A Detection Method for Small Kuiper Belt Objects: The Search for
... where ϕmax is the maximum expected angular radius of KBOs (this value is not critical since we know that big KBOs are very rare; i.e., δ(ϕ, i) must be vanishingly small for large ϕ) and ϕlim is the angular radius of the smallest KBO detectable by occultation. Let us now discuss the three main parame ...
... where ϕmax is the maximum expected angular radius of KBOs (this value is not critical since we know that big KBOs are very rare; i.e., δ(ϕ, i) must be vanishingly small for large ϕ) and ϕlim is the angular radius of the smallest KBO detectable by occultation. Let us now discuss the three main parame ...
29 Reflection and Refraction
... When you watch the sun set, you see the sun for several minutes after it has really sunk below the horizon. Since the density of the atmosphere changes gradually, refracted rays bend gradually to produce a curved path. The same thing occurs at sunrise, so our daytimes are about 5 minutes longer beca ...
... When you watch the sun set, you see the sun for several minutes after it has really sunk below the horizon. Since the density of the atmosphere changes gradually, refracted rays bend gradually to produce a curved path. The same thing occurs at sunrise, so our daytimes are about 5 minutes longer beca ...
Variability of young solar-type stars: Spot cycles, rotation
... This thesis could not have become a reality without the support and input of my supervisors Dr. Lauri Jetsu and Dr. Thomas Hackman who introduced me to the fields of stellar activity and time series analysis all the way back during writing my bachelor’s thesis. I am grateful for their practical suppo ...
... This thesis could not have become a reality without the support and input of my supervisors Dr. Lauri Jetsu and Dr. Thomas Hackman who introduced me to the fields of stellar activity and time series analysis all the way back during writing my bachelor’s thesis. I am grateful for their practical suppo ...
![arXiv:1601.01542v1 [astro-ph.GA] 7 Jan 2016](http://s1.studyres.com/store/data/017487687_1-243c4cbda96da53325dd347b0c588a3e-300x300.png)
- SelectedWorks
... ture (Dehnen & Binney 1998). For a dynamical entity such as the Galaxy, this structure is as fundamental as the spatial arrangement of its stars, and should contain a mass of information as to the system’s current state, as well as archaeological clues as to how it formed. Unfortunately, such data f ...
... ture (Dehnen & Binney 1998). For a dynamical entity such as the Galaxy, this structure is as fundamental as the spatial arrangement of its stars, and should contain a mass of information as to the system’s current state, as well as archaeological clues as to how it formed. Unfortunately, such data f ...
90377 Sedna
... squared, divided by its semi-major axis to the 3/2 power, times a constant 1.7×1016 .[58](see equation 4) If an object’s Λ is greater than 1, then that object will eventually clear its neighbourhood, and it can be considered for planethood. Using the unlikely highest estimated mass for Sedna of 2×10 ...
... squared, divided by its semi-major axis to the 3/2 power, times a constant 1.7×1016 .[58](see equation 4) If an object’s Λ is greater than 1, then that object will eventually clear its neighbourhood, and it can be considered for planethood. Using the unlikely highest estimated mass for Sedna of 2×10 ...
Diffraction-Based Sensitivity Analysis of Apodized Pupil Mapping
... By pupil mapping we mean a system of two lenses, or mirrors, that takes a flat input field at the entrance pupil and produce an output field that is amplitude modified but still flat in phase (at least for on-axis sources). The Pupil Mapping Concept. The pupil mapping concept has received considerab ...
... By pupil mapping we mean a system of two lenses, or mirrors, that takes a flat input field at the entrance pupil and produce an output field that is amplitude modified but still flat in phase (at least for on-axis sources). The Pupil Mapping Concept. The pupil mapping concept has received considerab ...
CHARACTERIZING DUST ATTENUATION IN LOCAL STAR FORMING GALAXIES: UV AND... REDDENING ABSTRACT The dust attenuation for a sample of ∼10000 local (z ....
... provided E(B − V )MW with the extinction curve of Fitzpatrick (1999). For the GALEX bands, we adopt the values of kFUV = 8.067 and kNUV = 8.05, which represent the average value of the MW extinction curve convolved with each filter on SEDs with UV slopes −2.5 < β < 0.5, the typical range for our SFG ...
... provided E(B − V )MW with the extinction curve of Fitzpatrick (1999). For the GALEX bands, we adopt the values of kFUV = 8.067 and kNUV = 8.05, which represent the average value of the MW extinction curve convolved with each filter on SEDs with UV slopes −2.5 < β < 0.5, the typical range for our SFG ...
The deep OB star population in Carina from the VST Photometric Hα
... Mapping these intrinsically luminous objects is important for another reason: they have long been valued as distant and bright backlighters of the ISM – much of what is known about interstellar extinction has been deduced from fitting the spectral energy distributions (SEDs) of OB stars (e.g. Cardel ...
... Mapping these intrinsically luminous objects is important for another reason: they have long been valued as distant and bright backlighters of the ISM – much of what is known about interstellar extinction has been deduced from fitting the spectral energy distributions (SEDs) of OB stars (e.g. Cardel ...
