Lichenicidin biosynthesis and search for novel antibacterial peptides

A estirpe Bacillus licheniformis I89 possui a capacidade de produzir alguns compostos com actividade antibacteriana. No presente estudo, a separação desses compostos foi realizada através da aplicação de vários procedimentos, incluindo extracção em fase sólida e cromatografia liquida de alta pressão. Dois destes compostos bioactivos constituem o lantibiótico de classe II lichenicidina e são caracterizados pela massas molecular de 3250 Da (Bliα) e 3020 Da (Bliβ). O cluster responsável pela biossíntese da lichenicidina foi heterologamente expresso em Escherichia coli, constituindo a primeira descrição da produção de um lantibiótico totalmente in vivo num hospedeiro Gram-negativo. Este sistema foi subsequentemente explorado com o objectivo de relacionar cada proteína codificada no cluster genético da lichenicidina na produção dos péptidos Bliα e Bliβ. O desenvolvimento do sistema de trans complementação possibilitou a produção de variantes destes péptidos. A análise das massas moleculares destas variantes assim como a análise dos padrões de fragmentação obtidos por MS/MS permitiu a revisão de algumas das características estruturais previamente proposta para Bliα e Bliβ. A análise dos genes hipoteticamente envolvidos na protecção da estirpe produtora contra a acção antibiótica da lichenicidina revelou, que em E. coli, a sua ausência não resulta no aumento da susceptibilidade a este composto. Verificou-se também que a presença destes genes não é essencial para a produção de lichenicidina em E. coli. Foi também confirmado experimentalmente que a membrana externa da E. coli constitui uma barreira natural para a entrada dos péptidos na célula. De facto, uma das características intrigantes da produção de lichenicidina por uma bactéria de Gram negativo reside no mecanismo de transporte dos dois péptidos através da membrana externa. Neste estudo foi demonstrado que na ausência da proteína de membrana TolC, a massa molecular de Bliα e Bliβ não foi identificada no sobrenadante de E. coli, demonstrando assim que a sua presença no ambiente extra-celular não se devia a um processo de lise bacteriana. Foi ainda avaliada a capacidade da maquinaria biossintética da lichenicidina para produzir o lantibiótico haloduracina, através do processamento de chimeras lichenicidina-haloduracina, contudo, os resultados foram negativos. Verificou-se ainda que em determinadas condições de incubação, a diferenciação da morfologia original da estirpe B. licheniformis I89 pode ocorrer. Esta dissociação implicou a transição da colónia parental e rugosa para uma colónia de aparência mais simples e suave. Desta forma, as diferenças das duas morfologias em termos de taxa de crescimento, esporulação e actividade antibiótica foram investigadas. Considerando especificamente Bliα e Bliβ verificou-se que a abundância destes péptidos nas culturas do fenótipo fino é geralmente inferior aquela identificada nas culturas do fenótipo parental. Por último, a diversidade de elementos genéticos constituintes de péptido sintetases não ribossomais (NRPS) foi investigada em lagoas no centro de Portugal e em solos provenientes de caves do sul de Portugal, revelando a presença de potenciais novas NRPS nestes ambientes.

In search of reliable centimeter-level indoor positioning: a smartphone-based approach

This thesis describes the design and implementation of a reliable centimeter-level indoor positioning system fully compatible with a conventional smartphone. The proposed system takes advantage of the smartphone audio I/O and processing capabilities to perform acoustic ranging in the audio band using non-invasive audio signals and it has been developed having in mind applications that require high accuracy, such as augmented reality, virtual reality, gaming and audio guides. The system works in a distributed operation mode, i.e. each smartphone is able to obtain its own position using only acoustic signals. To support the positioning system, a Wireless Sensor Network (WSN) of synchronized acoustic beacons is used. To keep the infrastructure in sync we have developed an Automatic Time Synchronization and Syntonization (ATSS) protocol with a standard deviation of the sync offset error below 1.25 μs. Using an improved Time Difference of Arrival (TDoA) estimation approach (which takes advantage of the beacon signals’ periodicity) and by performing Non-Line-of-Sight (NLoS) mitigation, we were able to obtain very stable and accurate position estimates with an absolute mean error of less than 10 cm in 95% of the cases and a mean standard deviation of 2.2 cm for a position refresh period of 350 ms.

The SOPHIE search for northern extrasolar planets: X. Detection and characterization of giant planets by the dozen

We present new radial velocity measurements of eight stars that were secured with the spectrograph SOPHIE at the 193 cm telescope of the Haute-Provence Observatory. The measurements allow detecting and characterizing new giant extrasolar planets. The host stars are dwarfs of spectral types between F5 and K0 and magnitudes of between 6.7 and 9.6; the planets have minimum masses Mp sin i of between 0.4 to 3.8 MJup and orbitalperiods of several days to several months. The data allow only single planets to be discovered around the first six stars (HD 143105, HIP 109600, HD 35759, HIP 109384, HD 220842, and HD 12484), but one of them shows the signature of an additional substellar companion in the system. The seventh star, HIP 65407, allows the discovery of two giant planets that orbit just outside the 12:5 resonance in weak mutual interaction. The last star, HD 141399, was already known to host a four-planet system; our additional data and analyses allow new constraints to be set on it. We present Keplerian orbits of all systems, together with dynamical analyses of the two multi-planet systems. HD 143105 is one of the brightest stars known to host a hot Jupiter, which could allow numerous follow-up studies to be conducted even though this is not a transiting system. The giant planets HIP 109600b, HIP 109384b, and HD 141399c are located in the habitable zone of their host star.

An extreme planetary system around HD 219828: one long-period super Jupiter to a hot-Neptune host star

Context. With about 2000 extrasolar planets confirmed, the results show that planetary systems have a whole range of unexpected properties. This wide diversity provides fundamental clues to the processes of planet formation and evolution. Aims: We present a full investigation of the HD 219828 system, a bright metal-rich star for which a hot Neptune has previously been detected. Methods: We used a set of HARPS, SOPHIE, and ELODIE radial velocities to search for the existence of orbiting companions to HD 219828. The spectra were used to characterise the star and its chemical abundances, as well as to check for spurious, activity induced signals. A dynamical analysis is also performed to study the stability of the system and to constrain the orbital parameters and planet masses. Results: We announce the discovery of a long period (P = 13.1 yr) massive (m sini = 15.1 MJup) companion (HD 219828 c) in a very eccentric orbit (e = 0.81). The same data confirms the existence of a hot Neptune, HD 219828 b, with a minimum mass of 21 M⊕ and a period of 3.83 days. The dynamical analysis shows that the system is stable, and that the equilibrium eccentricity of planet b is close to zero. Conclusions: The HD 219828 system is extreme and unique in several aspects. First, ammong all known exoplanet systems it presents an unusually high mass ratio. We also show that systems like HD 219828, with a hot Neptune and a long-period massive companion are more frequent than similar systems with a hot Jupiter instead. This suggests that the formation of hot Neptunes follows a different path than the formation of their hot jovian counterparts. The high mass, long period, and eccentricity of HD 219828 c also make it a good target for Gaia astrometry as well as a potential target for atmospheric characterisation, using direct imaging or high-resolution spectroscopy. Astrometric observations will allow us to derive its real mass and orbital configuration. If a transit of HD 219828 b is detected, we will be able to fully characterise the system, including the relative orbital inclinations. With a clearly known mass, HD 219828 c may become a benchmark object for the range in between giant planets and brown dwarfs.