Dorado and its member galaxies

Rampazzo, R.; Mazzei, P.; Marino, A.; Bianchi, Luciana; Postma, J.; Ragusa, Rossella; Spavone, M.; Iodice, E.; Ciroi, S.; Held, E. V.

doi:10.1051/0004-6361/202243726

A&A

2022

DOI: 10.1051/0004-6361/202243726

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Dorado and its member galaxies

R. Rampazzo

P. Mazzei

A. Marino

et al.

Abstract: Context. We are investigating the star formation in galaxies of the actively evolving Dorado group where, for a large fraction of both early-and late-type galaxies, signatures of interactions and merging events are revealed by optical and radio observations. Aims. Our previous Hα+[N II] study, probing ≈10 Myrs timescales, suggested that star formation is still ongoing in early-type galaxies. In this work, we use far-UV (FUV) imaging to map recent star formation on longer timescales, on the order of 100 Myrs . … Show more

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2024

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Cited by 3 publications

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MHONGOOSE discovery of a gas-rich low surface brightness galaxy in the Dorado group

Maccagni,

de Blok,

Mancera Piña

et al. 2024

A&A

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We present the discovery of a low-mass, gas-rich low surface brightness galaxy in the Dorado group, at a distance of 17.7 Mpc. Combining deep MeerKAT 21-cm observations from the MeerKAT Observations of Nearby Galactic Objects: Observing Southern Emitters (MHONGOOSE) survey with deep photometric images from the VST Early-type Galaxy Survey (VEGAS) we find a stellar and neutral atomic hydrogen ( gas mass of $M_ and respectively. This low surface brightness galaxy is the lowest-mass detection found in a group beyond the local Universe ($D 10$ Mpc). The dwarf galaxy has the typical overall properties of gas-rich low surface brightness galaxies in the Local group, but with some striking differences. Namely, the MHONGOOSE observations reveal a very low column density ($ disk with asymmetrical morphology possibly supported by rotation and higher velocity dispersion in the centre. There, deep optical photometry and UV observations suggest a recent enhancement of the star formation. Found at galactocentric distances where in the Local Group dwarf galaxies are depleted of cold gas (at a projected distance of $390$ kpc from the group centre), this galaxy is likely on its first orbit within the Dorado group. We discuss the possible environmental effects that may have caused the formation of the disk and the enhancement of star formation (SF), highlighting the short-lived phase (a few hundreds million years) of the gaseous disk, before either SF or hydrodynamical forces will deplete the gas of the galaxy.

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MHONGOOSE discovery of a gas-rich low surface brightness galaxy in the Dorado group

Maccagni,

de Blok,

Mancera Piña

et al. 2024

A&A

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The impact of stellar bars on star-formation quenching: Insights from a spatially resolved analysis in the local Universe

Scaloni,

Rodighiero,

Enia

et al. 2024

A&A

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Stellar bars are common morphological structures in the local Universe; according to optical and NIR surveys, they are present in about two-thirds of disc galaxies. These elongated structures are also believed to play a crucial role in secular evolutionary processes, because they are able to efficiently redistribute gas, stars, and angular momentum within their hosts, although it remains unclear as to whether they enhance or suppress star formation. A useful tool to investigate this ambiguity is the main sequence (MS) relation, which tightly links stellar mass ($M_ star $) and star formation rate (SFR). The main goal of this work is to explore star-formation processes in barred galaxies in order to assess the relevance of bars in star-formation quenching and whether or not they affect the typical log-linear trend of the resolved MS. To this purpose, we carried out a spatially resolved analysis on subkiloparsec (subkpc) scales for a sample of six nearby barred galaxies. We collected multi-wavelength photometric data from far-ultraviolet (FUV) to far-infrared (FIR) from the DustPedia database and applied a panchromatic spectral energy distribution (SED) fitting procedure on square apertures of fixed angular size ( arcsec times arcsec ) using the magphys code. For each galaxy, we obtain the distributions of stellar mass and SFR surface density and relate them in the $ star SFR $ plane, deriving the spatially resolved MS relation. Although significant galaxy-to-galaxy variations are in place, we infer the presence of a common anti-correlation track in correspondence with the bar-hosting region, which shows systematically lower SFRs. This central quiescent signature can be interpreted as the result of a bar-driven depletion of gas reservoirs and a consequent halting of star formation. Our findings appear to support an inside-out quenching scenario.

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Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies

Tomičić,

Werle,

Vulcani

et al. 2024

ApJ

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Star formation rates (SFRs) in galaxies offer a view of various physical processes across them, and are measured using various tracers, such as Hα and ultraviolet (UV). Different physical mechanisms can affect Hα and UV emission, resulting in a discrepancy in the corresponding SFR estimates (ΔSFR). We investigate the effects of ram pressure on the SFR measurements and ΔSFR across five galaxies from the GASP survey caught in the late stages of gas stripping due to ram pressure. We probe spatially resolved ΔSFR at pixel scales of 0.5 kpc, and compare disks to tails and regions dominated by the dense gas to diffuse ionized gas (DIG) regions. The regions dominated by dense gas show similar SFR values for UV and Hα tracers, while the regions dominated by the DIG show up to 0.5 dex higher SFR(UV). There is a large galaxy-by-galaxy variation in ΔSFR, with no difference between the disks and the tails. We discuss the potential causes of variations in ΔSFR between the dense gas and DIG areas. We conclude that the dominant cause of discrepancy are recent variations in star formation histories, where star formation recently dropped in the DIG-dominated regions leading to changes in ΔSFR. The areal coverage of the tracers shows areas with Hα and no UV emission; these areas have LINER-like emission (excess in [O i λ6300]/Hα line ratio), indicating that they are ionized by processes other than star formation.

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Dorado and its member galaxies

Cited by 3 publications

References 86 publications

MHONGOOSE discovery of a gas-rich low surface brightness galaxy in the Dorado group

MHONGOOSE discovery of a gas-rich low surface brightness galaxy in the Dorado group

The impact of stellar bars on star-formation quenching: Insights from a spatially resolved analysis in the local Universe

Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies

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