Book Describing Techniques to Detect Transiting ExoPlanets
... Not only are amateurs capable of helping in the discovery of exoplanets through collaborations with professionals, but amateurs are well-positioned to contribute to the discovery of Earth-like exoplanets and their moons! This is explained in Chapter 22. How can this be? After all, the professionals ...
... Not only are amateurs capable of helping in the discovery of exoplanets through collaborations with professionals, but amateurs are well-positioned to contribute to the discovery of Earth-like exoplanets and their moons! This is explained in Chapter 22. How can this be? After all, the professionals ...
Exploring the Most Bizarre Ideas in Cosmology Astronomers
... appears to be filled with vast amounts of energy, particles which are also waves, "empty" space which can nevertheless stretch as if it is some kind of expandable fabric and so forth. Most scientists understand these things as being relatively established and non-controversial. But then there are mo ...
... appears to be filled with vast amounts of energy, particles which are also waves, "empty" space which can nevertheless stretch as if it is some kind of expandable fabric and so forth. Most scientists understand these things as being relatively established and non-controversial. But then there are mo ...
Gaia 1 and 2. A pair of new satellites of the Galaxy
... for the faint sub-structures in the stellar halo. Ultra-faint satellites and stellar streams appear as low-level enhancements of the stellar density field and as such can either be destroyed or mimicked by the survey systematics. For example, for a given exposure on a given telescope, a combination ...
... for the faint sub-structures in the stellar halo. Ultra-faint satellites and stellar streams appear as low-level enhancements of the stellar density field and as such can either be destroyed or mimicked by the survey systematics. For example, for a given exposure on a given telescope, a combination ...
Chandra Characterization of X-ray Emission in the Young F
... spectra for the “West” and “East” sources, each over an r=1.6 pixel circular aperture (Fig 3a). After allowing for 30 counts from the brighter Western source in the fainter Eastern source's aperture, this provided a reasonable separation of the two source photon populations, with 1200 counts for the ...
... spectra for the “West” and “East” sources, each over an r=1.6 pixel circular aperture (Fig 3a). After allowing for 30 counts from the brighter Western source in the fainter Eastern source's aperture, this provided a reasonable separation of the two source photon populations, with 1200 counts for the ...
a wide-field survey for variable stars
... Tauri variable stars. The nearby dusty, yellow cloud is Hind’s Variable Nebula (NGC 1555/1554). Over 400 light-years away, at the edge of a molecular cloud, both star and nebula are seen to vary significantly in brightness but not necessarily at the same time, adding to the mystery of the intriguing ...
... Tauri variable stars. The nearby dusty, yellow cloud is Hind’s Variable Nebula (NGC 1555/1554). Over 400 light-years away, at the edge of a molecular cloud, both star and nebula are seen to vary significantly in brightness but not necessarily at the same time, adding to the mystery of the intriguing ...
Luminosity profiles and sizes of massive star clusters in NGC 7252
... provide coverage in the blue and red part of the optical, and to be wide in order to maximize the throughput and signal-to-noise ratio (S/N) of the brightness profiles. The total exposure time through each filter was 2120 s, split into four 500 s exposures plus two short 60 s exposures to avoid satu ...
... provide coverage in the blue and red part of the optical, and to be wide in order to maximize the throughput and signal-to-noise ratio (S/N) of the brightness profiles. The total exposure time through each filter was 2120 s, split into four 500 s exposures plus two short 60 s exposures to avoid satu ...
Chapter 19
... • To View the presentation as a slideshow with effects select “View” on the menu bar and click on “Slide Show.” • To advance through the presentation, click the right-arrow key or the space bar. • From the resources slide, click on any resource to see a presentation for that resource. • From the Cha ...
... • To View the presentation as a slideshow with effects select “View” on the menu bar and click on “Slide Show.” • To advance through the presentation, click the right-arrow key or the space bar. • From the resources slide, click on any resource to see a presentation for that resource. • From the Cha ...
Stars & Galaxies - newmanlib.ibri.org
... • Globular clusters are so named because they tend to have a rather spherical shape. • They are much larger and more tightly packed than galactic clusters,typically having tens of thousands of stars. • They move in a halo around the galaxy rather than in the galactic plane. ...
... • Globular clusters are so named because they tend to have a rather spherical shape. • They are much larger and more tightly packed than galactic clusters,typically having tens of thousands of stars. • They move in a halo around the galaxy rather than in the galactic plane. ...
High-mass star-forming cloud G0.38+0.04 in the Galactic center dust
... excess of H2 CO and SiO masers. If the H2 O masers come primarily from outflows, it may be that the greater turbulence in the CMZ prevents an adequate path length from being assembled in CMZ gas. Another possibility is that existing H2 O maser observations are not sensitive enough, and a population ...
... excess of H2 CO and SiO masers. If the H2 O masers come primarily from outflows, it may be that the greater turbulence in the CMZ prevents an adequate path length from being assembled in CMZ gas. Another possibility is that existing H2 O maser observations are not sensitive enough, and a population ...
Chandra News March 2005 Published by the Chandra X-ray Center (CXC)
... a scan of the Galactic plane with a rocket-borne detector. In 1979, the first Einstein observation of this region showed that this source was the Carina Nebula, over 1 degree in extent - a bright (by present standards) diffuse source sprinkled with dozens of point-like O stars. Although η Carinae it ...
... a scan of the Galactic plane with a rocket-borne detector. In 1979, the first Einstein observation of this region showed that this source was the Carina Nebula, over 1 degree in extent - a bright (by present standards) diffuse source sprinkled with dozens of point-like O stars. Although η Carinae it ...
THE MONTHLY SKY GUIDE, SIXTH EDITION
... Most bright stars, and several not-so-bright ones, have strangesounding names. Other stars are known merely by letters and numbers. These designations arose in various ways, as follows. A number of star names date back to Greek and Roman times. For example, the name of the brightest star in the sky, ...
... Most bright stars, and several not-so-bright ones, have strangesounding names. Other stars are known merely by letters and numbers. These designations arose in various ways, as follows. A number of star names date back to Greek and Roman times. For example, the name of the brightest star in the sky, ...
AstroImageJ: Image Processing and Photometric Extraction for Ultra
... rotation to preferences. This option is useful for cases where at least one image in a time-series has been plate-solved, but others have not. The blue aperture shown near the center of Figure 2 moves with the mouse pointer. As the mouse pointer is moved around in the image, the value of the pixel a ...
... rotation to preferences. This option is useful for cases where at least one image in a time-series has been plate-solved, but others have not. The blue aperture shown near the center of Figure 2 moves with the mouse pointer. As the mouse pointer is moved around in the image, the value of the pixel a ...
Horace Welcome Babcock - National Academy of Sciences
... distance from the center of the system). He analyzed the velocities, advised by Lick astronomer R. J. Trumpler, and found that they did not match the rotation curve calculated for the constant mass-to-light ratio, then the usual assumption made for starlight. Upon converting his radial velocities to ...
... distance from the center of the system). He analyzed the velocities, advised by Lick astronomer R. J. Trumpler, and found that they did not match the rotation curve calculated for the constant mass-to-light ratio, then the usual assumption made for starlight. Upon converting his radial velocities to ...
The KStars Handbook - KDE Documentation
... From an object’s popup menu, you can open its Detailed Information Window, where you can examine positional data about the object, and query a huge treasury of online databases for professional-grade astronomical data and literature references about the object. You can even attach your own Internet ...
... From an object’s popup menu, you can open its Detailed Information Window, where you can examine positional data about the object, and query a huge treasury of online databases for professional-grade astronomical data and literature references about the object. You can even attach your own Internet ...
Galaxies Astronomy 1 — Elementary Astronomy LA Mission College Spring F2015
... A. never had blue stars in the galaxy. B. had blue stars that are not present anymore but were at one time long ago. C. has been around long enough for blue stars to all evolve into the red main sequence stars we see. D. never contained enough gas to have blue stars develop. E. as blue stars that ar ...
... A. never had blue stars in the galaxy. B. had blue stars that are not present anymore but were at one time long ago. C. has been around long enough for blue stars to all evolve into the red main sequence stars we see. D. never contained enough gas to have blue stars develop. E. as blue stars that ar ...
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.