The achromatic design of an atmospheric dispersion corrector for
... aberrations of L1 and L2. It is worth pointing out that in contrast to linear ADCs, the proposed ADC does not use any tilt or decentering of M3, M4 and M5. The diameter of the largest lens covering the 10-arcmin full technical field is less than 780 mm and the total length of the ADC is less than 85 ...
... aberrations of L1 and L2. It is worth pointing out that in contrast to linear ADCs, the proposed ADC does not use any tilt or decentering of M3, M4 and M5. The diameter of the largest lens covering the 10-arcmin full technical field is less than 780 mm and the total length of the ADC is less than 85 ...
LaPalma_telescopes_2008
... design, this leads to acceptable image quality and is widely used in smaller telescopes For larger apertures a shorter focal ratio is essential and the field of tolerable aberration becomes very small Large telescopes, if they have a prime focus, need correctors (more later). Hyperbolic primaries ca ...
... design, this leads to acceptable image quality and is widely used in smaller telescopes For larger apertures a shorter focal ratio is essential and the field of tolerable aberration becomes very small Large telescopes, if they have a prime focus, need correctors (more later). Hyperbolic primaries ca ...
Differential measurement of atmospheric
... an all-reflecting Schmidt one and consists of three mirrors: a beam combiner, a flat-folding mirror and a spherical primary mirror, as shown in figure 2. The beam combiner is made from a polished zerodur blank, cut into two halves and reassembled with a wedge angle of 29 degree. The star light from two ...
... an all-reflecting Schmidt one and consists of three mirrors: a beam combiner, a flat-folding mirror and a spherical primary mirror, as shown in figure 2. The beam combiner is made from a polished zerodur blank, cut into two halves and reassembled with a wedge angle of 29 degree. The star light from two ...
2014 - Society for Astronomical Sciences
... SN 2014G also had competition for limited observing resources because in January 2014 SN 2014G was shortly followed by SN 2014J in M82, a nearby Type Ia with potential to help calibrate the cosmic distance scale. As expected, SN 2014J attracted a good deal of the finite attention and resources devot ...
... SN 2014G also had competition for limited observing resources because in January 2014 SN 2014G was shortly followed by SN 2014J in M82, a nearby Type Ia with potential to help calibrate the cosmic distance scale. As expected, SN 2014J attracted a good deal of the finite attention and resources devot ...
Miniaturized Shack-Hartmann Wavefront-Sensors for Starbugs
... atmospheric turbulence to maximize telescope efficiency. Recent techniques such as Multi-Object Adaptive Optics (MOAO) [2] have increased the need for multiple wavefront sensors placed at the focal plane. Positioning of these devices to within the accuracy and time constraints is a challenging probl ...
... atmospheric turbulence to maximize telescope efficiency. Recent techniques such as Multi-Object Adaptive Optics (MOAO) [2] have increased the need for multiple wavefront sensors placed at the focal plane. Positioning of these devices to within the accuracy and time constraints is a challenging probl ...
Document
... • I will expect you to do the reading BEFORE class • Then if you want, go back and read more deeply after the lecture, to resolve areas which seem confusing • From time to time I will give small “Reading Quizzes” at the start of a class, where I ask three questions that you’ll be able to answer easi ...
... • I will expect you to do the reading BEFORE class • Then if you want, go back and read more deeply after the lecture, to resolve areas which seem confusing • From time to time I will give small “Reading Quizzes” at the start of a class, where I ask three questions that you’ll be able to answer easi ...
astronomical eyepieces - Amateur Astronomers Association Delhi
... are also known as ocular lens. Eyepiece is used to magnify the image formed by objective lens or mirror of the telescope. Eyepieces are specified by their focal length, apparent field of view (FOV). These parameters can be used to derive any other information required. Magnification that an eyepiece ...
... are also known as ocular lens. Eyepiece is used to magnify the image formed by objective lens or mirror of the telescope. Eyepieces are specified by their focal length, apparent field of view (FOV). These parameters can be used to derive any other information required. Magnification that an eyepiece ...
The COMPLETE Survey of Star-Forming Regions
... resolution8 to a depth of about 5 magnitudes AV (see Figure 2, below.). 2. The NASA SIRTF Legacy project, “From Molecular Cores to Planet-forming Disks” (Neal Evans, PI), will spend hundreds of hours of SIRTF time (in ~2003) mapping out five molecular cloud complexes in far-infrared emission and tak ...
... resolution8 to a depth of about 5 magnitudes AV (see Figure 2, below.). 2. The NASA SIRTF Legacy project, “From Molecular Cores to Planet-forming Disks” (Neal Evans, PI), will spend hundreds of hours of SIRTF time (in ~2003) mapping out five molecular cloud complexes in far-infrared emission and tak ...
Concept and performance of multiple laser guide stars for 8-m
... considered as the next generation of A0 systems for 8-m telescopes and represents a necessary intermediate step toward A0 systems for Extremely Large Telescopes. Multiple guide stars allow to correct the cone effect which affects single LGS systems and prevents from going to wavelengths shorter than ...
... considered as the next generation of A0 systems for 8-m telescopes and represents a necessary intermediate step toward A0 systems for Extremely Large Telescopes. Multiple guide stars allow to correct the cone effect which affects single LGS systems and prevents from going to wavelengths shorter than ...
The last gasps of VY CMa: Aperture synthesis and adaptive optics
... each image frame represents the FWHM of the central component as displayed, 30 mas for the 1.65 µm and 2.26 µm images and 40 mas for the 3.08 µm observations. In addition to eliminating spurious features in the reconstructions as judged by internal consistency from multiple data sets, this process a ...
... each image frame represents the FWHM of the central component as displayed, 30 mas for the 1.65 µm and 2.26 µm images and 40 mas for the 3.08 µm observations. In addition to eliminating spurious features in the reconstructions as judged by internal consistency from multiple data sets, this process a ...
Optical interferometry in astronomy
... at average observing sites and hence even small telescopes cannot be used at their diffractionlimit in the visible. In such cases, the observed angular size of a point-source will be determined entirely by r0 (λ) at a given wavelength, and is known as the seeing disc size, seeing (λ). The Kolmogoro ...
... at average observing sites and hence even small telescopes cannot be used at their diffractionlimit in the visible. In such cases, the observed angular size of a point-source will be determined entirely by r0 (λ) at a given wavelength, and is known as the seeing disc size, seeing (λ). The Kolmogoro ...
9. Telescope structure and kinematics
... achievable limits of structural eigen-frequencies impose that image stabilisation be implemented downstream in the optical train. The mechanical structure shall be seen as a “skeleton”, which supports all the sub-systems of the telescope. The demonstration of its feasibility is therefore one of the ...
... achievable limits of structural eigen-frequencies impose that image stabilisation be implemented downstream in the optical train. The mechanical structure shall be seen as a “skeleton”, which supports all the sub-systems of the telescope. The demonstration of its feasibility is therefore one of the ...
Night-time image quality at Roque de los Muchachos Observatory
... Seeing is referred to zenith taking into account the appropriate air-mass correction, the zenithal angle being small (≤ 30◦ ). FWHM is accurate to better than 0.100 and, under reasonably good conditions it is possible to monitor the seeing with a temporal sampling rate of less than half a minute for ...
... Seeing is referred to zenith taking into account the appropriate air-mass correction, the zenithal angle being small (≤ 30◦ ). FWHM is accurate to better than 0.100 and, under reasonably good conditions it is possible to monitor the seeing with a temporal sampling rate of less than half a minute for ...
than a one-hit wonder. Falk, Dan Astronomy
... viewer to alternate quickly between two plates, each of them aligned so the star images remain in the same apparent position. The task was, to say the least, daunting. Each plate -- even those from star fields far from the Milky Way -- had at least 40,000 star images. Even the least-heavily populate ...
... viewer to alternate quickly between two plates, each of them aligned so the star images remain in the same apparent position. The task was, to say the least, daunting. Each plate -- even those from star fields far from the Milky Way -- had at least 40,000 star images. Even the least-heavily populate ...
Measurement of the Polarization of the Cosmic Microwave Background Byron J. Philhour
... Measurement of cosmic microwave background (CMB) polarization will provide a powerful check on the model that describes CMB ∆T fluctuations as arising from density fluctuations in the early universe, break degeneracies between cosmological parameters that arise in interpreting ∆T fluctuations, and m ...
... Measurement of cosmic microwave background (CMB) polarization will provide a powerful check on the model that describes CMB ∆T fluctuations as arising from density fluctuations in the early universe, break degeneracies between cosmological parameters that arise in interpreting ∆T fluctuations, and m ...
Galileo, my first term paper
... turned his telescope on the night sky and began to make remarkable discoveries. In about two months he made more discoveries that changed the world than anyone has ever made before or since. ...
... turned his telescope on the night sky and began to make remarkable discoveries. In about two months he made more discoveries that changed the world than anyone has ever made before or since. ...
Slide 1
... Numbers Using Backbones Leif Svalgaard Stanford University 5th Space Climate Symposium, Oulu, 2013 The ratio between Group SSN and Wolf [Zürich, International] SSN has a marked discontinuity ~1882: ...
... Numbers Using Backbones Leif Svalgaard Stanford University 5th Space Climate Symposium, Oulu, 2013 The ratio between Group SSN and Wolf [Zürich, International] SSN has a marked discontinuity ~1882: ...
Full Presentation Here
... • Precise Measurement of the GRH lead to a new technique to measure m and – Independent from other techniques currently used. – No standard-candle ( but uniform and isotropic EBL ) – Active Galactic Nuclei highest observable redshift • The precision of this technique is dominated by the system ...
... • Precise Measurement of the GRH lead to a new technique to measure m and – Independent from other techniques currently used. – No standard-candle ( but uniform and isotropic EBL ) – Active Galactic Nuclei highest observable redshift • The precision of this technique is dominated by the system ...
Parallax - Georgia State University
... This is done by “Dependencies” (D), which contain all the rotation, translation and scaling necessary to place each reference star in each frame where it's supposed to be. These look nasty. The position of the target star is calculated based on the average of these dependencies. ...
... This is done by “Dependencies” (D), which contain all the rotation, translation and scaling necessary to place each reference star in each frame where it's supposed to be. These look nasty. The position of the target star is calculated based on the average of these dependencies. ...
PDF only
... magnification dependent upon the diameters of convex lenses, and not on its “focal length.”9 In an attempt to shed light on how Galileo’s could have realized the correlation between the focal length of a convex lens and the magnification of the spyglass, “Conception (2)” appeals to a standard practi ...
... magnification dependent upon the diameters of convex lenses, and not on its “focal length.”9 In an attempt to shed light on how Galileo’s could have realized the correlation between the focal length of a convex lens and the magnification of the spyglass, “Conception (2)” appeals to a standard practi ...
Refereed Publications - Center for Astrophysics and Space
... Earle, L., Glenn, J., Matsuhara, H., Naylor, B.J., Nguyen, H., Yun, M, & Zmuidzinas, J. “Z-Spec: a broadband millimeter-wave grating spectrometer—design, construction, and first cryogenic measurements”. Proceedings of SPIE—The International Society for Optical Engineering conference on Millimeter an ...
... Earle, L., Glenn, J., Matsuhara, H., Naylor, B.J., Nguyen, H., Yun, M, & Zmuidzinas, J. “Z-Spec: a broadband millimeter-wave grating spectrometer—design, construction, and first cryogenic measurements”. Proceedings of SPIE—The International Society for Optical Engineering conference on Millimeter an ...
Discovery of Cluster-Scale Lensed Quasars using the Subaru
... quasars. So far we have succeeded in discovering two cluster-scale lensed quasars, SDSS J1004+4112 and SDSS J1029+2623. We used the Subaru Telescope for the discoveries and further follow-up observations of both of them. ...
... quasars. So far we have succeeded in discovering two cluster-scale lensed quasars, SDSS J1004+4112 and SDSS J1029+2623. We used the Subaru Telescope for the discoveries and further follow-up observations of both of them. ...
Project_Description2
... astronomical telescope mirrors. It is easy to deposit, has reflectance above 90% for most of the optical-UV to the near IR (although there is a significant drop in the 700-900nm region), and it develops a native layer that enables it to survive for 2-3 years before recoating is necessary. However, i ...
... astronomical telescope mirrors. It is easy to deposit, has reflectance above 90% for most of the optical-UV to the near IR (although there is a significant drop in the 700-900nm region), and it develops a native layer that enables it to survive for 2-3 years before recoating is necessary. However, i ...
DOBSONIAN TELESCOPE - Raleigh Astronomy Club
... This manual is designed to instruct you in the proper use of your Celestar telescope. The instructions are for assembly, initial use, long term operation, and maintenance. There are seven major sections to the manual. The first section covers the proper procedure for setting up your Celestar telesco ...
... This manual is designed to instruct you in the proper use of your Celestar telescope. The instructions are for assembly, initial use, long term operation, and maintenance. There are seven major sections to the manual. The first section covers the proper procedure for setting up your Celestar telesco ...
Allen Telescope Array
The Allen Telescope Array (ATA), formerly known as the One Hectare Telescope (1hT) is a radio telescope array dedicated to astronomical observations and a simultaneous Search for Extraterrestrial Intelligence (SETI). The array is situated at the Hat Creek Radio Observatory, 290 miles (470 km) northeast of San Francisco, California.Originally developed as a joint effort between the SETI Institute and the Radio Astronomy Laboratory (RAL) at the University of California, Berkeley (UC Berkley) with funds obtained from an initial US$11.5 million donation by the Paul G. Allen Family Foundation, the project completed the first phase of construction and become operational on 11 October 2007 with 42 antennas (ATA-42), after Paul Allen (co-founder of Microsoft) pledged an additional $13.5 million to support the construction of the first and second phases.Though overall Allen has contributed more than $30 million to the project, the project has not succeeded in building the 350 six metre (19.7 feet) dishes originally conceived, and suffered an operational hiatus due to funding shortfalls between April and August 2011. Subsequently, UC Berkeley exited the project, completing divestment in April 2012. The facility is now managed by SRI International (formerly Stanford Research Institute), an independent, nonprofit research institute.In August 2014 the installation was threatened by a forest fire in the area and was briefly forced to shut down, but ultimately emerged largely unscathed.