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Journal articles on the topic 'Galaxy: general'

Author: Grafiati

Published: 4 June 2021

Last updated: 26 July 2025

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1

Wang, Qingqing, Xin Ren, Bo Wang, Yi-Fu Cai, Wentao Luo, and Emmanuel N. Saridakis. "Galaxy–Galaxy Lensing Data: f(T) Gravity Challenges General Relativity." Astrophysical Journal 969, no. 2 (2024): 119. http://dx.doi.org/10.3847/1538-4357/ad47c0.

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Abstract We use galaxy–galaxy lensing data to test general relativity and f(T) gravity at galaxy scales. We consider an exact spherically symmetric solution of f(T) theory, which is obtained from an approximate quadratic correction, and thus it is expected to hold for every realistic deviation from general relativity. Quantifying the deviation by a single parameter Q, and following the post-Newtonian approximation, we obtain the corresponding deviation in the gravitational potential, shear component, and effective excess surface density profile. We used five stellar mass samples and divided th

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2

Martínez-González, E., and J. L. Sanz. "The General Galaxy Luminosity Function." Symposium - International Astronomical Union 130 (1988): 582. http://dx.doi.org/10.1017/s007418090013709x.

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The general luminosity function of galaxies is believed to be well represented by the Schechter function with exponent α ≃ −1 and L* ≃ 1010L⊙, but with a wide range of variation from one sample to another. This function decreases exponentially at high luminosities and has a power law behaviour increasing towards low luminosities with no present evidence of turn over or cut-off.

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3

Grimm, Nastassia, Fulvio Scaccabarozzi, Jaiyul Yoo, Sang Gyu Biern, and Jinn-Ouk Gong. "Galaxy power spectrum in general relativity." Journal of Cosmology and Astroparticle Physics 2020, no. 11 (2020): 064. http://dx.doi.org/10.1088/1475-7516/2020/11/064.

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4

Smith, Keith T. "Testing General Relativity on galaxy scales." Science 360, no. 6395 (2018): 1310.8–1311. http://dx.doi.org/10.1126/science.360.6395.1310-h.

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5

Yoo, Jaiyul. "Incompatibility of standard galaxy bias models in general relativity." Journal of Cosmology and Astroparticle Physics 2023, no. 10 (2023): 054. http://dx.doi.org/10.1088/1475-7516/2023/10/054.

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Abstract The standard model for galaxy bias is built in a Newtonian framework, and several attempts have been made in the past to put it in a relativistic framework. The focus of past works was, however, to use the same Newtonian formulation, but to provide its interpretation in a relativistic framework by either fixing a gauge condition or transforming to a local coordinate system. Here we demonstrate that these reverse-engineered approaches do not respect the diffeomorphism symmetry in general relativity, and we need to develop a covariant model of galaxy bias that is diffeomorphism compatib

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6

Andrianomena, Sambatra, Camille Bonvin, David Bacon, et al. "Testing general relativity with the Doppler magnification effect." Monthly Notices of the Royal Astronomical Society 488, no. 3 (2019): 3759–71. http://dx.doi.org/10.1093/mnras/stz1905.

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ABSTRACT The apparent sizes and brightnesses of galaxies are correlated in a dipolar pattern around matter overdensities in redshift space, appearing larger on their near side and smaller on their far side. The opposite effect occurs for galaxies around an underdense region. These patterns of apparent magnification induce dipole and higher multipole terms in the cross-correlation of galaxy number density fluctuations with galaxy size/brightness (which is sensitive to the convergence field). This provides a means of directly measuring peculiar velocity statistics at low and intermediate redshif

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7

Raccanelli, Alvise, Francesco Montanari, Daniele Bertacca, Olivier Doré, and Ruth Durrer. "Cosmological measurements with general relativistic galaxy correlations." Journal of Cosmology and Astroparticle Physics 2016, no. 05 (2016): 009. http://dx.doi.org/10.1088/1475-7516/2016/05/009.

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8

Anosova, J., S. Iyer, and R. K. Varma. "Clusters and Voids in General Galaxy Field." Symposium - International Astronomical Union 168 (1996): 523–24. http://dx.doi.org/10.1017/s0074180900110563.

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In our previous works (Anosova 1987, Anosova, Iyer, Varma 1994), we developed a new method for determination of the structure of a clustered distribution. In this work, we apply this method studying the observed distribution of galaxies in the Universe.

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9

Eyer, L. "Understanding the Galaxy." Proceedings of the International Astronomical Union 14, S339 (2017): 50–55. http://dx.doi.org/10.1017/s174392131800220x.

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AbstractThis general overview of our understanding of the Galaxy followed the lines of its main structures (halo, disc, bulge/bar) and emphasized some time-domain astronomy contributions. On the one hand the distance and tangential motions of the stars are essential to that understanding, and are obtained through multi-epoch surveys. On the other hand the chemistry of the stars and their radial velocities are also key elements for mapping the Galactic (sub-)structures, and unravelling their history and evolution. Contemporary surveys are revolutionizing our view of the Milky Way and of galaxie

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10

Zhdanov, V. I. "The General Relativistic Potential of Astrometric Studies at Microarcsecond Level." Symposium - International Astronomical Union 166 (1995): 295–300. http://dx.doi.org/10.1017/s0074180900228234.

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The relativistic effects in positioning of distant objects at microarcsecond level are studied. The main points are: statistics of random variations of the image position of a distant radiation source due to the gravitational field of moving stars, motion of the image due to individual invisible gravitators, and possibilities to obtain information on their masses and velocities. The gravitators shifting the object image may be stars of our Galaxy or of a lensing galaxy.

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11

Saburova, A. S., A. V. Kasparova, I. Yu Katkov, D. V. Bizyaev, and I. V. Chilingarian. "On the general structure of giant low surface brightness galaxy Malin 2." Proceedings of the International Astronomical Union 8, S295 (2012): 236. http://dx.doi.org/10.1017/s1743921313004900.

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AbstractWe carried out the multicolor surface photometry in BVR and griz filters parallel with stellar kinematic measurements from the long slit spectra for the low surface brightness galaxy Malin 2. The use of the multicolor surface photometry as well as the available HI rotation curve allowed us to construct the mass distribution model of the galaxy. Photometrical and dynamical mass estimates agree with the dark halo mass fraction of about 70% within four disc radial scalelengths (~ 70 kpc). We used our dynamical model to obtain radial profiles of the equilibrium disc volume density and gas

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12

Brand, J., and J. G. A. Wouterloot. "Far-Outer Galaxy Molecular Clouds." Symposium - International Astronomical Union 169 (1996): 561–66. http://dx.doi.org/10.1017/s0074180900230337.

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The outer Galaxy (defined as those parts of the Galaxy with galactocentric distances R>R0=8.5 kpc) in general and particularly the outermost regions (R ≳ 16 kpc; the far-outer Galaxy or FOG) has not received the attention that has been dedicated to the inner Galaxy and the solar neighbourhood.

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13

Castorina, Emanuele, and Enea Di Dio. "The observed galaxy power spectrum in General Relativity." Journal of Cosmology and Astroparticle Physics 2022, no. 01 (2022): 061. http://dx.doi.org/10.1088/1475-7516/2022/01/061.

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Abstract Measurements of the clustering of galaxies in Fourier space, and at low wavenumbers, offer a window into the early Universe via the possible presence of scale dependent bias generated by Primordial Non Gaussianites. On such large scales a Newtonian treatment of density perturbations might not be sufficient to describe the measurements, and a fully relativistic calculation should be employed. The interpretation of the data is thus further complicated by the fact that relativistic effects break statistical homogeneity and isotropy and are potentially divergent in the Infra-Red (IR). In

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14

Scaccabarozzi, Fulvio, Jaiyul Yoo, and Sang Gyu Biern. "Galaxy two-point correlation function in general relativity." Journal of Cosmology and Astroparticle Physics 2018, no. 10 (2018): 024. http://dx.doi.org/10.1088/1475-7516/2018/10/024.

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15

Hojman, Roberto, Leda Pena, and Nelson Zamorano. "A general relativistic hydrostatic model for a galaxy." Astrophysical Journal 411 (July 1993): 541. http://dx.doi.org/10.1086/172856.

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16

Shiga, David. "Ghostly Galaxy." Science News 167, no. 9 (2005): 131. http://dx.doi.org/10.2307/4015891.

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17

Moraes, Bruno Azevedo Lemos. "Galaxy surveys." Cadernos de Astronomia 5, no. 1 (2024): 39–65. http://dx.doi.org/10.47456/cad.astro.v5n1.43769.

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Neste artigo, abordamos o desenvolvimento dos mapeamentos de galáxias e a sua importância para a astrofísica extragaláctica e para a cosmologia. Acompanhando a evolução dos telescópios, instrumentos e técnicas de observação astronômica desde o século XIX, discutimos como os avanços tecnológicos permitiram desvelar propriedades fundamentais do universo, tal como sua dinâmica, composição e sua estrutura em grande escala. Os mapeamentos de galáxias também revelaram a presença de matéria escura em diferentes escalas e seu impacto tanto na topologia da teia cósmica quanto nos processos de formação

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18

Meno, Frank M., and Kassem Awada. "Galaxy Evolution." Physics Essays 12, no. 1 (1999): 106–14. http://dx.doi.org/10.4006/1.3025353.

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19

Courteau, Stéphane, Michele Cappellari, Roelof S. de Jong, et al. "Galaxy masses." Reviews of Modern Physics 86, no. 1 (2014): 47–119. http://dx.doi.org/10.1103/revmodphys.86.47.

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20

Struck, Curtis. "Galaxy collisions." Physics Reports 321, no. 1-3 (1999): 1–137. http://dx.doi.org/10.1016/s0370-1573(99)00030-7.

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21

Longair, Malcolm S., and Matthias Steinmetz. "Galaxy Formation." Physics Today 52, no. 9 (1999): 62. http://dx.doi.org/10.1063/1.882825.

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22

Paturel, G., C. Petit, Ph Prugniel, and R. Garnier. "Galaxy coordinates." Astronomy and Astrophysics Supplement Series 140, no. 1 (1999): 89–92. http://dx.doi.org/10.1051/aas:1999517.

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23

Paturel, G., C. Petit, R. Garnier, and P. Prugniel. "Galaxy coordinates." Astronomy and Astrophysics Supplement Series 144, no. 3 (2000): 475–80. http://dx.doi.org/10.1051/aas:2000345.

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24

Lindholmer, Mikkel O., and Kevin A. Pimbblet. "Redshift measurement through star formation." Astronomy & Astrophysics 629 (August 23, 2019): A7. http://dx.doi.org/10.1051/0004-6361/201833046.

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In this work we use the property that, on average, star formation rate increases with redshift for objects with the same mass – the so called galaxy main sequence – to measure the redshift of galaxy clusters. We use the fact that the general galaxy population forms both a quenched and a star-forming sequence, and we locate these ridges in the SFR–M⋆ plane with galaxies taken from the Sloan Digital Sky Survey in discrete redshift bins. We fitted the evolution of the galaxy main sequence with redshift using a new method and then subsequently apply our method to a suite of X-ray selected galaxy c

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25

Carneiro, Carlos R. M., Cristina Furlanetto, and Ana L. Chies-Santos. "Constraining general relativity at z ∼ 0.299 MUSE Kinematics of SDP.81." Proceedings of the International Astronomical Union 15, S359 (2020): 260–61. http://dx.doi.org/10.1017/s174392132000191x.

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AbstractGeneral Relativity has been successfully tested on small scales. However, precise tests on galactic and larger scales have only recently begun. Moreover, the majority of these tests on large scales are based on the measurements of Hubble constant (H0), which is currently under discussion. Collett et al. (2018) implemented a novel test combining lensing and dynamical mass measurements of a galaxy, which are connected by a γ parameter, and found γ=0.97±0.09, which is consistent with unity, as predicted by GR. We are carrying out this same technique with a second galaxy, SDP.81 at z=0.299

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26

COOPERSTOCK, F. I., and S. TIEU. "GALACTIC DYNAMICS VIA GENERAL RELATIVITY: A COMPILATION AND NEW DEVELOPMENTS." International Journal of Modern Physics A 22, no. 13 (2007): 2293–325. http://dx.doi.org/10.1142/s0217751x0703666x.

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We consider the consequences of applying general relativity to the description of the dynamics of a galaxy, given the observed flattened rotation curves. The galaxy is modeled as a stationary axially symmetric pressure-free fluid. In spite of the weak gravitational field and the nonrelativistic source velocities, the mathematical system is still seen to be nonlinear. It is shown that the rotation curves for various galaxies as examples are consistent with the mass density distributions of the visible matter within essentially flattened disks. This obviates the need for a massive halo of exotic

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27

Suh, Paul K. "Quantum Cosmology Explains the General Galaxy-Black Hole Correlation." International Journal of Astronomy and Astrophysics 02, no. 02 (2012): 101–12. http://dx.doi.org/10.4236/ijaa.2012.22014.

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28

Hartnett, John G. "Spiral Galaxy Rotation Curves Determined from Carmelian General Relativity." International Journal of Theoretical Physics 45, no. 11 (2006): 2118–36. http://dx.doi.org/10.1007/s10773-006-9178-0.

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29

Zeng, Jiqing. "A Symmetric Ring Galaxy Model Explains the Rotation Curve of Galaxies." Applied Physics Research 15, no. 2 (2023): 110. http://dx.doi.org/10.5539/apr.v15n2p110.

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This paper proposes a symmetric ring galaxy (SRG) model based on the general structure of galaxies. Based on this model, we have obtained results that are consistent with the actual observation results of the galaxy rotation curve, thus solving the problem of inconsistency between the observation results of the galaxy rotation curve and the expected results, which has long plagued the astronomical community. This article also analyzes the root causes of the problem of galaxy rotation curves, and finds that the main reason is that people use unrealistic galaxy models and incorrect calculation m

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30

Chen, Yiru. "Examination of Star Formation Rate enhancement in galaxy pairs selected based on data from Illstris TNG." Journal of Physics: Conference Series 2441, no. 1 (2023): 012021. http://dx.doi.org/10.1088/1742-6596/2441/1/012021.

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Abstract Star Formation Rate (SFR) is one of the most important properties of galaxies, which offers a good insight of galaxy evolution. Generally, interactions with the small and large scale environment may affect the SFR of the galaxy. Therefore, an examination of SFR of galaxy pairs is carried out in this paper to investigate the partner galaxy impacts on the evolution process of one galaxy. Compared with isolated galaxies, the SFR of galaxy pairs is enhanced due to interactions with the large scale environment (e.g., the tidal force). This finding confirms that interactions with the large

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31

Lovisari, Lorenzo, Stefano Ettori, Massimo Gaspari, and Paul A. Giles. "Scaling Properties of Galaxy Groups." Universe 7, no. 5 (2021): 139. http://dx.doi.org/10.3390/universe7050139.

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Galaxy groups and poor clusters are more common than rich clusters, and host the largest fraction of matter content in the Universe. Hence, their studies are key to understand the gravitational and thermal evolution of the bulk of the cosmic matter. Moreover, because of their shallower gravitational potential, galaxy groups are systems where non-gravitational processes (e.g., cooling, AGN feedback, star formation) are expected to have a higher impact on the distribution of baryons, and on the general physical properties, than in more massive objects, inducing systematic departures from the exp

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32

ELLIS, RICHARD. "Galaxy Evolution." Annals of the New York Academy of Sciences 688, no. 1 (1993): 207–17. http://dx.doi.org/10.1111/j.1749-6632.1993.tb43897.x.

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33

Vaccari, M. "GAIA Galaxy Survey: A Multi-Colour Galaxy Survey with GAIA." EAS Publications Series 2 (2002): 313–19. http://dx.doi.org/10.1051/eas:2002031.

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34

Conselice, Christopher J. "How do Galaxies get their Baryons?" Proceedings of the International Astronomical Union 6, S277 (2010): 267–72. http://dx.doi.org/10.1017/s1743921311022927.

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AbstractUnderstanding how galaxies obtain baryons, their stars and gas, over cosmic time is traditionally approached in two different ways - theoretically and observationally. In general, observational approaches to galaxy formation include measuring basic galaxy properties, such as luminosities, stellar masses, rotation speeds, star formation rates and how these features evolve through time. Theoretically, cosmologically based models collate the physical effects driving galaxy assembly - mergers of galaxies, accretion of gas, star formation, and feedback, amongst others, to form predictions w

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35

Tchernyshyov, Kirill, Jessica K. Werk, Matthew C. Wilde, et al. "The CGM² Survey: Circumgalactic O vi from Dwarf to Massive Star-forming Galaxies." Astrophysical Journal 927, no. 2 (2022): 147. http://dx.doi.org/10.3847/1538-4357/ac450c.

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Abstract We combine 126 new galaxy-O vi absorber pairs from the CGM2 survey with 123 pairs drawn from the literature to examine the simultaneous dependence of the column density of O vi absorbers (N O VI) on galaxy stellar mass, star-formation rate, and impact parameter. The combined sample consists of 249 galaxy-O vi absorber pairs covering z = 0–0.6, with host galaxy stellar masses M * = 107.8–1011.2 M ⊙ and galaxy-absorber impact parameters R ⊥ = 0–400 proper kiloparsecs. In this work, we focus on the variation of N O VI with galaxy mass and impact parameter among the star-forming galaxies

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36

Vallenari, Antonella. "Unveiling the Galaxy with Gaia." Proceedings of the International Astronomical Union 9, S298 (2013): 253–64. http://dx.doi.org/10.1017/s1743921313006443.

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AbstractThe Gaia Mission due for launch this year will revolutionise our understanding of the formation and evolution of the Milky Way and of the astrophysics in general. This paper reviews the current status of the Mission, and the expected accuracies as derived from instrument performance assessment.

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37

Alexeyev, Stanislav, Boris Latosh, and Vsevolod Echeistov. "Restrictions on Extended Gravity at Galaxy Clusters Scales." EPJ Web of Conferences 191 (2018): 07008. http://dx.doi.org/10.1051/epjconf/201819107008.

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Following [1] we discuss the predictions of Starobinsky model of f(R)-gravity with vanishing cosmological constant at galaxy and galaxy clusters scales. As a result we demonstrate that at the current observational accuracy level there is no significant difference in cut-off radius values for Starobinsky model and general relativity (GR) in the mass range from 109MS un till galaxy clusters ones (1018MS un) that shows the good applicability of GR at these ranges.

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38

Tamrakar, Amit Kumar, and Laxmikant Chaware. "NGC 5216: An interesting galaxy with a sign of merging activity." Journal of Physics: Conference Series 2576, no. 1 (2023): 012013. http://dx.doi.org/10.1088/1742-6596/2576/1/012013.

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Abstract We present results of isophotal shape analysis of an interesting elliptical galaxy NGC 5216 with a clear sign of merging activity with its companion galaxy NGC 5218. We have used r-bands image analysis of the galaxy from Sloan Digital Sky Survey Data Release 9 (i.e. SDSS DR9) to perform bulge-disk decomposition of the light profile of the galaxy. We look for the correlation between systematic departure of isophotes from pure ellipses along the semi-major axis of the galaxies. The contour image of the galaxy clearly indicates that stellar mass exchange is taking place via a star formin

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39

Kreckel, Kathryn, Jacqueline H. van Gorkom, Burcu Beygu, et al. "The Void Galaxy Survey: Galaxy Evolution and Gas Accretion in Voids." Proceedings of the International Astronomical Union 11, S308 (2014): 591–99. http://dx.doi.org/10.1017/s1743921316010644.

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AbstractVoids represent a unique environment for the study of galaxy evolution, as the lower density environment is expected to result in shorter merger histories and slower evolution of galaxies. This provides an ideal opportunity to test theories of galaxy formation and evolution. Imaging of the neutral hydrogen, central in both driving and regulating star formation, directly traces the gas reservoir and can reveal interactions and signs of cold gas accretion. For a new Void Galaxy Survey (VGS), we have carefully selected a sample of 59 galaxies that reside in the deepest underdensities of g

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40

Zarodnyuk, A., E. Trofimova, A. Solovyov, and D. Gradoboev. "Galaxy Clusters Reconstruction." Journal of Physics: Conference Series 1740 (January 2021): 012017. http://dx.doi.org/10.1088/1742-6596/1740/1/012017.

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41

Meno, Frank M., and Kassem Awada. "Galaxy Size Limit." Physics Essays 11, no. 4 (1998): 589–92. http://dx.doi.org/10.4006/1.3025341.

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42

Moskvitch, Katia. "Our wobbly galaxy." Physics World 27, no. 04 (2014): 24–26. http://dx.doi.org/10.1088/2058-7058/27/04/38.

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43

Hodge, Paul, and Gérard De Vaucouleurs. "The Andromeda Galaxy." Physics Today 46, no. 4 (1993): 62. http://dx.doi.org/10.1063/1.2808873.

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44

Band, D. L., D. H. Hartmann, and B. E. Schaefer. "Host galaxy statistics." Astronomy and Astrophysics Supplement Series 138, no. 3 (1999): 481–82. http://dx.doi.org/10.1051/aas:1999319.

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45

Nazri, Nurnabilah, and Adlyka Annuar. "X-ray Sources Population in NGC 1559." Jurnal Kejuruteraan si3, no. 1 (2020): 7–14. http://dx.doi.org/10.17576/jkukm-2020-si3(1)-02.

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We present Chandra observation of the nearby spiral galaxy NGC 1559 to study the X-ray sources population in the galaxy. Based on our analysis, we detect twenty-four X-ray sources in the galaxy, of which six have 0.5–8 keV luminosities exceeding 10<sup>39</sup> erg s<sup>-1</sup>, suggesting that they are possibly ultra-luminous X-ray source (ULX) candidates. The remaining eighteen sources have 0.5–8 keV luminosities below this threshold value, suggesting that they are likely to be X-ray binary candidates. We perform X-ray spectral analysis for the six ULX candidates an

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46

Zenteno, Alfredo. "Galaxy population study of the 26 most massive galaxy clusters within the SPT footprint." Proceedings of the International Astronomical Union 10, S309 (2014): 355. http://dx.doi.org/10.1017/s1743921314010461.

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AbstractWe present optical properties of the 26 most massive galaxy clusters in the South Pole Telescope 2500 sq-deg footprint. We find a general consistency between our results and results found in the literature on samples built with different selection techniques. Most interesting, we find a preference for an evolution in the slope of the Schechter function, α, with its value increasing at higher redshift.

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47

Liu, Xiao-Hui, Zhen-Hua Li, Jing-Zhao Qi, and Xin Zhang. "Galaxy-scale Test of General Relativity with Strong Gravitational Lensing." Astrophysical Journal 927, no. 1 (2022): 28. http://dx.doi.org/10.3847/1538-4357/ac4c3b.

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Abstract Although general relativity (GR) has been precisely tested at the solar system scale, precise tests at a galactic or cosmological scale are still relatively insufficient. Here, in order to test GR at the galactic scale, we use the newly compiled galaxy-scale strong gravitational lensing (SGL) sample to constrain the parameter γ PPN in the parameterized post-Newtonian (PPN) formalism. We employ the Pantheon sample of Type Ia supernova observations to calibrate the distances in the SGL systems using the Gaussian Process method, which avoids the logical problem caused by assuming a cosmo

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48

Umeh, Obinna, Kazuya Koyama, Roy Maartens, Fabian Schmidt, and Chris Clarkson. "General relativistic effects in the galaxy bias at second order." Journal of Cosmology and Astroparticle Physics 2019, no. 05 (2019): 020. http://dx.doi.org/10.1088/1475-7516/2019/05/020.

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49

Coimbra-Araújo, C. H., and P. S. Letelier. "A general relativistic model of galaxy bulges in GEDi paradigm." Proceedings of the International Astronomical Union 3, S245 (2007): 239–40. http://dx.doi.org/10.1017/s1743921308017766.

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AbstractRecently a new approach was presented where astronomical objects as galaxies and clusters are idealized as self-gravitating systems living in a universe endowed with more than 3+1 dimensions. A such paradigm, named GEDi (Gravitation with Extra Dimensions), may solve exactly the missing mass problem for rotation curves of galaxies or gravitational lensing of clusters with no dark matter particles. Here we present an introductory discussion about the construction of a real galaxy using a Miyamoto-Nagai solution for isotropical coordinates to mimic spiral galaxies with bulges.

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50

Bertacca, Daniele, Nicola Bartolo, Marco Bruni, et al. "Galaxy bias and gauges at second order in general relativity." Classical and Quantum Gravity 32, no. 17 (2015): 175019. http://dx.doi.org/10.1088/0264-9381/32/17/175019.

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