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PDF only - at www.arxiv.org.
... Since 1928 the Bosscha Observatory is engaged in visual double stars studies, with the main purpose to develop new observational techniques in order to obtain results with accuracy greater than that attained till now. Two different observing techniques in the last decade have been developed for doub ...
... Since 1928 the Bosscha Observatory is engaged in visual double stars studies, with the main purpose to develop new observational techniques in order to obtain results with accuracy greater than that attained till now. Two different observing techniques in the last decade have been developed for doub ...
My Constellation
... curving rows of glittering stars. Several hundred stars make up the group, which is perhaps 2500 light years away. Õ The Eskimo Nebula (NGC 2392) is one of the more distant nebulae at an estimated distance of 10,000 light years. There is a tenth-magnitude central star. If you do have a large enough ...
... curving rows of glittering stars. Several hundred stars make up the group, which is perhaps 2500 light years away. Õ The Eskimo Nebula (NGC 2392) is one of the more distant nebulae at an estimated distance of 10,000 light years. There is a tenth-magnitude central star. If you do have a large enough ...
LET THE STARS GET IN YOUR EYES SKY MOTIONS
... Stars come in all sizes and colors. Betelgeuse in Orion is one of the largest stars known. It is over 800 times larger than our Sun. The smallest visible stars are white dwarfs which are about the size of the Earth. Neutron stars are about the size of a city but are only detected by radio waves. Our ...
... Stars come in all sizes and colors. Betelgeuse in Orion is one of the largest stars known. It is over 800 times larger than our Sun. The smallest visible stars are white dwarfs which are about the size of the Earth. Neutron stars are about the size of a city but are only detected by radio waves. Our ...
Notes on Stars
... this observation. The real starting point of solar (and stellar) spectroscopy were Fraunhofers pioneering studies in 1816-1820 in Benediktbeuren and in the Munich Observatory together with von Soldner. Fraunhofer discovered numerous absorption lines in the solar spectrum and documented them with imp ...
... this observation. The real starting point of solar (and stellar) spectroscopy were Fraunhofers pioneering studies in 1816-1820 in Benediktbeuren and in the Munich Observatory together with von Soldner. Fraunhofer discovered numerous absorption lines in the solar spectrum and documented them with imp ...
Science Grade 08 Unit 11 Exemplar Lesson 02: Classifying Stars
... 5. Ask students to open their notebooks to the Handout: Galaxies and Stars Questions (previously distributed and affixed). 6. Project the Teacher Resource: PowerPoint: Galaxies and Stars, and discuss slides 7–9 with students. Instruct students to watch for underlined words or phrases as they continu ...
... 5. Ask students to open their notebooks to the Handout: Galaxies and Stars Questions (previously distributed and affixed). 6. Project the Teacher Resource: PowerPoint: Galaxies and Stars, and discuss slides 7–9 with students. Instruct students to watch for underlined words or phrases as they continu ...
Luminosity and Mass Functions of Galaxies
... Malmquist Bias: brighter galaxies are easier to detect and are detectable at greater distances. Weight galaxies by 1/Vmax , the maximum volume over which they can be detected. Φ = Σi 1/Vmax,i Accounts for many selection effects: luminosity, redshift, etc. Agrees well with fancier methods. Not strong ...
... Malmquist Bias: brighter galaxies are easier to detect and are detectable at greater distances. Weight galaxies by 1/Vmax , the maximum volume over which they can be detected. Φ = Σi 1/Vmax,i Accounts for many selection effects: luminosity, redshift, etc. Agrees well with fancier methods. Not strong ...
Part2
... o We have ignored metallicity effects, enhancement due to intereactions. In reality, low mass galaxies are hard to see at all and mergers can be very bright. o Unlike GMCs, it isn’t always straightforward to get all of the galaxy inside the beam. We’ll talk a bit about the intermediate case next… We ...
... o We have ignored metallicity effects, enhancement due to intereactions. In reality, low mass galaxies are hard to see at all and mergers can be very bright. o Unlike GMCs, it isn’t always straightforward to get all of the galaxy inside the beam. We’ll talk a bit about the intermediate case next… We ...
Late Summer Messier Objects
... a nebula filter. A few isolated bright patches do show through under good conditions, notably near the mag 7 star E of NGC 6530 and around 9 Sgr. M8 is very obvious to the naked eye under dark skies, looking like a small disjoint piece of the Milky Way some distance W of the main body, and somewhat ...
... a nebula filter. A few isolated bright patches do show through under good conditions, notably near the mag 7 star E of NGC 6530 and around 9 Sgr. M8 is very obvious to the naked eye under dark skies, looking like a small disjoint piece of the Milky Way some distance W of the main body, and somewhat ...
Chapter 15 THE MILKY WAY IN RELATION TO OTHER GALAXIES
... show evidence for a central black hole of 8 106 M⊙ . NGC 205 has a profile that cannot be fit with either an R1/4 or an exponential and has a starlike nucleus. The observed extent is 1.6 kpc and the integrated magnitude MV = −16.1 (2.4 108 L⊙ ). NGC 185 also has a complicated profile, but no nucleus ...
... show evidence for a central black hole of 8 106 M⊙ . NGC 205 has a profile that cannot be fit with either an R1/4 or an exponential and has a starlike nucleus. The observed extent is 1.6 kpc and the integrated magnitude MV = −16.1 (2.4 108 L⊙ ). NGC 185 also has a complicated profile, but no nucleus ...
What Can You See With a Telescope
... 250 asteroids larger than 62 miles in diameter and perhaps 1,000,000 with diameters greater than one-half a mile. Asteroid Brightness—Another Factor to Consider The size of the majority of asteroids is quite small, but that is not the whole story. An asteroid’s brightness varies according to its orb ...
... 250 asteroids larger than 62 miles in diameter and perhaps 1,000,000 with diameters greater than one-half a mile. Asteroid Brightness—Another Factor to Consider The size of the majority of asteroids is quite small, but that is not the whole story. An asteroid’s brightness varies according to its orb ...
WORD - Astrophysics
... example, the venerable CGS4 InSb detector on UKIRT cannot be pushed much further than a flat fielding accuracy of 1 in 1000, as it is essential to keep the light from the source on as small a number of rows as possible. An ELT's light gathering power could be used to disperse a spectrum laterally ac ...
... example, the venerable CGS4 InSb detector on UKIRT cannot be pushed much further than a flat fielding accuracy of 1 in 1000, as it is essential to keep the light from the source on as small a number of rows as possible. An ELT's light gathering power could be used to disperse a spectrum laterally ac ...
Small Bodies in the Outer Solar System
... density of objects brighter than a given magnitude. For the Centaurs and KBOs the CLF is well known for mR < 26 mags. (Jewitt et al. 1998; Trujillo et al. 2001; Allen et al. 2002; Millis et al. 2002; Trujillo & Brown 2003). To determine the size distribution of the KBOs we assume they follow a diffe ...
... density of objects brighter than a given magnitude. For the Centaurs and KBOs the CLF is well known for mR < 26 mags. (Jewitt et al. 1998; Trujillo et al. 2001; Allen et al. 2002; Millis et al. 2002; Trujillo & Brown 2003). To determine the size distribution of the KBOs we assume they follow a diffe ...
20_Testbank
... 1) Explain how we estimate that there are about 50-100 billion galaxies in the observable universe. Answer: Obviously it's impossible to count so many galaxies one by one, but by observing a small part in detail, we can extrapolate to get the total number. As an example, the Hubble deep field shows ...
... 1) Explain how we estimate that there are about 50-100 billion galaxies in the observable universe. Answer: Obviously it's impossible to count so many galaxies one by one, but by observing a small part in detail, we can extrapolate to get the total number. As an example, the Hubble deep field shows ...
File - Mr. Catt`s Class
... Hubble’s Tuning Fork Diagram 1. Hubble’s tuning fork diagram relates the various types of galaxies. In his plan, S0 galaxies form the connecting link, because they have characteristics of both elliptical and spiral galaxies. 2. Astronomers once also thought the diagram represented an evolutionary s ...
... Hubble’s Tuning Fork Diagram 1. Hubble’s tuning fork diagram relates the various types of galaxies. In his plan, S0 galaxies form the connecting link, because they have characteristics of both elliptical and spiral galaxies. 2. Astronomers once also thought the diagram represented an evolutionary s ...
Galaxy Hunters Article, Cosmology Information, First Star Facts
... the idea that the seeds of galaxy formation—the primordial lumps in the early universe created by dark matter—left tiny temperature variations in the cosmic microwave background, now cooled to a frigid 2.73 degrees above absolute zero. Famed cosmologist Stephen Hawking pronounced the finding the "d ...
... the idea that the seeds of galaxy formation—the primordial lumps in the early universe created by dark matter—left tiny temperature variations in the cosmic microwave background, now cooled to a frigid 2.73 degrees above absolute zero. Famed cosmologist Stephen Hawking pronounced the finding the "d ...
100 Binocular Deep Sky Objects
... M38 has stars that are spaced openly. All the stars are pretty faint, probably the reason why so many can’t seem to find this cluster with mid-sized binocs. It has many stars easily seen, well spaced and all evenly bright, but all pretty faint with the brightest star only mag 9.5. In 20x80s, M38 is ...
... M38 has stars that are spaced openly. All the stars are pretty faint, probably the reason why so many can’t seem to find this cluster with mid-sized binocs. It has many stars easily seen, well spaced and all evenly bright, but all pretty faint with the brightest star only mag 9.5. In 20x80s, M38 is ...
15_Testbank
... 16) Which of the following statements about spectral types of stars is true? A) The spectral type of a star can be used to determine its surface temperature. B) The spectral type of a star can be used to determine its color. C) A star with spectral type A is cooler than a star with spectral type B. ...
... 16) Which of the following statements about spectral types of stars is true? A) The spectral type of a star can be used to determine its surface temperature. B) The spectral type of a star can be used to determine its color. C) A star with spectral type A is cooler than a star with spectral type B. ...
Astronomy 140 Lecture Notes, Spring 2008 c
... The majority of stars in a volume limited sample are arranged in a one dimensional track known as the main sequence. These are the stars that are burning H → He in their cores. After about 10% of the total mass of the star has been converted from hydrogen to helium, the star expands to become a red ...
... The majority of stars in a volume limited sample are arranged in a one dimensional track known as the main sequence. These are the stars that are burning H → He in their cores. After about 10% of the total mass of the star has been converted from hydrogen to helium, the star expands to become a red ...
Cosmic variance in [O/Fe] in the Galactic disk
... S, and Ti, Nissen found a tight correlation between their abundance ratio to iron and stellar age, inferred from the comparison with models of stellar structure and evolution, and thanks to the extreme accuracy of the atmospheric parameters provided by the differential analysis relative to the Sun. ...
... S, and Ti, Nissen found a tight correlation between their abundance ratio to iron and stellar age, inferred from the comparison with models of stellar structure and evolution, and thanks to the extreme accuracy of the atmospheric parameters provided by the differential analysis relative to the Sun. ...
The Magellan 20 Telescope Science Goals
... Detailed measurement of the ground layer wave-front distortions should be possible nearly anywhere in the sky using natural guide stars in the field. Rayleigh laser beacons may be used if higher photon rates are required. The potential scientific gains are large. For point sources in the background- ...
... Detailed measurement of the ground layer wave-front distortions should be possible nearly anywhere in the sky using natural guide stars in the field. Rayleigh laser beacons may be used if higher photon rates are required. The potential scientific gains are large. For point sources in the background- ...
Chapter 12: Stars and Galaxies
... Although Bellatrix is the closest of these stars to Earth, Betelgeuse and Rigel appear brighter. This is because Betelgeuse, a red supergiant, and Rigel, a blue supergiant, have much greater luminosities and therefore, smaller absolute magnitudes. ...
... Although Bellatrix is the closest of these stars to Earth, Betelgeuse and Rigel appear brighter. This is because Betelgeuse, a red supergiant, and Rigel, a blue supergiant, have much greater luminosities and therefore, smaller absolute magnitudes. ...
Dark Matter In The 21st Century
... Coma cluster than in our galaxy 4) The vast majority of the Coma cluster’s mass is in non-luminous material (dark matter) To discriminate between these various possibilities, it would be necessary to study other clusters and see if they too had large mass-to-light ratios (Sinclair Smith, in 1936, f ...
... Coma cluster than in our galaxy 4) The vast majority of the Coma cluster’s mass is in non-luminous material (dark matter) To discriminate between these various possibilities, it would be necessary to study other clusters and see if they too had large mass-to-light ratios (Sinclair Smith, in 1936, f ...
2 Galaxy morphology and classification
... The spheroid is the smooth elliptical distribution of stars found in elliptical galaxies. It is composed primarily of an old, metal-poor, population of stars typically having ages „ 12 Gyr or more. The spheroid is thought to be among the first stellar components to form. The stellar halo is a di↵use ...
... The spheroid is the smooth elliptical distribution of stars found in elliptical galaxies. It is composed primarily of an old, metal-poor, population of stars typically having ages „ 12 Gyr or more. The spheroid is thought to be among the first stellar components to form. The stellar halo is a di↵use ...
flat field determinations using an isolated point source
... uncertainty in any single value of C/P. The 1 uncertainty from photon statistics that approach a million detected electrons is ~0.001. The differences, KF06T2-GD153, in C/P for F435W range from -0.022 to +0.031 for 13167 and from -0.012 to +0.032 for 13602, which suggests that the transmission of ...
... uncertainty in any single value of C/P. The 1 uncertainty from photon statistics that approach a million detected electrons is ~0.001. The differences, KF06T2-GD153, in C/P for F435W range from -0.022 to +0.031 for 13167 and from -0.012 to +0.032 for 13602, which suggests that the transmission of ...
Malmquist bias
The Malmquist bias is an effect in observational astronomy which leads to the preferential detection of intrinsically bright objects. It was first described in 1922 by Swedish astronomer Gunnar Malmquist (1893–1982), who then greatly elaborated upon this work in 1925. In statistics, this bias is referred to as a selection bias and affects the survey results in a brightness limited survey, where stars below a certain apparent brightness are not included. Since observed stars and galaxies appear dimmer when farther away, the brightness that is measured will fall off with distance until their brightness falls below the observational threshold. Objects which are more luminous, or intrinsically brighter, can be observed at a greater distance, creating a false trend of increasing intrinsic brightness, and other related quantities, with distance. This effect has led to many spurious claims in the field of astronomy. Properly correcting for these effects has become an area of great focus.