- ID:
- ivo://CDS.VizieR/J/AJ/161/295
- Title:
- Obs. with Differential Speckle Survey Instrument. X.
- Short Name:
- J/AJ/161/295
- Date:
- 09 Mar 2022 22:00:00
- Publisher:
- CDS
- Description:
- This paper details speckle observations of binary stars taken at the Lowell Discovery Telescope, the WIYN telescope, and the Gemini telescopes between 2016 January and 2019 September. The observations taken at Gemini and Lowell were done with the Differential Speckle Survey Instrument (DSSI), and those done at WIYN were taken with the successor instrument to DSSI at that site, the NN-EXPLORE Exoplanet Star and Speckle Imager (NESSI). In total, we present 378 observations of 178 systems, and we show that the uncertainty in the measurement precision for the combined data set is ~2mas in separation, ~1{deg}-2{deg} in position angle depending on the separation, and ~0.1mag in magnitude difference. Together with data already in the literature, these new results permit 25 visual orbits and one spectroscopic- visual orbit to be calculated for the first time. In the case of the spectroscopic-visual analysis, which is done on the ternary star HD173093, we calculate masses with a precision of better than 1% for all three stars in that system. Twenty-one of the visual orbits calculated have a K-dwarf as the primary star; we add these to the known orbits of K-dwarf primary stars and discuss the basic orbital properties of these stars at this stage. Although incomplete, the data that exist so far indicate that binaries with K-dwarf primaries tend not to have low-eccentricity orbits at separations of one to a few tens of astronomical units, that is, on solar system scales.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/PASP/107/299
- Title:
- Occultation Binaries Catalog
- Short Name:
- J/PASP/107/299
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The observation of lunar occultation phenomena allows for the determination of binary star data which can not always be obtained using classical techniques. No complete catalog has been compiled since that of Evans (1981a) in spite of a 99% increase in the available data. This catalog presents a catalog of photoelectric and occultation measures of binary and multiple systems complete through 1994.
- ID:
- ivo://CDS.VizieR/I/110
- Title:
- Occultation Double-Star Observations
- Short Name:
- I/110
- Date:
- 28 Jan 2022 08:30:21
- Publisher:
- CDS
- Description:
- (no description available)
- ID:
- ivo://CDS.VizieR/J/AJ/161/46
- Title:
- (O-C) curve of the binary system KIC 06852488
- Short Name:
- J/AJ/161/46
- Date:
- 10 Dec 2021
- Publisher:
- CDS
- Description:
- The continuous and unbroken time-series photometry data of Kepler and the Transiting Exoplanet Survey Satellite (TESS) provide a good opportunity to study the continuous variations in the light curve of binary stars. This paper reports the discoveries of the correlation between the two maxima on the light curve of KIC06852488 and the correlation between the O'Connell effect and the O-C curve. The Max I and Max II vary with a same cycle length of ~2000days and a 180{deg} phase difference, and the variation of the Max II coincides with the O-C curve of the primary light minima. After analyzing the Kepler and TESS light curves, it is detected that this binary is a semi-detached system with a mass ratio of 0.4622({+/-}0.0036). The secondary component is filling its critical Roche lobe, while the primary component is only filling 12.25({+/-}0.10)% of the lobe volume that contributes more than 85% luminosity of the total system. The variation of the O'Connell effect could be explained by an evolving hot spot on the primary component and an evolving cool spot on the secondary component. It is found that their positions are symmetrical with the inner Lagrange L1 point. After subtracting the binary brightness changes, six optical flares are detected that come from the cool secondary. We calculated the energy of flares and found that all of the flares are superflares. Both the flares and an evolving dark spot on the lobe-filling secondary component make the system a very interesting source to investigate the effects of binary interaction on the magnetic activities.
- ID:
- ivo://CDS.VizieR/J/MNRAS/457/1320
- Title:
- OGLE-III planet detection efficiency
- Short Name:
- J/MNRAS/457/1320
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We use six years (2003-2008) of Optical Gravitational Lensing Experiment-III microlensing observations to derive the survey detection efficiency for a range of planetary masses and projected distances from the host star. We perform an independent analysis of the microlensing light curves to extract the event parameters and compute the planet detection probability given the data. 2433 light curves satisfy our quality selection criteria and are retained for further processing. The aggregate of the detection probabilities over the range explored yields the expected number of microlensing planet detections. We employ a Galactic model to convert this distribution from dimensionless to physical units, {alpha}/au and M_{earth}_ The survey sensitivity to small planets is highest in the range 1-4au, shifting to slightly larger separations for more massive ones.
- ID:
- ivo://CDS.VizieR/J/A+A/522/A29
- Title:
- OGLE2-TR-L9 g'r'i'z' light curves
- Short Name:
- J/A+A/522/A29
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Repeated observations of exoplanet transits allow us to refine the planetary parameters and probe them for any time dependent variations. In particular deviations of the period from a strictly linear ephemeris, transit timing variations (TTVs), can indicate the presence of additional bodies in the planetary system. Aims: Our goal was to reexamine the largely unstudied OGLE2-TR-L9 system with high cadence, multi-color photometry in order to refine the planetary parameters and probe the system for TTVs. From our analysis we find that the semi-major axis and the inclination differ from the previously published values. With the newly observed transits, we were able to refine the ephemeris to 2454492.80008(+/-0.00014) +2.48553417(+/-6.4)x10^-7^E. The newly derived parameters are a=0.0418(+/-0.0015)AU, r_p_=1.67(+/-0.05) R_j_, and inc=82.47{deg}(+/-0.12), differing significantly in a and inc from the previously published values. Within our data, we find indications for TTVs.
- ID:
- ivo://CDS.VizieR/J/A+A/627/A57
- Title:
- ONC binary and triple stars
- Short Name:
- J/A+A/627/A57
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Recently published high-quality OmegaCAM photometry of the 3x3deg around the Orion Nebula Cluster (ONC) in r, and i filters revealed three well-separated pre-main sequences in the color-magnitude diagram (CMD). The objects belonging to the individual sequences are concentrated toward the center of the ONC. The authors concluded that there are two competitive scenarios: a population of unresolved binaries and triples with an exotic mass ratio distribution, or three stellar populations with different ages (~=1Myr age differences). We use Gaia DR2 in combination with the photometric OmegaCAM catalog to test and confirm the presence of the putative three stellar populations. We also study multiple stellar systems in the ONC for the first time using Gaia DR2. We selected ONC members based on parallaxes and proper motions and take advantage from OmegaCAM photometry that performs better than Gaia DR2 photometry in crowded regions. We identify two clearly separated sequences with a third suggested by the data. We used Pisa stellar isochrones to estimate ages of the stellar populations with absolute magnitudes computed using Gaia parallaxes on a star by star basis. (1) We confirm that the second and third sequence members are more centrally concentrated toward the center of the ONC. In addition we find an indication that the parallax and proper motion distributions are different among the members of the stellar sequences. The age difference among stellar populations is estimated to be 1-2Myr. (2) We use Gaia proper motions and other measures to identify and remove as many unresolved multiple system candidates as possible. Nevertheless we are still able to recover two well-separated sequences with evidence for the third one, supporting the existence of the three stellar populations. (3) Due to having ONC members with negligible fore- or background contamination we were able to identify a substantial number of wide binary objects (separation between 1000 and 3000 au) and with relative proper motions of the binary components consistent with zero. This challenges previously inferred values that suggested no wide binary stars exist in the ONC. Our inferred wide-binary fraction is ~=5%. We confirm the three populations correspond to three separated episodes of star formation. Based on this result, we conclude that star formation is not happening in a single burst in this region. In addition we identify 5% of wide-binary stars in the ONC that were thought not to be present.
- ID:
- ivo://CDS.VizieR/J/ApJ/727/102
- Title:
- On the frequency of Jupiter analogs
- Short Name:
- J/ApJ/727/102
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Anglo-Australian Planet Search has now accumulated 12 years of radial-velocity data with long-term instrumental precision better than 3m/s. In this paper, we expand on earlier simulation work, to probe the frequency of near-circular, long-period gas-giant planets residing at orbital distances of 3-6AU -the so-called Jupiter analogs. We present the first comprehensive analysis of the frequency of these objects based on radial-velocity data. We find that 3.3% of stars in our sample host Jupiter analogs; detailed, star-by-star simulations show that no more than 37% of stars host a giant planet between 3 and 6AU.
- ID:
- ivo://CDS.VizieR/J/ApJ/710/L30
- Title:
- On the multiplicity of the O star Herschel 36
- Short Name:
- J/ApJ/710/L30
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the analysis of high-resolution optical spectroscopic observations of the zero-age main-sequence O star Herschel 36 spanning six years. This star is definitely a multiple system, with at least three components detected in its spectrum. Based on our radial-velocity (RV) study, we propose a picture of a close massive binary and a more distant companion, most probably in wide orbit about each other. The orbital solution for the binary, whose components we identify as O9V and B0.5V, is characterized by a period of 1.5415+/-0.0006 days. With a spectral type O7.5V, the third body is the most luminous component of the system and also presents RV variations with a period close to 498 days. Some possible hypotheses to explain the variability are briefly addressed and further observations are suggested.
- ID:
- ivo://CDS.VizieR/J/MNRAS/454/3094
- Title:
- Optical transit light curves of WASP-57
- Short Name:
- J/MNRAS/454/3094
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Transits in the WASP-57 planetary system have been found to occur half an hour earlier than expected. We present 10 transit light curves from amateur telescopes, on which this discovery was based, 13 transit light curves from professional facilities which confirm and refine this finding, and high-resolution imaging which show no evidence for nearby companions. We use these data to determine a new and precise orbital ephemeris, and measure the physical properties of the system. Our revised orbital period is 4.5 s shorter than found from the discovery data alone, which explains the early occurrence of the transits. We also find both the star and planet to be larger and less massive than previously thought. The measured mass and radius of the planet are now consistent with theoretical models of gas giants containing no heavy-element core, as expected for the subsolar metallicity of the host star. Two transits were observed simultaneously in four passbands. We use the resulting light curves to measure the planet's radius as a function of wavelength, finding that our data are sufficient in principle but not in practise to constrain its atmospheric properties. We conclude with a discussion of the current and future status of transmission photometry studies for probing the atmospheres of gas-giant transiting planets.
