The Evolution of the Mass-Size relation to z = 3.5 in the GOODS
... in narrow mass bins for all galaxies from CDF-S. The UV bright galaxies are in general larger than normal field galaxies at the same mass. ...
... in narrow mass bins for all galaxies from CDF-S. The UV bright galaxies are in general larger than normal field galaxies at the same mass. ...
Testing the Initial-Final Mass Relationship of White Dwarfs Silvia Catal´ an Ruiz
... The initial-final mass relationship can be determined using two different approaches. The first approach involves an indirect measurement. This is done by studying the influence of the initial-final mass relationship in the two fundamental tools typically used to statistically analyze the properties ...
... The initial-final mass relationship can be determined using two different approaches. The first approach involves an indirect measurement. This is done by studying the influence of the initial-final mass relationship in the two fundamental tools typically used to statistically analyze the properties ...
PhD thesis
... 3.2.2 Expanded Very Large Array . . . . . . . . . . . . . . . . . . 3.2.3 Combined Array for Research in Millimeter-wave Astronomy 3.3 Continuum results . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3.3.1 Centimeter and millimeter continuum results . . . . . . . . . 3.3.2 Spectral energy d ...
... 3.2.2 Expanded Very Large Array . . . . . . . . . . . . . . . . . . 3.2.3 Combined Array for Research in Millimeter-wave Astronomy 3.3 Continuum results . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3.3.1 Centimeter and millimeter continuum results . . . . . . . . . 3.3.2 Spectral energy d ...
University of Groningen Late-type spiral galaxies Ganda, Katia
... whose formation and evolutionary pattern are not properly understood yet. Carollo et al. (2007) also performed a population analysis on nine late-type spiral galaxies (types between Sa and Sc) on the basis of HST ACS and NICMOS optical and near-infrared colours. The high spatial resolution of their ...
... whose formation and evolutionary pattern are not properly understood yet. Carollo et al. (2007) also performed a population analysis on nine late-type spiral galaxies (types between Sa and Sc) on the basis of HST ACS and NICMOS optical and near-infrared colours. The high spatial resolution of their ...
The white dwarf luminosity function
... Over fifty years ago it was first recognized that the coolest (faintest) white dwarfs are remnants of the earliest stars to form in the Solar neighborhood (Schmidt, 1959), and that cooling theory could be used to estimate the time elapsed since star formation commenced in the Galactic disk (Mestel, ...
... Over fifty years ago it was first recognized that the coolest (faintest) white dwarfs are remnants of the earliest stars to form in the Solar neighborhood (Schmidt, 1959), and that cooling theory could be used to estimate the time elapsed since star formation commenced in the Galactic disk (Mestel, ...
Stellar Mass Loss in Globular - Jodrell Bank Centre for Astrophysics
... 47 Tucanae and ω Centauri, finding 47 Tuc V1 (and possibly V18) and ω Cen V6 surrounded by circumstellar silicate dust. ω Cen V42 may also be surrounded by carbon-rich dust. Much of this work is devoted to finding the threshold for dust production and the mass-loss rates from cluster stars with both c ...
... 47 Tucanae and ω Centauri, finding 47 Tuc V1 (and possibly V18) and ω Cen V6 surrounded by circumstellar silicate dust. ω Cen V42 may also be surrounded by carbon-rich dust. Much of this work is devoted to finding the threshold for dust production and the mass-loss rates from cluster stars with both c ...
Rotation Curves of Spiral Galaxies
... galaxy, and Wolf (1914) detected inclined lines in the nuclear spectrum of M81. This evidence led Pease (1918) to use the Mt. Wilson 60-inch to \investigate the rotation of the great nebula in Andromeda" by obtaining a minor axis long slit spectrum of M31 with an exposure of 84 hours taken during cl ...
... galaxy, and Wolf (1914) detected inclined lines in the nuclear spectrum of M81. This evidence led Pease (1918) to use the Mt. Wilson 60-inch to \investigate the rotation of the great nebula in Andromeda" by obtaining a minor axis long slit spectrum of M31 with an exposure of 84 hours taken during cl ...
H-alpha Imaging of Early-type (Sa
... only a few massive stars, whereas H II regions in late-type spirals can contain hundreds or even thousands of stars. The seventeen galaxies included in category 1 resemble what most astronomers identify as classical early-type spirals. Morphologically, most category 1 galaxies appear undisturbed in ...
... only a few massive stars, whereas H II regions in late-type spirals can contain hundreds or even thousands of stars. The seventeen galaxies included in category 1 resemble what most astronomers identify as classical early-type spirals. Morphologically, most category 1 galaxies appear undisturbed in ...
COMPACT GROUPS OF GALAXIES
... four or five galaxies in close proximity to one another. Such groups do not necessarily form a distinct class but may instead be extreme examples of systems having a range of galaxy density and population. Because of this, the properties of the groups in any particular sample may be strongly influen ...
... four or five galaxies in close proximity to one another. Such groups do not necessarily form a distinct class but may instead be extreme examples of systems having a range of galaxy density and population. Because of this, the properties of the groups in any particular sample may be strongly influen ...
Formation and evolution of giant molecular clouds in a barred spiral
... inter-arm region. 3) We modelled the triangles are Type C, which are unbound, transient clouds. barred spiral galaxy, M83. M83 is a nearby galaxy and has been observed at various wavelengths. Its GMC properties are being observed by ALMA (Hirota et al., in preparation), and we would directly compare ...
... inter-arm region. 3) We modelled the triangles are Type C, which are unbound, transient clouds. barred spiral galaxy, M83. M83 is a nearby galaxy and has been observed at various wavelengths. Its GMC properties are being observed by ALMA (Hirota et al., in preparation), and we would directly compare ...
Constraints on the physical properties and chemical evolution of star
... The emission from interstellar gas heated by young stars in galaxies contains valuable clues about both the nature of these stars and the physical conditions in the interstellar medium. In particular, prominent emission lines produced by H ii regions, diffuse ionized gas and a potential active galac ...
... The emission from interstellar gas heated by young stars in galaxies contains valuable clues about both the nature of these stars and the physical conditions in the interstellar medium. In particular, prominent emission lines produced by H ii regions, diffuse ionized gas and a potential active galac ...
Classical Be Stars: Rapidly Rotating B Stars with Viscous Keplerian
... well, but due to the weakness of the ionizing radiation this vanishes quickly towards later types. From the spectral appearance, it is quite conceivable to ascribe those shell lines to disks, and thus regard them as the late-type extension of Be stars. As the example of 51 Oph has shown, however, th ...
... well, but due to the weakness of the ionizing radiation this vanishes quickly towards later types. From the spectral appearance, it is quite conceivable to ascribe those shell lines to disks, and thus regard them as the late-type extension of Be stars. As the example of 51 Oph has shown, however, th ...
the nuclear reddening curve for active galactic nuclei and the shape
... structure, creating composite UV-optical spectra of 13–18 objects each. The four subsets are R 1, 0:1 R < 1, R < 0:1, and compact steep-spectrum (CSS) radio sources. Baker & Hunstead (1995) also give mean line strengths for the four subsets. In addition to the MQS AGNs, we also considered the si ...
... structure, creating composite UV-optical spectra of 13–18 objects each. The four subsets are R 1, 0:1 R < 1, R < 0:1, and compact steep-spectrum (CSS) radio sources. Baker & Hunstead (1995) also give mean line strengths for the four subsets. In addition to the MQS AGNs, we also considered the si ...
Morphology and dynamics of the cosmic web Aragón Calvo
... de Lapparent et al., 1986; Colless et al., 2001). Computer simulations have successfully replicated these features in the galaxy distribution (Efstathiou, 1996; Jenkins et al., 1998; Evrard et al., 2002; Springel et al., 2005) indicating that the observed cellular patterns are a natural aspect of st ...
... de Lapparent et al., 1986; Colless et al., 2001). Computer simulations have successfully replicated these features in the galaxy distribution (Efstathiou, 1996; Jenkins et al., 1998; Evrard et al., 2002; Springel et al., 2005) indicating that the observed cellular patterns are a natural aspect of st ...
Direct Evidence for Termination of Obscured Star Formation by
... Most discussions of AGN feedback condense the four feedback mechanisms described above into two simplified paradigms; ‘quasar’ mode feedback and ‘radio’ mode feedback. Quasar mode feedback assumes that radiation from an accretion disk terminates star formation in the host galaxy, usually by coupling ...
... Most discussions of AGN feedback condense the four feedback mechanisms described above into two simplified paradigms; ‘quasar’ mode feedback and ‘radio’ mode feedback. Quasar mode feedback assumes that radiation from an accretion disk terminates star formation in the host galaxy, usually by coupling ...
The Physical Origins of The Morphology
... structure and gas content of a galaxy. Tidal interactions with other galaxies or the potential of a large halo can strip an in-falling galaxy from gas, and reduce the stellar disk as well (Moore et al. 1996). There are two reasons why it is surprisingly difficult to interpret the MDR, constrain its ...
... structure and gas content of a galaxy. Tidal interactions with other galaxies or the potential of a large halo can strip an in-falling galaxy from gas, and reduce the stellar disk as well (Moore et al. 1996). There are two reasons why it is surprisingly difficult to interpret the MDR, constrain its ...
https://tel.archives-ouvertes.fr/file/index/docid/1058049/filename/HOU_XIAN_2013.pdf
... This is a milestone in my life, even though there is still definitely a long way to go in the ultimate pursuit of science. I owe my deep acknowledgements to all who have made me who I am today. First of all, I’m extremely grateful to David Smith, my thesis supervisor, for having accepted me to be a ...
... This is a milestone in my life, even though there is still definitely a long way to go in the ultimate pursuit of science. I owe my deep acknowledgements to all who have made me who I am today. First of all, I’m extremely grateful to David Smith, my thesis supervisor, for having accepted me to be a ...
Evolutionary and pulsational properties of white dwarf stars
... asymptotic giant branch (AGB), they are significant contributors to the chemical evolution of the Galaxy. More than 10,000 spectroscopically identified white dwarfs with determined effective temperatures (Teff ) and gravities (log g) have been detected to date (Kleinman et al. 2004; Kepler et al. 20 ...
... asymptotic giant branch (AGB), they are significant contributors to the chemical evolution of the Galaxy. More than 10,000 spectroscopically identified white dwarfs with determined effective temperatures (Teff ) and gravities (log g) have been detected to date (Kleinman et al. 2004; Kepler et al. 20 ...
Modeling Spatially and Spectrally Resolved Observations to
... In extragalactic astronomy, a central challenge is that we cannot directly watch what happens to galaxies before and after they are observed. This dissertation focuses on linking predictions of galaxy time-evolution directly with observations, evaluating how interactions, mergers, and other processe ...
... In extragalactic astronomy, a central challenge is that we cannot directly watch what happens to galaxies before and after they are observed. This dissertation focuses on linking predictions of galaxy time-evolution directly with observations, evaluating how interactions, mergers, and other processe ...
β Relation for Local Galaxies
... unbiased, representative, and statistically robust sample of nearby star-forming galaxies. Furthermore, by restricting our analysis to galaxies with little dust content, we remove one degree of freedom and can more accurately than in previous studies, pin down the role of stellar population ages and ...
... unbiased, representative, and statistically robust sample of nearby star-forming galaxies. Furthermore, by restricting our analysis to galaxies with little dust content, we remove one degree of freedom and can more accurately than in previous studies, pin down the role of stellar population ages and ...
Liverpool Telescope 2: a new robotic facility for rapid transient follow
... of the explosion, which mostly reflect the size and degree of stripping of the progenitor at the time of explosion. It is important that we link these observed differences with differences in the physical parameters of the progenitors. One of the main heterogeneities is the presence or absence of hy ...
... of the explosion, which mostly reflect the size and degree of stripping of the progenitor at the time of explosion. It is important that we link these observed differences with differences in the physical parameters of the progenitors. One of the main heterogeneities is the presence or absence of hy ...
ULTRA-COMPACT HII REGIONS AND MASSIVE STAR FORMATION
... lower-mass cluster members. They are likely to be surrounded by an equatorial accretion disk and a massive bipolar outflow along their spin axes. Their outflow masses, momenta, and kinetic energies are much larger than those of low-mass protostars, and they are generally poorly collimated relative t ...
... lower-mass cluster members. They are likely to be surrounded by an equatorial accretion disk and a massive bipolar outflow along their spin axes. Their outflow masses, momenta, and kinetic energies are much larger than those of low-mass protostars, and they are generally poorly collimated relative t ...
Physics of Neutron Star Crusts - Institut d`Astronomie et d
... resulting from pressure, a solid crust can support an elastic strain. Elastic properties are reviewed in Section 7. A separate subsection is devoted to the elastic parameters of the so-called “pasta” layers which behave like liquid crystals. The inner crust is permeated by a neutron superfluid. Vario ...
... resulting from pressure, a solid crust can support an elastic strain. Elastic properties are reviewed in Section 7. A separate subsection is devoted to the elastic parameters of the so-called “pasta” layers which behave like liquid crystals. The inner crust is permeated by a neutron superfluid. Vario ...
A Wide-Field Study of the z~ 0.8 Cluster RX J0152. 7
... that cluster galaxies comprise a small fraction of their z ∼ 1 sample, Cooper et al. (2006, 2007) argue against processes such as ram pressure stripping and harassment as the sole origin of the observed color-density trend found at low redshift. Instead, they suggest that processes that form the hig ...
... that cluster galaxies comprise a small fraction of their z ∼ 1 sample, Cooper et al. (2006, 2007) argue against processes such as ram pressure stripping and harassment as the sole origin of the observed color-density trend found at low redshift. Instead, they suggest that processes that form the hig ...
Astrophysical X-ray source
Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.