A spectroscopic study of detached binary systems using precise radial velocities
... A complete understanding of a binary system’s orbital characteristics, as well as the measurement of the all-important stellar masses, is almost always only achieved after the binary system has been studied using two or more complementary observing techniques. Two of the suitable techniques are astr ...
... A complete understanding of a binary system’s orbital characteristics, as well as the measurement of the all-important stellar masses, is almost always only achieved after the binary system has been studied using two or more complementary observing techniques. Two of the suitable techniques are astr ...
Abstract The Star Formation History of Low Surface Brightness Galaxies
... The star formation histories of low surface brightness galaxies are interesting but poorly constrained. These objects tend to be rather blue, contradicting the initial impression that they may simply be faded remnants of higher surface brightness galaxies whose star formation has finished. Other sce ...
... The star formation histories of low surface brightness galaxies are interesting but poorly constrained. These objects tend to be rather blue, contradicting the initial impression that they may simply be faded remnants of higher surface brightness galaxies whose star formation has finished. Other sce ...
Star Formation in the Milky Way and Nearby Galaxies Further
... The past decade has witnessed an unprecedented stream of new observational information on star formation on all scales, thanks in no small part to new facilities such as the Galaxy Evolution Explorer (GALEX), the Spitzer Space Telescope, and the Herschel Space Observatory; the introduction of powerf ...
... The past decade has witnessed an unprecedented stream of new observational information on star formation on all scales, thanks in no small part to new facilities such as the Galaxy Evolution Explorer (GALEX), the Spitzer Space Telescope, and the Herschel Space Observatory; the introduction of powerf ...
An X-Ray, Optical and Infra-red study of High-Mass X
... First and foremost I would like to thank my supervisor, Malcolm Coe, for his continued guidance and support. His drive to obtain and exploit all manner of data has given me a wealth of information on which to base my thesis and sent me to some of the world’s most incredible places in the process. I ...
... First and foremost I would like to thank my supervisor, Malcolm Coe, for his continued guidance and support. His drive to obtain and exploit all manner of data has given me a wealth of information on which to base my thesis and sent me to some of the world’s most incredible places in the process. I ...
Radio Emission Toward Regions of Massive Star Formation
... convention, stars with enough mass to end their lives as core-collapse supernovae (M∗ ≥ 8.0 M ) are considered ‘high-mass’ stars. High-mass stars have difficulty forming in this fashion, because the onset of fusion occurs before they reach their final main-sequence mass. This works against monolith ...
... convention, stars with enough mass to end their lives as core-collapse supernovae (M∗ ≥ 8.0 M ) are considered ‘high-mass’ stars. High-mass stars have difficulty forming in this fashion, because the onset of fusion occurs before they reach their final main-sequence mass. This works against monolith ...
Introduction_to_pulsar_astronomy
... In the 1940’s, it was found that the supernova event that resulted in the Crab Nebula was witnessed by Chinese astronomers in the year 1054. Radio emission from the Crab nebula was first detected by Bolton, Stanley and Slee (1949). It is one of the most powerful radio sources known, with a flux of 1 ...
... In the 1940’s, it was found that the supernova event that resulted in the Crab Nebula was witnessed by Chinese astronomers in the year 1054. Radio emission from the Crab nebula was first detected by Bolton, Stanley and Slee (1949). It is one of the most powerful radio sources known, with a flux of 1 ...
- National Optical Astronomy Observatory
... limit of the telescope at 5 microns is ~0.8 arcseconds. Spatially sampling at ~0.4 arcseconds would then be about right under good seeing.) ! Input scan parameters (number of steps, number of spectral frames, integration time, etc.) ! Start the scan sequence and simultaneously begin stepping the tra ...
... limit of the telescope at 5 microns is ~0.8 arcseconds. Spatially sampling at ~0.4 arcseconds would then be about right under good seeing.) ! Input scan parameters (number of steps, number of spectral frames, integration time, etc.) ! Start the scan sequence and simultaneously begin stepping the tra ...
