H I emission and disturbed or lopsided stellar emission. There are two clear cases of ram pressure shaping the H I, with the LTDs displaying compressed H I on the side closest to the cluster centre and a one-sided, starless tail pointing away from the cluster centre. The H I-detected dwarfs avoid the most massive potentials (i.e. cluster centre and massive galaxies), consistent with massive galaxies playing an active role in the removal of H I. We created a simple toy model to quantify the timescale of H I stripping in the cluster by reproducing the observed Mr′–MHI relation. We find that a MHI = 108 M⊙ dwarf is stripped in ∼240 Myr. The model is consistent with our observations, where low-mass LTDs are directly stripped of their H I from a single encounter and more massive LTDs can harbour a disturbed H I morphology due to longer times or multiple encounters being required to fully strip their H I. This is the first time dwarf galaxies with MHI ≲ 1 × 106 M⊙ have been detected and resolved beyond the local group and in a galaxy cluster.

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Fornax3D project: Assembly history of massive early-type galaxies in the Fornax cluster from deep imaging and integral field spectroscopy

Cited by 6 publications

References 77 publications

The MeerKAT Fornax Survey

The MeerKAT Fornax Survey

The Fornax3D project: Environmental effects on the assembly of dynamically cold disks in Fornax cluster galaxies

The MeerKAT Fornax Survey

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