Alignment between Filaments and Galaxy Spins from the MaNGA Integral-field Survey

Krolewski, Alex; Ho, Shirley; Chen, Yen‐Chi; Chan, Pui-man; Tenneti, Ananth; Bizyaev, Dmitry; Kraljic, Katarina

doi:10.3847/1538-4357/ab1010

Cited by 54 publications

(70 citation statements)

References 91 publications

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“…The mass dependence of the spin alignment signal is however debated. While some works confirmed the existence of a galaxy spin transi- tion from parallel to perpendicular with respect to the filament's direction (Dubois et al 2014;Codis et al 2018;Kraljic et al 2020b), and analogously with respect to walls (Codis et al 2018;Kraljic et al 2020b), others (Ganeshaiah Veena et al 2019;Krolewski et al 2019) found preferential perpendicular orientation with respect to filaments at all masses with no sign of a spin transition. A possible interpretation of this lack of detection of a clear transition is the nature of the filaments, with galaxies in thinner filaments having their spins more likely perpendicular to the filament's axis, compared to galaxies of similar mass in thicker filaments (Ganeshaiah Veena et al 2019).…”

Section: Introductionmentioning

confidence: 92%

SDSS-IV MaNGA: 3D spin alignment of spiral and S0 galaxies

Kraljic

Duckworth

Tojeiro

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We investigate the 3D spin alignment of galaxies with respect to the large-scale filaments using the MaNGA survey. The cosmic web is reconstructed from the Sloan Digital Sky Survey using disperse and the 3D spins of MaNGA galaxies are estimated using the thin disc approximation with integral field spectroscopy kinematics. Late-type spiral galaxies are found to have their spins parallel to the closest filament’s axis. The alignment signal is found to be dominated by low-mass spirals. Spins of S0-type galaxies tend to be oriented preferentially in perpendicular direction with respect to the filament’s axis. This orthogonal orientation is found to be dominated by S0s that show a notable misalignment between their kinematic components of stellar and ionized gas velocity fields and/or by low-mass S0s with lower rotation support compared to their high-mass counterparts. Qualitatively similar results are obtained when splitting galaxies based on the degree of ordered stellar rotation, such that galaxies with high spin magnitude have their spin aligned, and those with low spin magnitude in perpendicular direction to the filaments. In the context of conditional tidal torque theory, these findings suggest that galaxies’ spins retain memory of their larger scale environment. In agreement with measurements from hydrodynamical cosmological simulations, the measured signal at low redshift is weak, yet statistically significant. The dependence of the spin-filament orientation of galaxies on their stellar mass, morphology, and kinematics highlights the importance of sample selection to detect the signal.

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Section: Introductionmentioning

confidence: 92%

SDSS-IV MaNGA: 3D spin alignment of spiral and S0 galaxies

Kraljic

Duckworth

Tojeiro

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…The BG effect [58][59][60][61] induces a temperature dipole, of a magnitude comparable to that of the rkSZ effect, with a decrease in CMB temperature following the galaxies' transverse proper motion (and a temperature increase opposite to the transverse proper motion). Regardless of the presence of systematic alignments between the directions of galaxies' spins and their proper motionsinduced, for instance, by filaments [57,[62][63][64]]-, we don't expect any systematic alignment in their sense. Thus, on spin-aligned stacks of large samples of galaxies, any BGinduced temperature dipole should average to zero.…”

Section: Detection Feasibilitymentioning

confidence: 92%

Probing gaseous galactic halos through the rotational kinematic Sunyaev-Zeldovich effect

Matilla

Haiman

2020

Phys. Rev. D

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The rotational kinematic Sunyaev-Zeldovich (rkSZ) signal, imprinted on the cosmic microwave background (CMB) by the gaseous halos (spinning "atmospheres") of foreground galaxies, would be a novel probe of galaxy formation. Although the signal is too weak to detect in individual galaxies, we analyze the feasibility of its statistical detection via stacking CMB data on many galaxies for which the spin orientation can be estimated spectroscopically. We use an "optimistic" model, in which fully ionized atmospheres contain the cosmic baryon fraction and spin at the halo's circular velocity vcirc, and a more realistic model, based on hydrodynamical simulations, with multi-phase atmospheres spinning at a fraction of vcirc. We incorporate realistic noise estimates into our analysis. Using low-redshift galaxy properties from the MaNGA spectroscopic survey (with median halo mass of 6.6 × 10 11 M ), and CMB data quality from Planck, we find that a 3σ detection would require a few×10 4 galaxies, even in the optimistic model. This is too high for current surveys, but upcoming higher-angular resolution CMB experiments will significantly reduce the requirements: stacking CMB data on galaxy spins in a ∼ 10 deg 2 can rule out the optimistic models, and ≈350 deg 2 will suffice for a 3σ detection with ACT. As a proof-of-concept, we stacked Planck data on the position of ≈ 2, 000 MaNGA galaxies, aligned with the galaxies' projected spin, and scaled to their halos' angular size. We rule out average temperature dipoles larger than ≈ 1.9 µK around field spiral galaxies.

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“…Subsequent work by Dubois et al (2014); Welker et al (2014); Codis et al (2018); showed a clear mass-dependent spin transition of galaxies from parallel to perpendicular in the Horizon AGN and Illustris hydro simulations. In contrast, Ganeshaiah Veena et al (2019) and Krolewski et al (2019) detected a mass dependent alignment but not a spin transition in SPH based EAGLE and Massive Black-2 simulations. Apart from galaxy stellar mass, the spin alignment trend depends on galaxy morphology (Wang & Kang 2017;Ganeshaiah Veena et al 2019), color (Codis et al 2018;, HI content and filament density (Kraljic, Davé & Pichon 2020).…”

Section: Galaxy Spin Alignmentsmentioning

confidence: 84%

“…The first robust observational evidence was provided by the Tempel, Stoica & Saar (2013) and Tempel & Libeskind (2013b) who have shown that the spins of spiral galaxies are preferentially aligned with the filament axis while the minor axis of elliptical galaxies, which are typically higher mass, is preferentially perpendicular to the filaments axis (see also Jones, van de Weygaert & Aragón-Calvo 2010; Hirv et al 2017). The same trend, although at a lower statistical significance due to the smaller sample, is seen when inferring the spin from the stellar or gaseous velocity maps, such as those obtained using SAMI or MaNGA (Krolewski et al 2019;Welker et al 2020;Blue Bird et al 2020) The present day alignment between halo and galaxy spin and their filaments is different from that predicted by TTT. For example, as we just discussed, the high-mass haloes have a propensity for perpendicular spin while TTT predicts a parallel alignment.…”

Section: Introductionmentioning

confidence: 83%

“…Few studies reported a parallel alignment for Scd galaxies (Hirv et al 2017), blue and red galaxies (Zhang et al 2013) and perpendicular for Sab type galaxies (Hirv et al 2017). Several other studies find either a slight deviation from random alignment or no alignment at all (Lee & Erdogdu 2007;Pahwa et al 2016;Krolewski et al 2019).…”

Section: Galaxy Spin Alignmentsmentioning

confidence: 99%

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The Cosmic Ballet: spinning in the web

Veena

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The exact conversation between Alexander and the gymnosophist is not known, but there are several versions of it in folk tales. 1.1: A glimpse into the unknown 3 The origin of rotation in galaxies remains an important question in the field of galaxy formation as it is not only linked to their morphology but also to the rotation of their host dark matter haloes. The key to answering these questions lies in studying the underlying cosmic web in which galaxies and dark matter haloes form and grow. Within this large-scale network of matter, galaxies stand out as majestic pearls and are spinning in a specific rhythm, resembling swirling ballerinas along the long filamentary strings of matter. This is akin to performing a grand ballet on this gigantic cosmic stage, the cosmic web, making us wonder how all of this has been set into motion. The most prominent example is the disc of our own galaxy, the Milky Way, which is spinning perpendicular to the underlying local web. In this thesis, we investigate how and why galaxies rotate from the point of the view of the large-scale cosmic web. We study how different features of the web influences properties such as spin and shape of galaxies and their dark matter haloes. We find explicit correlations between spin and the host cosmic web components in which they are growing. Ω Λ = Λ 3H 2 0 = 0.691, H 0 = 67.74 km s −1 Mpc −1. These fractions are given with respect to the critical density ρ c = 3H 2 0 8πG , defined as the density for which the Universe is spatially flat. The Hubble parameter H is defined as H =ȧ a where a is the expansion factor and H 0 is the Hub-Here, v is the peculiar velocity, which is the relative velocity of a particle with respect to the Hubble flow, and it is given as: u = Hr + v, (1.6) where u is the total velocity and r = ax. At a certain stage in the structure formation process, the regions of overdensities corresponding to δ > 0 overtake and matter accumulates rapidly in these regions. At this stage, the linear approximation, which is valid for |δ| 1, 1.3: Numerical simulations The simulations are carried out with periodic boundary conditions to account for the cosmological principle that the Universe is homogeneous and isotropic on large scales. The power spectrum for cold dark matter is usually used to initialize a simulation. Positions and velocities are assigned to each dark matter particle and are evolved from a uniform distribution using the linear theory approximation (as described in subsection 1.4.1). This sets up the initial conditions for the simulation. 1.3: Numerical simulations Successes of hydro simulations: The recent decade has seen several large volume simulations that can reproduce surprisingly well many global properties of galaxies, such as the stellar mass function, the bimodality of star-formation rates and colours, and galaxy morphologies. Some of the most studied and most advanced hydrodynamical simulations include: Illustris(Vogelsberger et al. 2014), eagle (Schaye et al. 2015), Horizon AGN (Dubois et al. 2014), Illustris TNG...

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Alignment between Filaments and Galaxy Spins from the MaNGA Integral-field Survey

Cited by 54 publications

References 91 publications

SDSS-IV MaNGA: 3D spin alignment of spiral and S0 galaxies

SDSS-IV MaNGA: 3D spin alignment of spiral and S0 galaxies

Probing gaseous galactic halos through the rotational kinematic Sunyaev-Zeldovich effect

The Cosmic Ballet: spinning in the web

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