16. Hubble`s Law and Dark Matter
... curves and motions of individual galaxies in galaxy clusters. • All measures show that a large amount of dark matter must exist. • Merger of small galaxies to form a larger galaxy is probably an important part of galaxy formation. • Collisions are also important. • Merger of spiral galaxies probably ...
... curves and motions of individual galaxies in galaxy clusters. • All measures show that a large amount of dark matter must exist. • Merger of small galaxies to form a larger galaxy is probably an important part of galaxy formation. • Collisions are also important. • Merger of spiral galaxies probably ...
Understanding the Astrophysics of Galaxy Evolution: the role of
... almost all galaxy properties are correlated. Galaxy mass correlates with morphological type, with colour, with metallicity, with star formation rate, with gas content and with local and large-scale environment. The correlation of property A with property B does not establish that B regulates A. With ...
... almost all galaxy properties are correlated. Galaxy mass correlates with morphological type, with colour, with metallicity, with star formation rate, with gas content and with local and large-scale environment. The correlation of property A with property B does not establish that B regulates A. With ...
A Deeper Look at Faint H $\ alpha $ Emission in Nearby Dwarf
... observed (i.e., no extinction corrections applied) Hα luminosity of these regions range from 5×1035 ergs s−1 to 2×1036 ergs s−1 , which corresponds to the ionizing fluxes of single B0V-O9V stars (Smith et al. 2002), assuming Case B recombination and that the HII regions are radiation bounded. If the ...
... observed (i.e., no extinction corrections applied) Hα luminosity of these regions range from 5×1035 ergs s−1 to 2×1036 ergs s−1 , which corresponds to the ionizing fluxes of single B0V-O9V stars (Smith et al. 2002), assuming Case B recombination and that the HII regions are radiation bounded. If the ...
Astronomy 112: The Physics of Stars Class 19 Notes: The Stellar
... fade out very quickly. The young ones are extremely bright, but they lose much of their brightness in their first few tens of Myr. Thereafter they dim greatly. It should be noted that this calculation does ignore one significant effect, which is important for very old clusters: the luminosity of red ...
... fade out very quickly. The young ones are extremely bright, but they lose much of their brightness in their first few tens of Myr. Thereafter they dim greatly. It should be noted that this calculation does ignore one significant effect, which is important for very old clusters: the luminosity of red ...
FINAL PROGRAM - Drifting through the Cosmic Web
... (Poster) Weak Lensing Signatures of the Connexion between Massive Dark Matter Halos and the Cosmic Web ...
... (Poster) Weak Lensing Signatures of the Connexion between Massive Dark Matter Halos and the Cosmic Web ...
Lecture 2
... Shortly ager the CMB was discovered one realized that there should be angular varia)ons in temperature, as a result of density inhomogenei)es in the Universe. The denser regions cause the CMB photons to be gravita)onally redshiged compared to photons arising in less dense regions. The am ...
... Shortly ager the CMB was discovered one realized that there should be angular varia)ons in temperature, as a result of density inhomogenei)es in the Universe. The denser regions cause the CMB photons to be gravita)onally redshiged compared to photons arising in less dense regions. The am ...
Spectroscopic confirmation of a galaxy at redshift z=8.6
... a flux density of log( f1,700Å (erg s21 cm22 Hz21)) 5 230.7 6 0.2 and an intrinsic luminosity density of log(L1,700Å (erg s21 Hz21)) 5 28.3 6 0.2. The continuum luminosity density is about one magnitude fainter than MUV*, the characteristic magnitude of the ultraviolet luminosity function, for gal ...
... a flux density of log( f1,700Å (erg s21 cm22 Hz21)) 5 230.7 6 0.2 and an intrinsic luminosity density of log(L1,700Å (erg s21 Hz21)) 5 28.3 6 0.2. The continuum luminosity density is about one magnitude fainter than MUV*, the characteristic magnitude of the ultraviolet luminosity function, for gal ...
Option D – Astrophysics
... away from Earth may be seen through a telescope as two separate ■■ Figure 16.6 An artist’s impression of a visual binary stars, but most binary stars are further away and appear as a single star system point of light. Binary star systems are important in astronomy because the period of their orbital ...
... away from Earth may be seen through a telescope as two separate ■■ Figure 16.6 An artist’s impression of a visual binary stars, but most binary stars are further away and appear as a single star system point of light. Binary star systems are important in astronomy because the period of their orbital ...
SXDS Highlights : Subaru / FOCAS Spectroscopy
... Results of “cloning” simulations show if there are large number of elliptical or bulge-dominated galaxies at z~3, they should be detected, and should be fitted well with large n-index. ...
... Results of “cloning” simulations show if there are large number of elliptical or bulge-dominated galaxies at z~3, they should be detected, and should be fitted well with large n-index. ...
Crash Galaxies
... event, experts can’t be certain what happened. For example, the outer spindly arms of Galaxy M33 are bent away from and out of the flat plane of the galaxy, a most unusual occurrence. Yet no galaxies seem to be near enough to have produced that effect through recent gravitational interaction (Ferri ...
... event, experts can’t be certain what happened. For example, the outer spindly arms of Galaxy M33 are bent away from and out of the flat plane of the galaxy, a most unusual occurrence. Yet no galaxies seem to be near enough to have produced that effect through recent gravitational interaction (Ferri ...
100 Binocular Deep Sky Objects
... in a group, but usually 2 objects in a group. Seeing DSOs in groups makes observing that much more enjoyable. Many of these objects are challenging and may not be seen unless observing with large binoculars or in very dark skies. In some cases I discuss what can be seen in various sizes of binocular ...
... in a group, but usually 2 objects in a group. Seeing DSOs in groups makes observing that much more enjoyable. Many of these objects are challenging and may not be seen unless observing with large binoculars or in very dark skies. In some cases I discuss what can be seen in various sizes of binocular ...
The California Planet Survey II. A Saturn
... stars, the relationships between the physical characteristics of stars and the properties of their planets will come into sharper focus. We are monitoring a sample of 147 late K and early M stars as part of the California Planet Survey at Keck Observatory with a current temporal baseline of ≈ 12 yea ...
... stars, the relationships between the physical characteristics of stars and the properties of their planets will come into sharper focus. We are monitoring a sample of 147 late K and early M stars as part of the California Planet Survey at Keck Observatory with a current temporal baseline of ≈ 12 yea ...
The IMF of intermediate-mass stars in young star clusters
... Griffiths (1998); Banks, Dodd & Sullivan (1995). These authors have also discussed the effects of improper correction of these parameters on the determination of the cluster MF slope. For example, it becomes flatter if correction for data incompleteness is not applied, while the lack of correction f ...
... Griffiths (1998); Banks, Dodd & Sullivan (1995). These authors have also discussed the effects of improper correction of these parameters on the determination of the cluster MF slope. For example, it becomes flatter if correction for data incompleteness is not applied, while the lack of correction f ...
Unit 6: The Present Universe
... bigger with time. Some structures are held together by forces sufficiently strong to prevent the expansion of space from increasing their size. This is true for galaxies (and everything in them) as well as for clusters of galaxies. However, gravitational attraction between the clusters and superclus ...
... bigger with time. Some structures are held together by forces sufficiently strong to prevent the expansion of space from increasing their size. This is true for galaxies (and everything in them) as well as for clusters of galaxies. However, gravitational attraction between the clusters and superclus ...
Science Grade 08 Unit 11 Exemplar Lesson 02: Classifying Stars
... This unit bundles student expectations that address components and characteristics of the universe. Students learn that stars and galaxies are part of the universe and how they can be classified by their characteristics. Prior to this unit, in Grade 8, students studied the effects resulting from cyc ...
... This unit bundles student expectations that address components and characteristics of the universe. Students learn that stars and galaxies are part of the universe and how they can be classified by their characteristics. Prior to this unit, in Grade 8, students studied the effects resulting from cyc ...
Disk
... • Disks found in B (proto)stars star formation by accretion as in low-mass stars • No disk found yet (only massive, rotating toroids) in O (proto)stars – observational bias (confusion, distance, rarity,…) – disks hidden inside toroids and/or truncated by tidal interactions with stellar companion ...
... • Disks found in B (proto)stars star formation by accretion as in low-mass stars • No disk found yet (only massive, rotating toroids) in O (proto)stars – observational bias (confusion, distance, rarity,…) – disks hidden inside toroids and/or truncated by tidal interactions with stellar companion ...
Astronomy Astrophysics + Infrared identification of 2XMM J191043.4
... hand the spectral classification of hot stars based on a K-band spectrum cannot be completed without ambiguities because of the lack of enough spectral features in that range (Hanson et al. 1996). This problem can be circumvented by combining data for several spectral bands, including the X-rays. On ...
... hand the spectral classification of hot stars based on a K-band spectrum cannot be completed without ambiguities because of the lack of enough spectral features in that range (Hanson et al. 1996). This problem can be circumvented by combining data for several spectral bands, including the X-rays. On ...
Notes for Class 14, April 21
... • Scientists usually not concerned with these issues or with philosophical uncertainty • Science many not be perfect, but it can still be very good • Many use technology but not the scientific foundation ...
... • Scientists usually not concerned with these issues or with philosophical uncertainty • Science many not be perfect, but it can still be very good • Many use technology but not the scientific foundation ...
a changing cosmos - Whittier Union High School District
... go out, its core collapses releasing a huge amount of gravitational energy. A blast wave ejects the star's outer layers into space. The Crab nebula supernova remnant is incredibly bright, even though it looks quite dim at our distance from it—6,300 light-years. If we were to observe it from much clo ...
... go out, its core collapses releasing a huge amount of gravitational energy. A blast wave ejects the star's outer layers into space. The Crab nebula supernova remnant is incredibly bright, even though it looks quite dim at our distance from it—6,300 light-years. If we were to observe it from much clo ...
the UKIRT Fundamental and Extended lists
... We present high-precision JHK photometry with the 3.8-m UK Infrared Telescope (UKIRT) of 82 standard stars, 28 from the widely used preliminary list known as the ‘UKIRT Faint Standards’, referred to here as the Fundamental List, and 54 additional stars referred to as the Extended List. The stars hav ...
... We present high-precision JHK photometry with the 3.8-m UK Infrared Telescope (UKIRT) of 82 standard stars, 28 from the widely used preliminary list known as the ‘UKIRT Faint Standards’, referred to here as the Fundamental List, and 54 additional stars referred to as the Extended List. The stars hav ...
JHK standard stars for large telescopes: the UKIRT Fundamental
... We present high-precision JHK photometry with the 3.8-m UK Infrared Telescope (UKIRT) of 82 standard stars, 28 from the widely used preliminary list known as the ‘UKIRT Faint Standards’, referred to here as the Fundamental List, and 54 additional stars referred to as the Extended List. The stars hav ...
... We present high-precision JHK photometry with the 3.8-m UK Infrared Telescope (UKIRT) of 82 standard stars, 28 from the widely used preliminary list known as the ‘UKIRT Faint Standards’, referred to here as the Fundamental List, and 54 additional stars referred to as the Extended List. The stars hav ...
candels
... Star-forming galaxies tend to be more z~2 have high Sersic indices: extended and more disk like • Correlation of star-formation with profile shape is much stronger than with stellar mass. ...
... Star-forming galaxies tend to be more z~2 have high Sersic indices: extended and more disk like • Correlation of star-formation with profile shape is much stronger than with stellar mass. ...
Survey of Astrophysics A110 The Milky Way Galaxy
... – 3. They are found in the Galactic halo. – 4. Spectral analysis shows that they have a smaller amount of heavy elements than the Sun (hence Pop. II). – 5. They have short main sequences on the HR diagram which indicate that they are old (i.e., they do not contain O, B, A, and F Population II stars) ...
... – 3. They are found in the Galactic halo. – 4. Spectral analysis shows that they have a smaller amount of heavy elements than the Sun (hence Pop. II). – 5. They have short main sequences on the HR diagram which indicate that they are old (i.e., they do not contain O, B, A, and F Population II stars) ...
Determination of kinetic energies of stars using Hipparcos data *
... precisely, we attempt to find the average kinetic energy per star in the vicinity of the Sun. As is well known, the stars of late spectral types have larger proper motions than the stars of early spectral types. There is a good deal of different hypotheses that aim to explain this phenomenon. One of ...
... precisely, we attempt to find the average kinetic energy per star in the vicinity of the Sun. As is well known, the stars of late spectral types have larger proper motions than the stars of early spectral types. There is a good deal of different hypotheses that aim to explain this phenomenon. One of ...
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.