Radial Velocity Confirmation of a Binary Detected From Pulse Timings

Barlow, B. N.; Dunlap, B. H.; Clemens, J. C.

doi:10.1088/2041-8205/737/1/l2

Cited by 18 publications

(15 citation statements)

References 16 publications

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“…For the non-linear, least-squared fitting process, we used the Levenberg-Marquardt (LM, hereafter) minimisation algorithm as implemented in the IDL routine MPFIT 1 (Markwardt et al 2009). This algorithm has found widespread applications within astronomy including timing-modeling (Barlow, Dunlap & Clemens 2011). In this routine, partial derivatives for computing the gradient field in a parameter space are calculated from numerical differentiations of model functions.…”

Section: Least-squared Fitting With Mpfitmentioning

confidence: 99%

“…The studies by Beuermann et al (2010) and Potter et al (2011) inferred the presence of additional massive objects by explaining the observed timing anomalies with the light-travel time (LTT, hereafter) effect. In the ideal case, the stellar components of an eclipsing binary system are orbiting their common centre of mass with a constant period.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

New light-travel time models and orbital stability study of the proposed planetary system HU Aquarii

Hinse

Lee

Goździewski

et al. 2012

Monthly Notices of the Royal Astronomical Society

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In this work we propose a new orbital architecture for the two proposed circumbinary planets around the polar eclipsing binary HU Aquarii. We base the new two-planet, light-travel time model on the result of a Monte Carlo simulation driving a least-squares Levenberg-Marquardt minimization algorithm on the observed eclipse egress times. Our best-fitting model with χ 2 r = 1.43 resulted in high final eccentricities for the two companions leading to an unstable orbital configuration. From a large ensemble of initial guesses, we examined the distribution of final eccentricities and semimajor axes for different χ 2 r parameter intervals and encountered qualitatively a second population of best-fitting parameters. The main characteristic of this population is described by low-eccentric orbits favouring long-term orbital stability of the system. We present our best-fitting model candidate for the proposed two-planet system and demonstrate orbital stability over one million years using numerical integrations.

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Section: Least-squared Fitting With Mpfitmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

New light-travel time models and orbital stability study of the proposed planetary system HU Aquarii

Hinse

Lee

Goździewski

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…V2051 Oph (AB) b, Qian et al 2015). In particular, the detection of a late-type main sequence star companion to the sdB CS 1246 by Barlow et al (2011b), subsequently confirmed with radial velocity data (Barlow et al 2011a), or other studies like Otani et al (2018), demonstrate the viability of this method in sdB systems. On the other hand, the particular example of V391 Peg b is currently under discussion (Silvotti et al 2018) because of possible non-linear interactions between different pulsation modes that change arrival times (see Zong et al 2018 for a detailed study of amplitude/frequency variations related to non-linear effects).…”

Section: Introductionmentioning

confidence: 62%

The EXOTIME project: signals in the O–C diagrams of the rapidly pulsating subdwarfs DW Lyn, V1636 Ori, QQ Vir, and V541 Hya

Mackebrandt

Schuh

Silvotti

et al. 2020

A&A

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Aims. We aim to investigate variations in the arrival time of coherent stellar pulsations due to the light-travel time effect to test for the presence of sub-stellar companions. Those companions are the key to one possible formation scenario of apparently single sub-dwarf B stars. Methods. We made use of an extensive set of ground-based observations of the four large amplitude p-mode pulsators DW Lyn, V1636 Ori, QQ Vir, and V541 Hya. Observations of the TESS space telescope are available on two of the targets. The timing method compares the phase of sinusoidal fits to the full multi-epoch light curves with phases from the fit of a number of subsets of the original time series. Results. Observations of the TESS mission do not sample the pulsations well enough to be useful due to the (currently) fixed two-minute cadence. From the ground-based observations, we infer evolutionary parameters from the arrival times. The residual signals show many statistically significant periodic signals, but no clear evidence for changes in arrival time induced by sub-stellar companions. The signals can be explained partly by mode beating effects. We derive upper limits on companion masses set by the observational campaign.

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“…Stellar pulsations can also serve as accurate clocks for discovering planets (see Schuh 2010). Confirmation of the pulse timing method's ability to find unseen companions has been provided in several cases (e.g., Vinko 1993; Barlow et al 2011), although none of the detected objects were planets. A few substellar and planetary detections have been reported, but without radial velocity confirmation (Silvotti et al 2007;Mullally et al 2008a).…”

Section: Stellar Pulsation Timing For Exoplanet Detectionmentioning

confidence: 98%

Evryscope Science: Exploring the Potential of All-Sky Gigapixel-Scale Telescopes

Law¹,

Fors²,

Ratzloff³

et al. 2015

Publications of the Astronomical Society of the Pacific

108

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Low-cost mass-produced sensors and optics have recently made it feasible to build telescope arrays which observe the entire accessible sky simultaneously. In this article we discuss the scientific motivation for these telescopes, including exoplanets, stellar variability and extragalactic transients. To provide a concrete example we detail the goals and expectations for the Evryscope, an underconstruction 780 MPix telescope which covers 8,660 square degrees in each two-minute exposure; each night, 18,400 square degrees will be continuously observed for an average of ≈6 hours. Despite its small 61mm aperture, the system's large field of view provides anétendue which is ∼10% of LSST. The Evryscope, which places 27 separate individual telescopes into a common mount which tracks the entire accessible sky with only one moving part, will return 1%-precision, many-year-length, highcadence light curves for every accessible star brighter than ∼ 16 th magnitude. The camera readout times are short enough to provide near-continuous observing, with a 97% survey time efficiency. The array telescope will be capable of detecting transiting exoplanets around every solar-type star brighter than m V =12, providing at least few-millimagnitude photometric precision in long-term light curves. It will be capable of searching for transiting giant planets around the brightest and most nearby stars, where the planets are much easier to characterize; it will also search for small planets nearby M-dwarfs, for planetary occultations of white dwarfs, and will perform comprehensive nearby microlensing and eclipse-timing searches for exoplanets inaccessible to other planet-finding methods. The Evryscope will also provide comprehensive monitoring of outbursting young stars, white dwarf activity, and stellar activity of all types, along with finding a large sample of very-long-period M-dwarf eclipsing binaries. When relatively rare transients events occur, such as gamma-ray bursts (GRBs), nearby supernovae, or even gravitational wave detections from the Advanced LIGO/Virgo network, the array will return minute-by-minute light curves without needing pointing towards the event as it occurs. By co-adding images, the system will reach V∼19 in one-hour integrations, enabling the monitoring of faint objects. Finally, by recording all data, the Evryscope will be able to provide pre-event imaging at two-minute cadence for bright transients and variable objects, enabling the first high-cadence searches for optical variability before, during and after all-sky events.

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Radial Velocity Confirmation of a Binary Detected From Pulse Timings

Cited by 18 publications

References 16 publications

New light-travel time models and orbital stability study of the proposed planetary system HU Aquarii

New light-travel time models and orbital stability study of the proposed planetary system HU Aquarii

The EXOTIME project: signals in the O–C diagrams of the rapidly pulsating subdwarfs DW Lyn, V1636 Ori, QQ Vir, and V541 Hya

Evryscope Science: Exploring the Potential of All-Sky Gigapixel-Scale Telescopes

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