Figure 2: The number of means per system in the WDS, from left to right the 1984.0, 1996.0, 2001.5, 2006.5 major releases of the catalog and a "current status" (2013.0). Note that while the total number of systems has increased significantly, the number of measures per system is also steadily increasing.
Figure 3: One source responsible for the increase in data is the prodigious publication of USNO speckle means. The three figures indicate all published USNO speckle data to 2013.0. At left is data obtained with the regular camera and the USNO 26", at middle is data obtained with the secondary (or backup camera) and the USNO 26" and the right is data obtained on other telescopes: the USNO Flagstaff Station 61", the McDonald 82", the Mt Wilson 100", and the two 4m telescopes of NOAO (KPNO & CTIO). Statistics are also provided. Note the variable margins in all figures for scaling.
A comparison of the contributions of the different techniques, both in their total number as well as mean and median separation are given here. Those techniques with no measures listed are unique to the Delta-m Catalog.
Primarily of historical interest, a list of the top 25 observers (based on the total number of measures and means) is presented . In this table, numbers are based on the WDS reference code. Totals are provided for the number of means (usually, as published --- a line of data in the WDS measurement database, each mean position often comes from several measures, usually increasing their accuracy).
One of the largest listings in both lists above is the effort (Wycoff et al. 2006). These double star measures were extracted from the WFC, a collection of 144 astrographic and transit circle catalogs covering a timebase of over one hundred years and most recently used in the computation of proper motions for the Tycho-2 project. While not intended as a double star reference, the utility of transit circle and photographic measures were known early in the 20th century, and many of the doubles in the were previously gleaned by Barton (1926) and others. However, there remained a plethora of double star measures in these catalogs which have now been cross-referenced with the WDS to produce these totals.
The cross-reference file has now been expanded and includes identifiers from the earlier Burnham Double Star (BDS; Burnham 1906) Catalogue, the Aitken Double Star (ADS; Aitken 1932) Catalogue, the Index Catalogue (IDS; Jeffers, van den Bos and Greeby 1963), the WDS designator and the "root" discovery designation (usually AB). BDS stars falling outside a criteria, based on magnitude and separation (and thus a likelyhood of physicality) were dropped from the ADS. Most of these stars were added back in the Index Catalogue of Visual Double Stars (IDS; Jeffers, van den Bos and Greeby 1963). Some of these stars were true binaries, and should be added back, others were added due to concerns due to common proper motion determinations or proximity. As mentioned above, duplicate and bogus systems included in the BDS or ADS have been excised for one of the following reasons:
Some detections are not included in the WDS. These include measures by long baseline interferometry where only visibilities and baselines are published (as opposed to a true separation and position angle) are not included. Also, various 1-d detection data (e.g., lunar occultation and some infrared speckle interferometry) are not included, as the measured separation is only a projection of the true separation. These data are available in the 4th Catalog of Interferometric Measurements of Binary Stars (Hartkopf, Mason, Wycoff, & McAlister 2001; hereafter Speckle Catalog). The absence of separation and position angle information for the long-baseline interferometry data is perhaps most tragic as these data cannot be readily combined with other ``classical'' double star data for a true combined solution. While older data is almost certainly of lower astrometric accuracy, the contribution that can be made defining the period over a much longer timebase is significant.
Other cross references include cross-references to the Struve lists (Wilhelm and Otto) & their appendices and the William Herschel doubles. The complete main lists followed by their appendices cross-referenced to their WDS number is provided in the file. The cross reference of William Herschel's doubles was generated from a file maintained by Bruce MacEvoy (see http://www.handprint.com/ASTRO/herschel.html), and his used by his kind permission.
Finally, a constellation designation is provided. This gives the constellation within which all pairs fall. This is based on the ten digit WDS designation and not the precise position. This identification is based on a program written by intern Korie Miles, utilizing FORTRAN code written by Francois Ochsenbein (CDS).
We have a more complete list of alternate constellation designations in our Bayer/Flamsteed listing below for selected pairs. This is cross-referenced to the current WDS and discovery designation and includes Bayer, Flamsteed, and variable star designations as well as some proper names. A few designations (flagged with ) were found in early 19th century papers by Madler and Smyth and are not in common use today. A few designations for constellations no longer extant are also included, as are some common names (e.g., Sirius or Capella). Specific components of wider pairs have been noted in some cases, but much of this work remains to be done.
For a variety of reasons, there exist a large subset of measures contained in the WDS database which have not been published. To make these data available to the astronomical community they are listed below. It is anticipated that this section will expand substantially as the data contained in the WDS are collated.
In the last 40 years, a limited group of Spanish amateurs has been systematically measuring visual double stars. Actually, they are preparing to publish all the measurements made between 1970 and 2001 --- over 10,000. This massive work has been presented at October, 2000, in the annual meeting of the Astronomic Society of France's Double Stars Commission, celebrated in Castelldefels, near Barcelona, Spain. (Josefina Ling, Circular UAI Commission-26 was in the meeting).
The first measurement catalogue entirely produced in Spain by an amateur was the Jose Luis Comellas (Doctor of Contemporaneous History, Sevilla University) one, published in 1973 (Catalogo de Estrellas Dobles Visuales 1973.0). It contained measurements from 1,200 double stars, using a simple micrometer and a 75mm aperture Polarex-Unitron refractor. Twelve years after, the same author published a second catalogue (Catalogo de Estrellas Dobles Visuales 1980.0) that included 5,104 doubles within reach of his new 102mm aperture Polarex-Unitron refractor, with a Ron Darbinian Filar Micrometer, of which he had personally measured over 3,500. For the quality and quantity of his publications, that included his exceptional Guia del Firmamento (1982) where he gathers together all his experience of more than thirty years of visual observation, as well for his extraordinary human condition, he is one of the most loved and admired authors in Spain and South America.
Since 1985 new observers have assured the continuity of J.L. Comellas work. Since 1976, I regularly collaborated with him, and in the mid 80s I had a little observatory supplied with a 102mm Polarex Unitron refractor and a filar micrometre, that enabled me to start systematic revision and update programs of the 1980.0 catalogue. In 1991, in conjunction with other colleagues, we coordinated the measurements sent to us by isolated observers, and started to publish a circular (RHO: Circular de Estrellas Dobles Visuales) for internal use, in order to coordinate our work and to make known our results.
Our equipment enhanced its measurement power with the purchase of new precision micrometers, Double Image Lyot-Chamichel-like, and CCD devices. Between 1992 and 2003 more than 5,000 new observations and measurements has been collected, provided by Spain-wide amateurs, and this has allowed to arrange a new catalogue suited to the 21st Century observers needs.
Given the huge bulk of filed data, it was necessary to develop our own database managing, analysis and ephemeris calculation software (MAIA). This job has been carried on by my colleague Jaume Planas, in collaboration with Jordi Cairol and Albert Sanchez, both members of OAG.
The evolution and development of this process has been made known in the meetings of the Astronomic Society of France's Double Stars Commission in Lyon (1995), Nice (1996), Bordeaux (1997), Tolouse (1999). This has enabled the Spanish visual double stars observers to break a certain isolation they were suffering since some decades ago.
Actually, the database and the different aplications it contains are for internal use only, but we are preparing an interactive version for Internet. In this way, our "OAG General Catalogue of 10,000 visual double stars measurements 1970-2000 (J2000.0)" wll be easily available to any worldwide observer.
Note about Garraf Astronomical Observatory
Garraf Astronomical Observatory (OAG), founded in 1991 from private and public investments, develops didactic and research programs. Our observatory (1992-1998) have a 3.5m diameter dome with a 300mm aperture Newton-Cassegrain (F/3,5 and F/13,5) reflector, and 150mm F/8 refractor. Is located 30km to the south of Barcelona, inside the Garraf Natural Park, 300m over the sea. Our observatory is fully equipped for a double stars programs, with CCD, Professional Double Image Lyot-Camichel Micrometer (made by MECAPRECIS-France) and various Micrometer Reticle Eyepiece (MEADE).
OAG wishes to contact and to establish research programs specialized in visual double stars with others observers and observation teams. It has accommodation facilities for up to 55 people.
(text by : Garraf Astronomical Observatory, e-mail: , http:// www.oagarraf.net)
While not unpublished, the work of the Webb Society Double Star Section has only a limited circulation and deserves special mention here. As these are sent to the WDS in electronic pre-formatted files, these are among the fastest additions to the WDS and the work of the society, confirming and measuring neglected pairs, determining precise positions of lost pairs and other tasks have made substantial improvements to the WDS.
A large number of systems in the WDS may be characterized as ``neglected.'' These include unconfirmed binaries as well as systems which have not been resolved for many years. The reasons for this neglect are varied: poor coordinates or large proper motion (so the systems are ``lost''), erroneous magnitude or delta-m estimates (so the systems are skipped over or misidentified), or true neglect (too many binaries and too few observers). While the veracity of some of these systems is certainly suspect, many (if not most) of these are bona fide double stars. Three sets of lists are provided in WDS format. The first set was compiled using the following selection parameters:
A total of 946 objects meet these criteria.
The second set of lists were compiled under the same criteria as above, but for separations under 3 arcseconds. A total of of 4376 systems fit these criteria.
The third and final set of lists includes all those neglected systems listed above, as well as those not covered by the previous lists. These then make a master "neglected list" that the user may sort based on their own parameter sets and capabilities. A total of 39,585 systems fit these criteria.
The complete list of observations of neglected pair by a specified reference code is given .
We can tailor observing lists to your specific needs. To have a custom-made observing list prepared with parameters different than those above, please fill out an observing list request form:
In 2001 an effort led by Claus Fabricius was begun to extract from the Tycho pixel data as many double stars, both new and known, as possible. This effort has resulted in the . A total of 25,232 additional double star measures (in addition to those included in the last major release of the WDS) were found. The numbering of new Tycho doubles (the TDS stars) includes the original set of 1,234 (subsequently reduced to 1,220) described above plus additional systems found in the Tycho Double Star Catalogue reduction. This second set of new doubles begins with TDS1235 (the retracted TDS numbers are not reused). A complication arose as a result of the magnitude of this work --- what to do when the number is 10,000 or more (i.e., after TDS9999, what next?). A makeshift strategy was employed by taking the next available designation, TDT (Tycho Doubles, too?), thus the next system after TDS9999 is TDT 1. The known and new doubles listings includes both analyses of the Tycho data. In addition, precise coordinates (better than arcsecond) are available for another subset of double stars seen as single by Tycho (due to the magnitude of the secondary and/or separation of the system). The improvements in the precision of the WDS is discussed below.
Examples of the first are the binaries first resolved by W. Herschel and both F.G.W. Struve and O. Struve. William Herschel published seven lists (I - VI, plus ``new'', or N), with stars of each list starting at number 1. In addition to their original discovery lists, each of the Struve's published an appendix, as well as a list of ``rejected'' doubles. These multiple lists were completely spelled out in the Aitken Double Star Catalogue (e.g., H IV 48), but when the Index (IDS) Catalogue was compiled at Lick all of these other designators were dropped for lack of space. As a result there are, for example, five components with the designation H 48! The source Herschel list was given in the notes file to the IDS. Appended and rejected stars from the lists of the Struve's were handled with an ``a'' or ``r'' towards the end of the WDS data line in most cases.
In the second (and fortunately rare) case, systems found quite near to known ones were given the same designation plus trailing character(s) (e.g., ES 1293a or BU 885 1/2). Sometimes both components were assigned these additional characters, sometimes only one; occasionally two pairs in an entirely different section of the sky were given the same designation by the author (probably by mistake).
Each of these cases is being handled in a different manner. For the William Herschel discoveries, a list identifier is added to column three of each designation. For example:H 19 (at 16 hours) was originally H II 19 and is now known as H 2 19, H 7 (at 18 hours) was originally H V 7 and is now known as H 5 7, and H 111 (at 06 hours) was originally H N 111 and is now known as H N 111.
In the case of the O. Struve appendix an A is added following STT in the name. For F. Struve, he provided two appendices. Those from the shorter list (Appendix II) are designated STFB. For example:STF 11 (appendix I) is now STFA 11. STF 11 (appendix II) is now STFB 11. STT 252 (appendix) is now STTA252.
Stars of the second type are given the same 3-letter discovery designation but a new number, starting with 9001, to indicate that they originally had a different designation. For example:BAL2356b is now BAL9001. BU 885 1/2 is now BU 9001. A complete list of stars of the second type is provided in the file. All changes in designation are described in the file. In addition to these, designations for 271 W. Herschel (H ), 110 F. Struve (STF) and 227 O. Struve (STT) systems have been changed. Note that for some of these systems, the former three character, four digit reference (a3i4) has been replaced by a four character, three digit reference (a4i3). Although, for all USNO applications (e.g., data or observing list request) an a7 read will see no difference.
For observations of double stars it is often necessary and beneficial to observe single stars. These can serve as an idealized point-source-function (psf) to determine the behavior of various elements in the optical chain, characterize various reduction algorithms, or be used to generate artificial double stars or other more complicated morphologies by use of calcite crystals, slit masks, aperture masks, etc.
Unfortunately, finding a good list of these calibrator sources is more difficult than it sounds. Generally speaking, the more that stars are studied the higher their multiplicity fraction. Erroneously labeled ``single stars'' can render vital calibration data useless through the discovery of a previously unknown companion or the slight modification of the psf by an unresolved component.
The basic data for this list come from the , which tabulates null detections from various duplicity surveys in addition to double star measures obtained by speckle interferometry and other high-resolution techniques. Stars from the (Hoffleit & Warren 1991) are checked against the WDS, the Speckle Catalog, and the Hipparcos Catalog (ESA 1997) and only considered to be ``single'' stars if all the following criteria are met:
The (non-frame version ) contains 1,170 systems fulfilling these criteria. In the future, it is planned to update this list to include systems which would be unresolved by optical interferometry.
Measures in the Washington Double Star Catalog have been collected, collated, and maintained since the early 1960's when the original IDS (Jeffers & van den Bos, 1963) was transferred from Lick Observatory to the U.S. Naval Observatory. Presented in order are the WDS J2000 coordinates, the discovery and component designation, the first and last measured epoch, the number of means, the first and last measured position angle (theta) in degrees, the first and last measured separation (rho) in arcseconds, the magnitudes of the primary and secondary, the spectral type of one or both components (if known), proper motion in RA and Dec (primary and secondary in milliarcseconds/yr), the Durchmusterung (DM) number (The DM of the object in the system used by the Henry Draper Catalogue: Bonn from +89 to -22 inclusive, Cordoba from -23 to -51 inclusive, Cape Photographic from -52 to -89 inclusive), and a notes column. It should be noted that the WDS is not a photometric or spectral type catalog, and while the catalogers strive to provide the most correct values for these parameters, they should not be considered definitive. Some characters in the notes column indicate specific entries in another file (i.e., an N indicates an entry in the notes file), catalog (an O in the Orbit Catalog, and a D in the Delta-m Catalog), or are referenced in the format file. The full Catalog is available below as are format, note, reference and other ancillary files. Now available via the links below are the WDS in an sql database form and with only the last relative position, but at a higher precision which is useful when planning observing on instruments with high angular resolution capabilities. The first version of the SQL code was written by Intern Danley Hsu (2014) and later improved by Damien Mattei (2018).
Addition of the delta-m information as well as other more significant changes to the WDS database are currently under consideration. The input from regular users of the database and other interested parties is greatly appreciated in our efforts to make the WDS as helpful and user-friendly as possible. Please provide comments on the format of the WDS, missed references, or any other items of interest to you on our .
Information is being added to the database on a continuing basis, and this edition of the WDS will also be updated regularly.
You may a reasonable amount of information from the double star catalog, a , a , or make a by e-mail.
We are in debt to for his work on the WDS database and his leadership in the speckle program at the USNO. The Washington Double Star Catalogs and USNO speckle program were conceived and nurtured by Charles Worley. Providing data in WDS format (or at least electronic format) has allowed the WDS to grow significantly. We would here like to acknowledge the contributions of Bob Argyle, Niall Deacon, Wulff Heintz, Elliott Horch, Josefina Ling, Wayne Orsborn, Francisco Manuel Rica Romero, Walt Sanders and Andrei Tokovinin.
The WDS has been significantly improved by many people who have taken heed to the "neglected doubles" listed above, significant among them are a cadre of enthusiastic amateurs (though, I think I prefer the term "financially uncompensated double star astronomers"), namely contributors to the publications the Double Star Observer, the Webb Society Circulars, members of the Yahoo groups, "binary-stars-uncensored" and "double stars," and others. While the list of contributors is too great to enumerate everyone by name, I want to mention a few who do not appear in the reference list for these contributions improving the basic information found in the database: Francisco Manuel Rica Romero and the LIADA Double Star Section for work on proper motions of secondaries, Richard Jaworski for precise positions of "lost" doubles, many hard to locate pairs of William Luyten, Brian Skiff for corrections and discovery of uncataloged pairs, Bruce MacEvoy, Gianluca Sordiglioni, Ross Gould, Wilfried Knapp and Chris Thueman for corrections as well as Friedrich Damm for many, many corrections, discovery of lost pairs, cross reference determinations and other corrections and enhancements too numerous to mention.
Summer Interns have over the past several decades made many contributions to the WDS. We acknowlege their work here.
``This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory.''
A notification of references to relevant papers is appreciated.