Final tests and commissioning of the UCL echelle spectrograph

Diego, F.; Charalambous, A.; Fish, A. C.; Walker, David D.

doi:10.1117/12.19119

Cited by 72 publications

(40 citation statements)

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“…Spectra were obtained with the High-Resolution Echelle Spectrometer (HIRES) on the 10 m telescope at Keck Observatory (Vogt et al 1994), the University College London Echelle Spectrograph (UCLES) on the 4 m Anglo-Australian Telescope (AAT) at Siding Spring Observatory (Diego et al 1990), and the Hamilton echelle spectrometer at Lick Observatory (Vogt 1987). Observations at Lick were obtained with both the 3 m Shane telescope and the 0.6 m coudé auxiliary telescope (CAT).…”

Section: Observationsmentioning

confidence: 99%

Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs

Valenti

Fischer

2005

ASTROPHYS J SUPPL S

1,309

1,152

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We present a uniform catalog of stellar properties for 1040 nearby F, G, and K stars that have been observed by the Keck, Lick, and AAT planet search programs. Fitting observed echelle spectra with synthetic spectra yielded effective temperature, surface gravity, metallicity, projected rotational velocity, and abundances of the elements Na, Si, Ti, Fe, and Ni, for every star in the catalog. Combining V-band photometry and Hipparcos parallaxes with a bolometric correction based on the spectroscopic results yielded stellar luminosity, radius, and mass. Interpolating Yonsei-Yale isochrones to the luminosity, effective temperature, metallicity, and -element enhancement of each star yielded a theoretical mass, radius, gravity, and age range for most stars in the catalog. Automated tools provide uniform results and make analysis of such a large sample practical. Our analysis method differs from traditional abundance analyses in that we fit the observed spectrum directly, rather than trying to match equivalent widths, and we determine effective temperature and surface gravity from the spectrum itself, rather than adopting values based on measured photometry or parallax. As part of our analysis, we determined a new relationship between macroturbulence and effective temperature on the main sequence. Detailed error analysis revealed small systematic offsets with respect to the Sun and spurious abundance trends as a function of effective temperature that would be inobvious in smaller samples. We attempted to remove these errors by applying empirical corrections, achieving a precision per spectrum of 44 K in effective temperature, 0.03 dex in metallicity, 0.06 dex in the logarithm of gravity, and 0.5 km s À1 in projected rotational velocity. Comparisons with previous studies show only small discrepancies. Our spectroscopically determined masses have a median fractional precision of 15%, but they are systematically 10% higher than masses obtained by interpolating isochrones. Our spectroscopic radii have a median fractional precision of 3%. Our ages from isochrones have a precision that varies dramatically with location in the Hertzsprung-Russell diagram. We plan to extend the catalog by applying our automated analysis technique to other large stellar samples.

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Section: Observationsmentioning

confidence: 99%

Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs

Valenti

Fischer

2005

ASTROPHYS J SUPPL S

1,309

1,152

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“…The PPPS used the UCLES echelle spectrograph (Diego et al 1990) at the AAT to obtain high-resolution spectra, with an observing procedure identical to that used by the 16-year Anglo-Australian Planet Search (AAPS). UCLES uses a 1-arcsec slit to deliver a resolving power of R ∼ 45 000.…”

Section: A At O B S E Rvat I O N S a N D S T E L L A R P Ro P E Rt I E Smentioning

confidence: 99%

The Pan-Pacific Planet Search III: five companions orbiting giant stars

Wittenmyer

Butler

Wang

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We report a new giant planet orbiting the K giant HD 155233, as well as four stellar-mass companions from the Pan-Pacific Planet Search, a Southern hemisphere radial velocity survey for planets orbiting nearby giants and sub-giants. We also present updated velocities and a refined orbit for HD 47205b (7 CMa b), the first planet discovered by this survey. HD 155233b has a period of 885 ± 63 d, eccentricity e = 0.03 ± 0.20, and m sin i = 2.0 ± 0.5 M Jup . The stellar-mass companions range in m sin i from 0.066 to 0.33 M . Whilst HD 104358B falls slightly below the traditional 0.08 M hydrogen-burning mass limit, and is hence a browndwarf candidate, we estimate only a 50 per cent a priori probability of a truly sub-stellar mass.Key words: techniques: radial velocities -planetary systems -planets and satellites: detection. I N T RO D U C T I O NRadial velocity planet search efforts have been underway for more than 20 yr, discovering hundreds of new planetary companions. However, brown-dwarf and stellar-mass companions tend to be largely ignored in these surveys: limited telescope time means that targets showing large amplitude variations ( 500 m s −1 ) are usually dropped from the observing queue. Only limited results on such massive companions have been published (Patel et al. 2007), with many objects featuring incomplete orbits. However, such objects remain valuable for exploring the lower end of the mass function and the properties of stellar systems in the Solar neighbourhood. The observed deficit of companions between 13 and 80 M Jup is known as the 'brown-dwarf desert' (Marcy & Butler 2000;Mazeh et al. 2003), and became evident in the earliest days of radial velocity planet searches (Campbell, Walker & Yang 1988;Murdoch, Hearnshaw & Clark 1993). A comprehensive, self-consistent study by Grether & Lineweaver (2006) confirmed the presence of a 'valley' in the brown-dwarf mass range at M = 31 +25 −18 M Jup . Stellar companions are also not to be ignored, since any binary system with a well-characterized orbit is useful for a range of follow-up science. Most obviously, a precisely determined binary orbit permits the search for E-mail: rob@phys.unsw.edu.au additional Doppler velocity signals due to planets orbiting one or both stars. Binary systems compose ∼50 per cent of nearby star systems (Duquennoy & Mayor 1991;Raghavan et al. 2010), yet are hosts to only ∼5 per cent of known extrasolar planets. The mechanisms and outcomes of planet formation in close binary systems remain significant questions virtually unexplored by observations.At the 3.9 m Anglo-Australian Telescope (AAT), we carried out a five-year survey for planets orbiting intermediate-mass evolved stars in an effort to characterize the dependence of planetary system properties on stellar mass Reffert et al. 2015). The initial sample was selected according to these criteria: 1.0 < (B − V) < 1.2, 1.8 < M V < 3.0, and V < 8.0. Of those stars meeting these criteria, 18 were discarded as binaries by their Hipparcos multiple systems flag. From the 167...

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“…AAPS Doppler measurements are made with the UCLES echelle spectrograph (Diego et al 1990). An iodine absorption cell provides wavelength calibration from 5000 to 6200 Å.…”

Section: Observationsmentioning

confidence: 99%

A Neptune-Mass Planet Orbiting the Nearby G Dwarf Hd 16417

O'Toole

Tinney

Butler

et al. 2009

ApJ

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Precision Doppler measurements from an intensive 48 night "Rocky Planet Search" observing campaign on the Anglo-Australian Telescope (AAT) have revealed the presence of a low-mass exoplanet orbiting the G1 dwarf HD 16417. Subsequent Doppler observations with the AAT, as well as independent observations obtained by the Keck Planet Search, have confirmed this initial detection and refine the orbital parameters to period 17.24 ± 0.01 d, eccentricity 0.20 ± 0.09, orbital semimajor axis 0.14 ± 0.01 AU, and minimum planet mass 22.1 ± 2.0 M Earth . HD 16417 raises the number of published exoplanets with minimum masses of less than 25 M Earth to 18. Interestingly, the distribution of detected sub-25 M Earth planets over the spectral types G, K, and M is almost uniform. The detection of HD 16417b by an intensive observing campaign clearly demonstrates the need for extended and contiguous observing campaigns when aiming to detect low-amplitude Doppler planets in short-period orbits. Perhaps most critically it demonstrates that the search for low-mass Doppler planets will eventually require these traditional "bright-time" projects to extend throughout dark lunations.

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Final tests and commissioning of the UCL echelle spectrograph

Cited by 72 publications

References 0 publications

Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs

Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs

The Pan-Pacific Planet Search III: five companions orbiting giant stars

A Neptune-Mass Planet Orbiting the Nearby G Dwarf Hd 16417

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