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... • The Local Group counts more than 54 galaxies (the majority are dwarf galaxies). • Its center is somewhere between the Milky Way and the Andromeda galaxy (M31). • Its diameter is ~10,000,000 light years. • The total mass of the Local Group is ~1012 the mass of our sun, and more that 2 times the tot ...
... • The Local Group counts more than 54 galaxies (the majority are dwarf galaxies). • Its center is somewhere between the Milky Way and the Andromeda galaxy (M31). • Its diameter is ~10,000,000 light years. • The total mass of the Local Group is ~1012 the mass of our sun, and more that 2 times the tot ...
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... between yearly epochs at the 5 level with the CFHT Legacy Survey optical catalog. • Rule out sources with optical hosts with the colors and morphology of a star or quasar. • Follow up galaxy hosts that do not have an hard X-ray detection with optical spectroscopy to look for signs of an AGN. • Trig ...
... between yearly epochs at the 5 level with the CFHT Legacy Survey optical catalog. • Rule out sources with optical hosts with the colors and morphology of a star or quasar. • Follow up galaxy hosts that do not have an hard X-ray detection with optical spectroscopy to look for signs of an AGN. • Trig ...
The Strikingly Uniform, Highly Turbulent Interstellar Medium of the
... The [C ii] line was placed at the center of the reference spectral window (spw0), assuming the redshift derived from optical lines (z = 4.593; Wu et al. 2012); the other three spectral windows probing the continuum blue-ward of the line. The on-source integration time was 956 s in array configuratio ...
... The [C ii] line was placed at the center of the reference spectral window (spw0), assuming the redshift derived from optical lines (z = 4.593; Wu et al. 2012); the other three spectral windows probing the continuum blue-ward of the line. The on-source integration time was 956 s in array configuratio ...
Activity : Milky Way
... used within our own Galaxy (apart from the sector masked by the Galactic Center) to trace spiral arms. These include: Young galactic clusters Regions of absorbing gas & dust HII regions HI regions Giant Molecular Clouds • Spiral arms do not rotate at the same rate as the stars that comprise them, bu ...
... used within our own Galaxy (apart from the sector masked by the Galactic Center) to trace spiral arms. These include: Young galactic clusters Regions of absorbing gas & dust HII regions HI regions Giant Molecular Clouds • Spiral arms do not rotate at the same rate as the stars that comprise them, bu ...
ppt
... One finds that the Andromeda Galaxy and the Milky Way are approaching one another at a speed of 100 - 140 km/sec. Some astronomers believe that Andromeda and the Milky Way will eventually merge together. The impact is predicted to occur in about 3 billion years. In that case the two galaxies will l ...
... One finds that the Andromeda Galaxy and the Milky Way are approaching one another at a speed of 100 - 140 km/sec. Some astronomers believe that Andromeda and the Milky Way will eventually merge together. The impact is predicted to occur in about 3 billion years. In that case the two galaxies will l ...
Every large galaxy seems to have a supermassive black hole at its
... there and the galaxy is not — or at least there’s not much of it.” Riechers puts it somewhat differently. “This doesn’t imply that black holes ‘seed’ galaxies,” he says. “They both can form at the same time, but they don’t grow at the same rate.” In the early going, the black hole grows at a faster ...
... there and the galaxy is not — or at least there’s not much of it.” Riechers puts it somewhat differently. “This doesn’t imply that black holes ‘seed’ galaxies,” he says. “They both can form at the same time, but they don’t grow at the same rate.” In the early going, the black hole grows at a faster ...
12 The Milky Way - Journigan-wiki
... They lie in the bulge or halo and have highly elliptical orbits that may be heavily tilted with respect to the galactic disk. These stars are mostly hydrogen and helium as well with only a few 100th’s of a ...
... They lie in the bulge or halo and have highly elliptical orbits that may be heavily tilted with respect to the galactic disk. These stars are mostly hydrogen and helium as well with only a few 100th’s of a ...
Formation of Globular Clusters: In and Out of Dwarf Galaxies
... Not easy. Assuming that GCs follow galactic star formation rate produces too many red/metal-rich clusters with a unimodal metallicity distribution. Globular clusters formed earlier than the majority of field stars in host galaxy. ...
... Not easy. Assuming that GCs follow galactic star formation rate produces too many red/metal-rich clusters with a unimodal metallicity distribution. Globular clusters formed earlier than the majority of field stars in host galaxy. ...
Universe, Dark Energy and Dark Matter
... It may be suggested that man takes the central position in the Universe and all the galaxies are running away from us. Other scientists state that the Universe is uniform by structure and all the points in it are equal. In this case the Universe would be isotropic when observed from any galaxy where ...
... It may be suggested that man takes the central position in the Universe and all the galaxies are running away from us. Other scientists state that the Universe is uniform by structure and all the points in it are equal. In this case the Universe would be isotropic when observed from any galaxy where ...
Notes on Integral Field Spectroscopy (IFS/3D) Sebastián F. Sánchez / IA-UNAM
... observations done with the 3.5m at CAHA, 80% of one of the UT/VLT). • Many of proposed or new generations instruments are IFUs (MUSE, MEGARA). • JWST will include an IFU. • There is science that can only be done with IFUs. • There are three major on-going IFU surveys: CALIFA, MaNGA, SAMI. • You shou ...
... observations done with the 3.5m at CAHA, 80% of one of the UT/VLT). • Many of proposed or new generations instruments are IFUs (MUSE, MEGARA). • JWST will include an IFU. • There is science that can only be done with IFUs. • There are three major on-going IFU surveys: CALIFA, MaNGA, SAMI. • You shou ...
Observational Constraints on Hot Gas Accretion
... Fit: A “beta” surface brightness component, a point source (< 5 kpc) + background ...
... Fit: A “beta” surface brightness component, a point source (< 5 kpc) + background ...
Summary: Star Formation Near and Far
... disks close to the central star, and that they are collimated along the rotation axis from the outset. It seems almost certain that the origin and collimation of these jets somehow involve magnetic fields twisted by the rotation of the disk, and that the basic energy source is provided by accretion ...
... disks close to the central star, and that they are collimated along the rotation axis from the outset. It seems almost certain that the origin and collimation of these jets somehow involve magnetic fields twisted by the rotation of the disk, and that the basic energy source is provided by accretion ...
Stars and Galaxies
... shifted towards the red part of the visible spectrum The faster they move away from us, the more they are redshifted. Thus, redshift is a reasonable way to measure the speed of an object. When we observe the redshift of galaxies, almost every galaxy appears to be moving away from us – the Univer ...
... shifted towards the red part of the visible spectrum The faster they move away from us, the more they are redshifted. Thus, redshift is a reasonable way to measure the speed of an object. When we observe the redshift of galaxies, almost every galaxy appears to be moving away from us – the Univer ...
Dark Matter— More Than Meets The Eye
... less than that calculated by the dynamics. Beyond the visible galaxy out to the largest distance to which rotation velocities have been measured, there is possibly five or ten times as much dark matter as luminous matter. Studies of the orbital velocity of stars near the sun revealed that there is a ...
... less than that calculated by the dynamics. Beyond the visible galaxy out to the largest distance to which rotation velocities have been measured, there is possibly five or ten times as much dark matter as luminous matter. Studies of the orbital velocity of stars near the sun revealed that there is a ...
Extragalactic Distances from Planetary Nebulae
... Elliptical galaxies do not have many (any?) 2 M main sequence stars. But they do have large numbers of 1 M stars. If some are in close binary systems which coalesce on the main sequence, the product may evolve into an [O III]-bright planetary. The ratio of bright planetaries to blue stragglers is ...
... Elliptical galaxies do not have many (any?) 2 M main sequence stars. But they do have large numbers of 1 M stars. If some are in close binary systems which coalesce on the main sequence, the product may evolve into an [O III]-bright planetary. The ratio of bright planetaries to blue stragglers is ...
Slide 1
... No and no. Black dwarf wannabes have not had enough time to cool to black. Exotic stellar remnants like black holes, if so common, would be observable interacting with the interstellar medium. Dark matter remains a mystery! ...
... No and no. Black dwarf wannabes have not had enough time to cool to black. Exotic stellar remnants like black holes, if so common, would be observable interacting with the interstellar medium. Dark matter remains a mystery! ...
WFIRST-2.4: What Every Astronomer Should Know
... fields, which will be observed many times over a 2-year interval, reaches 0.5 – 2.5 magnitudes fainter than the HLS (see Table 1). Figure 3 shows the emission line sensitivity of the HLS spectroscopic survey. For moderately extended sources, the 7σ detection threshold is ≈ 1.0–1.5×10-16 erg s-1 cm-2 ...
... fields, which will be observed many times over a 2-year interval, reaches 0.5 – 2.5 magnitudes fainter than the HLS (see Table 1). Figure 3 shows the emission line sensitivity of the HLS spectroscopic survey. For moderately extended sources, the 7σ detection threshold is ≈ 1.0–1.5×10-16 erg s-1 cm-2 ...
Supplementary Information
... galaxies, in particular BM/BX objects, typically are fainter in the K-band, have lower stellar masses (median ~2x1010 M), and lower star formation rates (median ~35 Myr-1), although the overlap in range of properties with star-forming BzK objects increases for Ks < 20 BM/BX galaxies (e.g., 5, 6, 7 ...
... galaxies, in particular BM/BX objects, typically are fainter in the K-band, have lower stellar masses (median ~2x1010 M), and lower star formation rates (median ~35 Myr-1), although the overlap in range of properties with star-forming BzK objects increases for Ks < 20 BM/BX galaxies (e.g., 5, 6, 7 ...
Document
... • According to “lookback time”, populations of ancient galaxies are seen when the Universe was very young, which makes no sense. ...
... • According to “lookback time”, populations of ancient galaxies are seen when the Universe was very young, which makes no sense. ...
Galaxies - Indiana University Astronomy
... Cepheid period measurements result from the difference in location of the Cepheid variables within M100? Why or why not? ...
... Cepheid period measurements result from the difference in location of the Cepheid variables within M100? Why or why not? ...
Star formation and internal kinematics of irregular galaxies
... the relatively slow rotation of the Irregulars makes it difficult to generate strong densitywave shocks (Gallagher & Hunter 1984). Without this periodic stimulus acting upon upon clouds in their ISM (Elmegreen & Elmegreen 1983), other processes that trigger star ...
... the relatively slow rotation of the Irregulars makes it difficult to generate strong densitywave shocks (Gallagher & Hunter 1984). Without this periodic stimulus acting upon upon clouds in their ISM (Elmegreen & Elmegreen 1983), other processes that trigger star ...
Microsoft Word 97
... 7) In the directions in which we see the Milky Way in the sky, we are looking through the relatively thin, pancake-like disk of matter that forms a major part of our Milky Way Galaxy. a) This disk is about 90,000 light years across, an enormous, gravitationally bound system of stars. b) The Milky Wa ...
... 7) In the directions in which we see the Milky Way in the sky, we are looking through the relatively thin, pancake-like disk of matter that forms a major part of our Milky Way Galaxy. a) This disk is about 90,000 light years across, an enormous, gravitationally bound system of stars. b) The Milky Wa ...
script
... average travel time between stars in our part of the galaxy is 4 years. Light, traveling at the cosmic speed limit, takes four years to get from one sprinkle to another, traveling across two football fields. What are the chances that we could send a space ship to other stars in our Galaxy? What are ...
... average travel time between stars in our part of the galaxy is 4 years. Light, traveling at the cosmic speed limit, takes four years to get from one sprinkle to another, traveling across two football fields. What are the chances that we could send a space ship to other stars in our Galaxy? What are ...
Goal: To understand the structure and makeup of our own Milky Way
... have supernovae. • Just behind that you have bubbles from where all the supernovae have merged. • After that you are left with normal stars and normal space which slowly cool until they hit the next spiral arm in a few hundred million years. • With this process, the Milky Way produces about 7 new st ...
... have supernovae. • Just behind that you have bubbles from where all the supernovae have merged. • After that you are left with normal stars and normal space which slowly cool until they hit the next spiral arm in a few hundred million years. • With this process, the Milky Way produces about 7 new st ...
Summary Of the Structure of the Milky Way
... nature of the Milky Way galaxy, but are not “deep” enough probes to fully reveal the structure of the Milky Way. • Open clusters can define the thickness of the Milky Way’s thin disk where star formation is active. • Globular clusters allow astronomers to know the direction to the center of our gala ...
... nature of the Milky Way galaxy, but are not “deep” enough probes to fully reveal the structure of the Milky Way. • Open clusters can define the thickness of the Milky Way’s thin disk where star formation is active. • Globular clusters allow astronomers to know the direction to the center of our gala ...
Galaxy
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A galaxy is a gravitationally bound system of stars, stellar remnants, interstellar gas and dust, and dark matter. The word galaxy is derived from the Greek galaxias (γαλαξίας), literally ""milky"", a reference to the Milky Way. Galaxies range in size from dwarfs with just a few thousand (103) stars to giants with one hundred trillion (1014) stars, each orbiting their galaxy's own center of mass. Galaxies are categorized according to their visual morphology, including elliptical, spiral, and irregular. Many galaxies are thought to have black holes at their active centers. The Milky Way's central black hole, known as Sagittarius A*, has a mass four million times greater than our own Sun. As of July 2015, EGSY8p7 is the oldest and most distant galaxy with a light travel distance of 13.2 billion light-years from Earth, and observed as it existed 570 million years after the Big Bang. Previously, as of May 2015, EGS-zs8-1 was the most distant known galaxy, estimated to have a light travel distance of 13.1 billion light-years away and to have 15% of the mass of the Milky Way.Approximately 170 billion (1.7 × 1011) to 200 billion (2.0 × 1011) galaxies exist in the observable universe. Most of the galaxies are 1,000 to 100,000 parsecs in diameter and usually separated by distances on the order of millions of parsecs (or megaparsecs). The space between galaxies is filled with a tenuous gas with an average density less than one atom per cubic meter. The majority of galaxies are gravitationally organized into associations known as galaxy groups, clusters, and superclusters. At the largest scale, these associations are generally arranged into sheets and filaments that are surrounded by immense voids.