Building an Automated Telescope with High Photometric Accuracy

Grauer, A. D.; Neely, Andrew J.; Lacy, Claud H.

doi:10.1086/591808

Cited by 21 publications

(16 citation statements)

References 9 publications

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“…Nearly all the observations after this date were obtained with the NFO, which is a robotic 24 inch Cassegrain reflector located near Silver City, NM, USA. See the article by Grauer et al (2008) for details about the NFO. Both telescopes used Bessel V filters consisting of 2.0 mm of GG495 and 3.0 mm of BG 39.…”

Section: Photometric Observations and Orbitmentioning

confidence: 99%

Absolute Properties of the Pre-Main-Sequence Eclipsing Binary Star Np Persei

Lacy¹,

Fekel²,

Pavlovski³

et al. 2016

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NP Per is a well-detached, 2.2 day eclipsing binary whose components are both pre-main-sequence stars that are still contracting toward the main-sequence phase of evolution. We report extensive photometric and spectroscopic observations with which we have determined their properties accurately. Their surface temperatures are quite different: 6420±90 K for the larger F5 primary star and 4540±160 K for the smaller K5e star. Their masses and radii are 1.3207±0.0087 solar masses and 1.372±0.013 solar radii for the primary, and 1.0456±0.0046 solar masses and 1.229±0.013 solar radii for the secondary. The orbital period is variable over long periods of time. A comparison of the observations with current stellar evolution models from MESA indicates that the stars cannot be fit at a single age: the secondary appears significantly younger than the primary. If the stars are assumed to be coeval and to have the age of the primary (17 Myr), then the secondary is larger and cooler than predicted by current models. The Hα spectral line of the secondary component is completely filled by, presumably, chromospheric emission due to a magnetic activity cycle.

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Section: Photometric Observations and Orbitmentioning

confidence: 99%

Absolute Properties of the Pre-Main-Sequence Eclipsing Binary Star Np Persei

Lacy¹,

Fekel²,

Pavlovski³

et al. 2016

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“…The NFO instrument consists of a 24-inch Cassegrain reflector with a field-widening correcting lens near 1 pamela and molly were written by Prof. Tom Marsh and are available at www.warwick.ac.uk/go/trmarsh the focus housed in a roll-off roof structure (Grauer et al 2008). At the focus is a camera based on the Kodak KAF-4301E charge coupled device (CCD) with a field of view of about 27 × 27 arcmin.…”

Section: Photometrymentioning

confidence: 99%

Precise mass and radius measurements for the components of the bright solar-type eclipsing binary star V1094 Tauri

Maxted

Hutcheon

Torres

et al. 2015

A&A

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Context. V1094 Tau is bright eclipsing binary star with an orbital period close to 9 days that contains two stars similar to the Sun. Aims. Our aim is to test models of Sun-like stars using precise and accurate mass and radius measurements for both stars in V1094 Tau. Methods. We present new spectroscopy of V1094 Tau, which we use to estimate the effective temperatures of both stars and to refine their spectroscopic orbits. We also present new, high-quality photometry covering both eclipses of V1094 Tau in the Strömgren uvby system and in the Johnson V-band. Results. The masses, radii, and effective temperatures of the stars in V1094 Tau are found to be M A = 1.0965 ± 0.

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“…The NFO WebScope is located near Silver City (New Mexico) in a roll-off roof structure, and consists of a 24 inch Cassegrain reflector with a field-widening correcting lens near the focus (see Grauer et al 2008). At the focus is a camera based on the Kodak KAF-4301E CCD chip, with a field of view of about 27× 27 arcminutes.…”

Section: Differential Photometrymentioning

confidence: 99%

Absolute Properties of the Eclipsing Binary System Aq Serpentis: A Stringent Test of Convective Core Overshooting in Stellar Evolution Models

Torres

Vaz

Lacy

et al. 2014

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We report differential photometric observations and radial-velocity measurements of the detached, 1.69 day period, double-lined eclipsing binary AQ Ser. Accurate masses and radii for the components are determined to better than 1.8% and 1.1%, respectively, and are M 1 = 1.417 ± 0.021 M , M 2 = 1.346 ± 0.024 M , R 1 = 2.451 ± 0.027 R , and R 2 = 2.281 ± 0.014 R . The temperatures are 6340 ± 100 K (spectral type F6) and 6430 ± 100 K (F5), respectively. Both stars are considerably evolved, such that predictions from stellar evolution theory are particularly sensitive to the degree of extra mixing above the convective core (overshoot). The component masses are different enough to exclude a location in the H-R diagram past the point of central hydrogen exhaustion, which implies the need for extra mixing. Moreover, we find that current main-sequence models are unable to match the observed properties at a single age even when allowing the unknown metallicity, mixing length parameter, and convective overshooting parameter to vary freely and independently for the two components. The age of the more massive star appears systematically younger. AQ Ser and other similarly evolved eclipsing binaries showing the same discrepancy highlight an outstanding and largely overlooked problem with the description of overshooting in current stellar theory.

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Building an Automated Telescope with High Photometric Accuracy

Cited by 21 publications

References 9 publications

Absolute Properties of the Pre-Main-Sequence Eclipsing Binary Star Np Persei

Absolute Properties of the Pre-Main-Sequence Eclipsing Binary Star Np Persei

Precise mass and radius measurements for the components of the bright solar-type eclipsing binary star V1094 Tauri

Absolute Properties of the Eclipsing Binary System Aq Serpentis: A Stringent Test of Convective Core Overshooting in Stellar Evolution Models

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