ASTRO2010 SCIENCE WHITE PAPER
... sensitivity is achieved when the resolution element matches the line width, but in the (background-limited) mid-IR region, higher-resolution observations can be binned to maximize the sensitivity. Secondly, because most lines are well resolved at these high resolutions (Fig. 2), the line profile can ...
... sensitivity is achieved when the resolution element matches the line width, but in the (background-limited) mid-IR region, higher-resolution observations can be binned to maximize the sensitivity. Secondly, because most lines are well resolved at these high resolutions (Fig. 2), the line profile can ...
Chapter 1 Seeing the Light: The Art and Science of Astronomy
... and Saturn. These celestial bodies aren’t wandering through the stars; they orbit around the Sun, our solar system’s central star. Today astronomers know that planets can be smaller or bigger than Earth, but they all are much smaller than the Sun. The planets in our solar system are so close to Eart ...
... and Saturn. These celestial bodies aren’t wandering through the stars; they orbit around the Sun, our solar system’s central star. Today astronomers know that planets can be smaller or bigger than Earth, but they all are much smaller than the Sun. The planets in our solar system are so close to Eart ...
Article PDF - IOPscience
... objects (CSOs) taken with the Infrared Spectrograph on the Spitzer Space Telescope. The hosts of these young, powerful radio galaxies show significant diversity in their mid-IR spectra. This includes multiple atomic fine-structure lines, H2 gas, polycyclic aromatic hydrocarbon (PAH) emission, warm d ...
... objects (CSOs) taken with the Infrared Spectrograph on the Spitzer Space Telescope. The hosts of these young, powerful radio galaxies show significant diversity in their mid-IR spectra. This includes multiple atomic fine-structure lines, H2 gas, polycyclic aromatic hydrocarbon (PAH) emission, warm d ...
harrold_kajubi_astro1
... Better photometry is needed to: Verify distance modulus from main sequence shift Verify cluster age from turn-off point ...
... Better photometry is needed to: Verify distance modulus from main sequence shift Verify cluster age from turn-off point ...
Planetary Nebula
... A dying star that was once about five times the mass of the Sun is at the center of this fury. It has ejected its envelope of gases and is now unleashing a stream of ultraviolet radiation that is making the cast-off material glow. This object is an example of a planetary nebula, so-named because man ...
... A dying star that was once about five times the mass of the Sun is at the center of this fury. It has ejected its envelope of gases and is now unleashing a stream of ultraviolet radiation that is making the cast-off material glow. This object is an example of a planetary nebula, so-named because man ...
Signal-to-Noise in Optical Astronomy 1 CCDs
... counts due to the readout noise. At the wavelengths where there are sky emission lines, the fractional noise goes up significantly. In the final extracted spectrum (much more about this later), you will have combined several rows containing object counts and often the S/N is calculated after averagi ...
... counts due to the readout noise. At the wavelengths where there are sky emission lines, the fractional noise goes up significantly. In the final extracted spectrum (much more about this later), you will have combined several rows containing object counts and often the S/N is calculated after averagi ...
www.astro.org.uk www.facebook.com/Stra ordAstro www.twi er.com
... of data on May 23, 1958 when its ba4eries died, but remained in orbit for more than 12 years. It made a fiery re-entry over the Pacific Ocean on March 31, 1970. ...
... of data on May 23, 1958 when its ba4eries died, but remained in orbit for more than 12 years. It made a fiery re-entry over the Pacific Ocean on March 31, 1970. ...
Preface
... Nagdimunov et al.; Edith Hadamcik et al.). It is, however, worth pointing out that the categorization is not unique and should be used with caution, since some of the studies are essentially interdisciplinary. To help the reader become aware of the new findings of the papers included in this issue, ...
... Nagdimunov et al.; Edith Hadamcik et al.). It is, however, worth pointing out that the categorization is not unique and should be used with caution, since some of the studies are essentially interdisciplinary. To help the reader become aware of the new findings of the papers included in this issue, ...
Neutron Stars and Black Holes
... Galactic Distances Quiz Cepheid variable stars are located in two different galaxies, A and B. Both stars have the same average apparent brightness. The star in galaxy A has a bright-dim-bright period of 10 days, while the one in galaxy B has a bright-dim-bright period of 30 days. Which of the two ...
... Galactic Distances Quiz Cepheid variable stars are located in two different galaxies, A and B. Both stars have the same average apparent brightness. The star in galaxy A has a bright-dim-bright period of 10 days, while the one in galaxy B has a bright-dim-bright period of 30 days. Which of the two ...
What is a standard candle?
... Galactic Distances Quiz Cepheid variable stars are located in two different galaxies, A and B. Both stars have the same average apparent brightness. The star in galaxy A has a bright-dim-bright period of 10 days, while the one in galaxy B has a bright-dim-bright period of 30 days. Which of the two ...
... Galactic Distances Quiz Cepheid variable stars are located in two different galaxies, A and B. Both stars have the same average apparent brightness. The star in galaxy A has a bright-dim-bright period of 10 days, while the one in galaxy B has a bright-dim-bright period of 30 days. Which of the two ...
MAGNITUDE AND COLOR SYSTEMS
... Calibration is more difficult the broader is the band. This is because of changes in the source SED and the weighting function within the band. Cf. equation (2) of Lecture 12. o For Vega, or any other A0 V type star, mi = mj = V for all i, j o The zero point of the system is defined by the SED of an ...
... Calibration is more difficult the broader is the band. This is because of changes in the source SED and the weighting function within the band. Cf. equation (2) of Lecture 12. o For Vega, or any other A0 V type star, mi = mj = V for all i, j o The zero point of the system is defined by the SED of an ...
Photometry of star clusters with SalsaJ - Eu-Hou
... Photometry is generally used to generate light curves of objects such as variable stars and supernovae, where the interest is the variation of total light energy output by the system over time. It can also be used to discover exoplanets, by measuring the intensity of a stars light over a period of t ...
... Photometry is generally used to generate light curves of objects such as variable stars and supernovae, where the interest is the variation of total light energy output by the system over time. It can also be used to discover exoplanets, by measuring the intensity of a stars light over a period of t ...
Andromeda Galaxy www.AssignmentPoint.com The Andromeda
... high velocity stars in the disk Type I and the older, red stars in the bulge Type II. This nomenclature was subsequently adopted for stars within the Milky Way, and elsewhere. (The existence of two distinct populations had been noted earlier by Jan Oort.) Baade also discovered that there were two ty ...
... high velocity stars in the disk Type I and the older, red stars in the bulge Type II. This nomenclature was subsequently adopted for stars within the Milky Way, and elsewhere. (The existence of two distinct populations had been noted earlier by Jan Oort.) Baade also discovered that there were two ty ...
AST1100 Lecture Notes
... The magnitude M which is based on flux integrated over all wavelengths is called the bolometric magnitude. The visual magnitude MV on the other hand, is based on the flux over a wavelength region defined by a filter function SV (λ). The filter function is a function which is centered at λ = 550nm wi ...
... The magnitude M which is based on flux integrated over all wavelengths is called the bolometric magnitude. The visual magnitude MV on the other hand, is based on the flux over a wavelength region defined by a filter function SV (λ). The filter function is a function which is centered at λ = 550nm wi ...
energy function behavior in optimization based image sequence
... occupied area. The energy function, which explicitly depends only on illumination values, cannot distinguish between these two types of disturbances. As a result, in our simulation, ...
... occupied area. The energy function, which explicitly depends only on illumination values, cannot distinguish between these two types of disturbances. As a result, in our simulation, ...
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.