... 000, 1­13 (2010) Printed 21 September 2011 A (MN L TEX style file v2.2) A universal ultraviolet-optical colour­colour­magnitude relation of galaxies I1gor V. Chilingarian1,2, and Ivan Yu. ... Received 2011 Sep 15; in original form 2011 Feb 6 ABSTRACT The bimodal galaxy distribution in the optical colour­magnitude diagram (CMD) comprises a narrow "red sequence" populated mostly by early-type galaxies and a broad "blue cloud" dominated by star-forming systems. ...

... Positions and Proper Motions of 258,997 Stars for the Epoch and |Equinox of 1950.0", Publ. of the Smithsonian Institution of |Washington, D.C., No. ... 1971-1979, "Lowell Proper Motion Survey" |(red dwarfs), Lowell Obs. ... LHS |Luyten, W. J. 1976, "A Catalog of Stars with Proper Motion |exceeding 0".5 annually", Publ. of Univ. of Minnesota, |Minneapolis, Minnesota; Luyten, W. J., Albers, H. 1979, "An |Atlas of Identification Chart for LHS Stars", Publ. of Univ. of |Minnesota, Minneapolis, Minnesota...

VARIABLE STARS, THE GALACTIC HALO AND GALAXY FORMATION C. Sterken, N. Samus and L. Szabados (Eds.) 2010 Formation Mechanisms for Spheroidal Stellar Systems O. K. Sil'chenko 1 Sternberg Astronomical Institute of the Moscow State University, Moscow, Russia Abstract. Spheroidal stellar systems on various scales include elliptical galaxies, dwarf spheroidal galaxies, and globular stellar clusters. ... The formation mechanisms of the oldest globular clusters represent a puzzle yet. ... 2009). ...

... 337, 275­292 (2002) The correlation of line strength with luminosity and redshift from composite quasi-stellar object spectra S. M. Croom,1 K. Rhook,1 E. A. Corbett,1 B. J. Boyle,1 H. Netzer,2 N. S. Loaring,3 L ... We measure highly significant Baldwin effects for most broad emission lines (C IV 1549, C III] 1909, Mg II 2798, H ,H ) and show that they are predominantly caused by correlations with luminosity, not redshift. ... The correlations of log W with log(1 + z ) for each line. ...

... The spectrum of the brightest star, our Sun, shows several dark gaps perpendicular to the flow of it’s colours (figure 1). These so called spectral absorption lines where discovered in 1802 by the English scientist William Wollaston. ... Some stars as Pollux show a spectrum similar to that of our sun with strong Ca II and Fe II lines, others as Sirius or Vega show strong absorption lines of hydrogen, others, as Mira show very complicated spectra due to molecular absorption lines (see figure 5). ...