PSST: The Planet Search Survey Telescope

Dunham, E. W.; Mandushev, Georgi; Taylor, B.; Oetiker, Brian

doi:10.1086/426303

Cited by 66 publications

(68 citation statements)

References 41 publications

(48 reference statements)

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“…[1][2][3] To confirm this identification, its electronic, vibrational, and rotational transitions have also been studied in the laboratory. [4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19] Apart from its astrophysical importance, the CH + ion has also attracted much attention such as BH and AlH due to their unusual magnetic properties [20][21][22][23][24][25][26][27][28][29][30][31][32][33] similar to temperature independent paramagnetism, antishielding, a large spin-rotation constant of the carbon atom, and a large and negative rotational g-factor, which are rarely found in closed shell molecules.…”

Section: Introductionmentioning

confidence: 88%

Communication: Rotational g-factor and spin-rotation constant of CH+

Sauer

2010

The Journal of Chemical Physics

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The rotational g-factor and spin-rotation constants of the methylidynium ion CH + have been calculated for the first time with a large multiconfigurational self-consistent field wave function and at the coupled-cluster singles and doubles level augmented by a perturbative triples correction. The results for an equilibrium internuclear distance as well as for the v =0, J = 1 vibration-rotational state are presented.

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Section: Introductionmentioning

confidence: 88%

Communication: Rotational g-factor and spin-rotation constant of CH+

Sauer

2010

The Journal of Chemical Physics

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“…The TrES survey was carried out by a network of three 10 cm telescopes: the Sleuth telescope at Mount Palomar, CA (O'Donovan et al 2004), the Planet Search Survey Telescope (PSST; Dunham et al 2004) at Lowell Observatory, AZ, and the STellar Astrophysics and Research on Exoplanets telescope (STARE; Alonso et al 2004b), on the island of Tenerife, in the Canary Islands, Spain. Each TrES telescope was equipped with a 2 K × 2 K CCD with 13 μm pixels, producing a plate scale of ∼10 pixel −1 and photometric apertures of ∼30 .…”

Section: Tres Observations Of L1495mentioning

confidence: 99%

“…Data from each TrES telescope were reduced independently, following the reduction procedures described in full by Dunham et al (2004), Mandushev et al (2005), and O' Donovan et al (2006Donovan et al ( , 2007. In brief, stars were detected in each individual frame using a modified version of the DAOPHOT II package (Stetson 1987(Stetson , 1992, with aperture photometry measured for each star from a difference image produced by subtracting each target image from a master reference frame with the ISIS code (Alard 2000).…”

Section: Tres Observations Of L1495mentioning

confidence: 99%

A Census of Rotation and Variability in L1495: A Uniform Analysis of Trans-Atlantic Exoplanet Survey Light Curves for Pre-Main-Sequence Stars in Taurus

Hong

Covey

Rebull

et al. 2012

ApJS

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We analyze light curves obtained by the Trans-atlantic Exoplanet Survey (TrES) for a field centered on the L1495 dark cloud in Taurus. The Spitzer Taurus Legacy Survey catalog identifies 179 bona fide Taurus members within the TrES field; 48 of the known Taurus members are detected by TrES, as well as 26 candidate members identified by the Spitzer Legacy team. We quantify the variability of each star in our sample using the ratio of the standard deviation of the original light curve (σ orig. ) to the standard deviation of a light curve that has been smoothed by 9 or 1001 epochs (σ 9 and σ 1001 , respectively). Known Taurus members typically demonstrate (σ orig. /σ 9 ) < 2.0, and (σ orig. /σ 1001 ) < 5, while field stars reveal (σ orig. /σ 9 ) ∼ 3.0 and (σ orig. /σ 1001 ) ∼ 10, as expected for light curves dominated by unstructured white noise. Of the 74 Taurus members/candidates with TrES light curves, we detect significant variability in 49 sources. Adapting a quantitative metric originally developed to assess the reliability of transit detections, we measure the amount of red and white noise in each light curve and identify 18 known or candidate Taurus members with highly significant period measurements. These appear to be the first periods measured for four of these sources (HD 282276, CX Tau, FP Tau, TrES J042423+265008), and in two other cases, the first non-aliased periods (LkCa 21 and DK Tau AB). For the remainder, the TrES measurements typically agree very well (δP < 1%) with previously reported values. Including periods measured at lower confidence for 15 additional sources, we report periods for 11 objects where no previous periods were found, including 8 confirmed Taurus members. We also identify 10 of the 26 candidate Taurus members that demonstrate variability levels consistent with being bona fide T Tauri stars. A Kolomgorov-Smirnov (K-S) test confirms that these new periods confirm the distinction between the rotation period distributions of stars with and without circumstellar disks, with only a 10% probability of the two populations sharing the same parent period distribution. K-S tests do suggest, however, that the updated Taurus period distribution now more closely resembles those measured in other young star-forming clusters (i.e., NGC 2264, NGC 6530, and the ONC). This improved agreement may reflect the exclusion of long rotation periods which are detected in Taurus at lower significance, and which may be beyond the limits of detectability in more distant star-forming regions.

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“…This telescope is part of TrES, with telescopes at Palomar Observatory ( USA), Lowell Observatory ( USA), and Instituto de Astrofísica de Canarias (Spain). The PSST is a 105 mm f/2.8 refractor equipped with a 2K ; 2K CCD and is described fully in Dunham et al (2004). Nearly all exposures were taken through a Kron-Cousins R filter with the exception of several hundred B and V images on 2003 March 7 and 8 that were used to estimate stellar colors.…”

Section: Wide-field Photometry Amentioning

confidence: 99%

“…While there is very little published observational data on the rate of false alarms in wide-field transit surveys, the statistics in Dunham et al (2004) and the preliminary results from the Vulcan survey ( Latham 2003) indicate that the frequency of false positives is very high, probably 20 or more times the number of true planetary transits. In the case of TrES-1, the only transiting planet discovered in such a survey (Alonso et al 2004), the ratio of transit candidates to true planets was 25:1.…”

Section: Introductionmentioning

confidence: 99%

The Challenge of Wide‐Field Transit Surveys: The Case of GSC 01944‐02289

Mandushev

Torres

Latham

et al. 2005

ApJ

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Wide-field searches for transiting extrasolar giant planets face the difficult challenge of separating true transit events from the numerous false positives caused by isolated or blended eclipsing binary systems. We describe here the investigation of GSC 01944-02289, a very promising candidate for a transiting brown dwarf detected by the Trans-Atlantic Exoplanet Survey ( TrES) network. The photometry and radial velocity observations suggested that the candidate was an object of substellar mass in orbit around an F star. However, careful analysis of the spectral line shapes revealed a pattern of variations consistent with the presence of another star whose motion produced the asymmetries observed in the spectral lines of the brightest star. Detailed simulations of blend models composed of an eclipsing binary plus a third star diluting the eclipses were compared with the observed light curve and used to derive the properties of the three components. Using the predicted stellar parameters, we were able to identify a second set of spectral lines corresponding to the primary of the eclipsing binary and derive its spectroscopic orbit. Our photometric and spectroscopic observations are fully consistent with a blend model of a hierarchical triple system composed of an eclipsing binary with G0 V and M3 V components in orbit around a slightly evolved F5 dwarf. The rotational broadening of the spectral lines of the F5 primary (v sin i % 34 km s À1 ) and its brightness relative to the eclipsing binary ($89% of the total light) made the discovery of the true nature of the system particularly difficult. We believe that this investigation will be helpful to other groups pursuing wide-field transit searches as this type of false detection could be more common than true transiting planets and difficult to identify.

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PSST: The Planet Search Survey Telescope

Cited by 66 publications

References 41 publications

Communication: Rotational g-factor and spin-rotation constant of CH+

Communication: Rotational g-factor and spin-rotation constant of CH+

A Census of Rotation and Variability in L1495: A Uniform Analysis of Trans-Atlantic Exoplanet Survey Light Curves for Pre-Main-Sequence Stars in Taurus

The Challenge of Wide‐Field Transit Surveys: The Case of GSC 01944‐02289

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