M1 image More About M1 Nice Color Picture . ... M16 image More About M16 HST image . ... M31 image More About M31 Nice Color Picture . ... M42 image ; M43 image More About M42/43 Nice Color CCD Picture . M51 image More About M51 Color Image of M51 M51 Supernova . M57 image More About M57 Nice Color CCD Picture Very Deep M57 Image . ... M81 image More About M81 M81 Supernova Ultraviolet Image of M81 More about Ultraviolet Imaging . M82 image More About M82 M82 False Color M82 True Color . ...

... The search for distant objects which can be both galaxies and quasars is one of the most important problems of observational astrphysics, because it allows one to determine cosmological parameters connected with the time of appearence and evolution of stellar systems, large scale structure of the Universe. ... Radio galaxies are important objects to be studied because they are sources of infrared-optical-ultraviolet continuum, emission lines and continual radio emission. ...

The presence of dust in starburst galaxies complicates the study of their stellar populations as the dust's effects are similar to those associated with changes in the galaxies' stellar ages and metallicities. ... We present the calibration of the flux ratio method for calculating the dust attenuation at a particular wavelength, Att(ЮЛ), based on the measurement of the F(IR)/F(ЮЛ) flux ratio. ... However, at longer wavelengths the relationship is dependent on the assumed stellar properties. ...

... Distant Galaxies in Radio Vision . ... Pentrating obscuring dust, the false-color EVN radio images are inset above according to their relative location in an optical image of the famous Hubble Deep Field region of the sky. ... Impressively, the radio sources appear to be so small, less than about 600 light-years across in actual size, that they are thought to be associated with massive central black holes in the distant deep field galaxies. ... Jumbled Galaxy Centaurus A . ...

Next: Evolution of Supernova Explosion Up: Gravitational Waves from Coalescing Previous: Gravitational Waves from Coalescing . The stochastic binary background produced by nearby galaxies from Tully's catalog at the frequency  Hz is shown in Figure  49 in terms of average strain metric amplitude per square degree in a given direction ( l , b ) on the sky: . where the sum is calculated over all sources in the given square degree of the sky; we assumed . ...

... QSO spectra in the ROSAT band are steeper than the background at harder energies, and furthermore at fluxes below 1E-14 ergs/(s cmќ) the quasar source counts flatten off and are replaced by more numerous populations of relatively low red-shift objects, apparently Narrow Emission Line Galaxies (NELG). ... We extracted the luminosity function from ROSAT Deep Survey results, and extrapolated by a factor of 2 - 3 to account for changes expected in the harder XMM band. ...

... The sample of the Local Volume galaxies (distance smaller than 10 Mpc) gives a unique opportunity to study the properties of galaxies including the weakest objects: the absolute magnitude M B -10 and the virial mass M vir 10 9 M x263C;. ... Luminosity function of the Local Volume galaxies. ... The luminosity functions for galaxies are presented: red dashed line - from the 2dFGRS survey (Norberg et al. 2002); blue dash-dotted line - from the SDSS survey (Blanton et al. ...

An Ancient Universe: How Astronomers Know the Vast Scale of Cosmic Time . THE ANCIENT UNIVERSE . c) The Age of Light from the Most Distant Galaxies: The "Time Machine" Effect . ... Thus we are actually seeing these galaxies not as they are today, but as they were billions of years ago. ... The Universe: An Overview | ... The Ancient Universe - The Age of the Expanding Universe - The Age of the Oldest Stars - The Age of Light From Distant Galaxies - The Age of the Chemical Elements | ...

As the Universe expands, gravity pulls on the Universe, and slows the expansion down over time. As we look to great distances, we are looking back in time. If we can measure how fast the Universe is expanding in the past, and compare it to how fast it is expanding now, we can see the total gravitational effect of all matter in the Universe. Here we plot the distance between two galaxies as a function of time. ... Universes with lots of material . ...

... We measured these galaxies individually, and they are distinguished in our list by the suffixes a, b, c,... in order of increasing J2000 right ascension. ... The first column contains the UGC catalog number, to which we have added lower-case suffixes a, b, c,\dots in order of increasing J2000 right ascension to distinguish individual galaxies in groups. ... The third column lists the degrees, arcminutes, and arcseconds of J2000 declination plus the rms uncertainty in arcseconds. ...

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