- ID:
- ivo://CDS.VizieR/I/187
- Title:
- Tokyo Photoelectric Meridian Circle Catalog 1987
- Short Name:
- I/187
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The third annual catalog of the Tokyo PMC is presented for 5748 stars which had been observed at least two times in the year 1987 period, that is, from January 1, 1987, to December 31, 1987. The positions of the stars given in the catalog are those at the mean epoch of observations. The coordinates of the catalog are referred to the equinox and equator of J2000.0, based on the FK5 system. The mean trends of the observed positions minus FK5 positions for the FK5 basics stars are constructed and compared with those of the Tokyo PMC 86 catalog. The part I of the catalog contains the positions of 1017 FK5 basics (=FK4 stars ), 533 FK4 Suppl. stars, 2421 AGK3R stars, 1167 OB stars, 113 NPZT stars, and 84 SAO stars, and the part II of the catalog contains the positions of 413 SAO stars for occultation studies. These two parts were merged into a single pmc87 file.
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- ID:
- ivo://CDS.VizieR/I/188
- Title:
- Tokyo Photoelectric Meridian Circle Catalog 1988
- Short Name:
- I/188
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The fourth annual catalog of the Tokyo PMC is presented for 3800 stars (Part I and Part II) which had been observed at least two times in the 1988 period, that is, from January 1, 1988, to December 31, 1988. The positions of the stars given in the catalog are those at the mean epoch of observations. The coordinates of the catalog are based on the FK5 system, and are referred to the equinox and equator of J2000.0. The positions of five major and nine minor planets are also given in the present catalog (Part III) for all individual observations made in 1986 to 1988. The planetary positions are based on the same coordinate systems as those of the corresponding annual star catalogs, the Tokyo PMC Catalogs 86, 87, and 88. The mean trends of the observed positions - FK5 positions for the basic FK5 stars are constructed and compared with those of the Tokyo PMC Catalogs 86 and 87. As for the planets, their observed positions are compared with the positions of the JPL's planetary ephemeris DE200. We find that the ephemerides of the outermost planets, Uranus and Neptune, have some systematic deviations of a few tenths of arcsec in longitudes.
- ID:
- ivo://CDS.VizieR/I/167
- Title:
- Tokyo Photoelectric Meridian Circle Catalog 1986
- Short Name:
- I/167
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The second annual catalog of the Tokyo Photoelectric Meridian Circle contains 3974 stars that were observed at least twice between 21 December 1985 and 31 December 1986. Specifically, it contains 1141 FK5 stars, 971 FK4 supplemental stars, 554 AGK3R stars, 403 OB stars, 421 NPZT stars, and 484 SAO stars. The positions are for the mean epoch of observation referred to the equinox and equator of J2000.0 and based on the FK5 system. The internal error of a single observation for the bright stars is 0.24" and 0.27" in right ascension and declination, respectively. The catalog contains, in addition to the positions, the catalog from which the star is taken and the number in that catalog, the mean epoch and number of observations of each component of the position and of the magnitude, the spectral type, the V magnitude, and the DM and AGK3 numbers. It also contains the residuals between the position in this catalog and that in the source catalog and mean errors for each component of the position and of the magnitude.
- ID:
- ivo://CDS.VizieR/I/248
- Title:
- Tokyo Photoelectric Meridian Circle Catalog 90-93
- Short Name:
- I/248
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The sixth annual catalog of the Tokyo PMC is presented for 6649 stars which were observed at least two times in January 1990 through March 1993. The mean positions of the stars observed in the above period are given in the catalog at the corresponding mean epochs of observations of individual stars. The coordinates of the catalog are based on the FK5 system, and referred to the equinox and equator of J2000.0. The mean local deviations of the observed positions from the FK5 catalog positions are constructed for the basic FK5 stars to compare with those of the Tokyo PMC Catalog 89 and preliminary Hipparcos results of H30. The catalog contains the positions of 1180 basic FK5 stars, 322 FK4 Suppl. stars, 3132 AGK3R stars, 141 OB stars, 252 NPZT stars, and 1601 SAO stars observed with the Tokyo Photoelectric Meridian Circle in the 1990 to 1993 periods based on the FK5 system. The positions of the stars are given for the mean epoch of the observations of individual stars referring to the equinox and equator of J2000.0. The values of (O-C)s in the catalog are calculated by using the positions given in the source catalog, and by evaluating those at the mean epoch of observations of each star, with the equinox and equator at the mean epoch. The magnitudes of the stars given in the catalog can be transformed into the V-magnitude of the standard UBV system by the equation : V = V(TPMC) + 0.063(B-V) - 0.045.
- ID:
- ivo://CDS.VizieR/J/BaltA/20/1
- Title:
- Tombaugh 5 Vilnius photometry
- Short Name:
- J/BaltA/20/1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results of eight-color CCD photometry of 674 stars in the direction of the open cluster Tombaugh 5 in Camelopardalis. The stars are observed in the Vilnius system supplemented by the broad-band I filter; the field is of 22' diameter, the limiting magnitude is V=17.7mag. The catalog contains the coordinates, V magnitudes, seven color indices, two-dimensional spectral types determined from photometric parameters, interstellar extinctions and distances. The color-magnitude diagram plotted for 480 individually dereddened stars is used to identify cluster members and to determine the distance (1.74kpc) and age (200-250Myr) of the cluster. The fain test cluster stars classified are of spectral class G0. The cluster contains two blue stragglers of spectral classes B2-B4, both of them seem to be visual binaries. The extinction AV for the cluster stars is non-uniform, being spread between 2 and 3mag, with a mean value of 2.42mag. The extinction vs. distance dependence can be modeled by the Parenago exponential curve with two dust concentrations in the Camelopardalis dark clouds at about 150pc and the Cam OB1 association clouds at 0.9-1.0kpc.
- ID:
- ivo://CDS.VizieR/J/A+A/656/A99
- Title:
- Tomography with Magnification Bias
- Short Name:
- J/A+A/656/A99
- Date:
- 21 Mar 2022 07:10:35
- Publisher:
- CDS
- Description:
- High-z submillimetre galaxies can be used as a background sample for gravitational lensing studies thanks to their magnification bias. In particular, the magnification bias can be exploited in order to constrain the free parameters of a halo occupation distribution (HOD) model and some of the main cosmological parameters. A pseudo-tomographic analysis shows that the tomographic approach should improve the parameter estimation. In this work the magnification bias has been evaluated as cosmological tool in a tomographic set up. The cross-correlation function (CCF) data have been used to jointly constrain the astrophysical parameters M_min_, M_1_ and {alpha} in each one of the selected redshift bins, as well as the cosmological parameter {Omega}_M_, {sigma}_8_ and H_0_ for the lambda cold dark matter ({Lambda}CMD). Moreover, we explore the possible time evolution of the dark energy density introducing the {omaga}_0_ and {omage}_a_ parameters in the joint analysis ({omega}_0_CDM and {omega}_0_{omega}_a_CDM). The CCF was measured between a foreground spectroscopic sample of Galaxy And Mass Assembly galaxies and a background sample of Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) galaxies. The foreground sample was divided into four redshift bins (0.1-0.2, 0.2-0.3, 0.3-0.5, and 0.5-0.8) and the sample of H-ATLAS galaxies has photometric redshifts >1.2. The CCF was modelled using a halo model description that depends on HOD and cosmological parameters. Then a Markov chain Monte Carlo method was used to estimate the parameters for different cases. For the {Lambda}CDM model the analysis yields a maximum posterior value at 0.26 with [0.17, 0.41] 68% C.I. for {Omega}_M_ and at 0.87 with [0.75, 1] 68% C.I. for {sigma}_8_. With our current results H_0_ is not yet constrained. With a more general {omega}_0_CDM model, the constraints on {Omega}_M_ and {sigma}_8_ are similar, but we found a maximum posterior value for {omega}_0_ at -1 with [-1.56, -0.47] 68% C.I. In the {omega}_0_{omega}_a_CDM model, the results are -1.09 with [-1.72, -0.66] 68% C.I. for {omega}_0_ and -0.19 with [-1.88, 1.48] 68% C.I. for {omega}_a_. The results on Mmin show a trend towards higher values at higher redshift confirming recent findings. The tomographic analysis presented in this work improves the constraints in the {sigma}_8_-{Omega}_M_ plane with respect to previous findings exploiting the magnification bias and it confirms that magnification bias results do not show the degeneracy found with cosmic shear measurements. Moreover, related to dark energy, we found a trend of higher {omega}_0_ values for lower H_0_ values.
- ID:
- ivo://CDS.VizieR/II/131
- Title:
- Tonantzintla Pleiades Flare Stars
- Short Name:
- II/131
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The original catalog lists the flare stars discovered by different astronomical observatories over an area slightly larger than 20 square degrees in the Pleiades regions centered on Alcyone. Not all the flare stars are members of this cluster, membership indicators are provided in the catalog. The catalog, combining Tables 1 and 2 of the publication, gives the data for 1531 flares of 519 flare stars.
- ID:
- ivo://edu.gavo.org/hd/topcat_aladin_together
- Title:
- TOPCAT and Aladin working together
- Date:
- 27 Dec 2024 08:31:05
- Publisher:
- The GAVO DC team
- Description:
- This tutorial will show how tabular data can be easily transferred from Topcat to Aladin or the other way, and it will illustrate the benefits of this inter-client communication for VO users. This is shown with a quick look at filtering members of the Coma Cluster from SDSS.
- ID:
- ivo://edu.euro-vo.org/extern/asterics_topcatadvanced
- Title:
- TOPCAT/STILTS Advanced Tutorial
- Date:
- 27 Dec 2024 08:31:03
- Publisher:
- The GAVO DC team
- Description:
- This tutorial is a dense course through the advanced functions of TOPCAT and STILTS. It covers detailed information of how to use TOPCAT and STILTS to find data in the VO, access them, perform crossmatches and how to do visualisations.
- ID:
- ivo://CDS.VizieR/J/A+A/653/A87
- Title:
- TOPGot sample, SEDs and CH3CN analysis
- Short Name:
- J/A+A/653/A87
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- The TOPGot project targets a sample of 86 high-mass star-forming regions in different evolutionary stages from starless cores to ultra compact HII regions. The aim of the survey is to analyze different molecular species in a statistically significant sample to study the chemical evolution in high-mass star-forming regions, and identify chemical tracers of the different phases. In the first paper we present the sample and analyze the spectral energy distributions (SEDs) of the TOPGot sources to derive physical parameters. We also use the MADCUBA software to analyze the emission of methyl cyanide (CH_3_CN), a well-known tracer of high-mass star formation. The emission of the CH_3_CN(5K-4K) K-transitions has been detected towards 73 sources (85% of the sample). The emission of CH_3_CN has been detected towards all evolutionary stages, with the mean abundances showing a clear increase of an order of magnitude from high-mass starless-cores to later evolutionary stages. We found a conservative abundance upper limit for high-mass starless cores of X_CH_3_CN_<4.0x10^-11^, and a range in abundance of 4.0x10^-11^<X_CH_3_CN_<7.0x10^-11^ for those sources that are likely high-mass starless cores or very early high-mass protostellar objects. In fact, in this range of abundance we have identified five sources previously not classified as being in a very early evolutionary stage. The abundance of CH_3_CN can thus be used to identify high-mass star-forming regions in early phases of star-formation.
