Relevant bibliographies by topics / Galaxies: abundance

Academic literature on the topic 'Galaxies: abundance'

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Published: 1 April 2023

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Journal articles on the topic "Galaxies: abundance"

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Skillman, Evan D. "Dwarf Galaxies as Low Surface Brightness Galaxies." International Astronomical Union Colloquium 171 (1999): 169–76. http://dx.doi.org/10.1017/s0252921100054270.

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AbstractBecause of the weak correlation between surface brightness and luminosity, as galaxy surveys reach to lower surface brightnesses, increasing numbers of dwarf galaxies are found. Thus, studies of dwarf galaxies are relevant to our understanding of the low surface brightness universe. In particular, studies of nearby LSB dwarfs may help to answer questions concerning: (1) star formation in low abundance and low mass surface density envrionments, (2) star formation histories of galaxies and the relative youth of LSB galaxies, and (3) the chemical evolution of LSB galaxies. HST WFPC2 photometry of the resolved stars in nearby dwarf galaxies is particularly useful for all three questions.H II region abundances remain the best probe of current ISM abundances. Current evidence favors total mass (or luminosity) as the primary factor for determining the present day chemical abundance in both LSB and HSB galaxies. It remains possible that mass surface density (or surface brightness) may be a second controlling parameter.
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Dutil, Yvan, and Jean-René Roy. "Evidence for a Morphological Evolution of Spiral Galaxies." Symposium - International Astronomical Union 204 (2001): 387. http://dx.doi.org/10.1017/s0074180900226302.

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A detailed analysis of the oxygen abundance profile has been carried out on a sample of spiral galaxies from which very good data was available. The early-type galaxies of our sample display gradients that are flatter, and overall levels of O/H abundances that are higher, than those of normal late-type galaxies. Early-type galaxies show an identical trend in the behavior of extrapolated central abundance versus morphological type to that shown by late-type galaxies with strong bars, even in the absence of a bar. On a diagram showing extrapolated central abundances versus morphological types, two clearly separated sequences appear: late-type barred galaxies and early-type (barred or unbarred) galaxies clearly fall on a sequence 0.5 dex in abundance below that of normal late-type galaxies. This behavior is consistent with theoretical models of morphological evolution of disk galaxies by the formation and dissolution of a bar over a period of a few 109 yr, where later type galaxies (Sd, Sc, SBc) evolve into earlier-type disk galaxies (Sb, Sa) through transitory SBc and SBb phases.
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Klypin, Anatoly, Igor Karachentsev, Dmitry Makarov, and Olga Nasonova. "Abundance of field galaxies." Monthly Notices of the Royal Astronomical Society 454, no. 2 (October 7, 2015): 1798–810. http://dx.doi.org/10.1093/mnras/stv2040.

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Boardman, N. F., G. Zasowski, J. A. Newman, S. F. Sanchez, A. Schaefer, J. Lian, D. Bizyaev, and N. Drory. "SDSS-IV MaNGA: galaxy gas-phase metallicity gradients vary across the mass–size plane." Monthly Notices of the Royal Astronomical Society 501, no. 1 (December 8, 2020): 948–53. http://dx.doi.org/10.1093/mnras/staa3785.

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ABSTRACT Gas-phase abundances and abundance gradients provide much information on past stellar generations, and are powerful probes of how galaxies evolve. Gas abundance gradients in galaxies have been studied as functions of galaxies’ mass and size individually, but have largely not been considered across the galaxy mass–size plane. Thus, we investigate gas-phase abundance gradients across this plane, using a sample of over 1000 galaxies selected from the MApping Nearby Galaxies at APO (MaNGA) spectroscopic survey. We find that gradients vary systematically such that above 1010 M⊙, smaller galaxies display flatter gradients than larger galaxies at a given stellar mass. This mass–size behaviour cannot be explained by instrumental effects, nor is it simply a reflection of known trends between gradients and morphology. We explore multiple possibilities for a physical origin for this pattern, though further work is needed to establish a firm physical interpretation.
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Pilyugin, L. S., E. K. Grebel, I. A. Zinchenko, Y. A. Nefedyev, and J. M. Vílchez. "Relations between abundance characteristics and rotation velocity for star-forming MaNGA galaxies." Astronomy & Astrophysics 623 (March 2019): A122. http://dx.doi.org/10.1051/0004-6361/201834239.

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We derive rotation curves, surface brightness profiles, and oxygen abundance distributions for 147 late-type galaxies using the publicly available spectroscopy obtained by the MaNGA survey. Changes of the central oxygen abundance (O/H)0, the abundance at the optical radius (O/H)R25, and the abundance gradient with rotation velocity Vrot were examined for galaxies with rotation velocities from 90 km s−1 to 350 km s−1. We find that each relation shows a break at Vrot∗ ∼ 200 km s−1. The central (O/H)0 abundance increases with rising Vrot and the slope of the (O/H)0–Vrot relation is steeper for galaxies with Vrot ≲ Vrot∗. The mean scatter of the central abundances around this relation is 0.053 dex. The relation between the abundance at the optical radius of a galaxy and its rotation velocity is similar; the mean scatter in abundances around this relation is 0.081 dex. The radial abundance gradient expressed in dex/kpc flattens with the increase of the rotation velocity. The slope of the relation is very low for galaxies with Vrot ≳ Vrot∗. The abundance gradient expressed in dex/R25 is roughly constant for galaxies with Vrot ≲ Vrot∗, flattens towards Vrot∗, and then again is roughly constant for galaxies with Vrot ≳ Vrot∗. The change of the gradient expressed in terms of dex/hd (where hd is the disc scale length), in terms of dex/Re, d (where Re, d is the disc effective radius), and in terms of dex/Re, g (where Re, g is the galaxy effective radius) with rotation velocity is similar to that for gradient in dex/R25. The relations between abundance characteristics and other basic parameters (stellar mass, luminosity, and radius) are also considered.
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Flury, Sophia R., and Edward C. Moran. "Chemical abundances in active galaxies." Monthly Notices of the Royal Astronomical Society 496, no. 2 (June 6, 2020): 2191–203. http://dx.doi.org/10.1093/mnras/staa1563.

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ABSTRACT The Sloan Digital Sky Survey (SDSS) has proved to be a powerful resource for understanding the physical properties and chemical composition of star-forming galaxies in the local Universe. The SDSS population of active galactic nuclei (AGNs) remains as of yet less explored in this capacity. To extend the rigorous study of H ii regions in the SDSS to AGNs, we adapt methods for computing direct-method chemical abundances for application to the narrow-line regions (NLR) of AGNs. By accounting for triply ionized oxygen, we are able to more completely estimate the total oxygen abundance. We find a strong correlation between electron temperature and oxygen abundance due to collisional cooling by metals. Furthermore, we find that nitrogen and oxygen abundances in AGNs are strongly correlated. From the metal–temperature relation and the coupling of nitrogen and oxygen abundances, we develop a new, empirically and physically motivated method for determining chemical abundances from the strong emission lines commonly employed in flux-ratio diagnostic diagrams (BPT diagrams). Our approach, which for AGNs reduces to a single equation based on the BPT line ratios, consistently recovers direct-method abundances over a 1.5 dex range in oxygen abundance with an rms uncertainty of 0.18 dex. We have determined metallicities for thousands of AGNs in the SDSS, and in the process have discovered an ionization-related discriminator for Seyfert and LINER galaxies.
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Feldmeier-Krause, A., I. Lonoce, and W. L. Freedman. "Stellar Population and Elemental Abundance Gradients of Early-type Galaxies*." Astrophysical Journal 923, no. 1 (December 1, 2021): 65. http://dx.doi.org/10.3847/1538-4357/ac281e.

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Abstract The evolution of galaxies is imprinted on their stellar populations. Several stellar population properties in massive early-type galaxies have been shown to correlate with intrinsic galaxy properties such as the galaxy’s central velocity dispersion, suggesting that stars formed in an initial collapse of gas (z ∼ 2). However, stellar populations change as a function of galaxy radius, and it is not clear how local gradients of individual galaxies are influenced by global galaxy properties and galaxy environment. In this paper, we study the stellar populations of eight early-type galaxies as a function of radius. We use optical spectroscopy (∼4000–8600 Å) and full spectral fitting to measure stellar population age, metallicity, slope of the initial mass function (IMF), and nine elemental abundances (O, Mg, Si, Ca, Ti, C, N, Na, and Fe) out to 1 R e for each galaxy individually. We find a wide range of properties, with ages ranging from 3–13 Gyr. Some galaxies have a radially constant, Salpeter-like IMF, and other galaxies have a super-Salpeter IMF in the center, decreasing to a sub-Salpeter IMF at ∼0.5 R e . We find a global correlation of the central [Z/H] with the central IMF and the radial gradient of the IMF for the eight galaxies, but local correlations of the IMF slope with other stellar population parameters hold only for subsets of the galaxies in our sample. Some elemental abundances also correlate locally with each other within a galaxy, suggesting a common production channel. These local correlations appear only in subsets of our galaxies, indicating variations of the stellar content among different galaxies.
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Dors, Oli L. "Chemical abundances in Seyfert galaxies – VI. Empirical abundance calibration." Monthly Notices of the Royal Astronomical Society 507, no. 1 (July 30, 2021): 466–74. http://dx.doi.org/10.1093/mnras/stab2166.

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ABSTRACT We derived a bi-dimensional calibration between the emission-line ratios $R_{23}= ([\mathrm{ O}\, {\small {\rm II}}]\,\lambda 3726 +\lambda 3729 +[\mathrm{ O}\mathrm{ }\, {\small {\rm III}}]\,\lambda 4959 + \lambda 5007)/\rm H\,\beta$, ${\it P}=[([\mathrm{ O}\, {\small {\rm III}}]\,\lambda 4959+\lambda 5007)/{\rm H}\,\beta ]/R_{23}$ and the oxygen abundance relative to hydrogen (O/H) in the gas phase of Seyfert 1 and 2 nuclei. In view of this, emission-line intensity ratios for a sample of objects taken from the Sloan Digital Sky Survey Data Release 7 measured by the MPA/JHU group and direct estimates of O/H based on Te-method, adapted for active galactic nuclei (AGNs), are considered. We find no variation of R23 observed along the radii of AGNs, which shows that this line ratio is a good oxygen abundance (O/H) indicator for the class of objects considered in this work. The derived O/H = f(R23, P) relation produces O/H values similar to estimations via Te-method in a wide range of metallicities [$\rm 8.0 \: \lesssim \: 12+\log \,(O/H) \: \lesssim \: 9.2$]. Conversely to star-forming regions in the high-metallicity regime, R23 shows a positive correlation trend with O/H in AGNs. This indicates that the hardness of ionizing radiation is not affected by the metallicities in these objects or narrow-line regions are not significantly modified by changes in the spectral energy distribution due to metallicity variations.
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Kovtyukh, V., B. Lemasle, G. Bono, I. A. Usenko, R. da Silva, A. Kniazev, E. K. Grebel, I. L. Andronov, L. Shakun, and L. Chinarova. "The MAGIC project – III. Radial and azimuthal Galactic abundance gradients using classical Cepheids." Monthly Notices of the Royal Astronomical Society 510, no. 2 (December 4, 2021): 1894–901. http://dx.doi.org/10.1093/mnras/stab3530.

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ABSTRACT Radial abundance gradients provide sound constraints for chemo-dynamical models of galaxies. Azimuthal variations of abundance ratios are solid diagnostics to understand their chemical enrichment. In this paper, we investigate azimuthal variations of abundances in the Milky Way using Cepheids. We provide the detailed chemical composition (25 elements) of 105 Classical Cepheids from high-resolution SALT spectra observed by the MAGIC project. Negative abundance gradients, with abundances decreasing from the inner to the outer disc, have been reported both in the Milky Way and in external galaxies, and our results are in full agreement with literature results. We find azimuthal variations of the oxygen abundance [O/H]. While a large number of external spirals show negligible azimuthal variations, the Milky Way seems to be one of the few galaxies with noticeable [O/H] azimuthal asymmetries. They reach ≈0.2 dex in the inner Galaxy and in the outer disc, where they are the largest, thus supporting similar findings for nearby spiral galaxies, as well as recent 2D chemo-dynamical models.
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Sen, Seyda, Reynier F. Peletier, Elisa Toloba, and Jaco J. Mentz. "Abundance Ratios in Dwarf Elliptical Galaxies." Proceedings of the International Astronomical Union 11, S321 (March 2016): 269. http://dx.doi.org/10.1017/s1743921316012503.

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AbstractThe aim of this study is to determine abundance ratios and star formation histories (SFH) of dwarf ellipticals in the nearby Virgo cluster. We perform a stellar population analysis of 39 dEs and study them using index-index and scaling relations. We find an unusual behaviour where [Na/Fe] is under-abundant w.r.t. solar while [Ca/Fe] is over-abundant.
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Dissertations / Theses on the topic "Galaxies: abundance"

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Hempel, Angela. "Classification and abundance of extremely red galaxies with R-J]= 5." [S.l. : s.n.], 2004. http://deposit.ddb.de/cgi-bin/dokserv?idn=973946733.

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SAMUROVIC, SRDJAN. "DARK MATTER IN EARLY-TYPE GALAXIES WITH X-RAY HALOES. A SPECTROSCOPIC STUDY OF DYNAMICS AND ABUNDANCE INDICES." Doctoral thesis, Università degli studi di Trieste, 2004. http://thesis2.sba.units.it/store/handle/item/12724.

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Sakr, Ziad. "Cosmology beyond ΛCDM model in the light of cluster abundance tension." Thesis, Toulouse 3, 2018. http://www.theses.fr/2018TOU30346.

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Le modèle ΛCDM permet de décrire avec une grande précision la plupart des présentes observations cosmologiques. Cependant, l'un de ses paramètres, σ 8, mesurant l'amplitude de fluctuations de la matière, présente une discordance entre sa valeur contrainte par le spectre de puissance angulaire du CMB de la mission Planck, les Cls, et celle déterminée à partir des amas SZ dans l'univers proche. Dans le présent travail on explore divers extensions du modèle ΛCDM comme origines possibles de cette anomalie. Pour tester les effets de ces extensions, nous avons effectué une analyse Monte Carlo on l'on compare les contraintes sur σ 8 à partir de ΛCDM avec celles résultantes de ces extensions, et ceci en utilisant principalement le spectre de puissance CMB seul ou combiné avec des comptages d'amas. Ces derniers sont basés sur différentes relations masse observables et couvrent différents redshift : des amas de rayons X dans l'univers local, des amas de la mission SZ Planck dans l'univers proche ou une estimation des amas détectés par leur richesse photométrique à partir du la future mission Euclid. Du fait qu'une mauvaise détermination de l'étalonnage de la masse des amas pourrait également être la raison de cette divergence, notre approche consistait, lorsqu'on combinait les deux sondes issues des amas et du CMB, à laisser le facteur d'étalonnage libre afin qu'il soit contraint comme les autres paramètres cosmologiques par les deux données. Dans le cas d'introduction de trois neutrinos massifs dégénérés, nous avons trouvé qu'ils n'ont aucun effet significatif sur la correction de l'écart entre les contraintes issues de comptage CMB et ceux issues des Xray ou SZ cluster. Nous avons ensuite permis à l'indice de croissance ƴ de varier. Nous trouvons une corrélation entre ƴ et le paramètre de calibration masse-observable des amas détectés par rayons X qui n'est pas affecté par la présence ou non des neutrinos massifs. [...]
The ΛCDM model has proved successful in describing to a high precision most of nowadays cosmological observations. However, one of its parameters, σ 8, measuring the present matter amplitude fluctuations, constrained from CMB angular power spectrum, the Cls, was found by the Planck mission, in significant tension with value constrained by SZ galaxy cluster counts in the near universe. In the present work we investigate extensions to ΛCDM model as possible origins behind this discrepancy. To test these extensions, we performed a Monte Carlo analysis to compare constraints on σ 8 in ΛCDM with constraints under these extensions, using mainly CMB Cls combined with cluster counts sample. The later were based on different mass observables relations and covered different redshift ranges: X-ray cluster in the local universe, SZ Planck mission clusters from the near universe or photometric richness estimated detected clusters from future high redshift upcoming Euclid alike mission. Because an improper determination of the calibration of cluster mass function could also be behind this discrepancy, our approach was, when combined with CMB, to leave the calibration factor free to vary and be constrained by data. Introducing three degenerate massive neutrinos, we found that they have no significant effect on fixing the discrepancy between CMB and Xray or SZ cluster counts. We then allowed the growth index ƴ to vary. We find a correlation in the confidence space between ƴ and the X-ray mass observable factor not affected by the presence of massive neutrinos, indicating that a modifying gravity is favored over massive neutrinos as a way to alleviate the tension. However, when a SZ cluster sample covering a larger redshift range was used, we found that the correlation between ƴ and the calibration factor, is constrained by the evolution of the growth through redshift and limited to a region where it cannot fix the discrepancy. [...]
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Diaz, Beltran A. I. "Chemical abundances in spiral galaxies." Thesis, University of Sussex, 1985. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.372064.

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Guo, Yicheng, David C. Koo, Yu Lu, John C. Forbes, Marc Rafelski, Jonathan R. Trump, Ricardo Amorín, et al. "STELLAR MASS–GAS-PHASE METALLICITY RELATION AT 0.5 ≤ z ≤ 0.7: A POWER LAW WITH INCREASING SCATTER TOWARD THE LOW-MASS REGIME." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621237.

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We present the stellar mass (M-*)-gas-phase metallicity relation (MZR) and its scatter at intermediate redshifts (0.5 <= z <= 0.7) for 1381 field galaxies collected from deep spectroscopic surveys. The star formation rate (SFR) and color at a given M-* of this magnitude-limited (R less than or similar to 24 AB) sample are representative of normal star-forming galaxies. For masses below 10(9) M-circle dot, our sample of 237 galaxies is similar to 10 times larger than those in previous studies beyond the local universe. This huge gain in sample size enables superior constraints on the MZR and its scatter in the low-mass regime. We find a power-law MZR at 10(8) M-circle dot < M-* < 10(11) M-circle dot: 12 + log (O/H) = (5.83 +/- 0.19)+(0.30 +/- 0.02) log (M-*/M-circle dot). At 10(9) M-circle dot < M-* < 10(10.5) M-circle dot, our MZR shows agreement with others measured at similar redshifts in the literature. Our power-law slope is, however, shallower than the extrapolation of the MZRs of others to masses below 10(9) M-circle dot. The SFR dependence of the MZR in our sample is weaker than that found for local galaxies (known as the fundamental metallicity relation). Compared to a variety of theoretical models, the slope of our MZR for low-mass galaxies agrees well with predictions incorporating supernova energy-driven winds. Being robust against currently uncertain metallicity calibrations, the scatter of the MZR serves as a powerful diagnostic of the stochastic history of gas accretion, gas recycling, and star formation of low-mass galaxies. Our major result is that the scatter of our MZR increases as M-* decreases. Our result implies that either the scatter of the baryonic accretion rate (sigma((M) over dot)) or the scatter of the M-*-M-halo relation (sigma(SHMR)) increases as M-* decreases. Moreover, our measure of scatter at z = 0.7 appears consistent with that found for local galaxies. This lack of redshift evolution constrains models of galaxy evolution to have both sigma((M) over dot) and sigma(SHMR) remain unchanged from z = 0.7 to z = 0.
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Lipman, Keith. "Chemical abundances of primeval galaxies from QSO absorption lines." Thesis, University of Cambridge, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.363292.

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Van, der Swaelmen Mathieu. "Évolution chimique du Grand Nuage de Magellan." Phd thesis, Université Nice Sophia Antipolis, 2013. http://tel.archives-ouvertes.fr/tel-00833887.

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Malgré des années de travaux théoriques et observationnels intensifs, nous sommes toujours loin d'une complète compréhension de l'univers proche, la Voie Lactée (MW) et ses galaxies voisines. Parmi les satellites de la MW, le Petit et le Grand Nuage de Magellan (LMC) sont particulièrement intéressants puisqu'ils forment le plus proche exemple de galaxies en interaction gravitationnelle et hydrodynamique, et partant, constituent un laboratoire unique pour étudier les effets des marées et l'échange de matière sur l'évolution chimique et l'histoire de la formation stellaire d'une galaxie. Le LMC est une galaxie de petite masse barrée à disque, prototype des galaxies riches en gaz que l'on pense jouer un rôle important dans la construction des grandes galaxies dans le cadre du ΛCDM. De plus, avec sa métallicité actuelle d'environ le tiers de la métallicité solaire, le chemin d'enrichissement chimique suivi par le LMC donne un grand poids aux yields des générations stellaires pauvres en métaux, ce qui fait du LMC un environnement idéal pour étudier la nucléosynthèse aux basses métallicités. Ce travail de doctorat vise à: 1) caractériser chimiquement la population de la barre du LMC, 2) comparer les tendances des éléments de la MW et du LMC et interpréter les différences ou ressemblance en termes d'évolution chimique et/ou de processus nucléosynthétiques (contraintes sur les sites et les processus nucléosynthétiques), 3) comparer l'évolution chimique de la barre et du disque interne du LMC et interpréter les différence ou ressemblance dans le contexte de la formation de la barre. Nos résultats montrent que l'histoire chimique du LMC a connu un forte contribution des supernovae de type I ainsi qu'un fort enrichissement en éléments s par les vents d'étoiles AGB pauvres en métaux. Par rapport à la MW, les étoiles massives ont eu une contribution plus petite à l'enrichissement chimique du LMC. Les différences observées entre la barre et le disque parlent en faveur d'un épisode de formation stellaire accrue il y a quelques Gyr, ayant lieu dans les zones centrales du LMC et conduisant à la formation de la barre. Ceci est en accord avec les histoires de la formation stellaire récemment dérivées.
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Jeon, Myoungwon, Gurtina Besla, and Volker Bromm. "Connecting the First Galaxies with Ultrafaint Dwarfs in the Local Group: Chemical Signatures of Population III Stars." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/627108.

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We investigate the star formation history (SFH) and chemical evolution of isolated analogs of Local Group (LG) ultrafaint dwarf galaxies (UFDs; stellar mass range of 10(2)M(circle dot) < M-*< 10(5) M-circle dot) and gas-rich, low-mass dwarfs (Leo P analogs; stellar mass range of 10(5)M(circle dot) < M-*< 10(6) M-circle dot). We perform a suite of cosmological hydrodynamic zoom-in simulations to follow their evolution from the era of the first generation of stars down to z=0. We confirm that reionization, combined with supernova (SN) feedback, is primarily responsible for the truncated star formation in UFDs. Specifically, halos with a virial mass of M-vir less than or similar to 2 x 10(9) M-circle dot form greater than or similar to 90% of stars prior to reionization. Our work further demonstrates the importance of Population. III stars, with their intrinsically high [C/Fe] yields and the associated external metal enrichment, in producing low-metallicity stars ([Fe/H] less than or similar to -4) and carbon-enhanced metal-poor (CEMP) stars. We find that UFDs are composite systems, assembled from multiple progenitor halos, some of which hosted only Population. II stars formed in environments externally enriched by SNe in neighboring halos, naturally producing extremely low metallicity Population II stars. We illustrate how the simulated chemical enrichment may be used to constrain the SFHs of true observed UFDs. We find that Leo P analogs can form in halos with M-vir similar to 4 x 10(9) M-circle dot 9 (z = 0). Such systems are less affected byreionization and continue to form stars until z = 0, causing higher-metallicity tails. Finally, we predict the existence of extremely low metallicity stars in LG UFD galaxies that preserve the pure chemical signatures of Population III nucleosynthesis.
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Spencer, Meghin E., Mario Mateo, Matthew G. Walker, and Edward W. Olszewski. "A Multi-epoch Kinematic Study of the Remote Dwarf Spheroidal Galaxy Leo II." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623237.

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We conducted a large spectroscopic survey of 336 red giants in the direction of the Leo II dwarf galaxy using Hectochelle on the Multiple Mirror Telescope, and we conclude that 175 of them are members based on their radial velocities and surface gravities. Of this set, 40 stars have never before been observed spectroscopically. The systemic velocity of the dwarf is 78.3 +/- 0.6 km s(-1) with a velocity dispersion of 7.4 +/- 0.4 km s(-1). We identify one star beyond the tidal radius of Leo II but find no signatures of uniform rotation, kinematic asymmetries, or streams. The stars show a strong metallicity gradient of -1.53 +/- 0.10 dex kpc(-1) and have a mean metallicity of -1.70 +/- 0.02 dex. There is also evidence of two different chemodynamic populations, but the signal is weak. A larger sample of stars would be necessary to verify this feature.
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Tinker, Jeremy L., Joel R. Brownstein, Hong Guo, Alexie Leauthaud, Claudia Maraston, Karen Masters, Antonio D. Montero-Dorta, et al. "The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624043.

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We present measurements of the clustering of galaxies as a function of their stellar mass in the Baryon Oscillation Spectroscopic Survey. We compare the clustering of samples using 12 different methods for estimating stellar mass, isolating the method that has the smallest scatter at fixed halo mass. In this test, the stellar mass estimate with the smallest errors yields the highest amplitude of clustering at fixed number density. We find that the PCA stellar masses of Chen et al. clearly have the tightest correlation with halo mass. The PCA masses use the full galaxy spectrum, differentiating them from other estimates that only use optical photometric information. Using the PCA masses, we measure the large-scale bias as a function of M-* for galaxies with logM(*) >= 11.4, correcting for incompleteness at the low-mass end of our measurements. Using the abundance matching ansatz to connect dark matter halo mass to stellar mass, we construct theoretical models of b(M-*) that match the same stellar mass function but have different amounts of scatter in stellar mass at fixed halo mass, sigma(logM*). Using this approach, we find sigma(logM*) = 0.18(+0.01) (-0.02). This value includes both intrinsic scatter as well as random errors in the stellar masses. To partially remove the latter, we use repeated spectra to estimate statistical errors on the stellar masses, yielding an upper limit to the intrinsic scatter of 0.16 dex.
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Books on the topic "Galaxies: abundance"

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Daniel, Friedli, ed. Abundance profiles: Diagnostic tools for galaxy history : proceedings from a workshop held at Université Laval, Québec, Canada, 12-15 October 1997. San Francisco, Calif: Astronomical Society of the Pacific, 1998.

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Observations of interstellar lines using the IUE satellite: Covering the years 1978-1988 : final report for NASA grant NSG-5248. Princeton, N.J: Princeton University Observatory, 1989.

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Book chapters on the topic "Galaxies: abundance"

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Vila-Costas, M. B. "Abundance Gradients in Spiral Galaxies." In The Interstellar Medium in Galaxies, 153–70. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5620-2_6.

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De Silva, Gayandhi. "Elemental Abundance Patterns of Disk Substructure." In Galaxies and their Masks, 293–304. New York, NY: Springer New York, 2010. http://dx.doi.org/10.1007/978-1-4419-7317-7_24.

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Díaz, Angeles I., and Enrique Pérez-Montero. "Empirical Abundance Determination for Ionized Nebulae." In The Evolution of Galaxies, 197. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-3313-7_43.

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Thomas, Daniel. "Abundance Ratios in Hierarchical Galaxy Formation." In The Evolution of Galaxies, 209. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-3313-7_49.

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De Freitas Pacheco, J. A., and R. D. D. Costa. "He Abundance in Red Giants." In The Stellar Populations of Galaxies, 418. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2434-8_85.

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Pipino, Antonio. "Abundances and Abundance Ratios in Stars and Hot Gas in Elliptical Galaxies." In Hot Interstellar Matter in Elliptical Galaxies, 163–206. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4614-0580-1_6.

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Palacios, A., J. Bolmont, C. Charbonnel, and F. Thévenin. "Abundance Anomalies in RGB Stars: Field vs GCs." In The Evolution of Galaxies, 213–14. Dordrecht: Springer Netherlands, 2002. http://dx.doi.org/10.1007/978-94-017-3311-3_40.

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Argast, D., M. Samland, O. E. Gerhard, and F. K. Thielemann. "Element Abundance Patterns of Metal-Poor Halo Stars." In The Evolution of Galaxies, 193. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-3313-7_41.

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Vila, M. B., and M. G. Edmunds. "Abundance Gradients and Physical Properties of Spiral Galaxies." In The Stellar Populations of Galaxies, 500. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2434-8_167.

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Skillman, Evan D. "Backyard Cosmology: Abundance Observations of Nearby Galaxies." In Chemical Evolution from Zero to High Redshift, 124–33. Berlin, Heidelberg: Springer Berlin Heidelberg, 1999. http://dx.doi.org/10.1007/978-3-540-48360-1_30.

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Conference papers on the topic "Galaxies: abundance"

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Walsh, Jeremy R., George H. Jacoby, Reynier F. Petetier, and Nicholas A. Walton. "Using planetary nebulae as abundance probes of galaxies." In Astronomical Telescopes and Instrumentation, edited by Jacqueline Bergeron. SPIE, 2000. http://dx.doi.org/10.1117/12.390136.

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François, P. "Abundance of heavy elements in extremely metal-poor stars." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: International Symposium on Origin of Matter and Evolution of Galaxies 2005: New Horizon of Nuclear Astrophysics and Cosmology. AIP, 2006. http://dx.doi.org/10.1063/1.2234403.

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Umeda, H. "The Abundance Pattern and Formation of Extremely Meta-Poor Stars." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: International Symposium on Origin of Matter and Evolution of Galaxies 2005: New Horizon of Nuclear Astrophysics and Cosmology. AIP, 2006. http://dx.doi.org/10.1063/1.2234384.

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Tachibana, Shogo. "The Abundance Of Live 60Fe In The Early Solar System." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: International Symposium on Origin of Matter and Evolution of Galaxies 2005: New Horizon of Nuclear Astrophysics and Cosmology. AIP, 2006. http://dx.doi.org/10.1063/1.2234417.

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Aoki, Misa, Wako Aoki, Yuhri Ishimaru, and Shinya Wanajo. "Diversity of abundance patterns of neutron-capture elements in very metal-poor stars." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2013: Proceedings of the 12th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG12). AIP Publishing LLC, 2014. http://dx.doi.org/10.1063/1.4874056.

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Konami, Saori, Kyoko Matsushita, and Toru Tamagawa. "A comparison of metal abundance patterns of inter-stellar medium in starburst and non-starburst galaxies." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2011. AIP, 2012. http://dx.doi.org/10.1063/1.4763393.

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Yokoyama, Tomohiro, and Nozomu Tominaga. "Nucleosynthesis in very massive Population III stars and the abundance patterns of the metal-poor stars." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2011. AIP, 2012. http://dx.doi.org/10.1063/1.4763434.

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Tominaga, N. "Population III Core-Collapse Supernova Yields and Extremely Metal-Poor Star Abundance Pattern." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: International Symposium on Origin of Matter and Evolution of Galaxies 2005: New Horizon of Nuclear Astrophysics and Cosmology. AIP, 2006. http://dx.doi.org/10.1063/1.2234468.

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Fujimoto, Shin-ichiro, Kei Kotake, Masa-aki Hashimoto, Masaomi Ono, Naofumi Ohnishi, Isao Tanihara, Hooi Jin Ong, et al. "Aspherical abundance distribution of ejecta from neutrino-driven core collapse supernova." In THE 10TH INTERNATIONAL SYMPOSIUM ON ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: OMEG—2010. AIP, 2010. http://dx.doi.org/10.1063/1.3485205.

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Aoki, W. "An abundance study of the most iron-poor star HE1327-2326 with Subaru/HDS." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: International Symposium on Origin of Matter and Evolution of Galaxies 2005: New Horizon of Nuclear Astrophysics and Cosmology. AIP, 2006. http://dx.doi.org/10.1063/1.2234382.

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You might also be interested in the extended bibliographies on the topic 'Galaxies: abundance' for particular source types:
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