Study of the Lynx-Cancer void galaxies. – V. The extremely isolated galaxy UGC 4722

Chengalur, Jayaram N.; Pustilnik, S. A.; Макаров, Д. И.; Perepelitsyna, Y. A.; Safonova, E. S.; Караченцев, И. Д.

doi:10.1093/mnras/stv086

Cited by 13 publications

(8 citation statements)

References 49 publications

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“…Id09002536: An isolated galaxy. Chengalur et al (2015) identified a disturbed HI morphology and argued that the galaxy has suffered recent minor merger. Id09562849: A merging dwarf candidate Annibali et al (2016) Id10080227: A merger origin compact early-type galaxy Id10545418: Interacting pair studied in Local Volume TiNy Titan (Pearson et al 2016) Id11451711: Interacting dwarf galaxies in the outskirt of a group environment (Paudel et al 2013).…”

Section: Appendixmentioning

confidence: 99%

A Catalog of Merging Dwarf Galaxies in the Local Universe

Paudel

Smith

Yoon

et al. 2018

ApJS

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We present the largest publicly available catalog of interacting dwarf galaxies. It includes 177 nearby merging dwarf galaxies of stellar mass M * < 10 10 M and redshifts z < 0.02. These galaxies are selected by visual inspection of publicly available archival imaging from two wide-field optical surveys (SDSS III and the Legacy Survey), and they possess low surface brightness features that are likely the result of an interaction between dwarf galaxies. We list UV and optical photometric data which we use to estimate stellar masses and star formation rates. So far, the study of interacting dwarf galaxies has largely been done on an individual basis, and lacks a sufficiently large catalog to give statistics on the properties of interacting dwarf galaxies, and their role in the evolution of low mass galaxies. We expect that this public catalog can be used as a reference sample to investigate the effects of the tidal interaction on the evolution of star-formation, morphology/structure of dwarf galaxies.Our sample is overwhelmingly dominated by star-forming galaxies, and they are generally found significantly below the red-sequence in the color-magnitude relation. The number of early-type galaxies is only 3 out of 177. We classify them, according to observed low surface brightness features, into various categories including shells, stellar streams, loops, antennae or simply interacting. We find that dwarf-dwarf interactions tend to prefer the low density environment. Only 41 out of the 177 candidate dwarf-dwarf interaction systems have giant neighbors within a sky projected distance of 700 kpc and a line of sight radial velocity range ±700 km/s and, compared to the LMC-SMC, they are generally located at much larger sky-projected distances from their nearest giant neighbor.

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Section: Appendixmentioning

confidence: 99%

A Catalog of Merging Dwarf Galaxies in the Local Universe

Paudel

Smith

Yoon

et al. 2018

ApJS

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“…Voids may contain groups of galaxies (like NGC 428 group, Egorova et al 2019), pairs and triplets (Chengalur & Pustilnik 2013;Pustilnik & Tepliakova 2011;Pustilnik et al 2019), interacting and merging systems (Chengalur et al 2017;Beygu et al 2013). In particular, Chengalur et al (2015) investigated another void galaxy UGC 4722 that was considered to be one of the most isolated galaxies in the Local Supercluster, though revealing the peculiar morphology. Authors conclude that actually it is a merging system, and the second component, a very gas-rich dwarf, was almost completely destroyed.…”

Section: Discussion and Summarymentioning

confidence: 99%

Search for gas accretion imprints in voids: II. The galaxy Ark 18 as a result of a dwarf-dwarf merger

Egorova,

Egorov,

Moiseev

et al. 2021

Preprint

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The low-mass low-surface brightness (LSB) disc galaxy Arakelian 18 (Ark 18) resides in the Eridanus void and because of its isolation represents an ideal case to study the formation and evolution mechanisms of such a galaxy type. Its complex structure consists of an extended blue LSB disc and a bright central elliptically-shaped part hosting a massive off-centered star-forming clump. We present the in-depth study of Ark 18 based on observations with the SCORPIO-2 long-slit spectrograph and a scanning Fabry-Perot interferometer at the Russian 6-m telescope complemented by archival multi-wavelength images and SDSS spectra. Ark 18 appears to be a dark matter dominated gas-rich galaxy without a radial metallicity gradient. The observed velocity field of the ionised gas is well described by two circularly rotating components moderately inclined with respect to each other and a possible warp in the outer disc. We estimated the age of young stellar population in the galaxy centre to be ∼140 Myr, while the brightest star-forming clump appears to be much younger. We conclude that the LSB disc is likely the result of a dwarf-dwarf merger with a stellar mass ratio of the components at least ∼5:1 that occurred earlier than 300 Myr ago. The brightest star forming clump was likely formed later by accretion of a gas cloud.

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“…Several studies have shown that a number of star-forming dwarf galaxies present filamentary H i and/or extended structures, which may indicate a recent cold gas infall/accretion (e.g. Chengalur et al 2015). In this sense, the extended structure of this galaxy could be a remnant of one of these processes.…”

Section: Tidal Interactions Mergers And/or Gas Infallmentioning

confidence: 94%

On the properties of the interstellar medium in extremely metal-poor blue compact dwarf galaxies. A VIMOS-IFU study of the cometary galaxy and Ly $α$ absorber Tol 65

Lagos,

Demarco,

Papaderos

et al. 2015

Preprint

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In this study we present high-resolution VIsible Multi-Object Spectrograph integral field unit spectroscopy (VIMOS-IFU) of the extremely metal-poor H ii/blue compact dwarf (BCD) galaxy Tol 65. The optical appearance of this galaxy shows clearly a cometary morphology with a bright main body and an extended and diffuse stellar tail. We focus on the detection of metallicity gradients or inhomogeneities as expected if the ongoing star-formation activity is sustained by the infall/accretion of metal-poor gas. No evidences of significant spatial variations of abundances were found within our uncertainties. However, our findings show a slight anticorrelation between gas metallicity and star-formation rate at spaxel scales, in the sense that high star-formation is found in regions of low-metallicity, but the scatter in this relation indicates that the metals are almost fully diluted. Our observations show the presence of extended Hα emission in the stellar tail of the galaxy. We estimated that the mass of the ionized gas in the tail M(H ii) tail ∼1.7×10 5 M ⊙ corresponds with ∼24 per cent of the total mass of the ionized gas in the galaxy. We found that the Hα velocity dispersion of the main body and the tail of the galaxy are comparable with the one found in the neutral gas by previous studies. This suggests that the ionized gas still retains the kinematic memory of its parental cloud and likely a common origin. Finally, we suggest that the infall/accretion of cold gas from the outskirts of the galaxy and/or minor merger/interaction may have produced the almost flat abundance gradient and the cometary morphology in Tol 65.

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Study of the Lynx-Cancer void galaxies. – V. The extremely isolated galaxy UGC 4722

Cited by 13 publications

References 49 publications

A Catalog of Merging Dwarf Galaxies in the Local Universe

A Catalog of Merging Dwarf Galaxies in the Local Universe

Search for gas accretion imprints in voids: II. The galaxy Ark 18 as a result of a dwarf-dwarf merger

On the properties of the interstellar medium in extremely metal-poor blue compact dwarf galaxies. A VIMOS-IFU study of the cometary galaxy and Ly $α$ absorber Tol 65

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