The Ubiquity and Dual Nature of Ultra Compact Dwarfs

We present the discovery of several Ultra Compact Dwarfs (UCDs) located in field/group environments. Examination of these objects, plus literature objects, confirms the existence of two distinct formation channels for UCDs. We find that the UCDs we have discovered around the group elliptical NGC3923 (and UCDs generally) have properties consistent with their being the most luminous members of the host galaxy's globular cluster (GC) system. We describe UCDs of this type as giant GCs (GGCs). In contrast, the UCD we have found associated with the isolated S0 NGC4546 is clearly the result of the stripping of a nucleated companion galaxy. The young age (~3.4 Gyr) of the UCD, the lack of a correspondingly young GC population, the apparently short dynamical friction decay timescale (~0.5 Gyr) of the UCD, and the presence of a counterrotating gas disc in the host galaxy (co-rotating with the UCD) together suggest that this UCD is the liberated nucleus remaining after the recent stripping of a companion by NGC4546. We suggest a general scheme that unifies the formation of GCs, UCDs, and galaxy nuclei. In this picture "normal" GCs are a composite population, composed of GCs formed in situ, GCs acquired from accreted galaxies, and a population of lower mass stripped dwarf nuclei masquerading as GCs. Above a "scaling onset mass" of 2x10^6 Msun (Mv ~ -10), UCDs emerge together with a mass-size relation and a likely mass-metallicity relation (the "blue tilt"). In the mass range up to 7x10^7 Msun (Mv ~ -13) UCDs comprise a composite population of GGCs and stripped nuclei. Above 7x10^7 Msun, UCDs must be almost exclusively stripped nuclei, as no sufficiently rich GC systems exist to populate such an extreme of the GCLF.Comment: 23 pages, 16 figures, accepted for publication in MNRA

On the problem of modeling for parameter identification in distributed structures

Structures are often characterized by parameters, such as mass and stiffness, that are spatially distributed. Parameter identification of distributed structures is subject to many of the difficulties involved in the modeling problem, and the choice of the model can greatly affect the results of the parameter identification process. Analogously to control spillover in the control of distributed-parameter systems, identification spillover is shown to exist as well and its effect is to degrade the parameter estimates. Moreover, as in modeling by the Rayleigh-Ritz method, it is shown that, for a Rayleigh-Ritz type identification algorithm, an inclusion principle exists in the identification of distributed-parameter systems as well, so that the identified natural frequencies approach the actual natural frequencies monotonically from above

The formation of early-type galaxies

This Thesis examines the formation and evolution of early-type elliptical and S0 galaxies. In order to shed light on the key processes which lead to the formation of elliptical and S0 galaxies a range of techniques have been employed. The kinematics and stellar populations of the major and minor axes of the nearby edge-on S0 galaxy NGC 3115 have been examined through deep Gemini-GMOS longslit spectroscopy. The behaviour of the radial profiles of the line strength indices is found to be well explained by a simple model where NGC 3115 is composed of two components; an older classical spheroidal component, which displays a negative (decreases outwards) metallicity gradient and is enhanced in α-elements relative to the solar value together with a younger, constant metallicity disc which displays close to solar [а/Ғе]. The kinematics and stellar populations of the integrated light of NGC 3115 are compared to those previously found for its globular duster (GC) system. The GCs are found to rotate in a manner consistent with the galaxy as a whole and the red GC sub-population is found to have ages, metallicities and [a/Fe] abundance indistinguishable from those displayed by the spheroid of NGC 3115 at 2 effective radii. This study provides strong support to the theory that the GC systems of galaxies are closely linked to galaxy spheroid formation. The formation and evolution of so galaxies is further examined through the study of 18 edge-on S0 galaxies observed in a manner identical to that presented for NGC 3115. These galaxies are all found to display significant stellar discs and to present regular disc kinematics. In several cases signatures of kinematic substructure such as inner discs or bars are found. Ionised gas emission is observed at a low level in 72% of the sample; the kinematics of this ionised gas is highly variable, with examples of regular disc-like kinematics, confused counter-rotation and streams not aligned with any axis observed. The kinematic data has been utilised to produce a B-band Tully-Fisher relation (TFR) for S0 galaxies. The S0 TFR is observed to be offset to fainter magnitudes from the TFR for local spirals, an observation which can crudely be explained by the formation of S0s through the truncation of star formation (and subsequent disc fading) in normal spiral galaxies. The offset from the spiral TFR for each galaxy is shown to correlate well with both disc and central age, in the correct sense, and with the correct magnitude, such that the large observed scatter in the S0 TFR can be explained as being due to the different times at which the progenitor spirals ceased forming stars and hence the different amounts they have faded up to the present. Multi-object spectroscopic observations of the GC system of the shell elliptical NGC3923 are presented, as well as a novel technique for examining the spectra of the integrated light of galaxies at the same time as observing their GC system. The observations are used to demonstrate that neither the integrated light nor the GC system of NGC 3923 shows evidence for significant rotation. The stellar populations of the red GCs are again found to be consistent in age, metallicity and [a/Fe] with that displayed by the integrated light of the spheroid of NGC 3923 at large radii (> 2R(_e)). The velocity dispersion profile of the integrated light and GC system of NGC 3923 are both observed to be flat at larger radii, a finding indicative of the presence of significant amounts of Dark Matter. Using the GC kinematic data, a simple spherical isotropic dynamical model is presented which demonstrates that a significant increase in mass-to-light (M/L) ratio is required to explain the observed constant velocity dispersion profile. The M/L profile determined is in good agreement with that measured independently from X-ray observations

The first and second Earls of Rutland and their part in the central and local politics of mid-Tudor England

This thesis investigates the role of Thomas and Henry Manners, first and second earls of Rutland, in the central and local politics of mid -Tudor England. In so doing, five factors are scrutinized throughout: landed property, political and military office -holding, Court politics, religion, and the Manners' network of friends, servants, and relatives. The thesis is divided into seven chapters, the first six of which explore how most or all of these factors influenced the political life of the family during a segment of time. The final chapter compares and contrasts the achievement of the Manners with other noble families.Chapter 1 deals with the beginnings of the family until the creation of Thomas Manners, Lord Roos, as earl of Rutland in 1525. The next chapter studies the political life of the new earl until 1536 and particu- larly emphasizes his being drawn into Henry's religious policy. Chapter 3 reveals the effects of his involvement in suppressing the rebels in the Pilgrimage of Grace, his increasing employment in the service of the Crown, and his ability to profit from the Dissolution of the Monasteries until his death in 1543. By this time the family had reached its Tudor economic peak.The themes of continuity and development are explored from the wardship of the next earl until his imprisonment in the Fleet for supporting Northumberland in the Lady Jane Grey crisis. This is followed by a chapter which probes the young earl's ability to come to terms with the Marian regime. Chapter 6 reveals that he experienced even higher favour during Elizabeth's reign, culminating in his office of president of the Council of the North, during which he fell ill and died in 1563.It is seen that the mid -Tudor Manners were able firmly to establish a powerbase in the north -east Midlands, to continue their involvement in the North, and to pass on a pattern of office -holding which would be utilized by successive earls of Rutland. Further, they were able to weather the turbulent mid -Tudor high politics because they were able to demonstrate that they were too useful and loyal to the Crown to be ignored and yet not dangerous enough to be eliminated.In comparison with other nobles at the time they were successful; and yet, they were in many ways typical of the high nobility. In fact, the story of the mid - Tudor Manners demonstrates that if there was a mid -Tudor crisis it was, at least in part, a crisis in the highest levels of leadership. The ruling powers during this time failed to make effective use of these willing and highly important servants of the Crown, and instead tended to place personal ambition or ideology above good governing

P-221 Working with hospices to ensure patients' digital legacy wishes are adhered to

The Digital Legacy Association (DLA) was launched at last year’s Hospice UK conference. Their work is focused on raising awareness and improving processes in areas relating to death and the internet. Over the last 12 months the DLA have published a free framework, developed training workshops, launched a free hospice inpatient resource, run ‘pop-up’ events, organised a Digital Legacy conference, carried out different forms of research and campaigned highlighting that end of life and bereavement in relation to the internet and electronic devices is an area requiring thought, governance and change. The DLA spend a lot of time working with hospices, CCGs, charities and trusts. The outcome is improved knowledge and skillsets applied at an organisational and/or at an individual level. The diffusion of the DLAs information occurs by supporting professionals through a variety of different channels. In turn this helps professionals to better support patients and their families. The DLA’s work often revolves around conversations and campaigning. Their recent work for Velindre NHS Trust, Aneurin Bevan UHB & Byw Nawr included building a TalkCPR awareness website. The goal of the TalkCPR campaign is to help increase dialogue around CPR and DNACPR within Wales. The TalkCPR campaign was recently nominated for a NHS Wales award. This paper will document the DLA’s journey over the last year, explain how they use creativity to address end-of-life and document how they plan to support every UK hospice over the course of 2017

Understanding the central kinematics of globular clusters with simulated integrated-light IFU observations

The detection of intermediate mass black holes in the centres of globular clusters is highly controversial, as complementary observational methods often deliver significantly different results. In order to understand these discrepancies, we develop a procedure to simulate integral field unit (IFU) observations of globular clusters: Simulating IFU Star Cluster Observations (SISCO). The input of our software are realistic dynamical models of globular clusters that are then converted in a spectral data cube. We apply SISCO to Monte Carlo cluster simulations from Downing et al. (2010), with a realistic number of stars and concentrations. Using independent realisations of a given simulation we are able to quantify the stochasticity intrinsic to the problem of observing a partially resolved stellar population with integrated-light spectroscopy. We show that the luminosity-weighted IFU observations can be strongly biased by the presence of a few bright stars that introduce a scatter in the velocity dispersion measurements up to $\simeq$40% around the expected value, preventing any sound assessment of the central kinematic and a sensible interpretation of the presence/absence of an intermediate mass black hole. Moreover, we illustrate that, in our mock IFU observations, the average kinematic tracer has a mass of $\simeq$0.75 solar masses, only slightly lower than the mass of the typical stars examined in studies of resolved line-of-sight velocities of giant stars. Finally, in order to recover unbiased kinematic measurements we test different masking techniques that allow us to remove the spaxels dominated by bright stars, bringing the scatter down to a level of only a few percent. The application of SISCO will allow to investigate state-of-the-art simulations as realistic observations.Comment: 13 pages, 9 figures, 1 table. Accepted for publication in MNRA