Chapter 1 Seeing the Light: The Art and Science of Astronomy
... and Saturn. These celestial bodies aren’t wandering through the stars; they orbit around the Sun, our solar system’s central star. Today astronomers know that planets can be smaller or bigger than Earth, but they all are much smaller than the Sun. The planets in our solar system are so close to Eart ...
... and Saturn. These celestial bodies aren’t wandering through the stars; they orbit around the Sun, our solar system’s central star. Today astronomers know that planets can be smaller or bigger than Earth, but they all are much smaller than the Sun. The planets in our solar system are so close to Eart ...
Lecture 5, Infrared Astronomy
... emission from the dust itself. Cirrus: emission from dust in the ISM dominates in far-IR at high galactic latitudes and in all IR bands in the Galactic plane Cosmic IR background: summed emission from distant, unresolved galaxies. Traces history of star formation. ...
... emission from the dust itself. Cirrus: emission from dust in the ISM dominates in far-IR at high galactic latitudes and in all IR bands in the Galactic plane Cosmic IR background: summed emission from distant, unresolved galaxies. Traces history of star formation. ...
File
... boxes: box A is full of books and weighs 133 N, box B has more books and weighs 111 N, box C contains his music collection on CDs and weighs 65 N, and box D contains clothes and weighs 47 N. The height of each box is 0.30 m. The center of gravity of each of the boxes is located at its center. In pre ...
... boxes: box A is full of books and weighs 133 N, box B has more books and weighs 111 N, box C contains his music collection on CDs and weighs 65 N, and box D contains clothes and weighs 47 N. The height of each box is 0.30 m. The center of gravity of each of the boxes is located at its center. In pre ...
wk11
... • The speed at which stars move (on average) within an elliptical galaxy can be measured by its `velocity dispersion' (or spread in velocity among the different stars relative to us) along the line of sight. • The indication is that elliptical galaxies too contain dark matter (a somewhat higher prop ...
... • The speed at which stars move (on average) within an elliptical galaxy can be measured by its `velocity dispersion' (or spread in velocity among the different stars relative to us) along the line of sight. • The indication is that elliptical galaxies too contain dark matter (a somewhat higher prop ...
Module 5 Modelling the universe - Pearson Schools and FE Colleges
... A planet is a relatively cold object in a nearly circular orbit around a star. Very little is known about planets other than the planets that orbit around our own star, the Sun. Telescopes only now have sufficient accuracy to detect the slight wobble of some stars as a result of planets rotating aro ...
... A planet is a relatively cold object in a nearly circular orbit around a star. Very little is known about planets other than the planets that orbit around our own star, the Sun. Telescopes only now have sufficient accuracy to detect the slight wobble of some stars as a result of planets rotating aro ...
What Lies Beyond
... and Motions of the Stars Apparent magnitude is a measure of the amount of light received from a celestial object This measure contrasts with luminosity – the rate at which electromagnetic energy is emitted from a celestial object Proper motion is the term for the angular velocity of a star as ...
... and Motions of the Stars Apparent magnitude is a measure of the amount of light received from a celestial object This measure contrasts with luminosity – the rate at which electromagnetic energy is emitted from a celestial object Proper motion is the term for the angular velocity of a star as ...
lecture1_1 - UMass Astronomy
... • These errors are “perturbations” that affect measures in an unpredictable way, sometime in excess, some other time in deficiency, i.e. they can unpredictably add or subtract an unknown amount from the true value • These errors are NOT mistakes; they are what makes an infinitely accurate measure im ...
... • These errors are “perturbations” that affect measures in an unpredictable way, sometime in excess, some other time in deficiency, i.e. they can unpredictably add or subtract an unknown amount from the true value • These errors are NOT mistakes; they are what makes an infinitely accurate measure im ...
DTU Chap 16 Galaxies v2
... The distances and recessional velocities of distant galaxies are plotted on this graph. The straight line is the “best fit” for the data. This linear relationship between distance and speed is called the Hubble law. For historical reasons, distances between galaxies, clusters of galaxies, and superc ...
... The distances and recessional velocities of distant galaxies are plotted on this graph. The straight line is the “best fit” for the data. This linear relationship between distance and speed is called the Hubble law. For historical reasons, distances between galaxies, clusters of galaxies, and superc ...
Galaxy Formation and Evolution
... different populations have different luminosity so there is a lot of scatter in the L-M relation. Younger populations are brighter (more massive stars). A very important statistic is the luminosity probability distribution function: LF. Most galaxies are low-L so they dominate the number density. Ho ...
... different populations have different luminosity so there is a lot of scatter in the L-M relation. Younger populations are brighter (more massive stars). A very important statistic is the luminosity probability distribution function: LF. Most galaxies are low-L so they dominate the number density. Ho ...
Document
... same plane and in the same direction. Halo stars also orbit the center of the galaxy, but with orbits randomly inclined to the disk of the galaxy. • How long does it take the Sun to orbit the galactic center? • Each orbit takes about 230 million years. • How do we determine galactic mass from stella ...
... same plane and in the same direction. Halo stars also orbit the center of the galaxy, but with orbits randomly inclined to the disk of the galaxy. • How long does it take the Sun to orbit the galactic center? • Each orbit takes about 230 million years. • How do we determine galactic mass from stella ...
Hot Stars With Cool Companions
... not be resolvable by current imaging systems are likely to have the largest impact on planet formation, a spectroscopic multiplicity survey of nearby intermediate-mass stars is needed. The multiplicity of A- and B-type stars can also help constrain the binary star formation mechanism and the relevan ...
... not be resolvable by current imaging systems are likely to have the largest impact on planet formation, a spectroscopic multiplicity survey of nearby intermediate-mass stars is needed. The multiplicity of A- and B-type stars can also help constrain the binary star formation mechanism and the relevan ...
Is Draco II one of the faintest dwarf galaxies? First study from Keck
... Furthermore, the stark difference between the spectra of stars 2 and 10, which must have very similar stellar parameters as they are confirmed Dra II member stars with almost identical colours and magnitudes ((0.53,18.87) and (0.55,18.98)), implies that these two member stars have significantly diff ...
... Furthermore, the stark difference between the spectra of stars 2 and 10, which must have very similar stellar parameters as they are confirmed Dra II member stars with almost identical colours and magnitudes ((0.53,18.87) and (0.55,18.98)), implies that these two member stars have significantly diff ...
Let there be an astronomical body i that is an aggregate of a very
... While any given fractal structure may feature other scaling behaviors, (1) and (2) are sufficient for the present analysis. Modern observations indicate that the distribution of galaxies throughout the observable universe is, to a certain extent, hierarchical and self-similar. The degree to which th ...
... While any given fractal structure may feature other scaling behaviors, (1) and (2) are sufficient for the present analysis. Modern observations indicate that the distribution of galaxies throughout the observable universe is, to a certain extent, hierarchical and self-similar. The degree to which th ...
KINEMATIC DISCOVERY OF A STELLAR STREAM LOCATED IN
... The metal-poor giant stars selected using the velocity criteria (i.e., red points in the top panels of Figure 3) are mostly clustered around [(g − r)0 , g0 ] = [0.55, 18.8] in the on-stream field (top left panel of Figure 3), while the more metal-rich stars (light blue points) scatter throughout the ...
... The metal-poor giant stars selected using the velocity criteria (i.e., red points in the top panels of Figure 3) are mostly clustered around [(g − r)0 , g0 ] = [0.55, 18.8] in the on-stream field (top left panel of Figure 3), while the more metal-rich stars (light blue points) scatter throughout the ...
(massive) binary stars
... focus on time-domain astronomy, is an ideal tool for collecting spectroscopic observational material required for the success of the proposed project. Since the project focuses mainly on bright binary stars, the desired signal-to-noise ratio (S/N) of ~100 per pixel can be obtained with 2m class tele ...
... focus on time-domain astronomy, is an ideal tool for collecting spectroscopic observational material required for the success of the proposed project. Since the project focuses mainly on bright binary stars, the desired signal-to-noise ratio (S/N) of ~100 per pixel can be obtained with 2m class tele ...
The local spiral structure of the Milky Way
... 1232 (Fig. 1). Still, today, there is no general agreement on the number, locations, orientations, and properties of the Milky Way’s spiral arms. The main impediments to determining spiral structure are the vast distances (up to about 60,000 ly) to stars across its extent and extinction by interstel ...
... 1232 (Fig. 1). Still, today, there is no general agreement on the number, locations, orientations, and properties of the Milky Way’s spiral arms. The main impediments to determining spiral structure are the vast distances (up to about 60,000 ly) to stars across its extent and extinction by interstel ...
The Essential Cosmic Perspective, 6e
... Answer: Far from just sitting still, we on Earth are moving relative to the Sun, planets, stars, and even other galaxies. The rotation of Earth causes the most noticeable changes in the sky. This motion around Earth's axis causes the Sun and stars to appear to rise and set, producing what we call a ...
... Answer: Far from just sitting still, we on Earth are moving relative to the Sun, planets, stars, and even other galaxies. The rotation of Earth causes the most noticeable changes in the sky. This motion around Earth's axis causes the Sun and stars to appear to rise and set, producing what we call a ...
Observational Data
... from R23 by using [O II], [O III] vs Hβ (or Hα by assuming intrinsic ratio of Hβ/Hα constant) as metallicity indicator. If these z~2 starbursts are progenitors of z~1 EROs and local ellipticals, their metallicity should be high, at least near-solar or more. Metallicity is a good indicator of stellar ...
... from R23 by using [O II], [O III] vs Hβ (or Hα by assuming intrinsic ratio of Hβ/Hα constant) as metallicity indicator. If these z~2 starbursts are progenitors of z~1 EROs and local ellipticals, their metallicity should be high, at least near-solar or more. Metallicity is a good indicator of stellar ...
key - Scioly.org
... - You are allowed up to two reference sources (e.g. laptops, binders) and any number of calculators. Using outside sources (e.g. internet) is not allowed and will result in disqualification. - There are a total of 322 + 69i points spread over 190 questions. - The test is 21 pages long and consists o ...
... - You are allowed up to two reference sources (e.g. laptops, binders) and any number of calculators. Using outside sources (e.g. internet) is not allowed and will result in disqualification. - There are a total of 322 + 69i points spread over 190 questions. - The test is 21 pages long and consists o ...
Baryons at Low Densities: The Stellar Halos around Galaxies
... focused on theoretical and observational studies of the faint surface brightness envelopes surrounding luminous galaxies. This field of research has gained much attention in recent years owing to the availability of wide-field cameras, deep and large-area surveys, as well as advances in modelling ga ...
... focused on theoretical and observational studies of the faint surface brightness envelopes surrounding luminous galaxies. This field of research has gained much attention in recent years owing to the availability of wide-field cameras, deep and large-area surveys, as well as advances in modelling ga ...
Collaborations with East Asian VLBI stations
... Target sources : Galactic masers (H2O@22GHz, SiO@43GHz) New aspect: dual-beam for phase-referencing ...
... Target sources : Galactic masers (H2O@22GHz, SiO@43GHz) New aspect: dual-beam for phase-referencing ...
Maximum Mass Limit of Stars on the Main Sequence
... young clusters. In this method, growth is promoted by the size and composition of the stars accretion domain. As mass increases, the gravitational reach increases as well. This implies that stars that are born in the center of a cluster have a greater opportunity to reach higher masses. This is part ...
... young clusters. In this method, growth is promoted by the size and composition of the stars accretion domain. As mass increases, the gravitational reach increases as well. This implies that stars that are born in the center of a cluster have a greater opportunity to reach higher masses. This is part ...
supplemental materials.
... profile would appear in terms of its luminosity and color. The radial abundance profile describes the composition of a star as a function of radius and is thus a more detailed version of metallicity and helium abundance. The computer models evolve a star by updating the abundance profile to account ...
... profile would appear in terms of its luminosity and color. The radial abundance profile describes the composition of a star as a function of radius and is thus a more detailed version of metallicity and helium abundance. The computer models evolve a star by updating the abundance profile to account ...
Stellar Continua
... I. The Paschen Continuum • The Paschen continuum slope (B-V) is a good temperature indicator • Varies smoothly with changing temperature • Slope is negative (blue is brighter) for hot stars and positive (visual is brighter) for cooler stars • B-V works as a temperature indicator from 3500K to 9000K ...
... I. The Paschen Continuum • The Paschen continuum slope (B-V) is a good temperature indicator • Varies smoothly with changing temperature • Slope is negative (blue is brighter) for hot stars and positive (visual is brighter) for cooler stars • B-V works as a temperature indicator from 3500K to 9000K ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.