Relative Orientation of Pairs of Spiral Galaxies in the Sloan Digital Sky Survey

Buxton, J. T.; Ryden, Barbara S.

doi:10.1088/0004-637x/756/2/135

Cited by 5 publications

(3 citation statements)

References 22 publications

(39 reference statements)

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“…Moon et al (2021, hereafter Paper III) proposed that SOA can be developed by interactions with neighboring galaxies. Some studies have found spin-spin alignment in interacting pairs (Mesa et al 2014;Koo & Lee 2018) although it is still controversial (Cervantes-Sodi et al 2010;Buxton & Ryden 2012;Lee 2012). This work focuses on SOA for dark matter halos with virialradius-wise interacting neighbors using a set of cosmological N -body simulations.…”

Section: Introductionmentioning

confidence: 99%

Living with Neighbors. IV. Dissecting the Spin$-$Orbit Alignment of Dark Matter Halos: Interacting Neighbors and the Local Large-scale Structure

An,

Kim,

Moon

et al. 2021

Preprint

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Spin-orbit alignment (SOA; i.e., the vector alignment between the halo spin and the orbital angular momentum of neighboring halos) provides an important clue to how galactic angular momenta develop. For this study, we extract virial-radius-wise contact halo pairs with mass ratios between 1/10 and 10 from a set of cosmological N -body simulations. In the spin-orbit angle distribution, we find a significant SOA in that 52.7 % ± 0.2 % of neighbors are on the prograde orbit. The SOA of our sample is mainly driven by low-mass target halos (< 10 11.5 h −1 M ) with close merging neighbors, corroborating the notion that the tidal interaction is one of the physical origins of SOA. We also examine the correlation of SOA with the adjacent filament and find that halos closer to the filament show stronger SOA. Most interestingly, we discover for the first time that halos with the spin parallel to the filament experience most frequently the prograde-polar interaction (i.e., fairly perpendicular but still prograde interaction; spin-orbit angle ∼ 70 • ). This instantly invokes the spin-flip event and the prograde-polar interaction will soon flip the spin of the halo to align it with the neighbor's orbital angular momentum. We propose that the SOA originates from the local cosmic flow along the anisotropic large-scale structure, especially that along the filament, and grows further by interactions with neighbors.

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Section: Introductionmentioning

confidence: 99%

Living with Neighbors. IV. Dissecting the Spin$-$Orbit Alignment of Dark Matter Halos: Interacting Neighbors and the Local Large-scale Structure

An,

Kim,

Moon

et al. 2021

Preprint

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“…Previous studies have found several types of alignments associated with galaxy pairs in which both the neighbor and the LSS play a role. First, the spins of the two galaxies in a pair tend to be preferentially aligned in the same direction (Flin 1993;Pestaña & Cabrera 2004;Slosar et al 2009;Cervantes-Sodi et al 2010;Mesa et al 2014;Koo & Lee 2018), although some controversy still remains (Oosterloo 1993;Buxton & Ryden 2012;Lee 2012). Such spin-spin alignment of galaxy pairs is generally interpreted as a result of the combined effect of the underlying LSS and the mutual interaction between paired galaxies (e.g., Sharp et al 1979;Helou 1984).…”

Section: Introductionmentioning

confidence: 99%

Living with Neighbors. III. The Origin of the Spin$-$Orbit Alignment of Galaxy Pairs: A Neighbor versus the Large-scale Structure

Moon,

An,

Yoon

2021

Preprint

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Recent observations revealed a coherence between the spin vector of a galaxy and the orbital motion of its neighbors. We refer to the phenomenon as "the spin-orbit alignment (SOA)" and explore its physical origin via the IllustrisTNG simulation. This is the first study to utilize a cosmological hydrodynamic simulation to investigate the SOA of galaxy pairs. In particular, we identify paired galaxies at z = 0 having the nearest neighbor with mass ratios from 1/10 to 10 and calculate the spin-orbit angle for each pair. Our results are as follows. (a) There exists a clear preference for prograde orientations (i.e., SOA) for galaxy pairs, qualitatively consistent with observations. (b) The SOA is significant for both baryonic and dark matter spins, being the strongest for gas and the weakest for dark matter. (c) The SOA is stronger for less massive targets and for targets having closer neighbors. (d) The SOA strengthens for galaxies in low-density regions, and the signal is dominated by central-satellite pairs in low-mass halos. (e) There is an explicit dependence of the SOA on the duration of interaction with its current neighbor. Taken together, we propose that the SOA witnessed at z = 0 has been developed mainly by interactions with a neighbor for an extended period of time, rather than tidal torque from the ambient large-scale structure.

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“…galaxy pairs remains inconclusive(Joachimi & Schneider 2010;Andrae & Jahnke 2011;Lee 2011;Buxton & Ryden 2012;Chisari et al 2015;Sifón et al 2015;Koo & Lee 2018;Krolewski et al 2019). Such alignment signals also seem to be subtly influenced by various intrinsic properties of the galaxies, including the halo mass(Li et al 2013;Trowland et al 2013;Xia et al 2017), bulge mass(Barsanti et al 2022), SF activity(Jimenez et al 2010;Shi et al 2021), and spiral morphology(Hu et al 1995;Lee 2011;Koo & Lee 2018).…”

mentioning

confidence: 99%

Living with Neighbors. V. Better-aligned Spiral+Spiral Galaxy Pairs Show Stronger Star Formation

Zee,

Moon,

Paudel

et al. 2024

ApJ

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Enhanced star formation (SF) with star-forming neighboring galaxies bolsters the hydrodynamical contributions during paired interactions. Although the relative spin orientation between interacting galaxies can influence this effect, it has not been comprehensively explored. In this study, utilizing a meticulously curated sample of nearby (0.02 < z < 0.06) spiral+spiral pairs and an isolated control sample from Sloan Digital Sky Survey Data Release 7, coupled with Galaxy Zoo 2, and an approach to estimate spin–spin alignment (SSA), we systematically compare the impact of relative orientation, cos ξ , on interaction-induced SF. We reveal that SSA plays a pivotal role along with the conventionally recognized parameters of projected separation and SF of neighboring galaxies. Our results show an increase in SF augmentation as configurations transition from perpendicular ( cos ξ ∼ 0 ) to well aligned ( cos ξ > 0.7 ). This enhancement is especially pronounced when neighboring galaxies have higher SF, suggesting that hydrodynamical processes drive the effects of relative orientation. The heightened hydrodynamical friction, attributed to increased ram pressure and the propensity for prograde orbits in well-aligned pairs, is consistent with our findings.

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Relative Orientation of Pairs of Spiral Galaxies in the Sloan Digital Sky Survey

Cited by 5 publications

References 22 publications

Living with Neighbors. IV. Dissecting the Spin$-$Orbit Alignment of Dark Matter Halos: Interacting Neighbors and the Local Large-scale Structure

Living with Neighbors. IV. Dissecting the Spin$-$Orbit Alignment of Dark Matter Halos: Interacting Neighbors and the Local Large-scale Structure

Living with Neighbors. III. The Origin of the Spin$-$Orbit Alignment of Galaxy Pairs: A Neighbor versus the Large-scale Structure

Living with Neighbors. V. Better-aligned Spiral+Spiral Galaxy Pairs Show Stronger Star Formation

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