Lab 14 Galaxy Morphology
... appeared similar to comets, but did not move. Others of these nebulae were resolved into clusters of stars as bigger telescopes were constructed, and used to examine them. Some of these fuzzy nebulae, however, did not break-up into stars no matter how big a telescope was used to look at them. While ...
... appeared similar to comets, but did not move. Others of these nebulae were resolved into clusters of stars as bigger telescopes were constructed, and used to examine them. Some of these fuzzy nebulae, however, did not break-up into stars no matter how big a telescope was used to look at them. While ...
THE CASSINI VISUAL AND INFRARED MAPPING SPECTROMETER
... Orbiter in 1974. A more refined concept was proposed for the Mariner Jupiter Uranus (MJU) mission in 1975. This design was accepted for the Jupiter Orbiter Probe (JOP, later named Galileo) Mission in 1977. After selection, this design rapidly evolved into that of the NIMS instrument. Further conside ...
... Orbiter in 1974. A more refined concept was proposed for the Mariner Jupiter Uranus (MJU) mission in 1975. This design was accepted for the Jupiter Orbiter Probe (JOP, later named Galileo) Mission in 1977. After selection, this design rapidly evolved into that of the NIMS instrument. Further conside ...
Gamma Ray Bursts
... Diversity of pulse shapes well explained by diversity of shapes and sizes of comets. Neutron stars are inside galactic disk. How to get isotropic distribution? Possible, if we see only nearby neutron stars. Having the number of neutron stars (from pulsar observations and supernovae) and the numer of ...
... Diversity of pulse shapes well explained by diversity of shapes and sizes of comets. Neutron stars are inside galactic disk. How to get isotropic distribution? Possible, if we see only nearby neutron stars. Having the number of neutron stars (from pulsar observations and supernovae) and the numer of ...
Measuring distances to the edge of the local group
... Scheduling constraints and non-usable dates (up to four lines). ...
... Scheduling constraints and non-usable dates (up to four lines). ...
Unraveling the Helix Nebula: Its Structure and Knots
... from an ionization front (although shock excitation is also possible in some regions, § 4.3). The knots begin to be observed at about the same distance from the central star that the HeII core gives way to the lower ionization H+ +He+ zone that produces the dominant [O III] emission. Throughout this ...
... from an ionization front (although shock excitation is also possible in some regions, § 4.3). The knots begin to be observed at about the same distance from the central star that the HeII core gives way to the lower ionization H+ +He+ zone that produces the dominant [O III] emission. Throughout this ...
ABSTRACT Exoplanet Habitability and an Analysis of Gliese 436 b
... for habitable exoplanets in the Milky Way.8 The transit method is similar to an eclipse of the moon. An exoplanet orbits in front of its host star as viewed from earth.8 A photon counting camera can then detect the decrease in perceived brightness from the host star.9 A light curve is then produced ...
... for habitable exoplanets in the Milky Way.8 The transit method is similar to an eclipse of the moon. An exoplanet orbits in front of its host star as viewed from earth.8 A photon counting camera can then detect the decrease in perceived brightness from the host star.9 A light curve is then produced ...
Origami Sunshield Concepts for Space Telescopes Lee Wilson and Sergio Pellegrino Rolf Danner
... in the packaged state and hence a preload will be required. This would cause wrinkling within the MLI membrane, which may remain after deployment. Physical prototypes incorporating MLI would need to be investigated to determine if this is a problem. B. ...
... in the packaged state and hence a preload will be required. This would cause wrinkling within the MLI membrane, which may remain after deployment. Physical prototypes incorporating MLI would need to be investigated to determine if this is a problem. B. ...
Galaxy Sorting
... gas and dust fill the disks of spiral galaxies, and new star formation continues to take place in their disks. Irregular galaxies appear chaotic, and often have many bright, young stars, the result of recent bursts of intense star formation. For many years, astronomers thought the dissimilarities ...
... gas and dust fill the disks of spiral galaxies, and new star formation continues to take place in their disks. Irregular galaxies appear chaotic, and often have many bright, young stars, the result of recent bursts of intense star formation. For many years, astronomers thought the dissimilarities ...
Axisymmetry in protoplanetary nebulae: using imaging polarimetry
... in the CSEs of PPNe when they are associated with bright central stars. Since PPNe are seen by scattered light in the optical and NIR, they are expected to be linearly polarized at these wavelengths. On the other hand, the stellar PSF, which is formed by scattering through tiny angles in the atmosph ...
... in the CSEs of PPNe when they are associated with bright central stars. Since PPNe are seen by scattered light in the optical and NIR, they are expected to be linearly polarized at these wavelengths. On the other hand, the stellar PSF, which is formed by scattering through tiny angles in the atmosph ...
The achromatic design of an atmospheric dispersion corrector for
... (0.59-0.81 µm), I band (0.78-1.02 µm), J band (1.06-1.44 µm), H band (1.5-1.7 µm), and K band (1.96-2.44 µm) at 45 degrees off Zenith. Although the spot size produced at each individual wavelength is smaller than the Airy disk (the black circle), the image of a star in the R band would appear elonga ...
... (0.59-0.81 µm), I band (0.78-1.02 µm), J band (1.06-1.44 µm), H band (1.5-1.7 µm), and K band (1.96-2.44 µm) at 45 degrees off Zenith. Although the spot size produced at each individual wavelength is smaller than the Airy disk (the black circle), the image of a star in the R band would appear elonga ...
optics7
... When possible, it is best to correct a patient’s refractive error by incorporating the correction directly into the ocular lens or as a lens cap at the eyepiece of the telescope. When using this method, the total magnification of the system remains the same and no adjustment of the tube length of an ...
... When possible, it is best to correct a patient’s refractive error by incorporating the correction directly into the ocular lens or as a lens cap at the eyepiece of the telescope. When using this method, the total magnification of the system remains the same and no adjustment of the tube length of an ...
structure and evolution of white dwarfs and their
... designated DO if HeII features are present (hotter than about 45000K) and DB if only HeI lines are visible. Small numbers of hybrid stars exist, with both hydrogen and helium present. In these cases, two classification letters are used, with the first indicating the dominant species. For example, DA ...
... designated DO if HeII features are present (hotter than about 45000K) and DB if only HeI lines are visible. Small numbers of hybrid stars exist, with both hydrogen and helium present. In these cases, two classification letters are used, with the first indicating the dominant species. For example, DA ...
A S R TRATEGY
... plan to install the corrected WFPC II in place of WFPC on the first servicing mission in 1993, and later, on a second mission in 1996, to install STIS or NICMOS either to recover spectroscopic capabilities (in the case of STIS) or to add new infrared capabilities (with NICMOS). This initial recovery ...
... plan to install the corrected WFPC II in place of WFPC on the first servicing mission in 1993, and later, on a second mission in 1996, to install STIS or NICMOS either to recover spectroscopic capabilities (in the case of STIS) or to add new infrared capabilities (with NICMOS). This initial recovery ...
... Telescope (GLAST), scheduled for launch in 2005 (Gehrels & Michelson 1999) has the same general features but will use solid state detectors with a factor of 10-30 improvement in sensitivity. The Third EGRET catalog (based on some four years of observation by EGRET) (Hartman et al. 1999) contains a l ...
The Secular and Rotational Brightness Variations of Neptune
... This is the seventh paper in a series which models the brightness, color and albedo of all the planets except Earth on the Johnson-Cousins magnitude system. Mercury (Mallama et al. 2002) and Venus (Mallama et al. 2006) were observed with the Solar and Heliospheric Observatory satellite. The SOHO mag ...
... This is the seventh paper in a series which models the brightness, color and albedo of all the planets except Earth on the Johnson-Cousins magnitude system. Mercury (Mallama et al. 2002) and Venus (Mallama et al. 2006) were observed with the Solar and Heliospheric Observatory satellite. The SOHO mag ...
April 2016 - Central Arkansas Astronomical Society
... From the 11th April 2015, all members who a end ASSA sanc oned public events MUST have a current NPC clearance cer ficate, or equivalent clearance le er from their employer, and MUST have provided ASSA with these ...
... From the 11th April 2015, all members who a end ASSA sanc oned public events MUST have a current NPC clearance cer ficate, or equivalent clearance le er from their employer, and MUST have provided ASSA with these ...
2014 - Society for Astronomical Sciences
... standard filter is Johnson V. The throughput for the B-band can also be low when combined with the response curve of more commonly available fontilluminated CCDs. With this in mind, we required all observers to contribute V images and made that band our top priority. In order after that we prioritiz ...
... standard filter is Johnson V. The throughput for the B-band can also be low when combined with the response curve of more commonly available fontilluminated CCDs. With this in mind, we required all observers to contribute V images and made that band our top priority. In order after that we prioritiz ...
The Swift satellite lives up to its name, revealing cosmic
... The Swift satellite (Gehrels et al. 2004), launched into low-Earth orbit in November 2004, detects GRBs at a rate of ∼100 per year. It carries 3 instruments: a widefield gamma-ray telescope named BAT (Burst Alert Telescope), an X-ray telescope named XRT and an optical and ultraviolet telescope named ...
... The Swift satellite (Gehrels et al. 2004), launched into low-Earth orbit in November 2004, detects GRBs at a rate of ∼100 per year. It carries 3 instruments: a widefield gamma-ray telescope named BAT (Burst Alert Telescope), an X-ray telescope named XRT and an optical and ultraviolet telescope named ...
Ground-Conjugate Wide Field Adaptive Optics for the ELTs F. Rigaut
... Figure 2 displays the natural and compensated median FWHMs at Cerro Pachon and Cerro Paranal for the three bands V, J and K, versus the eld of view. This gure shows that this compensation scheme, like any other phase compensation method, is very wavelength dependant. Apparently, a threshold is pas ...
... Figure 2 displays the natural and compensated median FWHMs at Cerro Pachon and Cerro Paranal for the three bands V, J and K, versus the eld of view. This gure shows that this compensation scheme, like any other phase compensation method, is very wavelength dependant. Apparently, a threshold is pas ...
21_Testbank
... B) Galaxies were much bigger in the past since they had not contracted completely. C) Galaxies were closer together in the past because the universe was smaller. D) Galaxies attracted each other more strongly in the past because they were more massive; they had not yet turned most of their mass into ...
... B) Galaxies were much bigger in the past since they had not contracted completely. C) Galaxies were closer together in the past because the universe was smaller. D) Galaxies attracted each other more strongly in the past because they were more massive; they had not yet turned most of their mass into ...
Focus and pointing adjustments necessary for laser guide star
... commands are sent to the DM to correct sensed wavefront errors. However, several characteristics of the LGS differ from the NGS, and not all wavefront errors visible in an NGS are visible in an LGS. At Keck, the use of off-axis laser projection complicates the laser pointing model. Focus complicatio ...
... commands are sent to the DM to correct sensed wavefront errors. However, several characteristics of the LGS differ from the NGS, and not all wavefront errors visible in an NGS are visible in an LGS. At Keck, the use of off-axis laser projection complicates the laser pointing model. Focus complicatio ...
120 Inch Telescope Aluminizing 2-7-06
... 22. Start testing mirror at this point, prepare area and chemicals and remove cardboard, tape, and foil. (50-51) 23. PREPARE to remove support assemblies. Leave defining units in place. (42) 24. Install support arms for mirror spreader bar on south end of mirror handling platform while work on mirro ...
... 22. Start testing mirror at this point, prepare area and chemicals and remove cardboard, tape, and foil. (50-51) 23. PREPARE to remove support assemblies. Leave defining units in place. (42) 24. Install support arms for mirror spreader bar on south end of mirror handling platform while work on mirro ...
PATBNTED OCT. 29. 1907. TELESCOPE.
... tagonal in form, although in substance it is the same as the triangular prism of Figs. 1 to 4, the additional mate rial marked A’ performing no function except that of 70 enabling the constructor to eliminatev air-to-glass sur— faces between the two prisms. ...
... tagonal in form, although in substance it is the same as the triangular prism of Figs. 1 to 4, the additional mate rial marked A’ performing no function except that of 70 enabling the constructor to eliminatev air-to-glass sur— faces between the two prisms. ...
Spitzer Space Telescope
The Spitzer Space Telescope (SST), formerly the Space Infrared Telescope Facility (SIRTF), is an infrared space observatory launched in 2003. It is the fourth and final of the NASA Great Observatories program.The planned mission period was to be 2.5 years with a pre-launch expectation that the mission could extend to five or slightly more years until the onboard liquid helium supply was exhausted. This occurred on 15 May 2009. Without liquid helium to cool the telescope to the very low temperatures needed to operate, most of the instruments are no longer usable. However, the two shortest-wavelength modules of the IRAC camera are still operable with the same sensitivity as before the cryogen was exhausted, and will continue to be used in the Spitzer Warm Mission. All Spitzer data, from both the primary and warm phases, are archived at the Infrared Science Archive (IRSA).In keeping with NASA tradition, the telescope was renamed after its successful demonstration of operation, on 18 December 2003. Unlike most telescopes that are named after famous deceased astronomers by a board of scientists, the new name for SIRTF was obtained from a contest open to the general public.The contest led to the telescope being named in honor of astronomer Lyman Spitzer, who had promoted the concept of space telescopes in the 1940s. Spitzer wrote a 1946 report for RAND Corporation describing the advantages of an extraterrestrial observatory and how it could be realized with available or upcoming technology. He has been cited for his pioneering contributions to rocketry and astronomy, as well as ""his vision and leadership in articulating the advantages and benefits to be realized from the Space Telescope Program.""The US$800 million Spitzer was launched from Cape Canaveral Air Force Station, on a Delta II 7920H ELV rocket, Monday, 25 August 2003 at 13:35:39 UTC-5 (EDT).It follows a heliocentric instead of geocentric orbit, trailing and drifting away from Earth's orbit at approximately 0.1 astronomical unit per year (a so-called ""earth-trailing"" orbit). The primary mirror is 85 centimeters (33 in) in diameter, f/12, made of beryllium and is cooled to 5.5 K (−449.77 °F). The satellite contains three instruments that allow it to perform astronomical imaging and photometry from 3 to 180 micrometers, spectroscopy from 5 to 40 micrometers, and spectrophotometry from 5 to 100 micrometers.