Y-band Imaging of Extragalatic Fields and High redshift
... Red line is SF galaxy evolution and blue line represents QSOs as z goes higher ...
... Red line is SF galaxy evolution and blue line represents QSOs as z goes higher ...
Closed Loop Performance
... At 1000 Hz closed loop we can achieve 65 nm rms error in tower ~95nm “on-sky”. NOTE that this is a linear stretch. This is much better than the 190 nm rms ...
... At 1000 Hz closed loop we can achieve 65 nm rms error in tower ~95nm “on-sky”. NOTE that this is a linear stretch. This is much better than the 190 nm rms ...
Document
... scales of the order of the inverse optical bandwidth. For instance, with the very narrow band pass of 1 A (0.1 nm) in the visible, through a definite polarization state, typical time scales are 10-11 seconds (10 picoseconds). However, the photon flux is very weak even from bright stars, so that onl ...
... scales of the order of the inverse optical bandwidth. For instance, with the very narrow band pass of 1 A (0.1 nm) in the visible, through a definite polarization state, typical time scales are 10-11 seconds (10 picoseconds). However, the photon flux is very weak even from bright stars, so that onl ...
telescopes - NPZ Optics
... When buying the telescope inspect the package to make sure that the original packaging is in good condition, and seals are not broken or missing. Having opened the package, check the presence of all components described in inventory list. Read instruction manual first before using the telescope. ...
... When buying the telescope inspect the package to make sure that the original packaging is in good condition, and seals are not broken or missing. Having opened the package, check the presence of all components described in inventory list. Read instruction manual first before using the telescope. ...
The Cook Memorial Library
... eyepiece. Now, turn the EZ Finder on and look through it. The object will appear in the field of view near the red dot. If the red dot is centered on the object in the eyepiece, you’re done! If not: Without moving the telescope, use the EZ Finder’s left/right (azimuth) and up/down (altitude) adjustm ...
... eyepiece. Now, turn the EZ Finder on and look through it. The object will appear in the field of view near the red dot. If the red dot is centered on the object in the eyepiece, you’re done! If not: Without moving the telescope, use the EZ Finder’s left/right (azimuth) and up/down (altitude) adjustm ...
ASTRO2010 SCIENCE WHITE PAPER
... motion, line width provides location in disk around RW Aur A (Knez et al. 2007). sensitivity is achieved when the resolution element matches the line width, but in the (background-limited) mid-IR region, higher-resolution observations can be binned to maximize the sensitivity. Secondly, because most ...
... motion, line width provides location in disk around RW Aur A (Knez et al. 2007). sensitivity is achieved when the resolution element matches the line width, but in the (background-limited) mid-IR region, higher-resolution observations can be binned to maximize the sensitivity. Secondly, because most ...
Data reduction strategies for lucky imaging
... produce time evolving short exposure images, oversampled at 8 times the Nyquist rate and sampled at 0.01 second intervals. Custom code was then used to rebin the images to represent Nyquist rate pixel spacing and realistic exposure times before the stochastic processes of photon arrival and detector ...
... produce time evolving short exposure images, oversampled at 8 times the Nyquist rate and sampled at 0.01 second intervals. Custom code was then used to rebin the images to represent Nyquist rate pixel spacing and realistic exposure times before the stochastic processes of photon arrival and detector ...
Slide 1 - Caltech Optical Observatories
... Operating at S/N less than one becomes possible, giving theoretically optimum performance through cloud fades, etc. Note that atmospheric transmission in LGS is round-trip, and is the square of the NGS one-way transmission. Operating with large background becomes possible – companions of bright obje ...
... Operating at S/N less than one becomes possible, giving theoretically optimum performance through cloud fades, etc. Note that atmospheric transmission in LGS is round-trip, and is the square of the NGS one-way transmission. Operating with large background becomes possible – companions of bright obje ...
DSSI at DCT: Superearth Validation with High
... Abstract: We will be bringing the Differential Speckle Survey Instrument (DSSI), a speckle camera, to Lowell Observatory's 4.3-m Discovery Channel Telescope (DCT) in March of 2014. DSSI will be employed in high-angular resolution work for the Kepler Follow-up Program; at the shortest wavelengths of ...
... Abstract: We will be bringing the Differential Speckle Survey Instrument (DSSI), a speckle camera, to Lowell Observatory's 4.3-m Discovery Channel Telescope (DCT) in March of 2014. DSSI will be employed in high-angular resolution work for the Kepler Follow-up Program; at the shortest wavelengths of ...
Spokane Public Library The Spokane Astronomical
... “Seeing” and Transparency: Atmospheric conditions vary significantly from night to night. “Seeing” refers to the steadiness of the Earth’s atmosphere at a given time. In conditions of poor seeing, atmospheric turbulence causes objects viewed through the telescope to “boil”. In conditions of good see ...
... “Seeing” and Transparency: Atmospheric conditions vary significantly from night to night. “Seeing” refers to the steadiness of the Earth’s atmosphere at a given time. In conditions of poor seeing, atmospheric turbulence causes objects viewed through the telescope to “boil”. In conditions of good see ...
5th
... The degree of brightness of a star or other object in the sky according to a scale on which the brightest star has a magnitude -1.4 and the faintest visible star has magnitude 6. Sometimes referred to as apparent magnitude. In this scale, each number is 2.5 times the brightness of the previous numbe ...
... The degree of brightness of a star or other object in the sky according to a scale on which the brightest star has a magnitude -1.4 and the faintest visible star has magnitude 6. Sometimes referred to as apparent magnitude. In this scale, each number is 2.5 times the brightness of the previous numbe ...
o - Salem State University
... 1.Let's say we find a star that is located on the following points or circles in the sky. Then, on the same night we move to a location on Earth that is some significant distance from our first location. There will now be a different star at or on: a. the celestial north pole b. the zenith c. the ce ...
... 1.Let's say we find a star that is located on the following points or circles in the sky. Then, on the same night we move to a location on Earth that is some significant distance from our first location. There will now be a different star at or on: a. the celestial north pole b. the zenith c. the ce ...
Orion StarBlast 4.5” Telescope STAR Program
... you can view in this telescope at different times of the year. Deep sky objects, also referred to as dim-fuzzies, are often hard to find. They are worth the effort, being some of most wonderful sights in the night sky. To find a deep sky object, look at the monthly Evening Sky Map (www. skymaps.com) ...
... you can view in this telescope at different times of the year. Deep sky objects, also referred to as dim-fuzzies, are often hard to find. They are worth the effort, being some of most wonderful sights in the night sky. To find a deep sky object, look at the monthly Evening Sky Map (www. skymaps.com) ...
presentation - CESAR Project website
... The main objective is to train students in both general science and engineering basics providing them with firsthand experience in astronomy in an IBSE learning environment Observations allow students to learn, with first-order scientific tools, the basics of an astronomical research, aiming to arou ...
... The main objective is to train students in both general science and engineering basics providing them with firsthand experience in astronomy in an IBSE learning environment Observations allow students to learn, with first-order scientific tools, the basics of an astronomical research, aiming to arou ...
File
... to map the distribution of hydrogen in the Milky Way galaxy. This is how they learned that the shape of our galaxy is a spiral. Radio waves have wavelengths that are millions of times longer than light waves, meaning that these waves give less resolution, but can penetrate dust clouds in the galaxy, ...
... to map the distribution of hydrogen in the Milky Way galaxy. This is how they learned that the shape of our galaxy is a spiral. Radio waves have wavelengths that are millions of times longer than light waves, meaning that these waves give less resolution, but can penetrate dust clouds in the galaxy, ...
Chapter 24 Studying the Sun Section 1 The Study of Light Key
... As you might guess, it’s a huge task to produce a large piece of high-quality, bubble-free glass for refracting telescopes. Most large optical telescopes are reflectors. Light does not pass through a mirror so the glass for a reflecting telescope does not have to be of optical quality. In addition, ...
... As you might guess, it’s a huge task to produce a large piece of high-quality, bubble-free glass for refracting telescopes. Most large optical telescopes are reflectors. Light does not pass through a mirror so the glass for a reflecting telescope does not have to be of optical quality. In addition, ...
OBJXlab-JCU_Alt
... light that falls on a small slit in the image plane of the telescope and uses a grating to spread the light out into a spectrum, a graph of intensity versus wavelength. The longer you expose the spectrum, the clear and more detailed it the graph will be. The intensity and wavelengths of points on th ...
... light that falls on a small slit in the image plane of the telescope and uses a grating to spread the light out into a spectrum, a graph of intensity versus wavelength. The longer you expose the spectrum, the clear and more detailed it the graph will be. The intensity and wavelengths of points on th ...
Title: Optical and NEar IR Interferometric or
... that an adaptive system such as the one envisaged for LBT, with a single artificial star and a single corrector, can achieve excellent correction (Strehl ratio of about 0.5 in the K band) over a large fraction of the sky. Both, quality of correction and sky coverage drop unfortunately going to shor ...
... that an adaptive system such as the one envisaged for LBT, with a single artificial star and a single corrector, can achieve excellent correction (Strehl ratio of about 0.5 in the K band) over a large fraction of the sky. Both, quality of correction and sky coverage drop unfortunately going to shor ...
Here
... 1.1 Preparing astronomical observations 1.2 Carrying out the observations 1.3 Data reduction and analysis 1.1 Preparing astronomical observations In order to use the telescope and its instrument (a CCD camera) you need first to get familiar with its use. This will be done at the beginning of your ob ...
... 1.1 Preparing astronomical observations 1.2 Carrying out the observations 1.3 Data reduction and analysis 1.1 Preparing astronomical observations In order to use the telescope and its instrument (a CCD camera) you need first to get familiar with its use. This will be done at the beginning of your ob ...
Telescopes: More Than Meets the Eye
... Magnification is by far the best known of these three functions, but it really is the least important. Most objects in space are so far away that no matter how much you magnify them, they still look pretty much the same, the only difference is they get dimmer. What really allows you to see more dist ...
... Magnification is by far the best known of these three functions, but it really is the least important. Most objects in space are so far away that no matter how much you magnify them, they still look pretty much the same, the only difference is they get dimmer. What really allows you to see more dist ...
Explores Angular Size - Chandra X
... Astronomers measure the sizes of objects in the sky in terms of their angular size. For instance, the moon appears to be about 1/2 degree in diameter. The planet Venus, when it is closest to Earth, appears to be even smaller - only about 1/60 of a degree. This small angle is called the arc-minute. T ...
... Astronomers measure the sizes of objects in the sky in terms of their angular size. For instance, the moon appears to be about 1/2 degree in diameter. The planet Venus, when it is closest to Earth, appears to be even smaller - only about 1/60 of a degree. This small angle is called the arc-minute. T ...
Document
... • SkyTools uses a scientific model of your camera, optics, location, atmospheric conditions, light pollution and target object • The model estimates the final Signal to Noise Ratio (SNR) for the image or image stack • The goal is to maximize SNR by making the best informed choices (where and when to ...
... • SkyTools uses a scientific model of your camera, optics, location, atmospheric conditions, light pollution and target object • The model estimates the final Signal to Noise Ratio (SNR) for the image or image stack • The goal is to maximize SNR by making the best informed choices (where and when to ...
Bad Astronomy - Eastbay Astronomical Society
... a part of such a great program to educate people about highenergy astronomy. Let me state here that I am not a NASA employee, and anything I say, pretty much ever, is not the official word from NASA! I always speak for no one but myself. I received my PhD in astronomy at the University of Virginia i ...
... a part of such a great program to educate people about highenergy astronomy. Let me state here that I am not a NASA employee, and anything I say, pretty much ever, is not the official word from NASA! I always speak for no one but myself. I received my PhD in astronomy at the University of Virginia i ...
the printable Hartness House Workshop Schedule in pdf
... many thousands of short exposure images, sorting them by quality, aligning and stacking them and then enhancing faint details of the image by wavelet analysis. Inexpensive digital video cameras used as webcams, surveillance cameras, and machine vision cameras are used for this purpose. Proper optica ...
... many thousands of short exposure images, sorting them by quality, aligning and stacking them and then enhancing faint details of the image by wavelet analysis. Inexpensive digital video cameras used as webcams, surveillance cameras, and machine vision cameras are used for this purpose. Proper optica ...
Draft Science Cases for KPAO
... would have to have this error added quadratically (so Subaru’s C188 residual phase due to fitting and cone effect errors would be 190nm r.m.s. – SR=8%, SH=57%, SK=75%). So it is quite clear that in LGS mode, only a system using multiple guide stars, such as KPAO will be able to provide diffraction-l ...
... would have to have this error added quadratically (so Subaru’s C188 residual phase due to fitting and cone effect errors would be 190nm r.m.s. – SR=8%, SH=57%, SK=75%). So it is quite clear that in LGS mode, only a system using multiple guide stars, such as KPAO will be able to provide diffraction-l ...
Astronomical seeing
Astronomical seeing refers to the blurring and twinkling of astronomical objects such as stars caused by turbulent mixing in the Earth's atmosphere varying the optical refractive index. The astronomical seeing conditions on a given night at a given location describe how much the Earth's atmosphere perturbs the images of stars as seen through a telescope.The most common seeing measurement is the diameter (or more correctly the full width at half maximum or FWHM) of the optical intensity across the seeing disc (the point spread function for imaging through the atmosphere). The FWHM of the point spread function (loosely called seeing disc diameter or ""seeing"") is a reference to the best possible angular resolution which can be achieved by an optical telescope in a long photographic exposure, and corresponds to the FWHM of the fuzzy blob seen when observing a point-like source (such as a star) through the atmosphere. The size of the seeing disc is determined by the astronomical seeing conditions at the time of the observation. The best conditions give a seeing disk diameter of ~0.4 arcseconds and are found at high-altitude observatories on small islands such as Mauna Kea or La Palma.Seeing is one of the biggest problems for Earth-based astronomy: while the big telescopes have theoretically milli-arcsecond resolution, the real image will never be better than the average seeing disc during the observation. This can easily mean a factor of 100 between the potential and practical resolution. Starting in the 1990s, new adaptive optics have been introduced that can help correct for these effects, dramatically improving the resolution of ground based telescopes.