Closed Loop Performance
... At 1000 Hz closed loop we can achieve 65 nm rms error in tower ~95nm “on-sky”. NOTE that this is a linear stretch. This is much better than the 190 nm rms ...
... At 1000 Hz closed loop we can achieve 65 nm rms error in tower ~95nm “on-sky”. NOTE that this is a linear stretch. This is much better than the 190 nm rms ...
Planets and Debris Disks: Results from a Spitzer/MIPS Search for IR
... Kuiper Belt objects - debris left over from the process of planet formation. This debris fills the solar system with dust produced by collisions between these small bodies and, in the case of comets, by sublimation of their surface ices. Though solar radiation removes the dust on timescales much sho ...
... Kuiper Belt objects - debris left over from the process of planet formation. This debris fills the solar system with dust produced by collisions between these small bodies and, in the case of comets, by sublimation of their surface ices. Though solar radiation removes the dust on timescales much sho ...
MIXED CHEMISTRY
... carbon (HAC) under UV irradiation have been sampled using time of flight (TOF) mass spectrometry. A notable feature is the appearance of … fullerenes such as C50 , C60 , and C70 . There is also evidence in these mass spectra for the ejection of small dehydrogenated polycyclic aromatic hydrocarbon (P ...
... carbon (HAC) under UV irradiation have been sampled using time of flight (TOF) mass spectrometry. A notable feature is the appearance of … fullerenes such as C50 , C60 , and C70 . There is also evidence in these mass spectra for the ejection of small dehydrogenated polycyclic aromatic hydrocarbon (P ...
The (galaxy-wide) IMF in giant elliptical galaxies: from top to bottom
... these systems. We suggest a two-stage formation scenario involving a time-dependent IMF to reconcile these observational constraints. In this model, an early strong starbursting stage with a top-heavy IMF is followed by a more prolonged stage with a bottom-heavy IMF. Such model is physically motivat ...
... these systems. We suggest a two-stage formation scenario involving a time-dependent IMF to reconcile these observational constraints. In this model, an early strong starbursting stage with a top-heavy IMF is followed by a more prolonged stage with a bottom-heavy IMF. Such model is physically motivat ...
mg_colloq - University of Massachusetts Amherst
... – Today, fraction of disk dominated SDSS galaxies with sSFR≤10-11 yr-1 and M*≥1010 M with n>2 is <5% – Dynamical properties being explored; certainly consistent with being massive, compact spheroids (Onodera et al. 2012; van Dokkum et al. 2011) – Some suggest that they include a significant (25-50% ...
... – Today, fraction of disk dominated SDSS galaxies with sSFR≤10-11 yr-1 and M*≥1010 M with n>2 is <5% – Dynamical properties being explored; certainly consistent with being massive, compact spheroids (Onodera et al. 2012; van Dokkum et al. 2011) – Some suggest that they include a significant (25-50% ...
Galaxies Chapter Twenty
... spiral, and irregular galaxies along with ellipticals • Giant elliptical galaxies are often found near the centers of rich clusters ...
... spiral, and irregular galaxies along with ellipticals • Giant elliptical galaxies are often found near the centers of rich clusters ...
Document
... spiral, and irregular galaxies along with ellipticals • Giant elliptical galaxies are often found near the centers of rich clusters ...
... spiral, and irregular galaxies along with ellipticals • Giant elliptical galaxies are often found near the centers of rich clusters ...
Star Location, Constellations and Intro to Solar System 1
... What to Remember - EW • What time during the day a star rises, is overhead, and sets changes with the seasons • look up on Star Chart (right ascension is the East-West location) • Changes 2 hours/month • Only on the Equator can all stars be viewed from a single location Hawaii or northern Chile a ...
... What to Remember - EW • What time during the day a star rises, is overhead, and sets changes with the seasons • look up on Star Chart (right ascension is the East-West location) • Changes 2 hours/month • Only on the Equator can all stars be viewed from a single location Hawaii or northern Chile a ...
Life of a Star Observations
... During this exercise, you will look at stars in the various stages of life, from before formation, through formation, life, and after death. Individual stars form, age, and die much too slowly to observe, so different stars must be seen in different stages of their life. For each object, sketch the ...
... During this exercise, you will look at stars in the various stages of life, from before formation, through formation, life, and after death. Individual stars form, age, and die much too slowly to observe, so different stars must be seen in different stages of their life. For each object, sketch the ...
10 Measuring The Stars
... The Hertzsprung–Russell Diagram Once many stars are plotted on an H–R diagram, a pattern begins to form: These are the 80 closest stars to us; note the dashed lines of constant radius. ...
... The Hertzsprung–Russell Diagram Once many stars are plotted on an H–R diagram, a pattern begins to form: These are the 80 closest stars to us; note the dashed lines of constant radius. ...
TRIFFID photometry of globular cluster cores – I. Photometric
... the photometric reductions. Photometry was first performed on archival HST/WFPC2 images of M15 in two filters – F439W which approximates to B, and F555W which approximates to V. These data were obtained under HST proposal GO 5324 (PI Brian Yanny). The first 43 rows and 51 columns of these images wer ...
... the photometric reductions. Photometry was first performed on archival HST/WFPC2 images of M15 in two filters – F439W which approximates to B, and F555W which approximates to V. These data were obtained under HST proposal GO 5324 (PI Brian Yanny). The first 43 rows and 51 columns of these images wer ...
March 15 Newsletter
... stretching endlessly into the distance. It is part of a filament in the outskirts of the Crab Nebula. On all sides I am enveloped in a milky-white fog. It is emission from the electrons. Stars are visible in every direction, for the nebula is transparent, so diffuse it is very nearly a vacuum. Never ...
... stretching endlessly into the distance. It is part of a filament in the outskirts of the Crab Nebula. On all sides I am enveloped in a milky-white fog. It is emission from the electrons. Stars are visible in every direction, for the nebula is transparent, so diffuse it is very nearly a vacuum. Never ...
Flow of Energy through the Star and Construction of Stellar Models
... transport. In addition, the "opacity" of the material to the motion of the energycarrying particles will also affect the efficiency. In the case of radiation, we have characterized this opacity by a collision cross section and the density. Another way to visualize this is via the notion of a mean fr ...
... transport. In addition, the "opacity" of the material to the motion of the energycarrying particles will also affect the efficiency. In the case of radiation, we have characterized this opacity by a collision cross section and the density. Another way to visualize this is via the notion of a mean fr ...
Dust in protoplanetary disks
... The derived inclination agrees well with the recent NIR inrferometric measurements for the inner (r ∼ 0.5 AU) disk Eisner et al. 2003; Millan-Gabet, Schloerb, & Traub 2001) nd with the constraint (less than 45!) obtained by the optical maging with the HST/Space Telescope Imaging Spectrograph STIS; G ...
... The derived inclination agrees well with the recent NIR inrferometric measurements for the inner (r ∼ 0.5 AU) disk Eisner et al. 2003; Millan-Gabet, Schloerb, & Traub 2001) nd with the constraint (less than 45!) obtained by the optical maging with the HST/Space Telescope Imaging Spectrograph STIS; G ...
Stellarium01 Starter Part A B Doc - ASTR101
... Start Stellarium. Use “Current Location” listed above by going to the Icon Bar at the left-hand side of the screen and find the Location window icon (shortcut key= “F6”, in some linux it is fn-f6) and click on it. Scroll through the list of locations in the window until you find the current location ...
... Start Stellarium. Use “Current Location” listed above by going to the Icon Bar at the left-hand side of the screen and find the Location window icon (shortcut key= “F6”, in some linux it is fn-f6) and click on it. Scroll through the list of locations in the window until you find the current location ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.