Titlebook: Highlights of Spanish Astrophysics II; Proceedings of the 4 Jaime Zamorano,Javier Gorgas,Jesús Gallego Conference proceedings 2001 Springer

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書目名稱Highlights of Spanish Astrophysics II影響因子(影響力)




書目名稱Highlights of Spanish Astrophysics II影響因子(影響力)學科排名




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書目名稱Highlights of Spanish Astrophysics II網絡公開度學科排名




書目名稱Highlights of Spanish Astrophysics II被引頻次




書目名稱Highlights of Spanish Astrophysics II被引頻次學科排名




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書目名稱Highlights of Spanish Astrophysics II年度引用學科排名




書目名稱Highlights of Spanish Astrophysics II讀者反饋




書目名稱Highlights of Spanish Astrophysics II讀者反饋學科排名

最低點

The Coma Cluster of Galaxies: Spectral Classification and Star Formation with the Sloan Digital Sky let analysis. We find that these classification schemes are in broad agreement and can provide physical insight into the evolutionary histories of our cluster galaxies. We find that a significant fraction (25%) of our observed Coma galaxies show signs of recent star-formation activity.

使人煩燥

Seyfert Galaxies at the Mid-Infrared: ISOCAM Observationsfrom 16 to 120 .m (ISOPHOT data). We find that the correlation between mid-IR nuclear emission and total emission is lost beyond 120 .m, which suggests that at far-IR the host galaxy emission dominates.

拋物線

恫嚇

Orgasm

Star-Forming Galaxies from the UCM-CIDA-YALE Surveyble to obtain a large sample of star-forming galaxy candidates in the local universe. The UCY survey aims to be the most extense colection of low luminosity star forming galaxies down to ..= ?12. The global properties of the survey are presented.

epicondylitis

枯萎將要

SPASM

A new Code for Hydrodynamical Simulations in Cosmologyimportant features of our code are: 1) it includes the ?. correction terms appearing when the spatial resolution .(., .) is not a constant, and 2) time stepping is performed from a PEC scheme (Predict — Evaluate -Correct) modified to allow for individual time-steps.

HIKE

Evolution of the Star Formation Rate in Different Cosmological ScenariosFrom our results, the existence of a characteristic epoch of star formation around . ~ 2 seems very unlikely, although it would be conve-nient to wait until the forthcoming high redshift surveys become available to confirm or reject this prediction.