Automating the Surveillance of Mosquito Vectors from Trapped Specimens Using Computer Vision Techniques

Among all animals, mosquitoes are responsible for the most deaths worldwide. Interestingly, not all types of mosquitoes spread diseases, but rather, a select few alone are competent enough to do so. In the case of any disease outbreak, an important first step is surveillance of vectors (i.e., those mosquitoes capable of spreading diseases). To do this today, public health workers lay several mosquito traps in the area of interest. Hundreds of mosquitoes will get trapped. Naturally, among these hundreds, taxonomists have to identify only the vectors to gauge their density. This process today is manual, requires complex expertise/ training, and is based on visual inspection of each trapped specimen under a microscope. It is long, stressful and self-limiting. This paper presents an innovative solution to this problem. Our technique assumes the presence of an embedded camera (similar to those in smart-phones) that can take pictures of trapped mosquitoes. Our techniques proposed here will then process these images to automatically classify the genus and species type. Our CNN model based on Inception-ResNet V2 and Transfer Learning yielded an overall accuracy of 80% in classifying mosquitoes when trained on 25,867 images of 250 trapped mosquito vector specimens captured via many smart-phone cameras. In particular, the accuracy of our model in classifying Aedes aegypti and Anopheles stephensi mosquitoes (both of which are deadly vectors) is amongst the highest. We present important lessons learned and practical impact of our techniques towards the end of the paper

Kinematics of Nearby Subdwarf Stars

We present an analysis of the space motions of 742 subdwarf stars based on the sample of Carney et al. (1994, CLLA). Hipparcos parallaxes, TYC2+HIP proper motions and Tycho2 proper motions were combined with radial velocities and metallicities from CLLA. The kinematical behavior is discussed in particular in relation to their metallicities. The majority of these sample stars have metal abundances of [Fe/H] >-1 and represent the thick disk population. The halo component, with [Fe/H] <-1.6, is characterized by a low mean rotation velocity and a radially elongated velocity ellipsoid. In the intermediate metallicity range (-1.6 < [Fe/H] <-1), we find a significant number of subdwarfs with disklike kinematics. We interpret this population of stars as a metal-weak thick disk population.Comment: 6 pages, 7 figures, accepted by Astronomy & Astrophysic

The Many Faces of Risk: A Qualitative Study of Risk in Outpatient Involuntary Treatment.

Objective: This study aimed to derive a conceptualisation of risk in outpatient involuntary psychiatric treatment that has utility and meaning for stakeholders. Methods: Thirty-eight participants –patients, caregivers, clinicians and legal decision makers – participated in qualitative interviews about their experiences of outpatient involuntary psychiatric treatment. Interview data was analysed using a general inductive method. Results: Six types of risk were identified: ‘actual harm’, ‘social adversity’, ‘therapeutic outcome/compromised treatment’, ‘the system’, ‘interpersonal distress’, and ‘epistemic’. There were overlaps between the discourses on risk, but variation in how different aspects of risk were emphasised. Conclusions: Based on the findings, a comprehensive model of “risk” contextualized to outpatient involuntary treatment is proposed. It incorporates the domains of “risk of harm to self or others”; “risk of social adversity”; “risk of excess distress”; and, “risk of compromised treatment”. This model may have instrumental value in the implementation and the scrutiny of risk-based mental health laws.funded by a discretionary grant from the Mental Health, Drug and Alcohol Office of NSW Healt

The lived experience of involuntary community treatment: a qualitative study of mental health consumers and carers

Objective: To describe the lived experiences of people subject to community treatment orders (CTOs) and their carers. Method: We recruited 11 participants (five mental health consumers and six carers) through consumer and carer networks in NSW, Australia, to take part in interviews about their experiences. We analysed the interview data set using established qualitative methodologies. Results: The lived experiences were characterised by ‘access’ concerns, ‘isolation’, ‘loss and trauma’, ‘resistance and resignation’ and ‘vulnerability and distress’. The extent and impact of these experiences related to the severity of mental illness, the support available for people with mental illnesses and their carers, the social compromises associated with living with mental illness, and the challenges of managing the relationships necessitated by these processes. Conclusions: The lived experience of CTOs is complex: it is one of distress and profound ambivalence. The distress is an intrinsic aspect of the experience of severe mental illness, but it also emerges from communication gaps, difficulty obtaining optimal care and accessing mental health services. The ambivalence arises from an acknowledgement that while CTOs are coercive and constrain autonomy, they may also be beneficial. These findings can inform improvements to the implementation of CTOs and the consequent experiences. Keywords: carer, community treatment order, interview, involuntary treatment, mental health, patient experience, qualitative researchsupported by the Mental Health, Drug and Alcohol Office (MHDAO) of NSW Health of Australia

An Overview of the Rotational Behavior of Metal--Poor Stars

The present paper describes the behavior of the rotational velocity in metal--poor stars ([Fe/H]<-0.5 dex) in different evolutionary stages, based on Vsini values from the literature. Our sample is comprised of stars in the field and some Galactic globular clusters, including stars on the main sequence, the red giant branch (RGB), and the horizontal branch (HB). The metal--poor stars are, mainly, slow rotators, and their Vsini distribution along the HR diagram is quite homogeneous. Nevertheless, a few moderate to high values of Vsini are found in stars located on the main sequence and on the HB. We show that the overall distribution of Vsini values is basically independent of metallicity for the stars in our sample. In particular, the fast-rotating main sequence stars in our sample present similar rotation rates as their metal-rich counterparts, suggesting that some of them may actually be fairly young, in spite of their low metallicity, or else that at least some of them would be better classified as blue straggler stars. We do not find significant evidence of evolution in Vsini values as a function of position on the RGB; in particular, we do not confirm previous suggestions that stars close to the RGB tip rotate faster than their less evolved counterparts. While the presence of fast rotators among moderately cool blue HB stars has been suggested to be due to angular momentum transport from a stellar core that has retained significant angular momentum during its prior evolution, we find that any such transport mechanisms must likely operate very fast as the star arrives on the zero-age HB (ZAHB), since we do not find a link between evolution off the ZAHB and Vsini values. We present an extensive tabulation of all quantities discussed in this paper, including rotation velocities, temperatures, gravitieComment: 22 pages, 10 figure

A new species of the fish louse genus Dipteropeltis Calman, 1912 (Crustacea: Branchiura) from Peru

Dipteropeltis es un género poco descrito de piojo de los peces endémico de Sudamérica. En una pequeña región de aguas negras en Loreto, Perú, se observaron y recolectaron 13 especímenes adultos y juveniles de una especie no identificada de Dipteropeltis Calman, 1912, así como un espécimen adulto de D. hirundo Calman, 1912. Se adquirieron micrografías electrónicas y ópticas de barrido para examinar y medir características clave de estos especímenes. Las diferencias morfológicas con las dos especies conocidas de Dipteropeltis, D. hirundo y D. Dipteropeltis Neethling et al., 2014, indican que los especímenes recogidos representan una nueva especie. Dipteropeltis longicaudatus sp. nov. se distingue por sus lóbulos abdominales alargados, un caparazón en forma de cresta y unos maxilares de forma única. Un espécimen representa el branquiuro más largo documentado hasta la fecha, con 31,5 mm. Además, se proporcionan los primeros datos de secuencia para este género utilizando códigos de barras de ADN, lo que corrobora la designación de una nueva especie. También se grabaron vídeos que documentan comportamientos como la fijación al hospedero, la pulsación de los lóbulos abdominales, el "desplazamiento" del disco de succión y la natación. Los hallazgos tienen implicaciones para sus hospederos teleósteos, Triportheus albus Cope, 1872 y Brycon amazonicus Spix & Agassiz, 1829, siendo este último una especie crítica para la acuicultura y la pesca comercial en la Amazonia.Revisión por pares

V474 Car: A Rare Halo RS CVn Binary in Retrograde Galactic Orbit

We report the discovery that the star V474 Car is an extremely active, high velocity halo RS CVn system. The star was originally identified as a possible pre-main sequence star in Carina, given its enhanced stellar activity, rapid rotation (10.3 days), enhanced Li, and absolute magnitude that places it above the main sequence. However, its extreme radial velocity (264 km s$^{-1}$) suggested that this system was unlike any previously known pre-MS system. Our detailed spectroscopic analysis of echelle spectra taken with the CTIO 4-m finds that V474 Car is both a spectroscopic binary with orbital period similar to the photometric rotation period, and metal poor ([Fe/H] $\simeq -$0.99). The star's Galactic orbit is extremely eccentric (e $\simeq$ 0.93) with perigalacticon of only $\sim$0.3 kpc of the Galactic center - and its eccentricity and smallness of its perigalacticon are only surpassed by $\sim$0.05%, of local F/G-type field stars. The observed characteristics are consistent with V474 Car being a high velocity, metal poor, tidally-locked chromospherically active binary (CAB), i.e.\ a halo RS CVn binary, and one of only a few such specimens known.Comment: Accepted to Astronomical Journa

Distances and ages of globular clusters using Hipparcos parallaxes of local subdwarfs

We discuss the impact of Population II and Globular Cluster (GCs) stars on the derivation of the age of the Universe, and on the study of the formation and early evolution of galaxies, our own in particular. The long-standing problem of the actual distance scale to Population II stars and GCs is addressed, and a variety of different methods commonly used to derive distances to Population II stars are briefly reviewed. Emphasis is given to the discussion of distances and ages for GCs derived using Hipparcos parallaxes of local subdwarfs. Results obtained by different authors are slightly different, depending on different assumptions about metallicity scale, reddenings, and corrections for undetected binaries. These and other uncertainties present in the method are discussed. Finally, we outline progress expected in the near future.Comment: Invited review article to appear in: `Post-Hipparcos Cosmic Candles', A. Heck & F. Caputo (Eds), Kluwer Academic Publ., Dordrecht, in press. 22 pages including 3 tables and 2 postscript figures, uses Kluwer's crckapb.sty LaTeX style file, enclose

Abundances of metal-weak thick-disc candidates

High resolution spectra of 5 candidate metal-weak thick-disc stars suggested by Beers & Sommer-Larsen (1995) are analyzed to determine their chemical abundances. The low abundance of all the objects has been confirmed with metallicity reaching [Fe/H]=-2.9. However, for three objects, the astrometric data from the Hipparcos catalogue suggests they are true halo members. The remaining two, for which proper-motion data are not available, may have disc-like kinematics. It is therefore clear that it is useful to address properties of putative metal-weak thick-disc stars only if they possess full kinematic data. For CS 22894-19 the abundance pattern similar to those of typical halo stars is found, suggesting that chemical composition is not a useful discriminant between thick-disc and halo stars. CS 29529-12 is found to be C enhanced with [C/Fe]=+1.0; other chemical peculiarities involve the s process elements: [Sr/Fe]=-0.65 and [Ba/Fe]=+0.62, leading to a high [Ba/Sr] considerably larger than what is found in more metal-rich carbon-rich stars, but similar to LP 706-7 and LP 625-44 discussed by Norris et al (1997a). Hipparcos data have been used to calculate the space velocities of 25 candidate metal-weak thick-disc stars, thus allowing us to identify 3 bona fide members, which support the existence of a metal-poor tail of the thick-disc, at variance with a claim to the contrary by Ryan & Lambert (1995).Comment: to be published in MNRA

Three-dimensional hydrodynamical simulations of red giant stars: semi-global models for the interpretation of interferometric observations

Context. Theoretical predictions from models of red giant branch stars are a valuable tool for various applications in astrophysics ranging from galactic chemical evolution to studies of exoplanetary systems. Aims. We use the radiative transfer code OPTIM3D and realistic 3D radiative-hydrodynamical (RHD) surface convection simulations of red giants to explore the impact of granulation on interferometric observables. Methods. We compute intensity maps for the 3D simulation snapshots in two filters: in the optical at 5000 \pm 300 {\AA} and in the K band 2.14 $\pm$ 0.26 {\mu}m FLUOR filter, corresponding to the wavelength-range of instruments mounted on the CHARA interferometer. From the intensity maps, we construct images of the stellar disks, accounting for center-to-limb variations. We then derive interferometric visibility amplitudes and phases. We study their behavior with position angle and wavelength. Results. We provide average limb-darkening coefficients for different metallicities and wavelength-ranges. We detail the prospects for the detection and characterization of granulation and center-to-limb variations of red giant stars with today's interferometers. We find that the effect of convective-related surface structures depends on metallicity and surface gravity. We provided theoretical closure phases that should be incorporated into the analysis of red giant planet companion closure phase signals. We estimate 3D-1D corrections to stellar radii determination: 3D models are ~ 3.5% smaller to ~ 1% larger in the optical with respect to 1D, and roughly 0.5 to 1.5% smaller in the infrared. Even if these corrections are small, they are important to properly set the zero point of effective temperature scale derived by interferometry and to strengthen the confidence of existing red giant catalogues of calibrating stars for interferometry.Comment: Accepted for publication on Astronomy & Astrophysics, 14 pages, 13 figure