3D Modeling of the Molecular Gas Kinematics in Optically Selected Jellyfish Galaxies

Mingozzi, Matilde; Poggianti, Bianca M.; Moretti, Alessia; Gullieuszik, Marco; Marasco, Antonino; Sodi, Bernardo Cervantes; Sánchez-García, Osbaldo; Vulcani, Benedetta; Werle, Ariel; Paladino, R.; Radovich, M.

doi:10.3847/1538-4357/acc9b9

Cited by 9 publications

(1 citation statement)

References 179 publications

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“…This result is consistent with the results by Zabel et al (2022), who concluded that H I deficiency does not necessarily mean H 2 deficiency and that the molecular gas content is affected by ram pressure on different timescales than the atomic gas. This suggests that the stripping is less severe on H 2 than on H I, which is likely because the former is denser and more gravitationally bound to the galaxy than the latter (Lee et al 2017;Boselli et al 2022;Bacchini et al 2023).…”

Section: Cold Gas Balancementioning

confidence: 99%

The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies

Moretti,

Serra,

Bacchini

et al. 2023

ApJ

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Cluster galaxies are affected by the surrounding environment, which influences, in particular, their gas, stellar content, and morphology. In particular, the ram pressure exerted by the intracluster medium promotes the formation of multiphase tails of stripped gas detectable both at optical wavelengths and in the submillimeter and radio regimes, tracing the cold molecular and atomic gas components, respectively. In this work we analyze a sample of 16 galaxies belonging to clusters at redshift ∼0.05 showing evidence of an asymmetric H i morphology (based on MeerKAT observations) with and without a star-forming tail. To this sample we add three galaxies with evidence of a star-forming tail and no H i detection. Here we present the galaxies’ H2 gas content from APEX observations of the CO (2–1) emission. We find that in most galaxies with a star-forming tail the H2 global content is enhanced with respect to undisturbed field galaxies with similar stellar masses, suggesting an evolutionary path driven by the ram pressure stripping. As galaxies enter into the clusters, their H i is displaced but also partially converted into H2, so that they are H2 enriched when they pass close to the pericenter, that is, when they also develop the star-forming tails that are well visible in UV or B broad bands and in Hα emission. An inspection of the phase-space diagram for our sample suggests an anticorrelation between the H i and H2 gas phases as galaxies fall into the cluster potential. This peculiar behavior is a key signature of the ram pressure stripping in action.

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Section: Cold Gas Balancementioning

confidence: 99%

The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies

Moretti,

Serra,

Bacchini

et al. 2023

ApJ

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The ALMA-ALPAKA survey

Rizzo,

Roman-Oliveira,

Fraternali

et al. 2023

A&A

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Context. Spatially resolved studies of the kinematics of galaxies provide crucial insights into their assembly and evolution, enabling one to infer the properties of the dark matter halos, derive the impact of feedback on the interstellar medium (ISM), as well as measure and characterize the outflow motions. To date, most of the kinematic studies at z = 0.5 − 3.5 have been obtained using emission lines tracing the warm, ionized gas (e.g., Hα, [OII], and [OIII]). However, whether these provide an exhaustive or only a partial view of the dynamics of galaxies and of the properties of the ISM is still debated. Complementary insights into the cold gas kinematics are therefore needed. Aims. We present the Archival Large Program to Advance Kinematic Analysis (ALPAKA), a project aimed at gathering high-resolution observations of CO and [CI] emission lines of star-forming galaxies at z = 0.5 − 3.5 from the Atacama Large Millimeter Array (ALMA) public archive. With ≈147 h of total integration time, ALPAKA assembles ∼0.25″ observations for 28 star-forming galaxies, which is the largest sample with spatially resolved cold gas kinematics as traced by either CO or [CI] at z ≳ 0.5, spanning 7 Gyr of cosmic history. A large fraction of ALPAKA galaxies (19 out of 28) lie in overdense regions (clusters, groups, and protoclusters). Methods. By combining multiwavelength ground- and space-based ancillary data, we derived the stellar masses (M⋆) and star-formation rates (SFRs) for the ALPAKA targets. We exploited the ALMA data to infer the dynamical state of the ALPAKA galaxies and derive their rotation curves and velocity dispersion profiles using 3DBAROLO. Results. ALPAKA probes the massive (M⋆ ≳ 1010 M⊙), actively star-forming (SFR ≈ 10 − 3000 M⊙ yr−1) part of the population of galaxies at z ∼ 0.5 − 3.5. Based on our kinematic classification, we find that 19 out of 28 ALPAKA galaxies are rotating disks, two are interacting systems, while for the remaining seven sources the classification is uncertain. The disks have velocity dispersion values that are typically larger in the innermost regions than in the outskirts, with a median value for the entire disk sample of 35−9+11 km s−1. Despite the bias of our sample toward galaxies hosting very energetic mechanisms, the ALPAKA disks have high ratios of ordered-to-random motion (V/σ) with a median value of 9−2+7.

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The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope

Werle,

Giunchi,

Poggianti

et al. 2024

A&A

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In this work, we aim to characterize the stellar populations of star-forming regions detached from the stellar disks of galaxies undergoing ram pressure stripping. Using images collected with the WFC3 camera on board of the Hubble Space Telescope, we detected stellar clumps in continuum-subtracted $H and the ultraviolet (F275W filter); such clumps are often embedded in larger regions (star-forming complexes) detected in the optical (F606W filter). Our sample includes 347 $H clumps, 851 F275W clumps, and 296 star-forming complexes. We modeled the photometry of these objects in five bands using bagpipes to obtain their stellar population parameters. The median mass-weighted stellar ages are 27 Myr for $H clumps and 39 Myr for F275W clumps and star-forming complexes, but the oldest stars in the complexes can be older than sim 300 Myr which indicates that star formation is sustained for long periods of time. Stellar masses vary from $ to 10$^ $ $M_ with star-forming complexes being more massive objects in the sample. Clumps and complexes found further away from the host galaxy are on average younger, less massive, and less obscured by dust. We interpret these trends as due to the effect of ram pressure in different phases of the interstellar medium. $H clumps form a well-defined sequence in the stellar mass--SFR plane with a slope of 0.73. Some F275W clumps and star-forming complexes follow the same sequence while others stray away from it and passively age. The difference in mean stellar age between a complex and its youngest embedded clump scales with the distance between the clump and the center of the optical emission of the complex, with the most displaced clumps being hosted by the most elongated complexes. This is consistent with a fireball-like morphology, where star formation proceeds in a small portion of the complex while older stars are left behind producing a linear stellar population gradient. The stellar masses of star-forming complexes are consistent with the ones of globular clusters, but their stellar mass surface densities are lower by 2 dex, and their properties are more consistent with the population of dwarf galaxies in clusters.

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3D Modeling of the Molecular Gas Kinematics in Optically Selected Jellyfish Galaxies

Cited by 9 publications

References 179 publications

The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies

The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies

The ALMA-ALPAKA survey

The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope

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