The Tully–Fisher relation for flat galaxies

Макаров, Д. И.; Zaitseva, Natalia A.; Bizyaev, Dmitry

doi:10.1093/mnras/sty1629

Cited by 8 publications

(6 citation statements)

References 62 publications

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“…There have been suggestions to reduce the dispersion in the TFR by including additional parameters such as type, color, or H I-to-stellar content (Rubin et al 1985;Giovanelli et al 1997;Makarov et al 2018). In this spirit, Masters et al (2006) fit the TFR at the I band for early-and late-type spirals separately.…”

Section: Tfr With Additional Parametersmentioning

confidence: 99%

Cosmicflows-4: The Calibration of Optical and Infrared Tully–Fisher Relations

Kourkchi

Tully

Anand

et al. 2020

ApJ

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This study is a part of the Cosmicflows-4 project with the aim of measuring the distances of more than ∼10,000 spiral galaxies in the local universe up to ∼15,000 km s 1 . New H I line width information has come primarily from the Arecibo Legacy Fast ALFA Survey. Photometry of our sample galaxies has been carried out in optical (SDSS u, g, r, i, and z) and infrared (WISE W1 and W2) bands. Inclinations have been determined using an online graphical interface accessible to a collaboration of citizen scientists. Galaxy distances are measured based on the correlation between the rotation rate of spirals and their absolute luminosity, known as the Tully-Fisher relation (TFR). In this study, we present the calibration of the TFR using a subsample of ∼600 spirals located in 20 galaxy clusters. Correlations among such observables as color, surface brightness, and relative H I content are explored in an attempt to reduce the scatter about the TFR with the goal of obtaining more accurate distances. A preliminary determination of the Hubble constant from the distances and velocities of the calibrator clusters is H 0 =76.0±1.1(stat.)±2.3(sys.)km s −1 Mpc −1 .

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Section: Tfr With Additional Parametersmentioning

confidence: 99%

Cosmicflows-4: The Calibration of Optical and Infrared Tully–Fisher Relations

Kourkchi

Tully

Anand

et al. 2020

ApJ

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“…the recent proceedings [47] for the galactic angular momentum paradox: How is it possible that spiral galaxies (originating from small random fluctuations in a hot homogeneous and isotropic universe) rotate so fast? Their orbital speed v satisfies the Tully-Fisher relation v 4 ∼ M , where M is the mass of a spiral galaxy [43].…”

Section: Slight Violation Of the Law Of Conservation Of Energymentioning

confidence: 99%

Do Einstein's Equations Describe Reality Well?

Křížek¹

2019

NNW

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The standard cosmological model that is based on Einstein's equations possesses many paradoxes. Therefore, we take a closer look at the equations themselves, and not only on cosmological scales. In this survey paper, we present 10 significant problems and drawbacks of Einstein's equations investigated by the author. They include their extremely large complexity, non-differentiability of the metric, difficulties with initial and boundary conditions, multiple divisions by zero, excessive extrapolations to cosmological distances leading to mysterious dark matter and dark energy entities, unconvincing relativistic tests, the absence of aberration effects, and scale non-invariance. We also discuss a slight violation of the laws of conservation of energy and of momentum.

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“…Their edge-on orientation eliminates one of the biggest uncertainties in the Tully-Fisher relation -the inclination correction. It allows us to estimate the distance modulus to flat galaxies with an accuracy of 0.32 mag (Makarov et al 2018). Additionally, bulgeless flat galaxies (also called simple discs) are an ideal tool to verify different galaxy formation scenarios that challenge the existing evolution theories of disc survival in a merger-dominated Universe (Kautsch 2009a).…”

Section: Introductionmentioning

confidence: 99%

The Edge-on Galaxies in the Pan-STARRS survey (EGIPS)

Makarov,

Savchenko,

Mosenkov

et al. 2022

Preprint

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We present a catalogue of 16,551 edge-on galaxies created using the public DR2 data of the Pan-STARRS survey. The catalogue covers the three quarters of the sky above Dec. = −30 • . The galaxies were selected using a convolutional neural network, trained on a sample of edge-on galaxies identified earlier in the SDSS survey. This approach allows us to dramatically improve the quality of the candidate selection and perform a thorough visual inspection in a reasonable amount of time. The catalogue provides homogeneous information on astrometry, SE photometry, and non-parametric morphological statistics of the galaxies. The photometry is reliably for objects in the 13.8-17.4 𝑟-band magnitude range. According to the HyperLeda database, redshifts are known for about 63 percent of the galaxies in the catalogue. Our sample is well separated into the red sequence and blue cloud galaxy populations. The edge-on galaxies of the red sequence are systematically Δ(𝑔 − 𝑖) ≈ 0.1 mag redder than galaxies oriented at an arbitrary angle to the observer. We found a variation of the galaxy thickness with the galaxy colour. The red sequence galaxies are thicker than the galaxies of the blue cloud. In the blue cloud, on average, thinner galaxies turn out to be bluer. In the future, based on this catalogue it is intended to explore the three-dimensional structure of galaxies of different morphologies, as well as to study the scaling relations for discs and bulges.

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The Tully–Fisher relation for flat galaxies

Cited by 8 publications

References 62 publications

Cosmicflows-4: The Calibration of Optical and Infrared Tully–Fisher Relations

Cosmicflows-4: The Calibration of Optical and Infrared Tully–Fisher Relations

Do Einstein's Equations Describe Reality Well?

The Edge-on Galaxies in the Pan-STARRS survey (EGIPS)

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