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Mining in the Hipparcos Raw Data? ASTRONOMY & ASTROPHYSICS MARCH I 1999, PAGE 231 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 135, 231–241 (1999) Mining in the Hipparcos raw data? J.L. Falin and F. Mignard Observatoire de la Cˆote d’Azur, CERGA, UMR CNRS 6527, Av. N. Copernic, F-06130 Grasse, France Received September 1; accepted October 21, 1998 Abstract. The Hipparcos solutions flagged as unreliable Hipparcos solutions are given below in Sect. 3, but by it- after the completion of the standard data processing have self this flagging was not a sufficient condition to start a been systematically revisited in the light of additional in- new processing. formation, primarily related to their multiplicity. In many First, new information not used in the mass process- cases improved solutions have been obtained, yielding at ing had to be available, otherwise there were no chances to the same time an Hipparcos based separation and position get something really different. Secondly, as a result of the angle and a better astrometric solution for the system. organisation of the file storage in the FAST consortium, The principles applied in this reprocessing are explained there were only about 20 000 stars detected as non-single and more than a hundred new solutions with absolute and for which a new double star treatment was feasible. Thus relative astrometry are presented and discussed. all the stars re-examined for duplicity problems were in this set. The vast majority of the improved solutions be- Key words: stars: fundamental parameters — binaries: long to this category. general — astrometry — stars: distances Unlike the results available in the Hipparcos Catalogue, the solutions presented in this paper do not follow from a cross-check between the two consortia and are entirely based on the software developed by teams 1. Introduction of the FAST consortium and published under the sole scientific responsability of the authors. The processing of the Hipparcos observations culminated in June 1997 with the official publication of the astro- metric solutions of nearly 118 000 stars included in the 2. The Hipparcos processing Hipparcos Catalogue (ESA 1997). The average astromet- ric precision for the bulk of the Catalogue is about 1 mas in Before proceeding with the new solutions it is worth each of the five astrometric parameters: position, parallax recalling the various categories of astrometric solutions and the two components of the proper motion. However, published in the Hipparcos Catalogue. The Hipparcos due to time constraints, it was known at the time of pub- Catalogue is the primary result of the observations and lication that the solutions for about one thousand stars reductions of the satellite data acquired over 37 months were not fully satisfactory and for 263 entries no solutions between November 1989 and March 1993. The Catalogue at all were found acceptable from the data. comprises 118 218 entries with median astrometric posi- The raw data have been archived by each of the two tions of the order of 1 milliarcsec and specific results (sep- consortia and intermediate data have been published with aration, magnitude difference) for double and multiple the other Hipparcos products. Relieved from the pressure systems. For single stars the standard astrometric model of the publication schedule we have revisited the solutions yields the five astrometric parameters (position, parallax not considered as final in the Hipparcos Catalogue, taking and the two components of the proper motion) together advantage of updated information regarding their multi- with their full covariance matrix. plicity status. The criteria used to identify the doubtful Many catalogue entries were known to be, or found to Send offprint requests to: F. Mignard, [email protected] be, components of a double or multiple system. The final ? Tables 1 to 7 are also available in electronic form at the astrometric solution for these complex entries, given either CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) for the photocenter of the system or for the brighter com- or via http://cdsweb.u-strasbg.fr/Abstract.html ponent, is fully independent of the relative position of the 232 J.L. Falin and F. Mignard: New Hipparcos solutions two components. In cases of detected duplicity the obser- errors in the Input Catalogue positions, while 253 so- vation model had to be extended to account for resolved lutions were finally rejected as inadequate. systems or for systems exhibiting a significant motion on 2. The solutions with a time dependent proper motion the sky over the mission. One major difficulty in the dou- (solutions flagged G in the Catalogue) refer probably ble star processing was the consequence of the large va- to astrometric binaries with periods above about 10 riety of categories of systems and the difficulty to solve years. There are 2622 such solutions. simultaneously for the relative and absolute astrometry. 3. The stochastic solutions (flagged X in the Catalogue) It was clear when the time came to publish the results that is to say published solutions for which it was that several hundred problem stars were left and their so- not possible to find an acceptable single or multiple lution could not be given with the same level of reliability star solution in reasonable agreement with the ran- as for the bulk of the Catalogue. The main problems were dom error of the abscissas. While a significant fraction primarily linked to the double and multiple star solutions might be short period astrometric binaries, many oth- and much more time would have been required to clear ers could be true double stars with inadequate relative the remaining difficulties for a subset no larger than a astrometry. thousand stars. The main sources of problems were: In addition to these broad categories, there are two other – Due to the presence of a periodic modulation grid, the indications that can be used to pinpoint questionable so- relative position between the two components of a dou- lutions: ble system may be wrong by an integral number of 1. Under field H29 one finds the percentage of data that grid periods, of about 1.2 arcsec. Should this happen, has been rejected in order to converge to an acceptable for particular elementary observations and provided it fit. In general this number is below 10% and a larger remained undetected, no reliable astrometric solution value is an indication that the solution should be taken can be obtained in the subsequent processing. with care as a significant number of outliers has been – The double star processing may provide numerous spu- discarded. rious solutions and in some instances the final choice 2. The field H30 attempts to quantify the quality of the was based on the fact that a solution was found in close final fit, when the outliers have been removed. Values agreement with the ground based configuration. If the larger than 3 or 4 indicate a bad fit to the data. latter was not correct, because of a misidentification or because of the relative motion since the measure- ment epoch, the error was propagated in the Hipparcos 4. Sources of new data solution. – Finally the data processing by FAST and NDAC may Most of the new solutions given in the following sections have led to different solutions for the parameters of were made possible because of the availability of several a binary and a choice was made at the end. Either pieces of information that were not used during the data one solution was retained or the entry was classified as processing for lack of time, or simply because the in- suspect binary and processed as single. In such a case formation did not exist at that time or was overlooked. the final fit was usually of poor quality and published Essentially, the new data consists of updated values for the with a warning or with large standard errors. relative astrometry and/or photometry of double stars. As mentioned above the grid step error could be 3. The doubtful solutions avoided if a good a priori separation and position angle could be secured to select the most likely solutions among The observations reinvestigated during this work are lim- the two or three possible. It is worth emphasising that ited to the Hipparcos entries for which a problem has been for the vast majority of the double stars solved from the detected in the routine processing. This does not mean Hipparcos data, the processing was self-sufficient and did that all such solutions are spurious, in fact most of them not need to rely on a good starting point. Only when the are correct, but the proportion of unreliable solutions is double star signal was too weak or the observation equa- larger in this group than in the rest of the Catalogue. tions poorly conditioned was the starting value more cru- The final statistics published in the Catalogue docu- cial. This concerned only a small fraction of the Hipparcos mentation (ESA 1997, Vol. 1) give an order of magnitude double stars, but a large fraction of the subset reinvesti- of the number of entries to be reinvestigated on a case by gated in this paper. case basis. In addition the different categories help under- Several sources were used to reprocess the Hipparcos stand what kind of problem may be expected in the re- observations of the selected doubtful solutions: processing and provide hints to orient the search for new – The Tycho Catalogue includes components of wide bi- information. naries (ρ ≥ 3 arcsec) observed as two independent 1. There were 263 entries with no astrometric solution entries provides they are brighter than V =10.5. published. Only 10 were not observed because of large From the individual astrometric solutions it was easy J.L.
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