Probing IGM large-scale flows: warps in galaxies at shells of voids

López-Corredoira, Martín; Florido, E.; Betancort-Rijo, J.; Trujillo, Ignacio; Carretero, C.; Guijarro, A.; Battaner, E.; Patiri, Santiago G.

doi:10.1051/0004-6361:20078057

Cited by 5 publications

(4 citation statements)

References 33 publications

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“…García-Ruiz et al (2002), Józsa (2007)] makes comprehensive warp statistics, studies of the structure of the IGM in different environments (Haan & Braun 2014), as well as studies of large-scale alignment of outer disk material, possible. Tracing the IGM through spin alignment of outer disks has been attempted using optical observations (Battaner et al 1990;López-Corredoira et al 2008). The wide-field access to the much better suited tracer HI, which is often detected far beyond the optical disk and including the kinematical information, will, however, mean an observational quantum step for studies of the ISM-IGM interface.…”

Section: All Sky Survey Of the Igmmentioning

confidence: 99%

See 1 more Smart Citation

Observations of the Intergalactic Medium and the Cosmic Web in the SKA era

Popping¹,

Meyer²,

Obreschkow³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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The interaction of galaxies with their environment, the Intergalactic Medium (IGM), is a very important aspect of galaxy formation. One of the most fundamental, but unanswered questions in the evolution of galaxies is how gas circulates in and around galaxies and how it enters the galaxies to support star formation. We have several lines of evidence that the observed evolution of star formation requires gas accretion from the IGM at all times and on all cosmic scales. This gas remains largely unaccounted for and the outstanding questions are where this gas resides and what the physical mechanisms of accretion are. The gas is expected to be embedded in an extended cosmic web made of sheets and filaments. Such large-scale filaments of gas are expected by cosmological numerical simulations, which have made significant progress in recent years. Such simulations do not only model the large scale structure of the cosmic web, but also investigate the neutral gas component. To truly make significant progress in understanding the distribution of neutral hydrogen in the IGM, column densities of N HI ∼10 18 cm −2 and below have to be probed over large areas on the sky at sub-arcminute resolution. These are the densities of the faintest structures known today around nearby galaxies, though mostly found with single dish telescopes which do not have the resolution to resolve these structures and investigate any kinematics. Existing interferometers lack the collecting power or short baselines to achieve brightness sensitivities typically below N HI ∼10 19 cm −2 . Reaching lower column densities with current facilities is feasible, however requires prohibitively long observing times. The SKA will for the first time break these barriers, enabling interferometric observations an order of magnitude deeper than current interferometers and with an order of magnitude better linear resolution than single-dish telescopes.Advancing Astrophysics with the Square Kilometre Array

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Section: All Sky Survey Of the Igmmentioning

confidence: 99%

“…The mechanism of IGM accretion onto the disc produces warps (López-Corredoira et al 2008). The ubiquity of the warp phenomenon might be used to reconstruct both the IGM density profile and the individual member orbits within galaxy groups (Haan & Braun 2014).…”

Section: All Sky Survey Of the Igmmentioning

confidence: 99%

Observations of the Intergalactic Medium and the Cosmic Web in the SKA era

Popping¹,

Meyer²,

Obreschkow³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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“…There is, however, only a weak correlation (Kollatschny & Dietrich 1990;Reshetnikov & Combes 1998;Schwarzkopf & Dettmar 2001) or even anticorrelation (García-Ruiz et al 2002) between the frequency of warps and the local environment, at variance with the conventional tidal scenario. Moreover, several isolated galaxies in the field exhibit warped disks (Briggs 1990;Verdes-Montenegro et al 1997;Ann 2007;López-Corredoira et al 2008b). Thus, other alternative warp formation mechanisms have been suggested, including cold gas flow (Ostriker & Binney 1989;Jiang & Binney 1999;Roškar et al 2010;Rahmani et al 2018), interaction with the intergalactic accretion onto disks (López-Corredoira et al 2002;Sánchez-Salcedo 2006), ram pressure by galaxies' movement with respect to the intergalactic medium (Haan & Braun 2014), misalignment between stellar disks and prolate/oblate dark matter halos (Sparke & Casertano 1988;Kuijken 1991;Nelson & Tremaine 1995;Ideta et al 2000;Jeon et al 2009;Dubinski & Chakrabarty 2009;Sellwood & Debattista 2022), and interaction with the intergalactic magnetic field (Battaner et al 1990;Battaner & Jiménez-Vicente 1998).…”

Section: Introductionmentioning

confidence: 99%

Warped Disk Galaxies. I. Linking U-type Warps in Groups/Clusters to Jellyfish Galaxies

Yoon

Moon

et al. 2022

ApJ

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Warped disk galaxies are classified into two morphologies: S and U types. Conventional theories routinely attribute both types to galactic tidal interaction and/or gas accretion, but reproducing U types in simulations is extremely challenging. Here we investigate whether both types are governed by the same mechanisms using the most extensive sample of ∼8000 nearby (0.02 < z < 0.06) massive (M */M ⊙ > 109) edge-on disks from the Sloan Digital Sky Survey. We find that U types show on average bluer optical colors and a higher specific star formation rate (sSFR) than S types, with more strongly warped U types having a higher sSFR. We also find that while the S-type warp properties correlate with the tidal force by the nearest neighbor regardless of the environment, there is no such correlation for U types in groups/clusters, suggesting a nontidal environmental could be at play for U types, such as ram pressure stripping (RPS). Indeed, U types are more common in groups/clusters than in fields and they have stellar mass, gas fraction, sSFR enhancement, and phase-space distribution closely analogous to RPS-induced jellyfish galaxies in clusters. We furthermore show that the stellar disks of most RPS galaxies in the IllustrisTNG simulation are warped in a U shape and bent in the opposite direction of stripped gas tails, satisfying theoretical expectations for stellar warps embedded in jellyfishes. We therefore suggest that despite the majority of U types that live in fields being still less explained, RPS can be an alternative origin for those in groups/clusters.

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“…Warps can appear in three flavours (cf. López-Corredoira et al 2008). The N-or S-like warps have ω R and ω L of the same sign, the signs of ω R and ω L for U-like warps differ, and L-like warps apply to galaxies in which only one side is warped.…”

Section: Warp Parametersmentioning

confidence: 99%

Near-infrared and optical observations of galactic warps: a common, unexplained feature of most discs

Guijarro

Peletier

Battaner

et al. 2010

A&A

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Context. Warps occurring in galactic discs have been studied extensively in HI and in the optical, but rarely in the near-infrared (NIR) bands that trace the older stellar populations. Aims. We provide NIR data of nearby edge-on galaxies, combined with optical observations, for direct comparison of the properties of galactic warps as a function of wavelength, and calculate warp curves for each galaxy and obtain the characteristic warp parameters. We discuss these properties as possible constraints to the different mechanisms that have been proposed for the development and persistence of galactic warps. Methods. We observed 20 galaxies that were selected from a statistically complete diameter-limited subsample of edge-on disc galaxies. We used the Cerro Tololo Infrared Imager (CIRIM) at the CTIO 1.5 m Ritchey-Chretien telescope to acquire the NIR data. We used the 1.54 m Danish and 0.92 m Dutch telescopes at the European Southern Observatory's La Silla site for our optical observations. Results. Our results show that 13 of our 20 sample galaxies are warped, with the warp more pronounced in the optical than at NIR wavelengths. In the remaining seven galaxies, no warp is apparent within the limitations of our automated detection method. The transition between the unperturbed inner disc and the outer, warped region is rather abrupt. S0 galaxies exhibit very small or no warps. The magnetic model remains one of a number of interesting formation scenarios.

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Probing IGM large-scale flows: warps in galaxies at shells of voids

Cited by 5 publications

References 33 publications

Observations of the Intergalactic Medium and the Cosmic Web in the SKA era

Observations of the Intergalactic Medium and the Cosmic Web in the SKA era

Warped Disk Galaxies. I. Linking U-type Warps in Groups/Clusters to Jellyfish Galaxies

Near-infrared and optical observations of galactic warps: a common, unexplained feature of most discs

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