The science case for - Astrophysics
... photons which re-ionised the Universe some 200million years after the Big Bang, and made it transparent? These objects may be visible through their supernovae, or their ionisation zones. How many types of matter exist? What is dark matter? Where is it? Most matter is transparent, and is detectable o ...
... photons which re-ionised the Universe some 200million years after the Big Bang, and made it transparent? These objects may be visible through their supernovae, or their ionisation zones. How many types of matter exist? What is dark matter? Where is it? Most matter is transparent, and is detectable o ...
JCMT HARP CO 3-2 Observations of Molecular Outflows in W5
... presented, totaling an area of ∼ 12000 arcmin2 with sensitivity better than 0.1 K per 0.4 km s−1 channel. We have discovered 55 CO outflow candidates, 40 of which are associated with W5. Most of the outflows are located on the periphery of the W5 HII region, but two clusters of outflows are > 5 pc f ...
... presented, totaling an area of ∼ 12000 arcmin2 with sensitivity better than 0.1 K per 0.4 km s−1 channel. We have discovered 55 CO outflow candidates, 40 of which are associated with W5. Most of the outflows are located on the periphery of the W5 HII region, but two clusters of outflows are > 5 pc f ...
ON THE SOURCE OF THE DUST EXTINCTION IN
... sense as dust reddening, but with an average value of the ratio of total-to-selective extinction, RV , that is significantly less than would be produced by normal interstellar dust in the Milky Way (Tripp 1998). The latter result has variously been interpreted as possible evidence that the extinctio ...
... sense as dust reddening, but with an average value of the ratio of total-to-selective extinction, RV , that is significantly less than would be produced by normal interstellar dust in the Milky Way (Tripp 1998). The latter result has variously been interpreted as possible evidence that the extinctio ...
Clusters as laboratories for the study of galaxy evolution
... collapse…[or] in the disks of less massive late-type galaxies which later merge to form the ellipticals, as long as the merging does not trigger significant star formation. From the lack of evolution in the shape of the bright end of the K-band LF we can however deduce that if the massive elliptical ...
... collapse…[or] in the disks of less massive late-type galaxies which later merge to form the ellipticals, as long as the merging does not trigger significant star formation. From the lack of evolution in the shape of the bright end of the K-band LF we can however deduce that if the massive elliptical ...
FIRST STELLAR ABUNDANCES IN THE DWARF IRREGULAR
... In Fig. 2 the Hα profiles of the three stars are shown. To obtain the stellar line profiles, the contribution of the diffuse Hα emission of Sextans A which was found for all stars was subtracted as part of the ’sky’ subtraction in the extraction process of the spectra. Inspecting the raw 2D spectra, ...
... In Fig. 2 the Hα profiles of the three stars are shown. To obtain the stellar line profiles, the contribution of the diffuse Hα emission of Sextans A which was found for all stars was subtracted as part of the ’sky’ subtraction in the extraction process of the spectra. Inspecting the raw 2D spectra, ...
A tale of two galaxies: light and mass in NGC 891 and NGC 7814
... the major axis. For a description of the method and a discussion of the uncertanties involved see Sancisi & Allen (1979). The rotational velocity was derived by fitting Gaussian functions with fixed dispersions to the high rotational velocity sides of the line profiles (i.e. the lowest radial veloci ...
... the major axis. For a description of the method and a discussion of the uncertanties involved see Sancisi & Allen (1979). The rotational velocity was derived by fitting Gaussian functions with fixed dispersions to the high rotational velocity sides of the line profiles (i.e. the lowest radial veloci ...
Barium and europium abundances in cool dwarf stars and
... iron group. Abundances of these elements in the solar system have contributions in differing proportions from two main processes, the s- and r-process of neutron capture. As supported by many observational and theoretical results (Travaglio et al. 1999, and references therein) s-nuclei are mainly sy ...
... iron group. Abundances of these elements in the solar system have contributions in differing proportions from two main processes, the s- and r-process of neutron capture. As supported by many observational and theoretical results (Travaglio et al. 1999, and references therein) s-nuclei are mainly sy ...
ASTRONOMY AND ASTROPHYSICS Barium and europium
... iron group. Abundances of these elements in the solar system have contributions in differing proportions from two main processes, the s- and r-process of neutron capture. As supported by many observational and theoretical results (Travaglio et al. 1999, and references therein) s-nuclei are mainly sy ...
... iron group. Abundances of these elements in the solar system have contributions in differing proportions from two main processes, the s- and r-process of neutron capture. As supported by many observational and theoretical results (Travaglio et al. 1999, and references therein) s-nuclei are mainly sy ...
Star Formation and Dynamics in the Galactic Centre
... (e.g. Sunyaev et al. 1993), especially the 6.4 keV Fe Kα line. This line is emitted by various molecular clouds in the GC (e.g. Ponti et al. 2010). The lines emitted from different clouds might be triggered by different sources (e.g. different X-ray binaries), but this possibility is not supported b ...
... (e.g. Sunyaev et al. 1993), especially the 6.4 keV Fe Kα line. This line is emitted by various molecular clouds in the GC (e.g. Ponti et al. 2010). The lines emitted from different clouds might be triggered by different sources (e.g. different X-ray binaries), but this possibility is not supported b ...
Luminosity and Mass Functions of Galaxies
... Need stellar mass-to-light ratios to convert luminosity function to mass function. (Total mass can be found dynamically.) Bell et al. (2003) develop conversion from luminosity and color to M/L. Create a grid of stellar populations with range of metalicities and star-formation histories. Compute colo ...
... Need stellar mass-to-light ratios to convert luminosity function to mass function. (Total mass can be found dynamically.) Bell et al. (2003) develop conversion from luminosity and color to M/L. Create a grid of stellar populations with range of metalicities and star-formation histories. Compute colo ...
Evolution in circumstellar envelopes of Be stars: From disks to rings?
... pedestal with the same total width as the other two lines. Like the Hα emission, this oxygen emission line is pumped by Lyβ emission, but it is optically thin. It should, therefore, trace large parts of the disk without its profile being contaminated by self-absorption or scattering. FV CMa (= HD 54 ...
... pedestal with the same total width as the other two lines. Like the Hα emission, this oxygen emission line is pumped by Lyβ emission, but it is optically thin. It should, therefore, trace large parts of the disk without its profile being contaminated by self-absorption or scattering. FV CMa (= HD 54 ...
The cosmic origin of fluorine and sulphur
... In this thesis I determine abundances of two of the least studied elements, fluorine and sulphur, in three different stellar populations in the Milky Way using infrared spectroscopy of giants. Regarding fluorine the chemical evolution is very unclear because the number of previous observations are smal ...
... In this thesis I determine abundances of two of the least studied elements, fluorine and sulphur, in three different stellar populations in the Milky Way using infrared spectroscopy of giants. Regarding fluorine the chemical evolution is very unclear because the number of previous observations are smal ...
Conference Abstract Booklet here.
... light curves of Cepheid variables using the Fourier decomposition and principal component analysis methods. The theoretical Cepheid light curves are obtained using the full amplitude, nonlinear, convective hydrodynamical models for chemical compositions relative to Cepheids in the Galaxy (Y=0.28, Z= ...
... light curves of Cepheid variables using the Fourier decomposition and principal component analysis methods. The theoretical Cepheid light curves are obtained using the full amplitude, nonlinear, convective hydrodynamical models for chemical compositions relative to Cepheids in the Galaxy (Y=0.28, Z= ...
POSTERS SESSION I: Atmospheres of Massive Stars
... wind, probably triggered by a companion star’s periastron approach. This indicates a surface instability that was not predicted and is stronger than one would normally have expected based on tidal and radiative effects. The hypothetical companion object continuously alters the primary star’s surface ...
... wind, probably triggered by a companion star’s periastron approach. This indicates a surface instability that was not predicted and is stronger than one would normally have expected based on tidal and radiative effects. The hypothetical companion object continuously alters the primary star’s surface ...
Catalogs of Hot White Dwarfs in the Milky Way from GALEX`s
... phases, in which they shed much of their mass. The ejected material enriches the interstellar medium (ISM) with newly synthesized nuclear products (mainly He, C, N, and possibly O), to different extents, depending on the initial stellar mass and exact evolutionary path (e.g. Marigo 2001, Karakas 201 ...
... phases, in which they shed much of their mass. The ejected material enriches the interstellar medium (ISM) with newly synthesized nuclear products (mainly He, C, N, and possibly O), to different extents, depending on the initial stellar mass and exact evolutionary path (e.g. Marigo 2001, Karakas 201 ...
Hunting for Substructure in the Milky Way
... between these two structures; when dynamical and chemical properties of stars in both are analysed there is much overlap. Therefore, some astronomers believe that no such distinction between the thick disk and the thin disk can be made. See Bovy et al. (2012) and Reddy et al. (2006) for two opposing ...
... between these two structures; when dynamical and chemical properties of stars in both are analysed there is much overlap. Therefore, some astronomers believe that no such distinction between the thick disk and the thin disk can be made. See Bovy et al. (2012) and Reddy et al. (2006) for two opposing ...
... This shows some of the general processes that might have operated when the Sun and planets were forming. The yellow region near the Sun is very hot, which vaporizes all the dust falling into the nebula. The young Sun emits vast quantities of energetic particles, which create winds in the nebula. Ris ...
Physical Properties of the Gas and Dust in the Orion B Molecular
... Table 1 summarizes our current knowledge about the global properties of GMCs in the solar neighborhood and their observed substructures. Note that especially the definition of a clump is highly uncertain and that such clumps are observed over a wide range of sizes and masses. With the exception of s ...
... Table 1 summarizes our current knowledge about the global properties of GMCs in the solar neighborhood and their observed substructures. Note that especially the definition of a clump is highly uncertain and that such clumps are observed over a wide range of sizes and masses. With the exception of s ...
2. The X-ray-Radio correlation for bulgeless galaxies
... Correlations between the X-ray and Radio emissions are observed for both galaxies with Active Galactic Nuclei (AGN) and in Star Forming galaxies. For the first case, the Xray/Radio correlation seems to present different slopes for Radio-loud and Radio-quiet AGN and may be used to estimate the mass o ...
... Correlations between the X-ray and Radio emissions are observed for both galaxies with Active Galactic Nuclei (AGN) and in Star Forming galaxies. For the first case, the Xray/Radio correlation seems to present different slopes for Radio-loud and Radio-quiet AGN and may be used to estimate the mass o ...
THE ORION NEBULA AND ITS ASSOCIATED POPULATION C. R. O
... to have produced three regions of massive star formation, the most luminous of which has produced M 42, but also nearby are imbedded groupings to the NW and SW of the tight clustering of early type stars known as the Trapezium. The historical interest in this region continues through the present, wi ...
... to have produced three regions of massive star formation, the most luminous of which has produced M 42, but also nearby are imbedded groupings to the NW and SW of the tight clustering of early type stars known as the Trapezium. The historical interest in this region continues through the present, wi ...
Evolution of Circumstellar Disks Around Normal Stars
... no strong correlation of cold dust mass with stellar age has been found. Bryden et al. (2006; see also Beichman et al., 2005) have completed a volume–limited survey of nearby sun–like stars with probable ages between 1–3 Gyr old. Overall the Spitzer statistics suggest a cold debris disk frequency of ...
... no strong correlation of cold dust mass with stellar age has been found. Bryden et al. (2006; see also Beichman et al., 2005) have completed a volume–limited survey of nearby sun–like stars with probable ages between 1–3 Gyr old. Overall the Spitzer statistics suggest a cold debris disk frequency of ...
Injection mechanisms of short-lived radionuclides and their
... (Bizzarro et al., 2007; Quitté and Markowski, 2007), however, did not find the expected excess 60Ni in SAH99555, a basaltic angrite with a well-constrained Pb–Pb age of 4564.55 ± 0.16 Myr (Connelly et al., 2008b) and evidence for live 26Al at the time of its crystallization (Baker et al., 2005). The ...
... (Bizzarro et al., 2007; Quitté and Markowski, 2007), however, did not find the expected excess 60Ni in SAH99555, a basaltic angrite with a well-constrained Pb–Pb age of 4564.55 ± 0.16 Myr (Connelly et al., 2008b) and evidence for live 26Al at the time of its crystallization (Baker et al., 2005). The ...
Cataclysmic Cosmic Events and How to Observe Them www.springer.com/series/5338
... astronomers could only dream of such instantaneous communication and processing ability. This new-found power in the hands of backyard observers has enabled them to reach outside the Solar System, and outside our own galaxy, and permitted them to monitor colossal outbursts and explosions taking plac ...
... astronomers could only dream of such instantaneous communication and processing ability. This new-found power in the hands of backyard observers has enabled them to reach outside the Solar System, and outside our own galaxy, and permitted them to monitor colossal outbursts and explosions taking plac ...
Spectroscopic Variability of Supergiant Star HD14134, B3Ia
... (∼ 18 km s−1 and ∼ 13 km s−1 correspondingly) during the same time have been observed (Fig.4). These variabilities can be explained by the pulsation. For a more precise determination of pulsation period of star the systematic observations of this star is necessary. 3.2 Kinematic slice of the stellar ...
... (∼ 18 km s−1 and ∼ 13 km s−1 correspondingly) during the same time have been observed (Fig.4). These variabilities can be explained by the pulsation. For a more precise determination of pulsation period of star the systematic observations of this star is necessary. 3.2 Kinematic slice of the stellar ...
Spectroscopic Variability of Supergiant Star HD14134, B3Ia
... (∼ 18 km s−1 and ∼ 13 km s−1 correspondingly) during the same time have been observed (Fig.4). These variabilities can be explained by the pulsation. For a more precise determination of pulsation period of star the systematic observations of this star is necessary. 3.2 Kinematic slice of the stellar ...
... (∼ 18 km s−1 and ∼ 13 km s−1 correspondingly) during the same time have been observed (Fig.4). These variabilities can be explained by the pulsation. For a more precise determination of pulsation period of star the systematic observations of this star is necessary. 3.2 Kinematic slice of the stellar ...