A new catalogue of clusters in the Large Magellanic Cloud has been constructed from searches of the IIIa-J component of the ESO/SERC Southern Sky Atlas. The catalogue contains coordinate and diameter measurements of 1762 clusters in a 25x25{deg} area of sky centred on the LMC, but excluding the very crowded 3.5 square deg. region around the Bar. The distribution of these clusters appears as two superimposed elliptical systems. The higher density inner system extends over about 8d; the lower density outer system can be represented by 13d X 10d disc inclined at 42d to the line of sight. There are suggestions of two weak "arms" in the latter.
This is CMC12 (Version 1.0), an astrometric and photometric catalogue of 6.3 million stars in the red magnitude range 9 to 17. The Carlsberg Meridian Telescope (CMT) underwent a major upgrade in March 1999. A 2k by 2k CCD camera was installed with a Sloan r' filter operating in a drift scan mode. With the new system, the magnitude limit is r'_CMT_=17 and the positional accuracy is about 0.035". The main task of the CMT is to map the sky in the declination range -3{deg} to +30{deg} with the aim of providing an astrometric, and photometric, catalogue that can accurately transfer the Hipparcos/Tycho reference frame to Schmidt plates. The current release (Version 1.0) comprises all the observations made between March 1999 and March 2002 with the new CCD in the declination band -3{deg} to +3{deg}. It is intended to release the rest of the catalogue later. A more complete description is available in the documentation at http://www.ast.cam.ac.uk/~dwe/SRF/cmc12/cmc12_documentation.ps or http://www.ast.cam.ac.uk/~dwe/SRF/cmc12/cmc12_documentation.pdf
The Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2) obtained spectroscopic redshifts for about 6200 galaxies to a nominal limit of R=21.5. The survey area of about 1.5 square degrees was spread over four patches on the sky. This catalog presents photometry and redshifts for all galaxies in the CNOC2 0223+00 Patch (area of 1409 square arcminutes). A future paper will provide catalogs for the other three patches.
Multiple star systems are commonly assumed to form coevally; they thus provide the anchor for most calibrations of stellar evolutionary models. In this paper, we study the binary population of the Taurus-Auriga association, using the component positions in an HR diagram in order to quantify the frequency and degree of coevality in young binary systems. After identifying and rejecting the systems that are known to be affected by systematic errors (due to further multiplicity or obscuration by circumstellar material), we find that the relative binary ages, |{Delta}log{tau}|, have an overall dispersion {sigma}_|{Delta}log{tau}|_~0.40dex.
The tutorial uses VOSA to analyse members of the Collinder 69 open
cluster by crossmatching a given local set of objects and accesses VO
services to crossmatch the objects with 2MASS to receive colors. The
resulting SEDs are analysed using different fit functions.
The Arecibo Ultra-Deep Survey (AUDS) is a blind HI survey aimed at detecting galaxies beyond the local Universe in the 21-cm emission line of neutral hydrogen (HI). The Arecibo L-band Feed Array (ALFA) was used to image an area of 1.35deg^2^ to a redshift depth of 0.16, using a total on-source integration time of over 700h. The long integration time and small observation area makes it one of the most sensitive HI surveys, with a noise level of ~75{mu}Jy per 21.4kHz (equivalent to 4.5km/s at redshift z=0). We detect 247 galaxies in the survey, more than doubling the number already detected in AUDS60. The mass range of detected galaxies is log(M_HI_[h_70_^-2^M_{sun}_])=6.32-10.76. A modified maximum likelihood method is employed to construct an H I mass function (HIMF). The best fitting Schechter parameters are low-mass slope {alpha}=-1.37+/-0.05, characteristic mass log(M^*^[h_70_^-2^M_{sun}_])=10.15+/-0.09, and density {Phi}_*_=(2.41+/-0.57)x10^-3^h_70_^3^Mpc^-3^/dex. The sample was divided into low- and high-redshift bins to investigate the evolution of the HIMF. No change in low-mass slope {alpha} was measured, but an increased characteristic mass M*, was noted in the higher redshift sample. Using Sloan Digital Sky Survey data to define relative galaxy number density, the dependence of the HIMF with environment was also investigated in the two AUDS regions. We find no significant variation in {alpha} or M*. In the surveyed region, we measured a cosmic HI density {Omega}_HI_=(3.55+/-0.30)x10^-4^h_70_^-1^. There appears to be no evolutionary trend in {Omega}_HI_ above 2{sigma} significance between redshifts of 0 and 0.16.
Within this use case you learn about the constellations of the
Zodiac, i.e. those crossed by the apparent path of the Sun during the
year. Together with some characteristics the orbital motion of the
Earth, in this use case you also find a short excursion into history
of astronomy. The use case also introduces the precession of the
equinoxes.
Here we list the CORALIE radial-velocity measurements for HD 75289 and HD 130322. CORALIE is a fiber-fed echelle spectrograph designed for high-precision radial-velocity measurements. It is mounted on the 1.2-m "Leonard Euler" Swiss Telescope at ESO-La Silla Observatory (Chile).
Table 1 contains the CORALIE radial-velocity measurements for the stellar system HD41004. CORALIE is a fiber-fed echelle spectrograph designed for high-precision radial-velocity measurements. It is mounted on the 1.2-m "Leonard Euler" Swiss Telescope at ESO-La Silla Observatory (Chile).
Table 1-6 contain the CORALIE radial-velocity measurements for the 6 Solar-type stars hosting planetary companions: GJ 3021 (HD 1237), HD 52265, HD 169830, iota Hor (HD 17051), HD 210277 and HD 217107. CORALIE is a fiber-fed echelle spectrograph designed for high-precision radial-velocity measurements. It is mounted on the 1.2-m "Leonard Euler" Swiss Telescope at ESO-La Silla Observatory (Chile).