The OWL@OUKA is the Optical Wide-field patroL (OWL) facility designed and built by Korea Astronomy and Space Science Institute (KASI) and installed in 2015 at Oukaimeden Observatory. For the first time we used the opportunities offered by this instrument for the detection and monitoring the exoplanets by the transit method. In this work, we present, first, the validation of the OWL@OUKA for the transit method by reporting the observations we have done to calibrate the instrument in order to chose the best exposure time for a given star. We report on the results obtained form the first observations, in V filter, of a known transit event of the planet Qatar-1b, a hot Jupiter orbiting a metal-rich K dwarf star (Teff = 5013.0, Vmag = 12.84). We have used the software AstroImagJ to reduce the data and the software EXOFASTv2 to fit the transit and extract the planetary parameters, where we obtained a transit depth 0.0207+0.0044-0.0040 and a planetary radius of 1.09 ± 0.11 RJ , that are in good consistence with the discovery paper. Given the good results obtained, we moved to the second stage of our program, which consists of tracking TESS candidates.
The new Extremely Large Telescope projects need accurate evaluation of the candidate sites. In this work we present the seeing, free seeing and isoplanatic angle comparison between Aklim site located in Moroccan Anti- Atlas at the geographic coordinates 30°7'39" N, 08 18'39" W, and the Observatorio del Roque de Los Muchachos (ORM), located in La Palma, Canary Islands, at 28°45'00 N, 17°53”10 W, the both sites are pre-selected to house the E-ELT. In this work we present the seeing statistics of (Ɛ), the free seeing (Ɛ free) and the isoplanatic angle ϴ0 measurements at each site, statistics of the mentioned parameters are obtained from the whole data recorded from 09 May 2008 to 09 November 2009 using the Multi Aperture Scintillation Sensor (MASS) - Differential Image Motion Monitor (DIMM) system, compare the common data between the tow sites, more representative results and statistics are shown hereafter.
In this paper we present an analysis of the statistical and temporal properties of seeing and isoplanatic angle measurements obtained with combined Differential Image Motion Monitor (DIMM) and Multi-Aperture Scintillation Sensor (MASS) at Jbel Aklim candidate site for the Eauropean Extremely Large Telescope (E-ELT). These data have been collected from February 2008 to Jun 2010. The overall seeing statistics for Jbel Aklim site are presented, broken into total seeing, free atmosphere seeing and isoplanatic angle, and ground-layer seeing (difference between the total and free-atmosphere seeing). We examine the statistical distributions of seeing measurements and investigate annual and nightly behavior. The properties of the seeing measurements are discussed in terms of the geography and meteorological conditions at Jbel Aklim site.
As part of the conceptual and preliminary design processes of the Extremely Large Telescope (ELT), the ELT site-testing team at Morocco has spent the last two years measuring the atmospheric properties at Aklim site as another 4 candidate mountains in North and South hemisphere, Aklim is the per-selected site for the ELT, is located in Moroccan Anti-Atlas at the geographic coordinates 30°7'39" N, 08°18'39" W.
In this paper we present the isoplanatic angle θ0 and the isopistonic angle θp, measurements at Aklim site, statistics of the mentioned parameters are obtained from the whole data recorded from April 2008 to December 2009 using the Multi Aperture Scintillation Sensor (MASS) - Differential Image Motion Monitor (DIMM) system, more representative results and statistics are shown hereafter.
In this paper we describe a new technique of circular aperture apodization. It is produced by interferometry.
The light, which is diffracted by a circular aperture, is split into two beams of different amplitudes where one of
them has undergone an homothety to change its radial dimensions, by using an afocal optical system. The two
beams are then combined coherently to form an apodized point spread function (PSF). This procedure allows
us to reduce the diffraction wings of the PSF with different reduction factors depending on the combination
parameters.
In this paper we report the detection and characterization of HD 189733b, the
peculiarity of this exoplanet is that the flow of the target star is decreased
significantly (~ 3%) during the transit. We determined the radius of the exoplanet
1.27 ± 0.03 RJ, the impact parameter 0.70 ± 0.02, and the inclination of the orbit
85.4 ± 0.1°. The transit of the extrasolar planet HD 189733b is already done using
the larger telescope. In this study, we used during the observation a telescope of
modest size.
We present here a new approach to estimate the astronomical seeing which is a fundamental parameter in high angular resolution, in adaptive optics and site testing. Based on this approach, we developed seeing monitor, called Interferential Seeing Monitor (hereafter ISM). The principle of
the ISM is based on the study of the diffraction-interference pattern produced by a Young's double-slit in a telescope focus.
From the shape of that pattern, we determine the phase difference between the diffracted light rays that meet on the image plane. Then, the phase structure function is calculated which leads to the seeing value.
The ESO OWL site survey plan includes the analysis of the astronomical
quality of the Atlas mountains in Morocco. In this paper we are presenting the first long time measurement of optical turbulence at Oukaimeden site. For this work we built an instrument called ADIMM for an Automated Differencial Image Motion Monitor, and we use it to the measure the optical turbulence at the Oukaimeden Site. We are describing the instrument and reporting the first results obtained after six month of working on this project. The results of night-time seeing measurements carried out during the period from Jun 14 up to October 01 2003 are presented. The median and mean values of the seeing for the entire period of observations are respectively 0.75" and 0.84".
This work was organized in the framework of contract Num.69651/ODG/02/9005/GWI between the European Southern Observatory (ESO) and Astrophysics and Physics of High Energy Laboratory of the Faculty of Sciences, Cadi Ayyad University (LPHEA).
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