Academic literature on the topic 'Galaxy evolution'

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Journal articles on the topic "Galaxy evolution"

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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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Dissertations / Theses on the topic "Galaxy evolution"

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Croton, Darren. "Galaxy Formation and Evolution." Diss., lmu, 2005. http://nbn-resolving.de/urn:nbn:de:bvb:19-44059.

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Ruggiero, Rafael. "Galaxy Evolution in Clusters." Universidade de São Paulo, 2018. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-14022019-140755/.

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In this thesis, we aim to further elucidate the phenomenon of galaxy evolution in the environment of galaxy clusters using the methodology of numerical simulations. For that, we have developed hydrodynamic models in which idealized gas-rich galaxies move within the ICM of idealized galaxy clusters, allowing us to probe in a detailed and controlled manner their evolution in this extreme environment. The main code used in our simulations is RAMSES, and our results concern the changes in gas composition, star formation rate, luminosity and color of infalling galaxies. Additionally to processes taking place inside the galaxies themselves, we have also described the dynamics of the gas that is stripped from those galaxies with unprecedented resolution for simulations of this nature (122 pc in a box including an entire 1e14 Msun cluster), finding that clumps of molecular gas are formed within the tails of ram pressure stripped galaxies, which proceed to live in isolation within the ICM of a galaxy cluster for up to 300 Myr. Those molecular clumps possibly represent a new class of objects; similar objects have been observed in both galaxy clusters and groups, but no comprehensive description of them has been given until now. We additionally create a hydrodynamic model for the A901/2 multi-cluster system, and correlate the gas conditions in this model to the locations of a sample of candidate jellyfish galaxies in the system; this has allowed us to infer a possible mechanism for the generation of jellyfish morphologies in galaxy cluster collisions in general.
Nesta tese, nós visamos a contribuir para o entendimento do fenômeno da evolução de galáxias no ambiente de aglomerados de galáxias usando a metodologia de simulações numéricas. Para isso, desenvolvemos modelos hidrodinâmicos nos quais galáxias idealizadas ricas em gás movem-se em meio ao gás difuso de aglomerados de galáxias idealizados, permitindo um estudo detalhado e controlado da evolução destas galáxias neste ambiente extremo. O principal código usado em nossas simulações é o RAMSES, e nossos resultados tratam das mudanças em composição do gás, taxa de formação estelar, luminosidade e cor de galáxias caindo em aglomerados. Adicionalmente a processos acontecendo dentro das próprias galáxias, nós também descrevemos a dinâmica do gás que é varrido dessas galáxias com resolução sem precedentes para simulações dessa natureza (122 pc em uma caixa incluindo um aglomerado de 1e14 Msun inteiro), encontrando que aglomerados de gás molecular são formados nas caudas de galáxias que passaram por varrimento de gás por pressão de arraste, aglomerados estes que procedem a viver em isolamento em meio ao gás difuso de um aglomerado de galáxias por até 300 Myr. Esses aglomerados moleculares possivelmente representam uma nova classe de objetos; objetos similares foram previamente observados tanto em aglomerados quanto em grupos de galáxias, mas um tratamento compreensivo deles não foi apresentado até agora. Nós adicionalmente criamos um modelo hidrodinâmico para o sistema multi-aglomerado A901/2, e correlacionamos as condições do gás nesse modelo com a localização de uma amostra de galáxias jellyfish nesse sistema; isso nos permitiu inferir um possível mecanismo para a geração de morfologias jellyfish em colisões de aglomerados de galáxias em geral.
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Curtis, Lake Emma. "Galaxy evolution with FMOS." Thesis, University of Oxford, 2010. http://ora.ox.ac.uk/objects/uuid:866b8ba5-5353-43a7-9898-a4b767ab0f6d.

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This thesis is concerned with the targeting of emission line galaxies with FMOS (Fibre Multi-Object Spectrograph) to determine properties of star forming galaxies at redshift ~1.5, and provide measurements of the growth rate of large-scale structure through Redshift Space Distortions (RSDs). I also consider the opportunities of targeting the passive galaxy population at high redshift, through measurements of their continuum. I start with the extensive broad-band photometric data available in the UKIDSS-UDS (United Kingdom Infrared Telescope Deep Sky Survey - Ultra-Deep Survey) field which is used to produce a band-merged catalogue, later used for determining photometric redshifts. In producing this catalogue, I approach the issue of source confusion present in the deep Spitzer imaging using z-band priors on profile position and shape and an iterative Expectation-Maximisation algorithm. Photometric redshift estimates are compared against colour selections as potential targeting techniques for a wide-area redshift survey with FMOS. Different photometry survey areas are considered, and the quality of selection given the available broad-band data tested, by adjusting the photometric catalogue produced for the UDS. The results indicate that the SWIRE (Spitzer Wide area InfraRed Extragalactic Survey) fields are too small to provide adequate sources with a consistent selection mechanism. The CFHTLS (Canada-Frace-Hawaii Telescope Legacy Survey) would have a large enough area given deeper z'-band imaging, and SWIRE-depth coverage in the Spitzer 3.6μm and 4.5μm bands. I present FMOS commissioning data obtained for the UDS field, including the spectroscopic targeting of sources form the High-Z Emission Line Survey (HiZELS). With this data, I am able to test the current quality of flux calibration using cool stars targeted simultaneously and the level of systematic errors left by sky-subtraction. The sample of HiZELS sources selected to place Hα at z~1.45 show low contamination from other emission lines, and only one out of 9 targets assigned a redshift has any indication of AGN activity. Finally, I present longslit observations of faint, passive galaxies at redshift z~1.9, selected as members of a possible cluster, JKCS 041, selected from broad band colours. One object was observed with high enough signal to noise to constrain the position of the 4000 Å / Balmer break, providing a tighter constraint on the photometric redshift of 1.8867 +0.0034 -0.0117.
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Linke, Laila Maria [Verfasser]. "Testing models of galaxy formation and evolution with galaxy-galaxy-galaxy lensing / Laila Maria Linke." Bonn : Universitäts- und Landesbibliothek Bonn, 2021. http://d-nb.info/1235524469/34.

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Martinet, Nicolas. "Galaxy clusters : a probe to galaxy evolution and cosmology." Thesis, Paris 6, 2015. http://www.theses.fr/2015PA066348/document.

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Cette thèse présente un certain nombre de résultats récents à propos de l'évolution des galaxies et la cosmologie, à partir de l'observation d'amas de galaxies en lumière visible. Nous introduisons d'abord les principales propriétés des amas de galaxies (Chapitre 1.1) et la façon dont ces objets permettent de contraindre le modèle cosmologique standard (Chapitre 1.2). Une grande partie des résultats présentés ici ont été obtenus à partir de l'étude du relevé d'amas DAFT/FADA, qui regroupe des amas dans la gamme de décalages spectraux 0.4
This thesis presents some recent results concerning galaxy evolution and cosmology,based on the observation of galaxy clusters at optical wavelengths. We first introduce the main properties of galaxy clusters (Sect. 1.1) and how they can be used for cosmology within the standard cosmological model (Sect. 1.2). A large fraction of the presented results comes from the study of the DAFT/FADA galaxy cluster survey at redshifts 0.4 < z < 0.9 (Sect. 1.3). We divide our study in two parts according to the observable that is considered: galaxy luminosity or galaxy shape. The distribution of galaxy luminosities is called the galaxy luminosity function (GLF), which can be used to probe the evolution of cluster galaxies (Sect. 2.1). Computing the GLFs for a sub sample of 25 DAFT/FADA clusters, we find that faint blue star forming galaxies are quenched into red quiescent galaxies from high redshift until today. Comparing to the field shows that this transformation is more efficient in high density environments.We also study the fraction of baryons in galaxy groups and clusters (Sect. 2.2). Wefind that in groups, the stars contained in galaxies can reach masses of the same order as those of the intra-cluster gas, while in clusters they are usually negligible relatively to the gas. Taking both stars and gas into account we constrain the matter density parameter Galaxy shapes are distorted by foreground objects that bend light in their vicinity. This lensing signal can be exploited to measure the mass distribution of a foreground cluster. We review the basic theory of weak lensing and shear measurement (Sect. 3.1), and then apply it to a subsample of 16 DAFT/FADA clusters, with Subaru/SuprimeCam or CFHT/MegaCam imaging (Sect. 3.2). We estimate the masses of these clusters, and take advantage of the large fields of view of our images to detect filaments and structures in the cluster vicinity, observationally supporting the hierarchical scenario of cluster growth. Finally, we detect shear peaks in Euclid-like simulations, and use their statistics as a cosmological probe, similarly to cluster counts (Sect. 3.3). We forecast the cosmological constraints that this technique will achieve when applied to the Euclid space mission, and develop a tomographic analysis that adds information from redshifts. We conclude with a discussion of our perspectives on future studies in all the fieldsinvestigated in the present thesis
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Cool, Richard Jacob. "Empirical Measurements of Massive Galaxy and Active Galaxy Evolution." Diss., The University of Arizona, 2008. http://hdl.handle.net/10150/195540.

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Using new wide-area galaxy redshift surveys, we explore the evolutionof the most massive galaxies and the most luminous quasars in the universe over much of cosmic history. Quasars and massive red galaxies both areextremes; the most luminous high redshift quasars likely play a key role in shaping their nearby environment and the universe as a whole. The mostmassive galaxies represent the end points of galaxy evolution and containa fossil record of the galaxy evolution process.Using the AGES redshift survey completed with the MMT and the Hectospecmulti-object spectrograph as well as new $z$-band observations of the NOAO Deep Wide-Field Survey Bootes field, we report the discovery of threenew quasars at z>5. We explore new mid-infrared selection in light of thesethree new quasars and place constraints on the slope of the high-redshiftquasar luminosity function.At lower redshift (0.12.2L*), we find that the scatter around the color-magnitude relation is quite small in colors studied.Each of three model star formation histories can reproduce the scatter we measure, none of the models producecolor distributions matching those observed.We measure the evolution of the LRG luminosity function in the redshift range 0.13L*)red galaxies have grown by less than 50% (at 99% confidence) since z=0.9 in stark contrast to the factor of 2 to 4 growth observed in the L* red galaxy population over the same epoch.Finally, we introduce the PRIsm MUlti-object Survey (PRIMUS), a new redshiftsurvey aimed at collecting ~300,000 galaxy spectra over 10 sq. deg toz~1. We summarize the current status of PRIMUS observations and datareductions and present several survey statistics. PRIMUS is the largestexisting redshift survey at intermediate redshift and holds the largestsample of redshifts for Spitzer and X-ray detected objects.
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Thomas, Daniel. "Chemical evolution and galaxy formation." Diss., lmu, 2000. http://nbn-resolving.de/urn:nbn:de:bvb:19-4637.

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Bothwell, Matthew Stuart. "Galaxy evolution : near and far." Thesis, University of Cambridge, 2011. https://www.repository.cam.ac.uk/handle/1810/265602.

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The formation of stars from interstellar gas is the cornerstone of galaxy evolution. This thesis represents work undertaken in order to characterise the role of cool interstellar gas, and its relation to star formation, in galaxy evolution across cosmic time. In particular, it concentrates on star forming galaxies at the extremes of the galaxy assembly spectrum - extremely faint dwarfs, and extremely luminous starbursts - in an attempt to test the limits of galaxy evolution models. The thesis falls into two complimentary halves, addressing topics in the low redshift and high redshift Universe respectively. In the low redshift Universe, I discuss multi-wavelength studies of large samples of z rv O galaxies, which include extremely faint dwarf galaxies in the Local Volume. Using these samples, it is possible to derive a multitude of physical parameters (including star formation rates, stellar masses, and gas masses) which allow the interrelationship between star formation and gas content to be assessed in a statistically significant manner. In particular, modern wide field surveys (combined with deep, volume-limited data) allow trends to be analysed across many orders of magnitude in galaxy mass and star formation rate, shedding light on the global properties of galaxies in the local Universe. Moving to higher redshift, I discuss targeted observations of molecular gas in extreme star forming galaxies in the early Universe. These 'sub-millimetre' galaxies number amongst the most luminous objects ever discovered, and molecular gas observations have the power to uncover many of their physical properties, including their morphologies, kinematics, and star formation behaviour. I begin by presenting high-resolution observations of a small number of these galaxies at z rv 2, and discussing the implications for galaxy evolution studies. The final chapter of this thesis consists of the results of a survey for molecular gas in sub-millimetre galaxies conducted over the last decade, which represents the largest single study of molecular gas in the early Universe to date.
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Moustakas, John. "Spectral Diagnostics of Galaxy Evolution." Diss., The University of Arizona, 2006. http://hdl.handle.net/10150/305142.

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Despite considerable progress in recent years, a complete description of the physical drivers of galaxy formation and evolution remains elusive, in part because of our poor understanding of star formation, and how star formation in galaxies is regulated by feedback from supernovae and massive stellar winds. Insight into the star formation histories of galaxies, and the interplay between star formation and feedback, can be gained by measuring their chemical abundances, which until recently has only been possible for galaxies in the nearby universe. However, reliable star formation and abundance calibrations have been hampered by various systematic uncertainties, and the lack of a suitable spectrophotometric sample with which to develop better calibrations. To address the limitations of existing surveys, we have obtained integrated optical spectra for a diverse sample of more than four hundred nearby star-forming galaxies. Using these data, in conjunction with observations from the Sloan Digital Sky Survey, we conduct a detailed analysis of optical star formation indicators, and develop empirical calibrations for the [O II] 3727 and H-beta 4861 nebular emission lines. Next, we investigate whether integrated spectroscopy of star forming galaxies can be used to infer their gas-phase oxygen abundances in the presence of radial abundance gradients, diffuse-ionized gas emission, and dust attenuation. We conclude that the integrated R23 parameter is generally insensitive to these systematic effects, enabling the gas-phase metallicity to be measured with a precision of +/-0.1 dex. We apply these methods to study the evolution in the luminosity-metallicity relation at 0
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Osmond, John Peter Francis. "The evolution of galaxy groups." Thesis, University of Birmingham, 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.422727.

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Books on the topic "Galaxy evolution"

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Van den Bosch, Frank, 1969- and White S, eds. Galaxy formation and evolution. Cambridge: Cambridge University Press, 2010.

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Spinrad, Hyron. Galaxy formation and evolution. Berlin, Germany: Springer, 2005.

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Galaxy formation and evolution. Berlin: Springer, 2005.

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Bender, Ralf, and Roger L. Davies, eds. New Light on Galaxy Evolution. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9.

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Lobo, Catarina, Margarida Serote Roos, and Andrea Biviano, eds. Galaxy Evolution in Groups and Clusters. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0107-6.

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Matteucci, Francesca. The Chemical Evolution of the Galaxy. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0967-6.

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The chemical evolution of the galaxy. Dordrecht: Kluwer Academic Publishers, 2001.

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Mysteries of galaxy formation. Berlin: Springer, 2010.

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Renzini, Alvio, and Ralf Bender, eds. Multiwavelength Mapping of Galaxy Formation and Evolution. Berlin, Heidelberg: Springer Berlin Heidelberg, 2005. http://dx.doi.org/10.1007/b96746.

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da Costa, Luiz Nicolaci, and Alvio Renzini, eds. Galaxy Scaling Relations: Origins, Evolution and Applications. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-540-69654-4.

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Book chapters on the topic "Galaxy evolution"

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Schneider, Peter. "Galaxy evolution." In Extragalactic Astronomy and Cosmology, 521–71. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-54083-7_10.

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Pagel, B. E. J. "Galactic Chemical Evolution." In The Galaxy, 341–64. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3925-7_16.

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Gardner, J. P. "Galaxy Evolution from Deep Galaxy Counts." In Stellar Populations, 311–19. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0125-7_30.

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Fuchs, Burkhard, and Roland Wielen. "Dynamical Evolution of the Galactic Disk." In The Galaxy, 375–98. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3925-7_18.

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van der Hulst, J. M., E. Hummel, W. C. Keel, and R. C. Kennicutt. "The Effects of Galaxy — Galaxy Interactions on Nuclear Activity." In Spectral Evolution of Galaxies, 103–10. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4598-2_11.

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Fioc, Michel. "UV to NIR Galaxy Evolution and Galaxy Counts." In New Light on Galaxy Evolution, 373. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9_85.

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Worthey, Guy. "Elliptical Galaxy Chemical Evolution." In Chemical Evolution from Zero to High Redshift, 168–74. Berlin, Heidelberg: Springer Berlin Heidelberg, 1999. http://dx.doi.org/10.1007/978-3-540-48360-1_42.

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Baan, Willem A. "Megamasers and Galaxy Evolution." In Windows on Galaxies, 351–55. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0543-6_45.

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Ellingson, E. "Galaxy Evolution in Clusters." In Galaxy Evolution in Groups and Clusters, 9–18. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0107-6_1.

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Guiderdoni, B. "Galaxy Evolution: An Overview." In The Evolution of Galaxies, 13–23. Dordrecht: Springer Netherlands, 2002. http://dx.doi.org/10.1007/978-94-017-3311-3_2.

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Conference papers on the topic "Galaxy evolution"

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Madore, Barry F. "GALEX: Galaxy Evolution Explorer." In THE SPECTRAL ENERGY DISTRIBUTIONS OF GAS-RICH GALAXIES: Confronting Models with Data; International Workshop. AIP, 2005. http://dx.doi.org/10.1063/1.1913948.

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Stanghellini, Carlo. "Radio galaxy Evolution." In First MCCT-SKADS Training School. Trieste, Italy: Sissa Medialab, 2008. http://dx.doi.org/10.22323/1.059.0015.

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Silk, Joseph, and Rychard Bouwens. "Simulating galaxy evolution." In AFTER THE DARK AGES. ASCE, 1999. http://dx.doi.org/10.1063/1.58639.

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Martin, Christopher, Thomas Barlow, William Barnhart, Luciana Bianchi, Brian K. Blakkolb, Dominique Bruno, Joseph Bushman, et al. "The Galaxy Evolution Explorer." In Astronomical Telescopes and Instrumentation, edited by J. Chris Blades and Oswald H. W. Siegmund. SPIE, 2003. http://dx.doi.org/10.1117/12.460034.

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Tonnesen, Stephanie. "Environmentally-Driven Galaxy Evolution." In Frank N. Bash Symposium 2011: New Horizons in Astronomy. Trieste, Italy: Sissa Medialab, 2012. http://dx.doi.org/10.22323/1.149.0008.

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HUGHES, DAVID H., and ENRIQUE GAZTAÑAGA. "SIMULATED SUBMILLIMETRE GALAXY SURVEYS." In Implications for Galaxy Formation and Evolution. WORLD SCIENTIFIC, 2001. http://dx.doi.org/10.1142/9789812811738_0027.

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Wyse, Rosemary, and Gerard Gilmore. "The dynamical evolution of the Galaxy." In Back to the Galaxy. AIP, 1992. http://dx.doi.org/10.1063/1.44001.

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Page, M. J., F. J. Carrera, J. A. Stevens, A. Comastri, L. Angelini, and M. Cappi. "QSO winds and galaxy evolution." In X-RAY ASTRONOMY 2009; PRESENT STATUS, MULTI-WAVELENGTH APPROACH AND FUTURE PERSPECTIVES: Proceedings of the International Conference. AIP, 2010. http://dx.doi.org/10.1063/1.3475264.

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Fraternali, Filippo, Victor P. Debattista, and C. C. Popescu. "Gas Circulation and Galaxy Evolution." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458468.

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Truran, J. W., and F. X. Timmes. "Chemical evolution of the galaxy." In The 3rd international symposium on nuclear astrophysics: Nuclei in the Cosmos III. AIP, 1995. http://dx.doi.org/10.1063/1.47329.

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Reports on the topic "Galaxy evolution"

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Arraki, Kenza Sigrid. Evolution of dwarf galaxy properties in local group environments. Office of Scientific and Technical Information (OSTI), May 2016. http://dx.doi.org/10.2172/1491856.

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Zhang, Yuanyuan. Looking Wider and Further: The Evolution of Galaxies Inside Galaxy Clusters. Office of Scientific and Technical Information (OSTI), January 2016. http://dx.doi.org/10.2172/1248222.

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Bunker, A. J., and W. J. M. van Breugel. The Hy-Redshift Universe: Galaxy Formation and Evolution at High Redshift. Office of Scientific and Technical Information (OSTI), November 1999. http://dx.doi.org/10.2172/793845.

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Meyer, B. S., and D. N. Schramm. General constraints on the age and chemical evolution of the Galaxy. Office of Scientific and Technical Information (OSTI), May 1986. http://dx.doi.org/10.2172/5797647.

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Hoversten, Erik A. Galaxy Evolution Insights from Spectral Modeling of Large Data Sets from the Sloan Digital Sky Survey. Office of Scientific and Technical Information (OSTI), October 2007. http://dx.doi.org/10.2172/935485.

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Galili, Naftali, Roger P. Rohrbach, Itzhak Shmulevich, Yoram Fuchs, and Giora Zauberman. Non-Destructive Quality Sensing of High-Value Agricultural Commodities Through Response Analysis. United States Department of Agriculture, October 1994. http://dx.doi.org/10.32747/1994.7570549.bard.

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Abstract:
The objectives of this project were to develop nondestructive methods for detection of internal properties and firmness of fruits and vegetables. One method was based on a soft piezoelectric film transducer developed in the Technion, for analysis of fruit response to low-energy excitation. The second method was a dot-matrix piezoelectric transducer of North Carolina State University, developed for contact-pressure analysis of fruit during impact. Two research teams, one in Israel and the other in North Carolina, coordinated their research effort according to the specific objectives of the project, to develop and apply the two complementary methods for quality control of agricultural commodities. In Israel: An improved firmness testing system was developed and tested with tropical fruits. The new system included an instrumented fruit-bed of three flexible piezoelectric sensors and miniature electromagnetic hammers, which served as fruit support and low-energy excitation device, respectively. Resonant frequencies were detected for determination of firmness index. Two new acoustic parameters were developed for evaluation of fruit firmness and maturity: a dumping-ratio and a centeroid of the frequency response. Experiments were performed with avocado and mango fruits. The internal damping ratio, which may indicate fruit ripeness, increased monotonically with time, while resonant frequencies and firmness indices decreased with time. Fruit samples were tested daily by destructive penetration test. A fairy high correlation was found in tropical fruits between the penetration force and the new acoustic parameters; a lower correlation was found between this parameter and the conventional firmness index. Improved table-top firmness testing units, Firmalon, with data-logging system and on-line data analysis capacity have been built. The new device was used for the full-scale experiments in the next two years, ahead of the original program and BARD timetable. Close cooperation was initiated with local industry for development of both off-line and on-line sorting and quality control of more agricultural commodities. Firmalon units were produced and operated in major packaging houses in Israel, Belgium and Washington State, on mango and avocado, apples, pears, tomatoes, melons and some other fruits, to gain field experience with the new method. The accumulated experimental data from all these activities is still analyzed, to improve firmness sorting criteria and shelf-life predicting curves for the different fruits. The test program in commercial CA storage facilities in Washington State included seven apple varieties: Fuji, Braeburn, Gala, Granny Smith, Jonagold, Red Delicious, Golden Delicious, and D'Anjou pear variety. FI master-curves could be developed for the Braeburn, Gala, Granny Smith and Jonagold apples. These fruits showed a steady ripening process during the test period. Yet, more work should be conducted to reduce scattering of the data and to determine the confidence limits of the method. Nearly constant FI in Red Delicious and the fluctuations of FI in the Fuji apples should be re-examined. Three sets of experiment were performed with Flandria tomatoes. Despite the complex structure of the tomatoes, the acoustic method could be used for firmness evaluation and to follow the ripening evolution with time. Close agreement was achieved between the auction expert evaluation and that of the nondestructive acoustic test, where firmness index of 4.0 and more indicated grade-A tomatoes. More work is performed to refine the sorting algorithm and to develop a general ripening scale for automatic grading of tomatoes for the fresh fruit market. Galia melons were tested in Israel, in simulated export conditions. It was concluded that the Firmalon is capable of detecting the ripening of melons nondestructively, and sorted out the defective fruits from the export shipment. The cooperation with local industry resulted in development of automatic on-line prototype of the acoustic sensor, that may be incorporated with the export quality control system for melons. More interesting is the development of the remote firmness sensing method for sealed CA cool-rooms, where most of the full-year fruit yield in stored for off-season consumption. Hundreds of ripening monitor systems have been installed in major fruit storage facilities, and being evaluated now by the consumers. If successful, the new method may cause a major change in long-term fruit storage technology. More uses of the acoustic test method have been considered, for monitoring fruit maturity and harvest time, testing fruit samples or each individual fruit when entering the storage facilities, packaging house and auction, and in the supermarket. This approach may result in a full line of equipment for nondestructive quality control of fruits and vegetables, from the orchard or the greenhouse, through the entire sorting, grading and storage process, up to the consumer table. The developed technology offers a tool to determine the maturity of the fruits nondestructively by monitoring their acoustic response to mechanical impulse on the tree. A special device was built and preliminary tested in mango fruit. More development is needed to develop a portable, hand operated sensing method for this purpose. In North Carolina: Analysis method based on an Auto-Regressive (AR) model was developed for detecting the first resonance of fruit from their response to mechanical impulse. The algorithm included a routine that detects the first resonant frequency from as many sensors as possible. Experiments on Red Delicious apples were performed and their firmness was determined. The AR method allowed the detection of the first resonance. The method could be fast enough to be utilized in a real time sorting machine. Yet, further study is needed to look for improvement of the search algorithm of the methods. An impact contact-pressure measurement system and Neural Network (NN) identification method were developed to investigate the relationships between surface pressure distributions on selected fruits and their respective internal textural qualities. A piezoelectric dot-matrix pressure transducer was developed for the purpose of acquiring time-sampled pressure profiles during impact. The acquired data was transferred into a personal computer and accurate visualization of animated data were presented. Preliminary test with 10 apples has been performed. Measurement were made by the contact-pressure transducer in two different positions. Complementary measurements were made on the same apples by using the Firmalon and Magness Taylor (MT) testers. Three-layer neural network was designed. 2/3 of the contact-pressure data were used as training input data and corresponding MT data as training target data. The remaining data were used as NN checking data. Six samples randomly chosen from the ten measured samples and their corresponding Firmalon values were used as the NN training and target data, respectively. The remaining four samples' data were input to the NN. The NN results consistent with the Firmness Tester values. So, if more training data would be obtained, the output should be more accurate. In addition, the Firmness Tester values do not consistent with MT firmness tester values. The NN method developed in this study appears to be a useful tool to emulate the MT Firmness test results without destroying the apple samples. To get more accurate estimation of MT firmness a much larger training data set is required. When the larger sensitive area of the pressure sensor being developed in this project becomes available, the entire contact 'shape' will provide additional information and the neural network results would be more accurate. It has been shown that the impact information can be utilized in the determination of internal quality factors of fruit. Until now,
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