Hubble Diagram Instruction Sheet
... Type Ia supernovae only. Type Ia supernovae are very important in astronomy as they offer the most reliable sources for measuring cosmic distances up to and beyond 1000 mega parsecs (Mpc). A parsec (pc) is a unit of length used to measure the distances to objects in space. One parsec is equal to 3.0 ...
... Type Ia supernovae only. Type Ia supernovae are very important in astronomy as they offer the most reliable sources for measuring cosmic distances up to and beyond 1000 mega parsecs (Mpc). A parsec (pc) is a unit of length used to measure the distances to objects in space. One parsec is equal to 3.0 ...
DSLR Photometry
... were obtained and any other such information that may be deemed important. Because the data will be combined with other data it is important to standardize how it is reported. For a typical night there will be one data point for each . observed and one observation date and time band for the evenings ...
... were obtained and any other such information that may be deemed important. Because the data will be combined with other data it is important to standardize how it is reported. For a typical night there will be one data point for each . observed and one observation date and time band for the evenings ...
Spiral Galaxies - Astronomy Centre
... Sizes range from about 3,000 to hundreds of thousands of light years No strong dependence of luminosity and size on Hubble type Mass is not so important in determining the appearance of a galaxy as it is for a star A large, distant galaxy looks similar to a nearby, smaller galaxy ...
... Sizes range from about 3,000 to hundreds of thousands of light years No strong dependence of luminosity and size on Hubble type Mass is not so important in determining the appearance of a galaxy as it is for a star A large, distant galaxy looks similar to a nearby, smaller galaxy ...
Star-D_Teacher_Guide - The University of Texas at Dallas
... Discuss the distances of the planets from the Sun in comparison with the distances between stars. Earth, as discussed earlier, is only 15 meters from the Sun on this scale model. Compared with ...
... Discuss the distances of the planets from the Sun in comparison with the distances between stars. Earth, as discussed earlier, is only 15 meters from the Sun on this scale model. Compared with ...
A6 - Vicphysics
... For this point it is useful to provide example maps of a region of the night sky for a specific time in two versions; one with an altitude-azimuth coordinate system (alt-az), the other using the right ascension-declination system. Students can determine the location of one or more identified stars u ...
... For this point it is useful to provide example maps of a region of the night sky for a specific time in two versions; one with an altitude-azimuth coordinate system (alt-az), the other using the right ascension-declination system. Students can determine the location of one or more identified stars u ...
the UKIRT Fundamental and Extended lists
... a fixed dynamic range, and as its sensitivity increases, so the brightest measurable sources become fainter. This is well illustrated by developments at UKIRT. After 1985 the IRCAM series of instruments (McLean et al. 1986) became the ‘workhorse’ imagers. The last of these, IRCAM3 (Puxley et al. 199 ...
... a fixed dynamic range, and as its sensitivity increases, so the brightest measurable sources become fainter. This is well illustrated by developments at UKIRT. After 1985 the IRCAM series of instruments (McLean et al. 1986) became the ‘workhorse’ imagers. The last of these, IRCAM3 (Puxley et al. 199 ...
JHK standard stars for large telescopes: the UKIRT Fundamental
... a fixed dynamic range, and as its sensitivity increases, so the brightest measurable sources become fainter. This is well illustrated by developments at UKIRT. After 1985 the IRCAM series of instruments (McLean et al. 1986) became the ‘workhorse’ imagers. The last of these, IRCAM3 (Puxley et al. 199 ...
... a fixed dynamic range, and as its sensitivity increases, so the brightest measurable sources become fainter. This is well illustrated by developments at UKIRT. After 1985 the IRCAM series of instruments (McLean et al. 1986) became the ‘workhorse’ imagers. The last of these, IRCAM3 (Puxley et al. 199 ...
Properties of Stars - Montana State University Extended University
... A G2 star appears 25 times dimmer than it would if it was at the standard distance of 10 parsecs used for the absolute magnitude. The G2 star is at a distance of = 10 × Sqrt[1/(1/25)] = 10 × Sqrt[25/1] = 50 parsecs from us. Distances to red giant and supergiant stars are found in a similar way but y ...
... A G2 star appears 25 times dimmer than it would if it was at the standard distance of 10 parsecs used for the absolute magnitude. The G2 star is at a distance of = 10 × Sqrt[1/(1/25)] = 10 × Sqrt[25/1] = 50 parsecs from us. Distances to red giant and supergiant stars are found in a similar way but y ...
Observing the Night Sky - Constellations
... If the night is clear, and you are diligent, you may be able to find some of the less prominent constellations that are located between the major constellations. Be sure to make use of the binoculars available to assist you in seeing the fainter stars. 3. Determine Limiting Magnitude - Your instruct ...
... If the night is clear, and you are diligent, you may be able to find some of the less prominent constellations that are located between the major constellations. Be sure to make use of the binoculars available to assist you in seeing the fainter stars. 3. Determine Limiting Magnitude - Your instruct ...
Globular Clusters
... contain one of the most popular intrinsic variable stars, the so-called RR LYRAE STARS. These stars have light variation amplitudes less than a couple of magnitudes and periods ranging from 0.2 to 1.1 days. Since their mean absolute magnitude is constant and fairly independent of metallicity (to wit ...
... contain one of the most popular intrinsic variable stars, the so-called RR LYRAE STARS. These stars have light variation amplitudes less than a couple of magnitudes and periods ranging from 0.2 to 1.1 days. Since their mean absolute magnitude is constant and fairly independent of metallicity (to wit ...
Camelopardalis-Better-Know-A-Constellation
... • Although Camelopardalis is the 18th largest constellation, (757 sq. deg. ) it is not a particularly bright constellation, as the brightest stars are only of fourth magnitude. • β Camelopardalis is the brightest star, at apparent magnitude 4.03. This star is a double star, with components of magnit ...
... • Although Camelopardalis is the 18th largest constellation, (757 sq. deg. ) it is not a particularly bright constellation, as the brightest stars are only of fourth magnitude. • β Camelopardalis is the brightest star, at apparent magnitude 4.03. This star is a double star, with components of magnit ...
Exploring the Variable Sky with the Catalina Real-Time
... • It is a fully open survey: all data are made public instantly, with no proprietary period at all – Benefits the entire community and maximizes the follow-up and the resulting science – A new “open data” sociology – the shifting focus from the ownership of data to the ownership of expertise ...
... • It is a fully open survey: all data are made public instantly, with no proprietary period at all – Benefits the entire community and maximizes the follow-up and the resulting science – A new “open data” sociology – the shifting focus from the ownership of data to the ownership of expertise ...
powerpoint - High Energy Physics at Wayne State
... Sun is ~ 30000 LY from the center of our Galaxy. From our location within the galaxy, we cannot see through its far rim because the space between stars is not empty – interstellar dust or gas which absorbs visible light. The interstellar gas is the fuel for the formation of stars. Yet, interstellar ...
... Sun is ~ 30000 LY from the center of our Galaxy. From our location within the galaxy, we cannot see through its far rim because the space between stars is not empty – interstellar dust or gas which absorbs visible light. The interstellar gas is the fuel for the formation of stars. Yet, interstellar ...
Chapter 15
... another. Take time to understand it now!!!! • Come to a consensus answer you both agree ...
... another. Take time to understand it now!!!! • Come to a consensus answer you both agree ...
The Hubble Ultra Deep Field Project Overview
... expanding, or similarly, find that the further away an object is, the rate at which it is moving increases. Using the Hubble Ultra Deep Field, in which a variety of galaxies distances and cosmological redshift velocities have been calculated. You will use this dataset, in combination with the princi ...
... expanding, or similarly, find that the further away an object is, the rate at which it is moving increases. Using the Hubble Ultra Deep Field, in which a variety of galaxies distances and cosmological redshift velocities have been calculated. You will use this dataset, in combination with the princi ...
Standing in Awe - Auckland Astronomical Society
... Libra lies prominently in the June sky, preceding the Scorpion across the sky. At 538° square in size, Libra is one of the larger constellations, though its stars are poorly shown, the brightest attaining magnitude 2.6. In fact, Libra is one of the poorer adorned constellations, there being only 2.4 ...
... Libra lies prominently in the June sky, preceding the Scorpion across the sky. At 538° square in size, Libra is one of the larger constellations, though its stars are poorly shown, the brightest attaining magnitude 2.6. In fact, Libra is one of the poorer adorned constellations, there being only 2.4 ...
lunar parallax measurement
... A basic knowledge of trigonometry is required in order that an accurate calculation of the distance to the moon can be carried out. However it is also possible to achieve this by a simpler, but less accurate method. This is particularly suitable for lower secondary school students and amateur astron ...
... A basic knowledge of trigonometry is required in order that an accurate calculation of the distance to the moon can be carried out. However it is also possible to achieve this by a simpler, but less accurate method. This is particularly suitable for lower secondary school students and amateur astron ...
Galaxies Galaxies M81
... • Beginning of the 20th century, what we now call galaxies were referred to as “spiral nebulae” • Believed to be clouds of gas and stars associated with Milky Way. • In 1924 Edwin Hubble measured distance to the “Great Nebula in Andromeda” (M 31) and found its distance to be much larger than the dia ...
... • Beginning of the 20th century, what we now call galaxies were referred to as “spiral nebulae” • Believed to be clouds of gas and stars associated with Milky Way. • In 1924 Edwin Hubble measured distance to the “Great Nebula in Andromeda” (M 31) and found its distance to be much larger than the dia ...
Advancing Physics A2
... The time dilation factor γ is very close to 1 for v substantially less than c but increases rapidly as v approaches c. We start with a discussion of what is involved in ‘thinking relatively’. In Question 50C Comprehension ‘Thinking relatively’ you have to learn to describe events seen from different ...
... The time dilation factor γ is very close to 1 for v substantially less than c but increases rapidly as v approaches c. We start with a discussion of what is involved in ‘thinking relatively’. In Question 50C Comprehension ‘Thinking relatively’ you have to learn to describe events seen from different ...
The Extragalactic Group of MPE and USM
... be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter luminosities, larger sample (~10000 galaxies in FDF and GOODS S sub-sample) • FORS Deep Field (IAB=26.8): 98% of all galaxies with dz/(1+z)<0.03; GOODS S (KAB=25.4): dz/(1+z)<0.055 • Deep I-selec ...
... be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter luminosities, larger sample (~10000 galaxies in FDF and GOODS S sub-sample) • FORS Deep Field (IAB=26.8): 98% of all galaxies with dz/(1+z)<0.03; GOODS S (KAB=25.4): dz/(1+z)<0.055 • Deep I-selec ...
Spectroscopic confirmation of a galaxy at redshift z=8.6
... systematic uncertainty of up to 30–40%, but this does not affect the estimate of the significance of the line detection. The night sky spectrum, scaled arbitrarily, is shown in grey. Regions of particularly deviant values in the spectrum correspond to strong night sky lines. The emission line from t ...
... systematic uncertainty of up to 30–40%, but this does not affect the estimate of the significance of the line detection. The night sky spectrum, scaled arbitrarily, is shown in grey. Regions of particularly deviant values in the spectrum correspond to strong night sky lines. The emission line from t ...
A Hero`s Little Horse: Discovery of a Dissolving Star Cluster in
... deg by using the fit bivariate normal function of the astroML package (VanderPlas et al. 2012). The error bars were derived from Poisson statistics. Overplotted is the best-fit Plummer profile (Plummer 1911) to parametrise the underlying stellar distribution. We obtain a half-light radius of 1.2 ± 0 ...
... deg by using the fit bivariate normal function of the astroML package (VanderPlas et al. 2012). The error bars were derived from Poisson statistics. Overplotted is the best-fit Plummer profile (Plummer 1911) to parametrise the underlying stellar distribution. We obtain a half-light radius of 1.2 ± 0 ...
File
... Spectroscopic parallax is simply comparison of brightness of identical stars. Standard candle is comparison of brightness of identical supernovae explosions. Tully-Fisher is a way to measure galaxy luminosity from its rotations speed. ...
... Spectroscopic parallax is simply comparison of brightness of identical stars. Standard candle is comparison of brightness of identical supernovae explosions. Tully-Fisher is a way to measure galaxy luminosity from its rotations speed. ...
Practice final exam -all multiple choice
... 17. A bicycle is redesigned such that the rims of the wheels are made lighter but more weight is added to the frame so the total weight of the bike remains unchanged. Compared to the old bike, when the new bike is moving at a given speed, its total kinetic energy is.. A: less. B: greater C: the same ...
... 17. A bicycle is redesigned such that the rims of the wheels are made lighter but more weight is added to the frame so the total weight of the bike remains unchanged. Compared to the old bike, when the new bike is moving at a given speed, its total kinetic energy is.. A: less. B: greater C: the same ...
VY Canis Majoris: The Astrophysical Basis of Its Luminosity
... Adopting this spectral type with the temperature scale proposed by Levesque, et al (2005) gives Tef f ∼ 3450–3535◦, while an older scale (used in Humphreys & McElroy 1984 from Flower 1977) yields Tef f ∼ 3200◦ for an M4-M5 star. However, one should be cautious in the case of VY CMa; we are not obser ...
... Adopting this spectral type with the temperature scale proposed by Levesque, et al (2005) gives Tef f ∼ 3450–3535◦, while an older scale (used in Humphreys & McElroy 1984 from Flower 1977) yields Tef f ∼ 3200◦ for an M4-M5 star. However, one should be cautious in the case of VY CMa; we are not obser ...
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.