Early-type stars observed in the ESO UVES Paranal observatory project - IV. studies of CN, CH+ and CH in the interstellar medium

High spectral resolution (~80 000) and signal-to-noise observations from the Ultraviolet and Visual Echelle Spectrograph Paranal Observatory Project (UVES-POP) are used to study the interstellarmolecular lines CN (3874 Å), CH⁺ (3957, 4232 Å) and CH (3886, 4300 Å) towards 74 O- and B-type stellar sightlines. Additionally, archive data are presented for 140 ELODIE early-type stellar sightlines at R = 42 000, plus 25 FEROS at R = 48 000 and 3 UVES at R > 50 000, mainly in the CH⁺ (4232 Å) and CH (3886, 4300 Å) transitions. Detection rates are ~45 per cent for CN and ~67 per cent for the other lines in the POP sample, and ~10-15 per cent for CH⁺ and CH lines in the additional sample. CH and CH⁺ are well correlated between log[N(CH) cm^-2]~12-14, implying that these clouds are CH⁺-like CH and not CN-like CH. CH is also very well correlated with Na I D in the range log[N(Na I cm^-2]) ~12.2-14.2. A few sightlines show tentative velocity shifts of ~2 km s^-1 between CH and CH⁺, which appear to be caused by differences in component strength in blends, and hence do not provide firm evidence for shocks. Finally, we describe a search for ¹³CH⁺ in a sightline towards HD 76341. No ¹³CH⁺ is detected, placing a limit on the ¹³CH⁺ to ¹²CH⁺ ratio of ~0.01. If a formal fit is attempted, the equivalent width ratio in the two isotopes is a factor ~90 but with large errors. 

Massive stars exploding in a He-rich circumstellar medium - V. Observations of the slow-evolving SN Ibn OGLE-2012-SN-006

We present optical observations of the peculiar Type Ibn supernova (SN Ibn) OGLE-2012-SN-006, discovered and monitored by the Optical Gravitational Lensing Experiment-IV survey, and spectroscopically followed by Public ESO Spectroscopic Survey of Transient Objects (PESSTO) at late phases. Stringent pre-discovery limits constrain the explosion epoch with fair precision to JD = 245 6203.8 +/- 4.0. The rise time to the I-band light-curve maximum is about two weeks. The object reaches the peak absolute magnitude M-I = -19.65 +/- 0.19 on JD = 245 6218.1 +/- 1.8. After maximum, the light curve declines for about 25 d with a rate of 4 mag (100 d)(-1). The symmetric I-band peak resembles that of canonical Type Ib/c supernovae (SNe), whereas SNe Ibn usually exhibit asymmetric and narrower early-time light curves. Since 25 d past maximum, the light curve flattens with a decline rate slower than that of the Co-56-Fe-56 decay, although at very late phases it steepens to approach that rate. However, other observables suggest that the match with the Co-56 decay rate is a mere coincidence, and the radioactive decay is not the main mechanism powering the light curve of OGLE-2012-SN-006. An early-time spectrum is dominated by a blue continuum, with only a marginal evidence for the presence of He I lines marking this SN type. This spectrum shows broad absorptions bluewards than 5000 angstrom, likely O II lines, which are similar to spectral features observed in superluminous SNe at early epochs. The object has been spectroscopically monitored by PESSTO from 90 to 180 d after peak, and these spectra show the typical features observed in a number of SN 2006jc-like events, including a blue spectral energy distribution and prominent and narrow (v(FWHM) approximate to 1900 km s(-1)) He I emission lines. This suggests that the ejecta are interacting with He-rich circumstellar material. The detection of broad (10(4) km s(-1)) O I and Ca II features likely produced in the SN ejecta (including the [OI] lambda lambda 6300,6364 doublet in the latest spectra) lends support to the interpretation of OGLE-2012-SN-006 as a core-collapse event.

Massive stars exploding in a He-rich circumstellar medium - IV. Transitional Type Ibn supernovae

We present ultraviolet, optical and near-infrared data of the Type Ibn supernovae (SNe) 2010al and 2011hw. SN 2010al reaches an absolute magnitude at peak of M-R = -18.86 +/- 0.21. Its early light curve shows similarities with normal SNe Ib, with a rise to maximum slower than most SNe Ibn. The spectra are dominated by a blue continuum at early stages, with narrow P-Cygni He I lines indicating the presence of a slow-moving, He-rich circumstellar medium. At later epochs, the spectra well match those of the prototypical SN Ibn 2006jc, although the broader lines suggest that a significant amount of He was still present in the stellar envelope at the time of the explosion. SN 2011hw is somewhat different. It was discovered after the first maximum, but the light curve shows a double peak. The absolute magnitude at discovery is similar to that of the second peak (M-R = -18.59 +/- 0.25), and slightly fainter than the average of SNe Ibn. Though the spectra of SN 2011hw are similar to those of SN 2006jc, coronal lines and narrow Balmer lines are clearly detected. This indicates substantial interaction of the SN ejecta with He-rich, but not H-free, circumstellar material. The spectra of SN 2011hw suggest that it is a transitional SN Ibn/IIn event similar to SN 2005la. While for SN 2010al the spectrophotometric evolution favours a H-deprived Wolf-Rayet progenitor (of WN-type), we agree with the conclusion of Smith et al. that the precursor of SN 2011hw was likely in transition from a luminous blue variable to an early Wolf-Rayet (Ofpe/WN9) stage.

Selecting superluminous supernovae in faint galaxies from the first year of the Pan-STARRS1 Medium Deep Survey

The Pan-STARRS1 (PS1) survey has obtained imaging in five bands (grizyP1) over 10 Medium Deep Survey (MDS) fields covering a total of 70 square degrees. This paper describes the search for apparently hostless supernovae (SNe) within the first year of PS1 MDS data with an aim of discovering superluminous supernovae (SLSNe). A total of 249 hostless transients were discovered down to a limiting magnitude of MAB ∼ 23.5, of which 76 were classified as Type Ia supernovae (SNe Ia). There were 57 SNe with complete light curves that are likely core-collapse SNe (CCSNe) or type Ic SLSNe and 12 of these have had spectra taken. Of these 12 hostless, non-Type Ia SNe, 7 were SLSNe of type Ic at redshifts between 0.5 and 1.4. This illustrates that the discovery rate of type Ic SLSNe can be maximized by concentrating on hostless transients and removing normal SNe Ia. We present data for two possible SLSNe; PS1-10pm (z = 1.206) and PS1-10ahf (z = 1.1), and estimate the rate of type Ic SLSNe to be between 3+3−2×10−53+3−2×10−53+3−2×10−5 and 8+2−1×10−58+2−1×10−58+2−1×10−5 that of the CCSN rate within 0.3 ≤ z ≤ 1.4 by applying a Monte Carlo technique. The rate of slowly evolving, type Ic SLSNe (such as SN2007bi) is estimated as a factor of 10 lower than this range.

Selection of burst-like transients and stochastic variables using multi-brand image differencing in the Pan-STARRS1 Medium Deep Survey

We present a novel method for the light-curve characterization of Pan-STARRS1 Medium Deep Survey (PS1 MDS) extragalactic sources into stochastic variables (SVs) and burst-like (BL) transients, using multi-band image-differencing time-series data. We select detections in difference images associated with galaxy hosts using a star/galaxy catalog extracted from the deep PS1 MDS stacked images, and adopt a maximum a posteriori formulation to model their difference-flux time-series in four Pan-STARRS1 photometric bands gP1, rP1, iP1, and zP1. We use three deterministic light-curve models to fit BL transients; a Gaussian, a Gamma distribution, and an analytic supernova (SN) model, and one stochastic light-curve model, the Ornstein-Uhlenbeck process, in order to fit variability that is characteristic of active galactic nuclei (AGNs). We assess the quality of fit of the models band-wise and source-wise, using their estimated leave-out-one cross-validation likelihoods and corrected Akaike information criteria. We then apply a K-means clustering algorithm on these statistics, to determine the source classification in each band. The final source classification is derived as a combination of the individual filter classifications, resulting in two measures of classification quality, from the averages across the photometric filters of (1) the classifications determined from the closest K-means cluster centers, and (2) the square distances from the clustering centers in the K-means clustering spaces. For a verification set of AGNs and SNe, we show that SV and BL occupy distinct regions in the plane constituted by these measures. We use our clustering method to characterize 4361 extragalactic image difference detected sources, in the first 2.5 yr of the PS1 MDS, into 1529 BL, and 2262 SV, with a purity of 95.00% for AGNs, and 90.97% for SN based on our verification sets. We combine our light-curve classifications with their nuclear or off-nuclear host galaxy offsets, to define a robust photometric sample of 1233 AGNs and 812 SNe. With these two samples, we characterize their variability and host galaxy properties, and identify simple photometric priors that would enable their real-time identification in future wide-field synoptic surveys.

SN2012ca: a stripped envelope core-collapse SN interacting with dense circumstellar medium

We report optical and near-infrared observations of SN2012ca with the Public ESO Spectroscopy Survey of Transient Objects (PESSTO), spread over one year since discovery. The supernova (SN) bears many similarities to SN1997cy and to other events classified as Type IIn but which have been suggested to have a thermonuclear origin with narrow hydrogen lines produced when the ejecta impact a hydrogen-rich circumstellar medium (CSM). Our analysis, especially in the nebular phase, reveals the presence of oxygen, magnesium and carbon features. This suggests a core-collapse explanation for SN2012ca, in contrast to the thermonuclear interpretation proposed for some members of this group. We suggest that the data can be explained with a hydrogen- and helium-deficient SN ejecta (Type I) interacting with a hydrogen-rich CSM, but that the explosion was more likely a Type Ic core-collapse explosion than a Type Ia thermonuclear one. This suggests that two channels (both thermonuclear and stripped envelope core-collapse) may be responsible for these SN 1997cy-like events.

Ultraluminous Supernovae as a New Probe of the Interstellar Medium in Distant Galaxies

We present the Pan-STARRS1 discovery and light curves, and follow-up MMT and Gemini spectroscopy of an ultraluminous supernova (ULSN; dubbed PS1-11bam) at a redshift of z = 1.566 with a peak brightness of M UV ≈ -22.3 mag. PS1-11bam is one of the highest redshift spectroscopically confirmed SNe known to date. The spectrum exhibits broad absorption features typical of previous ULSNe (e.g., C II, Si III), and strong and narrow Mg II and Fe II absorption lines from the interstellar medium (ISM) of the host galaxy, confirmed by an [O II]λ3727 emission line at the same redshift. The equivalent widths of the Fe II λ2600 and Mg II λ2803 lines are in the top quartile of the quasar intervening absorption system distribution, but are weaker than those of gamma-ray burst intrinsic absorbers (i.e., GRB host galaxies). We also detect the host galaxy in pre-explosion Pan-STARRS1 data and find that its UV spectral energy distribution is best fit with a young stellar population age of τ* ≈ 15-45 Myr and a stellar mass of M * ≈ (1.1-2.6) × 109 M ⊙ (for Z = 0.05-1 Z ⊙). The star formation rate inferred from the UV continuum and [O II]λ3727 emission line is ≈10 M ⊙ yr-1, higher than in previous ULSN hosts. PS1-11bam provides the first direct demonstration that ULSNe can serve as probes of the ISM in distant galaxies. The depth and red sensitivity of PS1 are uniquely suited to finding such events at cosmologically interesting redshifts (z ~ 1-2); the future combination of LSST and 30 m class telescopes promises to extend this technique to z ~ 4.

A Pilot Study of Reciprocal Peer Tutoring in Irish Medium Schools

A pilot study to investigate the effects of mathematics peer tutoring in Irish medium primary schools was undertaken. Five schools and 90 students took part in the pilot. Materials and resources that had previously been shown to work in English medium Scottish schools were translated into Irish by CCEA. Irish medium teachers attended three professional development days. Teachers implemented the peer tutoring techniques during mathematics lessons during a period of 16 weeks. Changes in attainment were measures with an Irish translation of the Scottish Survey of Achievement Mathematics Test. Results were positive. Student attainment was significantly raised during the 16-week implementation period by over one standard deviation. This equated to one-year’s worth of mathematics development during this time period. Results must be treated with caution. No control group was used in the pilot study. However, results are very promising and indicate that reciprocal role peer tutoring may be a useful pedagogy in Irish medium education. Further work would be required to establish this definitively.

Growing Up On an Interface: Findings and Implications for the Social Needs, Mental Health and Lifetime Opportunities of Belfast Youth

In this research we aimed to find out what types of risk (if any) affected young people and children growing up in places of high religious segregation or what we normally call interface communities. This is important as we know that risk and experiences of harm and violence can have negative impacts upon development, emotional well-being and future prospects. It is important to understand what types of risk affect young people and children so as we can respond to these in terms of aiding better personal and community development with regard to health, work, education and wider opportunities.

Development of sialons colloidally processed in aqueous medium

Desenvolveu-se um novo método de processamento coloidal em meio aquoso para consolidar cerâmicos de α-Y-SiAlON, os quais foram sinterizados por prensagem isostática a quente (HIP) e por spark plasma sintering (SPS). Preparou-se com sucesso uma suspensão aquosa de pós precursores de YSiAlON (Si3N4, Al2O3, Y2O3 e AlN), temporariamente estável, usando Dolapix PC21 como dispersante, permitindo a fabricação de pós granulados pela técnica de aspersão-congelamento-liofilização e a consolidação de corpos em verde por enchimento por barbotina. Avaliou-se o efeito do excesso de oxigénio introduzido pelo processamento aquoso no desenvolvimento microestrutural e nas propriedades mecânicas. Os corpos de Y-SiAlON consolidados por enchimento por barbotina e sinterizados por HIP a 1800ºC apresentaram microestruturas e propriedades mecânicas similares a corpos consolidados por prensagem a seco. Estes materiais exibiram densificação completa, dureza Vickers máxima de 2003 e tenacidade à fractura (método SEVNB) máxima de 5.20 MPam1/2. Foi ainda possível estabelecer uma relação estreita entre o aumento do conteúdo em oxigénio das amostras sinterizadas e a diminuição da tenacidade à fractura. Na tentativa de melhorar a tenacidade à fractura dos materiais, procedeu-se à incorporação nas suspensões de sementes de Ca-α-SiAlON de geometria alongada produzidas por síntese por combustão, adicionadas como agentes de reforço. A síntese por combustão realizada em larga escala (cargas até 1 kg) não produziu efeitos negativos óbvios nos produtos da reacção. Investigara-se os efeitos da adição de 5 % em peso de sementes nas propriedades mecânicas e no desenvolvimento microestrutural de amostras densificadas por HIP. Em comparação com os materiais sem sementes, a tenacidade à fractura (método SEVNB) aumentou 13%, mas a dureza Vickers resultou 14,5% inferior. A sinterização por SPS permitiu obter densificação completa a temperaturas tão baixas como 1600ºC a partir dos pós granulados de Y-SiAlON sem a adição extra de Y2O3 para aumentar o teor de fase líquida. Os materiais sinterizados a 1700ºC e 1600ºC mostraram valores máximos de tenacidade à fractura de 4.36 e 4.20 MPam1/2 (método SEVNB), e de dureza Vickers de 2089 e 2084, respectivamente. Esta técnica de sinterização permitiu ainda obter corpos sinterizados translúcidos com uma transmitância máxima de 61% numa amostra de 2mm de espessura. Os corpos translúcidos apresentaram dureza Vickers de 2154 e tenacidade à fractura 3.74 MPam1/2 (método SEVNB).

Sensores de Bragg para bioaplicações

Nas últimas décadas, os sensores de Bragg têm sido frequentemente utilizados em inúmeras aplicações, em resultado das características únicas desta tecnologia. Contudo, a comunidade científica tem feito um esforço contínuo em desenvolver sensores que respondam tanto quanto possível aos requisitos e interesses de cada aplicação em particular. As bioaplicações são um campo de crescente interesse pelos sensores de Bragg, atendendo à heterogeneidade e complexidade dos meios de análise em questão. No âmbito desta dissertação foi realizada uma análise teórica dos princípios de funcionamento das redes de Bragg, focada em redes uniformes e inclinadas. Foi também descrito o processo de produção de redes de Bragg regeneradas. Redes de Bragg uniformes foram aplicadas na caracterização da reacção de polimerização e cura de materiais dentários, nomeadamente resina para base de dentadura, cimentos e gessos. Foi feita uma análise comparativa do desempenho de diferentes tipos de cimentos e gessos. Em relação ao gesso foi ainda avaliada a influência do rácio água/pó nas propriedades do material. Devido à importância que o índice de refracção tem na detecção de substâncias, doenças e controlo de qualidade de produtos, foi desenvolvido um sensor de índice de refracção baseado numa rede de Bragg inclinada. Implementaram-se também sensores para medição simultânea de índice de refracção e deformação, índice de refracção e temperatura e índice de refracção, deformação e temperatura, todos baseados numa única rede inclinada. O último dispositivo foi validado em ambiente laboratorial. Com o propósito de desenvolver um sensor baseado em redes de Bragg para monitorização da deformação óssea, foi avaliada a biocompatibilidade da fibra óptica em cultura de células osteoblásticas, e analisada a integridade física e funcionalidade da rede de Bragg nesse meio. O interesse em aumentar a sensibilidade e alargar a gama de trabalho dos sensores conduziu ao revestimento das fibras ópticas. Atendendo ao potencial índole biológica e biomédica do trabalho, usou-se como material de recobrimento o diamante, dada a excelente resposta em termos de biocompatibilidade, resistência à corrosão, não toxicidade e afinidade para espécies químicas e biológicas. Os filmes foram obtidos por deposição química a partir da fase vapor assistida por filamento quente. Para além de amostras de fibra óptica, foram revestidas redes de Bragg uniformes e regeneradas. Os sensores revestidos com diamante foram caracterizados à deformação e à temperatura.