Background Ehrlichia, Anaplasma, and Babesia spp. are canine pathogens transmitted by the Rhipicephalus sanguineus tick which can cause varied clinical signs. These pathogens have been investigated in the Philippines, but coinfection has not been reported yet. Aim The aim of this study was to evaluate the presence of Ehrlichia/Anaplasma and Babesia spp. in Philippine dogs. Materials and methods A total of 100 dogs from seven different veterinary establishments in Cebu, Philippines, were examined for Ehrlichia/Anaplasma and Babesia spp. infection using peripheral blood smear examination and polymerase chain reaction (PCR). Inclusion criteria included a history or presence of tick infestation, anemia, and/or thrombocytopenia. Clinical signs were recorded. Statistical analyses were performed between PCR positivity and clinical signs and hematological results. Results A total of 10 and 18 dogs were found to be positive for Ehrlichia/Anaplasma and Babesia spp., respectively. One animal was PCR positive for both pathogens, which is the first report of coinfection in the country. The most common clinical signs observed include inappetence (89%), lethargy (80%), thrombocytopenia (85%), and anemia (74%). Analyses revealed that inappetence (p=0.044) and weight loss (p=0.028) were found statistically significant with Ehrlichia/Anaplasma infection. Basophil (p=0.001) and eosinophil counts (p=0.000) were also found significantly different between Ehrlichia/Anaplasma spp.-positive and -negative dogs. On the other hand, differential monocyte count (p=0.009) was found significantly different between Babesia spp.-positive and -negative dogs. Conclusion The present study showed low infection rates of canine ehrlichiosis/anaplasmosis and babesiosis and provided additional evidence for the presence of the pathogens in the area.

/pdf/detection-of-ehrlichia-anaplasma-and-babesia-spp-in-dogs-of-4vajhjvjnx.pdf

Detection of Ehrlichia, Anaplasma, and Babesia spp. in dogs of Cebu, Philippines.

. In this paper, we show the result of the joint use of the OMT-800 telescope, the CoLiTec software, and the V¨ais¨al¨a method. The paper considers in detail several of the discovered (rediscovered) asteroids: 2017 AB8, 2017 QX33, and 2017 RV12 from a long list of small bodies of the Solar System

First reported observation of asteroids 2017 AB8, 2017 QX33, and 2017 RV12

A rapid method is proposed for determining a meteoroid’s trajectory in the Earth’s atmosphere and its height and velocity at individual points The method is designed for use with video material (regardless of the motion speed of the video recorder) for daytime bolide events Kinematic parameters are obtained for the superbolide event followed by the Chelyabinsk meteorite shower on February 15, 2013 The (geodetic) azimuth of the meteoroid’s trajectory in the Earth’s atmosphere is 28339° ± 17° (or 10109° ± 17° toward the radiant) The radiant altitude over the site with observations of the end of the first fragmentation phase is 205° The geodetic coordinates of the beginning of the bolide phenomenon and the point of suspension of the radiating material at the end of the first fragmentation phase are (64°00′0274″ ± 21′ east longitude; 54°30′5466″ ± 30′ north latitude) and (61°11′0188″ ± 16′ east longitude; 54°52′0668″ ± 31′ north latitude), respectively The atmospheric entry velocity is 1929 ± 089 km s−1 The height of the start of the light emission is 1024 km; those of the main fragmentation phases are 280 and 244 km The calculated elements for the heliocentric orbit of the Chelyabinsk meteoroid are: Q = 266 ± 120 AU, q = 073 ± 001 AU, a = 167 ± 010 AU, e = 057 ± 003, i = 707° ± 054°, Ω = 32642°, and ω = 10628° ± 254° These parameters are compared with the results obtained by other authors

Main parameters of meteoroid motion during the fall of the Chelyabinsk meteorite shower on February 15, 2013

Photometric study of the C/2014 Q2 (Lovejoy) comet plasma tails

A New 800 mm Automatic Telescope

A review of TV and telescopic methods of meteor observations and of the problems of meteor astronomy addressed using these methods is presented. A meteor patrol developed at the Astronomical Observatory of Odessa National University and based on a Schmidt telescope and a TV detector is described. The meteor patrol allows meteor events to be recorded with a time resolution of 0.04 s. The investigated characteristics of the patrol are reported, and some aspects of the methods of observations and reduction employed are considered. The results of observations made during the period 2003–2004 are reported. A total of 368 meteors were recorded on 1093 individual frames during a total patrol time of 679 hours within a 36′ × 48′ field of view. The statistical data for meteor observations are reported, and classification of meteor images is presented. The specific features of some recorded meteor events are analyzed.

Methods and statistics of TV observations of telescopic meteors

We examine the hypothesis about the formation of meteor streams near the Sun. Families of short-perihelion orbit comets, many of which pass just a few radii from the solar surface at perihelion and have high dust production efficiencies, are assumed to be candidates for the parent bodies of these meteor streams. Our statistical analysis of orbital and kinematic parameters for short-perihelion meteoric particles recorded at the Earth and comets from the Kreutz family and the Marsden, Kracht, and Meyer groups led us to certain conclusions regarding the proposed hypothesis. We found a correlation between the ecliptic longitude of perihelion for comet and meteor orbits and the perihelion distance. This correlation may be suggestive of either a genetic connection between the objects of these two classes or the result of an as yet unknown mechanism that equally acts on short-perihelion comet and meteor orbits. A reliable conclusion about this genetic connection can be reached for the meteors that belong to the Arietids stream and the Marsden comet group.

Young Meteor Swarms Near the Sun: I. Statistical Correlation of Meteors with Families of Short-Perihelion Comets

A method for calculation of slant-range differences to the active geostationary telecommunication satellite (GEO Telecom Satellite) is described in the article. The method is developed in the “Mykolaiv Astronomical Observatory” Research Institute. The results of observation of the “Eutelsat-25C” and “Eutelsat-13B” satellites with two receiving stations of digital satellite TV are discussed. The accuracy of determination of slant-range differences to the GEO Telecom Satellite is presented. Key words: radio interferometer, geostationary satellite, digital satellite television Manuscript submitted 29.05.2015 Radio phys. radio astron. 2015, 20(3): 238-246 REFERENCES 1. BUSHUEV, F. I., KALIUZHNYI, N. A., SLIVINSKY, A. P. and SHULGA, A. V., 2012. Determination of the Range to Geostationary Telecommunications Geostationary Satellites Using the Signals of Satellite Television. Radio Phys. Radio Astron ., vol. 17, no. 3, pp. 281–290 (in Russian). 2. EUROPEAN TELECOMMUNICATIONS STANDARDS INSTITUTE., 1997. Digital Video broadcasting (DVB); Framing structure, channel coding and modulation for 11/12 GHz satellite services. European Standard (Telecommunications series).EN 300 421 V1.1.2 (1997-08). Sophia Antipolis: ETSI. 3. EUROPEAN TELECOMMUNICATIONS STANDARDS INSTITUTE., 2009. Digital Video Broadcasting (DVB); Second generation framing structure, channel coding and modulation systems for Broadcasting, Interactive Services, News Gathering and other broadband satellite applications (DVB-S2). European Standard (Telecommunications series). ETSI EN 302 307 V1.2.1 (2009-08) . Sophia Antipolis: ETSI. 4. Reconstruction of signal by interpolation [online]. Available from: http://fourier.eng.hmc.edu/e101/lectures/Sampling_theorem/node3.html 5. CABOT R., 1981. A note on the application of the Hilbert transform to time delay estimation. IEEE Trans. Acoust. Speech Signal Processing , vol. 29, no. 3, pp. 607–609. DOI: https://doi.org/10.1109/TASSP.1981.1163564

/pdf/method-and-first-results-of-calculation-of-slant-range-4eqq6r3i5k.pdf

Method and First Results of Calculation of Slant-Range Differences to Active Geostationary Telecommunication Satellite

We present the results of our positional reduction of the observational material obtained using a meteor patrol based on a Schmidt telescope and a TV CCD detector. More that 1000 telescopic meteors were recorded in three years of meteor patrolling. Techniques for the cataloging and positional reduction of 3050 TV images with meteor trails are described. We have developed a technique for measuring the images of reference stars to determine the rectangular coordinates in the image frame. We discuss the achieved accuracy of determining the equatorial coordinates of reference and check stars by Turner’s method (of the order of a few arcseconds). We have developed software that allows the rectangular coordinates of meteor trajectory points to be determined after the meteor image reduction. These coordinates are used to determine the equatorial coordinates of the poles of the great circles of meteor trajectories (the angular length is not less than 15′ with an accuracy of at least 4′. We consider the possibility of using Stanyukovich’s method to determine the equatorial coordinates of radiants for non-basis meteor observations. The accuracy of determining the radiant coordinates has been estimated to be 4′–5′. Prospects for obtaining the kinematic characteristics of meteor particles are discussed.

Techniques for positional measurements of telescopic meteor TV images

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