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International audience; Cosmic explosions have emerged as a major field of astrophysics over the last years with our increasing capability to monitor large parts of the sky in different wavelengths and with different messengers (photons, neutrinos, and gravitational waves). In this context, gamma-ray bursts (GRBs) play a very specific role, as they are the most energetic explosions in the Universe. The forthcoming Sino-French SVOM mission will make a major contribution to this scientific domain by improving our understanding of the GRB phenomenon and by allowing their use to understand the infancy of the Universe. In order to fulfill all of its scientific objectives, SVOM will be complemented by a fast robotic 1.3 m telescope, COLIBRI, with multiband photometric capabilities (from visible to infrared). This telescope is being jointly developed by France and Mexico. The telescope and one of its instruments are currently being extensively tested at OHP in France and will be installed in Mexico in spring 2023.

Introducción: El equilibrio neuromuscular consiste en la coordi- nación muscular dinámica entre la relación y la actividad de los músculos masticatorios. La férula oclusal tiene como objetivo principal producir una posición mandibular estable y reproducible. Objetivo: Analizar posibles variaciones en el equilibrio neuromus- cular con base en los registros electromiográficos de los múscu- los maseteros previos y posteriores al uso de férula oclusal en pacientes con malposiciones dentarias. Material y métodos: Se siguió una cohorte de 52 pacientes provenientes de dos clínicas odontológicas durante el periodo de agosto a diciembre de 2018, mediante un muestreo a conveniencia se realizó el examen clínico general, regional y local. Se realizó el análisis cefalométrico de las radiografías laterales de cráneo y la evaluación de la electromio- grafía mediante programas específicos, además de la elaboración y colocación de férulas oclusales fisiológicas. Se realizó un análisis bivariado [χ2 y regresión lineal, rangos de Wilcoxon (STATA)]. Resultados: La media de edad fue 22 años, 75% correspondió al género femenino y al tipo de maloclusión esquelética clase II (48%). El uso de férula provocó una disminución en las diferen- cias RMS de 27 (59%) y un aumento en 19 (41%) pacientes. La significancia asintótica del análisis determinó una diferencia signi- ficativa en la variación de la diferencia de RMS y en el índice de asimetría muscular previa y posterior al uso de férula. Con base en el estadístico de contraste (p < 0.05) no existe evidencia sufi- ciente para este conjunto de datos respecto a que las diferencias de RMS y del índice de asimetría muscular dependen del uso de férula. Conclusiones: Cualquier tratamiento dental es complejo debido a que altera la función del sistema estomatognático y estos cambios influyen en la actividad muscular, mismos que deberían considerarse correctos posterior a ser evaluados mediante patrones fisiológicos de actividad muscular.

Electromyography is a useful tool in orthodontics to evaluate and monitor muscle activity for diagnosis and during treatment Objectives: The aim of this study was to determine changes in electric muscular activity during different phases of orthodontic treatment. Material and methods: We performed a cohort study and measured bilateral electromyographic activity (EMG) for 30 seconds in maximum intercuspation. EMG activity was measured monthly for 15 months during 4 phases in orthodontic treatment: preatreatment (P0), splint wear (P1); leveling and aligning (P2); space closure (P3); and fi nishing stage (P4). EMG was measured using a digital electromyograph developed by our group (hardware and software) to determine μV every 0.002 seconds. The root mean square (RMS) value was estimated as a mean value of EGM. Patients were treated at the Orthodontics Department and the Physiology Laboratory of UNAM during 2014-2016. We performed a descriptive, bivariate analysis and a random effects linear regression model for repeated measurements adjusted by age, gender, malocclusion and extractions. Results: Our pilot study included 10 patients (6 female and 4 male); mean age was 20 years. At baseline, maximum median EMG was recorded (median 239 μV, IQR 143 μV-561 μV), Multivariate analysis showed that EMG measurements decreased at P1 (regression coeffi cient [Coef]. -180.97; 95% CI -330.37, -31.56; p = 0.018), P3 (Coef. -168; 95% CI -332.36; -3.76; p = 0.045) and P4 (Coef. -184.21; 95% CI -326.91, -41.5; p = 0.011). Conclusions: EMG changes decreased randomly during orthodontic phases and not constantly as generally believed.

La electromiografia es una herramienta util en la ortodoncia para evaluar y monitorear la actividad muscular. Objetivo: Determinar los cambios en la actividad electrica muscular durante las diferentes fases del tratamiento ortodontico. Material y metodos: Se realizo un estudio de cohorte y se midio la actividad electromiografica bilateral (EMG) durante 30 segundos en maxima intercuspidacion. Se realizaron 15 mediciones mensuales de la EMG durante cuatro fases en el tratamiento ortodoncico: basal (P0); uso de la ferula (P1); nivelacion y alineacion (P2); cierre de espacios (P3); y la etapa de finalizacion (P4). Se uso un electromiografo (EMG) digital, desarrollado por nuestro grupo (hardware y software) para determinar μV cada 0.002 segundos y el valor medio cuadratico (RMS) fue estimado como un valor medio de EGM. Los pacientes fueron tratados en el Departamento de Ortodoncia y el Laboratorio de Fisiologia en la UNAM durante 2014-2016. Se realizo un analisis descriptivo, un modelo de regresion lineal de efectos aleatorios para medidas repetidas ajustadas univariado y otro multivariado ajustado por variables confusoras. Resultados: Se incluyo a 10 pacientes, con edad promedio de 20.6 anos. La medicion basal de EMG fue de 239 μV (RIC 143-561). El modelo multivariado mostro una disminucion de la EMG en P1 (coeficiente de regresion [Coef.] -180.97; IC 95% -330.37, -31.56; p = 0.018), P3 (Coef. -168; IC 95% -332.36; -3.76; p = 0.045) y P4 (Coef. -184.21; IC 95% -326.91, -41.5; p = 0.011), en comparacion con la basal. Conclusiones: Los cambios EMG disminuyeron durante las fases ortodoncicas aleatoriamente durante las etapas de tratamiento no de manera constante como generalmente se asume.

We derive limits on any electromagnetic counterpart to the compact binary merger S190814bv, whose parameters are consistent with the merger of a black hole and a neutron star. We present observations with the new wide-field optical imager DDOTI and also consider Swift/BAT observations reported by Palmer et al. (2019). We show that Swift/BAT would have detected a counterpart with similar properties to a typical on-axis short GRB at the 98 per cent confidence level, whereas our DDOTI observations only rule out such a counterpart at the 27 per cent confidence level. Neither have sufficient sensitivity to rule out an off-axis counterpart like GW 170817. We compare the efficiency of Swift/BAT and DDOTI for future observations, and show that DDOTI is likely to be about twice as efficient as Swift/BAT for off-axis events up to about 100 Mpc., Accepted by MNRAS. 6 pages. Fixed typos and references

Objective Evaluate the electromyographic changes in the Masseter (MM) and Temporalis (TM) muscles during voluntary clenching of the teeth both before and after orthognathic surgery in patients aged 18 years and older and diagnosed with mandibular prognathism. Methods Eleven patients with prognathism were included in the study, in all of whom the initial phase of orthodontic treatment had been completed. The orthognathic procedure to reduce prognathism comprised intraoral oblique sliding (or subsigmoid) osteotomy, after which intermaxillary fixation with ligaments in the maxilla and mandible was undertaken in all patients for 6 weeks post-surgery. Electromyographic activity was recorded during the baseline maximum voluntary contraction of the teeth, with the same measurement taken 3 and then 6 months after orthognathic surgery. Results Significant differences were found in the mean amplitude (17.0 vs 14.7, P = 0.020) and peak-to-peak amplitude (left [761.6 vs 457.0, P = 0.003] and right [676.9 vs 357.4, P = 0.007]) for the MM between the baseline score and 6 months after surgery. Likewise, significant differences were found in the mean amplitude (18.2 vs 25.6, P = 0.009) and peak-to-peak amplitude (left [856.4 vs 1594.2, P = 0.004] and right [804.4 vs 1813.4, P = 0.004]) for the TM between the baseline score and that taken 6 months post-surgery. Only 18.2% (2/11) presented orthodontic appliances problem in the 3 months post-surgery. Conclusion Electromyographic activity was restored 6 months after the orthognathic surgery. From a clinical perspective, the results obtained confirm that orthognathic surgery has not only an esthetic but also a functional objective in terms of achieving equilibrium and occlusal harmony.

We present optical photometry of the afterglow of the long GRB 180205A with the COATLI telescope from 217 seconds to about 5 days after the {\itshape Swift}/BAT trigger. We analyse this photometry in the conjunction with the X-ray light curve from {\itshape Swift}/XRT. The late-time light curves and spectra are consistent with the standard forward-shock scenario. However, the early-time optical and X-ray light curves show non-typical behavior; the optical light curve exhibits a flat plateau while the X-ray light curve shows a flare. We explore several scenarios and conclude that the most likely explanation for the early behavior is late activity of the central engine.

Existen diferentes medidas cefalométricas para evaluar las dimensiones de las vías aéreas superiores a partir del uso de la radiografía lateral de cráneo. Se desconoce qué características o factores de las vías aéreas son identificables y posibles de estudiar a partir de las mediciones disponibles y cuáles son las mediciones más útiles para dicho fin. Objetivo: Identificar los factores de las mediciones de las vías aéreas superiores y determinar su asociación a las dimensiones craneofaciales. Material y métodos: Estudio transversal. Analizamos las radiografías laterales y realizamos un análisis factorial principal para las mediciones de las vías respiratorias superiores: N-S-Ba, Ba-S-PNS, AD1, AD2, PTV a adenoides (DPTV) y Airway% (A%). Resultados: Analizamos 151 registros, sin tratamiento de ortodoncia previo ni síndrome craneofacial. Identificamos dos factores principales: el factor 1 (F1) incluye AD1, AD2, DPTV y A%, y el factor 2 (F2) incluye N-S-Ba y Ba-S-ENP. Conclusiones: F1 se relacionó con las dimensiones lineales y F2 con las características estructurales.

A fast photometry methodology is described. We use a cooled Ixon Ultra emCCD in photon counter mode to acquire data. A dissipation system is added to stabilize the temperature down to -96 C. The sensibility of this system makes it ideal even for small telescopes.

We present in this article some of the techniques applied at the Instituto de Astronomia of the Universidad Nacional Autonoma de Mexico (IA-UNAM) to the mechanical structural design for astronomical instruments. With this purpose we use two recent projects developed by the Instrumentation Department. The goal of this work is to give guidelines about support structures design for achieving a faster and accurate astronomical instruments design. The main guidelines that lead all the design stages for instrument subsystems are the high-level requirements and the overall specifications. From these, each subsystem needs to get its own requirements, specifications, modes of operation, relative position, tip/tilt angles, and general tolerances. Normally these values are stated in the error budget of the instrument. Nevertheless, the error budget is dynamic, it is changing constantly. Depending on the manufacturing accuracy achieved, the error budget is again distributed. That is why having guidelines for structural design helps to know some of the limits of tolerances in manufacture and assembly. The error budget becomes then a quantified way for the interaction between groups; it is the key for teamwork.

International audience; We present an overview of the development of the end-to-end simulations programs developed for COLIBRI (Catching OpticaL and Infrared BRIght), a 1.3m robotic follow-up telescope of the forthcoming SVOM (Space Variable Object Monitor) mission dedicated to the detection and study of gamma-ray bursts (GRBs). The overview contains a description of the Exposure Time Calculator, Image Simulator and photometric redshift code developed in order to assess the performance of COLIBRI. They are open source Python packages and were developed to be easily adaptable to any optical/ Near-Infrared imaging telescopes. We present the scientific performances of COLIBRI, which allows detecting about 95% of the current GRB dataset. Based on a sample of 500 simulated GRBs, a new Bayesian photometric redshift code predicts a relative photometric redshift accuracy of about 5% from redshift 3 to 7.

COATLI is a new instrument and telescope that will provide 0.3 arcsec FWHM images from 550 to 920 nm over a large fraction of the sky. It consists of a robotic 50-cm telescope with a diffraction-limited imager. The imager has a steering mirror for fast guiding, a blue channel using an EMCCD from 400 to 550 nm to measure image motion, a red channel using a standard CCD from 550 to 920 nm, and an active optics system based on a deformable mirror to compensate static aberrations in the red channel. Since the telescope is small, fast guiding will provide diffraction-limited image quality in the red channel over a large fraction of the sky, even in relatively poor seeing. The COATLI telescope will be installed at the Observatorio Astronomico Nacional in Sierra San Pedro Martir, Baja California, Mexico, in 2016 and will initially operate with a simple interim imager. The definitive COATLI instrument will be installed in 2017. In this work we present the general optomechanical and control electronics design of COATLI.

DDOTI will be a wide-field robotic imager consisting of six 28-cm telescopes with prime focus CCDs mounted on a common equatorial mount. Each telescope will have a field of view of 12 square degrees, will have 2 arcsec pixels, and will reach a 10-sigma limiting magnitude in 60 seconds of r = 18.7 in dark time and r = 18.0 in bright time. The set of six will provide an instantaneous field of view of about 72 square degrees. DDOTI uses commercial components almost entirely. The first DDOTI will be installed at the Observatorio Astron\'omico Nacional in Sierra San Pedro Mart\'ir, Baja California, M\'exico in early 2017. The main science goals of DDOTI are the localization of the optical transients associated with GRBs detected by the GBM instrument on the Fermi satellite and with gravitational-wave transients. DDOTI will also be used for studies of AGN and YSO variability and to determine the occurrence of hot Jupiters. The principal advantage of DDOTI compared to other similar projects is cost: a single DDOTI installation costs only about US$500,000. This makes it possible to contemplate a global network of DDOTI installations. Such geographic diversity would give earlier access and a higher localization rate. We are actively exploring this option., Comment: To appear in the proceedings of SPIE conference 9910 "Observatory Operations: Strategies, Processes, and Systems VI". 12 pages

BACKGROUND Erosive tooth wear is the irreversible loss of dental hard tissue as a result of chemical processes. When the surface of a tooth is attacked by acids, the resulting loss of structural integrity leaves a softened layer on the tooth's surface, which renders it vulnerable to abrasive forces. The authors' objective was to estimate the prevalence of erosive tooth wear and to identify associated factors in a sample of 14- to 19-year-old adolescents in Mexico. METHODS The authors performed a cross-sectional study on a convenience sample (N = 417) of adolescents in a school in Mexico City, Mexico. The authors used a questionnaire and an oral examination performed according to the Lussi index. RESULTS The prevalence of erosive tooth wear was 31.7% (10.8% with exposed dentin). The final logistic regression model included age (P < .01; odds ratio [OR], 1.64; 95% confidence interval [CI], 1.26-2.13), high intake of sweet carbonated drinks (P = .03; OR, 1.81; 95% CI, 1.06-3.07), and xerostomia (P = .04; OR, 2.31; 95% CI, 1.05-5.09). CONCLUSIONS Erosive tooth wear, mainly on the mandibular first molars, was associated with age, high intake of sweet carbonated drinks, and xerostomia. PRACTICAL IMPLICATIONS Knowledge regarding erosive tooth wear in adolescents with relatively few years of exposure to causal factors will increase the focus on effective preventive measures, the identification of people at high risk, and early treatment.

This paper describes the development of a masticatory refleximetry system to be used in clinic during the track of treatment to people with craniomandibular dysfunctions such as bruxism and temporomandibular joint disorders; proposing two alternative methods to evoke the masseter inhibitory reflex (MIR).

Astronomical observatories and telescopes are becoming increasingly large and complex systems, demanding to any potential user the acquirement of great amount of information previous to access them. At present, the most common way to overcome that information is through the implementation of larger graphical user interfaces and computer monitors to increase the display area. Tonantzintla Observatory has a 1-m telescope with a remote observing system. As a step forward in the improvement of the telescope software, we have designed a Virtual Reality (VR) environment that works as an extension of the remote system and allows us to operate the telescope. In this work we explore this alternative technology that is being suggested here as a software platform for the operation of the 1-m telescope.

Over the years astronomical instrumentation projects are becoming increasingly complex making necessary to find efficient ways for project communication management. While all projects share the need to communicate project information, the required information and the methods of distribution vary widely between projects and project staff. A particular problem experienced on many projects regardless of their size, is related to the amount of design, planning information and how that is distributed among the project stakeholders. One way to improve project communications management is to use a workflow that offers a predefined way to share information in a project. Virtual Reality (VR) offers the possibility to get a visual feedback of designed components without the expenses of prototype building, giving an experience that mimics real life situations using a computer. In this contribution we explore VR as a communication technology that helps to manage instrumentation projects by means of a workflow implemented on a software package called Discut designed at Universidad Nacional Autonoma de Mexico (UNAM). The workflow can integrate VR environments generated as CAD models.

The Institute of Astronomy at the Universidad Nacional Autonoma de Mexico have developed and tested a CCD controller based on Texas Instruments Digital Signal Processor (DSP) TMS30C31@50MHz. Images are temporally stored in a 2MB static RAM attached to the DSP and transferred to the host computer running under Linux. Both tasks, acquisition and timing, are programmable so it can be conditioned to control any bidimensional detector. Analog voltage for bias, offsets and gains are fully programmable also. The system has been tested on an infrared Hawaii detector and fast Marconi 80x80 pixels CCD.

In the last two years the National Observatory at Tonantzintla Puebla, Mexico (OAN Tonantzintla), has been undergoing several facilities upgrades in order to bring to the observatory suitable conditions to operate as a modern Observational Astronomy Teaching Laboratory. In this paper, we present the management, requirement definition and project advances. We made a quantitative diagnosis about of the functionality of the Tonantzintla Observatory (mainly based in the 1m f/15 telescope) to take aim to educational objectives. Through this project we are taking the steps to correct, to actualize and to optimize the observatory astronomical instrumentation according to modern techniques of observation. We present the design and the first actions in order to get a better and efficient use of the main astronomical instrumentation, as well as, the telescope itself, for the undergraduate, postgraduate levels Observacional Astronomy students and outreach publics programs for elementary school. The project includes the development of software and hardware components based in as a common framework for the project management. The Observatory is located at 150 km away from the headquarters at the Instituto de Astronomia, Universidad Nacional Autonoma de Mexico (IAUNAM), and one of the goals is use this infrastructure for a Remote Observatory System.

We have designed and installed a new active remote observing system for the 1-m, f/15 telescope at the Tonantzintla Observatory. This remote system is operated in real-time through the Internet, allowing an observer to control the building, the telescope (pointing, guiding and focusing) and the CCD image acquisition at the main and finder telescopes from the Instituto de Astronomia headquarters in Mexico City (150 KM away). The whole system was modeled within the Unified Modeling Language (UML) and the design has proved to be versatile enough for a variety of astronomical instruments. We describe the system architecture and how different subsystems (telescope control, main telescope and finder image acquisition, weather station, videoconference, etc.) that are based on different operative system platforms (Linux, Windows, uIP) have been integrated. We present the first results of an IPv6 over IPv4 tunnel. Recent remote direct imaging and spectroscopic observations have been used to test the astronomical site. We conclude that this remote system is an excellent tool for supporting research and graduated observational astronomy programs.

The Observatorio Astronomico Nacional at San Pedro Martir is situated on the summit of the San Pedro Martir Sierra in the Baja California peninsula of Mexico, at 2800m above sea level. For as long as three decades, a number of groups and individuals have gathered extremely valuable data leading to the site characterization for astronomical observations. Here we present a summary of the most important results obtained so far. The aspects covered are: weather, cloud coverage, local meteorology, atmospheric optical extinction, millimetric opacity, geotechnical studies, seeing, optical turbulence profiles, wind profiles and 3D simulations of atmospheric turbulence. The results place San Pedro Martir among the most favorable sites in the world for astronomical observations. It seems to be particularly well-suited for extremely large telescopes because of the excellent turbulence and local wind conditions, to mention but two characteristics. Long-term monitoring of some parameters still have to be undertaken. The National University of Mexico (UNAM) and other international institutions are putting a considerable effort in that sense.

We describe the configuration and operation modes of the IR camera/spectrograph: TEQUILA based on a 1024 X 1024 HgCdTe FPA. The optical system will allow three possible modes of operation: direct imaging, low and medium resolution spectroscopy and polarimetry. The basic system is being designed to consist of the following: 1) A LN 2 dewar that allocates the FPA together with the preamplifiers and a 24 filter position cylinder. 2) Control and readout electronics based on DSP modules linked to a workstation through fiber optics. 3) An opto-mechanical assembly cooled to -30 degrees that provides an efficient operation of the instrument in its various modes. 4) A control module for the moving parts of the instrument. The opto-mechanical assembly will have the necessary provision to install a scanning Fabry-Perot interferometer and an adaptive optics correction system. The final image acquisition and control of the whole instrument is carried out in a workstation to provide the observer with a friendly environment. The system will operate at the 2.1 m telescope at the Observatorio Astronomico Nacional in San Pedro Martir, B.C. (Mexico), and is intended to be a first-light instrument for the new 7.8m Mexican IR-Optical Telescope.

The system called PUMA is an instrument consisting of a focal reducer coupled to a scanning Fabry-Perot interferometer (SFPI), which is being developed for the Observatorio Astronomicao Nacional at San Pedro Martir, B.C. It will be installed at the 2.0 m Ritchey-Chretien telescope with a focal ratio of F/7.9. It has interference filters, a calibration system, and field diaphragms. The SFPI can be moved out of the optical path in order to acquire direct images. The images produced by this instrument will be focused on an optoelectronic detector, a CCD, or a Mepsicron, depending on the spectral range used.

ResumenLa pérdida de las piezas dentarias provoca cambios importantes en la actividad sensorio-motora de los pacientes que la sufren, cambios que a su vez pueden afectarse al colocar una dentadura completa (DC) y todos en conjunto pueden alterar el proceso de la masticación a tal grado que se afecten condiciones generales de salud como, por ejemplo, una adecuada alimentación, por lo que ha sido importante estudiar la respuesta de los músculos masticatorios ante la colocación de una DC y además comparar entre aquellos pacientes que previamente han usado DC y aquellos que la utilizan por vez primera, considerando que pudiera existir un estado funcional diferente. Para ello se hicieron registros electromiográficos (EMG) en los músculos maseteros de 29 pacientes, antes (1asesión), a los 8 y 30 días (2ay 3asesión respectivamente) de la colocación de la DC. Formando dos grupos: el grupo 1 (G1) (n=15; 12♀, 5♂, edad promedio 67.2 años) aquellos que previamente estaban usando ya una DC y el grupo 2 (G2) (n=12; 8♀, 4♂, edad promedio 66.5 años) los que nunca antes la habían usado. Los resultados indican que existe una diferencia funcional entre los músculos de aquellos pacientes que previamente han usado una DC con respecto a la de los músculos de los pacientes que no han usado antes DC. Se registró menor amplitud EMG en la 1a sesión en el G1 con respecto al G2 y una menor capacidad de generar los ciclos masticatorios, ello podría influir, también a largo plazo, en una disminución de la capacidad masticatoria y en la calidad de vida de los pacientes. Es necesario continuar este tipo de estudios tanto para corroborar los resultados reportados en el presente trabajo como para que, en su caso, se implementen medidas que coadyuven a una mejor adaptación a la DC.AbstractTeeth loss elicits significant changes in the sensory-motor activity of patients thus afflicted. These changes can in turn be affected upon placement of a full denture (FD). Overall changes can alter mastication processes, to the point of affecting the patient´s general state of health, as would be the case when impinging on proper feeding. This shows the importance of studying masticatory muscles response to the placement of a full denture. It is as well opportune to compare patients who have previously worn dentures with new denture wearers, since it must be borne in mind they could present different functional states. To this end, electromyographic records (EMR) were conducted in masseter muscles of 29 patients before (1st session) at 8 and 30 days (2nd and 3rd session) of FD placement. Two groups were tailored: Group 1 (G1) (n=15, 12♀, 5♂, average age 67.2 years) those who had previously worn a full denture, and group 2 (G2), (n=12, 8♀, 4♂, average age 66.5 years) comprising individuals who had never before worn a full denture. Results indicated there was functional difference among muscles of patients having previously worn FD when compared to muscles of patients who had never worn a FD. Lesser EMG amplitude was found in G1 when compared to G2 in the first session as well as lesser ability to generate masticatory cycles. In the long run, this could also bear upon masticatory ability decrease and patients quality of life. It is necessary to continue this type of studies to substantiate recorded results of the present study, as well as to implement measures geared at contributing to improved FD adaptation.

COATLI will provide 0.3 arcsec FWHM images from 550 to 900 nm over a large fraction of the sky. It consists of a robotic 50-cm telescope with a diffraction-limited fast-guiding imager. Since the telescope is small, fast guiding will provide diffraction-limited image quality over a field of at least 1 arcmin and with coverage of a large fraction of the sky, even in relatively poor seeing. The COATLI telescope will be installed at the at the Observatorio Astron\'omico Nacional in Sierra San Pedro M\'artir, M\'exico, during 2016 and the diffraction-limited imager will follow in 2017., Comment: To appear in the proceedings of SPIE conference 9908 "Ground-based and Airborne Instrumentation for Astronomy VI". 9 pages