We collected 44 spectra using HARPS-N at the Telescopio Nazionale Galileo (TNG), in La Palma (Cosentino et al. 2012SPIE. 8446E.. 1VC), with the goal of precisely determining the mass of the USP planet. To reach this goal, we followed a twofold strategy: we gathered at least two points each night (when weather allowed) in order to remove activity variations by applying nightly offsets (eg, Hatzes et al. 2011ApJ... 743... 75H; Pepe et al. 2013Natur. 503.. 377P), and we observed the target for a duration of a few stellar rotations to be able to use a Gaussian process (GP) regression (eg, Haywood et al. 2014MNRAS. 443.2517 H; Rajpaul et al. 2015MNRAS. 452.2269 R) to model the stellar activity signals directly.

We report g, V, and r photometric time series of HD 149026 spanning predicted times of transit of the Saturn-mass planetary companion, which was recently discovered by Sato and collaborators. We present a joint analysis of our observations and the previously reported photometry and radial velocities of the central star. We refine the estimate of the transit ephemeris to Tc = (2,453,527.87455) + (2.87598)N (HJD). Assuming that the star has a radius of 1.45 ± 0.10 R☉ and a mass of 1.30 ± 0.10 M☉, we estimate the planet radius to be (0.726 ± 0.064)RJup, which implies a mean density of 1.07 g cm-3. This density is significantly greater than predicted for models that include the effects of stellar insolation and in which the planet has only a small core of solid material. Thus, we confirm that this planet likely contains a large core and that the ratio of core mass to total planet mass is more akin to that of Uranus and Neptune than to either Jupiter or Saturn.

We observed the young open cluster NGC 2301 for 14 nights in 2004 February using the orthogonal transfer CCD camera OPTIC. We used point-spread function shaping techniques ("square stars") during the observations, allowing us to obtain a larger dynamic range (4.5 mag) of high photometric precision results (<= 2 mmag). These results are better than similar observing campaigns using standard CCD imagers. This paper discusses our observational techniques and presents initial results for the variability statistics found in NGC 2301. Details of the variability statistics as functions of color, variability type, stellar type, and cluster location will appear in Paper II.

We obtained R‐band time‐series observations of the young, metal‐rich open cluster NGC 2301 for 12 nights in 2004 February. B‐band images were also obtained, and color‐magnitude diagrams with limits of R = 19.5 and B = 21.5 were produced. Only a small effort was made to determine cluster membership, as our magnitude limits are far deeper than previously published values. Our photometric precision for the brightest 5 mag of sources is 1–2 mmag. We determine that for the ∼4000 stars that have time‐series data, 56% are variable, and of these, approximately 13% are observed to exhibit periodic light curves ranging from tens of minutes to days. We present some examples of the light curves obtained, and produce cuts in variability space based on parameters such as color and amplitude. The percentage of variability is approximately equal across all colors, with the majority of variables having amplitudes of 0.15 mag or less. In general, redder stars show larger variability amplitudes. We find a smooth decline in the number of periodic variables toward longer period. This decline is probably due to a transition from intrinsic to extrinsic variability, and also due in part to our limited observing period of 12 nights. Essentially all the A and F main‐sequence stars in our sample are variable (∼2 mmag and larger), and most present complex light curves containing multiple periods that are suggestive of their inclusion in the δ Scuti and γ Doradus classes. A variable non–cluster member giant and two variable white dwarf candidates are discussed. Our equational description of variability is shown to be an excellent predictive tool for determining the cumulative fraction of variables that will be observed in a photometric survey. Our entire data set is available electronically.

Astronomische NachrichtenVolume 325, Issue 6-8 p. 651-651 Original Paper The optical detection of gamma ray bursts with the 1.3 m robotically controlled telescope on Kitt Peak C. H. McGruder III, C. H. McGruder III [email protected] Search for more papers by this authorJ. R. Mattox, J. R. Mattox Fayetteville State University, 1200 Murchison Road, Fayetteville NC 28301, USASearch for more papers by this authorM. T. Carini, M. T. Carini Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorD. R. Davis, D. R. Davis Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson AZ 85719-2395, USASearch for more papers by this authorM. E. Everett, M. E. Everett Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson AZ 85719-2395, USASearch for more papers by this authorR. Gelderman, R. Gelderman Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorE. F. Guinan, E. F. Guinan Department of Astronomy and Astrophysics, Villanova University, 800 Lancaster Avenue, Villanova PA 19085, USASearch for more papers by this authorS. B. Howell, S. B. Howell WIYN Observatory & NOAO, 950 N. Cherry Avenue, Tucson AZ 85719, USASearch for more papers by this authorS. Marchenko, S. Marchenko Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorD. K. Walter, D. K. Walter Department of Physical Sciences, South Carolina State University, 300 College Street, Orangeburg SC 29115, USASearch for more papers by this author C. H. McGruder III, C. H. McGruder III [email protected] Search for more papers by this authorJ. R. Mattox, J. R. Mattox Fayetteville State University, 1200 Murchison Road, Fayetteville NC 28301, USASearch for more papers by this authorM. T. Carini, M. T. Carini Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorD. R. Davis, D. R. Davis Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson AZ 85719-2395, USASearch for more papers by this authorM. E. Everett, M. E. Everett Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson AZ 85719-2395, USASearch for more papers by this authorR. Gelderman, R. Gelderman Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorE. F. Guinan, E. F. Guinan Department of Astronomy and Astrophysics, Villanova University, 800 Lancaster Avenue, Villanova PA 19085, USASearch for more papers by this authorS. B. Howell, S. B. Howell WIYN Observatory & NOAO, 950 N. Cherry Avenue, Tucson AZ 85719, USASearch for more papers by this authorS. Marchenko, S. Marchenko Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorD. K. Walter, D. K. Walter Department of Physical Sciences, South Carolina State University, 300 College Street, Orangeburg SC 29115, USASearch for more papers by this author First published: 13 October 2004 https://doi.org/10.1002/asna.200410309Citations: 1AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onEmailFacebookTwitterLinkedInRedditWechat No abstract is available for this article. References Akerlof, C., Balsano, R., Bathelmy, S., Bloch, J., Butterworth, P., et al.: 1999, Nature 398, 400 10.1038/18837 CASGoogle Scholar Katz, J.L.: 1994, ApJ 432, L107 10.1086/187523 Web of Science®Google Scholar Meszaros, P., Rees, M.J.: 1997, ApJ 476, 232 10.1086/303625 Web of Science®Google Scholar Rosswog, S.: 2004, Sci 303, 46 10.1126/science.1091767 CASPubMedWeb of Science®Google Scholar Sari, R., Piran, T.: 1999, ApJ 517, L109 10.1086/312039 Web of Science®Google Scholar Citing Literature Volume325, Issue6-8October 2004Pages 651-651 ReferencesRelatedInformation

The 1.3-m telescope at Kitt Peak National Observatory was originally commissioned in 1964 as the “Remotely Controlled Telescope”, a pioneering project in unattended, remote observing. Forty years of technological advances later, the 1.3-m has been refurbished, automated and reborn as the “Robotically Controlled Telescope”. The RCT is used to pursue a variety of research programs which incorporate techniques to achieve extremely high precision photometric monitoring of stars and AGN, as well as to search for transits of extrasolar planets. Since spring of 2003 the RCT has been controlled through pre-scheduled scripts, without interactive human control, to collect imaging data. The work on automation of the observatory system is continuing, with the ultimate goal being that the computer will control the telescope through semiintelligent software to make observations as efficiently as a well-trained human astronomer. (© 2004 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)

Astronomische NachrichtenVolume 325, Issue 6-8 p. 662-662 Original Paper Automated image reduction at the RCT M. E. Everett, M. E. Everett [email protected] Search for more papers by this authorD. R. Davis, D. R. Davis Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson, AZ 85719, USASearch for more papers by this authorS. B. Howell, S. B. Howell Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson, AZ 85719, USA WIYN Observatory & NOAO, 950 N. Cherry Ave., Tucson, AZ 85719, USASearch for more papers by this authorD. K. Walter, D. K. Walter Dept. of Physical Sciences, South Carolina State University, 300 College St., Orangeburg, SC 29115, USASearch for more papers by this authorC. H. McGruder III, C. H. McGruder III Dept. of Physics and Astronomy, Western Kentucky University, Bowling Green, KY 42101, USASearch for more papers by this authorR. Gelderman, R. Gelderman Dept. of Physics and Astronomy, Western Kentucky University, Bowling Green, KY 42101, USASearch for more papers by this authorE. F. Guinan, E. F. Guinan Dept. of Astronomy and Astrophysics, Villanova University, 800 Lancaster Ave., Villanova, PA 19085, USASearch for more papers by this authorJ. R. Mattox, J. R. Mattox Fayetteville State University, 1200 Murchison Rd., Fayetteville, NC 28301, USASearch for more papers by this author M. E. Everett, M. E. Everett [email protected] Search for more papers by this authorD. R. Davis, D. R. Davis Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson, AZ 85719, USASearch for more papers by this authorS. B. Howell, S. B. Howell Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson, AZ 85719, USA WIYN Observatory & NOAO, 950 N. Cherry Ave., Tucson, AZ 85719, USASearch for more papers by this authorD. K. Walter, D. K. Walter Dept. of Physical Sciences, South Carolina State University, 300 College St., Orangeburg, SC 29115, USASearch for more papers by this authorC. H. McGruder III, C. H. McGruder III Dept. of Physics and Astronomy, Western Kentucky University, Bowling Green, KY 42101, USASearch for more papers by this authorR. Gelderman, R. Gelderman Dept. of Physics and Astronomy, Western Kentucky University, Bowling Green, KY 42101, USASearch for more papers by this authorE. F. Guinan, E. F. Guinan Dept. of Astronomy and Astrophysics, Villanova University, 800 Lancaster Ave., Villanova, PA 19085, USASearch for more papers by this authorJ. R. Mattox, J. R. Mattox Fayetteville State University, 1200 Murchison Rd., Fayetteville, NC 28301, USASearch for more papers by this author First published: 13 October 2004 https://doi.org/10.1002/asna.200410317AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onFacebookTwitterLinkedInRedditWechat No abstract is available for this article. Volume325, Issue6-8October 2004Pages 662-662 RelatedInformation

Astronomische NachrichtenVolume 325, Issue 6-8 p. 648-648 Original Paper Searching for extrasolar planets with the 1.3 m Robotically Controlled Telescope on Kitt Peak C.H. McGruder III, C.H. McGruder III charles.mcgruder@wku.edu Search for more papers by this authorM. E. Everett, M. E. Everett Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson AZ 85719-2395, USASearch for more papers by this authorS. B. Howell, S. B. Howell WIYN Observatory & NOAO, 950 N. Cherry Avenue, Tucson AZ 85719, USASearch for more papers by this authorM. T. Carini, M. T. Carini Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorD. R. Davis, D. R. Davis Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson AZ 85719-2395, USASearch for more papers by this authorR. Gelderman, R. Gelderman Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorE. F. Guinan, E. F. Guinan Department of Astronomy and Astrophysics, Villanova University, 800 Lancaster Avenue, Villanova PA 19085, USASearch for more papers by this authorS. Marchenko, S. Marchenko Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorJ. R. Mattox, J. R. Mattox Fayetteville State University, 1200 Murchison Road, Fayetteville NC 28301, USASearch for more papers by this authorD. K. Walter, D. K. Walter Department of Physical Sciences, South Carolina State University, 300 College Street, Orangeburg SC 29115, USASearch for more papers by this author C.H. McGruder III, C.H. McGruder III charles.mcgruder@wku.edu Search for more papers by this authorM. E. Everett, M. E. Everett Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson AZ 85719-2395, USASearch for more papers by this authorS. B. Howell, S. B. Howell WIYN Observatory & NOAO, 950 N. Cherry Avenue, Tucson AZ 85719, USASearch for more papers by this authorM. T. Carini, M. T. Carini Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorD. R. Davis, D. R. Davis Planetary Science Institute, 1700 Ft. Lowell Suite 106, Tucson AZ 85719-2395, USASearch for more papers by this authorR. Gelderman, R. Gelderman Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorE. F. Guinan, E. F. Guinan Department of Astronomy and Astrophysics, Villanova University, 800 Lancaster Avenue, Villanova PA 19085, USASearch for more papers by this authorS. Marchenko, S. Marchenko Department of Physics and Astronomy,Western Kentucky University , Bowling Green KY 42101, USASearch for more papers by this authorJ. R. Mattox, J. R. Mattox Fayetteville State University, 1200 Murchison Road, Fayetteville NC 28301, USASearch for more papers by this authorD. K. Walter, D. K. Walter Department of Physical Sciences, South Carolina State University, 300 College Street, Orangeburg SC 29115, USASearch for more papers by this author First published: 13 October 2004 https://doi.org/10.1002/asna.200410308AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onFacebookTwitterLinkedInRedditWechat No abstract is available for this article. Volume325, Issue6-8October 2004Pages 648-648 RelatedInformation

The Faint Sky Variability Survey is aimed at finding photometric and/or astrometric variable objects in the brightness range between ∼16th and ∼24th mag on time-scales between tens of minutes and years with photometric precisions ranging from 3 millimag for the brightest to 0.2 mag for the faintest objects. An area of ∼23 deg2, located at mid and high Galactic latitudes, has been covered using the Wide Field Camera on the 2.5-m Isaac Newton Telescope on La Palma. Here we describe the main goals of the Faint Sky Variability Survey and the data reduction process.

We present extensive optical and infrared photometry of the afterglow of gamma-ray burst (GRB) 030329 and its associated supernova (SN) 2003dh over the first two months after detection (2003 March 30-May 29 UT). Optical spectroscopy from a variety of telescopes is shown and, when combined with the photometry, allows an unambiguous separation between the afterglow and SN contributions. The optical afterglow of the GRB is initially a power-law continuum but shows significant color variations during the first week that are unrelated to the presence of an SN. The early afterglow light curve also shows deviations from the typical power-law decay. An SN spectrum is first detectable ~7 days after the burst and dominates the light after ~11 days. The spectral evolution and the light curve are shown to closely resemble those of SN 1998bw, a peculiar Type Ic SN associated with GRB 980425, and the time of the SN explosion is close to the observed time of the GRB. It is now clear that at least some GRBs arise from core-collapse SNe.

Employing the transit method and the technique of ensemble differential photometry with the newly refurbished 1.3 m telescope on Kitt Peak we will search dense stellar fields to detect extrasolar planets. For a single exposure of a few minutes we will achieve a photometric precision, sigma similar to 500 mumag (0.0005(m)) for the brighter stars (V, R similar to 12(m)) and sigma similar to 10 millimag (0.01(m)) for the fainter stars (V, R similar to 19(m)). This level of precision will allow us to detect jupiter-sized planets for all stars imaged, but also neptune-sized planets transiting the brighter stars. Our approach enables the detection of extrasolar planets around faint, distant stars (d <similar to kpc). Thus, we will be able to provide statistics on the distribution of jupiter-sized planets outside the solar neighborhood over a wide range of metallicity and age, which is currently unaccessible to spectroscopic radial velocity studies and also to wide-field imaging telescopes.

Orthogonal transfer CCDs (OTCCDs) were developed to compensate for real-time image motion, essentially providing tip/tilt corrections without additional optics or moving parts. Because of the complex gate structures of OTCCDs, their ability to provide high-precision photometric observations and their use as highspeed photometers were unclear. We detail new observations obtained with the OPTIC camera at the University of Hawaii's 2.2 m telescope on Mauna Kea that explore both of these areas. We find that OTCCDs provide equally good results in terms of typical time-series differential photometry (compared with typical CCDs) and that their high-speed photometric application is superb. Using point-spread function-shaping techniques, we obtained time-series photometric observations with precisions of less than or similar to660 mumag per 180 s integration. Extending this technique to very bright stars, the potential to reach differential precisions near 10(-5) per exposure is investigated.

We present results from a 5 night wide-field time-series photometric survey that detects variable field stars. We find that the fraction of stars whose light curves show variations depends on color and magnitude, reaching 17% for the brightest stars in this survey (Vsimilar to14) for which the photometric precision is best. The fraction of stars found to be variable is relatively high at colors bluer than the Sun and relatively low at colors similar to the Sun and increases again for stars redder than the Sun. We present light curves for a sample of the pulsating and eclipsing variables. Most of the stars identified as pulsating variables have low amplitudes (DeltaV = 0.01-0.05), relatively blue colors, and multiple periods. There are 13 stars we identify as either SX Phoenicis or delta Scuti stars. These classes represent a significant contribution to the total number of blue variables found in this survey. Another 17 stars are identified as eclipsing variables, which have a wide range in color, magnitude, and amplitude. Two variable giants are observed, and both show night-to-night similar to1% variations. We present data for 222 variables in total, most of which are not classified. Implications of surveys for stellar variability and interferometry are briefly discussed.

We present techniques for wide-field ultrahigh-precision time-sampled CCD photometry. Representing a survey of field stars, our data consist of UBVRI photometry and a V-band time series of exposures on 5 consecutive nights covering 11,500 stars in a similar to1 deg(2) field. The resulting light curves reach precisions of 0.0020 mag per exposure in the brightest stars (V similar to 14). Light curves binned and averaged over 4.5 hr reach precisions of 0.00019 mag for the brightest stars. We present example light curves and discuss one application for surveys of this type: the search for transits by extrasolar planets.

We present here initial results from the Faint Sky Variability Survey: (i) summary and database location of the survey; (ii) follow-up spectroscopic observations; (iii) initial matching to already known objects in the survey from SIMBAD; (iv) the search for cataclysmic variables; and (v) a look at the very red objects found.

A network of longitudinally spaced imaging telescopes is described. Due to the limitations of the radial velocity method extrasolar planets have only been found around bright stars (less than 10 mag). Employment of the network and the photometric method to detect extrasolar planets will lead to the discovery of extrasolar planets at much fainter magnitudes (less than 19 mag).

A network of three longitudinally-spaced robotic imaging telescopes is described. So far planets have been found only around bright stars (m < 1Om). Employment of the network and the photometric method for the detection of extrasolar planets will lead to the discovery of planets around stars of much fainter magnitudes (m < 19m).

Searching for planets orbiting other suns has become an area of intense interest in recent years. Most search programs use high precision radial velocity methods and use long term, detailed monitoring of a few bright F,G stars. Photometric methods have been briefly considered over the last few years, but are generally thought to be unable to reach the needed precision levels. We present here an initial report on the development of a low-cost, photometric search program telescope. Our inexpensive system is capable of producing ultra-high photometric measurements, currently yielding standard deviations as low as +/-0.004 magnitudes or 0.4% photometric precision. However, a number of limiting factors resulting from both the equipment and from our current lack of complete understanding of ultra-high precision photometry have been identified. We show that with a system such as described herein, detections of planetary transits by Jupiter-sized bodies in orbit around F-M dwarfs could be accomplished.