<i>GALEX</i>UV properties of the polar ring galaxy MCG-05-07-001 and the shell galaxies NGC 1210 and NGC 5329

Marino, A.; Iodice, E.; Tantalo, R.; Piovan, L.; Bettoni, D.; Buson, L. M.; Chiosi, C.; Galletta, G.; Rampazzo, R.; Rich, R. Michael

doi:10.1051/0004-6361/200911819

Cited by 25 publications

(21 citation statements)

References 81 publications

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“…the ring is not at 90 degrees to the galaxy), and the knotting of the ring is similar to the knotting instability seen in the no-polar-ring Cartwheel galaxy, the presence of a ring surrounding an SB0 recalls shell and polar ring early-type galaxies, commonly thought to have undergone accretion and/or merging phenomena (e.g. Marino et al 2009). …”

Section: Introductionmentioning

confidence: 72%

NGC 4262: a Virgo galaxy with an extended ultraviolet ring

Bettoni

Buson

Galletta³

2010

A&A

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Context. The Galaxy Ultraviolet Explorer (GALEX) satellite has recently shown the presence of an extended, outer ring studded with UV-bright knots surrounding the lenticular galaxy NGC 4262. Such a structure-not detected in the optical-is coupled with a ring of atomic (HI) gas. Aims. We want to show that both star-forming and HI rings surrounding this SB0 galaxy share the same radial distance from the galaxy center and spatial orientation. We also model the kinematics of the ring(s) and of the galaxy body. Methods. We make use of archive FUV and NUV GALEX data plus HI observations from the literature. Results. We confirm that the UV-bright and atomic gas rings of NGC 4262 have the same extent and projected spatial orientation. Their kinematics is not coupled with that of the galaxy stars. Conclusions. It is possible that NGC 4262 has undergone a major gas stripping event in the past that was the origin of the present "necklace" of UV-bright knots.

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Section: Introductionmentioning

confidence: 72%

NGC 4262: a Virgo galaxy with an extended ultraviolet ring

Bettoni

Buson

Galletta³

2010

A&A

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“…Several redder low surface brightness structures are seen outside the main body of the galaxy, reminiscent of the appearance of shell galaxies (e.g. Marino et al 2009;Bettoni et al 2011). From the central starforming parts Lyα is only seen in absorption, while a faint halo emerges at larger radii.…”

Section: A10 Lars 10 (Mrk 0061)mentioning

confidence: 96%

The Lyman alpha reference sample

Herenz

Gruyters

Orlitová

et al. 2016

A&A

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We present integral field spectroscopic observations with the Potsdam Multi-Aperture Spectrophotometer of all 14 galaxies in the z ∼ 0.1 Lyman Alpha Reference Sample (LARS). We produce 2D line-of-sight velocity maps and velocity dispersion maps from the Balmer α (Hα) emission in our data cubes. These maps trace the spectral and spatial properties of the LARS galaxies' intrinsic Lyα radiation field. We show our kinematic maps that are spatially registered onto the Hubble Space Telescope Hα and Lyman α (Lyα) images. We can conjecture a causal connection between spatially resolved Hα kinematics and Lyα photometry for individual galaxies, however, no general trend can be established for the whole sample. Furthermore, we compute the intrinsic velocity dispersion σ 0 , the shearing velocity v shear , and the v shear /σ 0 ratio from our kinematic maps. In general LARS galaxies are characterised by high intrinsic velocity dispersions (54 km s −1 median) and low shearing velocities (65 km s −1 median). The v shear /σ 0 values range from 0.5 to 3.2 with an average of 1.5. It is noteworthy that five galaxies of the sample are dispersion-dominated systems with v shear /σ 0 < 1, and are thus kinematically similar to turbulent star-forming galaxies seen at high redshift. When linking our kinematical statistics to the global LARS Lyα properties, we find that dispersion-dominated systems show higher Lyα equivalent widths and higher Lyα escape fractions than systems with v shear /σ 0 > 1. Our result indicates that turbulence in actively star-forming systems is causally connected to interstellar medium conditions that favour an escape of Lyα radiation.

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“…Furthermore, we notice some NUV knots in the northwest side of the galaxy along the edge of the shell. These NUV knots along the NW ripple of NGC 3934 offer a similarity with another shell galaxy, NGC 1210 (Marino et al 2009). In this latter galaxy several knots, visible both in the NUV and the FUV bands, follow a tail-like structure in coincidence with a HI tail/ring.…”

Section: Uv Morphology and Integrated Propertiesmentioning

confidence: 74%

“…This is confirmed also by the presence of some NUV knots along the NW ripple of NGC 3934 similar to those detected by GALEX in another shell galaxy, NGC 1210. These features are the debris of a recent accretion event that is responsible for the shell structure (Marino et al 2009). …”

Section: Discussionmentioning

confidence: 99%

NGC 3934: a shell galaxy in a compact galaxy environment

Bettoni

Galletta²,

Rampazzo³

et al. 2011

A&A

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Context. Mergers/accretions are considered the main drivers of the evolution of galaxies in groups. We investigate the NGC 3933 poor galaxy association that contains NGC 3934, which is classified as a polar-ring galaxy. Aims. The multi-band photometric analysis of NGC 3934 allows us to investigate the nature of this galaxy and to re-define the NGC 3933 group members with the aim to characterize the group's dynamical properties and its evolutionary phase. Methods. We imaged the group in the far (FUV, λ eff = 1539 Å) and near (NUV, λ eff = 2316 Å) ultraviolet (UV) bands of the Galaxy Evolution Explorer (GALEX). From the deep optical imaging we determined the fine structure of NGC 3934. We measured the recession velocity of PGC 213894 which shows that it belongs to the NGC 3933 group. We derived the spectral energy distribution (SED) from FUV to far-IR emission of the two brightest members of the group. We compared a grid of smooth particle hydrodynamical (SPH) chemo-photometric simulations with the SED and the integrated properties of NGC 3934 and NGC 3933 to devise their possible formation/evolutionary scenarios. Results. The NGC 3933 group has six bright members: a core composed of five galaxies, which have Hickson's compact group characteristics, and a more distant member, PGC 37112. The group velocity dispersion is relatively low (157 ± 44 km s −1 ). The projected mass, from the NUV photometry, is ∼7 × 10 12 M with a crossing time of 0.04 Hubble times, suggesting that at least in the center the group is virialized. We do not find evidence that NGC 3934 is a polar-ring galaxy, as suggested by the literature, but find that it is a disk galaxy with a prominent dust-lane structure and a wide type-II shell structure. Conclusions. NGC 3934 is a quite rare example of a shell galaxy in a likely dense galaxy region. The comparison between physically motivated SPH simulations with multi-band integrated photometry suggests that NGC 3934 is the product of a major merger.

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GALEXUV properties of the polar ring galaxy MCG-05-07-001 and the shell galaxies NGC 1210 and NGC 5329

Cited by 25 publications

References 81 publications

NGC 4262: a Virgo galaxy with an extended ultraviolet ring

NGC 4262: a Virgo galaxy with an extended ultraviolet ring

The Lyman alpha reference sample

NGC 3934: a shell galaxy in a compact galaxy environment

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