Lab 2
... -Cass: A Be emission line-star. Antares ( Sco). A red supergiant. P-Cygni: A mass losing supergiant. This is about mV ~ 5 and will require long exposures. Do only the part of the spectrum centered on H-alpha. Jupiter: This planet is now available. I want to see if we can (a) detect the [SII] 67 ...
... -Cass: A Be emission line-star. Antares ( Sco). A red supergiant. P-Cygni: A mass losing supergiant. This is about mV ~ 5 and will require long exposures. Do only the part of the spectrum centered on H-alpha. Jupiter: This planet is now available. I want to see if we can (a) detect the [SII] 67 ...
γ The potential for intensity interferometry with -ray telescope arrays
... overview see [12]), ensuring that a substantial fraction of the low-mass members are still in their PMS contraction phase. Measurements of their angular size can be used in the calibration of evolutionary tracks, fundamental in deriving the properties of star forming regions and young stellar cluste ...
... overview see [12]), ensuring that a substantial fraction of the low-mass members are still in their PMS contraction phase. Measurements of their angular size can be used in the calibration of evolutionary tracks, fundamental in deriving the properties of star forming regions and young stellar cluste ...
Chapter 2 User`s Guide to the Sky: Patterns and Cycles
... • For example, the Big Dipper is an asterism you probably recognize that is part of the constellation Ursa Major (the Great Bear). ...
... • For example, the Big Dipper is an asterism you probably recognize that is part of the constellation Ursa Major (the Great Bear). ...
1.1 Fundamental Observers
... λ0 where λobs is the observed wavelength of a given spectral line, and λ0 is the rest-frame wavelength of the same atomic transition, as measured in the laboratory. ...
... λ0 where λobs is the observed wavelength of a given spectral line, and λ0 is the rest-frame wavelength of the same atomic transition, as measured in the laboratory. ...
ph507lecnote06
... units such as in feet, km, light years, parsecs etc. It has been excrutiatingly difficult to measure astronomical distances until this century. Unfortunately most stars are so far away that it is impossible to directly measure the distance using the classic technique of triangulation. Trignometric p ...
... units such as in feet, km, light years, parsecs etc. It has been excrutiatingly difficult to measure astronomical distances until this century. Unfortunately most stars are so far away that it is impossible to directly measure the distance using the classic technique of triangulation. Trignometric p ...
An introduce of the spectrograph of the GALEX
... core-collapse supernovae, which applies primarily to z<~1. (...) The traditional Salpeter IMF, assumed for convenience by many authors, is known to be a poor representation at low stellar masses (<~1 Msolar), and we show that recently favored IMFs are also constrained. (...) To resolve the outstandi ...
... core-collapse supernovae, which applies primarily to z<~1. (...) The traditional Salpeter IMF, assumed for convenience by many authors, is known to be a poor representation at low stellar masses (<~1 Msolar), and we show that recently favored IMFs are also constrained. (...) To resolve the outstandi ...
AST301.Ch18.InterstelMed - University of Texas Astronomy
... Also, because this is a spectral line (unlike dust, which gives us only continuous absorption), we can get radial velocities of the gas motions this way (Fig. 18.18). The results show that our galaxy has an overall rotation (we’ll return to this later—this rotation is one of the primary indicators o ...
... Also, because this is a spectral line (unlike dust, which gives us only continuous absorption), we can get radial velocities of the gas motions this way (Fig. 18.18). The results show that our galaxy has an overall rotation (we’ll return to this later—this rotation is one of the primary indicators o ...
ABSOLUTE AND APPARENT MAGNITUDES
... As a general (not vastly accurate, but close enough) rule of thumb, the highest apparent magnitude that the naked eye can see under ideal viewing conditions is about +6. Objects can cast visible shadows around an apparent magnitude -4 (you’d need a very dark night to see them though - they’d get pr ...
... As a general (not vastly accurate, but close enough) rule of thumb, the highest apparent magnitude that the naked eye can see under ideal viewing conditions is about +6. Objects can cast visible shadows around an apparent magnitude -4 (you’d need a very dark night to see them though - they’d get pr ...
2009_ASU_Exam
... 13) Star N and Star O are both main sequence stars. Star N is of spectral class A0 and Star O is of spectral class K5. They have the same apparent magnitude as observed from earth. If an observer were able to move 10 pcs closer to both stars, which star will appear brighter from the new observation ...
... 13) Star N and Star O are both main sequence stars. Star N is of spectral class A0 and Star O is of spectral class K5. They have the same apparent magnitude as observed from earth. If an observer were able to move 10 pcs closer to both stars, which star will appear brighter from the new observation ...
Locating True North in Ancient China
... We saw above that the eastern and western walls of Dìng are typically depicted as two parallel lines comprising two stars apiece. But they share an even more important characteristic in common. If one looks at the meridians in the chart in Figure 1, which reflects the situation in 650 BCE (around th ...
... We saw above that the eastern and western walls of Dìng are typically depicted as two parallel lines comprising two stars apiece. But they share an even more important characteristic in common. If one looks at the meridians in the chart in Figure 1, which reflects the situation in 650 BCE (around th ...
– 1 – 1. Chemical Evolution 1.1.
... Note that the transformation from luminosity to mass (the IMF is a function of stellar mass) is not as well determined for the lowest mass stars). In their most recent work, Weidner, Kroupa & Bonell (2010, MNRAS, 401, 275) explore the statistical issues associated with massive stars forming in clust ...
... Note that the transformation from luminosity to mass (the IMF is a function of stellar mass) is not as well determined for the lowest mass stars). In their most recent work, Weidner, Kroupa & Bonell (2010, MNRAS, 401, 275) explore the statistical issues associated with massive stars forming in clust ...
Astronomy Part 1 Regents Questions
... toward the ultraviolet end of the spectrum and the star is moving toward Earth. B) The star’s spectral lines have shifted toward the ultraviolet end of the spectrum and the star is moving away from Earth. C) The star’s spectral lines have shifted toward the infrared end of the spectrum and the star ...
... toward the ultraviolet end of the spectrum and the star is moving toward Earth. B) The star’s spectral lines have shifted toward the ultraviolet end of the spectrum and the star is moving away from Earth. C) The star’s spectral lines have shifted toward the infrared end of the spectrum and the star ...
Word version of Episode 704
... Speed was much easier to measure (from the Doppler shift) than distance. There are real problems in setting a length scale. Different methods are used at the ever increasing distances, each overlapping to allow a (hopefully) consistent calibration. Hubble found v d; for each increase in distance o ...
... Speed was much easier to measure (from the Doppler shift) than distance. There are real problems in setting a length scale. Different methods are used at the ever increasing distances, each overlapping to allow a (hopefully) consistent calibration. Hubble found v d; for each increase in distance o ...
The Properties of Stars Early in its history, the universe organized
... distributed these heavier elements throughout the galaxy so that late-generation stars had small but significant amounts of elements heavier than helium. Our sun, which formed 4.6 billion years ago, is one such star. The Sun: An Average Star After eons of observing the fiery ball they saw in the day ...
... distributed these heavier elements throughout the galaxy so that late-generation stars had small but significant amounts of elements heavier than helium. Our sun, which formed 4.6 billion years ago, is one such star. The Sun: An Average Star After eons of observing the fiery ball they saw in the day ...
galaxy solar system supernova
... 1. An astronomer is a scientist who studies planets, stars, galaxies, and other objects in space. 2. You would expect an astronomer to use a telescope. 3. She wants to be an astronomer someday, so she is taking many science classes in college. ...
... 1. An astronomer is a scientist who studies planets, stars, galaxies, and other objects in space. 2. You would expect an astronomer to use a telescope. 3. She wants to be an astronomer someday, so she is taking many science classes in college. ...
ACTIVE GALAXIES
... • The Hubble Space Telescope has revealed that star velocities rise to very high values close to center of many galaxies and gas is orbiting rapidly, e.g. M87 • Disks have been seen via MASERS in some nearby Seyfert AGN. • VLBI: radio jets formed within 1 pc of center. • There are several other more ...
... • The Hubble Space Telescope has revealed that star velocities rise to very high values close to center of many galaxies and gas is orbiting rapidly, e.g. M87 • Disks have been seen via MASERS in some nearby Seyfert AGN. • VLBI: radio jets formed within 1 pc of center. • There are several other more ...
Coordinate Systems - AST 114, Astronomy Lab II for Spring 2017!
... The method to measure azimuth takes advantage of the fact that you already know the specific azimuths of the 4 cardinal directions. First, locate due north (which is 0o), then locate the point on the horizon directly below the object you are interested in. From this point, use your hands to estimate ...
... The method to measure azimuth takes advantage of the fact that you already know the specific azimuths of the 4 cardinal directions. First, locate due north (which is 0o), then locate the point on the horizon directly below the object you are interested in. From this point, use your hands to estimate ...
Ursa Major
Ursa Major /ˈɜrsə ˈmeɪdʒər/ (also known as the Great Bear and Charles' Wain) is a constellation in the northern celestial hemisphere. One of the 48 constellations listed by Ptolemy (second century AD), it remains one of the 88 modern constellations. It can be visible throughout the year in most of the northern hemisphere. Its name, Latin for ""the greater (or larger) she-bear"", stands as a reference to and in direct contrast with Ursa Minor, ""the smaller she-bear"", with which it is frequently associated in mythology and amateur astronomy. The constellation's most recognizable asterism, a group of seven relatively bright stars commonly known as the ""Big Dipper"", ""the Wagon"" or ""the Plough"" (among others), both mimicks the shape of the lesser bear (the ""Little Dipper"") and is commonly used as a navigational pointer towards the current northern pole star, Polaris in Ursa Minor. The Big Dipper and the constellation as a whole have mythological significance in numerous world cultures, usually as a symbol of the north.The third largest constellation in the sky, Ursa Major is home to many deep-sky objects including seven Messier objects, four other NGC objects and I Zwicky 18, the youngest known galaxy in the visible universe.