1,723,746 research outputs found
Modification of the cannulation for the dorsal aorta of Atlantic salmon (Salmo salar)
No full textRE: 6 ref.; SC: CA; VE; ZA; 0ISource type: Electronic(1) http://upei-resolver.asin-risa.ca?sid=SP:CABI&id=pmid:&id=&issn=0023-6764&isbn=&volume=44&issue=5&spage=540&pages=540-541&date=1994&title=Laboratory%20Animal%20Science&atitle=Modification%20of%20the%20cannulation%20for%20the%20dorsal%20aorta%20of%20Atlantic%20salmon%20%28Salmo%20salar%29.&aulast=Pye-MacSwain&pid=%3Cauthor%3EPye%20MacSwain%2c%20J%20K%3bCawthron%2c%20E%20G%3bRainnie%2c%20D%20J%3bJohnson%2c%20G%20R%3C%2Fauthor%3E%3CAN%3E19952203533%3C%2FAN%3E%3CDT%3EJournal%20article%3C%2FDT%3
ERP characteristics of function and content words in Broca's aphasics with agrammatic comprehension
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6764.pdf (Publisher’s version ) (Open Access
PARSEC-SCALE IMAGING OF THE RADIO-BUBBLE SEYFERT GALAXY NGC 6764
No full textWe have observed the composite active galactic nucleus (AGN)-starburst galaxy NGC 6764 with the Very Long Baseline Array at 1.6 and 4.9 GHz. These observations have detected a "core-jet" structure and a possible weak counterjet component at 1.6 GHz. The upper limits to the core and jet (1.6-4.9 GHz) spectral index are 0.6 and 0.3, respectively. Taken together with the high brightness temperature of similar to 10(7) K for the core region, the radio emission appears to be coming from a synchrotron jet. At a position angle of similar to 25 degrees, the parsec-scale jet seems to be pointing closely toward the western edge of the southern kpc-scale bubble in NGC 6764. A real connection between the parsec-and sub-kpc-scale emission would not only suggest the presence of a curved jet, but also a close link between the AGN jet and the radio bubbles in NGC 6764. We demonstrate that a precessing jet model can explain the radio morphology from parsec to sub-kpc scales, and the model best-fit parameters of jet speed and orientation are fully consistent with the observed jet-to-counterjet surface brightness ratio. The jet however appears to be disrupted on scales of hundreds of parsecs, possibly due to interaction with and entrainment of the interstellar medium gas, which subsequently leads to the formation of bubbles. The jet energetics in NGC 6764 suggest that it would take 12-21 Myr to inflate the (southern) bubble. This timescale corresponds roughly to the starburst episode that took place in NGC 6764 about 15-50 Myr ago, and could be indicative of a close connection between jet formation and the starburst activity in this galaxy
Parsec-scale imaging of the radio-bubble Seyfert galaxy NGC 6764
No full textWe have observed the composite active galactic nucleus (AGN)-starburst galaxy NGC 6764 with the Very Long Baseline Array at 1.6 and 4.9 GHz. These observations have detected a "core-jet" structure and a possible weak counterjet component at 1.6 GHz. The upper limits to the core and jet (1.6-4.9 GHz) spectral index are 0.6 and 0.3, respectively. Taken together with the high brightness temperature of ~107 K for the core region, the radio emission appears to be coming from a synchrotron jet. At a position angle of ~25°, the parsec-scale jet seems to be pointing closely toward the western edge of the southern kpc-scale bubble in NGC 6764. A real connection between the parsec- and sub-kpc-scale emission would not only suggest the presence of a curved jet, but also a close link between the AGN jet and the radio bubbles in NGC 6764. We demonstrate that a precessing jet model can explain the radio morphology from parsec to sub-kpc scales, and the model best-fit parameters of jet speed and orientation are fully consistent with the observed jet-to-counterjet surface brightness ratio. The jet however appears to be disrupted on scales of hundreds of parsecs, possibly due to interaction with and entrainment of the interstellar medium gas, which subsequently leads to the formation of bubbles. The jet energetics in NGC 6764 suggest that it would take 12-21 Myr to inflate the (southern) bubble. This timescale corresponds roughly to the starburst episode that took place in NGC 6764 about 15-50 Myr ago, and could be indicative of a close connection between jet formation and the starburst activity in this galaxy
6764 Kirillavrov: A Binary Asteroid
No full textMutual events appearing in the lightcurve of 6764 Kirrillavrov unambiguously show that it is a binary asteroid with a rotation period of 4.739 ± 0.001 h, and an orbital period of 30.41 ± 0.01 h. Follow-up observations conducted during the 2021 opposition did not detect the mutual events due to unfavorable viewing geometry. Further observations during subsequent oppositions are encouraged.Fil: Polakis, Tom. Command Module Observatory; IslandiaFil: Oey, Julian. Blue Mountains Observatory; AustraliaFil: Colazo, Milagros Rita. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Facultad de Matemática, Astronomía y Física; Argentin
6764 Kirillavrov: A Binary Asteroid
No full textMutual events appearing in the lightcurve of 6764 Kirrillavrov unambiguously show that it is a binary asteroid with a rotation period of 4.739 ± 0.001 h, and an orbital period of 30.41 ± 0.01 h. Follow-up observations conducted during the 2021 opposition did not detect the mutual events due to unfavorable viewing geometry. Further observations during subsequent oppositions are encouraged.Fil: Polakis, Tom. Command Module Observatory; IslandiaFil: Oey, Julian. Blue Mountains Observatory; AustraliaFil: Colazo, Milagros Rita. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Facultad de Matemática, Astronomía y Física; Argentin
Going Beyond Counting First Authors in Author Co-citation Analysis
Get PDFThe present study examines one of the fundamental aspects of author co-citation analysis (ACA) - the way co-citation
counts are defined. Co-citation counting provides the data on which all subsequent statistical analyses and mappings
are based, and we compare ACA results based on two different types of co-citation counting - the traditional type that
only counts the first one among a cited work's authors on the one hand and a non-traditional type that takes into
account the first 5 authors of a cited work on the other hand. Results indicate that the picture produced through this non-traditional author co-citation counting contains more coherent author groups and is therefore considerably clearer. However, this picture represents fewer specialties in the research field being studied than that produced through the traditional first-author co-citation counting when the same number of top-ranked authors is selected and analyzed. Reasons for these effects are discussed
ISO observations of the Wolf-Rayet galaxies NGC 5430, NGC 6764, Mrk 309 and VII Zw 19
No full textObservations of four WR galaxies (NGC 5430, NGC 6764, Mrk 309 and VII Zw 19) using the Infrared Space Observatory are presented here. ISOCAM maps of NGC 5430, Mrk 309 and NGC 6764 revealed the location of star formation regions in each of these galaxies. ISOPHOT spectral observations from 4 to 12 μm detected the ubiquitous PAH bands in the nuclei of the
targets and several of the disk star forming regions, while LWS spectroscopy detected [O I] and [C II] emission lines from two galaxies, NGC 5430 and NGC 6764.
Using a combination of ISO and IRAS flux densities, a dust model based on the sum of modified blackbody components was successfully fitted to the available data. These models were
then used to calculate new values for the total IR luminosities for each galaxy, the size of the various dust populations, and the global SFR.
The derived flux ratios, the SFRs, the high L(PAH)/L(40–120 μm) and F(PAH 7.7 μm)/F(7.7 μm continuum) values suggest that most of these galaxies are home to only a compact burst of star formation. The exception is NGC 6764, whose
F(PAH 7.7 μm)/F(7.7 μm continuum) value of 1.22 is consistent with the presence of an AGN, yet the L(PAH)/L(40–120 μm) is more in line with a starburst, a
finding in line with a compact low-luminosity AGN dominated by the starburst.
Variations on the Author
Get PDF“Variations on the Author” discusses two of Eduardo Coutinho’s recent films (Um Dia na Vida, from 2010, and Últimas Conversas, posthumously released in 2015) and their contribution to the general question of documentary authorship. The director’s filmography is characterized by a consistent yet self-effacing form of authorial self-inscription: Coutinho often features as an interviewer that rather than express opinions propels discourses; an interviewer that is good at listening. This mode of self-inscription characterizes him as an author who is not expressive but who is nonetheless markedly present on the screen. In Um Dia na Vida, however, Coutinho is completely absent form the image, while Últimas Conversas, on the contrary, includes a confessional prologue that moves the director from the margins to the center of his films. This article examines the ways in which these works stand out in the filmography of a director who offers new insights into the notion of cinematic authorship
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