- ID:
- ivo://CDS.VizieR/I/274
- Title:
- CCDM (Catalog of Components of Double & Multiple stars)
- Short Name:
- I/274
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This is the second edition of the Catalogue of the Components of Double and Multiple stars (CCDM). The first one, of which a detailed description has been given in Communication de l'Observatoire Royal de Belgique, Serie A, 115, 1994, may be found at the CDS under reference <I/211>. The complete description of this second edition is published (in French and English) in "Observations et Travaux", a review edited by the Societe Astronomique de France. A detailed historical sketch of the creation and development of the catalogue -- which served as double star data base for the preparation of the HIpparcos Input Catalogue <I/196> -- has been published in issue 25, pp.29-31 (1999) of this same review. There are no fundamental differences between the two editions: format, presentation and construction are similar. The main difference lies in the important increase of the considered systems of which number expands from 34.031 to 49.325. Few additions exist in the description of the contents of the various columns, and some new codes had to be used for references to astronomical positions, especially related to the introduction of new Hipparcos systems or components to known systems (see the "refpos.dat" file). Concerning the names of the systems in columns 16 to 22, one has also to mention some additions to those given in the INDEX-WDS (C.E.Worley, 1984). They are: AOT = Oss. di Torino ACG = Astr.Cat.Greenw. BAC = P.Bacchus BEW = U.Bastian et al. CRI = F.Crifo DUF = M.Duflot DYL = J. Doyle HDS = Hipparcos JRN = A. Jorissen JKS = M.P.Jenniskens KZA = S.M.Kazeza LMP = P.Lampens LYS = L. Louys MCO = McCormick NYS = O.Nys ONL = Occult. News Letters PWS = Th.Pauwels RSU = M.Rousseau SLE = G.Soulie VHS = P.Verhas Note that: MAL = McAlister in WDS 1984 MCA = McAlister in WDS 1994 Some changes have finally been brought to the names of particular STT and STF systems (App) as shown here, to avoid some confusion that exists with the non (App) systems: --> For STF (App)I, addition of 4000, i.e. STF 4001 instead of STF 1(App)I STF 4002 instead of STF 2(App)I ............... STF 4060 instead of STF 60(App)I --> For STF (App)II, addition of 5000, i.e. STF 5003 instead of STF 3(App)II ............... STF 5012 instead of STF 12(App)II --> For STT (App)I, addition of 4000, i.e. STT 4001 instead of STT 1(App) STT 4005 instead of STT 5(App) ............... STT 4256 instead of STT 256(App)
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- ID:
- ivo://CDS.VizieR/I/211
- Title:
- CCDM (Components of Double and Multiple stars)
- Short Name:
- I/211
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The introduction to this catalogue has been the subject of a publication in the "Communications de l'Observatoire Royal de Belgique" (Serie A, number 115). Detailed are: its origins, its aims, its realization, the search of identifiers, the compilation of astrometric data and the related problems as well as the fundamental ties between the CCDM and the HIPPARCOS INPUT CATALOGUE (HIC). It also contains a complete bibliography of the referred papers. The contents of the general catalogue (63,463 systems) is also described as well as the conditions of its availability to the astronomical community and the projects underway for the next edition. For all these items, the user is invited to refer to this publication because hereafter only the format and the contents of the catalogue follow. To identify the systems and their components, we adopted the clever numbering process of the authors of the INDEX consisting in combining the right ascension and declination, respectively limited to 0.1 minute of time and to 1 minute of arc. In order to distinguish the CCDM numbers from the INDEX numbers - in addition to their different equinox: 2000 for the CCDM and 1900 for the INDEX - we adopted the signs + and - instead of the letters N and S for separating the coordinates. Consequently, in the INDEX and in the CCDM, one entry is devoted to a same system but the contrary to the INDEX, where a sub-entry is assigned to each group of two components, whatever the multiplicity of the system may be, the CCDM allows one sub-entry and thus one record per component. The present edition contains only the 34,031 systems (table below, part I) for which an accurate position has been found for at least one component. The catalogue extends thus much over the sample of the somewhat 14,000 systems finally retained for the HIPPARCOS INPUT CATALOGUE and assembled in its Annex 1.
- ID:
- ivo://CDS.VizieR/J/A+AS/111/229
- Title:
- CCD meas. of visual binaries
- Short Name:
- J/A+AS/111/229
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report CCD measurements of 33 visual double stars observed at the 1-meter coude reflector of the Observatorio de Llano del Hato located at Merida, Venezuela. We also present an algorithm to determine the stars' centroids for superimposed images as well as a brief comparison of accuracies attained by the algorithm and the program CENTER of the IRAF package.
- ID:
- ivo://CDS.VizieR/J/A+AS/123/487
- Title:
- CCD measurements of double and multiple stars
- Short Name:
- J/A+AS/123/487
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The CCD measurements for 123 double stars with ST-6 camera attached to the Zeiss 65/1055 cm Refractor of the Belgrade Observatory are communicated.
- ID:
- ivo://CDS.VizieR/J/A+A/378/954
- Title:
- CCD measurements of double stars
- Short Name:
- J/A+A/378/954
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present measurements of visual double stars made by CCD imaging from 1996 to 1999. In the article, Table 1 contains the measurements of 51 binaries with known orbit. The residuals are discussed in the text. Table 2 presents new measurements for 555 binaries. Angular separation, position angle and magnitude difference are given.
- ID:
- ivo://CDS.VizieR/J/AJ/156/134
- Title:
- CCD measurements of multiple stars at ASV & NAOR
- Short Name:
- J/AJ/156/134
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The results of classical CCD observations for 371 double or multiple stars (450 pairs) obtained at both, Serbian Astronomical Station on the mountain of Vidojevica (ASV) and Bulgarian National Astronomical Observatory at Rozhen (NAOR) are presented. At ASV the observations were performed with the 0.6 m telescope in the first half of 2016 during 11 nights, and with the newly mounted 1.4 m telescope in the second half of 2016 during 16 nights. At NAOR, the observations were performed with the 2 m telescope during four nights. In this paper, we present 477 measurements (position angle and angular separation) for these 450 pairs. Among them there are 41 pairs with published orbital or linear elements and residuals are given for them. Some pairs have measurements for several epochs. Our observed pairs have angular separations in the interval from 1.60" to 190.30", with a mean angular separation of 14.87" and a median value of 4.34". Two new pairs and linear elements for four pairs which are calculated for the first time are also presented.
- ID:
- ivo://CDS.VizieR/J/AJ/146/52
- Title:
- CCD measurements of multiple stars at NAOR and ASV
- Short Name:
- J/AJ/146/52
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using the 2m telescope of the Bulgarian National Astronomical Observatory at Rozhen, observations of 222 double or multiple stars were carried out during three nights in 2011. This is the sixth series of measurements of CCD frames of double and multiple stars obtained at Rozhen. Also in 2011, using the 0.6m telescope of the Serbian Astronomical Station on the mountain of Vidojevica, observations of 208 double or multiple stars were carried out during six nights. This is the first series of measurements of CCD frames of double and multiple stars obtained at this station. In this paper, we present the results for the position angle and angular separation for 337 pairs and residuals for 72 pairs with published orbital elements or linear solutions. These observations have angular separations in the range from 1.37'' to 172.81'', with a median angular separation of 7.66''. We also present the recalculated linear solutions for four pairs and one linear solution that has been calculated for the first time.
- ID:
- ivo://CDS.VizieR/J/other/IBVS/5493
- Title:
- 2003 CCD minima of eclipsing binaries
- Short Name:
- J/other/IBVS/549
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- - Observatory and telescope: Sylvester Robotic Observatory (SRO): 33cm f/4.5 Newtonian on Paramount GT-1100s mount - Detector: SRO: SBIG ST7e, 1.24 pixels, 15.8x10.5 FOV, cooled -10<T<-30{deg}C - Method of data reduction: Aperture photometry using MIRA, by Axiom Research - Method of minimum determination: Digital tracing paper method, bisection of chords, curve fitting, and (occasionally) Kwee and van Woerden (1956BAN....12..327K)
- ID:
- ivo://CDS.VizieR/J/A+A/400/1095
- Title:
- 1995-1999 CCD observation of Saturnian satellite
- Short Name:
- J/A+A/400/1095
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Astrometric positions of the first eight largest Saturnian satellites and the Lagrangian satellites Helene, Telesto and Calypso are presented from 493 CCD frames taken at the oppositions in 1995 through 1999. The images were obtained over 27 nights. Observed positions are compared with the calculated ones from Vienne and Duriez (1995A&A...297..588V) TASS 1.7 for the large satellites and from JPL positions for the Lagrangian satellites. The rms is about 0.12" for the former but 0.20" for Iapetus and 0.28" for Hyperion. For the Lagrangian satellites it is about 0.21" for Helene, 2.02" for Telesto and 0.60" for Calypso.
- ID:
- ivo://CDS.VizieR/J/AJ/156/199
- Title:
- CCD observations in BVRI bands for TY Pup
- Short Name:
- J/AJ/156/199
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- TY Pup is a well-known bright eclipsing binary with an orbital period of 0.8192 days. New light curves in B, V, (RI)_C_ bands were obtained with the 0.61 m reflector robotic telescope (PROMPT-8) at CTIO in Chile during 2015 and 2017. By analyzing those photometric data with the W-D method, it is found that TY Pup is a low-mass-ratio (q~0.184) and deep-contact binary with a high fill-out factor (84.3%). An investigation of all available times of minimum light including three new ones obtained with the 60 cm and the 1.0 m telescopes at Yunnan Observatories in China indicates that the period change of TY Pup is complex. An upward parabolic variation in the O-C diagram is detected to be superimposed on a cyclic oscillation. The upward parabolic change reveals a long-term continuous increase in the orbital period at a rate of dP/dt=5.57(+/-0.08)x10^-8^ days/yr. The period increase can be explained by mass transfer from the less massive component (M_2_~0.3 M_{sun}_) to the more massive one (M_1_~1.65 M_{sun}_). The binary will be merging when it meets the criterion that the orbital angular momentum is less than three times the total spin angular momentum, i.e., J_orb_<3J_rot_. This suggests that the system will finally merge into a rapid-rotating single star and may produce a luminous red nova. The cyclic oscillation in the O-C diagram can be interpreted by the light-travel time effect via the presence of a third body.
