Compact stellar systems in the polar ring galaxies NGC 4650A and NGC 3808B: Clues to polar disk formation

Órdenes-Briceño, Yasna; Georgiev, Iskren Y.; Puzia, Thomas H.; Goudfrooij, Paul; Arnaboldi, M.

doi:10.1051/0004-6361/201527025

Cited by 6 publications

(6 citation statements)

References 68 publications

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“…This mechanism is the most plausible explanation for SPRC-74 and 238. These galaxies show very faint bridges of the material falling from the donor onto the PRG, similar to what is observed in the pair NGC 3808 (Ordenes-Briceñao et al 2016). This mechanism finds good observational support in the literature (see e.g.…”

Section: Discussionsupporting

confidence: 83%

“…In addition, several interacting systems are observed in which matter is directly transferred from one member to another with the formation of a large-scale PS (e.g. NGC 3808A/B, NGC 6285/86 - Reshetnikov et al 1996, Ordenes-Briceñao et al 2016.…”

Section: Introductionmentioning

confidence: 99%

“…An example of applying this scenario to a giant spiral galaxy AM 1934-563 is presented in Reshetnikov et al (2006). In addition, several interacting systems are observed in which matter is directly transferred from one member to another with the formation of a large-scale PS (e.g., NGC 3808A/B, NGC 6285/86 - Reshetnikov et al 1996;Ordenes-Briceñao et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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Unveiling the Nature of Polar-ring Galaxies from Deep Imaging

Mosenkov¹,

Решетников²,

Skryabina³

et al. 2022

Res. Astron. Astrophys.

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General structural properties and low surface brightness tidal features hold important clues to the formation of galaxies. In this paper, we study a sample of polar-ring galaxies (PRGs) based on optical imaging from the Sloan Digital Sky Survey (SDSS) Stripe 82 and other deep surveys. We investigate the deepest images of candidates for PRGs to date. We carry out photometric decomposition on the host galaxies and associated polar structures that allows us to derive the structural properties of both components. We are able to detect very faint tidal structures around most PRGs in our sample. For several galaxies, we can directly observe the formation of the polar ring due to merging, which is manifested in debris of the victim galaxy and an arc-like polar structure made up of its material. In a few cases, we can discern signs of tidal accretion. The results obtained indicate that the gravitational interaction and merging of galaxies are the most plausible mechanisms for the formation of polar-ring galaxies.

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Section: Discussionsupporting

confidence: 83%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Unveiling the Nature of Polar-ring Galaxies from Deep Imaging

Mosenkov¹,

Решетников²,

Skryabina³

et al. 2022

Res. Astron. Astrophys.

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“…Such objects may include so-called polar-ring galaxies a rather rare class of objects whose subsystems (disk and ring) rotate in almost orthogonal planes. In some close galaxies of this type it is possible to trace differences between star-forming regions and stellar clusters in the ring and in the disk [2,15]. Although the reasons for the formation of polar subsystems may be different, and there are ongoing disputes about the nature of polar rings in specific galaxies [21,26], in any case, we are talking about the fact that a galaxy captures external matter with a moment of rotation, which is very different from that of the disk.…”

Section: Introductionmentioning

confidence: 99%

Study of Star-Forming Regions in the Peculiar Galaxies NGC 660, NGC 1512, NGC 4395, and NGC 4618

Smirnova,

Wiebe,

Moiseev

et al. 2020

Preprint

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The star-forming regions (SFRs) in the peculiar galaxies NGC 660, NGC 1512, NGC 4395 and NGC 4618 are studied. The relationships between such characteristics of star forming regions as UV, nearand far-IR fluxes, as well as in the Hα and HI lines, surface brightness in these ranges, and the scatter of the radial velocities of ionized and neutral hydrogen are considered. It is shown that in all the galaxies considered, the IR fluxes from SFRs are less than in the "normal" galaxies, but for different reasons: in the galaxies with signs of recent interaction NGC 660 and NGC 1512, this is due to the low surface brightness of SFRs; in the lopsided galaxies NGC 4395 and NGC 4618, the low brightness of SFRs in the infrared range is due to their compact size. These differences indicate that the star formation process depends not only on the morphological type of a galaxy, but also on many other factors.

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“…shells, rings, tails, and to the onset of star formation inside and outside galaxies (e.g. Toomre 1977; Mendes de Oliveira et al 2004;Schiminovich, van Gorkom, & van der Hulst 2013;Ueda et al 2014;Ordenes-Briceño et al 2016) depending on the nature and evolutionary stage of the on-going tidal interaction. In particular, after a close encounter of two gas-rich systems of similar mass, the gas may be stripped from the interacting galaxies forming long filaments or tidal tails driven by gravity torques (e.g.…”

Section: Introductionmentioning

confidence: 99%

Star formation in low density HI gas around the elliptical galaxy NGC 2865

Urrutia-Viscarra

Torres-Flores

Oliveira

et al. 2017

A&A

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Context. Interacting galaxies surrounded by Hi tidal debris are ideal sites for the study of young clusters and tidal galaxy formation. The process that triggers star formation in the low-density environments outside galaxies is still an open question. New clusters and galaxies of tidal origin are expected to have high metallicities for their luminosities. Spectroscopy of such objects is, however, at the limit of what can be done with existing 8-10m class telescopes, which has prevented statistical studies of these objects. Aims. NGC 2865 is an UV-bright merging elliptical galaxy with shells and extended Hi tails. The regions observed in this work were previously detected using multi-slit imaging spectroscopy. Methods. We obtain new multi-slit spectroscopy of six young star-forming regions around NGC 2865, to determine their redshifts and metallicities. Results. The six emission-line regions are located 16-40 kpc from NGC 2865 and they have similar redshifts. They have ages of ∼ 10 Myears and an average metallicity of ∼ 12+log(O/H)∼8.6, suggesting a tidal origin for the regions. It is noted that they coincide with an extended Hi tail, which has projected density of N HI < 10 19 cm −2 , and displays a low surface brightness counterpart. These regions may represent the youngest of the three populations of star clusters already identified in NGC 2865. Conclusions. The high, nearly-solar, oxygen abundances found for the six regions in the vicinity of NGC 2865 suggest that they were formed by pre-enriched material from the parent galaxy, from gas removed during the last major merger. Given the mass and the location of the Hii regions, we can speculate that these young star-forming regions are potential precursors of globular clusters that will be part of the halo of NGC 2865 in the future. Our result supports the use of the multi-slit imaging spectroscopy as a useful tool for finding nearly-formed stellar systems around galaxies.

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Compact stellar systems in the polar ring galaxies NGC 4650A and NGC 3808B: Clues to polar disk formation

Cited by 6 publications

References 68 publications

Unveiling the Nature of Polar-ring Galaxies from Deep Imaging

Unveiling the Nature of Polar-ring Galaxies from Deep Imaging

Study of Star-Forming Regions in the Peculiar Galaxies NGC 660, NGC 1512, NGC 4395, and NGC 4618

Star formation in low density HI gas around the elliptical galaxy NGC 2865

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