The work that is presented is in its early stage. The intention of this document is to present the conceptual proposal of the design of the cell for Nasmyth-f/5 secondary mirror (TSPM-M2-f/5-Nasmyth), its support system and the mirror of this configuration for the “Telescopio San Pedro Mártir” (TSPM) project. In order to obtain more precise input data for the requirements of the telescope in terms of its: weight, center of gravity, interfaces with the telescope spider assembly and manufacturing viability. The goal of providing accurate data for the mechanical studies of the telescope was fulfilled. With this we ensure more realistic results in the opto-mechanics performance analysis of the whole telescope´s. The telescope´s requirements are the input data for the Opto - mechanics performance and survival analyses, both studies done by CIDESI. For this, it is necessary to have for this telescope configuration a conceptual proposal design of TSPMM2- f/5-Nasmyth. We present the TSPM-f/5 Nasmyth support system proposal, which include the M2 cell, mirror and interface. Finite Elements Analyses (FEA) results of the support system and the mirror are presented too. In the conclusion we present some evidence of the pending future work for this study.
We present the optical design, the error budget, the differential distortion budget and the baffle design of the Telescopio San Pedro Mártir f/5 Nasmyth configuration. The TSPM in its Cassegrain configuration will be assembled around a closed design (converted MMT/Magellan telescope) with most of its optical parts already manufactured. To anticipate for future possible upgrades, the project includes the design of an extreme f/5 Nasmyth configuration. Our optical design demonstrates the feasibility of the configuration, closes the interfaces to the telescope, provides a full picture of the expected performance, and identifies the critical points involved in the configuration.
The Telescopio San Pedro Martir project intends to construct a 6.5m telescope to be installed at the Observatorio Astron´omico Nacional in the Sierra San Pedro M´artir in northern Baja California, Mexico. The project is an association of Mexican institutions, lead by the Instituto Nacional de Astrofısica, Optica y Electronica and UNAM’s Instituto de Astronomia, in partnership with the Smithsonian Astrophysical Observatory and the University of Arizona’s Department of Astronomy and Steward Observatory. The project is advancing through the design stage, having completed five design reviews of different subsystems in 2016 and 2017 (enclosure and services: PDR, CDR; optical design: PDR; optics: progress review; telescope: PDR). Once completed, the partners plan to operate the MMT and TSPM as a binational astrophysical observatory.
Gengis Toledo-Ramirez, Vicente Bringas-Rico, Noe Reyes, Jorge Uribe, Aldo Lopez, Carlos Tovar, Xochitl Caballero, Luis Del-Llano, Cesar Martinez, Eduardo Macias, William Lee, Alberto Carramiñana, Michael Richer, Jesús González, Beatriz Sanchez, Diana Lucero, Rogelio Manuel, Jose Segura, Saul Rubio, German Gonzalez, Obed Hernandez, Mary García, Jose Lazaro, Fabian Rosales-Ortega, Joel Herrera, Gerardo Sierra, Hazael Serrano
KEYWORDS: Optical instrument design, Telescope design, Mirrors, Telescopes, Telescopes, Optical instrument design, Mirrors, Astronomy, Control systems, Systems engineering, Manufacturing, Systems modeling, Control systems design
The Telescopio San Pedro Martir (TSPM) is a new ground-based optical telescope project, with a 6.5 meters honeycomb primary mirror, to be built in the Observatorio Astronomico Nacional on the Sierra San Pedro Martir (OAN-SPM) located in Baja California, Mexico. The OAN-SPM has an altitude of 2830 meters above sea level; it is among the best location for astronomical observation in the world. It is located 1830 m higher than the atmospheric inversion layer with 70% of photometric nights, 80% of spectroscopic nights and a sky brightness up to 22 mag/arcsec2.
The TSPM will be suitable for general science projects intended to improve the knowledge of the universe established on the Official Mexican Program for Science, Technology and Innovation 2014-2018. The telescope efforts are headed by two Mexican institutions in name of the Mexican astronomical community: the Universidad Nacional Autonoma de Mexico and the Instituto Nacional de Astrofisica, Optica y Electronica. The telescope has been financially supported mainly by the Consejo Nacional de Ciencia y Tecnologia (CONACYT). It is under development by Mexican scientists and engineers from the Center for Engineering and Industrial Development. This development is supported by a Mexican-American scientific cooperation, through a partnership with the University of Arizona (UA), and the Smithsonian Astrophysical Observatory (SAO). M3 Engineering and Technology Corporation in charge of enclosure and building design.
The TSPM will be designed to allow flexibility and possible upgrades in order to maximize resources. Its optical and mechanical designs are based upon those of the Magellan and MMT telescopes. The TSPM primary mirror and its cell will be provided by the INAOE and UA. The telescope will be optimized from the near ultraviolet to the near infrared wavelength range (0.35-2.5 m), but will allow observations up to 26μm. The TSPM will initially offer a f/5 Cassegrain focal station. Later, four folded Cassegrain and two Nasmyth focal stations are contemplated, nominally with focal ratios of f/5 and f/11. The concept will allow the use of existing instruments like MMIRS and MEGACAM. Available experience from currently working ground-based telescopes will be integrated with up-to-date technology specially for control and information management systems.
Its mount is the well-known azimuth-elevation configuration. The telescope total mass is estimated in about 245 metric tons, with a total azimuth load of 185 metric tons including around 110 metric tons as the total elevation load. A tracking error lower than 0.03 arcsec RMS is expected under steady wind up to 50 Km/h. An open-loop pointing accuracy between 10 and 2 arcsec is planned. The TSPM is in its design phase. It is the first large optical ground-based telescope to be designed and developed primarily by Mexican scientists and engineers. This endeavor will result in the improvement of the scientific and technical capabilities of Mexico including complex scientific instruments development, systems engineering and project management for large engineering projects. In this paper, which aims to gather the attention of the community for further discussions, we present the engineering preliminary design, the basic architecture and challenging technical endeavors of the TSPM project.
The Telescopio San Pedro Mártir project intends to construct a 6.5m telescope to be installed at the Observatorio Astronómico Nacional in the Sierra San Pedro Mártir in northern Baja California, Mexico. The project is an association of Mexican institutions, lead by the Instituto Nacional de Astrofísica, Óptica y Electrónica and the Instituto de Astronomía at the Universidad Nacional Autónoma de México, in partnership with the Smithsonian Astrophysical Observatory and the University of Arizona’s Department of Astronomy and Steward Observatory. The project is currently in the planning and design stage. Once completed, the partners plan to operate the MMT and TSPM as a binational astrophysical observatory.
This paper is focused on an engineering project applied to astronomy for scientific purposes. The project consisted
elementally on the design, fabrication and characterization of an interface or mechanism to align and focus the lens of the
Echelle spectrograph and its CCD camera. This instrument is part of the 2.1 m telescope of the Observatorio
Astronómico Nacional located at the Sierra de San Pedro Martir, B. C., Mexico (OAN-SPM).
The mechanism described in this article is composed functionally of the next pieces: two half- clamps, three profiles type
"L" (that function as support columns), a fixed plate, a reference sliding plate, and three digital sensors for measuring the
relative position between the camera interface of the spectrograph and the plane of its dewar. The cryostat system has a
lens that must be focused and aligned with the spectrograph. The cryostat and the mechanism have to be attached and it
has to allow rotational movements around the three axes with linear adjustments along them.
Similarly there is a brief description of the adjacent elements to understand the mechanism and functionality design
criteria used in order to ensure the proper functionality of the mechanism that has been tested and integrated in the
telescope. Such results are also described as well as the technical specifications, the manufacturing process and the
manufacturing drawings.
A brief description of the scientific instrument and some finite element simulations are also included in this work.
Finally, some recommendations and future work that may be carried out as a continuous improvement mechanism are
presented.
The Reionization and Transients InfraRed camera (RATIR) is a simultaneous optical/NIR multi-band imaging
camera which is 100% time-dedicated to the followup of Gamma-ray Bursts. The camera is mounted on the
1.5-meter Johnson telescope of the Mexican Observatorio Astronomico Nacional on Sierra San Pedro Martir in
Baja California. With rapid slew capability and autonomous interrupt capabilities, the system will image GRBs
in 6 bands (i, r, Z, Y, J, and H) within minutes of receiving a satellite position, detecting optically faint afterglows
in the NIR and quickly alerting the community to potential GRBs at high redshift (z>6-10). We report here
on this Spring's first light observing campaign with RATIR. We summarize the instrumental characteristics,
capabilities, and observing modes.
Eduardo de la Fuente, J. Manuel Nuñez, Salvador Zazueta, Salomon Eduardo Ibarra, Benjamin García, Benjamin Martínez, José Luis Ochoa, Gerardo Sierra, Fransisco Lazo, David Hirart, Luis Corral, Jorge Flores, Jaime Almaguer, Simon Kemp, Silvana Navarro, Alberto Nigoche-Netro, Gerardo Ramos-Larios, John Peter Phillips, Arturo Chávez, Guillermo García-Torales, Oscar Blanco Alonso, Tomas Oceguera-Becerra, Durruty de Alba, Ruben Bautista
We present the results of a modification performed in the optical system of the 62 cm telescope (f/14.32) at observatory
“Severo Díaz Galindo” Universidad de Guadalajara, Mexico. This modification consists of a change of distance between
the primary and secondary mirrors from 1020 to 1135 mm. With this, a change in the image plane from 5200 mm to 600
mm, measured from the vertex of the primary mirror, is obtained. The latter allow to get the first astronomical images of
The Telescope. This modification was necessary because alignment errors, such as distance between primary and
secondary mirrors in the original system were presented. Besides, the telescope has a new accurate and adequate
mechanical system installed on November 2011. Details and the first images obtained, are here presented.
ESOPO will be a spectrograph of medium resolution for the 2.1 m telescope of the National Observatory at San
Pedro Martir, Baja California, Mexico. It has been developed by the Instituto de Astronomia of the Universidad
Nacional Autonoma de Mexico (IA-UNAM). The main goal of this instrument is to modernize the capabilities
of making science with that particular telescope. It is planned to achieve a spectral resolution between 500 and
5000. ESOPO is split into two arms; each one specialized in a specific wavelength range covering together all the
visible light. A very important issue in spectrographs is to avoid inside thermal gradients. Different temperatures
in the optical elements produce mechanical movements and image quality degradation during an exposition. The
error budget analysis developed for ESOPO allows establishing the required limits for temperature gradients. In
this paper is described the thermal analysis of the spectrograph, including specifications, finite element models,
thermal equations and expected thermal gradients.
This work presents the specifications, requirements, design, finite element analysis and results of the assembled
subsystems: slit-mask, and the acquisition and guiding zone mechanisms of the ESOPO spectrograph. This spectrograph
is a project of the Institute of Astronomy, National University of Mexico.
The structure of the spectrograph ESOPO is the stiff mount that will maintain fixed all optics elements, electronics and
mechanical subsystems. The ESOPO spectrograph is a project of the "Instituto de Astronomia de la Universidad
Nacional Autonoma de Mexico" (IAUNAM) to upgrade its 2.1m telescope as a competitive facility for the next decade.
The scientific purpose is to obtain a modern high efficient intermediate-low dispersion spectrograph optimized for the
3500 - 9000 Å spectral interval with a spectral resolution of 500 ≤ R ≤ 5000. It is to be used at the cassegrain f/7.5 focus
of the 2.1 m telescope for general astronomical purposes. This work presents the mechanical design process and the form
in which the structure was verified to comply with the ESOPO's top level image quality and stability requirements. The
latter was not a lineal process. The way we resolved it is to run FEAs on the complete system and with the instrument in
different operation positions during a normal cycle of observations. These results are validated through the error budget
of the ESOPO. The structure is currently under construction.
In this paper we present the Medium Resolution Spectrograph ESOPO, an instrument designed and built for the 2.1m
Telescope at the Observatorio Astronómico Nacional at San Pedro Mártir. We discuss the Scientific Goals and the High
Level Requirements necessary to translate these goals to optical, mechanical and control specifications. We make an
introduction to its conceptual dual-arm design. The optical design is based on a non-classical configuration. The gratings
are illuminated in a conical mode working in a quasi Littrow configuration which has the advantage of optimizing the
efficiency and the pupil area on the grating. We show here the results of an experimental evaluation of the concept. The
optical design, mechanical structure, slit-mask and acquisition system, control systems, and a study of thermal
compensators, are discussed briefly, references to more extended contributions in these proceedings are made. The
management schematics of the project are briefly discussed.
The Mexican Infrared Telescope is one of the most important projects in the Institute for Astronomy of the National University of Mexico. As part of the design we pretend to simulate different components of the telescope by the Finite Element Method (FEM). One of the most important parts of the structure is the primary mirror support. This structure is under stress, causing deformations in the primary mirror; these deformations shouldn't be over 40 nanometers, which is the maximum permissible tolerance. One of the most interesting subjects to develop in this project is to make the segmented primary mirror to work like if it were a monolithic one. Each segment has six degrees of freedom, whose control needs actuators and sensors with stiff mechanical structures. Our purpose is to achieve these levels of design using FEM aided by computer and we pretend to study several models of the structure array using the Conceptual Design Method, in an effort to optimize the design.
We present the conceptual design of the primary mirror support system of the 7.8 m Mexican Infrared-Optical Telescope. The primary mirror consists of 19 hexagonal off- axis parabolic Zerodur segments, which are carried by a tubular, lightweight and high stiffness cell structure. Each segment is actively supported by 19 pneumatic actuators, that cover the whole back area and provide a uniform force distribution. The array of actuators will be able to correct for high order aberrations. Each of these actuators contains a hydraulic damping system to provide a stiff coupling to the tubular cell to sustain the wind buffeting. The tip/tilt and piston control of each segment will be done through three axial, nanometer resolution position defining actuators. The lateral positioning of each segment is performed through 3 independent electro-mechanical actuators. With the combination of the whole set of actuators and differential positioning sensors, the phasing or coherent superposition of images of the segments, will be more feasible. The whole system will be cost effective, since several subsystems have already been tested on our 2.1 m telescope.
We present the Mexican Infrared-Optical New Technology Telescope Project (TIM). The design and construction of a 7.8 m telescope, which will operate at the Observatorio Astronomico Nacional in San Pedro Martir, B.C. (Mexico), are described. The site has been selected based on seeing and sky condition measurements taken for several years. The f/1.5 primary mirror consists of 19 hexagonal off-axis parabolic Zerodur segments. The telescope structure will be alt-az, lightweight, low cost, and high stiffness. It will be supported by hydrostatic bearings. The single secondary will complement a Ritchey-Chretien f/15 design, delivering to Cassegrain focus instrumentation. The telescope will be infrared optimized to allow observations ranging from 0.3 to 20 microns. The TIM mirror cell provides an independent and full active support system for each segment, in order to achieve both, phasing capability and very high quality imaging (0.25 arcsec).
In this paper, the characteristics of a mount for secondary mirror of an astronomical telescope are presented. The mount has five freedom degrees. The control allows to focus with errors of +/- 1 micron and to align with inclinations and displacements with error of +/- 3.48 arcsec and +/- 8.3 micron respectively. The optical tests are presented before and after placing this mount, as well as control electronics and mechanical details.
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