Red Giants in the Small Magellanic Cloud. II. Metallicity Gradient and Age-Metallicity Relation

We present results from the largest CaII triplet line metallicity study of Small Magellanic Cloud (SMC) field red giant stars to date, involving 3037 objects spread across approximately 37.5 sq. deg., centred on this galaxy. We find a median metallicity of [Fe/H]=-0.99+/-0.01, with clear evidence for an abundance gradient of -0.075+/-0.011 dex / deg. over the inner 5 deg. We interpret the abundance gradient to be the result of an increasing fraction of young stars with decreasing galacto-centric radius, coupled with a uniform global age-metallicity relation. We also demonstrate that the age-metallicity relation for an intermediate age population located 10kpc in front of the NE of the Cloud is indistinguishable from that of the main body of the galaxy, supporting a prior conjecture that this is a stellar analogue of the Magellanic Bridge. The metal poor and metal rich quartiles of our RGB star sample (with complementary optical photometry from the Magellanic Clouds Photometric Survey) are predominantly older and younger than approximately 6Gyr, respectively. Consequently, we draw a link between a kinematical signature, tentatively associated by us with a disk-like structure, and the upsurges in stellar genesis imprinted on the star formation history of the central regions of the SMC. We conclude that the increase in the star formation rate around 5-6Gyr ago was most likely triggered by an interaction between the SMC and LMC.Comment: To appear in MNRA

Red Giants in the Small Magellanic Cloud. I. Disk and Tidal Stream Kinematics

We present results from an extensive spectroscopic survey of field stars in the Small Magellanic Cloud (SMC). 3037 sources, predominantly first-ascent red giants, spread across roughly 37.5 sq. deg, are analysed. The line of sight velocity field is dominated by the projection of the orbital motion of the SMC around the LMC/Milky Way. The residuals are inconsistent with both a non-rotating spheroid and a nearly face on disk system. The current sample and previous stellar and HI kinematics can be reconciled by rotating disk models with line of nodes position angle, theta, ~ 120-130 deg., moderate inclination (i ~ 25-70 deg.), and rotation curves rising at 20-40 km/s/kpc. The metal-poor stars exhibit a lower velocity gradient and higher velocity dispersion than the metal-rich stars. If our interpretation of the velocity patterns as bulk rotation is appropriate, then some revision to simulations of the SMC orbit is required since these are generally tuned to the SMC disk line-of-nodes lying in a NE-SW direction. Residuals show strong spatial structure indicative of non-circular motions that increase in importance with increasing distance from the SMC centre. Kinematic substructure in the north-west part of our survey area is associated with the tidal tail or Counter-Bridge predicted by simulations. Lower line-of-sight velocities towards the Wing and the larger velocities just beyond the SW end of the SMC Bar are probably associated with stellar components of the Magellanic Bridge and Counter-Bridge, respectively. Our results reinforce the notion that the intermediate-age stellar population of the SMC is subject to substantial stripping by external forces.Comment: To appear in MNRA

Investigation of the electrical properties of Si₁-×Ge× channel pMOSFETs with high-κ dielectrics

It is now apparent that the continued performance enhancements of silicon metal-oxide-semiconductor field effect transistors (MOSFETs) can no longer be met by scaling alone. High-mobility channel materials such as strained Si1-xGex and Ge are now being seriously considered to maintain the performance requirements specified by the semiconductor industry. In addition, alternative gate dielectric, or high-κ dielectrics, will also be required to meet gate leakage requirements. This work investigates the properties of using strained Si1-xGex or Ge as alternative channel materials for pMOSFETs incorporating hafnium oxide (HfO2) high-κ gate dielectric. Whilst the SiGe pMOSFETs (x = 0.25) exhibited an enhancement in hole mobility (300 K) over comparable silicon control pMOSFETs with sputtered HfO2 dielectric, high Coulomb scattering and surface roughness scattering relating to the dielectric deposition process meant that the effective hole mobilities were degraded with respect to the silicon universal curve. Germanium channel pMOSFETs with halo-doping and HfO2 gate dielectric deposited by atomic layer deposition showed high hole mobilities of 230 cm2V-1s-1 and 480 cm2V-1s-1 at room temperature and 77 K, respectively. Analysis of the off-state current for the Ge pMOSFETs over a range of temperatures indicated that band-to-band tunnelling, gate-induced drain leakage and other defect-assisted leakage mechanisms could all be important. Hole carrier velocity and impact ionisation were also studied in two batches of buried channel SiGe pMOSFET with x = 0.15 and x = 0.36, respectively. SiGe channel pMOSFETs were found to exhibit reduced impact ionisation compared to silicon control devices, which has been attributed to a strain-induced reduction of the density of states in the SiGe conduction and valence bands. Analysis of the hole carrier velocity indicated that pseudomorphic SiGe offered no performance enhancements over Si below 100 nm, possibly due to higher ion implantation damage and strain relaxation of the strained SiGe channel. The results indicate that velocity overshoot effects might not provide the performance improvements at short channel lengths that was previously hoped for

Near-infrared spectroscopy of the very low mass companion to the hot DA white dwarf PG1234+482

We present a near-infrared spectrum of the hot ($T_{\rm eff}$ $\approx$ 55,000 K) DA white dwarf PG 1234+482. We confirm that a very low mass companion is responsible for the previously recognised infrared photometric excess. We compare spectra of M and L dwarfs, combined with an appropriate white dwarf model, to the data to constrain the spectral type of the secondary. We find that uncertainties in the 2MASS $HK$ photometry of the white dwarf prevent us from distinguishing whether the secondary is stellar or substellar, and assign a spectral type of L0$\pm$1 (M9-L1).Therefore, this is the hottest and youngest ($\approx 10^6$ yr) DA white dwarf with a possible brown dwarf companion.Comment: 5 pages, 2 figures, accepted by MNRA

Further investigation of white dwarfs in the open clusters NGC2287 and NGC3532

We report the results of a CCD imaging survey, complimented by astrometric and spectroscopic follow-up studies, that aims to probe the fate of heavy-weight intermediate mass stars by unearthing new, faint, white dwarf members of the rich, nearby, intermediate age open clusters NGC3532 and NGC2287. We identify a total of four white dwarfs with distances, proper motions and cooling times which can be reconciled with membership of these populations. We find that WDJ0643-203 in NGC2287, with an estimated mass of M=1.02-1.16Msun, is potentially the most massive white dwarf so far identified within an open cluster. Guided by the predictions of modern theoretical models of the late-stage evolution of heavy-weight intermediate mass stars, we conclude that there is a distinct possibility it has a core composed of O and Ne. We also determine that despite the cooling times of the three new white dwarfs in NGC3532 and the previously known degenerate member NGC3532-10 spanning ~90Myr, they all have remarkably similar masses (M~0.9-1Msun). This is fully consistent with the results from our prior work on a heterogeneous sample of ~50 white dwarfs from 12 stellar populations, on the basis of which we argued that the stellar initial mass-final mass relation is less steep at Minit>4Msun than in the adjacent lower initial mass regime. This change in the gradient of the relation could account for the secondary peak observed in the mass distribution of the field white dwarf population and mitigate the need to invoke close binary evolution to explain its existence. Spectroscopic investigation of numerous additional candidate white dwarf members of NGC3532 unearthed by a recent independent study would be useful to confirm (or otherwise) these conclusions.Comment: 8 Figures, 8 tables. Accepted for publication in MNRA

Barriers and solutions to participation in exercise for moderately disabled people with multiple sclerosis not currently exercising: a consensus development study using nominal group technique

Background: Multiple sclerosis (MS) is a chronic, progressive neurological condition. The aim of this study was to explore consensus on the barriers and solutions to exercise for people with MS living in Scotland. Method: Thirty-five people with MS, not regularly exercising, were recruited and took part in five Nominal Group Technique groups throughout Scotland. Background information was collected on participants prior to each group. Participants individually and silently listed their barriers and solutions to participating in exercise. Group discussion then clarified, amended and merged ideas. Participants then ranked ideas by choosing five barriers and solutions to exercise participation. Data were analyzed using descriptive statistics and by carrying out a thematic grouping. Results: Consensus was that fatigue was a barrier to exercise participation . Other identified barriers were a lack of support and advice, the impairments arising from the condition and time. No single item achieved consensus for solutions but exercising with others, receiving support, having a positive attitude, finding time and minimizing environmental barriers were all suggested as solutions to assist in exercise participation. Conclusions: People with MS should be provided with information on how to manage their fatigue alongside any exercise prescription. Information and support should be given on how to personalize exercise to suit individual needs and abilities to overcome some of the barriers suggested within this study. Implications for rehabilitation More exercise opportunities are required. Exercise should be personalized to address the individual needs of the person with MS. Any identified barriers to exercise should be addressed

Reverse graded relaxed buffers for high Ge content SiGe virtual substrates

An innovative approach is proposed for epitaxial growth of high Ge content, relaxed Si1−xGex buffer layers on a Si(001) substrate. The advantages of the technique are demonstrated by growing such structures via chemical vapor deposition and their characterization. Relaxed Ge is first grown on the substrate followed by the reverse grading approach to reach a final buffer composition of 0.78. The optimized buffer structure is only 2.8 µm thick and demonstrates a low surface threading dislocation density of 4×106 cm−2, with a surface roughness of 2.6 nm. The buffers demonstrate a relaxation of up to 107%

Irradiated brown dwarfs

We have observed the post common envelope binary WD0137-349 in the near infrared $J$, $H$ and $K$ bands and have determined that the photometry varies on the system period (116 min). The amplitude of the variability increases with increasing wavelength, indicating that the brown dwarf in the system is likely being irradiated by its 16500 K white dwarf companion. The effect of the (primarily) UV irradiation on the brown dwarf atmosphere is unknown, but it is possible that stratospheric hazes are formed. It is also possible that the brown dwarf (an L-T transition object) itself is variable due to patchy cloud cover. Both these scenarios are discussed, and suggestions for further study are made.Comment: 5 pages, 2 figures. Proceedings from "Brown dwarfs come of age" meeting in Fuerteventura 201

PHL 5038: a spatially resolved white dwarf + brown dwarf binary

A near-infrared excess is detected at the white dwarf PHL 5038 in UKIDSS photometry, consistent with the presence of a cool, substellar companion. We have obtained H- and K-grism spectra and images of PHL 5038 using NIRI on Gemini North. The target is spatially and spectrally resolved into two components: an 8000 K DA white dwarf, and a likely L8 brown dwarf companion, separated by 0.94\arcsec. The spectral type of the secondary was determined using standard spectral indices for late L and T dwarfs. The projected orbital separation of the binary is 55 AU, so it becomes only the second known wide WD+dL binary to be found after GD 165AB. This object could potentially be used as a benchmark for testing substellar evolutionary models at intermediate to older ages