A Physical Model for the Anisotropies of Cosmic Far-infrared Background
... Summary of Our Model • Gas accretion rate ∝ dark matter accretion rate • Feedback and gas ejection (see the next slide) • Star formation rate (SFR) = Mgas/tsf • LIR = SFR/K (Kennicutt 98) • Mdust ∝ metal mass ...
... Summary of Our Model • Gas accretion rate ∝ dark matter accretion rate • Feedback and gas ejection (see the next slide) • Star formation rate (SFR) = Mgas/tsf • LIR = SFR/K (Kennicutt 98) • Mdust ∝ metal mass ...
Big Bang
... On even greater scales the galaxy clusters themselves form clusters called superclusters that can be tens to hundreds of millions of light years across. ...
... On even greater scales the galaxy clusters themselves form clusters called superclusters that can be tens to hundreds of millions of light years across. ...
Globular Cluster Formation in CDM Cosmologies
... study. Galaxies studied here are members of galactic clusters (eg. Virgo, Hydra, etc) ...
... study. Galaxies studied here are members of galactic clusters (eg. Virgo, Hydra, etc) ...
Clusters
... shows a peak in the center, and gently declines out to 0.2 R180 Beyond 0.2 R180 the metallicity is ≈ 0.2 solar and flat No evidence of profile evolution from z = 0.1 to z = 0.3 ...
... shows a peak in the center, and gently declines out to 0.2 R180 Beyond 0.2 R180 the metallicity is ≈ 0.2 solar and flat No evidence of profile evolution from z = 0.1 to z = 0.3 ...
Week 12
... and dust that can be used to form stars NOW? (Hint: what kind of stars will only be around for a ...
... and dust that can be used to form stars NOW? (Hint: what kind of stars will only be around for a ...
Document
... for which we can measure: o their redshift ( recession velocity) o their distance (independently of their redshift) If we plot recession velocity versus distance on a graph, and our data lies on (or close to) a straight line, then the slope of the line is the Hubble constant. (Astro II students wil ...
... for which we can measure: o their redshift ( recession velocity) o their distance (independently of their redshift) If we plot recession velocity versus distance on a graph, and our data lies on (or close to) a straight line, then the slope of the line is the Hubble constant. (Astro II students wil ...
Spitzer Observations of Star Formation in Several
... gravitational center of the system, but with efficiencies comparable to those of ULIRGs. The spatial distributions of atomic gas, molecular gas, warm dust and ionizing photons are indicative of a progressive change from denser gas concentrations to forming stars in clusters. Thre observed active sup ...
... gravitational center of the system, but with efficiencies comparable to those of ULIRGs. The spatial distributions of atomic gas, molecular gas, warm dust and ionizing photons are indicative of a progressive change from denser gas concentrations to forming stars in clusters. Thre observed active sup ...
PPT
... expensive in telescope time and in general these galaxies have not been detected in CO. • The nearest galaxies after SMC and LMC are ten times further away and we have been able to observe in CO (@10pc resolution) and continuum only a dozen of molecular cloud region in the ...
... expensive in telescope time and in general these galaxies have not been detected in CO. • The nearest galaxies after SMC and LMC are ten times further away and we have been able to observe in CO (@10pc resolution) and continuum only a dozen of molecular cloud region in the ...
galaxy
... • Reading the H-R Diagram The diagonal pattern on the H-R diagram where most stars lie is called the main sequence. ...
... • Reading the H-R Diagram The diagonal pattern on the H-R diagram where most stars lie is called the main sequence. ...
Galaxies The Milky Way
... There are galaxies of various shapes and patterns, but they can be grouped into four main types – spiral, barred spiral, elliptical, and irregular. Like moons and planets, galaxies spin and move around in space. They are travelling away from each other at up to 112 651 km per second. The largest gal ...
... There are galaxies of various shapes and patterns, but they can be grouped into four main types – spiral, barred spiral, elliptical, and irregular. Like moons and planets, galaxies spin and move around in space. They are travelling away from each other at up to 112 651 km per second. The largest gal ...
Milky Way Galaxy
... Galaxies are made up of stars that give off light (EM radiation). The types of radiation depends on the source. Hubble expected to find certain wavelengths of radiation from certain galaxies. What he actually noticed was that waves were actually longer than expected. Having longer waves caused them ...
... Galaxies are made up of stars that give off light (EM radiation). The types of radiation depends on the source. Hubble expected to find certain wavelengths of radiation from certain galaxies. What he actually noticed was that waves were actually longer than expected. Having longer waves caused them ...
05_CASCA_band3 - Astronomy Research Centre
... the incredibly faint whispers of radiation that reach earth from the remotest parts of the cosmos. These receivers are of paramount importance to the project because they will be used not only for many science applications but also for final adjustment of the antenna panels and for regular calibrati ...
... the incredibly faint whispers of radiation that reach earth from the remotest parts of the cosmos. These receivers are of paramount importance to the project because they will be used not only for many science applications but also for final adjustment of the antenna panels and for regular calibrati ...
Document
... – Stellar core (hottest part, dense gas in a plasmic state) – Convection zone (rising gas from the core that cools) – Photosphere (the region from which externally received ...
... – Stellar core (hottest part, dense gas in a plasmic state) – Convection zone (rising gas from the core that cools) – Photosphere (the region from which externally received ...
Chapter 15.3 Galaxy Evolution
... • What is the power source for quasars and other active galactic nuclei? • Do supermassive black holes really exist? ...
... • What is the power source for quasars and other active galactic nuclei? • Do supermassive black holes really exist? ...
Galaxies
... • In space, nebulas are giant clouds of gas and dust. • Some types of nebulas glow by themselves, while others absorb light and hide stars. • Some nebulas are regions where new stars form (like the Eagle nebula to the left). • Spiral galaxies generally contain nebulas, but elliptical galaxies do not ...
... • In space, nebulas are giant clouds of gas and dust. • Some types of nebulas glow by themselves, while others absorb light and hide stars. • Some nebulas are regions where new stars form (like the Eagle nebula to the left). • Spiral galaxies generally contain nebulas, but elliptical galaxies do not ...
Dark Energy and Cosmic Sound
... measure in the clustering of galaxies today: baryon acoustic oscillations. This signature has a size that we can calculate accurately. Measuring this as an angle allows us to infer the distance to a sample of galaxies. Measuring accurate distances is a key way to study the acceleration of the Univer ...
... measure in the clustering of galaxies today: baryon acoustic oscillations. This signature has a size that we can calculate accurately. Measuring this as an angle allows us to infer the distance to a sample of galaxies. Measuring accurate distances is a key way to study the acceleration of the Univer ...
Dwarf Galaxies
... Dwarf Galaxies: •! Different types of dwarf galaxies –! Dwarf ellipticals (dE): Note that these are structurally very different from luminous E’s. Gas-poor, old stellar population. Note that many dE’s have nuclei (dE,N). –! Dwarf spheroidals (dSph): Gas-poor, diffuse systems. Low luminosity (low sur ...
... Dwarf Galaxies: •! Different types of dwarf galaxies –! Dwarf ellipticals (dE): Note that these are structurally very different from luminous E’s. Gas-poor, old stellar population. Note that many dE’s have nuclei (dE,N). –! Dwarf spheroidals (dSph): Gas-poor, diffuse systems. Low luminosity (low sur ...
Abell 85
... The temperature map shows a small decrease in the very center and south; the metallicity in these zones is higher ...
... The temperature map shows a small decrease in the very center and south; the metallicity in these zones is higher ...
Far-infrared line emission from high
... on the [C II] luminosity arising from a gamma-ray burst host galaxy and two LAEs with moderate SFR. Other interesting fine-structure lines are [O I] 63 μm, tracing neutral (higher density) gas, and [N II] 122 μm probing the ionized ISM phase. [O I] detections have been reported in two lensed ultralu ...
... on the [C II] luminosity arising from a gamma-ray burst host galaxy and two LAEs with moderate SFR. Other interesting fine-structure lines are [O I] 63 μm, tracing neutral (higher density) gas, and [N II] 122 μm probing the ionized ISM phase. [O I] detections have been reported in two lensed ultralu ...
Cosmic Castaways Scene Chart
... for these elusive objects. The most promising place to seek the light of these castaways is the nearby Virgo Cluster of Galaxies; the nearest galaxy cluster to Earth. It is about 55 million light years away, and contains several thousand galaxies. Using a special telescope designed to search for th ...
... for these elusive objects. The most promising place to seek the light of these castaways is the nearby Virgo Cluster of Galaxies; the nearest galaxy cluster to Earth. It is about 55 million light years away, and contains several thousand galaxies. Using a special telescope designed to search for th ...
Emergency Substitute class orders
... 4. Which of the following sets contains only objects that shine as a result of reflected light? A moons, planets, and comets B moons, comets, and stars C planets, stars, and comets D planets, stars, and moons ...
... 4. Which of the following sets contains only objects that shine as a result of reflected light? A moons, planets, and comets B moons, comets, and stars C planets, stars, and comets D planets, stars, and moons ...
ASTRONOMY 0089: EXAM 3 Class Meets M,W,F, 1:00 PM April 19
... Now answer all 46 questions. Students should choose the best answer of those given. There is only one correct answer for each question. Read all questions carefully before answering. INSTRUCTIONS: ...
... Now answer all 46 questions. Students should choose the best answer of those given. There is only one correct answer for each question. Read all questions carefully before answering. INSTRUCTIONS: ...
The first billion years of galaxy formation and evolution
... supermassive black holes form? -What was the inter-relationship between supermassive black hole and host galaxy growth at these early epochs? This requires large, robust samples of z > 4 galaxies! ...
... supermassive black holes form? -What was the inter-relationship between supermassive black hole and host galaxy growth at these early epochs? This requires large, robust samples of z > 4 galaxies! ...
Seyfert galaxy
Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei (very luminous, distant and bright sources of electromagnetic radiation) with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.Seyfert galaxies account for about 10% of all galaxies and are some of the most intensely studied objects in astronomy, as they are thought to be powered by the same phenomena that occur in quasars, although they are closer and less luminous than quasars. These galaxies have supermassive black holes at their centers which are surrounded by accretion discs of in-falling material. The accretion discs are believed to be the source of the observed ultraviolet radiation. Ultraviolet emission and absorption lines provide the best diagnostics for the composition of the surrounding material.Seen in visible light, most Seyfert galaxies look like normal spiral galaxies, but when studied under other wavelengths, it becomes clear that the luminosity of their cores is of comparable intensity to the luminosity of whole galaxies the size of the Milky Way.Seyfert galaxies are named after Carl Seyfert, who first described this class in 1943.