The CryoSat System The CryoSat System
... viewer. The prominent features visible are the solar arrays, giving a roof-like appearance, and the three star trackers which are mounted on the rigid structure supporting the SIRAL antennas. The structure forming the ‘nose’ at the very front of the satellite is a thermal radiator for the heat gener ...
... viewer. The prominent features visible are the solar arrays, giving a roof-like appearance, and the three star trackers which are mounted on the rigid structure supporting the SIRAL antennas. The structure forming the ‘nose’ at the very front of the satellite is a thermal radiator for the heat gener ...
Dishing Up the Data: The Role of Australian Space Tracking and
... Goldstone, California. In order to maintain continuous communications with lunar and planetary spacecraft, a minimum of three tracking stations, located around the globe at approximately 120° apart, is required to ensure that a spacecraft remains under constant observation despite the rotation of E ...
... Goldstone, California. In order to maintain continuous communications with lunar and planetary spacecraft, a minimum of three tracking stations, located around the globe at approximately 120° apart, is required to ensure that a spacecraft remains under constant observation despite the rotation of E ...
WFIRST-2.4: What Every Astronomer Should Know
... observing program for a 5-year prime mission, which is summarized in Table 1 and detailed in subsequent sections. WFIRST-2.4 will support a wide range of science programs during its primary mission. Each of these programs has unique constraints involving the field of regard, cadence, and S/C roll an ...
... observing program for a 5-year prime mission, which is summarized in Table 1 and detailed in subsequent sections. WFIRST-2.4 will support a wide range of science programs during its primary mission. Each of these programs has unique constraints involving the field of regard, cadence, and S/C roll an ...
Alternate Surface Measurements for GMT Primary Mirror
... An ideal parabolic mirror will focus rays parallel to the axis to a point at the focus. One can measure errors in the surface by sending parallel rays into the mirror and measuring where they intercept the focal plane. The scanning pentaprism system uses a collimated light source and a pentaprism to ...
... An ideal parabolic mirror will focus rays parallel to the axis to a point at the focus. One can measure errors in the surface by sending parallel rays into the mirror and measuring where they intercept the focal plane. The scanning pentaprism system uses a collimated light source and a pentaprism to ...
1. The diagram shows the concave mirror of a Cassegrain reflecting
... A converging lens of focal length 100mm is used to produce a magnified image of a small object. The magnification is × 2. Draw rays on the diagrams to show how the images are produced. The principal foci are each labelled F. The diagrams need not be drawn to scale. (a) ...
... A converging lens of focal length 100mm is used to produce a magnified image of a small object. The magnification is × 2. Draw rays on the diagrams to show how the images are produced. The principal foci are each labelled F. The diagrams need not be drawn to scale. (a) ...
Than Our Eyes Can See - Cool Cosmos
... would be exposed by the camera’s own light, long before you ever got a chance to take a picture! Infrared astronomers face the same problem when they try to detect heat from space. At room temperature, their telescopes and instruments are shining brilliantly in the infrared. In order to record faint ...
... would be exposed by the camera’s own light, long before you ever got a chance to take a picture! Infrared astronomers face the same problem when they try to detect heat from space. At room temperature, their telescopes and instruments are shining brilliantly in the infrared. In order to record faint ...
669 - Caltech Optical Observatories
... The concept of mounting the NGAO narrow field deformable mirror (DM) on a tip-tilt mount to steer the light beam on the science instrument was proposed in KAON 558: “One can imagine steering the light beam on and around the science array with high accuracy using a steering mirror or a probe arm inst ...
... The concept of mounting the NGAO narrow field deformable mirror (DM) on a tip-tilt mount to steer the light beam on the science instrument was proposed in KAON 558: “One can imagine steering the light beam on and around the science array with high accuracy using a steering mirror or a probe arm inst ...
TRAPPIST: TRAnsiting Planets and PlanetesImals Small Telescope
... ment. An uninterruptable power supply (UPS) keeps the observatory running for 45 minutes during an electrical power cut and an emergency shutdown is trig gered at the end of this period. Several webcams inside and outside the building help us to check what is going on in the observatory if needed. ...
... ment. An uninterruptable power supply (UPS) keeps the observatory running for 45 minutes during an electrical power cut and an emergency shutdown is trig gered at the end of this period. Several webcams inside and outside the building help us to check what is going on in the observatory if needed. ...
paper
... ment. An uninterruptable power supply (UPS) keeps the observatory running for 45 minutes during an electrical power cut and an emergency shutdown is trig gered at the end of this period. Several webcams inside and outside the building help us to check what is going on in the observatory if needed. ...
... ment. An uninterruptable power supply (UPS) keeps the observatory running for 45 minutes during an electrical power cut and an emergency shutdown is trig gered at the end of this period. Several webcams inside and outside the building help us to check what is going on in the observatory if needed. ...
A Model of Sky Brightness in the Stratosphere
... observatory any night of the year. A balloon-borne telescope will also have the ability for daytime observing. It is believed that the daytime sky background decreases by roughly a factor of two for every 5 kilometers in altitude. If this is true, bright objects, such as Uranus and Neptune, can easi ...
... observatory any night of the year. A balloon-borne telescope will also have the ability for daytime observing. It is believed that the daytime sky background decreases by roughly a factor of two for every 5 kilometers in altitude. If this is true, bright objects, such as Uranus and Neptune, can easi ...
Copyright 2003 Society of Photo-Optical Instrumentation Engineers
... All materials have different Coefficients of Thermal Expansion (CTE, α). Some are large, like rubber and plastics (α = 100-200 ppm). Some are medium, like aluminium (α = 23 ppm) or steel (α = 10 ppm). Some have a low CTE like Invar (α = 1-2 ppm) and wood (α = 3-5 ppm). Some have almost zero expansio ...
... All materials have different Coefficients of Thermal Expansion (CTE, α). Some are large, like rubber and plastics (α = 100-200 ppm). Some are medium, like aluminium (α = 23 ppm) or steel (α = 10 ppm). Some have a low CTE like Invar (α = 1-2 ppm) and wood (α = 3-5 ppm). Some have almost zero expansio ...
Student Manual - Gettysburg College
... XMM-Newton is an X-ray satellite launched into Earth’s orbit on December 10, 1999 by the European Space Agency (ESA). XMM-Newton is actually a fully-functioning observatory, carrying three very advanced X-ray telescopes. They each contain 58 highprecision concentric mirrors, nested to offer the larg ...
... XMM-Newton is an X-ray satellite launched into Earth’s orbit on December 10, 1999 by the European Space Agency (ESA). XMM-Newton is actually a fully-functioning observatory, carrying three very advanced X-ray telescopes. They each contain 58 highprecision concentric mirrors, nested to offer the larg ...
Document
... ps time resolution with count rates as high as 15 MHz, and a fair QE. The main drawback of SPADs was the lack of CCD-like arrays. To overcome both the SPAD limitations and the difficulties of a reasonable optical design (coupling the pupil of large telescope to a single 50 - 100 m detector ), we de ...
... ps time resolution with count rates as high as 15 MHz, and a fair QE. The main drawback of SPADs was the lack of CCD-like arrays. To overcome both the SPAD limitations and the difficulties of a reasonable optical design (coupling the pupil of large telescope to a single 50 - 100 m detector ), we de ...
NASA`s Spitzer Images Out-of-This
... view from Spitzer, the area around the invisible black hole is blue and the ring of stars, white. The black hole is huge, about 100 million times the mass of our sun, and is feeding off gas and dust along with the occasional unlucky star. Our Milky Way's central black hole is tame by comparison, wit ...
... view from Spitzer, the area around the invisible black hole is blue and the ring of stars, white. The black hole is huge, about 100 million times the mass of our sun, and is feeding off gas and dust along with the occasional unlucky star. Our Milky Way's central black hole is tame by comparison, wit ...
Optical Design and Fabrication
... Harder to polish (not close to round shape) Edge sensor positions vary from one segment to another ...
... Harder to polish (not close to round shape) Edge sensor positions vary from one segment to another ...
675 x 4.5” Reflector Telescope
... Attach Control Cables, Counterweight and Eyepieces • Locate the Fine Adjustment Cables (5). Loosen the silver screws located at the end of the Fine Adjustment Cables and attach the Fine Adjustment Cables to the two silver posts found on the Equatorial Mount. The first post is located just above the ...
... Attach Control Cables, Counterweight and Eyepieces • Locate the Fine Adjustment Cables (5). Loosen the silver screws located at the end of the Fine Adjustment Cables and attach the Fine Adjustment Cables to the two silver posts found on the Equatorial Mount. The first post is located just above the ...
Inexpensive mount for a large millimeter
... performance using active control based on strut temperature measurements, without the cost and complexity of a panel edge sensor system. Thermal deformation of the primary can be calculated using a finite element model, but the model must be optimized based on surface error measurements with differe ...
... performance using active control based on strut temperature measurements, without the cost and complexity of a panel edge sensor system. Thermal deformation of the primary can be calculated using a finite element model, but the model must be optimized based on surface error measurements with differe ...
Polar Winter Differential image motion monitor (PWD)
... I already have a technique to control SBIG CCD camera using Linux. Furthermore, ST-i has a compact body (1.25” x 3.5”), light weight (68g), and USB bus power drive. ...
... I already have a technique to control SBIG CCD camera using Linux. Furthermore, ST-i has a compact body (1.25” x 3.5”), light weight (68g), and USB bus power drive. ...
RFO Yard Sale Inventory – as of May 29, 2013
... They are somewhat buried in their current location, so it is difficult to access their exact size and condition. My best estimate is that they are about one foot wide and between six and eight feet long. Each is supported on a trestle and the metal one appears to be adjustable in height. We would li ...
... They are somewhat buried in their current location, so it is difficult to access their exact size and condition. My best estimate is that they are about one foot wide and between six and eight feet long. Each is supported on a trestle and the metal one appears to be adjustable in height. We would li ...
Astronomy Astrophysics − Astrophysical parameters of the peculiar X-ray transient
... The far intersection with the Sagittarius-Carina arm (outside the solar circle) results in CO emission at positive LSR velocities (Cohen et al. 1985). The star HD 97253, located at d ≈ 2.5 kpc (290.◦8, +0.◦ 1), only shows negative radial velocities in its interstellar Na i lines (which are otherwise ...
... The far intersection with the Sagittarius-Carina arm (outside the solar circle) results in CO emission at positive LSR velocities (Cohen et al. 1985). The star HD 97253, located at d ≈ 2.5 kpc (290.◦8, +0.◦ 1), only shows negative radial velocities in its interstellar Na i lines (which are otherwise ...
The Dimensions Program - Asnuntuck Community College
... The second method to collect light on the NPOI is through three Astrometric Array Siderostat Stations that are fixed on each arm (see Figure 1 cover page for location). These are used to help create accurate maps of the sky. This is mostly what the U.S. Naval Observatory is interested in, since part ...
... The second method to collect light on the NPOI is through three Astrometric Array Siderostat Stations that are fixed on each arm (see Figure 1 cover page for location). These are used to help create accurate maps of the sky. This is mostly what the U.S. Naval Observatory is interested in, since part ...
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).