VizieR Online Data Catalog: Double-lined spectroscopic binaries catalog (Piccotti+, 2020)
Abstract
To compile the orbit list, we combined data from both ORB6 and SB9. Table 1 lists the orbital elements common to the two catalogs: hereafter, for each star, the first two upper rows represent ORB6 catalog orbital elements and the two lower lines represent SB9 catalog orbital elements. Column 1 specifies the catalog: ORB6 or SB9. The second column gives the Washington Double Stars (WDS) code (coord. 2000) of the binary and below, its HD (Henry Draper) catalog number, if any. The system identifier adopted in the WDS ("discoverer designation" as a visual binary) is given in the third column. Columns 4, 5, 6 and 7 contain, for each catalog, the orbital elements in the first line and their formal uncertainties in the following one: the orbital period, P, in days, the epoch of periastron passage, T, in Modified Julian Date (MJD, JD-2400000.5 days), the eccentricity, e, and the argument of periastron, omega, in degrees. The orbit grades are given in the ORB6 system, where 1 and 2 grades mean definitive and good orbits, respectively. The SB9 catalogue contains 2694 orbits of 2386 systems (SB1 and SB2) and 55 spectroscopic triple systems (http://sb9.astro.ulb.ac.be/). It provides easy access in order to search for the object using catalogues identifiers (HD, HIP, BD), coordinates, publication's bibcode, etc. It lists the parameters of components, magnitudes, the spectral type, the orbital elements with their standard uncertainties, the orbit grades and radial velocity curve. Grades of old orbits are taken from The Eighth catalog of the orbital elements of spectroscopic binary stars (SB8) (Batten, Fletcher & MacCarthy, 1989PDAO...17....1B) (5-best, 1-worst), for new orbits they are not entered, pending a development of new automatic grading system. Column 13 contains the original references of the orbits.
The semi-major axes, expressed in au, are listed in Table 2, where we have combined the visual and spectroscopic orbits, as we explained before using the equations 1, 2 and 3. In Columns 2, 3, and 4, list the values of asini and their uncertainties, with Column 4 indicating the power of 10 that affects the values of both columns 2 and 3, the values of asinine, in au, and a, in au, appear with their uncertainties in columns 5 to 8. In Table 3 we compared the parallaxes: both the orbital and the dynamical one, calculated by us, with those provided by Hipparcos space mission and/or Gaia when available. We have for 16 systems the orbital parallax that falls within 3σ of the dynamic parallax, for 35 that falls within 3σ of the parallax of Hipparcos and for 23 that falls within 3σ of the parallax of Gaia. But, on the other hand, we have 45 systems whose orbital parallax falls within 3σ of at least one of the three parallax values (dynamical, Hipparcos and Gaia). This discrepancy is probably due to the oldness of several spectroscopic orbits because the common orbital elements do not coincide perfectly with those of the visual orbit (see table 1), and it is therefore desirable to recalculate a number of spectroscopic orbits. The orbital, the dynamical, Hipparcos and Gaia parallaxes are given in columns 2, 3, 4, and 5, respectively, with their corresponding uncertainties. In Table 3 we represent in bold the stars whose orbital parallax differs from the Gaia parallax by 3 sigma, while in italics the stars whose orbital parallax differs from the Hipparcos parallax by 3 sigma, when the Gaia parallax is not published. In Table 5 we compared the individual masses of the two components of each system using the four parallaxes when available. The masses of the primary, using the orbital, the dynamical, Hipparcos, and Gaia parallaxes, are presented in columns 2, 3, 4, and 5, respectively, with their uncertainties; the masses of the secondary, using the orbital, the dynamical, Hipparcos, and Gaia parallaxes, are found in columns 6, 7, 8, and 9, respectively, with their uncertainties. Table 6 collects the magnitudes in the visual band (V), calculated as described in the equations 8, 9 and 10. The description by columns is: (1) Henry Draper (HD) catalog number; (2) Composite apparent magnitude in the visual band (V), taken from the SIMBAD database; (3) Apparent magnitude of the primary in the visual band; (4) Apparent magnitude of the secondary in the visual band; (5) Magnitude difference between the two components. This value was obtained averaging the corresponding data from speckle measurements collected in INT4 catalog and discarding the extreme values; (6) Composite absolute magnitude in the visual band without interstellar extinction; (7) Absolute magnitude of the primary in the visual band without interstellar extinction; (8) Absolute magnitude of the secondary in the visual band without interstellar extinction; (9) Galactic latitude, in degrees; (10) Interstellar extinction, in magnitudes; (11) Composite absolute magnitude in the visual band with interstellar extinction; (12) primary absolute magnitude in the visual band with interstellar extinction; (13) secondary absolute magnitude in the visual band with interstellar extinction. In Table 7 we collected the spectral types, temperatures, colour in- dices, and bolometric corrections (Gray, 2005). The description by columns is: (1) Henry Draper (HD) catalog number; (2) Spectral Type of the primary; (3) Class of the Luminosity of the primary; (4) Spectral Type of the secondary; (5) Class of the Luminosity of the secondary; (6) Effective Temperature of the primary; (7) Effective Temperature of the secondary; (8) colour index (B-V) of the primary; (9) colour index (B-V) of the secondary; (10) colour index (V-R) of the primary; (11) colour index (V-R) of the secondary; (12) Bolometric Correction of the primary; (13) Bolometric Correction of the secondary. Once the evolutionary track is chosen to be representative of a given primary (or secondary) star from the CMD, it is straightforward to obtain the estimation of the age, the luminosity, and the effective temperature from the same theoretical model. The results for the primaries are represented in Table 11, and Table 12 provides the results for the secondary. The format of both Tables is the same. Column 2 lists the mass in solar masses; in Column 3, the logarithm of luminosity in solar luminosity is shown; in Column 4, the logarithm of effective temperature appears, and finally, in Column 5, the logarithm of age is given. (9 data files).- Publication:
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VizieR Online Data Catalog
- Pub Date:
- November 2019
- Bibcode:
- 2019yCat..74922709P
- Keywords:
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- Stars: double and multiple;
- Binaries: spectroscopic