Essential physics of early galaxy formation
... further star formation. As halos build-up mass with time, their DM potential well can sustain much larger star formation rates (SFR) without losing gas. This naturally implies that, at any given time, there is a limiting star formation efficiency such that the energy produced by newly-formed stars i ...
... further star formation. As halos build-up mass with time, their DM potential well can sustain much larger star formation rates (SFR) without losing gas. This naturally implies that, at any given time, there is a limiting star formation efficiency such that the energy produced by newly-formed stars i ...
Lecture 8: Spiral Structure
... the result of density waves moving through the Galaxy’s disk. The spiral structure of a galaxy is regarded as a wave pattern resulting from gravitational instabilities. The density wave moves through the stellar and interstellar material as a configuration whose shape stays fixed. It rotates at a sp ...
... the result of density waves moving through the Galaxy’s disk. The spiral structure of a galaxy is regarded as a wave pattern resulting from gravitational instabilities. The density wave moves through the stellar and interstellar material as a configuration whose shape stays fixed. It rotates at a sp ...
1Cmoles.pdf
... with broad-band filters. The resulting precision in z obtained via photometric redshift techniques (∼ 0.1 in ∆z/(1 + z), at best) and in Spectral Energy Distribution (SED) determination are correspondingly rough. At the other extreme in spectral resolution, spectroscopic surveys cannot go as deep as ...
... with broad-band filters. The resulting precision in z obtained via photometric redshift techniques (∼ 0.1 in ∆z/(1 + z), at best) and in Spectral Energy Distribution (SED) determination are correspondingly rough. At the other extreme in spectral resolution, spectroscopic surveys cannot go as deep as ...
Spiral Arms - Harry Kroto
... The spiral arms are regions where stars' and gas clouds' orbits bunch up closer to one another and the region becomes overdense. Stars go in and move out of the pattern, but the pattern persists and moves at its own rate. Since the region is overdense when gas clouds enter it they are compressed and ...
... The spiral arms are regions where stars' and gas clouds' orbits bunch up closer to one another and the region becomes overdense. Stars go in and move out of the pattern, but the pattern persists and moves at its own rate. Since the region is overdense when gas clouds enter it they are compressed and ...
M81/M82/NGC3077
... M81 — -35 km/sec (3.63 ± 0.34 Mpc) (CBR value: 48 km/sec) M82 — 202 km/sec (3.9 ± 0.3 Mpc) (CBR value: 296 km/sec) M81 is closer and approaching, while M82 is farther away and receding; ...
... M81 — -35 km/sec (3.63 ± 0.34 Mpc) (CBR value: 48 km/sec) M82 — 202 km/sec (3.9 ± 0.3 Mpc) (CBR value: 296 km/sec) M81 is closer and approaching, while M82 is farther away and receding; ...
Our galaxy - School of Physics
... The different star populations, and the different components of the galaxy, reflect the order in which the Galaxy formed. In the first stage, a single gas cloud a few hundred thousand light years across began to swirl and collapse. Small spheres of gas (of about 1,000,000 solar masses) collapsed fi ...
... The different star populations, and the different components of the galaxy, reflect the order in which the Galaxy formed. In the first stage, a single gas cloud a few hundred thousand light years across began to swirl and collapse. Small spheres of gas (of about 1,000,000 solar masses) collapsed fi ...
Lecture Topics 1023
... These are the headings of the paragraphs into which ASTR 1023 lectures are divided. Use them to check your notes for completeness, and to see how the course is organized. It is also a good idea to cross-check these topics with your reading assignments, because some topics are not in the textbook. Le ...
... These are the headings of the paragraphs into which ASTR 1023 lectures are divided. Use them to check your notes for completeness, and to see how the course is organized. It is also a good idea to cross-check these topics with your reading assignments, because some topics are not in the textbook. Le ...
Sample
... black hole originates from its immense mass and density. Astronomers know that a neutron star with a mass that is three times greater than the mass of the Sun cannot hold itself up under its own gravity and will compress into an infinitesimal point called a singularity, where the original matter is ...
... black hole originates from its immense mass and density. Astronomers know that a neutron star with a mass that is three times greater than the mass of the Sun cannot hold itself up under its own gravity and will compress into an infinitesimal point called a singularity, where the original matter is ...
Institute for Astrophysical Research Seminar Series
... Brian Chaboyer (Dartmouth College) Ages of Old Star Clusters in the Milky Way ...
... Brian Chaboyer (Dartmouth College) Ages of Old Star Clusters in the Milky Way ...
Document
... mass of the gas in the disk. As we discuss in Chapter 16, the outer part of the halo extends much farther, out to perhaps 200,000 or 300,000 light-years. Believe it or not, this Galactic outer halo apparently contains 5 or 10 times as much mass as the nucleus, disk, and inner halo together—but we do ...
... mass of the gas in the disk. As we discuss in Chapter 16, the outer part of the halo extends much farther, out to perhaps 200,000 or 300,000 light-years. Believe it or not, this Galactic outer halo apparently contains 5 or 10 times as much mass as the nucleus, disk, and inner halo together—but we do ...
Girardi
... For a SSP of age t, the number of stars in any post-main sequence evolutionary phase k will be proportional to its the birth rate b(t), and to the lifetime τk . Nk ' b(t)τk ...
... For a SSP of age t, the number of stars in any post-main sequence evolutionary phase k will be proportional to its the birth rate b(t), and to the lifetime τk . Nk ' b(t)τk ...
Survey of Astrophysics A110 The Milky Way Galaxy
... – 1. Supernovae explosions will sweep up gas into elongated string-like structures where new stars will form. The rotation of the galaxy, which can be observed by studying stellar proper motions and Doppler shifts, then orders these concentrations of stars into a spiral-like pattern. – 2. The densit ...
... – 1. Supernovae explosions will sweep up gas into elongated string-like structures where new stars will form. The rotation of the galaxy, which can be observed by studying stellar proper motions and Doppler shifts, then orders these concentrations of stars into a spiral-like pattern. – 2. The densit ...
Chapter 1 - Princeton University Press
... Hubble studied the Andromeda Nebula, which had been thought by many, including Shapley, to be a gas cloud within the Milky Way. The word nebula comes from the Latin nubes, or “cloud,” denoting the fuzzy appearance of these objects. By careful observations with the new 100-inch telescope, Hubble disc ...
... Hubble studied the Andromeda Nebula, which had been thought by many, including Shapley, to be a gas cloud within the Milky Way. The word nebula comes from the Latin nubes, or “cloud,” denoting the fuzzy appearance of these objects. By careful observations with the new 100-inch telescope, Hubble disc ...
arXiv:1502.04693v1 [gr
... of the lensing B-mode power. Calculating optimal combinations of different large-scale-structure tracers for delensing, we find that co-adding CIB data and external arcminute-resolution CMB lensing reconstruction can lead to significant additional improvements in delensing performance. We investigat ...
... of the lensing B-mode power. Calculating optimal combinations of different large-scale-structure tracers for delensing, we find that co-adding CIB data and external arcminute-resolution CMB lensing reconstruction can lead to significant additional improvements in delensing performance. We investigat ...
Introduction to Observational Cosmology
... about 1 L* galaxy / 100 Mpc3 ; M* (now)=-20.8 in r-band (Note: by convention H0=100) Schechter function is a good representation LF (= abundance distribution) depends on the intrinsic color of the galaxy Vatican 2003 Lecture 20 HWR ...
... about 1 L* galaxy / 100 Mpc3 ; M* (now)=-20.8 in r-band (Note: by convention H0=100) Schechter function is a good representation LF (= abundance distribution) depends on the intrinsic color of the galaxy Vatican 2003 Lecture 20 HWR ...
Moitinho et al. - Wiley Online Library
... not include spiral arms in the region of the 3GQ under analysis. Our results are based on UBV RI five-band photometry which does allow the determination of unique solutions. The reason is that, apart from CMDs, two-colour diagrams (TCDs), which are distanceindependent, are also used in the analysis. ...
... not include spiral arms in the region of the 3GQ under analysis. Our results are based on UBV RI five-band photometry which does allow the determination of unique solutions. The reason is that, apart from CMDs, two-colour diagrams (TCDs), which are distanceindependent, are also used in the analysis. ...
Spiral structure of the Third Galactic Quadrant and the solution to the
... to be younger than 100 million years. These are listed in Table 1 and plotted in Fig. 2 which represents the third quadrant of the Galactic plane seen from above. Also plotted, are the BPs detected in the backgrounds of several clusters. A strip about 1.5 kpc wide, extending from l=210o to l=260o , ...
... to be younger than 100 million years. These are listed in Table 1 and plotted in Fig. 2 which represents the third quadrant of the Galactic plane seen from above. Also plotted, are the BPs detected in the backgrounds of several clusters. A strip about 1.5 kpc wide, extending from l=210o to l=260o , ...
- Cosmotography
... in each bin, subsequently applying a Gaussian smoothing kernel with σsmooth = 130 pc. There are typically 7–9 stars per bin in the stream. Figure 2(a) shows the resulting Subaru-based stellardensity map, where the overall stream morphology is indistinguishable from the BBRO integrated-light results. ...
... in each bin, subsequently applying a Gaussian smoothing kernel with σsmooth = 130 pc. There are typically 7–9 stars per bin in the stream. Figure 2(a) shows the resulting Subaru-based stellardensity map, where the overall stream morphology is indistinguishable from the BBRO integrated-light results. ...
MESSIER - EarthLink
... His first own deep sky discovery of globular cluster M3, cataloged on May 3, probably causes him to undertake a systematical search for nebulous objects, leading to the observation and recording of the objects M3-M40, many of which were own discoveries, but several from old catalogs. Messier was mad ...
... His first own deep sky discovery of globular cluster M3, cataloged on May 3, probably causes him to undertake a systematical search for nebulous objects, leading to the observation and recording of the objects M3-M40, many of which were own discoveries, but several from old catalogs. Messier was mad ...
FREE Sample Here
... A) It contains between 100 billion and 1 trillion stars. B) Our solar system is located very close to the center of the Milky Way Galaxy. C) The galaxy is about 100,000 light-years in diameter. D) One rotation of the galaxy takes about 200 million years. Answer: B 25) Which of the following correctl ...
... A) It contains between 100 billion and 1 trillion stars. B) Our solar system is located very close to the center of the Milky Way Galaxy. C) The galaxy is about 100,000 light-years in diameter. D) One rotation of the galaxy takes about 200 million years. Answer: B 25) Which of the following correctl ...
Results from the search for tidal disruption flares in the GALEX Deep
... • All time-domain products, notably variable object alerts, will be immediately made public for community follow-up • Produce automated pipeline triggers to generate IAU and/or GCN circulars • Prevalence of UV-bright early evolution of flaring objects • The TDS may detect: supernovae, gamma-ray fain ...
... • All time-domain products, notably variable object alerts, will be immediately made public for community follow-up • Produce automated pipeline triggers to generate IAU and/or GCN circulars • Prevalence of UV-bright early evolution of flaring objects • The TDS may detect: supernovae, gamma-ray fain ...
Starburst Galaxies Under the Microscope: High
... superstarclusters, or that the PAH emission is not preferentially excited by the superstarclusters, but is dominated by more diffuse emission, excited by the softer UV radiation from more widespread young stars of slightly later type. Understanding which of these explanations is correct is important ...
... superstarclusters, or that the PAH emission is not preferentially excited by the superstarclusters, but is dominated by more diffuse emission, excited by the softer UV radiation from more widespread young stars of slightly later type. Understanding which of these explanations is correct is important ...
Chapter 15 Stars, Galaxies, and Universe
... •Star systems – two or more stars together •Binary stars – two stars or double stars •One star brighter, more massive •Dimmer star’s gravity causes “wobble” •Eclipsing binary – one star blocks light from another star •Triple stars – 3 stars together •Found at least 500 other planets that revolve aro ...
... •Star systems – two or more stars together •Binary stars – two stars or double stars •One star brighter, more massive •Dimmer star’s gravity causes “wobble” •Eclipsing binary – one star blocks light from another star •Triple stars – 3 stars together •Found at least 500 other planets that revolve aro ...
FREE Sample Here - Find the cheapest test bank for your
... A) It contains between 100 billion and 1 trillion stars. B) Our solar system is located very close to the center of the Milky Way Galaxy. C) The galaxy is about 100,000 light-years in diameter. D) One rotation of the galaxy takes about 200 million years. Answer: B 25) Which of the following correctl ...
... A) It contains between 100 billion and 1 trillion stars. B) Our solar system is located very close to the center of the Milky Way Galaxy. C) The galaxy is about 100,000 light-years in diameter. D) One rotation of the galaxy takes about 200 million years. Answer: B 25) Which of the following correctl ...
FREE Sample Here
... A) It contains between 100 billion and 1 trillion stars. B) Our solar system is located very close to the center of the Milky Way Galaxy. C) The galaxy is about 100,000 light-years in diameter. D) One rotation of the galaxy takes about 200 million years. Answer: B 25) Which of the following correctl ...
... A) It contains between 100 billion and 1 trillion stars. B) Our solar system is located very close to the center of the Milky Way Galaxy. C) The galaxy is about 100,000 light-years in diameter. D) One rotation of the galaxy takes about 200 million years. Answer: B 25) Which of the following correctl ...
Galaxy
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.