The 1.5 meter solar telescope GREGOR
... since the outer atmosphere is probed with very strong spectral lines with line-core intensities of a tenth or less of the photospheric intensity. For a high photometric accuracy, sufficient photon flux is needed. Compared to the 70 cm VTT, GREGOR will provide a substantial increase in photon flux an ...
... since the outer atmosphere is probed with very strong spectral lines with line-core intensities of a tenth or less of the photospheric intensity. For a high photometric accuracy, sufficient photon flux is needed. Compared to the 70 cm VTT, GREGOR will provide a substantial increase in photon flux an ...
CSU Remote Telescope - Education Services Australia
... Prime focus camera for magnified views, eyepiece. This is the SX camera. ...
... Prime focus camera for magnified views, eyepiece. This is the SX camera. ...
Topic 5 - Holy Cross Collegiate
... radio sources. Radio telescopes cannot “see” radio sources. In the early days of professional radio astronomy, the movement of dials and needles monitored the incoming radio waves. The needle is similar to the kind you see in an ammeter or voltmeter. Astronomers then graphed the data. Today, compute ...
... radio sources. Radio telescopes cannot “see” radio sources. In the early days of professional radio astronomy, the movement of dials and needles monitored the incoming radio waves. The needle is similar to the kind you see in an ammeter or voltmeter. Astronomers then graphed the data. Today, compute ...
Astronomical Techniques Course
... 14) A star of certain brightness is observed with HCT for 30min. exposure time. The resultant image has S/N= 60. How large aperture is need to attain S/N=200 with the same set-up? 15.) When does the Sun reaches closest to the Polaris and what is the angle between them? ...
... 14) A star of certain brightness is observed with HCT for 30min. exposure time. The resultant image has S/N= 60. How large aperture is need to attain S/N=200 with the same set-up? 15.) When does the Sun reaches closest to the Polaris and what is the angle between them? ...
4242 MR304SC Spec.indd
... 23.5 cm/s, fixed Scan rate 82 spectra per second at 16 cm-1 apodized resolution FOV of interferometer 45 mrad (without input collimator or telescope) Maximum optical throughput 8.1 x 10-3 cm2 sr Detectors InSb: 1,800-5,000 cm-1 (2-5.5 μm) MCT: 667-2,500 cm-1 (4-15 μm) Detector cooling Stirling cryoco ...
... 23.5 cm/s, fixed Scan rate 82 spectra per second at 16 cm-1 apodized resolution FOV of interferometer 45 mrad (without input collimator or telescope) Maximum optical throughput 8.1 x 10-3 cm2 sr Detectors InSb: 1,800-5,000 cm-1 (2-5.5 μm) MCT: 667-2,500 cm-1 (4-15 μm) Detector cooling Stirling cryoco ...
BlackHoleintheCenter..
... These stars are spiraling around the black hole at speeds of up to three million miles per hour-about 10 times the speed at which stars typically move. In order to account for the rapid speeds of these stars, Ghez determined that an object 2.6 million times more massive than our Sun must be concentr ...
... These stars are spiraling around the black hole at speeds of up to three million miles per hour-about 10 times the speed at which stars typically move. In order to account for the rapid speeds of these stars, Ghez determined that an object 2.6 million times more massive than our Sun must be concentr ...
1 GS106 Lab 3 Answer Key - How We Use Light in Astronomy Pre
... atmosphere, to your skin. The wave energy excites the electrons in the cell tissue of your skin, which in turn excites the nerve endings in your body, and tells your brain "ouch, that's hot!" Tuning Fork Experiment: the vibrational mechanical "sound" energy is transfered via wave transmission from o ...
... atmosphere, to your skin. The wave energy excites the electrons in the cell tissue of your skin, which in turn excites the nerve endings in your body, and tells your brain "ouch, that's hot!" Tuning Fork Experiment: the vibrational mechanical "sound" energy is transfered via wave transmission from o ...
Tipp2011VerUpgrade
... • Creates shower in upper atmosphere • Secondary pairs emit Cherenkov radiation • Large light pool area: Aeff ~105m2 • Shower imaged in multi-PMT Cameras at telescope focus ...
... • Creates shower in upper atmosphere • Secondary pairs emit Cherenkov radiation • Large light pool area: Aeff ~105m2 • Shower imaged in multi-PMT Cameras at telescope focus ...
What does the universe look like? - Harvard
... Why can't I see the individual stars in the galaxies that I've imaged? At the scale of your image, each individual star in the galaxy would be smaller than a single atom! It is truly amazing that the combined light of the stars can form the beautiful galaxy images you have created. Why do the galax ...
... Why can't I see the individual stars in the galaxies that I've imaged? At the scale of your image, each individual star in the galaxy would be smaller than a single atom! It is truly amazing that the combined light of the stars can form the beautiful galaxy images you have created. Why do the galax ...
Answer Choices
... on_Nebula,_X_ray_and_Infrared.jpg These objects emit infrared radiation which can be detected with infrared telescopes. This is an infrared image of the Sombrero galaxy. ...
... on_Nebula,_X_ray_and_Infrared.jpg These objects emit infrared radiation which can be detected with infrared telescopes. This is an infrared image of the Sombrero galaxy. ...
YAAYS_M57_poster
... students, teachers, and scientists at Yerkes Observatory. We have identified archival Hubble Space Telescope (HST) observations of the Ring Nebula (NGC 6720 or M57) for an initial exercise in the emerging field of astronomical data mining and curation. The multi-wavelength images of this object with ...
... students, teachers, and scientists at Yerkes Observatory. We have identified archival Hubble Space Telescope (HST) observations of the Ring Nebula (NGC 6720 or M57) for an initial exercise in the emerging field of astronomical data mining and curation. The multi-wavelength images of this object with ...
gunclubscope
... We have established the fact that the telescope on the Rocky Mountains was not the right instrument to follow the travel of the 9-ft cannon ball toward the Moon. It was out of the possibilities of the instrument to see such a little object, notwithstanding the tremendous enlarging power employed. Ab ...
... We have established the fact that the telescope on the Rocky Mountains was not the right instrument to follow the travel of the 9-ft cannon ball toward the Moon. It was out of the possibilities of the instrument to see such a little object, notwithstanding the tremendous enlarging power employed. Ab ...
Transit of TrES-2 b
... χ2 test compares a null hypothesis to an alternative hypothesis. Depending on where the test statistic lies on the χ2k distribution curve, we either accept or reject the null hypothesis. If the test statistic is greater than the χ2k value, then we reject the null hypothesis.4 To show if TrES-2 is va ...
... χ2 test compares a null hypothesis to an alternative hypothesis. Depending on where the test statistic lies on the χ2k distribution curve, we either accept or reject the null hypothesis. If the test statistic is greater than the χ2k value, then we reject the null hypothesis.4 To show if TrES-2 is va ...
here - IPAC
... Massachusetts and Caltech’s Infrared Processing and Analysis Center, imaged the entire sky in the nearinfrared 1-2.2 m window using ground-based telescopes in Arizona (northern hemisphere) and Chile (southern hemisphere). The survey was optimally designed to detect and measure the brightness of sta ...
... Massachusetts and Caltech’s Infrared Processing and Analysis Center, imaged the entire sky in the nearinfrared 1-2.2 m window using ground-based telescopes in Arizona (northern hemisphere) and Chile (southern hemisphere). The survey was optimally designed to detect and measure the brightness of sta ...
Student Project - Ott Planetarium
... This camera will be used to study dark matter and dark energy, two of the greatest mysteries of the Universe. The Cosmic Origins Spectograph (COS), also new, uses the ultraviolet range, and will be used to determine the composition of the universe. Hubble also has an Advanced Camera for Surveys (ACS ...
... This camera will be used to study dark matter and dark energy, two of the greatest mysteries of the Universe. The Cosmic Origins Spectograph (COS), also new, uses the ultraviolet range, and will be used to determine the composition of the universe. Hubble also has an Advanced Camera for Surveys (ACS ...
Speckle-Averaging Phase Conjugative Adaptive Optics
... turbulences in the optical path of an optical setup. Typical for such a system is e.g. an astronomical telescope where a laser beam is used to produce a laser beacon on the sky and the returned light from this beacon is picked up by the telescope and the phase aberrations then measured by a wavefron ...
... turbulences in the optical path of an optical setup. Typical for such a system is e.g. an astronomical telescope where a laser beam is used to produce a laser beacon on the sky and the returned light from this beacon is picked up by the telescope and the phase aberrations then measured by a wavefron ...
Towards the Intensity Interferometry Stellar Imaging System
... to image hot stars (typical diameters < 1 mas) SAI would need considerably longer baselines, and would need to operate in the visible (difficult) or blue (very difficult). Intensity interferometry is well matched to blue/visible operation, and scales to long baselines with ease (the atmospheric stab ...
... to image hot stars (typical diameters < 1 mas) SAI would need considerably longer baselines, and would need to operate in the visible (difficult) or blue (very difficult). Intensity interferometry is well matched to blue/visible operation, and scales to long baselines with ease (the atmospheric stab ...
equipment introduction
... Purpose: The purpose of this lab is to begin to familiarize you with the sky, the telescopes, making and recording observations, and angular measurements, all of which you use throughout the rest of the semester. This lab involves several different kinds of tasks, most of which will center around th ...
... Purpose: The purpose of this lab is to begin to familiarize you with the sky, the telescopes, making and recording observations, and angular measurements, all of which you use throughout the rest of the semester. This lab involves several different kinds of tasks, most of which will center around th ...
EUVE Measurements of Interplanetary Helium
... Adaptive optics tutorial* Turbulence in earth’s atmosphere makes stars twinkle More importantly, turbulence spreads out light; makes it a blob rather than a point *Adapted from AO lectures of Claire Max, Astro 289C, UC Santa Cruz ...
... Adaptive optics tutorial* Turbulence in earth’s atmosphere makes stars twinkle More importantly, turbulence spreads out light; makes it a blob rather than a point *Adapted from AO lectures of Claire Max, Astro 289C, UC Santa Cruz ...
Edwin Hubble
... Hubble’s Law Continued • In other words: – he showed that galaxies are moving away from us with a speed proportional to their distance – Aka: the Universe is expanding ...
... Hubble’s Law Continued • In other words: – he showed that galaxies are moving away from us with a speed proportional to their distance – Aka: the Universe is expanding ...
The Radio Jets of AGN
... Active Galactic Nuclei (AGN): extremely compact, generate much more energy than a normal galaxy. Activity due to accretion onto a supermassive (~109 solar masses! ) black hole Sometimes eject “jets” of radio-emitting plasma extending far beyond optical (visible) galaxy. ...
... Active Galactic Nuclei (AGN): extremely compact, generate much more energy than a normal galaxy. Activity due to accretion onto a supermassive (~109 solar masses! ) black hole Sometimes eject “jets” of radio-emitting plasma extending far beyond optical (visible) galaxy. ...
Very Large Telescope
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The Very Large Telescope (VLT) is a telescope operated by the European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT consists of four individual telescopes, each with a primary mirror 8.2 m across, 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. The telescopes form an array which is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture.The VLT operates at visible and infrared wavelengths. Each individual telescope can detect objects roughly four billion times fainter than can be detected with the naked eye, and when all the telescopes are combined, the facility can achieve an angular resolution of about 0.001 arc-second (This is equivalent to roughly 2 meters resolution at the distance of the Moon).In single telescope mode of operation angular resolution is about 0.05 arc-second.The VLT is the most productive ground-based facility for astronomy, with only the Hubble Space Telescope generating more scientific papers among facilities operating at visible wavelengths. Among the pioneering observations carried out using the VLT are the first direct image of an exoplanet, the tracking of individual stars moving around the supermassive black hole at the centre of the Milky Way, and observations of the afterglow of the furthest known gamma-ray burst.