Le PHARE
... where prog-name is the name of the program, followed by a configuration file called with -c configurationfile and a list of parameters. Any -Parameter value statement in the command-line overrides the values written in the configuration file. The part enclosed within brackets is optional, if not spe ...
... where prog-name is the name of the program, followed by a configuration file called with -c configurationfile and a list of parameters. Any -Parameter value statement in the command-line overrides the values written in the configuration file. The part enclosed within brackets is optional, if not spe ...
1 L5: Diffraction L5 DIFFRACTION Objectives Aims From this
... known as Fresnel diffraction, can be mathematically very complex. However, calculations are greatly simplified if both the source and the screen are at very large distances from the aperture (i.e. if those distances are much greater than the diameter of the aperture). We will deal quantitatively onl ...
... known as Fresnel diffraction, can be mathematically very complex. However, calculations are greatly simplified if both the source and the screen are at very large distances from the aperture (i.e. if those distances are much greater than the diameter of the aperture). We will deal quantitatively onl ...
Stars and dust in the Galactic Center
... Mean radial velocities along the Galactic plane for our SINFONI Ks-surface brightness profile of the central Galaxy . . . . . . . . Extinction corrected radial distribution of stars and flux . . . . Stellar density in and orthogonal to the Galactic plane . . . . . Nuker fits to the late-type stars surf ...
... Mean radial velocities along the Galactic plane for our SINFONI Ks-surface brightness profile of the central Galaxy . . . . . . . . Extinction corrected radial distribution of stars and flux . . . . Stellar density in and orthogonal to the Galactic plane . . . . . Nuker fits to the late-type stars surf ...
Bulk Entanglement Spectrum Reveals Quantum
... subsystem A. Using the exponential decay of Cðr; r0 Þ at large distance jr − r0 j, we prove [28] that HA is short ranged and resembles a physical Hamiltonian, provided that the volume of A does not exceed that of B. In the opposite case, HA has bands at ∞ [28]; nonetheless, the low-lying part of th ...
... subsystem A. Using the exponential decay of Cðr; r0 Þ at large distance jr − r0 j, we prove [28] that HA is short ranged and resembles a physical Hamiltonian, provided that the volume of A does not exceed that of B. In the opposite case, HA has bands at ∞ [28]; nonetheless, the low-lying part of th ...
Chapter 17. Creating New Domains
... code for each Domain interacts with the Ptolemy kernel. This overview describes the general structure of the various classes that are used by a Domain in its interaction with the kernel. The Ptolemy User’s Manual has a more complete overview of this information. A functional block, such as an adder ...
... code for each Domain interacts with the Ptolemy kernel. This overview describes the general structure of the various classes that are used by a Domain in its interaction with the kernel. The Ptolemy User’s Manual has a more complete overview of this information. A functional block, such as an adder ...
as PDF - Minnesota Academy of Science
... the right, with ten streamel'8, is a naked-eye view of the same comet, made also by Professor Bond, October 10, following. The drawing below on the right (3) represents the comet as seen five days earlier, while its head W88 passing the bright star, Arcturus, which we, have chosen al! the reference ...
... the right, with ten streamel'8, is a naked-eye view of the same comet, made also by Professor Bond, October 10, following. The drawing below on the right (3) represents the comet as seen five days earlier, while its head W88 passing the bright star, Arcturus, which we, have chosen al! the reference ...
Kinematics of H $\ mathsf {_2} $ O masers in high
... In this section we present the VLBI maps of the observed water maser sources. From a comparison between these VLBI maps and those, at lower resolution, available in the literature, we can obtain further insights on the nature of the sources responsible for the water maser excitation. VLA maps of the ...
... In this section we present the VLBI maps of the observed water maser sources. From a comparison between these VLBI maps and those, at lower resolution, available in the literature, we can obtain further insights on the nature of the sources responsible for the water maser excitation. VLA maps of the ...
![[CII] in the nuclear region of M33: HerM33es](http://s1.studyres.com/store/data/016974860_1-2848b26c9bc0383003a9db0691112ce5-300x300.png)
Detection of Fluorescence from Single Molecules
... You will learn how to manipulate laser light using lenses. Specifically, you will measure the focal length of a lens. Using the light source and lens, you will verify the thin lens relation. Day 2: Alignment of the excitation pathway – Part 1 You will direct collimated laser light into the microscop ...
... You will learn how to manipulate laser light using lenses. Specifically, you will measure the focal length of a lens. Using the light source and lens, you will verify the thin lens relation. Day 2: Alignment of the excitation pathway – Part 1 You will direct collimated laser light into the microscop ...
nexstar_gt_60,80114.. - Downloads
... observing sessions to become familiar with your NexStar, so you should keep this manual handy until you have fully mastered your telescope’s operation. The NexStar hand control has built-in instructions to guide you through all the alignment procedures needed to have the telescope up and running in ...
... observing sessions to become familiar with your NexStar, so you should keep this manual handy until you have fully mastered your telescope’s operation. The NexStar hand control has built-in instructions to guide you through all the alignment procedures needed to have the telescope up and running in ...
the formation of giant molecular clouds
... and its relation to interesting physical parameters of the clouds are important, and are briefly reviewed in §2.1. The masses of giant molecular clouds (by which we mean all clouds of mass M > 10 4 M¯ ) can be estimated by several different techniques. Diffuse γ-ray emission, for example, can be use ...
... and its relation to interesting physical parameters of the clouds are important, and are briefly reviewed in §2.1. The masses of giant molecular clouds (by which we mean all clouds of mass M > 10 4 M¯ ) can be estimated by several different techniques. Diffuse γ-ray emission, for example, can be use ...
Astronomy WHS Sow
... With the discovery during the latter half of the 20th century of more objects within the Solar System and large objects around other stars, disputes arose over what should constitute a planet. There was particular disagreement over whether an object should be considered a planet if it was part of a ...
... With the discovery during the latter half of the 20th century of more objects within the Solar System and large objects around other stars, disputes arose over what should constitute a planet. There was particular disagreement over whether an object should be considered a planet if it was part of a ...
Two Upper Limits on the Rossiter-McLaughlin Effect, with Differing
... ∼ 6250 K (i.e., mass ∼ 1.2M ) tend to have an orbital axis misaligned with respect to the stellar spin axis, i.e., a high stellar obliquity. In contrast, the two axes are generally well-aligned for systems in which the host star is cooler (i.e., less massive). These authors noted that this could re ...
... ∼ 6250 K (i.e., mass ∼ 1.2M ) tend to have an orbital axis misaligned with respect to the stellar spin axis, i.e., a high stellar obliquity. In contrast, the two axes are generally well-aligned for systems in which the host star is cooler (i.e., less massive). These authors noted that this could re ...
How to measure seeing
... can divide astronomical observing into daily and night observing. The daily observing is limited by the brightness of the Sun. The Sun is the most sought after object for the daily observing. It is necessary to use a special solar filter to protect our sight. In day we can also observe other objects ...
... can divide astronomical observing into daily and night observing. The daily observing is limited by the brightness of the Sun. The Sun is the most sought after object for the daily observing. It is necessary to use a special solar filter to protect our sight. In day we can also observe other objects ...
Noise analysis of spectrometers based on speckle pattern
... sensitivity to experimental noise has not been fully investigated. Previous work on the photonic bandgap fiber bundle spectrometer considered several sources of noises, such as the discrete intensity resolution of a CCD array, the ambient light, and the variation of illumination condition of the bun ...
... sensitivity to experimental noise has not been fully investigated. Previous work on the photonic bandgap fiber bundle spectrometer considered several sources of noises, such as the discrete intensity resolution of a CCD array, the ambient light, and the variation of illumination condition of the bun ...
LCM SerieS
... the LCM telescope is up and running after locating just three bright celestial objects. It’s the perfect combination of power and portability. If you are new to astronomy, you may wish to start off by using the LCM’s built-in Sky Tour feature, which commands the LCM to find the most interesting obje ...
... the LCM telescope is up and running after locating just three bright celestial objects. It’s the perfect combination of power and portability. If you are new to astronomy, you may wish to start off by using the LCM’s built-in Sky Tour feature, which commands the LCM to find the most interesting obje ...
Chapter 5. Mouse and Tackball
... elements of the detector (as shown in Figure 0-9) and each will generate a current that is proportional to the amount of light striking it. These currents are usually very low, on the order of 50 to 100 nanoamperes, and must be amplified and converted to voltages before they can be easily interprete ...
... elements of the detector (as shown in Figure 0-9) and each will generate a current that is proportional to the amount of light striking it. These currents are usually very low, on the order of 50 to 100 nanoamperes, and must be amplified and converted to voltages before they can be easily interprete ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.