PIRATE: A Remotely Operable Telescope Facility for Research and Education

Holmes, S.; Kolb, U.; Haswell, C. A.; Burwitz, V.; Lucas, Robert J.; Rodríguez, J.; Rolfe, Samantha; Rostron, John; Barker, J. G.

doi:10.1086/662148

Cited by 18 publications

(17 citation statements)

References 24 publications

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“…67 images of J093010 (55 each in Baader G and B filters, 57 in R) were taken with the Open University's robotic 0.425 m PIRATE telescope (Holmes et al 2011;Kolb 2014) in Mallorca on the night of 30-31 December 2012, monitored by R. Busuttil. All exposures were 80 s; short enough to avoid phase smearing for the shorter-period system.…”

Section: Photometrymentioning

confidence: 99%

The doubly eclipsing quintuple low-mass star system 1SWASP J093010.78+533859.5

Lohr

Norton

Gillen

et al. 2015

A&A

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Our discovery of 1SWASP J093010.78+533859.5 as a probable doubly eclipsing quadruple system, containing a contact binary with P ∼ 0.23 d and a detached binary with P ∼ 1.31 d, was announced in 2013. Subsequently, Koo and collaborators confirmed the detached binary spectroscopically, and identified a fifth set of static spectral lines at its location, corresponding to an additional noneclipsing component of the system. Here we present new spectroscopic and photometric observations, allowing confirmation of the contact binary and improved modelling of all four eclipsing components. The detached binary is found to contain components of masses 0.837 ± 0.008 and 0.674 ± 0.007 M , with radii of 0.832 ± 0.018 and 0.669 ± 0.018 R and effective temperatures of 5185 +25 −20and 4325 +20 −15 K, respectively; the contact system has masses 0.86 ± 0.02 and 0.341 ± 0.011 M , radii of 0.79 ± 0.04 and 0.52 ± 0.05 R , respectively, and a common effective temperature of 4700 ± 50 K. The fifth star is of similar temperature and spectral type to the primaries in the two binaries. Long-term photometric observations indicate the presence of a spot on one component of the detached binary, moving at an apparent rate of approximately one rotation every two years. Both binaries have consistent system velocities around −11 to −12 km s −1 , which match the average radial velocity of the fifth star; consistent distance estimates for both subsystems of d = 78 ± 3 and d = 73 ± 4 pc are also found, and, with some further assumptions, of d = 83 ± 9 pc for the fifth star. These findings strongly support the claim that both binaries -and very probably all five stars -are gravitationally bound in a single system. The consistent angles of inclination found for the two binaries (88.2 ± 0.3 • and 86 ± 4 • ) may also indicate that they originally formed by fragmentation (around 9-10 Gyr ago) from a single protostellar disk, and subsequently remained in the same orbital plane.

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Section: Photometrymentioning

confidence: 99%

The doubly eclipsing quintuple low-mass star system 1SWASP J093010.78+533859.5

Lohr

Norton

Gillen

et al. 2015

A&A

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“…An additional three egress times were obtained from the eclipse observations carried out with the PIRATE telescope equipped with the SBIG STL1001E CCD camera (Holmes et al 2011). PIRATE, funded by the Open University, Department of Physics and Astronomy, is a remote-controlled telescope located at the Astronomical Observatory of Mallorca (OAM), Spain.…”

Section: Observations With Optima and Other Instrumentsmentioning

confidence: 99%

On the HU Aquarii planetary system hypothesis

Goździewski

Nasıroğlu

Słowikowska

et al. 2012

Monthly Notices of the Royal Astronomical Society

130

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In this work, we investigate the eclipse timing of the polar binary HU Aquarii that has been observed for almost two decades. Recently, Qian et al. attributed large (O-C) deviations between the eclipse ephemeris and observations to a compact system of two massive jovian companions. We improve the Keplerian, kinematic model of the Light Travel Time (LTT) effect and re-analyse the whole currently available data set. We add almost 60 new, yet unpublished, mostly precision light curves obtained using the time high-resolution photo-polarimeter OPTIMA, as well as photometric observations performed at the MONET/N, PIRATE and TCS telescopes. We determine new mid--egress times with a mean uncertainty at the level of 1 second or better. We claim that because the observations that currently exist in the literature are non-homogeneous with respect to spectral windows (ultraviolet, X-ray, visual, polarimetric mode) and the reported mid--egress measurements errors, they may introduce systematics that affect orbital fits. Indeed, we find that the published data, when taken literally, cannot be explained by any unique solution. Many qualitatively different and best-fit 2-planet configurations, including self-consistent, Newtonian N-body solutions may be able to explain the data. However, using high resolution, precision OPTIMA light curves, we find that the (O-C) deviations are best explained by the presence of a single circumbinary companion orbiting at a distance of ~4.5 AU with a small eccentricity and having ~7 Jupiter-masses. This object could be the next circumbinary planet detected from the ground, similar to the announced companions around close binaries HW Vir, NN Ser, UZ For, DP Leo or SZ Her, and planets of this type around Kepler-16, Kepler-34 and Kepler-35.Comment: 20 pages, 18 figures, accepted to Monthly Notices of the Royal Astronomical Society (MNRAS

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“…The transit of WASP-65b was also observed on 2012 February 18 by the PIRATE Facility 2 (PIRATE Mk II configuration) located at the Observatori Astronòmic de Mallorca (for details see Holmes et al 2011). The time series is composed of 120-s exposures that captured nearly 6 h of out-of-transit light curve (with the pier flip after about 2 h), as well as the ingress.…”

Section: Pirate Observationsmentioning

confidence: 99%

“…The data sets were calibrated in the standard way using flat field, dark and bias frames. We constructed the light curves using the ensemble photometry pipeline described in Holmes et al (2011). Pre-and post-pier flip branches were analysed separately.…”

Section: Pirate Observationsmentioning

confidence: 99%

Discovery of WASP-65b and WASP-75b: Two hot Jupiters without highly inflated radii

Chew¹,

Faedi²,

Pollacco³

et al. 2013

A&A

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We report the discovery of two transiting hot Jupiters, WASP-65b (M pl = 1.55 ± 0.16 M J ; R pl = 1.11 ± 0.06 R J ), and WASP-75b (M pl = 1.07 ± 0.05 M J ; R pl = 1.27 ± 0.05 R J ). They orbit their host star every ∼2.311, and ∼2.484 days, respectively. The planet host WASP-65 is a G6 star (T eff = 5600 K, [Fe/H] = −0.07 ± 0.07, age 8 Gyr); WASP-75 is an F9 star (T eff = 6100 K, [Fe/H] = 0.07 ± 0.09, age ∼ 3 Gyr). WASP-65b is one of the densest known exoplanets in the mass range 0.1 and 2.0 M J (ρ pl = 1.13 ± 0.08 ρ J ), a mass range where a large fraction of planets are found to be inflated with respect to theoretical planet models. WASP-65b is one of only a handful of planets with masses of ∼1.5 M J , a mass regime surprisingly underrepresented among the currently known hot Jupiters. The radius of WASP-75b is slightly inflated ( 10%) as compared to theoretical planet models with no core, and has a density similar to that of Saturn (ρ pl = 0.52 ± 0.06 ρ J ).

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PIRATE: A Remotely Operable Telescope Facility for Research and Education

Cited by 18 publications

References 24 publications

The doubly eclipsing quintuple low-mass star system 1SWASP J093010.78+533859.5

The doubly eclipsing quintuple low-mass star system 1SWASP J093010.78+533859.5

On the HU Aquarii planetary system hypothesis

Discovery of WASP-65b and WASP-75b: Two hot Jupiters without highly inflated radii

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