The SAMI Galaxy Survey: first detection of a transition in spin orientation with respect to cosmic filaments in the stellar kinematics of galaxies

Welker, Charlotte; Bland-Hawthorn, Joss; Sande, Jesse van de; Lagos, Claudia del P.; Elahi, Pascal J.; Obreschkow, Danail; Bryant, Julia J.; Pichon, Christophe; Cortese, Luca; Richards, Samuel N.; Croom, S. M.; Goodwin, Michael; Lawrence, Jon; Sweet, Sarah M.; López-Sánchez, Ángel R.; Medling, Anne M.; Owers, Matt S.; Dubois, Yohan; Devriendt, Julien

doi:10.1093/mnras/stz2860

Cited by 92 publications

(120 citation statements)

References 93 publications

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“…3 in which the dark matter filaments appear 'fluffier'). This can have important implications for the galaxies themselves (Birnboim & Dekel 2003;Pichon et al 2011;Danovich et al 2012) and their distribution in clusters (Welker et al 2020). Note that this result refers to massive clusters at z=0, where gas filaments could be more perturbed than at higher redshifts (Dubois et al 2012).…”

Section: Dark Matter and Gas Characteristics Of Cluster Filamentsmentioning

confidence: 91%

the threehundred: the structure and properties of cosmic filaments in the outskirts of galaxy clusters

Rost

Kuchner

Welker

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Galaxy cluster outskirts are described by complex velocity fields induced by diffuse material collapsing towards filaments, gas, and galaxies falling into clusters, and gas shock processes triggered by substructures. A simple scenario that describes the large-scale tidal fields of the cosmic web is not able to fully account for this variety, nor for the differences between gas and collisionless dark matter. We have studied the filamentary structure in zoom-in resimulations centred on 324 clusters from the threehundred project, focusing on differences between dark and baryonic matter. This paper describes the properties of filaments around clusters out to five R200, based on the diffuse filament medium where haloes had been removed. For this, we stack the remaining particles of all simulated volumes to calculate the average profiles of dark matter and gas filaments. We find that filaments increase their thickness closer to nodes and detect signatures of gas turbulence at a distance of ${\sim}2 \rm {{{~h^{-1}\,{\rm Mpc}}}}$ from the cluster. These are absent in dark matter. Both gas and dark matter collapse towards filament spines at a rate of ${\sim}200 \,\rm {km ~ s^{-1}\, h^{-1}}$. We see that gas preferentially enters the cluster as part of filaments, and leaves the cluster centre outside filaments. We further see evidence for an accretion shock just outside the cluster. For dark matter, this preference is less obvious. We argue that this difference is related to the turbulent environment. This indicates that filaments act as highways to fuel the inner regions of clusters with gas and galaxies.

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Section: Dark Matter and Gas Characteristics Of Cluster Filamentsmentioning

confidence: 91%

the threehundred: the structure and properties of cosmic filaments in the outskirts of galaxy clusters

Rost

Kuchner

Welker

et al. 2020

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: 91%

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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“…1). In addition, as Welker et al (2019) pointed out, a correction based on the compression of groups can only be applied for rich groups ( 10 members). Moreover, it does not account for boundary effects that can cause spurious filaments along the line of sight.…”

Section: Compression Of Virialized Structuresmentioning

confidence: 99%

“…The outskirts of galaxy clusters are thus areas of increasing interest for both cosmology and astrophysics. Cosmological simulations of galaxy cluster formation depict cluster outskirts as the playing field for large-scale structure formation as it happens: the rich, thermal, kinematic and chemical content of merging sub-clusters, infalling groups, clumps of gas and gas trapped in collapsed dark matter halos funnelled through cold filamentary streams are part of yet-to-be explored accretion physics (Dekel et al 2009;Danovich et al 2012;Welker et al 2019;Walker et al 2019).…”

Section: Introductionmentioning

confidence: 99%

“…The last decade has seen a number of excellent methods to identify and classify features of the cosmic web (e.g., Aragón-Calvo et al 2007;Sousbie 2011;Cautun et al 2012;Courtois et al 2013;Tempel et al 2014;Falck & Neyrinck 2015), each designed to tackle specific problems to be applied to different kinds of data and thus disagreements are understandable and well documented (e.g., Libeskind et al 2017;Rost et al 2020b). Structure finding methods are successfully being applied to simulated and observed datasets alike, including photometric and spectroscopic surveys such as SDSS (Tempel et al 2013;Kuutma et al 2017;Chen et al 2016;Malavasi et al 2020), COS-MOS (Darvish et al 2017;Laigle et al 2017) and GAMA (Kraljic et al 2018;Welker et al 2019) amongst others (Malavasi et al 2016;Sarron et al 2019;Santiago-Bautista et al 2020). The main goal of many of these studies is to investigate galaxy properties such as mass, colour, morphology and gas content, and, increasingly so, alignments and spin orientation with respect to cosmic filaments.…”

Section: Introductionmentioning

confidence: 99%

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Cosmic filaments in galaxy cluster outskirts: quantifying finding filaments in redshift space

Kuchner

Aragón-Salamanca

Rost

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Inferring line-of-sight distances from redshifts in and around galaxy clusters is complicated by peculiar velocities, a phenomenon known as the ”Fingers of God” (FoG). This presents a significant challenge for finding filaments in large observational data sets as these artificial elongations can be wrongly identified as cosmic web filaments by extraction algorithms. Upcoming targeted wide-field spectroscopic surveys of galaxy clusters and their infall regions such as the WEAVE Wide-Field Cluster Survey motivate our investigation of the impact of FoG on finding filaments connected to clusters. Using zoom-in resimulations of 324 massive galaxy clusters and their outskirts from The ThreeHundred project, we test methods typically applied to large-scale spectroscopic data sets. This paper describes our investigation of whether a statistical compression of the FoG of cluster centres and galaxy groups can lead to correct filament extractions in the cluster outskirts. We find that within 5R200 (∼15 h−1Mpc) statistically correcting for FoG elongations of virialized regions does not achieve reliable filament networks compared to reference filament networks based on true positions. This is due to the complex flowing motions of galaxies towards filaments in addition to the cluster infall, which overwhelm the signal of the filaments relative to the volume we probe. While information from spectroscopic redshifts is still important to isolate the cluster regions, and thereby reduce background and foreground interlopers, we expect future spectroscopic surveys of galaxy cluster outskirts to rely on 2D positions of galaxies to extract cosmic filaments.

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The SAMI Galaxy Survey: first detection of a transition in spin orientation with respect to cosmic filaments in the stellar kinematics of galaxies

Cited by 92 publications

References 93 publications

the threehundred: the structure and properties of cosmic filaments in the outskirts of galaxy clusters

the threehundred: the structure and properties of cosmic filaments in the outskirts of galaxy clusters

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

Cosmic filaments in galaxy cluster outskirts: quantifying finding filaments in redshift space

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