A startrail of Magellanic Clouds around the South Pole
In the left side of the sky we can see the trail of Sirius star. Moving to the right in the center of the image, is located the Canopus startrail, as well the draged motion of Large and Small Magellanic Clouds. Below them, the rotational motion of Earth helped to find with precision the right position of the South Pole in the sky. In the ground, we can see the white dome of Residencia where astronomers from ESO working daily on VLT complex, are hosted.
The Very Large Telescope (VLT) is a telescope operated by the ESO – European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT is the world’s most advanced optical instrument, consisting of four Unit Telescopes with main mirrors of 8.2m diameter, which are generally used separately but can be used together to achieve very high angular resolution. The four separate optical telescopes are known as Antu, Kueyen, Melipal and Yepun, which are all words for astronomical objects in the Mapuche language, with optical elements that can combine them into an astronomical interferometer (VLTI), which is used to resolve small objects. The interferometer is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture. The 8.2m diameter Unit Telescopes can also be used individually. With one such telescope, images of celestial objects as faint as magnitude 30 can be obtained in a one-hour exposure. This corresponds to seeing objects that are four billion (four thousand million) times fainter than what can be seen with the unaided eye. The telescopes can work together, to form a giant ‘interferometer’, the ESO Very Large Telescope Interferometer, allowing astronomers to see details up to 25 times finer than with the individual telescopes. The light beams are combined in the VLTI using a complex system of mirrors in underground tunnels where the light paths must be kept equal to distances less than 1/1000 mm over a hundred metres. With this kind of precision the VLTI can reconstruct images with an angular resolution of milliarcseconds, equivalent to distinguishing the two headlights of a car at the distance of the Moon.
Image taken taken in 17/10/2015 from Cerro Paranal, Atacama desert, Chile.
Magellanic Clouds, Zodiacal Light and Gegenschein on a VLT Panorama
In the left side of this – almost 360º- panoramic view, we can see Canopus star and the Large (LMC) and Small (SMC) Magellanic Clouds. Above the horizon, in the beginning of Milky Way arc, are yet visible the bright stars Alpha and Beta Centauri. At the center, lie down the galactic arm with the Zodiacal Light as a background of Antu telescope. Next to the last telescope is clearly visible the elongated diffuse light coming from Andromeda galaxy. In the upper part of the image and opposite direction of Magellanic Clouds, is shining a Gegenschein, that is a faint brightening of the night sky in the region of the antisolar point. Like the zodiacal light, the Gegenschein is sunlight scattered by interplanetary dust. Most of this dust is orbiting the Sun in about the ecliptic plane. It is distinguished from zodiacal light by its high angle of reflection of the incident sunlight on the dust particles. Below right and near the horizon, the Pleiades (M45) star cluster is visible next the tower silhouette.
The Very Large Telescope (VLT) is a telescope operated by the ESO – European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT is the world’s most advanced optical instrument, consisting of four Unit Telescopes with main mirrors of 8.2m diameter, which are generally used separately but can be used together to achieve very high angular resolution. The four separate optical telescopes are known as Antu, Kueyen, Melipal and Yepun, which are all words for astronomical objects in the Mapuche language, with optical elements that can combine them into an astronomical interferometer (VLTI), which is used to resolve small objects. The interferometer is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture. The 8.2m diameter Unit Telescopes can also be used individually. With one such telescope, images of celestial objects as faint as magnitude 30 can be obtained in a one-hour exposure. This corresponds to seeing objects that are four billion (four thousand million) times fainter than what can be seen with the unaided eye. The telescopes can work together, to form a giant ‘interferometer’, the ESO Very Large Telescope Interferometer, allowing astronomers to see details up to 25 times finer than with the individual telescopes. The light beams are combined in the VLTI using a complex system of mirrors in underground tunnels where the light paths must be kept equal to distances less than 1/1000 mm over a hundred metres. With this kind of precision the VLTI can reconstruct images with an angular resolution of milliarcseconds, equivalent to distinguishing the two headlights of a car at the distance of the Moon.
Image taken taken in 16/10/2015 from Cerro Paranal, Atacama desert, Chile.
Twlight on VLT and the Southern Crescent Moon
Twilight behind the Yepun VLT Telescope (at left) and Survey Telescope VST (at right) while they start opening his doors, preparing for a night of research. The faint and inverted crescent moon of the southern hemisphere, can be seen in the center of the image.
The Very Large Telescope (VLT) is a telescope operated by the ESO – European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT is the world’s most advanced optical instrument, consisting of four Unit Telescopes with main mirrors of 8.2m diameter, which are generally used separately but can be used together to achieve very high angular resolution. The four separate optical telescopes are known as Antu, Kueyen, Melipal and Yepun, which are all words for astronomical objects in the Mapuche language, with optical elements that can combine them into an astronomical interferometer (VLTI), which is used to resolve small objects. The interferometer is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture. The 8.2m diameter Unit Telescopes can also be used individually. With one such telescope, images of celestial objects as faint as magnitude 30 can be obtained in a one-hour exposure. This corresponds to seeing objects that are four billion (four thousand million) times fainter than what can be seen with the unaided eye. The telescopes can work together, to form a giant ‘interferometer’, the ESO Very Large Telescope Interferometer, allowing astronomers to see details up to 25 times finer than with the individual telescopes. The light beams are combined in the VLTI using a complex system of mirrors in underground tunnels where the light paths must be kept equal to distances less than 1/1000 mm over a hundred metres. With this kind of precision the VLTI can reconstruct images with an angular resolution of milliarcseconds, equivalent to distinguishing the two headlights of a car at the distance of the Moon.
Image taken taken in 15/10/2015 from Cerro Paranal, Atacama desert, Chile.
Milky Way Arc above the Yepun and VST Telescopes
Milky Way arc of gas and dust lying behind the Yepun (UT4) VLT Telescope, in the foreground, while it is capturing the light coming from deep space. Below left we can see the bright light of the moon and above it, the planet Saturn. At the right edge of the image, we can see the VLT Survey Telescope (VST), that is the latest telescope to be added to ESO’s Paranal Observatory in the Atacama Desert of northern Chile. Above the VST is shinning the bright star Vega, forming in the upper right area, the well known asterism as The Summer Triangle.
The Very Large Telescope (VLT) is a telescope operated by the ESO – European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT is the world’s most advanced optical instrument, consisting of four Unit Telescopes with main mirrors of 8.2m diameter, which are generally used separately but can be used together to achieve very high angular resolution. The four separate optical telescopes are known as Antu, Kueyen, Melipal and Yepun, which are all words for astronomical objects in the Mapuche language, with optical elements that can combine them into an astronomical interferometer (VLTI), which is used to resolve small objects. The interferometer is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture. The 8.2m diameter Unit Telescopes can also be used individually. With one such telescope, images of celestial objects as faint as magnitude 30 can be obtained in a one-hour exposure. This corresponds to seeing objects that are four billion (four thousand million) times fainter than what can be seen with the unaided eye. The telescopes can work together, to form a giant ‘interferometer’, the ESO Very Large Telescope Interferometer, allowing astronomers to see details up to 25 times finer than with the individual telescopes. The light beams are combined in the VLTI using a complex system of mirrors in underground tunnels where the light paths must be kept equal to distances less than 1/1000 mm over a hundred metres. With this kind of precision the VLTI can reconstruct images with an angular resolution of milliarcseconds, equivalent to distinguishing the two headlights of a car at the distance of the Moon.
Image taken taken in 15/10/2015 from Cerro Paranal, Atacama desert, Chile.
Sunset Between the VLT Telescopes
Sunset rays illuminating with an orange light the left face of Antu Telescope (the first one). In the foreground, at right, we can see the Melipal Telescope few minutes before start opening his doors to the Universe. The faint and inverted crescent moon of the southern hemisphere, can be seen at the left upper edge of the telescope, surrounded by the blue sky of twilight.
The Very Large Telescope (VLT) is a telescope operated by the ESO – European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT is the world’s most advanced optical instrument, consisting of four Unit Telescopes with main mirrors of 8.2m diameter, which are generally used separately but can be used together to achieve very high angular resolution. The four separate optical telescopes are known as Antu, Kueyen, Melipal and Yepun, which are all words for astronomical objects in the Mapuche language, with optical elements that can combine them into an astronomical interferometer (VLTI), which is used to resolve small objects. The interferometer is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture. The 8.2m diameter Unit Telescopes can also be used individually. With one such telescope, images of celestial objects as faint as magnitude 30 can be obtained in a one-hour exposure. This corresponds to seeing objects that are four billion (four thousand million) times fainter than what can be seen with the unaided eye. The telescopes can work together, to form a giant ‘interferometer’, the ESO Very Large Telescope Interferometer, allowing astronomers to see details up to 25 times finer than with the individual telescopes. The light beams are combined in the VLTI using a complex system of mirrors in underground tunnels where the light paths must be kept equal to distances less than 1/1000 mm over a hundred metres. With this kind of precision the VLTI can reconstruct images with an angular resolution of milliarcseconds, equivalent to distinguishing the two headlights of a car at the distance of the Moon.
Image taken taken in 15/10/2015 from Cerro Paranal, Atacama desert, Chile.
The Great Milky Way above Antu, Kueyen and Melipal VLT Telescopes
In this close-up of the central region of the Milky Way full of gas and dust, star clusters and emission nebulae, lies as the perfect background to framing the right alignment (from left to right) between the VLT telescopes Antu (UT1), Kueyen (UT2) and Melipal (UT3). In Mapuche language, Antu means “The Sun”, Kueyen “The Moon” and Melipal “The Southern Cross”.
The Very Large Telescope (VLT) is a telescope operated by the ESO – European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT is the world’s most advanced optical instrument, consisting of four Unit Telescopes with main mirrors of 8.2m diameter, which are generally used separately but can be used together to achieve very high angular resolution. The four separate optical telescopes are known as Antu, Kueyen, Melipal and Yepun, which are all words for astronomical objects in the Mapuche language, with optical elements that can combine them into an astronomical interferometer (VLTI), which is used to resolve small objects. The interferometer is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture. The 8.2m diameter Unit Telescopes can also be used individually. With one such telescope, images of celestial objects as faint as magnitude 30 can be obtained in a one-hour exposure. This corresponds to seeing objects that are four billion (four thousand million) times fainter than what can be seen with the unaided eye. The telescopes can work together, to form a giant ‘interferometer’, the ESO Very Large Telescope Interferometer, allowing astronomers to see details up to 25 times finer than with the individual telescopes. The light beams are combined in the VLTI using a complex system of mirrors in underground tunnels where the light paths must be kept equal to distances less than 1/1000 mm over a hundred metres. With this kind of precision the VLTI can reconstruct images with an angular resolution of milliarcseconds, equivalent to distinguishing the two headlights of a car at the distance of the Moon.
Image taken taken in 15/10/2015 from Cerro Paranal, Atacama desert, Chile.
A Desert Oasis on a Fulldome
A fish-eye view of the fulldome from the ESO’s Paranal Residencia. It provides a relaxing environment for astronomers and support staff that come to visit the telescopes at ESO’s Paranal Observatory. To the visitor who arrives at the Paranal Residencia from the harsh natural environment, the welcoming feeling under the dome is unexpected and instantly pleasant. This is a true “oasis” in a form of a small garden with a swimming pool. There is a strong sense of calm and serenity and, above all, a feeling of coming home. At night, the lighting below the roofing closure fabric is spectacular and the impression on the mind is overwhelming. The vertical structure at the centre is an umbrella that is deployed at sunset and during the night, protecting the observatories from all artificial light.
Image taken taken in 17/10/2015 from inside the “Residencia” of Cerro Paranal, Atacama desert, Chile
Oasis in the Atacama Desert
A fish-eye view of the ESO’s Paranal Residence known as “La Residencia”. It provides a relaxing environment for astronomers and support staff that come to visit the telescopes at ESO’s Paranal Observatory. To the visitor who arrives at the Paranal Residencia from the harsh natural environment, the welcoming feeling under the dome is unexpected and instantly pleasant. This is a true “oasis” in a form of a small garden with a swimming pool. There is a strong sense of calm and serenity and, above all, a feeling of coming home. At night, the lighting below the roofing closure fabric is spectacular and the impression on the mind is overwhelming. The vertical structure at the centre is an umbrella that is deployed at sunset and during the night, protecting the observatories from all artificial light.
Image taken taken in 17/10/2015 from inside the “Residencia” of Cerro Paranal, Atacama desert, Chile
A Startrail Fish-Eye View Above VLT Telescopes
A startrail fish-eye view of a draged Milky Way behind a cloudy sky, above the VLT Unit Telescopes in Cerro Paranal. At left, we also can see the light coming from the moonset. The Very Large Telescope (VLT) is a telescope operated by the ESO – European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT is the world’s most advanced optical instrument, consisting of four Unit Telescopes with main mirrors of 8.2m diameter, which are generally used separately but can be used together to achieve very high angular resolution. The four separate optical telescopes are known as Antu, Kueyen, Melipal and Yepun, which are all words for astronomical objects in the Mapuche language, with optical elements that can combine them into an astronomical interferometer (VLTI), which is used to resolve small objects. The interferometer is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture.
The 8.2m diameter Unit Telescopes can also be used individually. With one such telescope, images of celestial objects as faint as magnitude 30 can be obtained in a one-hour exposure. This corresponds to seeing objects that are four billion (four thousand million) times fainter than what can be seen with the unaided eye. The telescopes can work together, to form a giant ‘interferometer’, the ESO Very Large Telescope Interferometer, allowing astronomers to see details up to 25 times finer than with the individual telescopes. The light beams are combined in the VLTI using a complex system of mirrors in underground tunnels where the light paths must be kept equal to distances less than 1/1000 mm over a hundred metres. With this kind of precision the VLTI can reconstruct images with an angular resolution of milliarcseconds, equivalent to distinguishing the two headlights of a car at the distance of the Moon.
Image taken taken in 17/10/2015 from Cerro Paranal, Atacama desert, Chile.
View to the top of Cerro Paranal
Panoramic view from VISTA telescope to the top of Cerro Paranal, where it is located the VLT. In the right side we can see the Milky Way behind a dark band of clouds. The Very Large Telescope (VLT) is a telescope operated by the ESO – European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT is the world’s most advanced optical instrument, consisting of four Unit Telescopes with main mirrors of 8.2m diameter, which are generally used separately but can be used together to achieve very high angular resolution. The four separate optical telescopes are known as Antu, Kueyen, Melipal and Yepun, which are all words for astronomical objects in the Mapuche language, with optical elements that can combine them into an astronomical interferometer (VLTI), which is used to resolve small objects. The interferometer is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture.
Image taken taken in 17/10/2015 from Cerro Paranal, Atacama desert, Chile.
Testing ALMA Band Receiver in Laboratory
This picture shows an electronic engineer while is photographing the components in one of the Band receivers cartridges built for the Atacama Large Millimeter/submillimeter Array (ALMA), one of the most sensitive and expensive parts of the Antennas. Extremely weak signals from space are collected by the ALMA antennas and focussed onto the receivers, which transform the faint radiation into an electrical signal. Before its construction is even completed, the new ALMA (Atacama Large Millimeter/submillimeter Array) telescope has embarked on an upgrade that will help astronomers investigate the earliest galaxies and search for water in other planetary systems, designing and building of an additional set of receivers with state-of-the-art performance, which will enable the telescope to access a portion of the spectrum of light that it cannot currently study. ALMA observes the Universe in radio waves: light which is invisible to our eyes. The weak glow coming from space is collected by the ALMA antennas and focused onto the receivers that transform the feeble radiation into an electrical signal. ALMA has 10 receiver bands to cover a wide range of observing frequency. For more effective reception of different bands of frequency, dedicated receivers have been developed for each band. The new receivers will be able to detect electromagnetic radiation with wavelengths between about 1.4 and 1.8 millimeters, one of the ranges of the spectrum to which Earth’s atmosphere is partially transparent, which allows the light to reach the ALMA antennas. These wavelengths correspond to radio frequencies between 163 and 211 Gigahertz. ALMA has reached a major milestone by extending its vision fully into the realm of the submillimetre, the wavelengths of cosmic light that hold intriguing information about the cold, dark, and distant Universe. Image taken in 14/10/2016 at the ALMA Operations Support Facility, close to San Pedro de Atacama in northern Chile.
Image taken taken in 14/10/2015 from ALMA Operations Support Facility, Atacama desert, Chile.
VISTA Telescope Startrail
A startrail in a cloudy sky as seen above the VISTA telescope in Paranal. VISTA ― the Visible and Infrared Survey Telescope for Astronomy ― is part of ESO’s Paranal Observatory. VISTA works at near-infrared wavelengths and is the world’s largest survey telescope. Its large mirror, wide field of view and very sensitive detectors are revealing a completely new view of the southern sky. The telescope is housed on the peak adjacent to the one hosting the ESO Very Large Telescope (VLT) and shares the same exceptional observing conditions. VISTA has a main mirror that is 4.1 meters across. In photographic terms it can be thought of as a 67 megapixel digital camera with a 13 000 mm f/3.25 mirror lens. At the heart of the telescope is a huge three-tonne camera with 16 state-of-the-art infrared-sensitive detectors.
Imagem taken in 17/10/2015 from Cerro Paranal, Atacama desert, Chile.