Science Olympiad Astronomy C Division Event Golden Gate
... movement may have caused this? 9. What DSO is in image 5? a. This system’s mass may exceed what mass limit for white dwarfs? b. The objects of this system will create what specific event? c. If one component of the system was more massive than the other, then the DSO may be what type of system? 10. ...
... movement may have caused this? 9. What DSO is in image 5? a. This system’s mass may exceed what mass limit for white dwarfs? b. The objects of this system will create what specific event? c. If one component of the system was more massive than the other, then the DSO may be what type of system? 10. ...
The Formation and Evolution of Massive Black Holes - Ira-Inaf
... MBHs become visible when they accrete gas directly from their surroundings, or, occasionally, when they disrupt an unlucky star passing too close by (20). The gravitational potential energy of the accreted mass is converted to radiation, making the black hole luminous. Luminous, accreting MBHs are g ...
... MBHs become visible when they accrete gas directly from their surroundings, or, occasionally, when they disrupt an unlucky star passing too close by (20). The gravitational potential energy of the accreted mass is converted to radiation, making the black hole luminous. Luminous, accreting MBHs are g ...
Blowin` in the wind: both `negative` and `positive` feedback in an
... 320 km/s) is consistent with the systemic redshift of the host galaxy (Brusa et al. 2010), and it is interpreted as due to the star formation in the host galaxy. We map the spatial extent of the Hα narrow component by fitting in each spaxels of the datacube the single Gaussian derived from the integr ...
... 320 km/s) is consistent with the systemic redshift of the host galaxy (Brusa et al. 2010), and it is interpreted as due to the star formation in the host galaxy. We map the spatial extent of the Hα narrow component by fitting in each spaxels of the datacube the single Gaussian derived from the integr ...
Drizzle: A Method for the Linear Reconstruction of Undersampled
... the blue. In contrast, a well-sampled detector would have ∼ > 2.5 pixels across the FWHM. Other HST cameras such as NICMOS, STIS and the future Advanced Camera for Surveys (ACS) also suffer from undersampling to varying degrees. The effect of undersampling on WF images is illustrated by the “Great E ...
... the blue. In contrast, a well-sampled detector would have ∼ > 2.5 pixels across the FWHM. Other HST cameras such as NICMOS, STIS and the future Advanced Camera for Surveys (ACS) also suffer from undersampling to varying degrees. The effect of undersampling on WF images is illustrated by the “Great E ...
Chapter 5 The Evolutionary Paths Of Nearby Galaxies
... hydrogen content. Unlike the AGN-hosts, which occupy the transition region only for masses M∗ & 1010 M⊙ , the Hi deficient galaxies tend to lie at the red edge of the blue sequence and in the transition region, independent of the stellar mass. More importantly, at fixed stellar mass, Hi deficient sy ...
... hydrogen content. Unlike the AGN-hosts, which occupy the transition region only for masses M∗ & 1010 M⊙ , the Hi deficient galaxies tend to lie at the red edge of the blue sequence and in the transition region, independent of the stellar mass. More importantly, at fixed stellar mass, Hi deficient sy ...
Comet Observers Club Chair
... As of 1995, 878 comets have been cataloged and their orbits at least roughly calculated. Of these, 184 are periodic comets (orbital periods less than 200 years); some of the remainder are no doubt periodic as well, but their orbits have not been determined with sufficient accuracy to tell for sure. ...
... As of 1995, 878 comets have been cataloged and their orbits at least roughly calculated. Of these, 184 are periodic comets (orbital periods less than 200 years); some of the remainder are no doubt periodic as well, but their orbits have not been determined with sufficient accuracy to tell for sure. ...
WORD - Astrophysics
... relevant to the sort of abundances modelled in the big codes. However, lines of sight through these regions are currently completely inaccessible. In our galaxy, optical studies of highly reddened stars in or behind dense clouds is certainly important, to determine properties which are currently est ...
... relevant to the sort of abundances modelled in the big codes. However, lines of sight through these regions are currently completely inaccessible. In our galaxy, optical studies of highly reddened stars in or behind dense clouds is certainly important, to determine properties which are currently est ...
astro-ph/0303282 PDF
... partially removed through combination of multiple images) our images are relatively uniform – sensitivity does not vary as a function of azimuth – though sensitivity is significantly lower in the northern offset field of Epsilon Eridani due to poor conditions. The Vega sensitivity limits come from t ...
... partially removed through combination of multiple images) our images are relatively uniform – sensitivity does not vary as a function of azimuth – though sensitivity is significantly lower in the northern offset field of Epsilon Eridani due to poor conditions. The Vega sensitivity limits come from t ...
On the nature of early-type emission line objects in NGC6611
... Intrinsic instellar reddening (E(B-V)) was measured for each star by means of the instellar lines detected at 443.0 and 661.3 nm, and was used to correct the UBVI, JHK (taken from the 2MASS survey), 3.6µm, 4.5µm, 5.7µm and 8µm (SPITZER) magnitudes. Each SED is normalized to the SED of a non ELS clas ...
... Intrinsic instellar reddening (E(B-V)) was measured for each star by means of the instellar lines detected at 443.0 and 661.3 nm, and was used to correct the UBVI, JHK (taken from the 2MASS survey), 3.6µm, 4.5µm, 5.7µm and 8µm (SPITZER) magnitudes. Each SED is normalized to the SED of a non ELS clas ...
MilkyWay
... Being searched for in particle accelerators and large detector experiments. MACHOs - Massive Compact Halo Objects White Dwarf Stars, Red Dwarfs (0.2 Msun), Brown Dwarfs (<0.08 Msun), Neutron Stars, Black Holes. Recall that the more massive remnants result from relatively rare high, mass stellar prog ...
... Being searched for in particle accelerators and large detector experiments. MACHOs - Massive Compact Halo Objects White Dwarf Stars, Red Dwarfs (0.2 Msun), Brown Dwarfs (<0.08 Msun), Neutron Stars, Black Holes. Recall that the more massive remnants result from relatively rare high, mass stellar prog ...
A6 - Vicphysics
... their purpose, optical system (reflecting, refracting), mount (altazimuth, equatorial) and data collection system (optical, electronic); ...
... their purpose, optical system (reflecting, refracting), mount (altazimuth, equatorial) and data collection system (optical, electronic); ...
The Milky Way Galaxy
... Being searched for in particle accelerators and large detector experiments. MACHOs - Massive Compact Halo Objects White Dwarf Stars, Red Dwarfs (0.2 Msun), Brown Dwarfs (<0.08 Msun), Neutron Stars, Black Holes. Recall that the more massive remnants result from relatively rare high, mass stellar prog ...
... Being searched for in particle accelerators and large detector experiments. MACHOs - Massive Compact Halo Objects White Dwarf Stars, Red Dwarfs (0.2 Msun), Brown Dwarfs (<0.08 Msun), Neutron Stars, Black Holes. Recall that the more massive remnants result from relatively rare high, mass stellar prog ...
September 2011 - Newbury Astronomical Society
... reduction) are of a reasonable quality. Binoculars with an aperture of less than 50mm are not best suited for astronomy as they cannot capture enough light. Most binoculars have the following features that are designed into the instrument to allow it to be adjusted to suit the user and the purpose o ...
... reduction) are of a reasonable quality. Binoculars with an aperture of less than 50mm are not best suited for astronomy as they cannot capture enough light. Most binoculars have the following features that are designed into the instrument to allow it to be adjusted to suit the user and the purpose o ...
Calculating the Age of a Planetary Nebula
... If you get the error message Use x1 zoom, simply click on the x1 button alongside the zoom buttons described above to bring the image back to the original size. The cursor will change shape and an Output window will pop up on the screen. Click at one edge of the main shell and the x,y-coordinates wi ...
... If you get the error message Use x1 zoom, simply click on the x1 button alongside the zoom buttons described above to bring the image back to the original size. The cursor will change shape and an Output window will pop up on the screen. Click at one edge of the main shell and the x,y-coordinates wi ...
Right Ascension
... telescopes on Hawaii, with 10m mirrors. At about 10 times the diameter of the largest refractor, they have 100 times the lightgathering capability. ...
... telescopes on Hawaii, with 10m mirrors. At about 10 times the diameter of the largest refractor, they have 100 times the lightgathering capability. ...
3. Chapter 12
... was reached by astronomers who made observations using the best instruments available to them at the time. Scientific theories develop and change as we learn more. New evidence can cause scientists to rethink existing theories. Between 1918 and 1929, the development of much more powerful telescopes ...
... was reached by astronomers who made observations using the best instruments available to them at the time. Scientific theories develop and change as we learn more. New evidence can cause scientists to rethink existing theories. Between 1918 and 1929, the development of much more powerful telescopes ...
www.aavso.org
... Even today, many amateur astronomers still measure magnitudes using their eyes and submit data to an organization such as the AAVSO (American Association of Variable Star Observers) which can be used by professional astronomers for research. ...
... Even today, many amateur astronomers still measure magnitudes using their eyes and submit data to an organization such as the AAVSO (American Association of Variable Star Observers) which can be used by professional astronomers for research. ...
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.