Reloj sin manecillas: Prólogo de Jesús Carrasco (Spanish Edition)

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The mirror manufacturing facility will be further discussed in the context of the Giant Magellan Telescope. The primary optic of this telescope is formed by 7 very large 8. It is interesting to note that each mirror is of the same size as the LSST mirror! Artist conception of the LSST, viewed from the telescope platform. The primary-tertiary mirror combination, polished to specifications and ready to be stored.

Two artist conceptions of the GMT telescope, showing the seven mirrors in a single structure and the enclosure. Notice several objects placed in the images for scale comparison. The concept of the Giant Magellan Telescope is depicted above. It will be placed in a 60 m tall enclosure, the equivalent of a 22 story building that will be required to rotate smoothly following the telescope position.

With the central mirror being symmetric, the six outside mirrors need to make a perfect parabolic curve. As mentioned before, these mirrors are manufactured at the University of Arizona by means of a process first implemented following an idea by the British-born American astronomer, Roger Angel, that has produced a large number of the most modern mirrors, from 1. Once completed, the GMT, equipped with Adaptive Optics, a technique used by several ground based telescopes, will exploit its optical limit and will have a resolution ten times better than the Hubble Space Telescope.

The process involves a very large furnace with the ability to rotate. Hexagonal cylinders made of refractory material are distributed inside this furnace. Pieces of borosilicate glass are placed on top of the hexagons, and the furnace is closed and the heaters turned on. The combination of the way the refractories are distributed, the amount of glass and the rotation speed will make the glass occupy the spaces between the refractories and leave a thin sheet of glass of roughly 5 cm with the correct approximate shape to be adjusted and polished to the stringent required specifications.

As for the GMT, it is impossible to cast and polish a single mirror of this size. This technique has already been used in the construction of the VLT and the Keck telescopes. Both techniques face big challenges. Comparison of the diameters of the primary mirrors of the three telescopes described here.

This is seriously beneficial for the instrument teams, simplifying the design and avoiding flexures that can make the design almost impossibly expensive. While the 7 GMT mirrors have to be perfectly aligned in order to form a 25 m mirror, the segments of the E-ELT have to align perfectly too, so as to produce a single giant mirror. This enables telescopes to provide an area that is gravitationally invariant, where very large instruments can be placed.

As mentioned above, the LSST will have one mission. Artist conception of the E-ELT. The blue boxes, to the right of the telescope correspond to just one of the instruments. Also shown is an example of 5 out of almost segments. Considering that these projects will increase the possibilities of observation from the ground by several orders of magnitude, it is likely that new problems for which we, for the time being, ignore the questions will open new horizons.

These images will be made compatible and combined, providing the deepest and most complete image of the universe, paying special attention to objects that vary in their intensity or position from killer asteroids to the most distant supernovae and possibly the sources of gravitational waves.

These giant telescopes will look for planets of nearby stars, with the stated objective of finding Earth-like ones and to study in detail their atmosphere for possible indications of biological activity; stellar populations in the Milky Way and other galaxies and the origin of black holes, with special attention to the one in the centre of our galaxy. The interaction of galaxies and the first light in the universe, and the most distant galaxies will be studied.

Cosmology and the origin of Dark Matter and Dark Energy are problems to be addressed also. As mentioned previously, telescopes need dark skies in order to fully exploit their capabilities. Contaminated skies inhibit the capabilities of large telescopes making them equivalent to smaller telescopes since the contrast is diminished and the background is filled with artificial spectral features.

Historically, large telescopes have been rendered close to useless because of this. Other articles will address this subject in more detail. Let us fight this with determination: The summit of Sierra Negra was selected for the positioning of the LMT as a result of the low water vapour content of its atmosphere, which is due to its altitude of almost 4, m. The site started developing infrastructure shortly after being chosen and the LMT itself was constructed between and Its first light on the millimetre-wave range was announced on 1 June , a few weeks before the passing of Alfonso Serrano, its initial and longtime promoter.

Since , the telescope has been used in scientific operations, with an aperture of 32 m, and is due to reach full 50 m operations by the end of The telescope is part of the Event Horizon Telescope initiative, a global project that aims to capture images of the black hole at the Galactic Centre in The development of basic infrastructure at Sierra Negra, specifically the access road, electricity and the internet, prompted the installation of other facilities benefiting from the thin atmosphere of this high altitude site.

The HAWC was installed 1 km north and m below the LMT, at an altitude of 4, m, and consists of an array of individual water Cherenkov detectors. Sierra Negra is an exceptional site providing tolerable conditions, such as relatively mild weather at more than 4, m and a very low electromagnetic interference noise. The conditions for optical astronomy have been partially studied, with optical seeing data obtained from to showing a median of 0.

Despite its location in a relatively populated region of Mexico, the sky at Sierra Negra is dark to the eye, a likely effect of its altitude. Future instruments needed for dark skies, which could be considered for Sierra Negra, are optical and atmospheric Cherenkov telescopes. Sin embargo, el resplandor real del cielo sigue estando por cuantificarse. The laminar flow of air coming from the ocean and reaching the first mountain range, almost unperturbed, provides ideal conditions for optical astronomical observations. The evolution of observational techniques in astronomy beyond the visible portion of the electromagnetic spectrum resulted in unprecedented demands for finding potential sites for new facilities.

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A relevant example in Mexico are radio experiments that require minimal electromagnetic interference. These conditions, recently measured on Guadalupe Island, may allow the unique exploration of the early universe. Moving towards the south, the Central Mexican Plateau has peaks higher than m. These peaks could be potentially exploited by scientific facilities that benefit from high altitude conditions.

The water vapour content of some of these peaks was monitored in the early s during the search for the site of the Large Millimetre Telescope Alfonso Serrano LMT. In February , the tallest of these sites, Sierra Negra, was selected and development began shortly afterwards. With an altitude of 4, m, Sierra Negra is the fifth highest mountain in Mexico, just a few metres shorter than Nevado de Toluca. While Sierra Negra is an old volcano without signs of volcanic activity, the crater of Pico de Orizaba is about 4, years old and has a record of minor eruptions and exhalations that started in and continues to the present day Rossotti, The LMT, the most ambitious science project undertaken by Mexico, was formally approved in Sierra Negra or Tliltepetl, the black mountain, in front of the white snowy Citlaltepetl, the mountain of the stars.

The most relevant parameter was the column density of water vapour in the atmosphere for which the main competing factors were the intrinsic drier conditions of the north of Mexico and the thinner atmosphere at high altitude. Monitoring of the Nevado de Toluca showed altitude to be dominant, leading to the eventual selection of the highest site monitored: The HAWC Very High-Energy, Ray Observatory Since , it has been recognized that very energetic particles from outer space, termed cosmic rays, continuously penetrate the terrestrial atmosphere Friedlander, This finding led to the construction of arrays of particle detectors, or Extensive Air Shower Arrays, for the study of high- 1.

The array is approximately m on each side, with a single detector 7. Between and , the high altitude Milagro EAS, located in New Mexico at an altitude of m, proved the feasibility of effectively distinguishing between cosmic ray and gamma ray induced cascades, opening the possibility of performing studies on astrophysical sources. The detection by Milagro of TeV gamma ray emission from sources like the Crab Nebula, Mkn and the Galactic Plane was the basis for proposing an improved designed detector to be located at a higher altitude: A Mexican interest group comprised of individuals from several institutions formed and, as a result, a site feasibility study was carried out for the installation of the HAWC at Sierra Negra.

A flattened platform of 22, m3 was prepared in for the installation of the array between and The array consists of water Cherenkov detectors, each 7. Temperature, atmospheric pressure, relative humidity and wind velocity at Sierra Negra for the different months left and hours right. The HAWC is unaffected by observational conditions, light pollution or weather, with the exception of extreme weather, like electric storms or heavy precipitation. In the next two years, a peripheral outrigger array will be installed around the HAWC.

It will be made of more than smaller detectors containing l of water each and separated by 10 to 15 m. The expanded HAWC array will cover a total area of , m2 centred on the current dense array, significantly increasing the response of the detector for gamma ray energies above 10 TeV Sandoval, Other Experiments at Sierra Negra There are some smaller experiments taking place in the area at the top of the mountain which were installed through agreements signed with the INAOE: It was installed between and in a hut just 70 m south-west of the LMT, starting operations shortly thereafter.

This instrument, originally a neutrino detector at the Fermi National Accelerator Laboratory, consists of 14, scintillator bars connected to multi-anode photomultiplier tubes and has been performing as a solar neutron detector and a high resolution cosmic ray detector at Sierra Negra since mid Sasai et al. The LAGO station at Sierra Negra is designed as an array of four water Cherenkov detectors, one of them of the same dimensions as those at the HAWC, while the other three are of the same diameter, but just 1 m tall.

Among the studies carried out, we can list the following, to be detailed further: Measurements of electromagnetic noise for frequencies between 20 and 40 GHz. The data is dominated by instrumental noise, with no detection of interference. These telescopes require dark and clear skies to operate and are sensitive to light pollution. The Conditions at the Sierra Negra Site Sierra Negra has had a particular history of monitoring, due to its origin as the site of the Large Millimetre Telescope Alfonso Opacity at Millimetre Wavelengths Measurements of the atmospheric opacity at a frequency of GHz were carried out between August and November for the site selection process.

The opacity measurements were correlated with contemporaneous precipitable water PPW vapour measurements in order to obtain extrapolated opacity estimates dating back to Sierra Negra was found to show opacities below 0. Meteorological Data One relevant aspect of Sierra Negra is the benign weather when considering the altitude of the site.

Statistics on weather data taken over more than seven years, between and , were presented by Carrasco et al. The weather station was located some m north-east of the LMT, at an altitude of 4, m. We noted that temperature medians do not vary significantly between day 2.

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Estimate of the light pollution effect of population centres on Sierra Negra, measured by the ratio between the increase of light and the natural level of sky brightness. Reproduced from Carrasco et al. The data also contained information regarding solar radiation incidents and was used to quantify the fraction of clear skies, showing this to vary significantly between the wet and dry seasons, May to October and November to April respectively.

Simultaneous data are currently being acquired at the two different altitudes, with the goals of correlating the weather variables and studying the structure of the atmosphere. Optical Seeing Optical seeing is a measure of the apparent size of a star, which is dominated by the widening effect of turbulent air in the atmosphere. As a result, while the Sun, located at one parsec 3. Astronomical seeing was measured at Sierra Negra between and using a Differential Image Motion Monitor, in order to evaluate the possibility of installing a large optical telescope at Sierra Negra.

The median of the seeing data acquired then was 0. Low frequency data showed signals from radio-FM, TVs, mobile telephones, radio-localization and radio-navigation systems, as expected. Aside from these signals recorded at frequencies below 3 GHz, no interference above the instrumental noise of the detector system, between —70 and —80 dBm, was perceived. Electromagnetic interference is an obvious concern for the LMT, in particular for frequencies above 75 GHz.


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However, its instrumentation is prone to interference at lower frequencies. These intermediate frequencies, often between 2 and 5 GHz, are more vulnerable to interference by systems like cellular phones or wireless links. In particular, all data generated at the site is transmitted through the on-site optical fibre, avoiding the use of microwave links.

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This note considers a km radius protection zone for the LMT, difficult to implement in practice. Currently, services above 75 GHz in Mexico are virtually non-existent and the National Park does provide some protection to the site against electromagnetic noise. Summary Mexico has an invaluable number of astronomical sites. Due to the nature of its facilities, Sierra Negra has been characterized in terms of the water vapour content of its atmosphere, its weather and radio frequency interference noise.

The optical seeing of Sierra Negra has been measured, showing the site to be competitive for astronomy in the visible spectrum. Located inside a national park, Sierra Negra has local conditions that allow it to keep its dark skies. Sky Brightness Sky brightness has not been properly studied at Sierra Negra, in part because there has not been a project with the resources to establish an optical telescope on site. The site is located near important population centres and their effect on the sky at the site was estimated in Carrasco et al.

The table shown in Carrasco et al. The values of log r , shown in Table 2, can only be indicative as they need to be updated and there is no consideration of the high altitude of the Sierra Negra site, which is bound to result in a lower level of light pollution as less urban light is scattered down. On-site measurements were made back in , using a inch telescope.

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These data are not sufficient to properly define sky brightness at Sierra Negra, where night images from the site show Carrasco, E. Weather at Sierra Negra: Optical seeing at Sierra Negra. Publications of the Astronomical Society of the Pacific, Vol. Site Conditions at Sierra Negra. National Table of Frequency Allocations: Milagro maps out gamma-ray frontier. The Latin American Giant Observatory: HAWC upgrade with a sparse outrigger array.

Performance of the SciBar cosmic ray telescope SciCRT toward the detection of high-energy solar neutrons in solar cycle Earth, Planets and Space, Vol. Evaluation of the long term behavior of sites for mm-wavelength radio-astronomy: Advances in Space Research, Vol. The night sky from Cerro Murphy, Chile. Chapter 4 The Protection of Dark Skies: As a country, Chile faces the challenge of fighting light pollution and protecting its dark skies in a context of sprawling urban growth and an ever-expanding mining industry that shares the same territory with astronomical observatories.

Whilst describing our experiences, I highlight the importance of approaching the problem of light pollution from all sides, involving all the relevant actors communities, national and local governments, lighting industry, environmentalists, astronomers and others. I also discuss how communication and timely coordination with potential problematic actors like industries, cities and some government agencies can be an effective tool to transform potential enemies into allies in the fight for the protection of the night sky. This is the largest and most powerful radio telescope in the world, consisting of a sixty-six 12 m antenna interferometer.

World Capital of Astronomy During the first half of the twentieth century, the largest telescopes in the world, like the inch Hooker Telescope at Mount Wilson and the Palomar inch Hale Telescope, were mostly concentrated in southern California, in the continental United States. In the s and s, American and European astronomers started scouting potential sites in the Atacama Desert in northern Chile.

This was part of an effort to find places offering superb observation conditions and also ensuring low levels of light pollution in the future. The urban sprawl of cities like Los Angeles and San Diego was quickly diminishing the capabilities of the most powerful telescopes in the world, and the low population density of the Atacama Desert and its remoteness seemed to offer decades, even centuries, of dark skies ahead.

Chile and its government see the development of astronomy as an opportunity for national development. The scientific cooperation between international observatories and Chilean universities has translated into enormous advances in the quality, quantity and impact of astronomy, astrophysics and astronomical instrumentation research that is conducted in Chile.

Today, Chilean universities are at the forefront of astronomical research and compete side by side with universities in Europe and North America. The international observatories in the Atacama have also sparked the attraction and training of highly qualified professionals in several fields of engineering, physical and mathematical sciences and computer science. The transfer of knowledge, expertise and technology between astronomical observatories, universities and the private sector offers enormous opportunities for the development of advanced technology engineering companies in Chile, an aspect of strategic importance for future economic growth and international competitiveness.

Light Pollution in Chile Until the early s, light pollution around important astronomical observatories in Chile was minimal. Initiatives, Education and Coordination sky brightness consistent with natural virgin levels. It is clear that the areas affected by light pollution have increased substantially over the years. The problem of light pollution is now evident to the naked eye in remote sites such as Las Campanas. Figure 2 shows a long exposure all sky image of the night sky at this site.

One can also see significant sources of light pollution from nearby mining operations, and the lights illuminating crossroads and toll plazas on a nearby stretch of the Panamerican Highway. A few decades ago, these levels of light pollution at such remote sites were unimaginable. Astronomers, in pursuit of good image quality and low sky brightness, usually conduct their observations by pointing their telescopes at high elevations above the horizon.

Astronomical observations, therefore, tend to avoid the areas most dramatically affected by light pollution. Beyond the direct detrimental effects of light pollution on the quality of astronomical observations, several other negative effects are now recognized to be associated with excessive, unnecessary levels of illumination. Moreover, in the particular case of Chile, light pollution threatens to take away all the evident benefits to our society that the development of astronomy is currently providing and will provide in the future. Light Pollution Regulation in Chile Figure 1. Evolution of light pollution in northern Chile Red squares mark the positions of the main optical astronomical observatories in Chile.

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From south to north: Falchi, University of Padova; C. Lorenz, University of Wisconsin-Madison. Astronomers in Chile had already began expressing serious concerns about the problem of light pollution and its dramatic evolution in the s. This enormously mitigated the growth of light pollution during the s, which, given the growth of cities in the region, could have been much worst during that decade.

This prompted the development of new regulation, now coming from the Ministry of Environment. While this new decree has the potential to be a powerful tool for controlling light pollution in the Atacama Desert, its implementation has suffered delays. Ensuring a significant level of compliance will require major efforts in education and coordination between the different actors involved in the problem of light pollution. Present day levels of light pollution at Las Campanas Observatory. Atacama and Coquimbo , where most of the observatories are located. It was created in the year and it currently has more than members, including 1.

Blue light produces more light pollution than red light as it scatters more easily in the atmosphere. Initiatives, Education and Coordination a minor issue that should be given low priority when it comes down to enacting and enforcing environmental protections. Therefore, the starting point for our work on light pollution education is the general public, and the most effective tool to reach this public is the press. During , we were mentioned approximately twelve times in the national newspapers, television and radio shows.

We also encourage all the members of our society to mention the subject of light pollution whenever they are interviewed about their scientific discoveries. This requires maintaining good relations with scientific journalists at the main news outlets in the country and also being fully available whenever an opportunity to raise the subject in the media arises.

These include, on one side, the astronomers, the environmentalists and the regulatory government agencies like the Ministry of Environment that have a vested interest in the fight against light pollution. On the other side, local communities, city governments, private industries and other national and regional government agencies related to energy and transportation, can all see different incentives to either produce more light pollution or reduce its levels.

For example, a local city government might want to increase the level of lighting in its streets in an effort to reduce night-time crime in the area, or it might want to reduce its electric bill by adopting better illumination practices that reduce the amount of wasted energy spent on illuminating the sky. If the problem of light pollution is to be addressed effectively, we must involve all the different actors, understand their needs and priorities, and find common ground and synergies that reasonably protect their interests while also protecting our dark skies.

Beyond the general public, a fundamental part of our strategy is to target specific interest groups such as companies that fabricate, import and distribute hardware for public and industrial lightning. For this, in close collaboration with the OPCC, we organized two workshops during that directly targeted the lighting industry. In these workshops, one of which included a presentation by the Chilean Minister of the Environment, Pablo Badenier, and other government authorities, we exposed the subject of light pollution and the technical requirements that the law mandates for illumination products to be certified for installation in protected regions.

In this context, SOCHIAS is involved in several initiatives aimed at protecting the dark skies of northern Chile, which target different actors in the problem of light pollution. These initiatives fall under two main categories: Both are essential tools in our fight to protect the unique resource that our country has in its night sky. We are seeing a very positive response from these companies and have taken away an important lesson from this experience.

Companies in the illumination business have an obvious interest in selling more of their products and therefore have traditionally been seen as adversaries of groups trying to decrease the levels of light pollution. As a result of the new relationship that has been established through these workshops, we are happy to see some companies embracing the fight against light pollution and viewing it as an opportunity to better market their products as environmentally friendly and up to standard with the strict requirements of the law.

They also see the need for massive replacement of old non-compliant luminaires as a potential business opportunity. This is a textbook case of how communication, education and an interest in understanding the Education Initiatives Education starts from raising awareness about the existence of the problem of light pollution and the importance of the protection of dark skies.

The first of these training programmes took place in June of in the cities of Coquimbo and La Serena. The first is aimed at understanding the negative impacts of light pollution and the second is aimed at understanding the technical requirements that Chilean law mandates in terms of characteristics and certifications for new luminaires. Similar experiences are regularly seen with companies in the mining sector, who because of worker safety concerns have a strong incentive for maintaining high levels of illumination in their facilities.

The experience of the OPCC shows how receptive these companies are when, by means of meetings and other instances of communication, they realise that by minimal investments they can maintain the same levels of safety while dramatically reducing their impact on light pollution. In the case of the mining sector, there is a strong incentive to reduce light pollution in order to offset other environmental impacts associated with mining and to maintain a good image of social responsibility and sustainability.

A fundamental goal of these instances is to also include regional authorities and local representatives of the national government, as well as members of the local communities for example, interested parties like astrotourism business owners. In this way, we can start creating a network of support for the municipalities that can help them push forward the necessary projects to improve their outdoor illumination systems. Maybe the most important actors in the protection of our dark skies are local city or county governments. Ultimately, these are the decision makers responsible for approving and executing most of the outdoor illumination projects in a particular region.

Surprisingly, most professional astronomers in the world are not actively involved in the protection of dark skies. Since the ability to observe the universe from places like the Atacama Desert is a fundamental part of their job, one would expect a much higher level of involvement in dark skies protection than what is currently seen. The low involvement of professional astronomers is caused in part by the enormously competitive and absorbing nature of academic work and research, but we have come to realise that there is another important factor: Almost all astronomers are aware of the problem of light pollution but do not know what they can do about it on an individual level.

While municipalities have a lot of influence on the way illumination is organized and implemented in their jurisdictions, they very often lack the economic resources to update their illumination systems, and they depend a lot on the national and regional governments to provide the necessary funding for such projects.

Also, municipalities are often not well informed about the requirements in terms of design and certification that lighting fixtures must fulfil, and this can translate into erroneous purchases and installations of noncompliant and pollutant illumination systems. Therefore, as a society we are trying to actively involve the Chilean astronomical community in our dark sky protection initiatives.

Since , we have reserved a space in the SOCHIAS Annual Meeting the most important and highly attended scientific conference on astronomy in Chile to have talks and open discussion about light pollution. Initiatives, Education and Coordination Figure 3: The photo shows the highway before and after the installation of new illumination systems at intersections and toll plazas that are not compliant with the new regulatory standards for light pollution in the region. This includes providing them with material that they can use in their classes and during outreach talks, showing them how to use the existing systems to denounce violations of the legislation that regulates light pollution in the country and offering them opportunities for involvement in the different initiatives we lead.

It is fundamental for us to actively involve the members of our society in the initiatives and activities that we push forward. Coordination While education is a fundamental tool in ensuring the long-term support of all the different actors involved in light pollution, it is a slow process, and there are immediate threats to the quality of our night sky that must be addressed today by means of direct involvement. The first of these is a major national programme being pushed forward by the Ministry of Energy of Chile and the Chilean Agency for Energy Efficiency AChEE in Spanish , which aims to replace , streetlights across the country for energy efficient LED lights during the next four years.

A swift reaction by the part of the OPCC, SOCHIAS and the astronomical observatories, together with a positive response from the Ministry of Foreign Relations and the agencies pushing forward the programme, now ensures that all the new luminaires installed in protected regions as part of this initiative will be compliant with the new standards. A greater level of oversight and coordination could have prevented this problem.

Today, there are plans for transforming this stretch of highway into a pilot project for testing Amber LED technology one of the most astronomy-friendly types of LED illumination on Chilean roads. If all goes well, such installations could become standard around major observatories in the country. In summary, there is a lesson to be learned from these experiences. We cannot assume that private parties and government agencies will be aware of light pollution and will consider it as an important priority during their decision making processes.

Therefore, constant vigilance by interested parties like observatories, scientific societies and environmental agencies is fundamental. In our experience, even minimal levels of communication, education and coordination can be successful at making people understand the problem of light pollution and see the overall benefits of avoiding it. Another experience that shows the need for constant oversight and coordination is an illumination project undertaken by the Chilean Ministry of Public Works on a stretch of the Panamerican Highway that crosses right in front of the La Silla and Las Campanas observatories.

As part of a major upgrade to the highway and in an effort to comply with current safety standards for road illumination, all new intersections and a newly installed toll plaza were fitted with extremely bright lightning.

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Protecting our Heritage and Final Conclusions The final and perhaps most important initiative that we are currently involved in, concerning the protection of our night sky, is an effort to recognize the Outstanding Universal Value that these marvellous sites in the Atacama Desert have for all of humanity. They are the places from which humanity learns about the cosmos, unveils its origins and comes to understand its place in the world. Figure 3 shows two photographs taken from Las Campanas Observatory, more than 1, m above the level of the highway, before and after this upgrade.

It is impressive to see the large amounts of light being emitted towards the sky from the highway, which, as also seen in Figure 1, is a major source of light pollution in the area. Initiatives, Education and Coordination It is this concept of preserving a unique and beautiful natural laboratory, which provides us with a window to the universe and to ourselves that guides our efforts.

Chile as a nation has the responsibility to protect what nature has endowed us with and it is exciting to see how governments, industries, scientists and the public are starting to share this realisation. There is still a lot of work to be done, but we are on the right path to ensure that future generations will have access to the same dark sky that we have inherited from our ancestors. Desert as Protected Areas.

Such recognitions would provide enormous leverage to institutions like SOHCIAS and the OPCC to push forward the protection of these sites against light pollution, but there is a more fundamental impact that we expect from such designations. We hope that the citizens of our country will start considering the beautiful clear and dark sky of the Atacama Desert as a fundamental part of their heritage. Something they should be proud of and something that their country as a nation must preserve for all humanity to enjoy for centuries to come. Abstract Thanks to its clear, stable and dark night skies, the quality of local infrastructure, a highly qualified workforce and a bold national commitment to protect the night sky, Chile has become one of the most significant centres for major astronomical observation projects in the world.

The region is home to the following observatories: These decrees serve to protect the skies of Antofagasta, Atacama and Coquimbo by limiting direct light emissions into the upper hemisphere from outdoor light sources. The second of the two decrees is stricter as it seeks to respond to the threat of the emergence of solid state technology LED , used mostly in outdoor billboards, and the mass use of cold light sources with strong blue components, both of which impair the visibility of the night sky more aggressively than warmer light sources.

This decree also strictly limits light emissions into the upper hemisphere from 0. In addition to these regulatory efforts to protect the night sky, the Government of Chile, the scientific community and astronomical observatories are currently examining protection options, including the Windows to the Universe initiative, a joint programme between UNESCO and the International Astronomical Union IAU , whose aim is to increase representation of the most relevant sites of astronomical observation, including those in northern Chile, on the World Heritage List.

El rango bajo nm no estaba convenientemente restringido, el correspondiente al color azul. Sus principales restricciones son las siguientes: Esto, para casi todas las aplicaciones: Todo esto referido respecto al rango visible. El seminario realizado en Mt. Uso de luz roja en balizamientos. In the last decade, the country has become aware of this exceptional situation and its implications in terms of opportunities and responsibilities.

In the s, when astronomical activities in Chile began, the country facilitated the establishment of several scientific projects in the region of Norte Chico and the Atacama Desert. In this regard, and perhaps without initially fully understanding the implications, the government has developed a policy of attracting astronomy projects to the country. Chile is responsible for preserving these exceptional sites for humanity and is committed to being a leader in efforts to protect the dark skies. To this end, the government has established a policy based on four pillars, which combines national and international interests to respond to the question, how can we create fruitful relationships between astronomy and national development?

The following article will explore this question in more detail using specific examples from Chile. Theater Without a Stage: Celestina and the Humanistic Comedy By: Calisto and Leriano in Love By: The Story of Hero and Leander: Approaches to Parody in Celestina By: The Politics of Prostitution in Celestina By: A Guidebook for Two Cities: Magic in Celestina By: Manuel da Costa Fontes. Celestina as a Precursor to the Picaresque By: View or edit your browsing history. Get to Know Us. English Choose a language for shopping. Would you like to report this content as inappropriate? Do you believe that this item violates a copyright?


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