Implicit theories of a desire for fame

The aim of the present studies was to generate implicit theories of a desire for fame among the general population. In Study 1, we were able to develop a nine-factor analytic model of conceptions of the desire to be famous that initially comprised nine separate factors; ambition, meaning derived through comparison with others, psychologically vulnerable, attention seeking, conceitedness, social access, altruistic, positive affect, and glamour. Analysis that sought to examine replicability among these factors suggested that three factors (altruistic, positive affect, and glamour) neither display factor congruence nor display adequate internal reliability. A second study examined the validity of these factors in predicting profiles of individuals who may desire fame. The findings from this study suggested that two of the nine factors (positive affect and altruism) could not be considered strong factors within the model. Overall, the findings suggest that implicit theories of a desire for fame comprise six factors. The discussion focuses on how an implicit model of a desire for fame might progress into formal theories of a desire for fame

The effect of the galaxy environment on the size and structure of galaxies

In this thesis, we explore the effect of the galaxy environment on the physical size and structure of the stellar distribution for relatively local galaxies (z < 0.3) using Hubble Space Telescope/Advanced Camera for Surveys imaging and data from the Space Telescope A901/2 galaxy evolution survey (STAGES). We determine the effect of the environment on the size of the stellar distribution (i.e. galaxy sizes) by comparing the stellar-mass-size relations in the field and cluster environments for different Hubble-type morphologies. For elliptical, lenticular, and high-mass (M* > 10^10 M_sun) spirals, we find no evidence to suggest that a galaxy's size (i.e. effective radius a_e) is dependent on the environment. This result suggests that internal drivers are responsible for any potential size evolution inherent to these galaxies. However, for intermediate-/low-mass spirals (M* ) being ~15-20 per cent larger in the field than in the cluster. This result is driven by a population of low-mass, large-a_e field spirals (observed to contain extended stellar discs) that are largely absent from the cluster environments. This difference implies that the fragile extended stellar discs of these spiral galaxies may not survive the environmental conditions in the cluster. We expand on this result by investigating the effect of the environment on the structure of galactic discs in spiral and S0 galaxies. Using V-band radial surface brightness mu(r) profiles, we identify break features in the stellar disc (down-bending break - truncation; up-bending break - antitruncation) and evaluate their dependence on the galaxy environment. For both spiral and S0 galaxies, we find no evidence to suggest an environmental dependence on the frequency of these break features. We also find no evidence to suggest an environmental dependence on the scalelength h of pure exponential discs, or the break strength T (outer-to-inner scalelength ratio) of broken exponential discs. These results indicate that the stellar distribution in the outer regions of spiral/S0 galaxies is not significantly influenced by the galaxy environment. In our structural analyses, one interesting observation was that truncated mu(r) profiles (down-bending breaks) are very rare in S0s; whereas in spiral galaxies they are commonplace. We expand on this result by comparing the structural properties of the disc (scalelength h, break strength T, break surface brightness mu_brk) in spiral and S0 galaxies. In these comparisons, we find no evidence to suggest that the scalelength h of pure exponential discs or the break surface brightness mu_brk of broken exponentials is dependent on the galaxy morphology. However, we do find some evidence to suggest that the break strength T is smaller (weaker) in S0s compared to spiral galaxies. This result suggests that some process inherent to the morphological transformation of spiral galaxies into S0s does affect the structure of the stellar disc causing a weakening of mu(r) breaks and may even eliminate truncations from S0 galaxies. In additional structural comparisons, we also find that the fraction of exponential bulges is the same (~20 per cent) in both spiral and S0 galaxies, suggesting that major mergers are not driving this transformation. Finally, we complement our structural analyses with an assessment of whether the excess light in the outer regions of antitruncated (up-bending) mu(r) profiles is caused by an outer exponential disc or an extended spheroidal component: we use bulge-disc decomposition in order to achieve this. For spiral galaxies, in the vast majority of cases, evidence indicates that the excess light at large radii is related to an outer shallow disc. We thus conclude that in the majority of spiral galaxies, antitruncated outer stellar discs cannot be explained by bulge light and thus remain a pure disc phenomenon. However, for S0s, bulge light can have a significant effect in the outer regions of the mu(r) profile. In approximately half of S0 antitruncations, the excess light at large radii can be entirely accounted for by light from an extended spheroidal component. These results suggest that as a galaxy evolves from a spiral into an S0, the galaxy naturally evolves into a more bulge-dominated system. We suggest a fading stellar disc (e.g. caused by gas stripping and the termination of star formation) is consistent with this result. In conclusion, our environmental studies indicate that the environment has little direct affect on the size and structure of a galaxy's stellar distribution. This result implies that physical processes directly affecting the structure of the stellar distribution (e.g. mergers or harassment), are not driving the observed morphology-density relation. With respect to both our environmental and morphological studies, we can conclude that more subtle processes acting on the gaseous component of a galaxy (e.g. ram-pressure stripping) are more likely to play an important role in the origin of the morphology-density relation and the transformation of spirals into S0s

Lives in the balance? Gender, age and assets in late-nineteenth-century England and Wales

Studies of wealth-holding in nineteenth-century Britain focus either on establishing aggregate measures or on individual case studies. These do not allow for a comparative analysis of the way that the composition of wealth was influenced by age and gender. This article explores the importance of these factors using both a case-study approach and a more comprehensive analysis of wealth left at death for a sample of 1,444 individuals. By establishing the age at death for 1,274 of these individuals, together with evidence from a series of death duty records, it is possible to determine the composition of assets by age and gender. For both men and women, shares became more important over the life course. Real estate was more important for men of all ages compared to women, for whom safe investments in government securities assumed greater significance with age. These findings confirm that both age and gender influenced the amount and composition of wealth and demonstrate that these factors need to be taken into account in any model that seeks to make generalizations about the pattern of wealth-holding in the population at large. Emphasizing these demand-side factors provides a different perspective on the rise of Britain as a 'nation of investors'

The effect of the galaxy environment on the size and structure of galaxies

In this thesis, we explore the effect of the galaxy environment on the physical size and structure of the stellar distribution for relatively local galaxies (z < 0.3) using Hubble Space Telescope/Advanced Camera for Surveys imaging and data from the Space Telescope A901/2 galaxy evolution survey (STAGES). We determine the effect of the environment on the size of the stellar distribution (i.e. galaxy sizes) by comparing the stellar-mass-size relations in the field and cluster environments for different Hubble-type morphologies. For elliptical, lenticular, and high-mass (M* > 10^10 M_sun) spirals, we find no evidence to suggest that a galaxy's size (i.e. effective radius a_e) is dependent on the environment. This result suggests that internal drivers are responsible for any potential size evolution inherent to these galaxies. However, for intermediate-/low-mass spirals (M* ) being ~15-20 per cent larger in the field than in the cluster. This result is driven by a population of low-mass, large-a_e field spirals (observed to contain extended stellar discs) that are largely absent from the cluster environments. This difference implies that the fragile extended stellar discs of these spiral galaxies may not survive the environmental conditions in the cluster. We expand on this result by investigating the effect of the environment on the structure of galactic discs in spiral and S0 galaxies. Using V-band radial surface brightness mu(r) profiles, we identify break features in the stellar disc (down-bending break - truncation; up-bending break - antitruncation) and evaluate their dependence on the galaxy environment. For both spiral and S0 galaxies, we find no evidence to suggest an environmental dependence on the frequency of these break features. We also find no evidence to suggest an environmental dependence on the scalelength h of pure exponential discs, or the break strength T (outer-to-inner scalelength ratio) of broken exponential discs. These results indicate that the stellar distribution in the outer regions of spiral/S0 galaxies is not significantly influenced by the galaxy environment. In our structural analyses, one interesting observation was that truncated mu(r) profiles (down-bending breaks) are very rare in S0s; whereas in spiral galaxies they are commonplace. We expand on this result by comparing the structural properties of the disc (scalelength h, break strength T, break surface brightness mu_brk) in spiral and S0 galaxies. In these comparisons, we find no evidence to suggest that the scalelength h of pure exponential discs or the break surface brightness mu_brk of broken exponentials is dependent on the galaxy morphology. However, we do find some evidence to suggest that the break strength T is smaller (weaker) in S0s compared to spiral galaxies. This result suggests that some process inherent to the morphological transformation of spiral galaxies into S0s does affect the structure of the stellar disc causing a weakening of mu(r) breaks and may even eliminate truncations from S0 galaxies. In additional structural comparisons, we also find that the fraction of exponential bulges is the same (~20 per cent) in both spiral and S0 galaxies, suggesting that major mergers are not driving this transformation. Finally, we complement our structural analyses with an assessment of whether the excess light in the outer regions of antitruncated (up-bending) mu(r) profiles is caused by an outer exponential disc or an extended spheroidal component: we use bulge-disc decomposition in order to achieve this. For spiral galaxies, in the vast majority of cases, evidence indicates that the excess light at large radii is related to an outer shallow disc. We thus conclude that in the majority of spiral galaxies, antitruncated outer stellar discs cannot be explained by bulge light and thus remain a pure disc phenomenon. However, for S0s, bulge light can have a significant effect in the outer regions of the mu(r) profile. In approximately half of S0 antitruncations, the excess light at large radii can be entirely accounted for by light from an extended spheroidal component. These results suggest that as a galaxy evolves from a spiral into an S0, the galaxy naturally evolves into a more bulge-dominated system. We suggest a fading stellar disc (e.g. caused by gas stripping and the termination of star formation) is consistent with this result. In conclusion, our environmental studies indicate that the environment has little direct affect on the size and structure of a galaxy's stellar distribution. This result implies that physical processes directly affecting the structure of the stellar distribution (e.g. mergers or harassment), are not driving the observed morphology-density relation. With respect to both our environmental and morphological studies, we can conclude that more subtle processes acting on the gaseous component of a galaxy (e.g. ram-pressure stripping) are more likely to play an important role in the origin of the morphology-density relation and the transformation of spirals into S0s

The evolution of post-starburst galaxies from z=2 to 0.5

We present the evolution in the number density and stellar mass functions of photometrically selected post-starburst galaxies in the UKIDSSUltraDeep Survey,with redshifts of 0.510. We find that this transitionary species of galaxy is rare at all redshifts, contributing ∼5 per cent of the total population at z ∼ 2, to <1 per cent by z ∼ 0.5. By comparing the mass functions of quiescent galaxies to post-starburst galaxies at three cosmic epochs, we show that rapid quenching of star formation can account for 100 per cent of quiescent galaxy formation, if the post-starburst spectral features are visible for ∼250 Myr. The flattening of the low-mass end of the quiescent galaxy stellar mass function seen at z ∼ 1 can be entirely explained by the addition of rapidly quenched galaxies. Only if a significant fraction of post-starburst galaxies have features that are visible for longer than 250 Myr, or they acquire new gas and return to the star-forming sequence, can there be significant growth of the red sequence from a slower quenching route. The shape of the mass function of these transitory post-starburst galaxies resembles that of quiescent galaxies at z ∼ 2, with a preferred stellar mass of log (M/M�) ∼10.6, but evolves steadily to resemble that of star-forming galaxies at z /~ 2 they are exclusively massive galaxies that have formed the bulk of their stars during a rapid assembly period, followed by complete quenching of further star formation; (2) at z </~1 they are caused by the rapid quenching of gas-rich star-forming galaxies, independent of stellar mass, possibly due to environment and/or gas-rich major mergers

Anti-truncated stellar light profiles in the outer regions of STAGES spiral galaxies: bulge or disc related?

We present a comparison of azimuthally averaged radial surface brightness mu(r) profiles and analytical bulge-disc decompositions (de Vaucouleurs, r^(1/4) bulge plus exponential disc) for spiral galaxies using Hubble Space Telescope/Advanced Camera for Surveys V-band imaging from the Space Telescope A901/2 Galaxy Evolution Survey (STAGES). In the established classification scheme, antitruncated mu(r) profiles (Type III) have a broken exponential disc with a shallower region beyond the break radius r_brk. The excess light at large radii (r > r_brk) can either be caused by an outer exponential disc (Type III-d) or an extended spheroidal component (Type III-s). Using our comparisons, we determine the contribution of bulge light at r > r_brk for a large sample of 78 (barred/unbarred, Sa-Sd) spiral galaxies with outer disc antitruncations (mu_brk > 24 mag arcsec^-2). In the majority of cases (~85 per cent), evidence indicates that excess light at r > r_brk is related to an outer shallow disc (Type III-d). Here, the contribution of bulge light at r > r_brk is either negligible (~70 per cent) or too little to explain the antitruncation (~15 per cent). However in the latter cases, bulge light can affect the measured disc properties (e.g. mu_brk, outer scalelength). In the remaining cases (~15 per cent), light at r > r_brk is dominated by the bulge (Type III-s). Here, for most cases the bulge profile dominates at all radii and only occasionally (3 galaxies, ~5 per cent) extends beyond that of a dominant disc and explains the excess light at r > r_brk. We thus conclude that in the vast majority of cases antitruncated outer discs cannot be explained by bulge light and thus remain a pure disc phenomenon.Comment: Accepted to MNRA

The environmental dependence of the stellar mass-size relation in STAGES galaxies

We present the stellar mass-size relations for elliptical, lenticular, and spiral galaxies in the field and cluster environments using HST/ACS imaging and data from the Space Telescope A901/2 Galaxy Evolution Survey (STAGES). We use a large sample of ~1200 field and cluster galaxies, and a sub-sample of cluster core galaxies, and quantify the significance of any putative environmental dependence on the stellar mass-size relation. For elliptical, lenticular, and high-mass (log M*/M_sun > 10) spiral galaxies we find no evidence to suggest any such environmental dependence, implying that internal drivers are governing their size evolution. For intermediate/low-mass spirals (log M*/M_sun < 10) we find evidence, significant at the 2-sigma level, for a possible environmental dependence on galaxy sizes: the mean effective radius a_e for lower-mass spirals is ~15-20 per cent larger in the field than in the cluster. This is due to a population of low-mass large-a_e field spirals that are largely absent from the cluster environments. These large-a_e field spirals contain extended stellar discs not present in their cluster counterparts. This suggests the fragile extended stellar discs of these spiral galaxies may not survive the environmental conditions in the cluster. Our results suggest that internal physical processes are the main drivers governing the size evolution of galaxies, with the environment possibly playing a role affecting only the discs of intermediate/low-mass spirals.Comment: 16 pages, 10 figures, accepted to MNRA

The environmental dependence of the structure of outer galactic discs in STAGES spiral galaxies

We present an analysis of V-band radial surface brightness profiles for spiral galaxies from the field and cluster environments using Hubble Space Telescope/Advanced Camera for Surveys imaging and data from the Space Telescope A901/2 Galaxy Evolution Survey (STAGES). We use a large sample of ~330 face-on to intermediately inclined spiral galaxies and assess the effect of the galaxy environment on the azimuthally averaged radial surface brightness mu profiles for each galaxy in the outer stellar disc (24 < mu < 26.5 mag per sq arcsec). For galaxies with a purely exponential outer disc (~50 per cent), we determine the significance of an environmental dependence on the outer disc scalelength h_out. For galaxies with a broken exponential in their outer disc, either down-bending (truncation, ~10 per cent) or up-bending (anti-truncation, ~40 per cent), we measure the strength T (outer-to-inner scalelength ratio, log_10(h_out/h_in) of the mu breaks and determine the significance of an environmental dependence on break strength T. Surprisingly, we find no evidence to suggest any such environmental dependence on either outer disc scalelength h_out or break strength T, implying that the galaxy environment is not affecting the stellar distribution in the outer stellar disc. We also find that for galaxies with small effective radii (r_e < 3 kpc) there is a lack of outer disc truncations in both the field and cluster environments. Our results suggest that the stellar distribution in the outer disc of spiral galaxies is not significantly affected by the galaxy environment.Comment: Accepted to MNRAS. Appendix A available at http://www.nottingham.ac.uk/~ppxdtm/STAGES_profiles_appendix.pd

The clustering of X-ray AGN at 0.5 < z < 4.5 : host galaxies dictate dark matter halo mass

We present evidence that active galactic nuclei (AGN) do not reside in 'special' environments, but instead show large-scale clustering determined by the properties of their host galaxies. Our study is based on an angular cross-correlation analysis applied to X-ray selected AGN in the COSMOS and UDS fields, spanning redshifts from z ∼ 4.5 to z ∼ 0.5. Consistent with previous studies, we find that AGN at all epochs are on average hosted by galaxies in dark matter haloes of 1012-1013 M⊙, intermediate between star-forming and passive galaxies. We find, however, that the same clustering signal can be produced by inactive (I.e. non-AGN) galaxies closely matched to the AGN in spectral class, stellar mass, and redshift. We therefore argue that the inferred bias for AGN lies in between the star-forming and passive galaxy populations because AGN host galaxies are comprised of a mixture of the two populations. Although AGN hosted by higher mass galaxies are more clustered than lower mass galaxies, this stellar mass dependence disappears when passive host galaxies are removed. The strength of clustering is also largely independent of AGN X-ray luminosity. We conclude that the most important property that determines the clustering in a given AGN population is the fraction of passive host galaxies. We also infer that AGN luminosity is likely not driven by environmental triggering, and further hypothesize that AGN may be a stochastic phenomenon without a strong dependence onenvironment.Publisher PDFPeer reviewe