Natasha Wood
... or the inside walls of the molecular torus should be more intense in Sy1 than in Sy2. Furthermore, the X-ray spectrum measured by Swift/BAT2 should be steeper for Sy1. To determine if this is true a sample of ~200 AGN will be statistically analyzed using a distribution of power law slopes (intensity ...
... or the inside walls of the molecular torus should be more intense in Sy1 than in Sy2. Furthermore, the X-ray spectrum measured by Swift/BAT2 should be steeper for Sy1. To determine if this is true a sample of ~200 AGN will be statistically analyzed using a distribution of power law slopes (intensity ...
Mark scheme - Unit A183/02 - Module P7 - Higher tier
... allow comment consistent with ecf from bi allow anything in range 2.6 – 2.9 to be similar accept reverse calculation giving 23.7, but must say this is similar to 24. ...
... allow comment consistent with ecf from bi allow anything in range 2.6 – 2.9 to be similar accept reverse calculation giving 23.7, but must say this is similar to 24. ...
Stellar Dynamics
... system. This helps promote the merging of galaxies, for example (see GALAXIES: INTERACTIONS AND MERGERS). The relaxation time τR of equation (4) is decreased significantly by a factor of order m/M. This is because the large mass difference induces gravitational excitations, known as grexons (also fr ...
... system. This helps promote the merging of galaxies, for example (see GALAXIES: INTERACTIONS AND MERGERS). The relaxation time τR of equation (4) is decreased significantly by a factor of order m/M. This is because the large mass difference induces gravitational excitations, known as grexons (also fr ...
A Massive Galaxy in its Core Formation Phase Three Billion Years
... universe. This high column density of gas in conjunction with the abundance of metals implies28 a very high extinction: AV & 100 for a screen, and AV & 6 if the dust and the stars are mixed. The detection of rest-frame optical flux, and of Hα emission, are inconsistent with such high values. The dus ...
... universe. This high column density of gas in conjunction with the abundance of metals implies28 a very high extinction: AV & 100 for a screen, and AV & 6 if the dust and the stars are mixed. The detection of rest-frame optical flux, and of Hα emission, are inconsistent with such high values. The dus ...
Terzan 5`s Pulsars Fastest
... cluster system. Remarkably, half of these are contained in only two clusters: Terzan 5 and 47 Tuc. ...
... cluster system. Remarkably, half of these are contained in only two clusters: Terzan 5 and 47 Tuc. ...
Overview Evolution of massive stars Evolution of massive stars
... Mass of progenitor star (solar masses) ...
... Mass of progenitor star (solar masses) ...
File
... Consider a relatively nearby, single star, that is, a star that is not a member of a binary system and has no known orbiting planets. Listed below are a few properties of this star. Classify each property as either something that we can observe or measure directly (with the aid of a telescope and in ...
... Consider a relatively nearby, single star, that is, a star that is not a member of a binary system and has no known orbiting planets. Listed below are a few properties of this star. Classify each property as either something that we can observe or measure directly (with the aid of a telescope and in ...
Answer Key 2
... e. published the results of his research towards the end of the 17th century. True/False 7. The modern approach to the origin of planetary nebulae was formed at the beginning of the 20th century. True/False lines 40-42 It was only in 1956 that the Soviet astrophysicist I.S. Shklovsky established th ...
... e. published the results of his research towards the end of the 17th century. True/False 7. The modern approach to the origin of planetary nebulae was formed at the beginning of the 20th century. True/False lines 40-42 It was only in 1956 that the Soviet astrophysicist I.S. Shklovsky established th ...
Galactic Evolution - Harvard-Smithsonian Center for Astrophysics
... genuine stars unless they accumulated more mass than stars typically do today. How much more is unknown, but if Pop-III stars really did exist, they must have contained hundreds of solar masses. No such colossal stars are seen today, the most massive star ever definitively “weighed” being ~76 M. (R ...
... genuine stars unless they accumulated more mass than stars typically do today. How much more is unknown, but if Pop-III stars really did exist, they must have contained hundreds of solar masses. No such colossal stars are seen today, the most massive star ever definitively “weighed” being ~76 M. (R ...
DoE LPPC 2006
... Principle: measure differential broadband flux (color) of objects with broad features in spectrum Photo-z gives redshifts (to 10%) from the colors of luminous red galaxies (LRG) Cluster member galaxies have scatter in redshift at 3% level PISCO measures photo-z’s of all galaxies in a cluster ...
... Principle: measure differential broadband flux (color) of objects with broad features in spectrum Photo-z gives redshifts (to 10%) from the colors of luminous red galaxies (LRG) Cluster member galaxies have scatter in redshift at 3% level PISCO measures photo-z’s of all galaxies in a cluster ...
Chapter 31: Galaxies and the Universe
... Only by mapping the galaxy with radio waves have astronomers been able to determine its shape. This is because radio waves can penetrate the interstellar gas and dust without being scattered or absorbed. Astronomers have discovered, by measuring radio waves as well as infrared radiation, that the ga ...
... Only by mapping the galaxy with radio waves have astronomers been able to determine its shape. This is because radio waves can penetrate the interstellar gas and dust without being scattered or absorbed. Astronomers have discovered, by measuring radio waves as well as infrared radiation, that the ga ...
Dark Matter in the Universe
... lose: the Milky Way will merge into the more massive M31. the astronomical jury is still out as to exactly what constitutes Computer models predict that in about four billion years the dark matter. In fact, one could say we are still at an early stage galactic pair will become one spheroidal galaxy. ...
... lose: the Milky Way will merge into the more massive M31. the astronomical jury is still out as to exactly what constitutes Computer models predict that in about four billion years the dark matter. In fact, one could say we are still at an early stage galactic pair will become one spheroidal galaxy. ...
FORMATION OF LATE-TYPE SPIRAL GALAXIES: GAS RETURN
... NGC 2903, 3198, 3621 (de Blok et al. 2009). The comparison of rotation curve with typical cases also corresponds to a shift by two categories in the Hubble classification scheme, from early-type disky galaxies to late-type disk-dominated galaxies, in agreement with the direct estimates of bulge frac ...
... NGC 2903, 3198, 3621 (de Blok et al. 2009). The comparison of rotation curve with typical cases also corresponds to a shift by two categories in the Hubble classification scheme, from early-type disky galaxies to late-type disk-dominated galaxies, in agreement with the direct estimates of bulge frac ...
The star formation history of galaxies in 3D: CALIFA perspective
... (Blanton & Moustakas 2009), following well the Hubble tuning-fork diagram. The bulge fraction seems to be one of the main physical parameters that produce the Hubble sequence, increasing from late to early spirals. In this scheme, S0 galaxies are a transition class between the spiral classes and the ...
... (Blanton & Moustakas 2009), following well the Hubble tuning-fork diagram. The bulge fraction seems to be one of the main physical parameters that produce the Hubble sequence, increasing from late to early spirals. In this scheme, S0 galaxies are a transition class between the spiral classes and the ...
The Stellar Population And Origin Of The Mysterious K.V. Getman
... The mysterious high galactic latitude cometary globule (CG) CG12 has been observed with the ACIS detector on board the Chandra X-ray Observatory. We detect 128 X-ray sources, of which a half are likely young stars formed within the globule's head. This new population of >=50 T-Tauri stars and one ne ...
... The mysterious high galactic latitude cometary globule (CG) CG12 has been observed with the ACIS detector on board the Chandra X-ray Observatory. We detect 128 X-ray sources, of which a half are likely young stars formed within the globule's head. This new population of >=50 T-Tauri stars and one ne ...
Course Outline - Tony Bacigalupo
... Note the rotation curve does not drop as it would in Keplerian motion If all the mass of the Galaxy was within the visible part, the rotation curve should follow the dashed line However, the curve actually rises out to the ~50 kpc ...
... Note the rotation curve does not drop as it would in Keplerian motion If all the mass of the Galaxy was within the visible part, the rotation curve should follow the dashed line However, the curve actually rises out to the ~50 kpc ...
Age-Dating of Young Stars and Stellar Systems
... The wavelength region between 1200 Å and 2000 Å is dominated by stellar-wind lines of, e.g., C IV λ1550 and Si IV λ1400, which are the strongest features of hot stars in a young population (e.g., Robert et al. 1993; Leitherer et al. 1995). In contrast, the optical and IR spectral regions show few, ...
... The wavelength region between 1200 Å and 2000 Å is dominated by stellar-wind lines of, e.g., C IV λ1550 and Si IV λ1400, which are the strongest features of hot stars in a young population (e.g., Robert et al. 1993; Leitherer et al. 1995). In contrast, the optical and IR spectral regions show few, ...
Dust Formation in a Galaxy with Primitive Abundances REPORTS
... the amount of dust remains unchanged (23, 24). Other properties of the outflows from carbon stars do depend on metallicity. As the metallicity of the sample drops, carbon stars produce less trace dust components such as SiC and MgS, even though the production of amorphous carbon does not change. The ...
... the amount of dust remains unchanged (23, 24). Other properties of the outflows from carbon stars do depend on metallicity. As the metallicity of the sample drops, carbon stars produce less trace dust components such as SiC and MgS, even though the production of amorphous carbon does not change. The ...
Gaia talk
... Planetary systems – Gaia will find some transiting systems, but the real value is definition of volume-complete stellar parent samples, plus direct astrometric discovery, and mass determinations, of nearby non-eclipsing jupiters. These will be ideal for follow-up direct coronographic imaging ...
... Planetary systems – Gaia will find some transiting systems, but the real value is definition of volume-complete stellar parent samples, plus direct astrometric discovery, and mass determinations, of nearby non-eclipsing jupiters. These will be ideal for follow-up direct coronographic imaging ...
m V
... • Mean dust density in the galactic disk is ndust ~ 10-6 grains/m3 Compare this to mean gas density of ngas ~ 10+6 gas atoms/m3 • Mean visual extinction in galactic plane (b = 0º) is AV ~ 1 to 2 mag. for each kpc of distance but the distribution is very patchy. ...
... • Mean dust density in the galactic disk is ndust ~ 10-6 grains/m3 Compare this to mean gas density of ngas ~ 10+6 gas atoms/m3 • Mean visual extinction in galactic plane (b = 0º) is AV ~ 1 to 2 mag. for each kpc of distance but the distribution is very patchy. ...
Satellities - stoweschools.com
... What is the velocity of the stars? v=2pr t v= 2 p ( 4x1010m) = 633 m/s (12.6yrs)(365d)(86400s) ( 1yr )( 1 day ) ...
... What is the velocity of the stars? v=2pr t v= 2 p ( 4x1010m) = 633 m/s (12.6yrs)(365d)(86400s) ( 1yr )( 1 day ) ...
ppt - CIERA - Northwestern
... masses up to and beyond 106 Msun and R1/2 ~ 2-5 pc. Densest stellar cluster--an extreme of star formation. SSCs cluster to make “starburst clumps” where SSC-SSC interactions are possible and which drive galactic winds. SSCs contain a full range of intermediate-high mass stars. Central stellar densit ...
... masses up to and beyond 106 Msun and R1/2 ~ 2-5 pc. Densest stellar cluster--an extreme of star formation. SSCs cluster to make “starburst clumps” where SSC-SSC interactions are possible and which drive galactic winds. SSCs contain a full range of intermediate-high mass stars. Central stellar densit ...
The physics of high-mass star formation
... Problems: • calibration error at least 10-20% on TMB • TMB is mean value over ΩB and line of sight • τ >> 1 only outer regions seen • different τ different parts of cloud seen • chemical inhomogeneities different molecules from different regions • for LVG collisional rates with H2 needed ...
... Problems: • calibration error at least 10-20% on TMB • TMB is mean value over ΩB and line of sight • τ >> 1 only outer regions seen • different τ different parts of cloud seen • chemical inhomogeneities different molecules from different regions • for LVG collisional rates with H2 needed ...
Living Things - Fairfield-Suisun Unified School District
... Universe What is the big bang theory? How did the solar system form? What do astronomers predict about the future of the universe? ...
... Universe What is the big bang theory? How did the solar system form? What do astronomers predict about the future of the universe? ...
Astronomy 140 Lecture Notes, Spring 2008 c
... for Fλ , or in Janskies: 1 Jy = 10−26 W/m2 /Hz = 10−23 erg/cm2 /sec/Hz. To actually determine the 0th magnitude flux F◦ is quite difficult, since it requires the comparison of a star with a laboratory standard light source. Stars are much fainter and hotter than lab standards, and are also much furt ...
... for Fλ , or in Janskies: 1 Jy = 10−26 W/m2 /Hz = 10−23 erg/cm2 /sec/Hz. To actually determine the 0th magnitude flux F◦ is quite difficult, since it requires the comparison of a star with a laboratory standard light source. Stars are much fainter and hotter than lab standards, and are also much furt ...
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.