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... Coated achromat in mounting. Clear lens diameter is 9mm and focal length is 40mm. Mounting is 13.5mm diameter by 8.9mm long, then machined to 9.5mm diameter by 5mm long with a center opening of 4.2mm. Clearly intended for a specific application. If you have a project that can use this achromat in it ...
... Coated achromat in mounting. Clear lens diameter is 9mm and focal length is 40mm. Mounting is 13.5mm diameter by 8.9mm long, then machined to 9.5mm diameter by 5mm long with a center opening of 4.2mm. Clearly intended for a specific application. If you have a project that can use this achromat in it ...
SPIE Astronomical Telescopes and Instrumentation Technical
... (Germany); P. Ferruit, B. Dorner, Observatoire de Lyon (France) The Near Infrared Spectrograph (NIRSpec) is one of four science instruments aboard the James Webb Space Telescope (JWST) scheduled for launch in 2014. NIRSpec is sensitive in the wavelength range from ~0.6 to 5.0 micron and will be capa ...
... (Germany); P. Ferruit, B. Dorner, Observatoire de Lyon (France) The Near Infrared Spectrograph (NIRSpec) is one of four science instruments aboard the James Webb Space Telescope (JWST) scheduled for launch in 2014. NIRSpec is sensitive in the wavelength range from ~0.6 to 5.0 micron and will be capa ...
Report from the Subaru Telescope for External
... used the Subaru telescope to discover the most distant galaxy ever found, SXDF-NB10062, at z = 7.215 at that time. This galaxy is slightly farther away than GN-108036, which the Subaru Telescope discovered in the previous year (Ono et al. 2012), at z = 7.213 and was the most distant galaxy discovere ...
... used the Subaru telescope to discover the most distant galaxy ever found, SXDF-NB10062, at z = 7.215 at that time. This galaxy is slightly farther away than GN-108036, which the Subaru Telescope discovered in the previous year (Ono et al. 2012), at z = 7.213 and was the most distant galaxy discovere ...
Astronomical Adaptive Optics using Multiple Laser Guide Stars
... Figure 3-6. Pupil model of the NGS WFS camera ............................................ 70 Figure 3-7. Power spectrum from a measured LGS mode ............................... 78 Figure 3-8. Measured r0 by Zernike radial order ............................................... 83 Figure 3-9. Wavefron ...
... Figure 3-6. Pupil model of the NGS WFS camera ............................................ 70 Figure 3-7. Power spectrum from a measured LGS mode ............................... 78 Figure 3-8. Measured r0 by Zernike radial order ............................................... 83 Figure 3-9. Wavefron ...
9 adaptive optics - Giant Magellan Telescope
... 35% for a tilt star 1′ off axis. The 200 nm RMS target is significantly better than is typically achieved with current systems, but our analysis later in this chapter shows it will be possible. Table 9-1 shows the corresponding on-axis Strehl ratios for other wavelengths. A second major goal for the ...
... 35% for a tilt star 1′ off axis. The 200 nm RMS target is significantly better than is typically achieved with current systems, but our analysis later in this chapter shows it will be possible. Table 9-1 shows the corresponding on-axis Strehl ratios for other wavelengths. A second major goal for the ...
Optical interferometry in astronomy
... patch, the rms phase error is ∼1.03 rad. At λ = 500 nm, r0 is typically 10 cm (toward zenith) 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 ...
... patch, the rms phase error is ∼1.03 rad. At λ = 500 nm, r0 is typically 10 cm (toward zenith) 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 ...
Gamma-Ray Bursts and Puzzles of Core
... First 21 GRB hosts: The Hubble diagram for GRB host galaxies with known (before June 2002) observable stellar magnitudes (or with upper R limits) and spectroscopic red shifts against the background of results of the photometric measurement of z applied to galaxies from the Hubble Deep Field (HDF) b ...
... First 21 GRB hosts: The Hubble diagram for GRB host galaxies with known (before June 2002) observable stellar magnitudes (or with upper R limits) and spectroscopic red shifts against the background of results of the photometric measurement of z applied to galaxies from the Hubble Deep Field (HDF) b ...
Differential measurement of atmospheric
... and direct simple idea is that the two sky regions can be observed simultaneous by a binocular telescope. But under the influence of the gravity and ambient temperature change, the tubes and the bracket of the binocular telescope may produce different deformation inevitably in the process of measurem ...
... and direct simple idea is that the two sky regions can be observed simultaneous by a binocular telescope. But under the influence of the gravity and ambient temperature change, the tubes and the bracket of the binocular telescope may produce different deformation inevitably in the process of measurem ...
PDF
... In mid-2009, the red arm of our workhorse multi-object spectrometer, LRIS, received a new dewar with a highly-sensitive detector mosaic that substantially improved the instrument’s red-side throughput (see the Summer 2009 issue). The CCD array operated well for several months, but then began deterio ...
... In mid-2009, the red arm of our workhorse multi-object spectrometer, LRIS, received a new dewar with a highly-sensitive detector mosaic that substantially improved the instrument’s red-side throughput (see the Summer 2009 issue). The CCD array operated well for several months, but then began deterio ...
Examples for Applications of collimators, telescopes, visual and
... 2.5 Testing of Transparent Wedges — Simultaneous Determination of Wedge Angle and Refractive Index 2.6 Testing of Transparent Wedges — Evaluation by Angular Deviation . . . . . . . . . . . . . . . . . . . 2.7 Testing of the 90◦ angle of a 90◦ -Glass Prism in double pass . . . . . . . . . . . . . . . ...
... 2.5 Testing of Transparent Wedges — Simultaneous Determination of Wedge Angle and Refractive Index 2.6 Testing of Transparent Wedges — Evaluation by Angular Deviation . . . . . . . . . . . . . . . . . . . 2.7 Testing of the 90◦ angle of a 90◦ -Glass Prism in double pass . . . . . . . . . . . . . . . ...
CHANDRA X-ray Center Ping Zhao
... Figures 10 and 11 show the optical axis and aimpoint positions on HRC-I and HRC-S. The blue diamonds show the optical axis positions. The red arrows show the aimpoint position drift. While the optical axis is relatively stable, the aimpoint has been drifting in the SIM [−Y,−Z] direction since the Ch ...
... Figures 10 and 11 show the optical axis and aimpoint positions on HRC-I and HRC-S. The blue diamonds show the optical axis positions. The red arrows show the aimpoint position drift. While the optical axis is relatively stable, the aimpoint has been drifting in the SIM [−Y,−Z] direction since the Ch ...
KAON 739 - Caltech Optical Observatories
... require access to celestial sources. Measurements that could be similar to calibrations but are made with celestial sources are considered part of the operations and optimization tasks of the NGAO system. These operations can occur before, during, or after science observations. It is beyond the scop ...
... require access to celestial sources. Measurements that could be similar to calibrations but are made with celestial sources are considered part of the operations and optimization tasks of the NGAO system. These operations can occur before, during, or after science observations. It is beyond the scop ...
I+D en IFCA para futuros aceleradores
... EUDAQ FRAMEWORK Hierarchy, distribution and communication between applications: ...
... EUDAQ FRAMEWORK Hierarchy, distribution and communication between applications: ...
Search for solar axions with the CAST experiment
... CAST: Tracking precision Solar filming Twice per year (March and September) we can film the Sun through the window A camera is placed on top of the magnet and is aligned with the bore axis Corrections for visible light refractions are taken into account ...
... CAST: Tracking precision Solar filming Twice per year (March and September) we can film the Sun through the window A camera is placed on top of the magnet and is aligned with the bore axis Corrections for visible light refractions are taken into account ...
FY96
... spectrograph on the Blanco 4-m telescope, Cote and Philippe Fischer (Michigan U.) have searched for main-sequence binaries with very short periods, between 2 days and 3 years, in the cluster M4. In a sample of 33 main-sequence stars, two show velocity differences of greater than 10 km/s in observati ...
... spectrograph on the Blanco 4-m telescope, Cote and Philippe Fischer (Michigan U.) have searched for main-sequence binaries with very short periods, between 2 days and 3 years, in the cluster M4. In a sample of 33 main-sequence stars, two show velocity differences of greater than 10 km/s in observati ...
Power Point Presentation
... Cosmology Professor Lynn Cominsky Department of Physics and Astronomy Offices: Darwin 329A and NASA EPO ...
... Cosmology Professor Lynn Cominsky Department of Physics and Astronomy Offices: Darwin 329A and NASA EPO ...
Mercury Flyby 3 - Messenger - The Johns Hopkins University
... October 2006, June 2007; Mercury (3) January 2008, October 2008, September 2009. ...
... October 2006, June 2007; Mercury (3) January 2008, October 2008, September 2009. ...
JWST Project Report to the PMC
... 1.) Orbit that assures thermal stability and low background 2.) Orbit that assures long dwell times 3.) A stable PSF and excellent pointing 4.) Infrared sensitivity (planetary temperatures; molecules) 5.) Aperture sufficient to permit medium resolution spectroscopy These are obtained with a large ap ...
... 1.) Orbit that assures thermal stability and low background 2.) Orbit that assures long dwell times 3.) A stable PSF and excellent pointing 4.) Infrared sensitivity (planetary temperatures; molecules) 5.) Aperture sufficient to permit medium resolution spectroscopy These are obtained with a large ap ...
XMM-Newton
The XMM-Newton, also known as the X-ray Multi-Mirror Mission and the High Throughput X-ray Spectroscopy Mission, is an orbiting X-ray observatory launched by ESA in December 1999 on an Ariane 5 rocket. It is named in honor of Sir Isaac Newton. The telescope was placed in a very eccentric 48 hour elliptical orbit at 40°; at its apogee it is nearly 114,000 kilometres (71,000 mi) from Earth, while the perigee is only 7,000 kilometres (4,300 mi).