On the method of spiral arms monotony to determine the orientation angles of galaxies

Poltorak, S. G.; Fridman, A. M.

doi:10.1134/s1063772907060042

Cited by 6 publications

(4 citation statements)

References 5 publications

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“…In this work we have used the MSA method (Poltorak & Fridman 2007, Fridman & Poltorak 2010. This method allows us to obtain values of both inclination and position angle.…”

Section: Inclinationmentioning

confidence: 99%

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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“…In this work we have used the MSA method (Poltorak & Fridman 2007, Fridman & Poltorak 2010. This method allows us to obtain values of both inclination and position angle.…”

Section: Inclinationmentioning

confidence: 99%

Pitch angle variations in spiral galaxies

Савченко¹,

Решетников²

2013

Monthly Notices of the Royal Astronomical Society

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“…It is interesting to note that the act of measuring pitch angle itself also yields a good indication of the true inclination angle of a galaxy(Poltorak & Fridman 2007).MNRAS 000, 1-18 (2017)…”

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confidence: 99%

Updating the (supermassive black hole mass)–(spiral arm pitch angle) relation: a strong correlation for galaxies with pseudobulges

Davis

Graham

Seigar

2017

Monthly Notices of the Royal Astronomical Society

137

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We have conducted an image analysis of the (current) full sample of 44 spiral galaxies with directly measured supermassive black hole (SMBH) masses, M BH , to determine each galaxy's logarithmic spiral arm pitch angle, φ. For predicting black hole masses, we have derived the relation:The total root mean square scatter associated with this relation is 0.43 dex in the log M BH direction, with an intrinsic scatter of 0.33 ± 0.08 dex. The M BH -φ relation is therefore at least as accurate at predicting SMBH masses in spiral galaxies as the other known relations. By definition, the existence of an M BH -φ relation demands that the SMBH mass must correlate with the galaxy discs in some manner. Moreover, with the majority of our sample (37 of 44) classified in the literature as having a pseudobulge morphology, we additionally reveal that the SMBH mass correlates with the largescale spiral pattern and thus the discs of galaxies hosting pseudobulges. Furthermore, given that the M BH -φ relation is capable of estimating black hole masses in bulgeless spiral galaxies, it therefore has great promise for predicting which galaxies may harbour intermediate-mass black holes (IMBHs, M BH < 10 5 M ). Extrapolating from the current relation, we predict that galaxies with |φ| ≥ 26. • 7 should possess IMBHs.

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“…In this paper, we decided to use the relatively new method of spiral-arm monotony (SAM; Poltorak and Fridman 2007;Fridman and Poltorak 2010). This method is based on the assumption that every spiral arm is a monotonic function, i.e., following along the spiral from the galaxy center to the periphery, the radius must increase monotonically ( dr dφ > 0, where r is the distance from a point in the spiral arm to the galaxy center and φ is the azimuthal angle).…”

Section: Determining the Orientation Of Galaxy Disksmentioning

confidence: 99%

Pitch angles of distant spiral galaxies

Савченко

Решетников

2011

Astron. Lett.

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We have studied the pitch angles of spiral arms for 31 distant galaxies at z~0.7 from three Hubble Deep Fields (HDF-N, HDF-S, HUDF). Using the pitch angle - rotation velocity relation calibrated from nearby galaxies, we have estimated the rotation velocities of galaxies from the deep fields. These estimates have a low accuracy (~50 km/s), but they allow low-mass and giant galaxies to be distinguished. The Tully-Fisher relation constructed using our velocity estimates shows satisfactory agreement with the actually observed relations for distant galaxies and provides evidence for the luminosity evolution of spiral galaxies.Comment: 9 pages, 6 figure

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On the method of spiral arms monotony to determine the orientation angles of galaxies

Cited by 6 publications

References 5 publications

Pitch angle variations in spiral galaxies

Pitch angle variations in spiral galaxies

Updating the (supermassive black hole mass)–(spiral arm pitch angle) relation: a strong correlation for galaxies with pseudobulges

Pitch angles of distant spiral galaxies

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