Relevant bibliographies by topics / Radial Tully-Fisher relation

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Academic literature on the topic 'Radial Tully-Fisher relation'

Author: Grafiati
Published: 14 March 2023

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Journal articles on the topic "Radial Tully-Fisher relation"

1

Yegorova, Irina A., and Paolo Salucci. "The radial Tully-Fisher relation for spiral galaxies - I." Monthly Notices of the Royal Astronomical Society 377, no. 2 (May 11, 2007): 507–15. http://dx.doi.org/10.1111/j.1365-2966.2007.11637.x.

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2

Wheeler, Coral, Philip F. Hopkins, and Olivier Doré. "The Radial Acceleration Relation Is a Natural Consequence of the Baryonic Tully–Fisher Relation." Astrophysical Journal 882, no. 1 (August 30, 2019): 46. http://dx.doi.org/10.3847/1538-4357/ab311b.

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Paranjape, Aseem, and Ravi K. Sheth. "The radial acceleration relation in a ΛCDM universe." Monthly Notices of the Royal Astronomical Society 507, no. 1 (July 24, 2021): 632–50. http://dx.doi.org/10.1093/mnras/stab2141.

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ABSTRACT We study the radial acceleration relation (RAR) between the total (atot) and baryonic (abary) centripetal acceleration profiles of central galaxies in the cold dark matter (CDM) paradigm. We analytically show that the RAR is intimately connected with the physics of the quasi-adiabatic relaxation of dark matter in the presence of baryons in deep potential wells. This cleanly demonstrates how the mean RAR and its scatter emerge in the low-acceleration regime ($10^{-12}{\rm \, m\, s}^{-2}\lesssim a_{\rm bary}\lesssim 10^{-10}{\rm \, m\, s}^{-2}$) from an interplay between baryonic feedback processes and the distribution of CDM in dark haloes. Our framework allows us to go further and study both higher and lower accelerations in detail, using analytical approximations and a realistic mock catalogue of ${\sim}342\, 000$ low-redshift central galaxies with Mr ≤ −19. We show that, while the RAR in the baryon-dominated high-acceleration regime ($a_{\rm bary}\gtrsim 10^{-10}{\rm \, m\, s}^{-2}$) is very sensitive to details of the relaxation physics, a simple ‘baryonification’ prescription matching the relaxation results of hydrodynamical CDM simulations is remarkably successful in reproducing the observed RAR without any tuning. And in the (currently unobserved) ultra-low-acceleration regime ($a_{\rm bary}\lesssim 10^{-12}{\rm \, m\, s}^{-2}$), the RAR is sensitive to the abundance of diffuse gas in the halo outskirts, with our default model predicting a distinctive break from a simple power-law-like relation for H i-deficient, diffuse gas-rich centrals. Our mocks also show that the RAR provides more robust, testable predictions of the ΛCDM paradigm at galactic scales, with implications for alternative gravity theories than the baryonic Tully–Fisher relation.
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van der Kruit, P. C. "The Surface Brightness of Our Galaxy and Other Spirals." Symposium - International Astronomical Union 139 (1990): 85–97. http://dx.doi.org/10.1017/s0074180900240424.

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In this review I discuss some aspects of the luminosity distributions in our Galaxy and external spiral galaxies. The major conclusions are the following: (1) the radial scale length of the luminosity distribution in the disk of our Galaxy is 5.0 ± 0.5 kpc, (2) on this basis the Hubble constant needs to be at most 65 ± 10 km s−1 Mpc−1, if our Galaxy and M31 are among the largest spirals, as the Fisher-Tully relation suggests, (3) the probable Hubble type of the Galaxy is SbI–II, (4) the bi-modal distribution function of face-on, central surface brightness μ0 and radial scale length h of spirals shows a preferred value for μ0 of about 22 B-mag arcsec2 and a distribution of h that declines with one e-folding per kpc, (5) the Galaxy is a normal, fairly large Sb galaxy, and (6) galaxies similar to our own in terms of large-scale, nonmorphological properties are NGC 891 and NGC 5033.
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Karachentsev, Igor D., and E. I. Kaisina. "Dwarf Galaxies in the Local Volume." Proceedings of the International Astronomical Union 14, S344 (August 2018): 381–83. http://dx.doi.org/10.1017/s1743921318005975.

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AbstractThe Updated Nearby Galaxy Catalog (=UNGC) of 1047 Local Volume (=LV) galaxies, situated within a distance of 11 Mpc, contains 870 dwarfs, i.e. 5/6 of the sample. Almost 40% of them have accurate distances measured with Hubble Space Telescope. Most of the LV dwarfs have been observed in HI and Hα emission lines, as well in far-ultraviolet with GALEX. We present basic properties of the LV dwarfs, their HI -mass content and star-formation rate in different local environments. We discuss a baryonic Tully-Fisher relation for the LV dwarfs, and apply it to determine TF -distances for several hundreds local galaxies. The accurate distances and radial velocities of the LV dwarfs are used by us to trace dark matter distribution within 11 Mpc. We discuss also does the Local Group may be treated as a typical or uncommon representative of the LV population.
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Sharina, M. E., V. E. Karachentseva, and D. I. Makarov. "Multiparametric scaling relations for dwarf irregular galaxies in different environments." Proceedings of the International Astronomical Union 8, S289 (August 2012): 236–39. http://dx.doi.org/10.1017/s1743921312021485.

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AbstractWe study the correlations of rotation velocity and absolute magnitude with surface brightness for low surface brightness dwarf irregular galaxies (dIrrs). We find that isolated objects contribute most to the scatter in the Tully–Fisher relation (TFR). Excluding these extreme cases, we develop a three-parameter (luminosity, Hi line width at 20% of peak flux level, i.e., W20, effective surface brightness) TFR for 60 dIrrs (with revised Hubble type T > 8) in the Local Volume (LV) with Cepheid and tip-of-the-red-giant-branch distance measurements. The relation is applied to galaxies of the same morphological type with radial velocities vLG ≤ 3500 km s−1 in the Local Supercluster. We obtained surface photometry and determined structural parameters using sdss images. The rotational velocities and derived photometric parameters for most galaxies in small groups agree well with those corresponding to the three-parameter TFR. However, isolated galaxies appear to have systematically lower surface brightnesses and longer scale lengths for the same luminosity than galaxies in small groups. This may indicate on average twice larger Hi-to-optical disk size ratios for our sample of isolated dIrrs, because their Hi surface densities calculated using the optical diameters look normal.
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7

Parnovsky, S. "Impact of the statistical effects on the Hubble constant value obtained from velocities of galaxies." Bulletin of Taras Shevchenko National University of Kyiv. Astronomy, no. 61 (2020): 20–22. http://dx.doi.org/10.17721/btsnua.2020.61.20-22.

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We can obtain the Hubble constant value for the late Universe from the sample of radial velocities of galaxies and independent estimations of distances to them based on any statistical relation such as Cepheid variables, Tully-Fisher relation etc. Usually, the method of least squares is used when processing such data. However, the value of the Hubble constant is somewhat underestimated due to a statistical effect similar to the wellknown Malmquist bias. The main source of underestimation is associated with the deviation of the distances determined from the statistical dependence from their true values. The decrease of obtained Hubble constant value is about 5% for an error in the distance estimation of 20% and about 9% with an error of 30%. This impact cannot explain the recently discovered tensions between the values of Hubble constant obtained from the early and the late Universe. The estimation H0 = 67.4 km/s/Mpc obtained from observations in the recombination era account for about 92% of the average of the estimations based on observations of not very distant objects H0 = 73.3 km/s/ Mpc. Indeed, the described effect leads to underestimation of the largest of these values.
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Vasylenko, M., and Yu Kudrya. "Dipole bulk velocity based on new data sample of galaxies from the catalogue 2MFGC." Advances in Astronomy and Space Physics 7, no. 1-2 (2017): 6–11. http://dx.doi.org/10.17721/2227-1481.7.6-11.

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We use the 2MFGC catalogue for investigation of large-scale flows on the basis of the Tully-Fisher relation (TFR). The catalogue contains 18020 galaxies selected from the extended sources of the infrared sky survey 2MASS XSC. The majority of galaxies in the catalogue are spiral galaxies of late morphological types whose discs are visible almost from the edge. For more than a decade of the catalogue usage, the number of galaxies in HyperLEDA database with the measured radial velocities and rotational velocities (that are necessary to construct the TFR) has been increased by about 17%. In this paper, an updated working sample of 2MFGC galaxies is presented and earlier results are revised taking into account new data. We have confined ourselves to comparison of only the "old" and "new" parameters of the dipole component of the velocity field. The dipole bulk motion of galaxies of this sample with respect to cosmic microwave radiation is characterised by a velocity of V=264±36 km/s in the direction l=308°±8°, b=-16°±6°.
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Gómez-López, J. A., P. Amram, B. Epinat, A. Boselli, M. Rosado, M. Marcelin, S. Boissier, J. L. Gach, M. Sánchez-Cruces, and M. M. Sardaneta. "An Hα kinematic survey of the Herschel Reference Survey." Astronomy & Astrophysics 631 (October 22, 2019): A71. http://dx.doi.org/10.1051/0004-6361/201935869.

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Aims. We present new 2D high resolution Fabry–Perot spectroscopic observations of 152 star-forming galaxies that are part of the Herschel Reference Survey (HRS), which is a complete K-band selected, volume-limited sample of nearby galaxies that spans a wide range of stellar mass and morphological types. Methods. By using improved data reduction techniques, that provide adaptive binning based on Voronoi tessellation, and using large field-of-view observations, we derived high spectral resolution (R > 10 000) Hα datacubes from which we computed Hα maps and radial 2D velocity fields that are based on several of thousand independent measurements. A robust method based on such fields allowed us to accurately compute rotation curves and kinematical parameters, for which uncertainties are calculated using a method based on the power spectrum of the residual velocity fields. Results. We checked the consistency of the rotation curves by comparing our maximum rotational velocities to those derived from H I data, and by computing the i-band, NIR, stellar, and baryonic Tully-Fisher relations. We used this set of kinematical data combined with those available at other frequencies to study, for the first time, the relation between the dynamical and the total baryonic mass (stars, atomic and molecular gas, metals, and dust) and to derive the baryonic and dynamical main sequence on a representative sample of the local universe.
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Cesare, Valentina. "Dark Coincidences: Small-Scale Solutions with Refracted Gravity and MOND." Universe 9, no. 1 (January 16, 2023): 56. http://dx.doi.org/10.3390/universe9010056.

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General relativity and its Newtonian weak field limit are not sufficient to explain the observed phenomenology in the Universe, from the formation of large-scale structures to the dynamics of galaxies, with the only presence of baryonic matter. The most investigated cosmological model, the ΛCDM, accounts for the majority of observations by introducing two dark components, dark energy and dark matter, which represent ∼95% of the mass-energy budget of the Universe. Nevertheless, the ΛCDM model faces important challenges on the scale of galaxies. For example, some very tight relations between the properties of dark and baryonic matters in disk galaxies, such as the baryonic Tully–Fisher relation (BTFR), the mass discrepancy–acceleration relation (MDAR), and the radial acceleration relation (RAR), which see the emergence of the acceleration scale a0≃1.2×10−10 m s−2, cannot be intuitively explained by the CDM paradigm, where cosmic structures form through a stochastic merging process. An even more outstanding coincidence is due to the fact that the acceleration scale a0, emerging from galaxy dynamics, also seems to be related to the cosmological constant Λ. Another challenge is provided by dwarf galaxies, which are darker than what is expected in their innermost regions. These pieces of evidence can be more naturally explained, or sometimes even predicted, by modified theories of gravity, that do not introduce any dark fluid. I illustrate possible solutions to these problems with the modified theory of gravity MOND, which departs from Newtonian gravity for accelerations smaller than a0, and with Refracted Gravity, a novel classical theory of gravity introduced in 2016, where the modification of the law of gravity is instead regulated by a density scale.
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Conference papers on the topic "Radial Tully-Fisher relation"

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Saburova, A., I. Chilingarian, A. Kasparova, O. Sil’chenko, I. Katkov, K. Grishin, and R. Uklein. "Observational insights on the formation scenarios of giant low surface brightness galaxies." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.161.

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Giant low surface brightness galaxies (gLSBGs) with the disk radii of up to 130 kpc represent a challenge for currentlyaccepted theories of galaxy formation and evolution, because it is difficult to build-up such large dynamically cold systemsvia mergers preserving extended disks. We summarize the in-depth study of the sample of 7 gLSBGs based on the resultsof the performed spectral long-slit observations at BTA SAO RAS, surface photometry and Hi data available in literature.Our study revealed that most gLSBGs do not deviate from the Tully-Fisher relation. We discovered compact elliptical (cE)satellites in 2 out of these 7 galaxies. Provided the low statistical frequencies of gLSBGs and cEs, the chance alignment isimprobable, so it can indicate that gLSBGs and cE are evolutionary connected and gives evidence in favor of the majormerger formation scenario. Other formation paths of gLSBGs are also discussed.
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