Transparencies - Rencontres de Moriond
... Broad-band (ugrizy; 350nm-1050nm) internal photometric accuracy of 0.010 mag (zero-point across the sky). Relative astrometric accuracy of 10 mas. ...
... Broad-band (ugrizy; 350nm-1050nm) internal photometric accuracy of 0.010 mag (zero-point across the sky). Relative astrometric accuracy of 10 mas. ...
Full Presentation Here
... • IACT do not see the -ray hitting the atmosphere but the erenkov light from the electro-magnetic shower developed in the atmosphere (calorimeter with atmosphere as active material) The light is collected and focused on the camera forming and image of the electro-magnetic shower. The image may com ...
... • IACT do not see the -ray hitting the atmosphere but the erenkov light from the electro-magnetic shower developed in the atmosphere (calorimeter with atmosphere as active material) The light is collected and focused on the camera forming and image of the electro-magnetic shower. The image may com ...
Diapositive 1
... - which instrument (MIDI/AMBER), and why? - which telescope UT/AT, and why? - number of telescopes “if AMBER (2-3)“, and why? - which configuration(s), and why? - number of hours you request (single point confirmation, model-fitting, image reconstruction), and why? - which epoch (i.e. to constrain a ...
... - which instrument (MIDI/AMBER), and why? - which telescope UT/AT, and why? - number of telescopes “if AMBER (2-3)“, and why? - which configuration(s), and why? - number of hours you request (single point confirmation, model-fitting, image reconstruction), and why? - which epoch (i.e. to constrain a ...
THE STRUCTURE OF HIGH STREHL RATIO POINT
... ratio images, when the first-order term is the dominant aberration. Sivaramakrishnan et al. (2002) demonstrated that these pinned speckles will still occur near the cores of images taken with arbitrarily shaped, unapodized entrance apertures and that first-order pinned speckles are part of an antisymm ...
... ratio images, when the first-order term is the dominant aberration. Sivaramakrishnan et al. (2002) demonstrated that these pinned speckles will still occur near the cores of images taken with arbitrarily shaped, unapodized entrance apertures and that first-order pinned speckles are part of an antisymm ...
SurplusShed • www.SurplusShed.com
... 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 ...
Atmospheric-Turbulence Compensation Experiments Using
... Compensation Experiment (LACE) satellite to measure the quality of the correction directly [5]. These atmospheric-compensation techniques were originally developed for use in the Strategic Defense Initiative ballistic-missile defense system, but are equally applicable to the imaging of astronomical ...
... Compensation Experiment (LACE) satellite to measure the quality of the correction directly [5]. These atmospheric-compensation techniques were originally developed for use in the Strategic Defense Initiative ballistic-missile defense system, but are equally applicable to the imaging of astronomical ...
PACS Calibration Status and Plans
... 2) Uranus (H2O), Neptune (H2O, CO), Saturn (H2O, NH3, PH3) 3) late type stars with water lines (5) 4) PNe (e.g. LWS calibrators) for wavelength checks/ secondary standards 5) AGB stars & PPNe with narrow intrinsic CO line widths (10 – 20 km s−1) ...
... 2) Uranus (H2O), Neptune (H2O, CO), Saturn (H2O, NH3, PH3) 3) late type stars with water lines (5) 4) PNe (e.g. LWS calibrators) for wavelength checks/ secondary standards 5) AGB stars & PPNe with narrow intrinsic CO line widths (10 – 20 km s−1) ...
Micki s report in MS Word format.
... Setup menu title; there the user may choose whatever interval time, exposure length, and number of images to stack they wish to have. With the completion of the STV controls, the next item to be programmed was the telescope movement. Since this project is monitoring the intensity of Polaris, a metho ...
... Setup menu title; there the user may choose whatever interval time, exposure length, and number of images to stack they wish to have. With the completion of the STV controls, the next item to be programmed was the telescope movement. Since this project is monitoring the intensity of Polaris, a metho ...
Free-space optical communications have distinct advantages over
... The surface over which takes the same value is called the wave-front of the beam. Before entering the atmosphere light from far away sources forms plane waves, i.e. the wave-front of the beam is flat. Though, inside the atmosphere the speed of light varies as the inverse of the refractive index. A ...
... The surface over which takes the same value is called the wave-front of the beam. Before entering the atmosphere light from far away sources forms plane waves, i.e. the wave-front of the beam is flat. Though, inside the atmosphere the speed of light varies as the inverse of the refractive index. A ...
ARGOS - The Laser Guide Star System for the LBT
... be seen after several hours of integration time even with the LBT‟s eight meter mirrors. The multiplexing capability of the LUCIFER MOS instrument allows for efficient observing of up to twenty galaxies in one pointing. Here only a few of the observed spectra in one frame are shown. ...
... be seen after several hours of integration time even with the LBT‟s eight meter mirrors. The multiplexing capability of the LUCIFER MOS instrument allows for efficient observing of up to twenty galaxies in one pointing. Here only a few of the observed spectra in one frame are shown. ...
スライド タイトルなし - X-ray Astronomy Group at ISAS
... Astro-E X-ray telescopes consist of nested conical thin-foil mirrors based on a similar design concept to the ASCA telescopes, but with several improvements. The half power-diameter (HPD) is better than ASCA's by about a factor of two. The ratio of the focal length to the diameter is smaller, making ...
... Astro-E X-ray telescopes consist of nested conical thin-foil mirrors based on a similar design concept to the ASCA telescopes, but with several improvements. The half power-diameter (HPD) is better than ASCA's by about a factor of two. The ratio of the focal length to the diameter is smaller, making ...
TALON - The Telescope Alert Operation
... packets; image object lists and site information. Site information is not stored, but is passed directly to the outgoing socket for the TALON monitor. Image object list packets are sent to decoding modules dedicated to each of the telescopes. Incoming networks such as GCN are also given their own de ...
... packets; image object lists and site information. Site information is not stored, but is passed directly to the outgoing socket for the TALON monitor. Image object list packets are sent to decoding modules dedicated to each of the telescopes. Incoming networks such as GCN are also given their own de ...
Finishing an engineered lightweight 396mm CA, f1.376 concave
... variables are things seasoned opticians should have learned in their first few years of polishing on a daily basis. Yet the mysticism surrounding lightweight mirrors has persisted for nearly 100 years. What we’ve seen is that the machine and the tool influence the smoothness, figure, control and co ...
... variables are things seasoned opticians should have learned in their first few years of polishing on a daily basis. Yet the mysticism surrounding lightweight mirrors has persisted for nearly 100 years. What we’ve seen is that the machine and the tool influence the smoothness, figure, control and co ...
PATBNTED OCT. 29. 1907. TELESCOPE.
... The object of my invention is to provide a telescope trapezoit'lal prism and the hypotenuse face of the of this character having high magnifying and light ‘ right, angled prism are either parallel or, preferably, 70 gathering power for its dimensions and so proportioned coincident. \\'hethcr these f ...
... The object of my invention is to provide a telescope trapezoit'lal prism and the hypotenuse face of the of this character having high magnifying and light ‘ right, angled prism are either parallel or, preferably, 70 gathering power for its dimensions and so proportioned coincident. \\'hethcr these f ...
Experiment 9 - The Ohio State University
... rays of light coming from an “object” (=physical thing) and bends them in a way such that they appear to be coming from an “image.” It is important to understand that when you look through a lens, you see the image created by the lens NOT the object itself 1. Identifying converging and diverging len ...
... rays of light coming from an “object” (=physical thing) and bends them in a way such that they appear to be coming from an “image.” It is important to understand that when you look through a lens, you see the image created by the lens NOT the object itself 1. Identifying converging and diverging len ...
System Level # Requirements Document
... report “Astronomy and Astrophysics in the New Millennium” (also known as the 2001 “Decadal Survey”). Responding to the Decadal Survey report, TMT is a 30-meter aperture facility with broad capabilities operating over the wavelength range 0.3-30 µm. TMT provides 9 times the collecting area of the cur ...
... report “Astronomy and Astrophysics in the New Millennium” (also known as the 2001 “Decadal Survey”). Responding to the Decadal Survey report, TMT is a 30-meter aperture facility with broad capabilities operating over the wavelength range 0.3-30 µm. TMT provides 9 times the collecting area of the cur ...
GM-8 manual-05.cdr
... time the system records the correction you make. It takes the worm gear eight minutes to make one complete revolution, hence the need to guide for eight minutes. The second step is to play back the corrections you made during the recording phase. The microcomputer inside the electronic console does ...
... time the system records the correction you make. It takes the worm gear eight minutes to make one complete revolution, hence the need to guide for eight minutes. The second step is to play back the corrections you made during the recording phase. The microcomputer inside the electronic console does ...
Slide 1
... Red error bars: Includes noise increase from subtracting 220 GHz to remove mid lat dust ...
... Red error bars: Includes noise increase from subtracting 220 GHz to remove mid lat dust ...
The GMT Consortium Large Earth Finder Sagi Ben-Ami Smithsonian Astrophysical Observatory
... A mosaic Mangin Fold Mirror of to three correct 300x400mm operating at a cylindrical fieldR4 curvature quasi-Littrow configuration. ...
... A mosaic Mangin Fold Mirror of to three correct 300x400mm operating at a cylindrical fieldR4 curvature quasi-Littrow configuration. ...
Wavefront Aberrations
... In the paraxial approximation, we keep just the first term on the right hand side. Seidel aberrations result from the third-order (3) term. Seidel Snell’s Law: n1( 3/3!) ≈ n2( 3/3!) In fact, an exact analysis of all aberrations can be done by not using any approximations, following a ...
... In the paraxial approximation, we keep just the first term on the right hand side. Seidel aberrations result from the third-order (3) term. Seidel Snell’s Law: n1( 3/3!) ≈ n2( 3/3!) In fact, an exact analysis of all aberrations can be done by not using any approximations, following a ...
Optical telescope
An optical telescope is a telescope that gathers and focuses light, mainly from the visible part of the electromagnetic spectrum, to create a magnified image for direct view, or to make a photograph, or to collect data through electronic image sensors.There are three primary types of optical telescope: refractors, which use lenses (dioptrics) reflectors, which use mirrors (catoptrics) catadioptric telescopes, which combine lenses and mirrorsA telescope's light gathering power and ability to resolve small detail is directly related to the diameter (or aperture) of its objective (the primary lens or mirror that collects and focuses the light). The larger the objective, the more light the telescope collects and the finer detail it resolves.People use telescopes and binoculars for activities such as observational astronomy, ornithology, pilotage and reconnaissance, and watching sports or performance arts.