Determining the Effect of Diffuse X-ray Emission on Point Source Detection
... was launched into orbit in 1999 to view the central region of our galaxy, the Milky Way. The data from all of these observations have been compounded into a single image of the 40 parsecs (pc) surrounding Sagittarius A*, the compact radio source that is thought to mark the location of the supermassi ...
... was launched into orbit in 1999 to view the central region of our galaxy, the Milky Way. The data from all of these observations have been compounded into a single image of the 40 parsecs (pc) surrounding Sagittarius A*, the compact radio source that is thought to mark the location of the supermassi ...
Resonant-Cavity Light-Emitting Diodes: a review
... quantisation in microcavities to enhance spontaneous emission properties, directionality, intensity and purity can as well denote key performance characteristics of LEDs. These assets make RCLEDs particularly suited for optical communication applications, more specifically data communication via Pla ...
... quantisation in microcavities to enhance spontaneous emission properties, directionality, intensity and purity can as well denote key performance characteristics of LEDs. These assets make RCLEDs particularly suited for optical communication applications, more specifically data communication via Pla ...
talk
... suggesting a chiral phase transition in RHIC collisions. We note that in most quark-matter scenarios, the QGP phase transition is usually accompanied by a chiral phase transition at about the same critical temperature. August 11, 2005 ...
... suggesting a chiral phase transition in RHIC collisions. We note that in most quark-matter scenarios, the QGP phase transition is usually accompanied by a chiral phase transition at about the same critical temperature. August 11, 2005 ...
What causes the large extensions of red supergiant
... The normalized flux spectra show typical spectra of RSGs in the K band (cf. Lançon et al. 2007; Arroyo-Torres et al. 2013). The flux variations at wavelengths below about 2.0 μm are due to a higher noise level, possibly caused by the lower atmospheric transmission. In the K-2.3 band, we observe a de ...
... The normalized flux spectra show typical spectra of RSGs in the K band (cf. Lançon et al. 2007; Arroyo-Torres et al. 2013). The flux variations at wavelengths below about 2.0 μm are due to a higher noise level, possibly caused by the lower atmospheric transmission. In the K-2.3 band, we observe a de ...
The Stellar Initial Mass Function and Beyond
... needed to clarify the quantitative details of this process and the initial properties of the collapsing clumps. In any case, many simulations of cloud collapse and fragmentation, both with and without turbulence, have demonstrated the formation of bound clumps whose masses are typically comparable t ...
... needed to clarify the quantitative details of this process and the initial properties of the collapsing clumps. In any case, many simulations of cloud collapse and fragmentation, both with and without turbulence, have demonstrated the formation of bound clumps whose masses are typically comparable t ...
Vacuum-ultraviolet to infrared supercontinuum in hydrogen
... Fig. 1. Experimental setup. (a) A kagomé-PCF is filled with hydrogen using a pair of gas cells with MgF2 windows. Ultrashort few-microjoule pulses are launched into the fiber using an achromatic lens. Two chirped mirrors compensate for pulse lengthening in air. (b) Diagnostics. Upper, the VUV spectr ...
... Fig. 1. Experimental setup. (a) A kagomé-PCF is filled with hydrogen using a pair of gas cells with MgF2 windows. Ultrashort few-microjoule pulses are launched into the fiber using an achromatic lens. Two chirped mirrors compensate for pulse lengthening in air. (b) Diagnostics. Upper, the VUV spectr ...
View PDF - Sara Seager
... discovery and follow-up observations with JWST and other telescopes. However, stars with spectral types later than M5 are rarer and optically faint. They could be observed advantageously at nearinfrared wavelengths, but this would greatly increase the mission’s cost, complexity, and risk. Furthermor ...
... discovery and follow-up observations with JWST and other telescopes. However, stars with spectral types later than M5 are rarer and optically faint. They could be observed advantageously at nearinfrared wavelengths, but this would greatly increase the mission’s cost, complexity, and risk. Furthermor ...
Document
... light is: 299,792.458 km/s It takes approximately 8.3 min for light from the sun the reach the earth. Taking the distance of the sun from Earth into account, which is 150,000,000 km, and the fact that light travels at 300,000 km/s, With the use of the SI units for wavelength (l), frequency (¦) and s ...
... light is: 299,792.458 km/s It takes approximately 8.3 min for light from the sun the reach the earth. Taking the distance of the sun from Earth into account, which is 150,000,000 km, and the fact that light travels at 300,000 km/s, With the use of the SI units for wavelength (l), frequency (¦) and s ...
Semiconductor lasers Nobel Lecture, December 11, 1964
... (I) The creation of quantum frequency oscillators of high stability and the transition to atomic standards of time made it possible to raise the question of solving the problem of the properties of atomic time. Dicke 2 in his paper at the first conference on quantum electronics pointed out the possi ...
... (I) The creation of quantum frequency oscillators of high stability and the transition to atomic standards of time made it possible to raise the question of solving the problem of the properties of atomic time. Dicke 2 in his paper at the first conference on quantum electronics pointed out the possi ...
They might be giants: luminosity class, planet frequency, and planet
... and exclude sub-giant and giant stars. Brown et al. (2011) used D51 (Mg Ib line) photometry and Sloan gD51 color to exclude giants, however this is also sensitive to temperature and metallicity and is not available for all targets. The KIC includes Sloan (griz) and 2MASS (JHK) magnitudes; stellar pa ...
... and exclude sub-giant and giant stars. Brown et al. (2011) used D51 (Mg Ib line) photometry and Sloan gD51 color to exclude giants, however this is also sensitive to temperature and metallicity and is not available for all targets. The KIC includes Sloan (griz) and 2MASS (JHK) magnitudes; stellar pa ...
Di raction and Interference PRECAUTION
... This experiment is greatly facilitated by the use of a laser as a light source. The laser light is highly monochromatic and coherent. Coherence means that there are surfaces, in this experiment approximately planes, in which the light is in phase. When such light falls on a ~ oscillates in phase ove ...
... This experiment is greatly facilitated by the use of a laser as a light source. The laser light is highly monochromatic and coherent. Coherence means that there are surfaces, in this experiment approximately planes, in which the light is in phase. When such light falls on a ~ oscillates in phase ove ...
Word File - UNESCO World Heritage Centre
... World's Astronomy Monuments is a project of serial transnational group of historico-cultural monuments, which have outstanding universal value and are connected with other observatories, architectural complexes and separate buildings in the world. Within the framework of the thematic initiative "Ast ...
... World's Astronomy Monuments is a project of serial transnational group of historico-cultural monuments, which have outstanding universal value and are connected with other observatories, architectural complexes and separate buildings in the world. Within the framework of the thematic initiative "Ast ...
Evolution, Mass Loss and Variability of Low and Intermediate
... envelope giving a planetary nebula (probably bipolar, certainly asymmetric). The central remnant star will be a close binary. The observed fraction of red giants that show ellipsoidal variability, combined with models for ellipsoidal light curves can be used to estimate the fraction of planetary neb ...
... envelope giving a planetary nebula (probably bipolar, certainly asymmetric). The central remnant star will be a close binary. The observed fraction of red giants that show ellipsoidal variability, combined with models for ellipsoidal light curves can be used to estimate the fraction of planetary neb ...
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.