PowerPoint File
... Measure the distance over which the density of stars significantly falls off with height above, or distance below, the galactic plane. The distance depends on the type of objects considered, but is roughly 100 – 200 parsecs. The galactic plane is much thinner than it is wide. ...
... Measure the distance over which the density of stars significantly falls off with height above, or distance below, the galactic plane. The distance depends on the type of objects considered, but is roughly 100 – 200 parsecs. The galactic plane is much thinner than it is wide. ...
Globular Clusters
... What is a globular cluster? How do stars evolve? Observing Filters, tri-color image Age of and Distance to M13 Age of the Universe ...
... What is a globular cluster? How do stars evolve? Observing Filters, tri-color image Age of and Distance to M13 Age of the Universe ...
NASA`s Spitzer Images Out-of-This
... Helou, deputy director of NASA's Spitzer Science Center at the California Institute of Technology in Pasadena. "Some theories hold that the black hole might quiet down and eventually enter a more dormant state like our Milky Way black hole." The ring around the black hole is bursting with new star f ...
... Helou, deputy director of NASA's Spitzer Science Center at the California Institute of Technology in Pasadena. "Some theories hold that the black hole might quiet down and eventually enter a more dormant state like our Milky Way black hole." The ring around the black hole is bursting with new star f ...
The Life Cycle of Spiral Arm Galaxies
... As a star goes supernova, it releases a great amount of energy (light) and also ejects a massive amount of matter (galactic cosmic rays), which are charged particles such as protons and pieces of ...
... As a star goes supernova, it releases a great amount of energy (light) and also ejects a massive amount of matter (galactic cosmic rays), which are charged particles such as protons and pieces of ...
NEO lecture 02 - Observations of NEOs
... Typical values for TOTAS 1 m aperture, f/4.4 CCD camera has four sensors, 2048 x 2048 px2 Pixel scale 1.2”/px, field-of-view 0.7 deg x 0.7 deg ...
... Typical values for TOTAS 1 m aperture, f/4.4 CCD camera has four sensors, 2048 x 2048 px2 Pixel scale 1.2”/px, field-of-view 0.7 deg x 0.7 deg ...
SO FAR:
... Observed MW rotation curve • In principle, for stars, clusters, etc: • measure distance d and vr • assume circular orbit ...
... Observed MW rotation curve • In principle, for stars, clusters, etc: • measure distance d and vr • assume circular orbit ...
Radiation: The Key to Understanding the Universe
... given radius of a galaxy monotonically increases way beyond the radius of the visible disk of the galaxy. Ample evidence for dark matter has been collected from observations of rotation curves using the 21 cm hyperfine transition line emitted by neutral hydrogen gas clouds which continue to be presen ...
... given radius of a galaxy monotonically increases way beyond the radius of the visible disk of the galaxy. Ample evidence for dark matter has been collected from observations of rotation curves using the 21 cm hyperfine transition line emitted by neutral hydrogen gas clouds which continue to be presen ...
Astro 13 Galaxies & Cosmology LECTURE 1 28 Mar 2001 D. Koo
... • The evolution of the Universe can be essentially derived using the Newtonian equations. This is due to a peculiarity of the Newtonian force: in spherical symmetry the force due to the exterior distribution is zero. Then one can easily compute the evolution of a spherical “piece” of the Universe of ...
... • The evolution of the Universe can be essentially derived using the Newtonian equations. This is due to a peculiarity of the Newtonian force: in spherical symmetry the force due to the exterior distribution is zero. Then one can easily compute the evolution of a spherical “piece” of the Universe of ...
At the Heart of the Matter: The Blue White Dwarf in M 57. Paul Temple
... DO He rich objects with temperatures in excess of 45,000K. The spectrum is dominated by the signature of HeII, although H and higher elements may be observed in smaller amounts. DB This class may be regarded as an extension of the DO group into lower temperature regions (below around 30,000K). The c ...
... DO He rich objects with temperatures in excess of 45,000K. The spectrum is dominated by the signature of HeII, although H and higher elements may be observed in smaller amounts. DB This class may be regarded as an extension of the DO group into lower temperature regions (below around 30,000K). The c ...
PDF Version
... brightness that we can see ourselves, is equal to the intrinsic brightness divided by the square of the distance from us to the star. Astronomers used Cepheid variables in a nearby galaxy, which are all about the same distance from us, to find the correlation between the period and the intrinsic bri ...
... brightness that we can see ourselves, is equal to the intrinsic brightness divided by the square of the distance from us to the star. Astronomers used Cepheid variables in a nearby galaxy, which are all about the same distance from us, to find the correlation between the period and the intrinsic bri ...
instructor notes: weeks 9/10
... Lenticular galaxies get their name because they are “lenslike,” but are more like spiral and barred spiral galaxies in possessing a flattened disk, rather than like elliptical galaxies which mostly possess an ellipsoidal symmetry. The distinguishing feature of lenticulars relative to spiral galaxie ...
... Lenticular galaxies get their name because they are “lenslike,” but are more like spiral and barred spiral galaxies in possessing a flattened disk, rather than like elliptical galaxies which mostly possess an ellipsoidal symmetry. The distinguishing feature of lenticulars relative to spiral galaxie ...
13.1 Galaxy Evolution: Introduction
... time ago. And, again from theory tested by observations of star clusters and so on, we need stellar population evolution tracks: how does distribution of stars and color magnitude space – the HR Diagram – changes as a function of time for given amount of chemical enrichment, and so on. You take ...
... time ago. And, again from theory tested by observations of star clusters and so on, we need stellar population evolution tracks: how does distribution of stars and color magnitude space – the HR Diagram – changes as a function of time for given amount of chemical enrichment, and so on. You take ...
Slide 1
... • Typical time scale for a stellar event is 1 to 2 months. • If the ’lens’ star has a planet, its gravity may also contribute to lensing the light from the ’source’. • This produces a secondary peak in the light curve. • Typical exoplanetary deviation lasts only hours to days. ...
... • Typical time scale for a stellar event is 1 to 2 months. • If the ’lens’ star has a planet, its gravity may also contribute to lensing the light from the ’source’. • This produces a secondary peak in the light curve. • Typical exoplanetary deviation lasts only hours to days. ...
The Milky Way Galaxy
... spheroid. A massive black hole marks the center of the Galaxy. The (Our) Sun sits far out in the disc and in visible light. Our view of the Galaxy is limited by interstellar dust. Consequently, the large-scale structure of the Galaxy must be inferred from observations made at infrared and radio wave ...
... spheroid. A massive black hole marks the center of the Galaxy. The (Our) Sun sits far out in the disc and in visible light. Our view of the Galaxy is limited by interstellar dust. Consequently, the large-scale structure of the Galaxy must be inferred from observations made at infrared and radio wave ...
The myopia in the Hubble space telescope
... So the main problem in testing a hyperboloid surface is the spherical aberration. It has been common for about thirty years ago, to construct an optical system with spherical surfaces but with a spherical aberration that has an opposite sign to that of the mirror. Then the whole system produces a pe ...
... So the main problem in testing a hyperboloid surface is the spherical aberration. It has been common for about thirty years ago, to construct an optical system with spherical surfaces but with a spherical aberration that has an opposite sign to that of the mirror. Then the whole system produces a pe ...
TCE Syllabus Summary Blank
... identify data sources, and gather, process and analyse information to assess one of the models of the Universe developed from the time of Aristotle to the time of Newton to identify limitations placed on the development of the model by the technology available at the time ...
... identify data sources, and gather, process and analyse information to assess one of the models of the Universe developed from the time of Aristotle to the time of Newton to identify limitations placed on the development of the model by the technology available at the time ...
1” “Sky-Notes” of the Open University Astronomy Club. October 2005
... star charts or those such as available from the Variable Star Section of the BAA. The Section operates a “mentor” system where novices to variable star observation are given guidance and support. ...
... star charts or those such as available from the Variable Star Section of the BAA. The Section operates a “mentor” system where novices to variable star observation are given guidance and support. ...
11.3 Measuring Distances in Space
... we see today from Andromeda took 3.5 million years to get here, it is 3.5 million years old! ...
... we see today from Andromeda took 3.5 million years to get here, it is 3.5 million years old! ...
The portion of light we detect from a star/blackbody depends on
... several factors that have nothing to do with the star! --The area of our detector --The wavelengths to which it is sensitive (visible? IR? just green?) --The fraction of the star’s area whose light we receive. --The angle of our detector with respect to the incoming light. ...
... several factors that have nothing to do with the star! --The area of our detector --The wavelengths to which it is sensitive (visible? IR? just green?) --The fraction of the star’s area whose light we receive. --The angle of our detector with respect to the incoming light. ...
Final Study Guide
... 29. Discuss the apparent magnitudes and luminosity of a star. How can knowing both of them give us a star’s distance? 30. Describe characteristics of the main sequence stars. 31. Describe the stages in the formation of a new star. 32. Describe the nature and properties of a neutron star 33. What is ...
... 29. Discuss the apparent magnitudes and luminosity of a star. How can knowing both of them give us a star’s distance? 30. Describe characteristics of the main sequence stars. 31. Describe the stages in the formation of a new star. 32. Describe the nature and properties of a neutron star 33. What is ...
File
... Example: The first star to be measured this way was a star in the constellation of Cygnus. The angular difference was found to be 0.292 arcseconds. This gives a distance of 3.48 pc, or 11.36 light years ...
... Example: The first star to be measured this way was a star in the constellation of Cygnus. The angular difference was found to be 0.292 arcseconds. This gives a distance of 3.48 pc, or 11.36 light years ...
Hubble Deep Field
The Hubble Deep Field (HDF) is an image of a small region in the constellation Ursa Major, constructed from a series of observations by the Hubble Space Telescope. It covers an area 2.5 arcminutes across, about one 24-millionth of the whole sky, which is equivalent in angular size to a 65 mm tennis ball at a distance of 100 metres. The image was assembled from 342 separate exposures taken with the Space Telescope's Wide Field and Planetary Camera 2 over ten consecutive days between December 18 and December 28, 1995.The field is so small that only a few foreground stars in the Milky Way lie within it; thus, almost all of the 3,000 objects in the image are galaxies, some of which are among the youngest and most distant known. By revealing such large numbers of very young galaxies, the HDF has become a landmark image in the study of the early universe, with the associated scientific paper having received over 900 citations by the end of 2014.Three years after the HDF observations were taken, a region in the south celestial hemisphere was imaged in a similar way and named the Hubble Deep Field South. The similarities between the two regions strengthened the belief that the universe is uniform over large scales and that the Earth occupies a typical region in the Universe (the cosmological principle). A wider but shallower survey was also made as part of the Great Observatories Origins Deep Survey. In 2004 a deeper image, known as the Hubble Ultra-Deep Field (HUDF), was constructed from a few months of light exposure. The HUDF image was at the time the most sensitive astronomical image ever made at visible wavelengths, and it remained so until the Hubble Extreme Deep Field (XDF) was released in 2012.