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    %Z References

    Neubauer, F. J.; Burwell, C. G.; Miller, W. C.

    Roberts, L. C., Jr.

    AA(first author's institution) AB(second author's institution) ...

    <EMAIL>email address</EMAIL>

    (C) 1990: American Astromomical Society

    %Z Bechtold,~J., \etal 1994, \aj, 108, 374
       Massa, D. L., & Savage, B. D. 1984, ApJ, 279, 310
       Savage, B. D., & Mathis, J. S. 1979, ARA&A, 17, 73

 %R 1993ApJ...415...50C
 %A Cavaliere, A.; Colafrancesco, S.; Menci, N.
 %J Astrophysical Journal, Part 1, vol.415, no. 1, p. 50-57.
 %D 09/1993
 %L 57
 %T Distant clusters of galaxies detected by X-rays
 %K Cosmic Plasma, Dark Matter, Galactic Clusters, X-ray Astronomy, Baryons, 
    Luminosity, Redshift
 %B The dynamical masses of groups and clusters of galaxies decrease on average
 with increasing redshift, after the hierarchical cosmogonies dominated by
 direct collapses of dark matter overdensities. We show that the masses of
 intracluster plasma emitting in the X-ray band are to decrease more rapidly. We
 also show that consideration of the intrinsic spread in the dynamical formation
 times leads us to predict more numerous faint sources at given dynamical mass.
 The model we compute yields steeper luminosity functions in the X-ray band with
 a specific change in lookback time: the bright end shifts back. Such negative
 evolution is fast even at modest redshifts z less than about 0.5 if the
 external gas infalling into groups of clusters was preheated and has cooled
 down after z of about 1.5-2. If so, the evolution is considerably faster in the
 X-ray than in the optical band, comparing interestingly with data from the
 existing surveys.
 %Z Abell, Ci. 0. 1958, ApJS, 3, 211
 Barcons, X., Fabian, A. C., & Rees, M. J. 1991, Nature, 350, 685
 Bardeen, J. M., Bond, J. R., Kaiser, N., & Szalay, A. 5. 1986, ApJ, 403, 15
 Blumenthal, Ci., Faber, S. M., Primack, J. R., & Rees, M. J. 1984, Nature, 311, 517
 Bohringer, H., et al. 1991, in Proc. NATO ASI "Clusters and
 %Superclusters of Galaxies," ed. A. C. Fabian (Dordrecht: Kluwer), 71 
 Burg, R., Cavaliere, A., & Menci, N. 1993, ApJ, 404, L55
 Cavaliere, A., Gursky, H., & Tucker, W. H. 1971, Nature, 231, 437
 Cavaliere, A., & Colafrancesco, 5. 1988, ApJ, 331, 660
 ---. 1990, in Clusters of Galaxies (Cambridge: Cambridge Univ. Press), 43
 Cavaliere, A., Burg, R., & Giacconi, R. 1991, ApJ, 366, L61
 
 %T Adsorption behavior of a textile dye of Reactive Blue 19 from
 aqueous solutions onto modified bentonite   
 %A Gök, Özer; Safa Özcan, A.;Özcan, Adnan
 %P 5439

 %T Seeing Red: Extremely Red Objects from the Cadis K' Survey
 %A Thompson, D.; Beckwith, S. V. W.
 %F Max-Planck-Institut fuer Astronomie, Koenigstuhl 17, D-69117
 Heidelberg, Germany
 %P 13
 %B We discuss various interpretations of the nature of extremely red
 objects (EROs), discovered in the first of 7 deep, wide-field K'
 images in the CADIS survey. Point sources with K' = 20.5 mag are
 detected at the 5 sigma level over an area of 125 arcmin^2. A total
 of 20 EROs meeting the selection criteria (R-K') >= 6^{m} and K' <=
 19.75 mag were selected from the data, giving a surface density of
 0.16 +/- 0.04 arcmin^{-2} for all EROs and 0.016 +/- 0.011
 arcmin^{-2} for bright (K' < 19^{m}) EROs.} 

 %T Chandra observations of M31 and their implications for its ISM
 %A Primini, F., Garcia, M., Murray, S., Forman, W., Jones, C., and McClintock, J.
 %F AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, USA),
 %AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, USA),
 %AC(Harvard-Smithsonian Center for Astrophysics, Cambridge, USA),
 %AD(Harvard-Smithsonian Center for Astrophysics, Cambridge, USA),
 %AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, USA),
 %AF(Harvard-Smithsonian Center for Astrophysics, Cambridge, USA) 
 %B We have been regularly observing the bulge and inner disk of M31
 for nearly one year, using both the HRC-I and ACIS-I instruments on
 the Chandra X-Ray Observatory. We present results from our program
 that are of interest to the study of the ISM in M31. In particular,
 we find that the unresolved emission within 3' of the center of M31
 has a distinctly softer spectrum than that of most of the resolved
 X-ray sources in the region. Preliminary spectral analysis of bright
 point sources in the bulge shows no evidence (within the poor
 statistics) for soft spectral components, but does reveal significant
 extra-galactic X-ray extinction (NH ~ 1021 cm-2). We find no new
 X-ray counterparts to supernova remnants to date. 

 %T We Do Not Forget Johannes Kepler
 %A Wszołek, B
 %B Year 2009 was announced as the International Year of
 Astronomy. This was to mark 400th anniversary of the first
 astronomical observation through a telescope by Galileo. From the
 other hand, this year marks 400th anniversary of Astronomia Nova, the
 famous work of Kepler published in Prague in 1609. Two laws of
 planetary motions opened human efforts to understand gravitational
 force; so the overall cosmic space conquest, with its great
 importance not only for astronomy, was developed thankful to Kepler's
 work. This contribution is thought to show the most inspiring ideas
 of Johannes Kepler, published in Astronomia Nova and in other his
 books. 
 %I PDF: FILE:proc16_02.pdf

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• Bibliographic Codes: Bibliographic codes are in the form: YYYYJJJJJVVVVPPPPPA, where YYYY is the year of publication, JJJJJVVVV is the abbreviation of the conference proceeding, PPPPP is the page number, and A is the first letter of the first author's surname (see Bibcodes )
  
  

        %R 1996eds..proc.....L
        %T The Extragalactic Distance Scale, Proceedings of the ST ScI May Symposium
        %A Livio, M.; Donahue, M.; Panagi, N.
        %J The Extragalactic Distance Scale, Proceedings of the ST ScI
           May Symposium, held in Baltimore, MD,
           May 7 - 10, 1996, Eds.: M. Livio, M. Donahue, and N. Panagia,
           Cambridge University Press.
        %D 00/1996