PDF
... Eric Høg in his 2001 Miraculous approval of Hipparcos, the key idea of using slits and photo cells to measure the position and brightness of stars as they pass in front of a detector, was posed first in 1926 by B. Strömgren. Høg himself in 1960 extended the idea by including counting techniques that ...
... Eric Høg in his 2001 Miraculous approval of Hipparcos, the key idea of using slits and photo cells to measure the position and brightness of stars as they pass in front of a detector, was posed first in 1926 by B. Strömgren. Høg himself in 1960 extended the idea by including counting techniques that ...
Exam 2
... hot remnant of the central star heats the gas, causing it to glow. For a few thousand years, the dying star is surrounded by a beautiful gleaming cloud known as a planetary nebula. Planetary nebulae have a spectacular array of shapes, sizes and structures. This diversity holds clues about stellar ev ...
... hot remnant of the central star heats the gas, causing it to glow. For a few thousand years, the dying star is surrounded by a beautiful gleaming cloud known as a planetary nebula. Planetary nebulae have a spectacular array of shapes, sizes and structures. This diversity holds clues about stellar ev ...
Chapter 12 Quiz, Nov. 28, 2012, Astro 162, Section 4 12-1
... 12-17. If a galaxy is moving away from us, its absorption lines will: a) change towards higher or lower wavelengths depending on the speed of the galaxy. b) remain at the same wavelengths as lines from galaxies not moving away from us. c) all change towards shorter wavelengths. d) all change towards ...
... 12-17. If a galaxy is moving away from us, its absorption lines will: a) change towards higher or lower wavelengths depending on the speed of the galaxy. b) remain at the same wavelengths as lines from galaxies not moving away from us. c) all change towards shorter wavelengths. d) all change towards ...
PSF - ESO
... First you must FIND the stellar-appearing objects in the frame. Each program has its own method - sometimes several methods – of performing this, but the basic idea is to produce an initial list of approximate centroid positions for all stars that can be distinguished in the two dimensional data arr ...
... First you must FIND the stellar-appearing objects in the frame. Each program has its own method - sometimes several methods – of performing this, but the basic idea is to produce an initial list of approximate centroid positions for all stars that can be distinguished in the two dimensional data arr ...
Astrophysical parameters of ten poorly studied open star clusters
... our investigated clusters to unify the estimation of the main parameters, especially ages, distances and reddening. JHK color-color diagrams (CCDs) do not strongly depend on metallicity whereas reddening is represented as a straight vector on the CCDs. On the other hand, for relatively young cluster ...
... our investigated clusters to unify the estimation of the main parameters, especially ages, distances and reddening. JHK color-color diagrams (CCDs) do not strongly depend on metallicity whereas reddening is represented as a straight vector on the CCDs. On the other hand, for relatively young cluster ...
The Milky Way and other Galaxies
... dwarf in a binary system): Type Ia supernovae have well known standard luminosities Compare to apparent magnitudes Find its distances Both are “Standard-candle” methods: Know absolute magnitude (luminosity) compare to apparent magnitude find distance. ...
... dwarf in a binary system): Type Ia supernovae have well known standard luminosities Compare to apparent magnitudes Find its distances Both are “Standard-candle” methods: Know absolute magnitude (luminosity) compare to apparent magnitude find distance. ...
1 Assignment Discovery Online Curriculum Lesson title
... 1. Parallax is the apparent change in position of an object when it's viewed from two different places. Astronomers use this phenomenon to measure the distances to some stars. They assume that the stars are fixed, and as the Earth moves in orbit they take measurements of the apparent shift in positi ...
... 1. Parallax is the apparent change in position of an object when it's viewed from two different places. Astronomers use this phenomenon to measure the distances to some stars. They assume that the stars are fixed, and as the Earth moves in orbit they take measurements of the apparent shift in positi ...
Activities
... This activity is meant to give you a review of math that will be both useful and important in Astronomy 101. If this is not a review and you find it difficult, please stop by my office hours, or study Appendix C of your text. ...
... This activity is meant to give you a review of math that will be both useful and important in Astronomy 101. If this is not a review and you find it difficult, please stop by my office hours, or study Appendix C of your text. ...
Galaxies - Mike Brotherton
... dwarf in a binary system): Type Ia supernovae have well known standard luminosities Compare to apparent magnitudes Find its distances Both are “Standard-candle” methods: Know absolute magnitude (luminosity) compare to apparent magnitude find distance. ...
... dwarf in a binary system): Type Ia supernovae have well known standard luminosities Compare to apparent magnitudes Find its distances Both are “Standard-candle” methods: Know absolute magnitude (luminosity) compare to apparent magnitude find distance. ...
01-Star Atlas Project - Mapping the Heavens
... Such a mysterious phrase. Well, actually only one of the three words is unfamiliar. ...
... Such a mysterious phrase. Well, actually only one of the three words is unfamiliar. ...
An analogy
... • The Hubble classification was thought to be evolutionary sequence: – galaxies on the left part of the tuning-fork (E) would evolve into the right-hand side types (S). This is why we often speak of early-type and late-type galaxies. ...
... • The Hubble classification was thought to be evolutionary sequence: – galaxies on the left part of the tuning-fork (E) would evolve into the right-hand side types (S). This is why we often speak of early-type and late-type galaxies. ...
presentation source
... suggested by looking at Galaxy Rotation Curves for all spiral galaxies, as we shall see ...
... suggested by looking at Galaxy Rotation Curves for all spiral galaxies, as we shall see ...
Pre-Lab
... northern sky, the Andromeda nebulae, as it was called before its true nature was known. It is a faint fuzzy patch in the region of the sky containing the stars of the constellation Andromeda. Two galaxies, the Large and Small Magellanic Clouds, can be seen with unaided eyes in the southern sky from ...
... northern sky, the Andromeda nebulae, as it was called before its true nature was known. It is a faint fuzzy patch in the region of the sky containing the stars of the constellation Andromeda. Two galaxies, the Large and Small Magellanic Clouds, can be seen with unaided eyes in the southern sky from ...
Galaxies - University of Iowa Astrophysics
... Why are Cepheid variable stars useful in determining distances? A) They all have the same distance. B) Their luminosity can be determined from their pulsation period. C) They all have the same luminosity. D) They all have the same radius. ...
... Why are Cepheid variable stars useful in determining distances? A) They all have the same distance. B) Their luminosity can be determined from their pulsation period. C) They all have the same luminosity. D) They all have the same radius. ...
White dwarfs from GAIA: The 7th dimension
... • The white dwarf luminosity function of Gaia is a sensitive probe of the averaged star formation rate • Due to their very short main-sequence lifetimes the shape of the SFR can be reconstructed from the luminosity function of massive white dwarfs • To achieve these goals, we need R~5000 spectroscop ...
... • The white dwarf luminosity function of Gaia is a sensitive probe of the averaged star formation rate • Due to their very short main-sequence lifetimes the shape of the SFR can be reconstructed from the luminosity function of massive white dwarfs • To achieve these goals, we need R~5000 spectroscop ...
Constellation ARA
... planet 12152 Aratus are Hades, and Poseidon. When the named in his honour youngest child, Zeus, was born, his mother Rhea hid him in Crete and gave Cronus a stone to swallow, telling him the stone was Zeus. When Zeus grew up, he made Cronus vomit his brothers and sisters. Once freed, they banded tog ...
... planet 12152 Aratus are Hades, and Poseidon. When the named in his honour youngest child, Zeus, was born, his mother Rhea hid him in Crete and gave Cronus a stone to swallow, telling him the stone was Zeus. When Zeus grew up, he made Cronus vomit his brothers and sisters. Once freed, they banded tog ...
Local Horizon View
... Meridian is the important North/South line through your zenith and also through both celestial poles. We look at our celestial objects while we are oriented along our North/South meridian ...
... Meridian is the important North/South line through your zenith and also through both celestial poles. We look at our celestial objects while we are oriented along our North/South meridian ...
There are 88 constellations in the sky around the Earth. 12 are the
... Principal stars are Hamal (Alpha ), magnitude 2.0 and Sheratan (Beta), magnitude 2.6. Mesartim (Gamma) is a nice optical double star, magnitudes 4.6 & 4.7, easily resolved with a small telescope. (Magnitude is a measure of how bright a star is – a magnitude 2 star is 2 ½ times fainter than a magnitu ...
... Principal stars are Hamal (Alpha ), magnitude 2.0 and Sheratan (Beta), magnitude 2.6. Mesartim (Gamma) is a nice optical double star, magnitudes 4.6 & 4.7, easily resolved with a small telescope. (Magnitude is a measure of how bright a star is – a magnitude 2 star is 2 ½ times fainter than a magnitu ...
Astrophysics Questions (DRAFT)
... 15. What is the moving cluster method of determining distances, and how does it work? 16. What is spectroscopic parallax? How would you use this method to determine the distance to a globular cluster? 17. What are \apparent magnitude," \absolute magnitude," and \bolometric magnitude"? What are U, B, ...
... 15. What is the moving cluster method of determining distances, and how does it work? 16. What is spectroscopic parallax? How would you use this method to determine the distance to a globular cluster? 17. What are \apparent magnitude," \absolute magnitude," and \bolometric magnitude"? What are U, B, ...
www.astro.org.uk www.facebook.com/Stra ordAstro www.twi er.com
... The improvement in the measurement of the distance to the Large Magellanic Cloud also gives be4er distances for many Cepheid variable stars . These bright pulsa:ng stars are used as standard candles to measure distances out to more remote galaxies and to determine the expansion rate of the Universe ...
... The improvement in the measurement of the distance to the Large Magellanic Cloud also gives be4er distances for many Cepheid variable stars . These bright pulsa:ng stars are used as standard candles to measure distances out to more remote galaxies and to determine the expansion rate of the Universe ...
presentation (PPT format)
... The difference between Sa, Sb and Sc may be related To the relative amounts of gas and dust that they contain 4% of the mass of a Sa galaxy is in gas & dust 8% for a Sb And 25% for Sc Sc has a greater proportion of its mass involed in star formation ...
... The difference between Sa, Sb and Sc may be related To the relative amounts of gas and dust that they contain 4% of the mass of a Sa galaxy is in gas & dust 8% for a Sb And 25% for Sc Sc has a greater proportion of its mass involed in star formation ...
ppt - NRAO
... With 10 times more sensitivity (after the VLBA sensitivity upgrade is complete), it should become possible to truly map out the distribution of star-forming regions around the Sun. Of course, better sensitivity also implies closer calibrators, and better calibration ...
... With 10 times more sensitivity (after the VLBA sensitivity upgrade is complete), it should become possible to truly map out the distribution of star-forming regions around the Sun. Of course, better sensitivity also implies closer calibrators, and better calibration ...
The Milky Way: Spiral galaxies:
... absorption. Note that spin flips are classically “forbidden”: on average, a single hydrogen atom will take 107 years to decay! The probability of an absorption is even rarer. •! HI gas mass is directly proportional to 21 cm line intensity •! HI disk is much more extended than optical light, typicall ...
... absorption. Note that spin flips are classically “forbidden”: on average, a single hydrogen atom will take 107 years to decay! The probability of an absorption is even rarer. •! HI gas mass is directly proportional to 21 cm line intensity •! HI disk is much more extended than optical light, typicall ...
Geoscience Astronomy Formative on Stellar Evolution and
... A rapidly spinning neutron star that emits bursts of radio and optical energy is a a. supernova c. black hole b. red giant d. pulsar Pulsars emanate from a. Black holes c. White dwarfs b. Neutron stars d. Electron degenerate cores The most massive stars will collapse into a. Neutron stars c. White d ...
... A rapidly spinning neutron star that emits bursts of radio and optical energy is a a. supernova c. black hole b. red giant d. pulsar Pulsars emanate from a. Black holes c. White dwarfs b. Neutron stars d. Electron degenerate cores The most massive stars will collapse into a. Neutron stars c. White d ...
Supermassive Black Holes in Inactive Galaxies Encyclopedia of Astronomy & Astrophysics eaa.iop.org
... BH masses are M• ~ 106–109.5M⊙. A wide array of phenomena can be understood within this picture. However, the subject has had an outstanding problem: there was no dynamical evidence that BHs exist. The search for BHs has therefore become one of the hottest topics in extragalactic astronomy. Since mo ...
... BH masses are M• ~ 106–109.5M⊙. A wide array of phenomena can be understood within this picture. However, the subject has had an outstanding problem: there was no dynamical evidence that BHs exist. The search for BHs has therefore become one of the hottest topics in extragalactic astronomy. Since mo ...
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.