New observations and a photographic atlas of polar-ring galaxies

Whitmore, Bradley C.; Lucas, Ray A.; McElroy, D. B.; Steiman-Cameron, T. Y.; Sackett, Penny D.; Olling, Rob P.

doi:10.1086/115614

Cited by 279 publications

(365 citation statements)

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“…PRGs were first classified by Whitmore et al (1990). From these observations, and more recent ones (van Driel et al 2000;Iodice et al 2002a,b;Arnaboldi et al 1993;van Driel et al 1995), we can summarize the main properties of PRGs that a formation scenario has to account for (Iodice 2001): -host galaxies are often SO or early-type galaxies: they morphologically look like SOs, but their photometry is typical of early-type spirals, as revealed by Iodice et al (2002b,c).…”

Section: Introductionmentioning

confidence: 68%

“…From their atlas of PRGs, Whitmore et al (1990) estimate that 4.5% of the possible host galaxies have acquired a polar ring, and say that this estimate is uncertain by about a factor 3. According to the merging scenario, polar rings are stable features, so that no polar rings would have disappeared.…”

Section: Abundance Of Polar Rings and Comparison Of Scenariosmentioning

confidence: 99%

“…A polar ring galaxy (PRG) is made up of an early-type, lenticular, or elliptical host galaxy, surrounded by a ring of gas and stars orbiting in a plane that is nearly polar (Whitmore et al 1990). The presence of two dynamical planes is thought to give an insight into the shape of dark halos in such systems, which explains why PRGs are interesting peculiar systems.…”

Section: Introductionmentioning

confidence: 99%

“…Some are ellipticals, as in AM 2020-504, or late-type gas rich spirals, as in NGC 660; -about 0.5% of the possible host galaxies in the local Universe (SO and early-type) are observed to have a polar ring or a robust polar ring candidate. Yet, only a specific line-of-sight makes it possible to detect the ring, so that Whitmore et al (1990) estimate the actual percentage to about 4.5%. It could be even greater if one also accounted for polar rings that may have been destroyed by more recent galaxy interactions.…”

Section: Introductionmentioning

confidence: 99%

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Formation of polar ring galaxies

Bournaud

Combes

2003

A&A

159

196

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Abstract. Polar ring galaxies are peculiar systems in which a gas-rich, nearly polar ring surrounds an early-type or elliptical host galaxy. Two formation scenarios for these objects have been proposed: they are thought to form either in major galaxy mergers or by tidal accretion of the polar material from a gas rich donor galaxy. Both scenarios are studied through N-body simulations including gas dynamics and star formation. Constraints on physical parameters are drawn out, in order to determine which scenario is the most likely to occur. Polar ring galaxies from each scenario are compared with observations and we discuss whether the accretion scenario and the merging scenario account for observational properties of polar ring galaxies. The conclusion of this study is that the accretion scenario is both the most likely and the most supported by observations. Even if the merging scenario is rather robust, most polar ring galaxies are shown to be the result of tidal gas accretion events.

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Section: Introductionmentioning

confidence: 68%

Section: Abundance Of Polar Rings and Comparison Of Scenariosmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Formation of polar ring galaxies

Bournaud

Combes

2003

A&A

159

196

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“…When the distortions are significant but the underlying axisymmetric structure remains identifiable, the best explanation is often the recent accretion of a gas-rich object or a gas stream onto a pre-exiting galaxy. For example, polar-ring galaxies are composed of a central component (usually an early-type disk galaxy) surrounded by an outer ring or disk made of gas, dust and stars, which orbits nearly perpendicular to the plane of the central galaxy (Whitmore et al 1990; see also Fig. 8).…”

Section: Kinematical Distortionsmentioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

183

130

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Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

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The Classification of Galaxies

Buta

2021

Galaxies

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New observations and a photographic atlas of polar-ring galaxies

Cited by 279 publications

References 0 publications

Formation of polar ring galaxies

Formation of polar ring galaxies

Star formation sustained by gas accretion

The Classification of Galaxies

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