The Tennessee State University Automatic Spectroscopic Telescope: Data Processing and Velocity Variation of Cool Giants

Eaton, J. A.; Williamson, Michael H.

doi:10.1086/521231

Cited by 82 publications

(58 citation statements)

References 43 publications

(36 reference statements)

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“…They derived M bol = −4.42, and estimated a mass of this object of 7.0-7.9 M . Their heliocentric radial velocity value of −42 km s −1 is in excellent agreement with other measurements in the literature (De Medeiros et al 2002;Valdes et al 2004;Eaton & Williamson 2007). Earlier studies of the stellar parameters found quite diverse results: van Paradijs (1973) measured a similar T eff = 4100 K, but a general overabundance of heavy elements by a factor of 1.6, while Luck & Bond (1980) derived for almost the same effective temperature a metallicity of [Fe/H] = −0.2.…”

Section: Hd 225212 K3 Isupporting

confidence: 85%

Crires-Pop

Lebzelter

Seifahrt

Uttenthaler

et al. 2012

A&A

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Context. New instrumental capabilities and the wealth of astrophysical information extractable from the near-infrared wavelength region have led to a growing interest in the field of high resolution spectroscopy at 1-5 μm. Aims. We aim to provide a library of observed high-resolution and high signal-to-noise-ratio near-infrared spectra of stars of various types throughout the Hertzsprung-Russell diagram. This is needed for the exploration of spectral features in this wavelength range and for comparison of reference targets with observations and models. Methods. High quality spectra were obtained using the CRIRES near-infrared spectrograph at ESO's VLT covering the range from 0.97 μm to 5.3 μm at high spectral resolution. Accurate wavelength calibration and correction for telluric lines were performed by fitting synthetic transmission spectra for the Earth's atmosphere to each spectrum individually. Results. We describe the observational strategy and the current status and content of the library which includes 13 objects. The first examples of finally reduced spectra are presented. This publication will serve as a reference paper to introduce the library to the community and explore the extensive amount of material.

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Section: Hd 225212 K3 Isupporting

confidence: 85%

Crires-Pop

Lebzelter

Seifahrt

Uttenthaler

et al. 2012

A&A

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“…From 2011 November through 2014 November, we acquired 56 high-quality spectra of NP Per with the Tennessee State University 2 m Automatic Spectroscopic Telescope (AST) and a fiber-fed echelle spectrograph (Eaton & Williamson 2007) at Fairborn Observatory in southeast Arizona. Of these spectra, 55 were suitable for radial velocity measurements.…”

Section: Spectroscopic Observations and Orbitsmentioning

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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“…T3 is one of eight automatic telescopes operated by Tennessee State University at Fairborn for automated photometry, spectroscopy, and imaging (Henry 1995(Henry , 1999Eaton et al 2003;Eaton & Williamson 2007). T3 is equipped with a precision photometer that employs an EMI 9924B photomultiplier tube (PMT) for the successive measurements of photon count rates through Johnson B and V filters.…”

Section: Observationsmentioning

confidence: 99%

Using Photometry to Probe the Circumstellar Environment of Δ Scorpii

Jones

Wiegert

Tycner

et al. 2013

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We acquired Johnson BV photometry of the binary Be disk system δ Scorpii during its 2009, 2010, 2011, and 2012 observing seasons and used it to probe the innermost regions of the disk. We found that several disk building events have occurred during this time, resulting in an overall brightening in the V band and reddening of the system. In addition to these long-term trends, we found cyclical variability in each observing season on timescales between 60 and 100 days. We were able to reproduce the changes in the magnitude and color of δ Sco using our theoretical models and found that variable mass-loss rates in the range 2.5-7.0 × 10 −9 M yr −1 over ∼35 days can reproduce the observed increase in brightness.

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The Tennessee State University Automatic Spectroscopic Telescope: Data Processing and Velocity Variation of Cool Giants

Cited by 82 publications

References 43 publications

Crires-Pop

Crires-Pop

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

Using Photometry to Probe the Circumstellar Environment of Δ Scorpii

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