Methanol Masers in the NGC6334F Star Forming Region
... flux density ~2.8 Jy at 8.5 GHz). • It is one of the strongest 6.7 GHz methanol maser sources (peak flux density of around 3300 Jy). • It shares many characteristics with the archetypal star forming region W3(OH). • It shows maser emission in a large number of class II methanol maser transitions, ma ...
... flux density ~2.8 Jy at 8.5 GHz). • It is one of the strongest 6.7 GHz methanol maser sources (peak flux density of around 3300 Jy). • It shares many characteristics with the archetypal star forming region W3(OH). • It shows maser emission in a large number of class II methanol maser transitions, ma ...
Star formation in quasar hosts and the origin of radio emission in
... Type 2 quasars are redder in the mid-infrared than type 1 quasars (Liu et al. 2013b). Specifically, the infrared power-law index between rest-frame 5 and 12 μm luminosities β (defined as νLν ∝ λβ ) is −0.05 ± 0.30 (mean and standard deviation) for type 1 quasars from Shi et al. (2007), whereas for t ...
... Type 2 quasars are redder in the mid-infrared than type 1 quasars (Liu et al. 2013b). Specifically, the infrared power-law index between rest-frame 5 and 12 μm luminosities β (defined as νLν ∝ λβ ) is −0.05 ± 0.30 (mean and standard deviation) for type 1 quasars from Shi et al. (2007), whereas for t ...
The most metal-poor galaxies
... A good, well defined, metallicity indicator would be the fraction of baryonic matter that has been converted into heavier elements by means of stellar nucleosynthesis. This material may have been returned to the ISM or may still be locked up in stars. Such a definition would indicate that our main ...
... A good, well defined, metallicity indicator would be the fraction of baryonic matter that has been converted into heavier elements by means of stellar nucleosynthesis. This material may have been returned to the ISM or may still be locked up in stars. Such a definition would indicate that our main ...
galaxy formation and evolution - Yale Astronomy
... we now observe may then just represent the smallest structures that have survived as discrete units (Peebles 1974). The detailed way in which structure develops and galaxies form depends on the nature of the initial density fluctuation spectrum, so it is important to try to constrain the form of thi ...
... we now observe may then just represent the smallest structures that have survived as discrete units (Peebles 1974). The detailed way in which structure develops and galaxies form depends on the nature of the initial density fluctuation spectrum, so it is important to try to constrain the form of thi ...
The HNC/HCN Ratio in Star-Forming Regions The Harvard
... barriers for these reactions had not been calculated theoretically, so Schilke et al. set the barriers to be 200 K, which best reproduced observations of OMC-1. Quantum chemical studies of these barriers have now been carried out and the results are used in many astrochemical networks, such as KIDA ...
... barriers for these reactions had not been calculated theoretically, so Schilke et al. set the barriers to be 200 K, which best reproduced observations of OMC-1. Quantum chemical studies of these barriers have now been carried out and the results are used in many astrochemical networks, such as KIDA ...
Chemical abundances of metal-poor RR Lyrae stars in the Magellanic Clouds
... studies. For et al. (2011) investigated the properties of eleven nearby field RR Lyrae stars and obtained very precise abundances for several elements. For the α-elements, they found a mean overabundance of [α/Fe] = 0.5 dex. This lack of information about α-elements for LMC RR Lyrae stars and the la ...
... studies. For et al. (2011) investigated the properties of eleven nearby field RR Lyrae stars and obtained very precise abundances for several elements. For the α-elements, they found a mean overabundance of [α/Fe] = 0.5 dex. This lack of information about α-elements for LMC RR Lyrae stars and the la ...
Gravitational-wave signal from binary neutron star merger
... different groups in the world. The advancements in this field of research have highly benefited from the realization of public numerical relativity codes, such as the LORENE library [52, 53], The Einstein Toolkit [54], and LIGO’s LAL library, which were used in this thesis, respectively, for generat ...
... different groups in the world. The advancements in this field of research have highly benefited from the realization of public numerical relativity codes, such as the LORENE library [52, 53], The Einstein Toolkit [54], and LIGO’s LAL library, which were used in this thesis, respectively, for generat ...
Talk
... refractive, and the index of refraction depends on RF. • At higher frequencies pulsed emission arrive earlier • Level of dispersion depends on total column density along the line of sight (Dispersion measure DM). ...
... refractive, and the index of refraction depends on RF. • At higher frequencies pulsed emission arrive earlier • Level of dispersion depends on total column density along the line of sight (Dispersion measure DM). ...
What Gaia can reveal about the matter distribution in the Milky Way
... Similar types of work The method outlined above has been used in smaller scale to estimate the local matter and dark matter densities (Holmberg & Flynn, 2000; Garbari et al., 2011). The difference this work has compared to these estimations is that in this case it will be possible to create a map wi ...
... Similar types of work The method outlined above has been used in smaller scale to estimate the local matter and dark matter densities (Holmberg & Flynn, 2000; Garbari et al., 2011). The difference this work has compared to these estimations is that in this case it will be possible to create a map wi ...
Testing the Initial-Final Mass Relationship of White Dwarfs Silvia Catal´ an Ruiz
... total age or metallicity, are available. Most of the works carried out up to now have focused in studying white dwarfs in open clusters (Ferrario et al. 2005, Dobbie et al. 2006), whose ages can be determined from model fits to the turn-off location in a color-magnitude diagram. One of the aims of t ...
... total age or metallicity, are available. Most of the works carried out up to now have focused in studying white dwarfs in open clusters (Ferrario et al. 2005, Dobbie et al. 2006), whose ages can be determined from model fits to the turn-off location in a color-magnitude diagram. One of the aims of t ...
The UV properties of E+ A galaxies: constraints on feedback
... Several plausible explanations for the E+A phenomenon have been proposed and studies indicate that there are multiple channels for creating such post-starburst spectral signatures. Since E+A galaxies were first detected in clusters, it was initially thought that their production required a cluster-s ...
... Several plausible explanations for the E+A phenomenon have been proposed and studies indicate that there are multiple channels for creating such post-starburst spectral signatures. Since E+A galaxies were first detected in clusters, it was initially thought that their production required a cluster-s ...
spatially resolved star formation history of milky way satellites
... galaxies and their own satellites form a self-gravitating association called the Local Group, and hence, the satellite galaxies that reside in it are called local dwarf galaxies. Local dwarf galaxies are crutial for understanding several key aspects of modern astrophysics (Mateo, 1998; Tolstoy et al ...
... galaxies and their own satellites form a self-gravitating association called the Local Group, and hence, the satellite galaxies that reside in it are called local dwarf galaxies. Local dwarf galaxies are crutial for understanding several key aspects of modern astrophysics (Mateo, 1998; Tolstoy et al ...
White dwarfs, black holes and neutron stars in close binaries
... and forms a sphere which in its centre has a temperature and pressure high enough to start hydrogen fusion. The star remains in this phase for most of its active life and only in the last ten percent of its active life its conditions change dramatically. Then the hydrogen fuel in its centre is exhau ...
... and forms a sphere which in its centre has a temperature and pressure high enough to start hydrogen fusion. The star remains in this phase for most of its active life and only in the last ten percent of its active life its conditions change dramatically. Then the hydrogen fuel in its centre is exhau ...
Simulating the outer layers of Procyon A: a comparison with the Sun
... Heavy element diffusion in the envelope is complicated by the fact that both radiative levitation of certain elements and turbulent mixing may also play an important role in inhibiting the gravitational settling (Richer et al. 1998). The Procyon atmosphere typifies the complex transition between the ...
... Heavy element diffusion in the envelope is complicated by the fact that both radiative levitation of certain elements and turbulent mixing may also play an important role in inhibiting the gravitational settling (Richer et al. 1998). The Procyon atmosphere typifies the complex transition between the ...
Galaxy Pairs in the Sloan Digital Sky Survey
... 2009; Brasseur et al. 2008) and pairs, of which this is the second paper in the series. In Paper I (Ellison et al. 2008) we focussed on a sample with strong emission lines to investigate the effect of galaxy interactions on the mass-metallicity relation and fraction of active galactic nuclei. In two ...
... 2009; Brasseur et al. 2008) and pairs, of which this is the second paper in the series. In Paper I (Ellison et al. 2008) we focussed on a sample with strong emission lines to investigate the effect of galaxy interactions on the mass-metallicity relation and fraction of active galactic nuclei. In two ...
Star Formation and Dynamics in the Galactic Centre
... The first attempts to estimate the mass enclosed in the central parsec are radial velocity measurements of ionized gas located in the structure which is known as minispiral (Lacy et al. 1980). On the other hand, the radial velocity of ionized gas may be affected by a plethora of processes besides gr ...
... The first attempts to estimate the mass enclosed in the central parsec are radial velocity measurements of ionized gas located in the structure which is known as minispiral (Lacy et al. 1980). On the other hand, the radial velocity of ionized gas may be affected by a plethora of processes besides gr ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.