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... LBC contour maps of the old and young populations is presented in Figure 3. Stars belonging to the kinematically cold, more metal-rich population are represented by filled (open) star symbols when they are within 1 j (2 j) of the Ibata et al. (2006) radial velocity peak of this component (see the to ...
... LBC contour maps of the old and young populations is presented in Figure 3. Stars belonging to the kinematically cold, more metal-rich population are represented by filled (open) star symbols when they are within 1 j (2 j) of the Ibata et al. (2006) radial velocity peak of this component (see the to ...
Ten Years Of XMM-Newton: Scientific Achievements And Future Prospects Norbert Schartel
... Detection of the filament in the soft-band X-rays with a 5σ with kT = 0.91±0.25 keV Baryon over-density of ρ/<ρC> ≈150, which is consistent with expectations for the densest and hottest parts of the warm-hot intergalactic medium Werner et al., 2008, A&A 482, 29 ...
... Detection of the filament in the soft-band X-rays with a 5σ with kT = 0.91±0.25 keV Baryon over-density of ρ/<ρC> ≈150, which is consistent with expectations for the densest and hottest parts of the warm-hot intergalactic medium Werner et al., 2008, A&A 482, 29 ...
Refraction of Light
... strange image of a distant object. A fata morgana actually is a superposition of several images of one object. Typically one image is upright more or less above two inverted images that may be mingled together. The images may undergo rapid changes as the air layers move slightly up and down relative ...
... strange image of a distant object. A fata morgana actually is a superposition of several images of one object. Typically one image is upright more or less above two inverted images that may be mingled together. The images may undergo rapid changes as the air layers move slightly up and down relative ...
Physics for Scientists & Engineers 2
... ! One can see from this equation that total internal reflection can only occur for light traveling from a medium with a higher index of refraction to one with a lower index of refraction because the sine of an angle cannot be greater than 1 ...
... ! One can see from this equation that total internal reflection can only occur for light traveling from a medium with a higher index of refraction to one with a lower index of refraction because the sine of an angle cannot be greater than 1 ...
Black Hole Binaries in Quiescence
... XRBs are a key precursor class for gravitational wave sources – empirical demographics are key for use of LIGO as an astronomical facility Transients with duty cycle >50 years recurrence time unavailable, so total numbers cannot be inferred A0620 is an exception: archival optical data shows outburst ...
... XRBs are a key precursor class for gravitational wave sources – empirical demographics are key for use of LIGO as an astronomical facility Transients with duty cycle >50 years recurrence time unavailable, so total numbers cannot be inferred A0620 is an exception: archival optical data shows outburst ...
Document
... between log vmax and log(Mdisk = M*+Mgas) than with M* alone → suggests that the M/L ratio (and thus the fraction of dark matter) is ± constant in a large range of galactic masses (disk-halo ...
... between log vmax and log(Mdisk = M*+Mgas) than with M* alone → suggests that the M/L ratio (and thus the fraction of dark matter) is ± constant in a large range of galactic masses (disk-halo ...
Document
... poorly defined. Hence, a distance determined by this method should be regarded as an estimate – This method has nothing to do with Parallax! ...
... poorly defined. Hence, a distance determined by this method should be regarded as an estimate – This method has nothing to do with Parallax! ...
sun.galaxy.notes
... • Hot stars are ______ in color • Cooler stars are ______in color • An H-R diagram is a graph that relates star ________ to star ...
... • Hot stars are ______ in color • Cooler stars are ______in color • An H-R diagram is a graph that relates star ________ to star ...
Looking back in time to the big bang theory
... Element can be used as part of teaching this topic or as a consolidation. Learners should be introduced to at least one alternative theory to the Big Bang and reasons why the evidence supports the Big Bang rather than these other theories. Common difficulties and misconceptions include learners thin ...
... Element can be used as part of teaching this topic or as a consolidation. Learners should be introduced to at least one alternative theory to the Big Bang and reasons why the evidence supports the Big Bang rather than these other theories. Common difficulties and misconceptions include learners thin ...
Weighing Ultracompact Dwarf Galaxies in the Fornax Cluster
... the advantage that no external processes, like mergers or tidal disruption, are needed. A considerable darkmatter component is expected if this formation channel applies. How can a massive star cluster be discerned from a low-mass compact galaxy? The answer may be hidden in the seen and unseen mass ...
... the advantage that no external processes, like mergers or tidal disruption, are needed. A considerable darkmatter component is expected if this formation channel applies. How can a massive star cluster be discerned from a low-mass compact galaxy? The answer may be hidden in the seen and unseen mass ...
The End of the Dark Ages
... As the temperature of the cosmic bath decreases, atoms start to recombine and therefore decouple from CMB radiation at redshift ≈ 1100. Current models of cosmic structure formation based on CDM scenarios predict that the first objects in principle able to make stars should form at redshift z ≈ 30 an ...
... As the temperature of the cosmic bath decreases, atoms start to recombine and therefore decouple from CMB radiation at redshift ≈ 1100. Current models of cosmic structure formation based on CDM scenarios predict that the first objects in principle able to make stars should form at redshift z ≈ 30 an ...
The stellar populations of Lyman Break Galaxies at z~5 in...
... sample is compared with those of z=2-3 sample in the figure below, where the histogram is normalized so that its peak value equals unity for comparison. For sample galaxies at z=2 and z=3, we use sample by Shapley et al. (2001) and Shapley et al. (2005), respectively. Although the detailed algorithm ...
... sample is compared with those of z=2-3 sample in the figure below, where the histogram is normalized so that its peak value equals unity for comparison. For sample galaxies at z=2 and z=3, we use sample by Shapley et al. (2001) and Shapley et al. (2005), respectively. Although the detailed algorithm ...