Stellar population models in the Near-Infrared Meneses
... spectral library of empirical stellar spectra. To construct a model, we determine the spectrum for each point in a so-called stellar isochrone, which is the distribution of stars with different masses in a single age and metallicity population. Subsequently, we integrate these spectra with a weight ...
... spectral library of empirical stellar spectra. To construct a model, we determine the spectrum for each point in a so-called stellar isochrone, which is the distribution of stars with different masses in a single age and metallicity population. Subsequently, we integrate these spectra with a weight ...
Here - Amateur Observers` Society of New York
... Observing Guide and The Observer's Handbook to plan your observations. When two or more celestial objects appear close together in the sky it is called a conjunction. These are regular occurrences that are listed in The Beginner’s Observing Guide, The Observer's Handbook and in popular astronomy mag ...
... Observing Guide and The Observer's Handbook to plan your observations. When two or more celestial objects appear close together in the sky it is called a conjunction. These are regular occurrences that are listed in The Beginner’s Observing Guide, The Observer's Handbook and in popular astronomy mag ...
Lecture 13 Local group chapter 4 of S+G
... which are dwarf ellipticals and irregulars with low mass; most are satellites of MW, M31 or M33 The gravitational interaction between these systems is complex but the local group is apparently bound. Major advantages – close and bright- all nearby enough that individual stars can be well measured as ...
... which are dwarf ellipticals and irregulars with low mass; most are satellites of MW, M31 or M33 The gravitational interaction between these systems is complex but the local group is apparently bound. Major advantages – close and bright- all nearby enough that individual stars can be well measured as ...
Tyler Gray - Angelfire
... observers of the Ferguson Observatory near Kenwood, CA have photographed G1 and four fainter M31 globulars. The astrophotographer is even better off, as he can gather the fainter light of the fine detail in the spiral arms, as in our image: Amateurs can obtain most striking pictures even with inexp ...
... observers of the Ferguson Observatory near Kenwood, CA have photographed G1 and four fainter M31 globulars. The astrophotographer is even better off, as he can gather the fainter light of the fine detail in the spiral arms, as in our image: Amateurs can obtain most striking pictures even with inexp ...
How do stars orbit in our galaxy?
... and expel them into space via supernovae and stellar winds. The supernovae and winds create hot bubbles in the interstellar medium, but the gas within these bubbles gradually slows and cools as they expand. Eventually, this gas cools enough to collect into clouds of atomic hydrogen. Further cooling ...
... and expel them into space via supernovae and stellar winds. The supernovae and winds create hot bubbles in the interstellar medium, but the gas within these bubbles gradually slows and cools as they expand. Eventually, this gas cools enough to collect into clouds of atomic hydrogen. Further cooling ...
19. Our Galaxy 19.1 The Milky Way Revealed Our goals for learning
... medium, but the gas moving outward with these bubbles gradually slows and cools. Eventually this gas cools enough to condense into clouds of atomic hydrogen. Further cooling allows atoms of hydrogen and other elements to collect into molecules, producing molecular clouds. These molecular clouds then ...
... medium, but the gas moving outward with these bubbles gradually slows and cools. Eventually this gas cools enough to condense into clouds of atomic hydrogen. Further cooling allows atoms of hydrogen and other elements to collect into molecules, producing molecular clouds. These molecular clouds then ...
DTU_9e_ch12
... Therefore, stars and other objects seen through interstellar clouds appear redder than they would otherwise. ...
... Therefore, stars and other objects seen through interstellar clouds appear redder than they would otherwise. ...
APOD 2016 Calendar
... missing from Charles Messier’s catalog of lustrous celestial sights. This colorful image from a small ground-based telescope shows off the galaxy’s gorgeous spiral arms traced by young, blue star clusters and pinkish star forming regions. Included are intriguing details of NGC 2903’s bright core, a ...
... missing from Charles Messier’s catalog of lustrous celestial sights. This colorful image from a small ground-based telescope shows off the galaxy’s gorgeous spiral arms traced by young, blue star clusters and pinkish star forming regions. Included are intriguing details of NGC 2903’s bright core, a ...
An Eclectic View of our Milky Way Galaxy
... for simple Galactic rotation. The Sun’s local standard of rest (LSR) velocity is ∼ 14 km s−1 rather than 20 km s−1 , the local circular velocity is 251±9 km s−1 rather than 220 km s−1 , and young groups of stars exhibit a 10–20 km s−1 “kick” relative to what is expected from Galactic rotation. By im ...
... for simple Galactic rotation. The Sun’s local standard of rest (LSR) velocity is ∼ 14 km s−1 rather than 20 km s−1 , the local circular velocity is 251±9 km s−1 rather than 220 km s−1 , and young groups of stars exhibit a 10–20 km s−1 “kick” relative to what is expected from Galactic rotation. By im ...
Galaxy Powerpoint Notes
... The creation of galaxies is a very mysterious topic as it is uncertain of how the universe was created. The most common theory however, is the theory of the Big Bang, which states that the universe expanded from a very dense state and continues to expand today. Another common prediction of how galax ...
... The creation of galaxies is a very mysterious topic as it is uncertain of how the universe was created. The most common theory however, is the theory of the Big Bang, which states that the universe expanded from a very dense state and continues to expand today. Another common prediction of how galax ...
X-ray Binaries in Nearby Galaxies
... and spatial distribution other properties, e.g., orbital period, donor masses known only for a few systems ...
... and spatial distribution other properties, e.g., orbital period, donor masses known only for a few systems ...
Galaxies - cloudfront.net
... billions of stars. Galaxies are divided into three types according to shape: spiral, elliptical, and irregular galaxies. • Spiral galaxies spin and appear as a rotating disk of stars and dust, with a bulge in the middle. Several spiral arms reach outward from the central bulge like the arms of a pin ...
... billions of stars. Galaxies are divided into three types according to shape: spiral, elliptical, and irregular galaxies. • Spiral galaxies spin and appear as a rotating disk of stars and dust, with a bulge in the middle. Several spiral arms reach outward from the central bulge like the arms of a pin ...
SPIRAL STRUCTURE IN THE OUTER GALACTIC
... According to the age and the places where they are located, clusters present a variety of challenges in deriving their intrinsic parameters. In the case of very young clusters, they are normally close to the Galactic plane where interstellar absorption and crowded stellar fields make membership assi ...
... According to the age and the places where they are located, clusters present a variety of challenges in deriving their intrinsic parameters. In the case of very young clusters, they are normally close to the Galactic plane where interstellar absorption and crowded stellar fields make membership assi ...
The Earth and Man In the Universe
... deduced from them, as to the distance of a star of the first magnitude, 46 for the minima and 497 for the maxima. It is conceivable that if the gauges were taken in every direction it would be possible to shape in this manner the exterior form of the visible starry universe, but as the circumpolar z ...
... deduced from them, as to the distance of a star of the first magnitude, 46 for the minima and 497 for the maxima. It is conceivable that if the gauges were taken in every direction it would be possible to shape in this manner the exterior form of the visible starry universe, but as the circumpolar z ...
The Physics of Massive Star Formation
... It is appealing to explain properties of massive stars in terms of massive cores …but if massive cores fragment to many stars, there is no direct core-star mapping, MF agreement is just a coincidence. Do massive cores fragment? ...
... It is appealing to explain properties of massive stars in terms of massive cores …but if massive cores fragment to many stars, there is no direct core-star mapping, MF agreement is just a coincidence. Do massive cores fragment? ...
THREE INTRIGUER NEBULAE IN CONSTELLATION CARINA
... (Hopp & Materne 1985, Nakazawa et al. 2000) that is the third nearest galaxy cluster to us, inhabiting the eastern part of this constellation (see picture on first page). Antlia cluster, also known as ACO S 0636, is centered at R.A. 10h 30m 01s Dec. –35° 19´ 35”. With a galactic latitude of 19 degr ...
... (Hopp & Materne 1985, Nakazawa et al. 2000) that is the third nearest galaxy cluster to us, inhabiting the eastern part of this constellation (see picture on first page). Antlia cluster, also known as ACO S 0636, is centered at R.A. 10h 30m 01s Dec. –35° 19´ 35”. With a galactic latitude of 19 degr ...
Starbursts – from 30 Doradus to Lyman
... local gas surface density (known as the Schmidt–Kennicutt law). Starburst properties, in addition, appear to be continuous across a range of amplitudes – and redshifts – suggesting a galaxy classification sequence similar to the Hubble tuning fork, but now from M82-like starbursts via ultraluminous ...
... local gas surface density (known as the Schmidt–Kennicutt law). Starburst properties, in addition, appear to be continuous across a range of amplitudes – and redshifts – suggesting a galaxy classification sequence similar to the Hubble tuning fork, but now from M82-like starbursts via ultraluminous ...
BSA Astronomy Merit Badge
... Limit movements to only those that are necessary. Don't massage or rub the person. Excessive, vigorous or jarring movements may trigger cardiac arrest. Move the person out of the cold. Move the person to a warm, dry location if possible. If you're unable to move the person out of the cold, shield hi ...
... Limit movements to only those that are necessary. Don't massage or rub the person. Excessive, vigorous or jarring movements may trigger cardiac arrest. Move the person out of the cold. Move the person to a warm, dry location if possible. If you're unable to move the person out of the cold, shield hi ...
PoS(EVN 2014)058 - Proceeding of science
... The aim of this project is to exploit the high-resolution capability and tremendous sensitivity of eMERLIN to assemble the most substantial radio dataset of an important massive stellar population within our Galaxy. COBRaS will produce extensive radio mapping of the OB rich stellar cluster at both C ...
... The aim of this project is to exploit the high-resolution capability and tremendous sensitivity of eMERLIN to assemble the most substantial radio dataset of an important massive stellar population within our Galaxy. COBRaS will produce extensive radio mapping of the OB rich stellar cluster at both C ...
ppt - Institute for Astronomy
... The solution is that FUor pairs are really quadruple systems which transformed from an unstable nonhierarchical configuration to an orderly hierarchical configuration. The quadruple then evolves slowly through viscous interactions until the components are so close that they erupt in FUor outbursts a ...
... The solution is that FUor pairs are really quadruple systems which transformed from an unstable nonhierarchical configuration to an orderly hierarchical configuration. The quadruple then evolves slowly through viscous interactions until the components are so close that they erupt in FUor outbursts a ...
A billion pixels, a billion stars
... tell us how many – end up being shepherded into “moving groups” of stars that travel together in velocity space and/or coordinate space. Finding and mapping these groups will give us a wealth of information about the large-scale structure and evolution of galactic discs. Away from the discs, the sta ...
... tell us how many – end up being shepherded into “moving groups” of stars that travel together in velocity space and/or coordinate space. Finding and mapping these groups will give us a wealth of information about the large-scale structure and evolution of galactic discs. Away from the discs, the sta ...
Star Formation in the Galaxy, An Observational Overview
... is again balanced by internal pressure. After this phase such stars will eject their outer atmospheres producing planetary nebula and leaving behind a white dwarf stellar remnant. More massive stars experience a more complex post-main sequence evolution during which they will fuse heavier elements i ...
... is again balanced by internal pressure. After this phase such stars will eject their outer atmospheres producing planetary nebula and leaving behind a white dwarf stellar remnant. More massive stars experience a more complex post-main sequence evolution during which they will fuse heavier elements i ...
Open cluster
An open cluster, also known as galactic cluster, is a group of up to a few thousand stars that were formed from the same giant molecular cloud and have roughly the same age. More than 1,100 open clusters have been discovered within the Milky Way Galaxy, and many more are thought to exist. They are loosely bound by mutual gravitational attraction and become disrupted by close encounters with other clusters and clouds of gas as they orbit the galactic center, resulting in a migration to the main body of the galaxy as well as a loss of cluster members through internal close encounters. Open clusters generally survive for a few hundred million years, with the most massive ones surviving for a few billion years. In contrast, the more massive globular clusters of stars exert a stronger gravitational attraction on their members, and can survive for longer. Open clusters have been found only in spiral and irregular galaxies, in which active star formation is occurring.Young open clusters may still be contained within the molecular cloud from which they formed, illuminating it to create an H II region. Over time, radiation pressure from the cluster will disperse the molecular cloud. Typically, about 10% of the mass of a gas cloud will coalesce into stars before radiation pressure drives the rest of the gas away.Open clusters are key objects in the study of stellar evolution. Because the cluster members are of similar age and chemical composition, their properties (such as distance, age, metallicity and extinction) are more easily determined than they are for isolated stars. A number of open clusters, such as the Pleiades, Hyades or the Alpha Persei Cluster are visible with the naked eye. Some others, such as the Double Cluster, are barely perceptible without instruments, while many more can be seen using binoculars or telescopes. The Wild Duck Cluster, M11, is an example.