Observations of Binary Stars with the Differential Speckle Survey Instrument. VIII. Measures of Metal-poor and Triple Stars from 2015 to 2018

Horch, Elliott; Tokovinin, Andreï; Weiss, Samuel A.; Lobb, J.; Casetti-Dinescu, Dana I.; Granucci, Nicole; Hess, Nicole M.; Everett, Mark E.; Belle, Gerald van; Winters, Jennifer G.; Nusdeo, Daniel A.; Henry, Todd J.; Howell, Steve B.; Teske, Johanna; Hirsch, Lea A.; Scott, Nicholas J.; Matson, Rachel A.; Kane, Stephen R.

doi:10.3847/1538-3881/aaf87e

Cited by 23 publications

(9 citation statements)

References 54 publications

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“…We assume that Δm i approaches zero at the diffraction limit. Since we are attempting to discover new companion stars (as opposed to detecting those already known to exist; Horch et al 2019), this assumption ensures that any companions will produce their own peaks in the image. Any peak that exceeds the 5σ value of Δm i at a specific angular distance is examined as a possible stellar companion.…”

Section: Speckle Imaging Observationsmentioning

confidence: 99%

“…Various observed properties of the companions including the position angle (PA), angular separation (α), and the product of seeing and separation ( ¢ q ; Horch et al 2004Horch et al , 2011 are listed in Table 3. For PA and α, we adopt representative uncertainties from Horch et al (2019). In Table 3, we also list the proper motion of the primary star in R.A. and decl.…”

Section: Speckle Imaging Observationsmentioning

confidence: 99%

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Speckle Imaging Characterization of Radial Velocity Exoplanet Systems

Dalba

Kane

Howell

et al. 2021

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We conducted speckle imaging observations of 53 stellar systems that were members of long-term radial velocity (RV) monitoring campaigns and exhibited substantial accelerations indicative of planetary or stellar companions in wide orbits. Our observations were made with blue and red filters using the Differential Speckle Survey Instrument at Gemini-South and the NN-Explore Exoplanet Stellar Speckle Imager at the WIYN telescope. The speckle imaging identifies eight luminous companions within 2″ of the primary stars. In three of these systems-HD1388, HD87359, and HD104304-the properties of the imaged companion are consistent with the RV measurements, suggesting that these companions may be associated with the primary and the cause of the RV variation. For all 53 stellar systems, we derive differential magnitude limits (i.e., contrast curves) from the imaging. We extend this analysis to include upper limits on companion mass in systems without imaging detections. In 25 systems, we rule out companions with masses greater than 0.2M e , suggesting that the observed RV signals are caused by late-M dwarfs or substellar (potentially planetary) objects. On the other hand, the joint RV and imaging analysis almost entirely rules out planetary explanations of the RV signal for HD19522 and suggests that the companion must have an angular separation below a few tenths of an arcsecond. This work highlights the importance of combined RV and imaging observations for characterizing the outer regions of nearby planetary systems.

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Section: Speckle Imaging Observationsmentioning

confidence: 99%

Section: Speckle Imaging Observationsmentioning

confidence: 99%

Speckle Imaging Characterization of Radial Velocity Exoplanet Systems

Dalba

Kane

Howell

et al. 2021

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“…For a recent study of the effects of metallicity on the MLR for M < 0.7M see Mann et al (2019). Our own speckle survey, described below, is focusing, in part, precisely on low-metallicity objects, following the pioneer study of Horch et al (2015bHorch et al ( , 2019a.…”

Section: Introductionmentioning

confidence: 99%

Orbital elements and individual component masses from joint spectroscopic and astrometric data of double-line spectroscopic binaries

Anguita-Aguero,

Mendez,

Claveria

et al. 2022

Preprint

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We present orbital elements, orbital parallaxes and individual component masses, for fourteen spatially resolved double-line spectroscopic binaries derived doing a simultaneous fit of their visual orbit and radial velocity curve. This was done by means a Markov Chain Monte Carlo code developed by our group, which produces posterior distribution functions and error estimates for all the parameters. Of this sample, six systems had high quality previous studies and were included as benchmarks to test our procedures, but even in these cases we could improve the previous orbits by adding recent data from our survey of southern binaries being carried out with the HRCam and ZORRO speckle cameras at the SOAR 4.1m and Gemini South 8.1m telescopes, respectively. We also give results for eight objects that did not have a published combined orbital solution, one of which did not have a visual orbit either. We could determine mass ratios with a typical uncertainty of less than 1%, mass sums with uncertainties of about 1% and individual component masses with a formal uncertainty of 0.01M in the best cases. A comparison of our orbital parallaxes with available trigonometric parallaxes from Hipparcos and Gaia eDR3, shows a good correspondence; the mean value of the differences being consistent with zero within the errors of both catalogs. We also present observational HR diagrams for our sample of binaries, which in combination with isochrones from different sources allowed us to asses their evolutionary status of and also the quality of their photometry.

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“…To complicate things further, there seems to be an intrinsic dispersion in the MLR caused by differences in age and chemical composition from star to star (see e.g. Horch et al (2015Horch et al ( , 2019).…”

Section: Introductionmentioning

confidence: 99%

Orbits and masses of binaries from Speckle Interferometry at SOAR

Mendez,

Claveria,

Costa

2021

Preprint

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We present results from Speckle inteferometric observations of fifteen visual binaries and one doubleline spectroscopic binary, carried out with the HRCam Speckle camera of the SOAR 4.1 m telescope. These systems were observed as a part of an on-going survey to characterize the binary population in the solar vicinity, out to a distance of 250 parsec.We obtained orbital elements and mass sums for our sample of visual binaries. The orbits were computed using a Markov Chain Monte Carlo algorithm that delivers maximum likelihood estimates of the parameters, as well as posterior probability density functions that allow us to evaluate their uncertainty. Their periods cover a range from 5 yr to more than 500 yr; and their spectral types go from early A to mid M -implying total system masses from slightly more than 4 M down to 0.2 M . They are located at distances between approximately 12 and 200 pc, mostly at low Galactic latitude.For the double-line spectroscopic binary YSC8 we present the first combined astrometric /radial velocity orbit resulting from a self-consistent fit, leading to individual component masses of 0.897 ± 0.027 M and 0.857 ± 0.026 M ; and an orbital parallax of 26.61 ± 0.29 mas, which compares very well with the Gaia DR2 trigonometric parallax (26.55 ± 0.27 mas).In combination with published photometry and trigonometric parallaxes, we place our objects on an H-R diagram and discuss their evolutionary status. We also present a thorough analysis of the precision and consistency of the photometry available for them.

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Observations of Binary Stars with the Differential Speckle Survey Instrument. VIII. Measures of Metal-poor and Triple Stars from 2015 to 2018

Cited by 23 publications

References 54 publications

Speckle Imaging Characterization of Radial Velocity Exoplanet Systems

Speckle Imaging Characterization of Radial Velocity Exoplanet Systems

Orbital elements and individual component masses from joint spectroscopic and astrometric data of double-line spectroscopic binaries

Orbits and masses of binaries from Speckle Interferometry at SOAR

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