Chapter 2 – Review of length measuring interferometers
... into two. After travelling along the reference and measurement paths the beams interfere with each other and are split again. One beam is given an extra phase difference of π/4 to produce two orthogonal outputs for example by using a quarterwave plate, as in figure 2.1, or by using a specially coate ...
... into two. After travelling along the reference and measurement paths the beams interfere with each other and are split again. One beam is given an extra phase difference of π/4 to produce two orthogonal outputs for example by using a quarterwave plate, as in figure 2.1, or by using a specially coate ...
Minutes SSWG_2 - Space Astronomy Laboratory
... instrumentation contribution to SALT. This could involve any or all of the following: Prime focus instrument Fibre feed subsystem Software control system Ken expressed some concern that the total instrument budget for SALT was too low. Generally astronomical instrument costs scale with telesco ...
... instrumentation contribution to SALT. This could involve any or all of the following: Prime focus instrument Fibre feed subsystem Software control system Ken expressed some concern that the total instrument budget for SALT was too low. Generally astronomical instrument costs scale with telesco ...
ULTRA Optics - Composite Mirror Applications Inc.
... For quantifying the wave front quality of the CFRP mirrors, we used a HASO-32 Shack-Hartman wave front sensor. The instrument has a large dynamic range and is relatively insensitive to atmospheric disturbances. The number 32 corresponds to the 32 X 32 micro-lenslet array used as the Shack-Hartman ar ...
... For quantifying the wave front quality of the CFRP mirrors, we used a HASO-32 Shack-Hartman wave front sensor. The instrument has a large dynamic range and is relatively insensitive to atmospheric disturbances. The number 32 corresponds to the 32 X 32 micro-lenslet array used as the Shack-Hartman ar ...
The photometric system of the One
... 2012). The yearly average and standard deviation of seeing in the past six years were calculated and are shown as red dots in the left panel of Figure 2 (the standard deviation is represented by error bars). The seeing condition has been stable in the past six years. The small variation is probably ...
... 2012). The yearly average and standard deviation of seeing in the past six years were calculated and are shown as red dots in the left panel of Figure 2 (the standard deviation is represented by error bars). The seeing condition has been stable in the past six years. The small variation is probably ...
3.2 Offner relay design - Caltech Optical Observatories
... The zemax model was optimized simultaneously for the NGS conjugate and two LGS conjugates at 90 km and 180 km. These two sources are available concurrently through the use of a beam splitter, and were arranged such that the NGS source is in reflection. This avoids any chromatic effects in the NGS so ...
... The zemax model was optimized simultaneously for the NGS conjugate and two LGS conjugates at 90 km and 180 km. These two sources are available concurrently through the use of a beam splitter, and were arranged such that the NGS source is in reflection. This avoids any chromatic effects in the NGS so ...
STARTRACKER SYSTEM - Galileo Telescope Makers
... or more evenly illuminated, concentric rings of light. The angular size of the central disc and the spacing of the rings are functions of the telescope's aperture and central obstruction, if any. The visible extent of the disc as well as the number of the rings visible varies from a given instrument ...
... or more evenly illuminated, concentric rings of light. The angular size of the central disc and the spacing of the rings are functions of the telescope's aperture and central obstruction, if any. The visible extent of the disc as well as the number of the rings visible varies from a given instrument ...
Polar Winter Differential image motion monitor (PWD)
... want to get the information during winter, we will have to operate the telescope remotely. • fully remote operation Tohoku-DIMM, which was put on the entrance of AIRT40 and was used for seeing measurement in 2010/2011 campaign, is not available because AIRT40 will be used for Infrared observation ne ...
... want to get the information during winter, we will have to operate the telescope remotely. • fully remote operation Tohoku-DIMM, which was put on the entrance of AIRT40 and was used for seeing measurement in 2010/2011 campaign, is not available because AIRT40 will be used for Infrared observation ne ...
a flat high-frequency scanning micromirror - EECS: www
... µm-long hinge (the hinge used for the 550 µm-diameter mirror with resonant frequency of 34 kHz) with a total scan of ±6.25° is approximately 1.8%. Mirrors have been operated at this level for over 200 million cycles without any noticeable degradation in performance, but this strain may be too high f ...
... µm-long hinge (the hinge used for the 550 µm-diameter mirror with resonant frequency of 34 kHz) with a total scan of ±6.25° is approximately 1.8%. Mirrors have been operated at this level for over 200 million cycles without any noticeable degradation in performance, but this strain may be too high f ...
VIRUS Instrument Collimator Assembly
... The optical design of a VIRUS unit spectrograph is a simple off-axis Schmidt collimator coupled with a traditional Schmidt vacuum camera. The VIRUS collimator has three optics: a spherical collimator mirror, a folding flat, and a volume-phase holographic (VPH) grating. These optics proved to be rela ...
... The optical design of a VIRUS unit spectrograph is a simple off-axis Schmidt collimator coupled with a traditional Schmidt vacuum camera. The VIRUS collimator has three optics: a spherical collimator mirror, a folding flat, and a volume-phase holographic (VPH) grating. These optics proved to be rela ...
jcmt carma aste smto
... Highly-ranked by NSF review and will be funded this year. observation from ~2015 (?) • Large (sub-)mm telescope will be very useful. ...
... Highly-ranked by NSF review and will be funded this year. observation from ~2015 (?) • Large (sub-)mm telescope will be very useful. ...
optics7
... should be able to read 1M print (standard size reading material) with a add power of (100/20 = 5) +5.00 sphere. Test circumstances such as illumination, contrast, and target type must be kept precisely the same……………..this is most of the time unable to be performed ...
... should be able to read 1M print (standard size reading material) with a add power of (100/20 = 5) +5.00 sphere. Test circumstances such as illumination, contrast, and target type must be kept precisely the same……………..this is most of the time unable to be performed ...
Propagation of Light Through Atmospheric Turbulence Lecture 5
... at your favorite wavelength. • At excellent sites such as Mauna Kea in Hawaii, r0 at λ = 0.5 micron is 10 - 30 cm. • But there is a big range from night to night, and at times also within a night. Page 30 ...
... at your favorite wavelength. • At excellent sites such as Mauna Kea in Hawaii, r0 at λ = 0.5 micron is 10 - 30 cm. • But there is a big range from night to night, and at times also within a night. Page 30 ...
Lab Manual part 2
... know you've found Polaris if it is also the first star in the Little Dipper and you can be sure that you have the Little Dipper if its pan is pouring into the Big Dipper and the Big Dipper's pan pours into the Little Dipper. 2. Set-up the tripod: Find the leg with the 'N' on it and line up this leg ...
... know you've found Polaris if it is also the first star in the Little Dipper and you can be sure that you have the Little Dipper if its pan is pouring into the Big Dipper and the Big Dipper's pan pours into the Little Dipper. 2. Set-up the tripod: Find the leg with the 'N' on it and line up this leg ...
instruction manual - Optical Vision Ltd
... Using the Camera Adapter Tube When you connect a camera directly to your telescope for "prime focus" photography, you sometimes require an adapter so that the camera can be focussed. Some reflectors need more length than the focuser can travel, in order to focus the camera, and some refractors are ...
... Using the Camera Adapter Tube When you connect a camera directly to your telescope for "prime focus" photography, you sometimes require an adapter so that the camera can be focussed. Some reflectors need more length than the focuser can travel, in order to focus the camera, and some refractors are ...
Acquisition, Tracking and Pointing control
... consists of two large gimbaled telescopes, that arc optically couplad and used to redirect, a laser beam from a ground-based source to a distant point. The attitude control system consists of reaction wheels, star trackers and gyros. The optical control system consists of fast steering mirrors and o ...
... consists of two large gimbaled telescopes, that arc optically couplad and used to redirect, a laser beam from a ground-based source to a distant point. The attitude control system consists of reaction wheels, star trackers and gyros. The optical control system consists of fast steering mirrors and o ...
INSTRUCTION MANUAL Orion® SpaceProbe 130mm EQ
... The telescope is now balanced on both axes. Now when you loosen the lock knob on one or both axes and manually point the telescope, it should move without resistance and should not drift from where you point it. Focusing the Telescope Insert the low-power 25mm eyepiece into the focuser and secure wi ...
... The telescope is now balanced on both axes. Now when you loosen the lock knob on one or both axes and manually point the telescope, it should move without resistance and should not drift from where you point it. Focusing the Telescope Insert the low-power 25mm eyepiece into the focuser and secure wi ...
Fabry-Perot Interferometer FABRYPEROT.TEX KB 20020122
... is more or less blocked. These conditions can be adjusted by changing the wavelength and/or the geometry. Thus Fabry-Perot plates can be used to measure or to control light wavelengths or to measure geometric properties. The geometric conditions are defined by several properties including thickness, ...
... is more or less blocked. These conditions can be adjusted by changing the wavelength and/or the geometry. Thus Fabry-Perot plates can be used to measure or to control light wavelengths or to measure geometric properties. The geometric conditions are defined by several properties including thickness, ...
Astronomical imaging using ground
... substantially over a large field. This will be of particular value to science programs that until now have not found any advantage in AO. Many observations that are normally carried out in the seeing limit will benefit from improved resolution and signal-to-noise, ultimately increasing scientific th ...
... substantially over a large field. This will be of particular value to science programs that until now have not found any advantage in AO. Many observations that are normally carried out in the seeing limit will benefit from improved resolution and signal-to-noise, ultimately increasing scientific th ...
![[75-79] Privett Review Skywatcher Apr06.indd](http://s1.studyres.com/store/data/023366319_1-a76758b4d0090512e8b7a8bcf6b3580b-300x300.png)
OPTIMIZATION OF THE FIBER-OPITC FABRY-PEROT INTERFEROMETER CONSTRUCTION Małgorzata Jędrzejewska-Szczerska,
... about the measurand (equation (8)), as shown in Fig.3. It can be noted that for ∆φ=0 there is no spectral modulation (Fig.3a)). If the phase difference between the interfering beams varies from zero, the function takes the form of the cosine curve (Fig.3b). The spacing of adjacent transmission peak ...
... about the measurand (equation (8)), as shown in Fig.3. It can be noted that for ∆φ=0 there is no spectral modulation (Fig.3a)). If the phase difference between the interfering beams varies from zero, the function takes the form of the cosine curve (Fig.3b). The spacing of adjacent transmission peak ...
BaBar Pascos 2003
... E.Giraud, I.Toledo, P.Valvin & G.Vasileiadis LPTA/Montpellier, Un.Cath Chile G.Vasileiadis, CTA Meeting 4-5 May-2006 ...
... E.Giraud, I.Toledo, P.Valvin & G.Vasileiadis LPTA/Montpellier, Un.Cath Chile G.Vasileiadis, CTA Meeting 4-5 May-2006 ...
A Synopsis of the Paper, “Optical Performance of the James Webb
... The WFE total for NIRCam is computed by the RSS of the OTE, ISIM, and WFS&C errors. Each of these subsystems have budgeted their allowable WFE to their respective individual components. For example a portion of the OTE allocation of 131 nm rms is allocated to design residual, alignment, and figure e ...
... The WFE total for NIRCam is computed by the RSS of the OTE, ISIM, and WFS&C errors. Each of these subsystems have budgeted their allowable WFE to their respective individual components. For example a portion of the OTE allocation of 131 nm rms is allocated to design residual, alignment, and figure e ...
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.