Modelling and Analysis of Vibrations in a UAV Helicopter with a Vision System

The analysis of the nature and damping of unwanted vibrations on Unmanned Aerial Vehicle (UAV) helicopters are important tasks when images from on‐board vision systems are to be obtained. In this article, the authors model a UAV system, generate a range of vibrations originating in the main rotor and design a control methodology in order to damp these vibrations. The UAV is modelled using VehicleSim, the vibrations that appear on the fuselage are analysed to study their effects on the on‐board vision system by using Simmechanics software. Following this, the authors present a control method based on an Adaptive Neuro‐Fuzzy Inference System (ANFIS) to achieve satisfactory damping results over the vision system on board

Non-lethal elephant-population-control methods: summary of the first ESAG workshop

Management interventions are necessary to control elephant numbers within fenced wildlife reserves in South Africa. Use of non-lethal control methods is increasing, but information about their suitability and effects are not widely available. Three such methods are currently available; immunocontraception with Porcine Zona Pellucida (PZP) vaccine, vasectomy, and Gonadotropin Releasing Hormone (GnRH) vaccine. Here we consolidate what we know about these methods, using published sources and material shared at a workshop held in South Africa in 2016, in order to provide up-to-date information for future policy decisions concerning the use of these methods in South Africa and elsewhere

Two compact HII regions at the remote outskirts of the Magellanic Clouds

The H II regions LMC N191 and SMC N77 are among the outermost massive star-forming regions in the Magellanic Clouds. So far, few works have dealt with these objects despite their interesting characteristics. We aim at studying various physical properties of these objects regarding their morphology (in the optical and Spitzer IRAC wavelengths), ionized gas emission, nebular chemical abundances, exciting sources, stellar content, age, presence or absence of young stellar objects, etc. This study is based mainly on optical ESO NTT observations, both imaging and spectroscopy, coupled with other archive data, notably Spitzer images (IRAC 3.6, 4.5, 5.8, and 8.0 microns) and 2MASS observations. We show the presence of two compact H II regions, a low-excitation blob (LEB) named LMC N191A and a high-excitation blob (HEB) named SMC N77A, and study their properties and those of their exciting massive stars as far as spectral type and mass are concerned. We also analyze the environmental stellar populations and determine their evolutionary stages. Based on Spitzer IRAC data, we characterize the YSO candidates detected in the direction of these regions. Massive star formation is going on in these young regions with protostars of mass about 10 and 20 M_sun in the process of formation.Comment: 14 pages, 8 figures, 6 tables; Accepted for publication in A&A. arXiv admin note: substantial text overlap with arXiv:1102.125

La Mulata in the Spanish Caribbean From Stage to Films Lecture by Yesenia Fernández Selier

In the last decades, several scholars have analyzed the semiotics of La Mulata\u27s ubiquitous presence in Cuban popular culture. Those visual and literary analyses have centered on the Island\u27s national production, leaving aside transnational renditions. Yet the icon of La Mulata traveled with the exile of Cuban minstrel theater after 1869 to Mexico and Puerto Rico, among other circum-Caribbean nations, adopting local themes and slang. La Mulata was already recognizable in Latin American popular culture by the 1920s and gained new levels of dissemination with the development of Latin American cinema. This lecture will partially map out the itinerary of La Mulata avatar in Latin American films and contemporary cultural practices. It will pay close attention to the intersection of the performers\u27race and the scenic discourses they enact, theorizing the functions of this translation and analyzing the relevance of the repertoire of La Mulata in today\u27s Latino visual and popular culture. Yesenia Fernandez Selier is a Cuban-born performer and researcher. She is currently a Ph.D. candidate in Media, Culture, and Communication at New York University. She also holds an M.A. in Latin American Studies from New York University and a B.A. in Psychology from the University of Havana. She has received fellowships from CLACSO, the CUNY Caribbean Exchange Program, and the Cuban Heritage Collection of the University of Miami Libraries. Her work on Afro-Cuban culture, encompassing dance, music, race, and identity has been published in Cuba, the United States, and Brazil. She is a recipient of the 2017 Dfaz-Ayala LibraryTravel Grants at FIU. View Part 1 and 2 of lecture here: http://digitalcommons.fiu.edu/crivideo/69/ http://digitalcommons.fiu.edu/crivideo/68/https://digitalcommons.fiu.edu/cri_events/1337/thumbnail.jp

The nature of the high Galactic latitude O-star HD93521: new results from X-ray and optical spectroscopy

Owing to its unusual location and its isolation, the nature of the high Galactic latitude O9.5Vp object HD93521 is still uncertain. We have collected X-ray and optical observations to characterize the star and its surroundings. X-ray images and spectra are analyzed to search for traces of a recent star formation event around HD93521 and to search for the signature of a possible compact companion. Optical echelle spectra are analysed with plane-parallel model atmosphere codes, assuming either a spherical star or a gravity darkened rotationally flattened star, to infer the effective temperature and surface gravity, and to derive the He, C, N and O abundances of HD93521. The X-ray images reveal no traces of a population of young low-mass stars coeval with HD93521. The X-ray spectrum of HD93521 is consistent with a normal late O-type star although with subsolar metallicity. No trace of a compact companion is found in the X-ray data. In the optical spectrum, He and N are found to be overabundant, in line with the effect of rotational mixing in this very fast rotator, whilst C and O are subsolar. A critical comparison with the properties of subdwarf OB stars, indicates that, despite some apparent similarities, HD93521 does not belong to this category. Despite some ambiguities on the runaway status of the star, the most likely explanation is that HD93521 is a Population I massive O-type star that was ejected from the Galactic plane either through dynamical interactions or a result of a supernova event in a binary system.Comment: Accepted for publication in Astronomy & Astrophysic

The VLT-FLAMES Tarantula Survey IV: Candidates for isolated high-mass star formation in 30 Doradus

Whether massive stars can occasionally form in relative isolation or if they require a large cluster of lower-mass stars around them is a key test in the differentiation of star formation theories as well as how the initial mass function of stars is sampled. Previous attempts to find O-type stars that formed in isolation were hindered by the possibility that such stars are merely runaways from clusters, i.e., their current isolation does not reflect their birth conditions. We introduce a new method to find O-type stars that are not affected by such a degeneracy. Using the VLT-FLAMES Tarantula Survey and additional high resolution imaging we have identified stars that satisfy the following constraints: 1) they are O-type stars that are not detected to be part of a binary system based on RV time series analysis; 2) they are designated spectral type O7 or earlier ; 3) their velocities are within 1\sigma of the mean of OB-type stars in the 30 Doradus region, i.e. they are not runaways along our line-of-sight; 4) the projected surface density of stars does not increase within 3 pc towards the O-star (no evidence for clusters); 5) their sight lines are associated with gaseous and/or dusty filaments in the ISM, and 6) if a second candidate is found in the direction of the same filament with which the target is associated, both are required to have similar velocities. With these criteria, we have identified 15 stars in the 30 Doradus region, which are strong candidates for being high-mass stars that have formed in isolation. Additionally, we employed extensive MC stellar cluster simulations to confirm that our results rule out the presence of clusters around the candidates. Eleven of these are classified as Vz stars, possibly associated with the zero-age main sequence. We include a newly discovered W-R star as a candidate, although it does not meet all of the above criteria.Comment: 14 pages, 13 figures, 5 tables; Accepted for publication by A&

An interesting candidate for isolated massive star formation in the Small Magellanic Cloud

The region of the Small Magellanic Cloud (SMC) with which this paper is concerned contains the highest concentration of IRAS/Spitzer sources, H I emission, and molecular clouds in this neighboring galaxy. However very few studies have been devoted to it, despite these signs of star formation. We present the first detailed study of the compact H II region N33 in the SMC by placing it in a wider context of massive star formation. Moreover, we show that N33 is a particularly interesting candidate for isolated massive star formation. This analysis is based mainly on optical ESO NTT observations, both imaging and spectroscopy, coupled with other archive data, notably Spitzer images (IRAC 3.6, 4.5, 5.8, and 8.0 mic) and 2MASS observations. We derive a number of physical characteristics of the compact H II region N33 for the first time. This gas and dust formation of 7".4 (2.2 pc) in diameter is powered by a massive star of spectral type O6.5-O7 V. The compact H II region belongs to a rare class of H II regions in the Magellanic Clouds, called high-excitation blobs (HEBs). We show that this H II region is not related to any star cluster. Specifically, we do not find any traces of clustering around N33 on scales larger than 10" (~ 3 pc). On smaller scales, there is a marginal stellar concentration, the low density of which, below the 3 sigma level, does not classify it as a real cluster. We also verify that N33 is not a member of any large stellar association. Under these circumstances, N33 is also therefore attractive because it represents a remarkable case of isolated massive-star formation in the SMC. Various aspects of the relevance of N33 to the topic of massive-star formation in isolation are discussed.Comment: 17 pages, 9 figures, 5 tables; Accepted for publication in A&

The social structure, distribution and demographic status of the African elephant population in the Central Limpopo River Valley of Botswana, Zimbabwe and South Africa

The Central Limpopo River Valley elephant population is a cross border population on which very little scientific data pertaining to numbers, distribution and demographic status is available. The total range was determined using published literature, reports, postal questionnaires and interviews. Numbers and dry season distribution were determined by means of three total aerial counts in 2000, 2001 and 2004 of the sections of the total range in which elephants were reported. Totals of 1388, 1424 and 1339 were recorded with the highest numbers in all counts in the Botswana section of the study area. Four sub groups within the population were identified. Human settlements and the distribution of rivers and fencing appeared to be the major factors influencing distribution and movement. The population is highly mobile within the total range, and numbers fluctuate markedly in any given section, but numbers in the total range appear to have been increasing slowly at below 2% per annum and the range expanding slightly over the last 30 years. Additional range is being provided by the creation of a Trans Frontier Conservation Area. Movements were determined through ground observations within the study area and seem to follow the major rivers namely the Shashe, Ramokgwabane, Simukwe, Shashani, Tuli, Umzingwane and Limpopo rivers. The social and demographic status of the population was determined through ground observations as well as total aerial counts conducted within the Northern Tuli Game Reserve from 1976 to 2004. The study has shown that group sizes increase with an increase in rainfall (average mean group size of 56.524, SDE 77.388) and decrease during low rainfall periods (mean group size of 24.157, SDE 22.223). The age structure was determined from aerial photographs during August 2000 and showed a high percentage of adults and sub adults, with infants estimated at 3%. The approximate birth rate (1.5%) calculated for 2000 is balanced by an average natural mortality determined between 1999 and 2004 of 1.8%. The inter calf interval determined from known herds observed in the Northern Tuli Game Reserve was estimated at 3.94% and suggests that the long-term birth rate for the population should be higher than that for the year 2000. The difference between the combined natural and human induced mortality rates (~4%) and the birth rate suggested by the age structure and the inter calf interval (~6%) gives the ~2% long-term increase observed in the numbers. Human elephant interactions within the study area were determined through published literature and interviews with local residents. Elephants and humans interact in both a positive and negative manor and interactions are related to human land use practices within the area. Elephants were indicated as the major problem animal in farming areas, but the major draw card within tourism operations.Dissertation (MSc (Wildlife Management))--University of Pretoria, 2008.Animal and Wildlife Sciencesunrestricte

Discovery of a parsec-scale bipolar nebula around MWC 349A

We report the discovery of a bipolar nebula around the peculiar emission-line star MWC 349A using archival Spitzer Space Telescope 24 um data. The nebula extends over several arcminutes (up to 5 pc) and has the same orientation and geometry as the well-known subarcsecond-scale (~400 times smaller) bipolar radio nebula associated with this star. We discuss the physical relationship between MWC 349A and the nearby B0 III star MWC 349B and propose that both stars were members of a hierarchical triple system, which was ejected from the core of the Cyg OB2 association several Myr ago and recently was dissolved into a binary system (now MWC 349A) and a single unbound star (MWC 349B). Our proposal implies that MWC 349A is an evolved massive star (likely a luminous blue variable) in a binary system with a low-mass star. A possible origin of the bipolar nebula around MWC 349A is discussed.Comment: 9 pages, 6 figures, accepted for publication in A&