On the direction of rotation of the spirals in galaxies

Pasha, I. I.; Смирнов, М. А.

doi:10.1007/bf00651844

Cited by 32 publications

(23 citation statements)

References 10 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As discussed in Pasha & Smirnov (1982), a fraction f = 0.04 of galaxies has gas angular momentum that is pointing in the opposite direction to the apparent galaxy spin inferred from orientation of spiral arms. If we momentarily distinguish between the actual and the apparent gas spin correlation functions, we can write since correlation function of spins will receive a negative contribution if exactly one spin (but not both) was randomly reversed.…”

Section: Correlations Of Projected Spinsmentioning

confidence: 93%

“…This quantity is strongly correlated with the real angular momentum of the gas. The correlation, however, is not perfect and observations show that the angular momentum vector of the gas points in the opposite direction in about 4 per cent of systems (Pasha & Smirnov 1982). In turn, there are theoretical expectations that there is a strong, but not perfect, correlation between the angular momentum vector of gas and that of the dark matter haloes hosting the galaxy (van den Bosch et al 2002).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Galaxy Zoo: chiral correlation function of galaxy spins^★

Slosar

Land

Bamford

et al. 2009

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Galaxy Zoo is the first study of nearby galaxies that contains reliable information about the spiral sense of rotation of galaxy arms for a sizeable number of galaxies. We measure the correlation function of spin chirality (the sense in which galaxies appear to be spinning) of face‐on spiral galaxies in angular, real and projected spaces. Our results indicate a hint of positive correlation at separations less than ∼0.5 Mpc at a statistical significance of 2σ–3σ. This is the first experimental evidence for chiral correlation of spins. Within the tidal torque theory, it indicates that the inertia tensors of nearby galaxies are correlated. This is complementary to the studies of nearby spin axis correlations that probe the correlations of the tidal field. Theoretical interpretation is made difficult by the small distances at which the correlations are detected, implying that substructure might play a significant role, and our necessary selection of face‐on spiral galaxies, rather than a general volume‐limited sample.

show abstract

Section: Correlations Of Projected Spinsmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Galaxy Zoo: chiral correlation function of galaxy spins^★

Slosar

Land

Bamford

et al. 2009

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Proceeding from the fact that the arms of the most spiral galaxies are trailing (Pasha & Smirnov 1982) we should postulate that in the Galaxy p < 0. As one can see, the geometrical form of a spiral arm is represented, as most other authors have done (Seigar & James 1998;Levine et al 2006;Hou et al 2009;Gusev & Efremov 2014;Vallée 2014), by a single logarithmic function or a spiral of constant pitch, r = r 0 e (ϕ−ϕ0) tan p .…”

Section: Velocity Fieldmentioning

confidence: 98%

A model for the Lin‐Shu type density‐wave structure of our Galaxy: Line‐of‐sight and transverse‐longitudinal velocities of 242 optically visible open clusters

Griv

Jiang

2015

Astron Nachr

View full text Add to dashboard Cite

In this paper, the fourth in a series, we examine again one of the implications of the Lin-Shu density-wave theory, specifically, the noncircular systematic motion of the Galactic objects. Our previous investigation is extended by analyzing simultaneously both the line-of-sight and transversal velocities of a sample of open clusters for which velocities, distances and ages are available. The ordinary equations of the Oort-Lindblad theory of galactic differential rotation are used. The minor effects caused by the two-dimensional tightly-wound density waves are also taken into account. The published data of 242 currently known optically visible clusters having distances r < 3 kpc from the Sun and −200 < z < 200 pc from the Galactic plane, and ages 2×10 8 < t < 2×10 9 yr are collected from Dias et al. (2014), excluding extremely far, high-velocity, young and old objects in our fitting. The most noteworthy result is the fact that the parameters of Lin-Shu type density waves estimated from two independent line-of-sight and transversal along the Galactic longitude velocities are nearly equal. We argue that the resemblance of these Galactic wave structures is so remarkable that no doubt is felt as to the theory's truth with respect to these data. The results obtained allow us to conclude that several low-m trailing density-wave patterns with different number of spiral arms m (say, m = 1, 2, 3, and 4), pitch angles (about 5• , 8• , 11• , and 14 • , respectively) and amplitudes of the perturbed gravitational potential may coexist in the Galaxy. The latter suggests the asymmetric multiarm, not well-organized ("flocculent") spiral structure of the system.

show abstract

“…NGC 5426 is a two-armed spiral galaxy with well-defined arms so we may assume it is a trailing spiral since leading spiral arms are an uncommon phenomena (Pasha & Smirnov 1982) and the dynamical theory to explain them is mostly associated to the formation of a single leading arm (Thomasson et al 1989). Considering this sens of rotation and the position of the approaching and the receding radial velocities we can infer this galaxy's orientation placing its western side closer to the observer than the eastern side.…”

Section: Discussionmentioning

confidence: 99%

The isolated interacting galaxy pair NGC 5426/27 (Arp 271)

Fuentes-Carrera

Rosado

Amram

et al. 2004

A&A

View full text Add to dashboard Cite

Abstract. We present Hα observations of the isolated interacting galaxy pair NGC 5426/27 using the scanning Fabry-Perot interferometer PUMA. The velocity field, various kinematical parameters and rotation curve for each galaxy were derived. The FWHM map and the residual velocities map were also computed to study the role of non-circular motions of the gas. Most of these motions can be associated with the presence of spiral arms and structure such as central bars. We found a small bar-like structure in NGC 5426, a distorted velocity field for NGC 5427 and a bridge-like feature between both galaxies which seems to be associated with NGC 5426. Using the observed rotation curves, a range of possible masses was computed for each galaxy. These were compared with the orbital mass of the pair derived from the relative motion of the participants. The rotation curve of each galaxy was also used to fit different mass distribution models considering the most common theoretical dark halo models. An analysis of the interaction process is presented and a possible 3D scenario for this encounter is also suggested.

show abstract

On the direction of rotation of the spirals in galaxies

Cited by 32 publications

References 10 publications

Galaxy Zoo: chiral correlation function of galaxy spins^★

Galaxy Zoo: chiral correlation function of galaxy spins^★

A model for the Lin‐Shu type density‐wave structure of our Galaxy: Line‐of‐sight and transverse‐longitudinal velocities of 242 optically visible open clusters

The isolated interacting galaxy pair NGC 5426/27 (Arp 271)

Contact Info

Product

Resources

About

On the direction of rotation of the spirals in galaxies

Cited by 32 publications

References 10 publications

Galaxy Zoo: chiral correlation function of galaxy spins★

Galaxy Zoo: chiral correlation function of galaxy spins★

A model for the Lin‐Shu type density‐wave structure of our Galaxy: Line‐of‐sight and transverse‐longitudinal velocities of 242 optically visible open clusters

The isolated interacting galaxy pair NGC 5426/27 (Arp 271)

Contact Info

Product

Resources

About

Galaxy Zoo: chiral correlation function of galaxy spins^★

Galaxy Zoo: chiral correlation function of galaxy spins^★