Infrared identification of high-mass X
... IBIS/ISGRI detector onboard the INTEGRAL observatory. Furthermore, they were all observed with other X-ray facilities to provide an accurate localization, which allowed us to determine the optical/NIR counterpart. The sample of 15 sources is given in Table 1. We present below our results on each sou ...
... IBIS/ISGRI detector onboard the INTEGRAL observatory. Furthermore, they were all observed with other X-ray facilities to provide an accurate localization, which allowed us to determine the optical/NIR counterpart. The sample of 15 sources is given in Table 1. We present below our results on each sou ...
Cosmos: A SpaceTime Odyssey (2014) Episode Scripts Based on
... And it includes the amount of helium in the cosmos and the glow of radio waves left over from the explosion. As it expanded, the universe cooled, and there was darkness for about 200 million years. Gravity was pulling together clumps of gas and heating them until the first stars burst into light on ...
... And it includes the amount of helium in the cosmos and the glow of radio waves left over from the explosion. As it expanded, the universe cooled, and there was darkness for about 200 million years. Gravity was pulling together clumps of gas and heating them until the first stars burst into light on ...
Extragalactic background light inferred from AEGIS
... assuming SED-type fractions that are a function of redshift within those magnitude bins. This is estimated by fitting our AEGIS galaxy sample to the 25 galaxy-SED templates from the SWIRE library. Then, luminosity densities are calculated from these magnitude bins from every galaxy population at all ...
... assuming SED-type fractions that are a function of redshift within those magnitude bins. This is estimated by fitting our AEGIS galaxy sample to the 25 galaxy-SED templates from the SWIRE library. Then, luminosity densities are calculated from these magnitude bins from every galaxy population at all ...
New Evidence for Mass-Loss from δ Cephei from H i 21
... the position of δ Cephei. Several marginally extended features of ∼ 3σ significance are also seen clustering near the stellar position in each of the next five contiguous channels, out to VLSR = 38.2 km s−1 . In Figure 3 we present velocity-integrated H i total intensity contours, derived from data sp ...
... the position of δ Cephei. Several marginally extended features of ∼ 3σ significance are also seen clustering near the stellar position in each of the next five contiguous channels, out to VLSR = 38.2 km s−1 . In Figure 3 we present velocity-integrated H i total intensity contours, derived from data sp ...
Cosmic Evolution - Planetarium Mannheim
... how could this sterile, elementary mixture give rise to the extraordinary diversity surrounding us today ...
... how could this sterile, elementary mixture give rise to the extraordinary diversity surrounding us today ...
an aluminum/calcium-rich, iron-poor, white dwarf star
... model for G149-28 was calculated with these parameters and the abundances of the observed elements Ca, Mg, Al, Fe, Ti, and Ni were varied until the model lines had approximately the same strength as the observed ones. This model was used as the starting point for the analysis of element abundances. ...
... model for G149-28 was calculated with these parameters and the abundances of the observed elements Ca, Mg, Al, Fe, Ti, and Ni were varied until the model lines had approximately the same strength as the observed ones. This model was used as the starting point for the analysis of element abundances. ...
the reality of the wolf 630 moving group - TigerPrints
... the efficient evaporation of younger clusters (i.e. interactions with giant molecular clouds Spitzer (1958)): they must either be formed outside of the disk or dynamically evolve there through some form of non-disruptive heating. Clearly open clusters, both young and old, are valuable targets in pie ...
... the efficient evaporation of younger clusters (i.e. interactions with giant molecular clouds Spitzer (1958)): they must either be formed outside of the disk or dynamically evolve there through some form of non-disruptive heating. Clearly open clusters, both young and old, are valuable targets in pie ...
Dust in Proto-Planetary Disks: Properties and Evolution
... Henning, 1997). Infrared spectroscopy roughly probes dust particles with sizes of up to a few microns (depending on material and wavelength), in the temperature range between 1500 and about 50 K. In protoplanetary disks, this implies that such spectra are sensitive to dust in the innermost regions, ...
... Henning, 1997). Infrared spectroscopy roughly probes dust particles with sizes of up to a few microns (depending on material and wavelength), in the temperature range between 1500 and about 50 K. In protoplanetary disks, this implies that such spectra are sensitive to dust in the innermost regions, ...
Grand Design and Flocculent Spirals in the Spitzer Survey of Stellar
... that later Hubble types have larger relative bar torques because the bulges are weaker. Combes & Elmegreen (1993) and Athanassoula & Misiriotis (2002) simulated flat and exponential bars by varying the inner rotation curve or halo concentration. Flat bars tend to occur in galaxies with sharply risin ...
... that later Hubble types have larger relative bar torques because the bulges are weaker. Combes & Elmegreen (1993) and Athanassoula & Misiriotis (2002) simulated flat and exponential bars by varying the inner rotation curve or halo concentration. Flat bars tend to occur in galaxies with sharply risin ...
FERMI GBM detections of four AXPs at soft gamma-rays
... Sketch drawing of a twisted magnetic loop. . . . . . . . . . . . . . . . Simulated inverse Compton spectrum. . . . . . . . . . . . . . . . . . Simulated magnetar spectra. . . . . . . . . . . . . . . . . . . . . . . . The response function (cm2 ) of the GBM detectors. . . . . . . . . . . The orientat ...
... Sketch drawing of a twisted magnetic loop. . . . . . . . . . . . . . . . Simulated inverse Compton spectrum. . . . . . . . . . . . . . . . . . Simulated magnetar spectra. . . . . . . . . . . . . . . . . . . . . . . . The response function (cm2 ) of the GBM detectors. . . . . . . . . . . The orientat ...
talk at lensing and dark matter conference Ohio state 2004
... • Optical depth = 2.18 +.45-.38 10-6, agrees with models (e.g. Gould and Han 1.63 10-6) • Also found optical depth as a function of (b,l) and gradient in optical depth ...
... • Optical depth = 2.18 +.45-.38 10-6, agrees with models (e.g. Gould and Han 1.63 10-6) • Also found optical depth as a function of (b,l) and gradient in optical depth ...
Dust in Proto-Planetary Disks: Properties and Evolution
... field, Schräpler and Henning, 2004, Dullemond and Dominik, 2005 and references therein) and the relative velocities may eventually become higher leading to the compaction of aggregates. Above the compaction limit, a runaway growth can be expected, where a few large aggregates grow by collisions wit ...
... field, Schräpler and Henning, 2004, Dullemond and Dominik, 2005 and references therein) and the relative velocities may eventually become higher leading to the compaction of aggregates. Above the compaction limit, a runaway growth can be expected, where a few large aggregates grow by collisions wit ...
Astronomy Astrophysics Carbon monoxide in the solar atmosphere &
... This way the convection in the lower part (ζ = 0) remains unaffected (r = 1), while the chromosphere (ζ = 1) can relax to hydrostatic, chemical, and radiative equilibrium. The initial models are constructed from the reference model without additional CO cooling (see Paper I). The lower part of the m ...
... This way the convection in the lower part (ζ = 0) remains unaffected (r = 1), while the chromosphere (ζ = 1) can relax to hydrostatic, chemical, and radiative equilibrium. The initial models are constructed from the reference model without additional CO cooling (see Paper I). The lower part of the m ...
Type II supernovae (Inma Dominguez)
... HELIUM SHELL BURNING – CONVECTIVE SHELL At central He exhaustion, He burning moves to a shell just outside the CO core The following evolution is characterized by the development of a convective He-burning shell limited by the CO core and by the H-burning shell. The chemical composition of this she ...
... HELIUM SHELL BURNING – CONVECTIVE SHELL At central He exhaustion, He burning moves to a shell just outside the CO core The following evolution is characterized by the development of a convective He-burning shell limited by the CO core and by the H-burning shell. The chemical composition of this she ...
WAVE OPTICS Jaan Kalda 1 Basics. Double slit diffraction.
... a1 (l1 )eikl1 and a2 (l2 )eikl2 adding up. The relative difference So, as long as we are not studying phenomena at ultra-short between l1 and l2 is small; hence, the dependence of the wave time-scale (ato- and picosecond-scale-physics), in order to be amplitude on distance affects the both waves in ...
... a1 (l1 )eikl1 and a2 (l2 )eikl2 adding up. The relative difference So, as long as we are not studying phenomena at ultra-short between l1 and l2 is small; hence, the dependence of the wave time-scale (ato- and picosecond-scale-physics), in order to be amplitude on distance affects the both waves in ...
09-03-08_Meixner
... • Dynamics of ISM in PDRs: is the ISM really hydrostatic? Do shocks contribute, how much? • Key to understanding how gas condenses into GMCs ...
... • Dynamics of ISM in PDRs: is the ISM really hydrostatic? Do shocks contribute, how much? • Key to understanding how gas condenses into GMCs ...
On the theory of light scattering in gases
... calculation of the radiation fields of the oscillators in the medium, but in the summation of the fields of the neighboring oscillators he made every effort to retain the homogeneity of the medium. In calculating the resultant sums, a large volume V is divided into cells, each of which contains stri ...
... calculation of the radiation fields of the oscillators in the medium, but in the summation of the fields of the neighboring oscillators he made every effort to retain the homogeneity of the medium. In calculating the resultant sums, a large volume V is divided into cells, each of which contains stri ...
Chapter 15 - dysoncentralne
... manufacture. The colors visible on the discs’ surfaces are characteristic of the light used in the photograph. Have students verify the ability of a compact disc to separate light into its particular spectrum by reflecting light from different sources off a compact disc’s surface. For example, sunli ...
... manufacture. The colors visible on the discs’ surfaces are characteristic of the light used in the photograph. Have students verify the ability of a compact disc to separate light into its particular spectrum by reflecting light from different sources off a compact disc’s surface. For example, sunli ...
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.