Journal articles: 'Galaxy evolution'

1

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

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

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Ziegler, Bodo. "Galaxy Evolution." Astronomische Nachrichten 325, S1 (August 2004): 39–46. http://dx.doi.org/10.1002/asna.200485066.

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Ziegler, Bodo. "Galaxy Evolution." Astronomische Nachrichten 324, S2 (June 30, 2003): 35–43. http://dx.doi.org/10.1002/asna.200385007.

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Gardner, J. P. "Galaxy Evolution from Deep Galaxy Counts." Symposium - International Astronomical Union 164 (1995): 311–19. http://dx.doi.org/10.1017/s007418090010871x.

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We present deep galaxy number counts and colours of K – band selected galaxy surveys. We argue that primeval galaxies are present within the survey data, but have remained unidentified. There are few objects with the colours of an L∗ elliptical galaxy at a redshift of z ≈ 1, in contradiction to standard luminosity evolution models. We present K – band photometry of the objects in a spectroscopic redshift survey selected at 21 < B < 22.5. The absolute K magnitudes of the galaxies are consistent with the no-evolution or pure luminosity evolution models. The excess faint blue galaxies seen in the B – band number counts at intermediate magnitudes are a result of a low normalization, and do not dominate the population until B ≈ 25. Extreme merging or excess dwarf models are not needed at z < 1.

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Saghiha, H., S. Hilbert, P. Schneider, and P. Simon. "Galaxy-galaxy(-galaxy) lensing as a sensitive probe of galaxy evolution." Astronomy & Astrophysics 547 (October 31, 2012): A77. http://dx.doi.org/10.1051/0004-6361/201219358.

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Wardlow, Julie. "Speedy galaxy evolution." Science 371, no. 6530 (February 11, 2021): 674–75. http://dx.doi.org/10.1126/science.abg2907.

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Kodama, Tadayuki, Yusei Koyama, Masao Hayashi, and Tadaki Ken-ichi. "PANORAMIC VIEWS OF GALAXY CLUSTER EVOLUTION: GALAXY ECOLOGY." Publications of The Korean Astronomical Society 25, no. 3 (September 30, 2010): 101–5. http://dx.doi.org/10.5303/pkas.2010.25.3.101.

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Fioc, Michel. "UV to NIR Galaxy Evolution and Galaxy Counts." Symposium - International Astronomical Union 171 (1996): 373. http://dx.doi.org/10.1017/s0074180900232920.

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We have improved in the NIR the model of galaxy evolution developed by Guiderdoni & Rocca-Volmerange (A&A 186, 1) in the UV and the visible, allowing thus a multispectral analysis of the evolution of galaxies and of faint galaxy counts. Since evolutionnary effects should be low in the near-infrared, cosmological ones might be put in evidence.

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Fraix-Burnet, Didier, Philippe Choler, Emmanuel J. P. Douzery, and Anne Verhamme. "Astrocladistics: A Phylogenetic Analysis of Galaxy Evolution I. Character Evolutions and Galaxy Histories." Journal of Classification 23, no. 1 (June 2006): 31–56. http://dx.doi.org/10.1007/s00357-006-0003-5.

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Mao, S., and C. S. Kochanek. "Limits on galaxy evolution." Monthly Notices of the Royal Astronomical Society 268, no. 2 (May 15, 1994): 569–80. http://dx.doi.org/10.1093/mnras/268.2.569.

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Henry, J. Patrick. "Evolution of galaxy clusters." Nature 377, no. 6544 (September 1995): 13. http://dx.doi.org/10.1038/377013a0.

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13

Cowie, Lennox L. "Galaxy formation and evolution." Physica Scripta T36 (January 1, 1991): 102–7. http://dx.doi.org/10.1088/0031-8949/1991/t36/011.

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Muldrew, Stuart I., Nina A. Hatch, and Elizabeth A. Cooke. "Galaxy evolution in protoclusters." Monthly Notices of the Royal Astronomical Society 473, no. 2 (September 25, 2017): 2335–47. http://dx.doi.org/10.1093/mnras/stx2454.

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Bagla, J. S. "Evolution of galaxy clustering." Monthly Notices of the Royal Astronomical Society 299, no. 2 (September 1, 1998): 417–24. http://dx.doi.org/10.1046/j.1365-8711.1998.01788.x.

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Kopylova, F. G., and A. I. Kopylov. "Evolution of galaxy groups." Astrophysical Bulletin 72, no. 2 (April 2017): 100–110. http://dx.doi.org/10.1134/s199034131702002x.

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Nagamine, Kentaro, Naveen Reddy, Emanuele Daddi, and Mark T. Sargent. "Galaxy Formation and Evolution." Space Science Reviews 202, no. 1-4 (July 25, 2016): 79–109. http://dx.doi.org/10.1007/s11214-016-0270-3.

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Gobat, R., and S. E. Hong. "Evolution of galaxy habitability." Astronomy & Astrophysics 592 (August 2016): A96. http://dx.doi.org/10.1051/0004-6361/201628834.

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Mazzei, P., A. Marino, R. Rampazzo, H. Plana, M. Rosado, and L. Arias. "Galaxy evolution in groups." Astronomy & Astrophysics 610 (February 2018): A8. http://dx.doi.org/10.1051/0004-6361/201731182.

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Context. Local Group (LG) analogs (LGAs) are galaxy associations dominated by a few bright spirals reminiscent of the LG. The NGC 3447/NGC 3447A system is a member of the LGG 225 group, a nearby LGA. This system is considered a physical pair composed of an intermediate-luminosity late-type spiral, NGC 3447 itself, and an irregular companion, NGC 3447A, linked by a faint, short filament of matter. A ring-like structure in the NGC 3447 outskirts has been emphasised by Galaxy Evolution Explorer (GALEX) observations. Aims. This work aims to contribute to the study of galaxy evolution in low-density environments, a favourable habitat to highly effective encounters, shedding light on the evolution of the NGC 3447/NGC 3447A system. Methods. We performed a multi-λ analysis of the surface photometry of this system to derive its spectral energy distribution and structural properties using ultraviolet (UV), Swift UVOT, and optical Sloan Digital Sky Survey (SDSS) images complemented with available far-IR observations. We also characterised the velocity field of the pair using two-dimensional Hα kinematical observations of the system obtained with PUMA Fabry-Perot interferometer at the 2.1 m telescope of San Pedro Mártir (Mexico). All these data are used to constrain smooth particle hydrodynamic simulations with chemo-photometric implementation to shed light on the evolution of this system. Results. The luminosity profiles, from UV to optical wavelengths, are all consistent with the presence of a disc extending and including NGC 3447A. The overall velocity field does not emphasise any significant rotation pattern, rather a small velocity gradient between NGC 3447 and NGC 3447A. Our simulation, detached from a large grid explored to best-fit the global properties of the system, suggests that this arises from an encounter between two halos of equal mass. Conclusions. NGC 3447 and NGC 3447A belong to the same halo, NGC 3447A being a substructure of the same disk including NGC 3447. The halo gravitational instability, enhanced by the encounter, fuels a long-lived instability in this dark-matter-dominated disk, driving the observed morphology. The NGC 3447/NGC 3447A system may warn of a new class of “false pairs” and the potential danger of a misunderstanding of such objects in pair surveys that could produce a severe underestimate of the total mass of a system.

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Linke, Laila, Patrick Simon, Peter Schneider, Thomas Erben, Daniel J. Farrow, Catherine Heymans, Hendrik Hildebrandt, et al. "KiDS+VIKING+GAMA: Testing semi-analytic models of galaxy evolution with galaxy–galaxy–galaxy lensing." Astronomy & Astrophysics 640 (August 2020): A59. http://dx.doi.org/10.1051/0004-6361/202038355.

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Context. Several semi-analytic models (SAMs) try to explain how galaxies form, evolve, and interact inside the dark matter large-scale structure. These SAMs can be tested by comparing their predictions for galaxy–galaxy–galaxy lensing (G3L), which is weak gravitational lensing around galaxy pairs, with observations. Aims. We evaluate the SAMs by Henriques et al. (2015, MNRAS, 451, 2663, hereafter H15) and by Lagos et al. (2012, MNRAS, 426, 2142, hereafter L12), which were implemented in the Millennium Run, by comparing their predictions for G3L to observations at smaller scales than previous studies and also for pairs of lens galaxies from different populations. Methods. We compared the G3L signal predicted by the SAMs to measurements in the overlap of the Galaxy And Mass Assembly survey (GAMA), the Kilo-Degree Survey (KiDS), and the VISTA Kilo-degree Infrared Galaxy survey (VIKING) by splitting lens galaxies into two colour and five stellar-mass samples. Using an improved G3L estimator, we measured the three-point correlation of the matter distribution with “mixed lens pairs” with galaxies from different samples, and with “unmixed lens pairs” with galaxies from the same sample. Results. Predictions by the H15 SAM for the G3L signal agree with the observations for all colour-selected samples and all but one stellar-mass-selected sample with 95% confidence. Deviations occur for lenses with stellar masses below 9.5 h−2 M⊙ at scales below 0.2 h−1 Mpc. Predictions by the L12 SAM for stellar-mass selected samples and red galaxies are significantly higher than observed, while the predicted signal for blue galaxy pairs is too low. Conclusions. The L12 SAM predicts more pairs of low stellar mass and red galaxies than the H15 SAM and the observations, as well as fewer pairs of blue galaxies. This difference increases towards the centre of the galaxies’ host halos. Likely explanations are different treatments of environmental effects by the SAMs and different models of the initial mass function. We conclude that G3L provides a stringent test for models of galaxy formation and evolution.

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Caplar, Neven, Simon J. Lilly, and Benny Trakhtenbrot. "AGN EVOLUTION FROM A GALAXY EVOLUTION VIEWPOINT." Astrophysical Journal 811, no. 2 (September 30, 2015): 148. http://dx.doi.org/10.1088/0004-637x/811/2/148.

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22

Poggianti, Bianca M., Rosa Calvi, Daniele Bindoni, Mauro D'Onofrio, Alessia Moretti, Tiziano Valentinuzzi, Giovanni Fasano, et al. "The evolution of galaxy sizes." Proceedings of the International Astronomical Union 8, S295 (August 2012): 151–54. http://dx.doi.org/10.1017/s1743921313004547.

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AbstractWe present a study of galaxy sizes in the local Universe as a function of galaxy environment, comparing clusters and the general field. Galaxies with radii and masses comparable to high-z massive and compact galaxies represent 4.4% of all galaxies more massive than 3 × 1010M⊙ in the field. Such galaxies are 3 times more frequent in clusters than in the field. Most of them are early-type galaxies with intermediate to old stellar populations. There is a trend of smaller radii for older luminosity-weighted ages at fixed galaxy mass. We show the relation between size and luminosity-weighted age for galaxies of different stellar masses and in different environments. We compare with high-z data to quantify the evolution of galaxy sizes. We find that, once the progenitor bias due to the relation between galaxy size and stellar age is removed, the average amount of size evolution of individual galaxies between high- and low-z is mild, of the order of a factor 1.6.

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23

Sahijpal, Sandeep. "Galaxy Formation and Chemical Evolution." International Journal of Astronomy and Astrophysics 04, no. 03 (2014): 491–98. http://dx.doi.org/10.4236/ijaa.2014.43045.

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IM, MVUNGSHIN. "GALAXY EVOLUTION IN DISTANT UNIVERSE." Journal of The Korean Astronomical Society 38, no. 2 (June 1, 2005): 135–40. http://dx.doi.org/10.5303/jkas.2005.38.2.135.

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25

Carlberg, R. G. "Merging and fast galaxy evolution." Astrophysical Journal 399 (November 1992): L31. http://dx.doi.org/10.1086/186599.

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26

Henry, J. Patrick, Ulrich G. Briel, and Hans Böhringer. "The Evolution of Galaxy Clusters." Scientific American 279, no. 6 (December 1998): 52–57. http://dx.doi.org/10.1038/scientificamerican1298-52.

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27

Cowen, R. "Galaxy Evolution: A Multiwavelength View." Science News 147, no. 23 (June 10, 1995): 358. http://dx.doi.org/10.2307/3979239.

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Seo, Hee‐Jong, Daniel J. Eisenstein, and Idit Zehavi. "Passive Evolution of Galaxy Clustering." Astrophysical Journal 681, no. 2 (July 10, 2008): 998–1016. http://dx.doi.org/10.1086/527553.

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29

Peacock, J. A. "The evolution of galaxy clustering." Monthly Notices of the Royal Astronomical Society 284, no. 4 (February 1, 1997): 885–98. http://dx.doi.org/10.1093/mnras/284.4.885.

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Rana, Narayan Chandra. "Chemical Evolution of the Galaxy." Annual Review of Astronomy and Astrophysics 29, no. 1 (September 1991): 129–62. http://dx.doi.org/10.1146/annurev.aa.29.090191.001021.

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Carlberg, R. G., and Stephane Charlot. "Faint galaxy evolution via interactions." Astrophysical Journal 397 (September 1992): 5. http://dx.doi.org/10.1086/171759.

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Poggianti, B. M., and G. Barbaro. "Galaxy Evolution in Distant Clusters." Symposium - International Astronomical Union 171 (1996): 433. http://dx.doi.org/10.1017/s0074180900233512.

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A significant evolution has been detected in intermediate redshift clusters (z < 0.9), first by photometric studies ([1], [2]), which showed an excess of blue objects; subsequent spectroscopic studies revealed anomalies in most of the galaxies, mainly consisting of excessively strong Balmer lines. In order to explain the spectroscopic observations, bursts of star formation superimposed to the traditional scenario of galactic evolution are needed. The analysis of spectral lines and colours by means of an evolutionary synthesis model ([3]), including both the stellar contribution and the emission of the ionized gas, allows in most of the cases the determination of the time elapsed since the end of the burst and the fraction of galactic mass involved in it. In the clusters considered (AC103, AC114, AC118 at z = 0.31, [4]), the theoretical analysis demonstrates that the bursts affect substantial galactic mass fractions, typically 30 % or more. The observations can be equally well reproduced by either elliptical+burst models or by spiral+burst models in which the star formation is truncated at the end of the burst. The analysis of an UV colour such as (1550-V) is proposed as a valid method to distinguish between the two cases for Hδ strong red galaxies.

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Carlberg, R. G. "Quasar evolution via galaxy mergers." Astrophysical Journal 350 (February 1990): 505. http://dx.doi.org/10.1086/168406.

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Bravo-Alfaro, H., C. A. Caretta, C. Lobo, F. Durret, and T. Scott. "Galaxy evolution in Abell 85." Astronomy & Astrophysics 495, no. 2 (November 20, 2008): 379–87. http://dx.doi.org/10.1051/0004-6361:200810731.

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Abraham, R. G., Tammy A. Smecker‐Hane, J. B. Hutchings, R. G. Carlberg, H. K. C. Yee, Erica Ellingson, Simon Morris, J. B. Oke, and Michael Rigler. "Galaxy Evolution in Abell 2390." Astrophysical Journal 471, no. 2 (November 10, 1996): 694–719. http://dx.doi.org/10.1086/177999.

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Reshetnikov, V. P., and N. Ya Sotnikova. "Tidal tails and galaxy evolution." Astronomical & Astrophysical Transactions 20, no. 1 (June 2001): 111–14. http://dx.doi.org/10.1080/10556790108208195.

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Scott, Douglas. "The evolution of galaxy formation." Astronomy & Geophysics 52, no. 6 (November 24, 2011): 6.31–6.33. http://dx.doi.org/10.1111/j.1468-4004.2011.52631.x.

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Hensler, Gerhard, Andi Burkert, Pavel Kroupa, and Elke Schumacher. "Environmental Effects on Galaxy Evolution." Astronomische Nachrichten 324, S3 (July 2003): 53–58. http://dx.doi.org/10.1002/asna.200385017.

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De Lucia, Gabriella, Adam Muzzin, and Simone Weinmann. "What Regulates Galaxy Evolution? Open questions in our understanding of galaxy formation and evolution." New Astronomy Reviews 62-63 (October 2014): 1–14. http://dx.doi.org/10.1016/j.newar.2014.08.001.

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Wyse, Rosemary F. G. "Chemical Evolution of the Galactic Disk and Bulge." Symposium - International Astronomical Union 164 (1995): 133–49. http://dx.doi.org/10.1017/s0074180900108502.

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The Milky Way Galaxy offers a unique opportunity for testing theories of galaxy formation and evolution. The study of the spatial distribution, kinematics and chemical abundances of stars in the Milky Way Galaxy allows one to address specific questions pertinent to this meeting such as (i)When was the Galaxy assembled? Is this an ongoing process? What was the merging history of the Milky Way?(ii)When did star formation occur in what is now “The Milky Way Galaxy”? Where did the star formation occur then? What was the stellar Initial Mass Function?(iii)How much dissipation of energy was there before and during the formation of the different stellar components of the Galaxy?(iv)What are the relationships among the different stellar components of the Galaxy?(v)Was angular momentum conserved during formation of the disk(s) of the Galaxy?(vi)What is the shape of the dark halo?(vii)Is there dissipative (disk) dark matter?

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41

Hopkins, Andrew. "Galaxy Metabolism." Publications of the Astronomical Society of Australia 27, no. 3 (2010): 233. http://dx.doi.org/10.1071/as10012.

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‘Galaxy Metabolism' was the second in the annual ‘Southern Cross Astrophysics Conference Series’ (http://www.aao.gov.au/AAO/southerncross/), supported by the Anglo-Australian Observatory and the Australia Telescope National Facility. It was held at the Australian National Maritime Museum in Darling Harbour, Sydney, from 22 to 26 June 2009, and was attended by 91 delegates from around the world.Over the past decade, both the star formation history and stellar mass density in galaxies spanning most of cosmic history have been well constrained. This provides the backdrop and framework within which many detailed investigations of galaxy growth are now placed. The mass-dependent and environment-dependent evolution of galaxies over cosmic history is now the focus of several surveys. Many studies are also exploring the role of gas infall and outflow in driving galaxy evolution, and the connection of these processes to massive star formation within galaxies.The aims of ‘Galaxy Metabolism’ were to bring together the global constraints on galaxy evolution, at both low and high redshift, with detailed studies of well-resolved systems, to define a clear picture of our understanding of galaxy metabolism: How do the processes of ingestion (infall), digestion (ISM physics, star formation) and excretion (outflow) govern the global properties of galaxies; how do these change over a galaxy's lifetime; and are the constraints from nearby well resolved studies consistent with those from large population surveys at low and high redshift?The conference was a great success, with an extensive variety of topics covered spanning many aspects of galaxy evolution, and brought together eloquently in a comprehensive conference summary by Warrick Couch. The four papers by De Lucia (2010), Cole (2010), Vlajić (2010) and Stocke et al. (2010) presented in this special collection of PASA are just a sampling of the depth and variety of the resentations given during the conference.

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Caplar, Neven, Simon J. Lilly, and Benny Trakhtenbrot. "AGN Evolution from the Galaxy Evolution Viewpoint. II." Astrophysical Journal 867, no. 2 (November 12, 2018): 148. http://dx.doi.org/10.3847/1538-4357/aae691.

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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 (March 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 scale environment will affect the galaxy evolution process and further work can be done to examine the impacts of other interactions. These results shed light on the deeper understanding of galaxy evolution process and call on more investigation of large scale environment of the galaxy.

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Silk, Joseph. "Formation and evolution of disk galaxies." Proceedings of the International Astronomical Union 4, S254 (June 2008): 401–10. http://dx.doi.org/10.1017/s1743921308027889.

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AbstractGlobal star formation is the key to understanding galaxy disk formation. This in turn depends on gravitational instability of disks and continuing gas accretion as well as minor merging. A key component is feedback from supernovae. Primary observational constraints on disk galaxy formation and evolution include the Schmidt-Kennicutt law, the Tully-Fisher relation and the galaxy luminosity function. I will review how theory confronts phenomenology, and discuss future prospects for refining our understanding of disk formation.

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45

Kreckel, Kathryn, Jacqueline H. van Gorkom, Burcu Beygu, Rien van de Weygaert, J. M. van der Hulst, Miguel A. Aragon-Calvo, and Reynier F. Peletier. "The Void Galaxy Survey: Galaxy Evolution and Gas Accretion in Voids." Proceedings of the International Astronomical Union 11, S308 (June 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 geometrically identified voids within the SDSS at distances of ∼100 Mpc, and pursued deep UV, optical, Hα, IR, and HI imaging to study in detail the morphology and kinematics of both the stellar and gaseous components. This sample allows us to not only examine the global statistical properties of void galaxies, but also to explore the details of the dynamical properties. We present an overview of the VGS, and highlight key results on the HI content and individually interesting systems. In general, we find that the void galaxies are gas rich, low luminosity, blue disk galaxies, with optical and HI properties that are not unusual for their luminosity and morphology. We see evidence of both ongoing assembly, through the gas dynamics between interacting systems, and significant gas accretion, seen in extended gas disks and kinematic misalignments. The VGS establishes a local reference sample to be used in future HI surveys (CHILES, DINGO, LADUMA) that will directly observe the HI evolution of void galaxies over cosmic time.

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46

May, A., C. A. Norman, and T. S. Van Albada. "Secular evolution in galaxies." Symposium - International Astronomical Union 106 (1985): 613–14. http://dx.doi.org/10.1017/s0074180900243258.

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We have adapted the N-body code of Van Albada (1982) to study the secular evolution of a hot collisionless stellar component (E galaxy or galactic bulge) due to slow changes in another component of the same galaxy. Our equilibrium starting model is a non-rotating triaxial ellipsoid with axial ratios 1.3:1.4:2.0; the effects of the “other component” are then simulated by various simple means.

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Twarog, Bruce A. "The chemical evolution of the Galaxy." Symposium - International Astronomical Union 106 (1985): 587–96. http://dx.doi.org/10.1017/s0074180900243210.

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Over the last few years, our picture of the chemical evolution of the Galaxy has changed substantially. These changes are of interest because chemical evolution provides a common point of contact for most astrophysical processes of importance to galaxy evolution. By astrophysical processes we mean star formation, stellar nucleosynthesis, gas dynamics, etc. An understanding of galactic chemical evolution would allow us to place constraints on all of these topics simultaneously. This property, however, is a double-edge sword because, with so many variables involved, unique solutions to problems in chemical evolution are almost impossible.

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Kolokythas, Konstantinos. "AGN feedback and galaxy evolution in nearby galaxy groups using CLoGS." Proceedings of the International Astronomical Union 15, S359 (March 2020): 180–81. http://dx.doi.org/10.1017/s1743921320001507.

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AbstractMuch of the evolution of galaxies takes place in groups where feedback has the greatest impact on galaxy formation and evolution. We summarize results from studies of the central brightest group early-type galaxies (BGEs) of an optically selected, statistically complete sample of 53 nearby groups (<80 Mpc; CLoGS sample), observed in radio 235/610 MHz (GMRT), CO (IRAM/APEX) and X-ray (Chandra and XMM-Newton) frequencies. We characterize the radio-AGN population of the BGEs, their group X-ray environment and examine the jet energetics impact on the intra-group gas. We discuss the relation between the radio properties of the BGEs and their group X-ray environment along with the relation between the molecular gas content and the star formation that BGEs present. We conclude that AGN feedback in groups can appear as relatively gentle near-continuous thermal regulation, but also as extreme AGN activity which could potentially shut down cooling for longer periods.

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49

Lacey, Cedric, and Joseph Silk. "Tidally triggered galaxy formation. I - Evolution of the galaxy luminosity function." Astrophysical Journal 381 (November 1991): 14. http://dx.doi.org/10.1086/170625.

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50

Mickaelian, A. M., L. A. Sargsyan, and G. A. Mikayelyan. "Byurakan–IRAS Galaxy Pairs as Indicators of Starburst and Galaxy Evolution." Proceedings of the International Astronomical Union 5, S267 (August 2009): 124. http://dx.doi.org/10.1017/s1743921310005855.

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The Byurakan–IRAS galaxies (BIG objects; Mickaelian 1995) are the result of a project of optical identifications of IRAS Point Source Catalog (PSC; IRAS 1988) in a 1500 square degree high-galactic latitude (|b|>15°) area based on the Digitized Sky Survey (DSS) images and the Digitized First Byurakan Survey (DFBS, or digitized Markarian survey) low-dispersion spectra. As a result, 1278 galaxies have been identified (as well as galactic objects, Byurakan–IRAS Stars [BIS]), including 42 PSC sources identified with 103 galaxies that make up 30 physical pairs and 12 multiples.

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Journal articles on the topic 'Galaxy evolution'

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