Pitch angles of distant spiral galaxies

Савченко, С. С.; Решетников, В. П.

doi:10.1134/s1063773711120097

Cited by 15 publications

(19 citation statements)

References 21 publications

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“…7 shows several known observational trends of the average pitch angles with general parameters of galaxies. As one can see in this figure, early-type, red and massive (with large values of Vmax) galaxies, on average, demon- strate tighter spiral arms in comparison with late-type, blue and less massive (see also Kennicutt 1981, Ma 2002, Savchenko & Reshetnikov 2011. We found no statistically significant correlation between the pitch angles and the total luminosity of galaxies.…”

Section: Pitch Angles and Their Variationsmentioning

confidence: 43%

Pitch angle variations in spiral galaxies

Савченко¹,

Решетников²

2013

Monthly Notices of the Royal Astronomical Society

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We present a detailed photometric study and measurements of spiral arm pitch angles for a sample of 50 non-barred or weakly barred grand-design spiral galaxies selected from Sloan Digital Sky Survey. In order to find pitch angles, we used a new method based on the window Fourier analysis of their images. This method allows us not only to infer the average pitch angle, but to obtain its value as a function of galactocentric radius as well. Our main results are as follows:(1) Spiral arms of most galaxies cannot be described by a single value of the pitch angle. About 2/3 of galaxies demonstrate pitch angle variations exceeding 20%. In most galaxies in the sample their pitch angle decreases by increasing the distance from the centre.(2) Pitch angle variations correlate with the properties of galaxies -with the shape of the surface brightness distribution (envelope-type or truncated disc), and with the sign of stellar disc colour gradient.(3) More luminous and bright bulges produce more tightly wound spiral arms, that is in agreement with current models for spiral arms formation.

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Section: Pitch Angles and Their Variationsmentioning

confidence: 43%

Pitch angle variations in spiral galaxies

Савченко¹,

Решетников²

2013

Monthly Notices of the Royal Astronomical Society

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“…The maximum rotational velocity does not only correlate with M BH (Figure 2), but it also correlates with, among other things, the spiral-arm pitch angle, φ (for an introduction, see Davis et al 2017). 31 Kennicutt (1981) observed a correlation between the maximum rotational velocity and the spiral-arm pitch angle, which was later reanalyzed and quantified by Savchenko & Reshetnikov (2011). Kennicutt (1981) described the anticorrelation as being "fairly strong," 32 and claimed that it supports the density-wave theory expectations for spiral-arm geometry .…”

Section: The V Max -φ Relationmentioning

confidence: 99%

A Consistent Set of Empirical Scaling Relations for Spiral Galaxies: The (v_max, M_oM)–(σ₀, M_BH, ϕ) Relations

Davis

Graham

Combes

2019

ApJ

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Using the latest sample of 48 spiral galaxies having a directly measured supermassive black hole mass, M BH , we determine how the maximum disk rotational velocity, v max (and the implied dark matter halo mass, M DM ), correlates with the (i) black hole mass, (ii) central velocity dispersion, σ 0 , and (iii) spiral-arm pitch angle, φ. We find that M BH ∝ v 10.62±1.37 max ∝ M 4.35±0.66 DM , significantly steeper than previously reported, and with a total root mean square scatter (0.58 dex) similar to that about the M BH -σ 0 relation for spiral galaxies-in stark disagreement with claims that M BH does not correlate with disks. Moreover, this M BH -v max relation is consistent with the unification of the Tully-Fisher relation (involving the total stellar mass, M * ,tot ) and the steep M BH ∝ M 3.05±0.53 * ,tot relation observed in spiral galaxies. We also find that DM, consistent with past studies connecting stellar bulges (with σ 0 100 km s −1 ), dark matter halos, and a nonconstant v max /σ 0 ratio. Finally, we report that tan |φ| ∝ (−1.18 ± 0.19) log v max ∝ (−0.48 ± 0.09) log M DM , providing a novel formulation between the geometry (i.e., the logarithmic spiral-arm pitch angle) and kinematics of spiral galaxy disks. While the v max -φ relation may facilitate distance estimations to face-on spiral galaxies through the Tully-Fisher relation and using φ as a proxy for v max , the M DM -φ relation provides a path for determining dark matter halo masses from imaging data alone. Furthermore, based on a spiral galaxy sample size that is double the size used previously, the self-consistent relations presented here provide dramatically revised constraints for theory and simulations.4 If we calculate the Tully-Fisher relation from our dataset, we find that M * ,tot ∝ v 3.94±1.01 rot , which is consistent with Equation (1) at the level of 0.05 σ. 5 The dynamics of newly assembled massive objects (DY-NAMO) project (Green et al. 2010(Green et al. , 2014Bassett et al. 2014) demonstrated that their more local (z ∼ 0.1) sample of galaxies, selected to have high star-formation rates, are analogs of turbulent z 2 disk galaxies, with similar vrot/σ 0 ratios. 46 The quantity vmax should not be confused with the circular rotation velocity of the disk of our Galaxy at the location of the Sun and equal to (238 ± 15) km s −1 (Bland-Hawthorn & Gerhard 2016) or (229.0 ± 0.2) km s −1 (Eilers et al. 2019).

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“…Along the Hubble sequence, spiral galaxies disks tend to be thinner (Ma 2002). Some correlations are also found with the pitch angle, like the one related with the central supermassive black hole in spiral galaxies whose mass seems to decrease with the pitch angle (Seigar et al 2008;Shields et al 2010); spiral galaxies with higher rotational velocity also have tighter spirals (Kennicutt 1981;Savchenko & Reshetnikov 2011); in the same manner, it seems that for disks with lower surface densities and lower total mass-luminosity ratios, pitch angles tend to be larger (Ma 2002).…”

Section: Introductionmentioning

confidence: 97%

Stellar Orbital Studies in Normal Spiral Galaxies. I. Restrictions to the Pitch Angle

Pérez-Villegas

Pichardo

Moreno

2013

ApJ

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We built a family of non-axisymmetric potential models for normal non-barred or weakly-barred spiral galaxies as defined in the simplest classification of galaxies: the Hubble sequence. For this purpose a three-dimensional self-gravitating model for spiral arms PERLAS is superimposed to the galactic axisymmetric potentials. We analyze the stellar dynamics varying only the pitch angle of the spiral arms, from 4 • to 40 • , for an Sa galaxy, from 8 • to 45 • , for an Sb galaxy, and from 10 • to 60 • , for an Sc galaxy. Self-consistency is indirectly tested through periodic orbital analysis, and through density response studies for each morphological type. Based on ordered behavior, periodic orbits studies show that for pitch angles up to approximately 15 • , 18 • , and 20 • for Sa, Sb and Sc galaxies, respectively, the density response supports the spiral arms potential, a requisite for the existence of a long-lasting large-scale spiral structure. Beyond those limits, the density response tends to "avoid" the potential imposed by mantaining lower pitch angles in the density response; in that case the spiral arms may be explained as transient features rather than long-lasting large-scale structures. In a second limit, from a phase space orbital study based on chaotic behavior, we found that for pitch angles larger than ∼ 30 • , ∼ 40 • and ∼ 50 • for Sa, Sb, and Sc galaxies, respectively, chaotic orbits dominate all phase space prograde region that surrounds the periodic orbits sculpting the spiral arms and even destroying them. This result seems to be in good agreement with observations of pitch angles in typical isolated normal spiral galaxies.

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Pitch angles of distant spiral galaxies

Cited by 15 publications

References 21 publications

Pitch angle variations in spiral galaxies

Pitch angle variations in spiral galaxies

A Consistent Set of Empirical Scaling Relations for Spiral Galaxies: The (v_max, M_oM)–(σ₀, M_BH, ϕ) Relations

Stellar Orbital Studies in Normal Spiral Galaxies. I. Restrictions to the Pitch Angle

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Pitch angles of distant spiral galaxies

Cited by 15 publications

References 21 publications

Pitch angle variations in spiral galaxies

Pitch angle variations in spiral galaxies

A Consistent Set of Empirical Scaling Relations for Spiral Galaxies: The (vmax, MoM)–(σ0, MBH, ϕ) Relations

Stellar Orbital Studies in Normal Spiral Galaxies. I. Restrictions to the Pitch Angle

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A Consistent Set of Empirical Scaling Relations for Spiral Galaxies: The (v_max, M_oM)–(σ₀, M_BH, ϕ) Relations