標(biāo)題: Titlebook: Galaxy Scaling Relations: Origins, Evolution and Applications; Proceedings of the E Luiz Nicolaci Costa,Alvio Renzini Conference proceeding [打印本頁(yè)] 作者: 從未沮喪 時(shí)間: 2025-3-21 17:08
書目名稱Galaxy Scaling Relations: Origins, Evolution and Applications影響因子(影響力)
書目名稱Galaxy Scaling Relations: Origins, Evolution and Applications影響因子(影響力)學(xué)科排名
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書目名稱Galaxy Scaling Relations: Origins, Evolution and Applications被引頻次
書目名稱Galaxy Scaling Relations: Origins, Evolution and Applications被引頻次學(xué)科排名
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書目名稱Galaxy Scaling Relations: Origins, Evolution and Applications年度引用學(xué)科排名
書目名稱Galaxy Scaling Relations: Origins, Evolution and Applications讀者反饋
書目名稱Galaxy Scaling Relations: Origins, Evolution and Applications讀者反饋學(xué)科排名
作者: Rinne-Test 時(shí)間: 2025-3-21 21:02
On Governance: Decision-Making in Families, . The ultraviolet Tully-Fisher relation of the HDF galaxies has a similar slope and zero-point to that of spiral galaxies nearby. These results should be taken with caution as there remain a number of potentially important systematic effects which remain to be calibrated.作者: Conclave 時(shí)間: 2025-3-22 03:10
The Role of Photoionization During Galaxy Formationating should have occurred in the past universe. Photoionization seems not to be adequate anyway. We briefly discussed an alternative possibility based on a warm IGM picture. In this picture photoionization may allow low mass galaxy formation which is inhibited otherwise.作者: intention 時(shí)間: 2025-3-22 06:32 作者: 條街道往前推 時(shí)間: 2025-3-22 11:03
The Physical Origin of the Fundamental Plane (of Elliptical Galaxies)le of orbital anisotropy and its relation with the FP thickness are also discussed. None of the explored solutions — albeit formally correct — are easily acceptable from a physical point of view, due to the ever-present problem of the required fine-tuning.作者: negligence 時(shí)間: 2025-3-22 16:31
1431-2433 .. in its own specific, peculiar way. Hence, for a complete description, galaxy taxonomy may ask for finer and finer classification schemes. However, for some applications it may be more fruitful to let details aside and focus on some global properties of galaxies. One is then seeking to measure jus作者: negligence 時(shí)間: 2025-3-22 17:35 作者: RLS898 時(shí)間: 2025-3-22 22:52
https://doi.org/10.1057/9780230339644f greater than allowed by observations. Unless halos of spiral galaxies formed at high redshift (. ? 1) and did not later accrete any significant amount of mass, the TullyFisher relation is not likely to be the direct result of cosmological initial conditions but rather a consequence of a subsequent feedback process.作者: allergy 時(shí)間: 2025-3-23 05:14
Survival Tips for the Younger Cliniciannd the upcoming wide-field cameras, super-seeing imaging instruments, and the 8-m class telescopes will provide a great opportunity for the study of the mass distribution of isolated and cluster galaxies.作者: Communal 時(shí)間: 2025-3-23 05:33
Christen D. Upper,Susan S. Hiranore formed early in elliptical galaxies, and give a reassuring confirmation of many previous contentions that the CM relation takes its origin at early times probably from galactic wind feedback. This conclusion is independent of the IMF, the SFR and the cosmological parameters.作者: glacial 時(shí)間: 2025-3-23 13:13
Can the Tully-Fisher Relation Be the Result of Initial Conditions?f greater than allowed by observations. Unless halos of spiral galaxies formed at high redshift (. ? 1) and did not later accrete any significant amount of mass, the TullyFisher relation is not likely to be the direct result of cosmological initial conditions but rather a consequence of a subsequent feedback process.作者: 舞蹈編排 時(shí)間: 2025-3-23 15:32
Dark Halo Scaling from Galaxy-Galaxy Lensingnd the upcoming wide-field cameras, super-seeing imaging instruments, and the 8-m class telescopes will provide a great opportunity for the study of the mass distribution of isolated and cluster galaxies.作者: 新陳代謝 時(shí)間: 2025-3-23 21:01 作者: 公社 時(shí)間: 2025-3-24 00:10 作者: MERIT 時(shí)間: 2025-3-24 03:32 作者: NOVA 時(shí)間: 2025-3-24 06:49 作者: reflection 時(shí)間: 2025-3-24 11:27
On the Phenomenology of Disk Galaxiesn-linearly with mass. These evidences provide observational constraints to models of disk-galaxy evolution. They find a natural interpretation if it is assumed that the time scale . of protogalaxy collapse is governed primarily by the system initial mass as ...作者: 無(wú)價(jià)值 時(shí)間: 2025-3-24 17:47 作者: neutral-posture 時(shí)間: 2025-3-24 20:04
Michael Prieler,Florian KohlbacherIn this brief contribution, I will outline hopes of understanding the origin of galaxy scaling relations using numerical simulations as a tool to gain understanding. The case of the Tully-Fisher relation for disk galaxies is used as a working example to illustrate the modest achievements to date and the difficult tasks ahead.作者: affect 時(shí)間: 2025-3-24 23:17 作者: adumbrate 時(shí)間: 2025-3-25 07:19 作者: Cardiac 時(shí)間: 2025-3-25 07:44
The Tully-Fisher Relation: A Numerical Simulator’s PerspectiveIn this brief contribution, I will outline hopes of understanding the origin of galaxy scaling relations using numerical simulations as a tool to gain understanding. The case of the Tully-Fisher relation for disk galaxies is used as a working example to illustrate the modest achievements to date and the difficult tasks ahead.作者: cognizant 時(shí)間: 2025-3-25 14:05 作者: 不要不誠(chéng)實(shí) 時(shí)間: 2025-3-25 19:30
Stellar Populations in Bulges of Spiral GalaxiesWe discuss the integrated properties of the stellar population in bulges along the Hubble sequence and new HST data for individual stars in the bulge of M31.作者: Androgen 時(shí)間: 2025-3-25 23:58 作者: 剛毅 時(shí)間: 2025-3-26 00:38 作者: 小溪 時(shí)間: 2025-3-26 06:36 作者: 不遵守 時(shí)間: 2025-3-26 11:18 作者: 注意力集中 時(shí)間: 2025-3-26 16:28 作者: FRAX-tool 時(shí)間: 2025-3-26 17:48 作者: 群居動(dòng)物 時(shí)間: 2025-3-26 22:59 作者: 廚房里面 時(shí)間: 2025-3-27 04:16 作者: Lacerate 時(shí)間: 2025-3-27 06:12
https://doi.org/10.1007/978-1-4419-1034-9ies and potentially to test the extent of their dark matter halos as a function of the density of the environment. Here I describe simulations of observational data and present a maximum likelihood method to infer the average properties of an ensemble of cluster galaxies.作者: intoxicate 時(shí)間: 2025-3-27 09:32 作者: VICT 時(shí)間: 2025-3-27 14:07 作者: 小平面 時(shí)間: 2025-3-27 21:32 作者: Intercept 時(shí)間: 2025-3-28 02:01 作者: 谷類 時(shí)間: 2025-3-28 05:35
https://doi.org/10.1007/978-3-540-85910-9henomenology of late-type galaxies in the local Universe is revised as follows: 1) M/L in the NIR is constant; 2) population I indicators, namely: the atomic hydrogen content, the current star formation rate, the luminosity and the surface brightness of the young stellar population, traced by the bl作者: intolerance 時(shí)間: 2025-3-28 06:29
Christen D. Upper,Susan S. Hirano) is adopted and model parameters are adjusted to reproduce the CM relation of Coma ellipticals. Two evolutionary sequences are calculated under the contexts of . and age ., both can equally explain the CM relation at the present epoch. The confrontation with the observational CM diagrams of E/SO ga作者: 揉雜 時(shí)間: 2025-3-28 13:33 作者: 擔(dān)心 時(shí)間: 2025-3-28 16:42
Galaxy Scaling Relations: Origins, Evolution and Applications978-3-540-69654-4Series ISSN 1431-2433 Series E-ISSN 1611-6143 作者: Panacea 時(shí)間: 2025-3-28 19:41
https://doi.org/10.1007/978-1-4419-1034-9ies and potentially to test the extent of their dark matter halos as a function of the density of the environment. Here I describe simulations of observational data and present a maximum likelihood method to infer the average properties of an ensemble of cluster galaxies.作者: 衣服 時(shí)間: 2025-3-29 00:34
Advocacy for Teacher Leadershipbution of lowmass early-type galaxies in the space of observable parameters. The changes in mass-tolight ratio from the faintest Local Group dwarf spheroidals to bright dwarf ellipticals, and the dark-matter content of early-type dwarfs, are also briefly discussed.作者: 南極 時(shí)間: 2025-3-29 06:57
Constraining the Mass Distribution of Cluster Galaxies by Weak Lensingies and potentially to test the extent of their dark matter halos as a function of the density of the environment. Here I describe simulations of observational data and present a maximum likelihood method to infer the average properties of an ensemble of cluster galaxies.作者: 啞巴 時(shí)間: 2025-3-29 10:57 作者: 性滿足 時(shí)間: 2025-3-29 14:59
The Physical Origin of Galaxy Scaling Relations dark and dissipationless and to cluster hierarchically from gaussian initial conditions. Gas moves under the gravitational influence of this dark matter, settling dissipatively at the centres of dark halos to form galaxies. The evolution of the dark matter component has been studied extensively by 作者: CON 時(shí)間: 2025-3-29 17:57 作者: Self-Help-Group 時(shí)間: 2025-3-29 23:38 作者: Conducive 時(shí)間: 2025-3-30 03:03
The Physical Origin of the Fundamental Plane (of Elliptical Galaxies)ties are presented that can produce the observed uniform departure from . (structural, dynamical) and/or from a constant . mass-to-light ratio. The role of orbital anisotropy and its relation with the FP thickness are also discussed. None of the explored solutions — albeit formally correct — are eas作者: Bombast 時(shí)間: 2025-3-30 07:17
The Role of Photoionization During Galaxy Formations well as in the mechanism controlling their distribution. The cooling criteria seems to be useful in order to distinguish halos which might form a galaxy from those which may form a cluster. However the same criteria imply the so-called “overcooling” problem, which pointed out that substantial rehe作者: 要求比…更好 時(shí)間: 2025-3-30 08:30 作者: 禍害隱伏 時(shí)間: 2025-3-30 13:45
Dark Halo Scaling from Galaxy-Galaxy Lensingw of the mass distribution in galaxies implies the existence of a dark halo which extends far beyond the radius at which dynamical tracers can be observed. Gravitational lensing by galaxies offers the possibility to trace the halo profile to radii beyond ,~ 30.. kpc and may become the most sensitive作者: 休戰(zhàn) 時(shí)間: 2025-3-30 19:57 作者: convulsion 時(shí)間: 2025-3-31 00:04
Galaxy-Galaxy Lensing in the Hubble Deep Field: the Halo Tully-Fisher Relation at High Redshiftt luminosities of galaxies. We detect a lensing signal at the ~ 98% confidence level from only 468 galaxies. Preliminary results suggest that the lensing galaxies in the HDF at a typical redshift of ~ 1.2 follow a Tully-Fisher-like relation with dark matter halo circular velocities of 200 ± 50 km s.作者: 圓錐體 時(shí)間: 2025-3-31 04:00 作者: Barter 時(shí)間: 2025-3-31 07:10 作者: Coma704 時(shí)間: 2025-3-31 11:09
Bimodality of Freeman’s Lawal surface brightnesses is found to be bimodal. The bimodality is particularly significant at . because obscuration is not a problem and because the high surface brightness galaxies are redder than the low surface brightness galaxies so the bifurcation is greater. The bimodality signal is especially
