Hierarchical Fringe Tracking (HFT) is a fringe tracking concept optimizing the sensitivity in optical long baseline by reducing to an absolute minimum the number of measurements used to correct the OPD fluctuations. By nature, the performances of an HFT do not decreases with the number of apertures of the interferometer and are set only by the flux delivered by the individual telescopes. This a critical feature for future interferometers with large number of apertures both for homodyne and heterodyne operation. Here we report the design and first optical bench tests of integrated optics HFT chips for a 4 telescopes interferometer such as the VLTI. These tests validate the HFT concept and confirm previous estimates that we could track accurately fringes on the VLTI up to nearly K~15.9 with the UTs and K~12.2 with the ATs with a J+H+K fringe tracker with one HFT chip per band. This is typically 2.5 magnitudes fainter than the best potential performance of the current ABCD fringe tracker in the K band. An active longitudinal and transverse chromatic dispersion correction allows the optimization of broad band fiber injections and instrumental contrast. We also present a preliminary evaluation of the potential of such a gain of sensitivity for the observations of AGNs with the VLTI.
S. Agayeva, V. Aivazyan, S. Alishov, M. Almualla, C. Andrade, Sarah Antier, J. M. Bai, A. Baransky, S. Basa, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, U. Bhardwaj, M. Blazek, O. Burkhonov, E. Burns, S. Caudill, N. Christensen, F. Colas, A. Coleiro, W. Corradi, M. Coughlin, T. Culino, D. Darson, D. Datashvili, G. de Wasseige, T. Dietrich, F. Dolon, D. Dornic, J. Dubouil, J.-G. Ducoin, P.-A. Duverne, A. Esamdin, A. Fouad, F. Guo, V. Godunova, P. Gokuldass, N. Guessoum, E. Gurbanov, R. Hainich, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, E.E.O. Ishida, N. Ismailov, T. Jegou du Laz, D.A. Kann, G. Kapanadze, S. Karpov, R.W. Kiendrebeogo, A. Klotz, N. Kochiashvili, A. Kaeouach, J.-P. Kneib, W. Kou, K. Kruiswijk, S. Lombardo, M. Lamoureux, N. Leroy, A. Le Van Su, J. Mao, M. Masek, T. Midavaine, A. Moeller, D. Morris, R. Natsvlishvili, F. Navarete, S. Nissanke, K. Noonan, K. Noysena, N.B. Orange, J. Peloton, M. Pilloix, T. Pradier, M. Prouza, G. Raaijmakers, Y. Rajabov, J.-P. Rivet, Y. Romanyuk, L. Rousselot, F. Ruenger, V. Rupchandani, T. Sadibekova, N. Sasaki, A. Simon, K. Smith, O. Sokoliuk, X. Song, A. Takey, Y. Tillayev, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, M. Vardosanidze, X.F. Wang, D. Vernet, Z. Vidadi, J. Zhu, Y. Zhu
GRANDMA is a world-wide collaboration with the primary scientific goal of studying gravitational-wave sources, discovering their electromagnetic counterparts and characterizing their emission. GRANDMA involves astronomers, astrophysicists, gravitational-wave physicists, and theorists. GRANDMA is now a truly global network of telescopes, with (so far) 30 telescopes in both hemispheres. It incorporates a citizen science programme (Kilonova-Catcher) which constitutes an opportunity to spread the interest in time-domain astronomy. The telescope network is an heterogeneous set of already-existing observing facilities that operate coordinated as a single observatory. Within the network there are wide-field imagers that can observe large areas of the sky to search for optical counterparts, narrow-field instruments that do targeted searches within a predefined list of host-galaxy candidates, and larger telescopes that are devoted to characterization and follow-up of the identified counterparts. Here we present an overview of GRANDMA after the third observing run of the LIGO/VIRGO gravitational-wave observatories in 2019 − 2020 and its ongoing preparation for the forthcoming fourth observational campaign (O4). Additionally, we review the potential of GRANDMA for the discovery and follow-up of other types of astronomical transients.
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.
Fireball camera networks are being pursued all over the world and continuously monitor the night sky for fire- balls produced as larger meteoroids enter the Earth’s atmosphere at high speeds. As well, in Morocco we have a new detection network calling MOFID network (Moroccan Observatory For Fireball Detection), which is a cooperation with the team of DFN network (Desert Fireball Network) in Australia. The first dual detection with the MOFID network was captured on December 25 at 19:32 local time (18:32 UTC) (lasted about 3.4 seconds).
We present here SPECULOOS, a new exoplanet transit search based on a network of 1m-class robotic telescopes targeting the ~1200 ultracool (spectral type M7 and later) dwarfs bright enough in the infrared (K-mag ≤ 12.5) to possibly enable the atmospheric characterization of temperate terrestrial planets with next-generation facilities like the James Webb Space Telescope. The ultimate goals of the project are to reveal the frequency of temperate terrestrial planets around the lowest-mass stars and brown dwarfs, to probe the diversity of their bulk compositions, atmospheres and surface conditions, and to assess their potential habitability.
The full scientific potential of the VLTI with its second generation instruments MATISSE and GRAVITY require fringe tracking up to magnitudes K>14 with the UTs and K>10 with the ATs. The GRAVITY fringe tracker (FT) will be limited to K~10.5 with UTs and K~7.5 with ATs, for fundamental conceptual reasons: the flux of each telescope is distributed among 3 cophasing pairs and then among 5 spectral channels for coherencing. To overcome this limit we propose a new FT concept, called Hierarchical Fringe Tracker (HFT) that cophase pairs of apertures with all the flux from two apertures and only one spectral channel. When the pair is cophased, most of the flux is transmitted as if it was produced by an unique single mode beam and then used to cophase pairs of pairs and then pairs of groups. At the deeper level, the flux is used in an optimized dispersed fringe device for coherencing. On the VLTI such a system allows a gain of about 3 magnitudes over the GRAVITY FT. On interferometers with more apertures such as CHARA (6 telescopes) or a future Planet Formation Imager (12 to 20 telescopes), the HFT would be even more decisive, as its performance does not decrease with the number of apertures. It would allow building a PFI reaching a coherent magnitude H~10 with 16 apertures with diameters smaller than 2 m. We present the HFT concept, the first steps of its feasibility demonstration from computer simulations and the optical design of a 4 telescopes HFT prototype.
Within the framework of the site prospection for the future European Extremely Large Telescope (E-ELT), a wide site characterization was achieved. Aklim site located at an altitude of 2350 m at the geographical coordinates: lat.= 30°07’38” N, long.= 8°18’31” W , in the Moroccan Middle Atlas Mountains, was one of the candidate sites chosen by the Framework Programme VI (FP6) of the European Union. To complete the fulfilled study ([19]; [21]), we have used the ModelOTP (model of optical turbulence profiles) established by [15] and improved by [6]. This model allows getting the built-in profiles of the optical turbulence under various conditions. In this paper, we present an overview of the Aklim database results, in the boundary layers and in the free atmosphere separately and we make a comparison with Cerro Pachon result [15].
The limiting magnitude is a key issue for optical interferometry. Pairwise fringe trackers based on the integrated optics concepts used for example in GRAVITY seem limited to about K=10.5 with the 8m Unit Telescopes of the VLTI, and there is a general “common sense” statement that the efficiency of fringe tracking, and hence the sensitivity of optical interferometry, must decrease as the number of apertures increases, at least in the near infrared where we are still limited by detector readout noise. Here we present a Hierarchical Fringe Tracking (HFT) concept with sensitivity at least equal to this of a two apertures fringe trackers. HFT is based of the combination of the apertures in pairs, then in pairs of pairs then in pairs of groups… The key HFT module is a device that behaves like a spatial filter for two telescopes (2TSF) and transmits all or most of the flux of a cophased pair in a single mode beam. We give an example of such an achromatic 2TSF, based on very broadband dispersed fringes analyzed by grids, and show that it allows piston measures from very broadband fringes with only 3 to 5 pixels per fringe tracker. We show the results of numerical simulation indicating that our device is a good achromatic spatial filter and allowing a first evaluation of its coupling efficiency, which is similar to this of a single mode fiber on a single aperture. Our very preliminary results indicate that HFT has a good chance to be a serious candidate for the most sensitive fringe tracking with the VLTI and also interferometers with much larger number of apertures. On the VLTI the first rough estimate of the magnitude gain with regard to the GRAVITY internal FT is between 2.5 and 3.5 magnitudes in K, with a decisive impact on the VLTI science program for AGNs, Young stars and planet forming disks.
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.
In site selection processes, one key parameter is the extinction coefficient. This parameter depends on aerosol load, water
vapor content and atmospheric gazes. Actually a lot of satellite instruments give the aerosol optical thickness over the
earth with good spatial and temporal resolutions.
The determination of the extinction coefficient at elevated altitudes from photometric surface measurements at lower
altitudes is very important in the field of site testing.
In the first part of this paper we make a comparison between the extinction coefficient measured at ground level and the
aerosol optical thickness measured from space at La Palma observatory in order to study the reliability of the aerosol
satellite instruments. We used the most popular ones: MODIS Terra and Aqua, MISR and Envisat Meris.
In the second part of the paper, we use three AERONET (Aerosol Robotic Network) stations close to one another at the
Canary Islands; Izana (longitude=16.5°W, latitude=28.3° N, altitude= 2367m), La laguna (longitude=16.32°W,
latitude=28.50°N, altitude=568 m) and Santa-Cruz Tenerife (longitude=16.25°W, latitude=28.5°N, altitude=52 m). The
aerosol optical thicknesses relative to these stations were studied in order to develop some empirical relationships that
help determine photometric quality of an astronomical observatory from satellite measurements (even with very low
resolution) or from in-situ measurements of very low elevated nearby places. LIDAR (Ligth Detection and Ranging) data
of Santa-Cruz Tenerife provided by the MPLNET (Micro-Pulse Lidar Network) network were also used.
We present a characterization of meteorological parameters: Wind and direction speed, temperature, relative
humidity and pressure. Data set is provided by the system of NCEP/NCAR Re-analysis. The statistical
treatment of data will cover the years between 2003 and 2006 for the Observatory Oukaïmeden. An analysis of
monthly, seasonal, and annual results is presented. We calculated the Richardson number for each month of the
year. In addition, this paper describes a comparison between balloon-sounding made at different stations and
coincident model-based meteorological analysis. The comparison allows the assessment reliability of the analysis
in studied period.
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 the framework of the E-ELT project a prospecting campaign was launched by the ESO to select the site that
will host the next generation of optical telescopes of 42 m diameter. Moroccan Anti-Atlas (Jbel Aklim) was
selected as well as other sites (ORM, Ventarrones and Macon) to be a possible potential location that will house
the E-ELT. In this paper we first present the reasons for the choice of Jbel Aklim as a E-ELT candidate through
various exploration campaigns that we have achieved. The second part concerns description of instruments used.
Finally we will present the preliminary results of the meteorological and MASS-DIMM measurements.
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.
Candidate sites of the future European Extremely Large Telescopes (E-ELT) need to be assessed and analytically
compared in their observing characteristics. In the site selection process, meteorological, photometric and seeing
qualities have to be studied and measured carefully.
Aklim site in Morocco is one among four candidates in the ELT project. In this paper, we present meteorological studies
of the Aklim site over eleven years. The meteorological parameters include wind speed and direction, relative humidity,
air temperature, cloud cover and water vapour content. Most of these data are taken from the National Center for
Environmental Prediction/National Center for Atmospheric Research NCEP/NCAR Reanalysis. The meteorological
analysis covers the vertical profile as well as surface layer meteorology.
Furthermore, in extensive literature, it has been demonstrated that the global circulation of atmospheric wind at 200 mb
can be used as a criterion to establish the suitability for the development of adaptive optics techniques. By using the
NOAA NCEP/NCAR reanalysis database, we analyse the monthly average wind velocity at 200 mb for eleven years
period and compare with famous observatories.
The instrumental noise is an important factor in any measurement.
In order to evaluate the amount of seeing introduced by the
instrumental noise, we have conducted an experiment using an
artificial light source as a star. In addition, we present a study
of the defocus effect on the DIMM results. The instrumental noise
variance was measured in the laboratory for different states of
defocusing. In this paper we will present the results of these
various experiments.
The aim of this paper is to characterize the aerosol loadings, their optical and microphysical properties over Morocco, by
use of the AERONET network and satellite data. Three AERONET stations in Morocco; Saada, Ras_El_Ain and Dakhla
are considered in this work. The aerosol parameters studied are the aerosol optical thickness, the Angstrom parameter,
the size distribution, the single scattering albedo and the refraction index. An inter-comparison with satellite data has
been achieved. The most popular satellite products, TOMS (Earth Probe and OMI), MODIS and MISR have been
considered. It comes out from this study that the mean aerosol optical thickness (550 nm) vary from 0.22 to 0.3, with a
peak in summer time of 0.56 for Dakhla, 0.42 for Ras_El_Ain and 0.35 for Saada. The Angstrom parameter mean is 0.6
for Dakhla and 0.75 for Saada and Ras_El_Ain with a summer minimum of 0.32 for Dakhla and 0.55 for Saada and
Ras_El_Ain. The size distribution is bimodal with a predominance of the coarse mode except for Saada in winter and
autumn. This region depicts desert dust predominant environment with a single scattering albedo varying from 0.72 to
0.96. Saada and Ras_El_Ain being at 52 km apart, their coincident daily AOT correlate with a correlation coefficient;
R=0.93. Concerning the correlation between satellite data and AERONET AOT, TOMS EP has a correlation coefficient
of 0.53 for Saada (all data), 0.68 for Dakhla (all data). TOMS OMI correlation coefficient is 0.68 for Saada (all data) and
0.71 for Ras_El_Ain (year 2006). MISR (level 3 data) correlation coefficient is 0.77 for Saada (all data) and 0.85 for
Dakhla (all data). MODIS (level 3) correlation coefficient is 0.86 for Saada (all data) and 0.92 for Dakhla (all data).
Level 2 MODIS correlation coefficient is 0.69 for Saada (year 2006), 0.86 for Ras_El_Ain (year 2006) and 0.97 for
Dakhla (year 2003).
In order to prospect for good astronomical sites in Morocco, we make a preliminary study in terms of aerosol characterization. For that purpose we use AERONET data and the Aerosol Index provided by Earth Probe platform. After establishing a good correlation between the aerosol optical thickness (AOT) and the aerosol index (AI) in three sites located in the area of interest, we try to extrapolate to areas where AERONET data are not available. The studied areas are: Marrakech, Dakhla located in Morocco, and Izana in the Canary Islands.
These areas exhibit a predominance of desert dust aerosol particles. The altitude seems to be the predominant factor influencing the distribution of the aerosol optical thickness during the year. A full characterization of these sites makes possible a determination of the aerosol optical thickness of neighbouring areas.
We discuss the specific potential of a long baseline optical interferometer at the Antarctica Dome C site for
high limiting magnitude observations. First we compute the potential limiting magnitude for cophasing an
interferometer with N diameter D apertures. Combining this with a computation of the isopistonic angle and of
the density of stars, we evaluate that an interferometer with 1.5 m telescopes performing off axis fringe tracking
will provide a minimum sky coverage of 50% in the direction of the galactic pole, while at Paranal, this could be
achieved only if the individual apertures are 10 times larger. This is due to the fact that most of optical seeing
at Dome C is produced in the first 30 meters above the ground. This makes the Dome C an unique site on earth
to permit optical interferometers to reach high magnitudes and therefore contribute to extra galactic science and
cosmology.
We combined aerosol index measurements of TOMS/Nimbus-7 and Earth Probe observations with CAMC visual extinction over La Palma from 1984 to 1997, to investigate the possibility to calibrate TOMS data in terms of astronomical extinction.
The results show that the correlation of the two sets of data is quite good for extinction values greater than about Av = 0.2 mag./airmass. A detailed analysis reveals that the satellite aerosol index is indeed sensitive to the desert dust, but does not show evidence of the extinction contribution of the volcanic smoke due to the Mt. Pinatubo eruption which affected astronomical observations in 1992-1993.
This calibrated aerosol index is then used to investigate the number and distribution of dusty events over the astronomical site of Oukaimeden, Morocco. We find a remarkable correlation of the extinction over the two sites.
Finally we study the long term variability of the extinction over the region including Oukaimeden and La Palma, and we conclude that there is some correlation with the Northern Atlantic Oscillation.
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).
KEYWORDS: Optical turbulence, Astronomy, Global system for mobile communications, Atmospheric optics, Stereolithography, Coherence (optics), Wavefronts, Spatial coherence, Temperature metrology, Refractive index
Here we analyse 168 optical turbulence profiles made at nine different locations worldwide by means of free flight balloons equipped with instrumentation. Optical turbulence outer scales Lo, as well as coherence outer scales ℓo are
derived for the different locations and taking into account the contribution of the surface layer [0, 50m], the boundary layer [0, 1km] and the free atmosphere [1km, 30km]. Noticeable changes are found between the different locations, mainly due to the boundary layer contribution. The free atmosphere contribution seems almost the same for each site. There is a very good coherence between the outer scale derived by us and that measured using the Generalized Seeing Monitor (GSM) technique.
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