Galaxies with conspicuous optical warps

Решетников, В. П.; Mosenkov, Aleksandr V.; Моисеев, А. В.; Kotov, S. S.; Савченко, С. С.

doi:10.1093/mnras/stw1623

Cited by 32 publications

(38 citation statements)

References 75 publications

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“…In other words, we exclude the discs whose galactic plane is not aligned along the major axis of their fitted elliptical apertures (e.g. warped edge-on discs, see Reshetnikov et al 2016). As a result, we select 106 SNe in edge-on host galaxies.…”

Section: Inclinationmentioning

confidence: 99%

Supernovae and their host galaxies – V. The vertical distribution of supernovae in disc galaxies

Hakobyan

Barkhudaryan

Karapetyan

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the height distributions of the different types of supernovae (SNe) from the plane of their host galaxies. We use a well-defined sample of 102 nearby SNe appeared inside high-inclined (i 85 • ), morphologically non-disturbed S0-Sd host galaxies from the Sloan Digital Sky Survey. For the first time, we show that in all the subsamples of spirals, the vertical distribution of core-collapse (CC) SNe is about twice closer to the plane of host disc than the distribution of SNe Ia. In Sb-Sc hosts, the exponential scale height of CC SNe is consistent with those of the younger stellar population in the Milky Way (MW) thin disc, while the scale height of SNe Ia is consistent with those of the old population in the MW thick disc. We show that the ratio of scale lengths to scale heights of the distribution of CC SNe is consistent with those of the resolved young stars with ages from ∼ 10 Myr up to ∼ 100 Myr in nearby edge-on galaxies and the unresolved stellar population of extragalactic thin discs. The corresponding ratio for SNe Ia is consistent with the same ratios of the two populations of resolved stars with ages from a few 100 Myr up to a few Gyr and from a few Gyr up to ∼ 10 Gyr, as well as with the unresolved population of the thick disc. These results can be explained considering the age-scale height relation of the distribution of stellar population and the mean age difference between Type Ia and CC SNe progenitors.

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Section: Inclinationmentioning

confidence: 99%

Supernovae and their host galaxies – V. The vertical distribution of supernovae in disc galaxies

Hakobyan

Barkhudaryan

Karapetyan

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Another frequent phenomenon seen in both gas and stellar disks are "warps", where the kinematic position angle in the outer disk is different from that of the inner disk, implying the presence of a disk with a radially varying inclination (Sancisi 1976;Bosma 1981a,b;García-Ruiz et al 2002;Reshetnikov et al 2002;Schwarzkopf & Dettmar 2001;Ann & Park 2006). Warps frequently begin at or just beyond the optical radius R 25 , the radius where the B band surface brightness reaches 25 mag arcsec −2 (Briggs 1990;Ann & Park 2006;van der Kruit 2007), although they can begin at smaller radii (van de Voort et al 2015;Reshetnikov et al 2016). The high frequency of asymmetric and warped disks suggests that these features are either frequently generated or long lived.…”

mentioning

confidence: 99%

SDSS-IV MaNGA: characterizing non-axisymmetric motions in galaxy velocity fields using the Radon transform

Stark

Bundy

Westfall

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We show how the Radon transform (defined as a series of line integrals through an image at different orientations and offsets from the origin) can be used as a simple, non-parametric tool to characterize galaxy velocity fields, specifically their global kinematic position angles (PA k ) and any radial variation or asymmetry in PA k . This method is fast and easily automated, making it particularly beneficial in an era where IFU and interferometric surveys are yielding samples of thousands of galaxies. We demonstrate the Radon transform by applying it to gas and stellar velocity fields from the first ∼2800 galaxies of the SDSS-IV MaNGA IFU survey. We separately classify gas and stellar velocity fields into five categories based on the shape of their radial PA k profiles. At least half of stellar velocity fields and two-thirds of gas velocity fields are found to show detectable deviations from uniform coplanar circular motion, although most of these variations are symmetric about the center of the galaxy. The behavior of gas and stellar velocity fields is largely independent, even when PA k profiles for both components are measured over the same radii. We present evidence that one class of symmetric PA k variations is likely associated with bars and/or oval distortions, while another class is more consistent with warped disks. This analysis sets the stage for more in-depth future studies which explore the origin of diverse kinematic behavior in the galaxy population.

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“…The asymmetry is more pronounced in conspicuous warps (Reshetnikov et al 2016). Asymmetric S-shaped warps could be formed by a variety of causes.…”

Section: Warp Asymmetrymentioning

confidence: 98%

Environmental Dependence of Warps in Spiral Galaxies

Ann¹,

Bae²

2016

Journal of The Korean Astronomical Society

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We determined the warp parameters of 192 warped galaxies which are selected from 340 edge-on galaxies using color images as well as r-band isophotal maps. We derive the local background density (Σ n ) to examine the dependence of the warp amplitudes on the galaxy environment. We find a clear trend that strongly warped galaxies are likely to be found in high density regions where tidal interactions are supposed to be frequent. However, the correlation between α w and Σ n is too weak for weakly warped galaxies (α w < 4• ) and the cumulative distributions of weakly warped galaxies are not significantly different from those of galaxies with no detectable warps. This suggests that tidal interactions do not play a decisive role in the formation of weak warps.

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Galaxies with conspicuous optical warps

Cited by 32 publications

References 75 publications

Supernovae and their host galaxies – V. The vertical distribution of supernovae in disc galaxies

Supernovae and their host galaxies – V. The vertical distribution of supernovae in disc galaxies

SDSS-IV MaNGA: characterizing non-axisymmetric motions in galaxy velocity fields using the Radon transform

Environmental Dependence of Warps in Spiral Galaxies

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