Browse this table... |
## MORBBINCAT - Dynamical Masses of Selected Orbital Binary Systems |
HEASARC Archive |

To compile the orbit list, the authors combined data from both OARMAC and ORB6. At this stage, they maintained systems without parallaxes, but removed systems without a period or semi-major axis. The resulting list contained 3139 orbits for 2278 pairs: 1588 pairs have a single orbit, 548 pairs have two orbits, 120 pairs have three orbits, 19 pairs have four orbits, one pair has five orbits, and two pairs have seven orbits.

Table 1 in the reference paper (not part of this HEASARC table) contains a compiled set of 3139 orbit solutions for visual binary stars. Separate entries are provided for different pairs in multiple systems. Several solutions per pair are possible. Each entry includes main orbital elements (Semi-major axis, period, eccentricity with corresponding uncertainties), indication of multiplicity and number of solutions, as well as visual magnitudes, spectral classes of the components, parallax and interstellar extinction estimate.

Table 2 in the reference paper (on which this HEASARC table is based) contains a refined set of 652 solely binary systems with reliable orbits and determined parallaxes. One entry in this table corresponds to one system. Three mass estimates are provided: (1) The dynamical mass with its uncertainty derived from Kepler's third law and its trigonometric parallax, (2) a photometric mass estimated from the visual magnitudes, parallax and mass-luminosity relation, and (3) a spectroscopic mass based on the mass-spectrum relation introduced by Straizys and Kuriliene (1981, Ap&SS, 80, 353). Also provided for each system are the main orbital elements, the parallax, and the component magnitudes and spectral types.

Dynamical masses of a selected sample of orbital binaries. Malkov O.Yu., Tamazian V.S., Docobo J.A., Chulkov D.A. <Astron. Astrophys. 546, A69 (2012)> =2012A&A...546A..69M

**Name**

The WDS binary system designation using the format recommended by the
Dictionary of Nomenclature of Celestial Objects, except that the final
suffixes identifying the specific components which are generally used to
identify binary systems in the WDS are not included herein. Thus the names
are of the form 'WDS JHHMMm+DDSS'.

**RA**

The approximate Right Ascension of the binary system in the selected
equinox. This was constructed by the HEASARC based on the J2000.0 position
string in the name of the system. Since the latter is given to only the
nearest 0.1 minutes of time in RA and 1 arcminute in Dec, these positions
are only illustrative and are NOT of astrometric quality.

**Dec**

The approximate Declination of the binary system in the selected
equinox. This was constructed by the HEASARC based on the J2000.0 position
string in the name of the system. Since the latter is given to only the
nearest 0.1 minutes of time in RA and 1 arcminute in Dec, these positions
are only illustrative and are NOT of astrometric quality.

**LII**

The approximate Galactic Longitude of the binary system.

**BII**

The approximate Galactic Latitude of the binary system.

**Comp1_Mag**

The visual magnitude of the primary component of the binary
system, taken from the WDS, or if absent from WDS, from Simbad.

**Comp2_Mag**

The visual magnitude of the secondary component of the binary
system, taken from the WDS, or if absent from WDS, from Simbad.

**Comp1_Spect_Type**

The spectral type of the primary component,
taken from the WDS, or if absent from WDS, from Simbad.

**Comp2_Spect_Type**

The spectral type of the secondary component,
taken from the WDS, or if absent from WDS, from Simbad.

**Parallax**

The trigonometric parallax (pi) of the binary system, in
milliarcseconds (mas), taken for van Leeuwen (2007, A&A, 474, 653).

**Parallax_Error**

The uncertainty in the trigonometric parallax of the binary
system, in milliarcseconds (mas), taken for van Leeuwen (2007, A&A, 474, 653).

**Vmag_Extinction**

The interstellar extinction towards the binary system in the
V band, A_V, in magnitudes. This was estimated using the well-known Parenago
(1940, AZh, 17, 3) formula, based on the distance (r) and galactic latitude
(b) of the system: A_{V} = [(a_{0} * beta) * (1 - e^{-C})] / |sin b|,
where C = r * |sin b| / beta, beta is the scale height and a_{0} is the
extinction to an object located in the galactic plane behind the absorbing
layer. The values of 1.6 mag/kpc and 114 pc were accepted for a_{0} and beta,
respectively.

**Orbital_Period**

The orbital period (P) of the binary system, in years.

**Orbital_Period_Error**

The uncertainty in the orbital period of the binary
system, in years.

**Semi_Major_Axis**

The semi-major axis (a") of the orbit of the binary
system, in arcseconds.

**Semi_Major_Axis_Error**

The uncertainty in the semi-major axis of the orbit
of the binary system, in arcseconds.

**Eccentricity**

The eccentricity (e) of the orbit of the binary system.

**Eccentricity_Error**

The uncertainty in the eccentricity of the orbit of
the binary system.

**Dynamical_Mass**

The dynamical total mass (M_{d}) of the binary system, in
solar masses, obtained using Kepler's Law, M_{d} = M_{1} + M_{2} = (a")^{3} /
[pi^{3} * P^{2}], where P is the orbital period (in years), M_{1,2} are the
masses (in solar mass), a" and pi are the semi-major axis and the parallax
(both in arcseconds), respectively.

**Dynamical_Mass_Error**

The uncertainty in the dynamical total mass of the
binary system, in solar masses. See Section 3 of the reference paper for
more details on how this was estimated.

**Photometric_Mass**

The photometric mass of the binary system, in solar masses. The photometric
masses of the components for each system were estimated from the observed
photometry, the trigonometric parallax, and a mass-luminosity relation. See
Section 3 of the reference paper for more details on how this was estimated.

**Spectroscopic_Mass**

The spectroscopic mass of the binary system, in solar masses. The
spectroscopic masses of the components for each system were estimated from
their spectral types using Table VI of Straizys and Kuriliene (1981, ApSS,
80, 363). See Section 3 of the reference paper for more details on how this
was estimated.

**Class**

The HEASARC Browse object classification, based on the spectral
type of the primary component (comp1_spect_type).