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1. Frass Production From Black Soldier Fly Larvae Reared On Palm Oil Wastes

Author

L Visvini, O Latifah, O H Ahmed, and W J Kurk

Abstract

The availability of decanter cake (DC) and palm kernel expeller (PKE) from palm oil processing remains high owing to the major revenue earned from palm oil industry. Rearing black soldier fly larvae (BSFL) using DC and PKE as substrate to produce frass could solve the indiscriminate disposal of these wastes. Rearing BSFL was carried out by hatching the black soldier fly eggs in the trays size of 65 cm length x 37 cm width x 15 cm depth laid with processed soybean as starter diet for a week. After seven days, the DC and PKE were fed to the BSFL as main substrates and continued for another 38 days until the BSFL reached to pupae stage. Temperatures of the ambient and rearing substrate were monitored daily for 45 days. The frass of BSFL was analyzed for some selected physico-chemical properties and germination test to ascertain the quality of the BSFL frass to be used as organic fertilizer. Colour of the BSFL frass, electrical conductivity (EC), organic matter (OM), pH, total carbon (C), nitrogen (N), C/N ratio, ammonium, and nitrate contents were determined using standard procedures. Frass was produced at 45 days of rearing BSFL after which the larvae were turn to pupae. Frass consists of excretions, substrate residues, and shed exoskeletons of the BSFL. The pH of BSFL frass was 7.41, whereas the EC (1.21 mS/cm) was in the range of permissible level for its uses as organic fertilizer. The BSFL frass contain 1.68% total N, 8870.19 mg kg−1 ammonium, and 5453.20 mg kg−1 nitrate which were higher than those of initial mixture of the feeding substrate due to the decomposition process of the organic substrates which is related to the lower content of total OM (45.23%) and C (26.23%). Germination of white radish (test crop) on a distilled water and the different extractions of BSFL frass were not significantly different suggested that the frass produced from BSFL fed on DC and PKE had no toxic effects on plant. Decanter cake and PKE could be used as rearing substrate for BSFL to produce frass based on the appropriate values of pH, EC, total N, ammonium, nitrate, total organic matter and total organic C, and C/N ratio.

Published
2022
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2. SPACE: the spectroscopic all-sky cosmic explorer

Author

A. Cimatti, M. Robberto, C. Baugh, S. V. W. Beckwith, R. Content, E. Daddi, G. De Lucia, B. Garilli, L. Guzzo, G. Kauffmann, M. Lehnert, D. Maccagni, A. Martínez-Sansigre, F. Pasian, I. N. Reid, P. Rosati, R. Salvaterra, M. Stiavelli, Y. Wang, M. Zapatero Osorio, M. Balcells, M. Bersanelli, F. Bertoldi, J. Blaizot, D. Bottini, R. Bower, A. Bulgarelli, A. Burgasser, C. Burigana, R. C. Butler, S. Casertano, B. Ciardi, M. Cirasuolo, M. Clampin, S. Cole, A. Comastri, S. Cristiani, J.-G. Cuby, F. Cuttaia, A. De Rosa, A. Diaz Sanchez, M. Di Capua, J. Dunlop, X. Fan, A. Ferrara, F. Finelli, A. Franceschini, M. Franx, P. Franzetti, C. Frenk, Jonathan P. Gardner, F. Gianotti, R. Grange, C. Gruppioni, A. Gruppuso, F. Hammer, L. Hillenbrand, A. Jacobsen, M. Jarvis, R. Kennicutt, R. Kimble, M. Kriek, J. Kurk, J.-P. Kneib, O. Le Fevre, D. Macchetto, J. MacKenty, P. Madau, M. Magliocchetti, D. Maino, N. Mandolesi, N. Masetti, R. McLure, A. Mennella, M. Meyer, M. Mignoli, B. Mobasher, E. Molinari, G. Morgante, S. Morris, L. Nicastro, E. Oliva, P. Padovani, E. Palazzi, F. Paresce, A. Perez Garrido, E. Pian, L. Popa, M. Postman, L. Pozzetti, J. Rayner, R. Rebolo, A. Renzini, H. Röttgering, E. Schinnerer, M. Scodeggio, M. Saisse, T. Shanks, A. Shapley, R. Sharples, H. Shea, J. Silk, I. Smail, P. Spanó, J. Steinacker, L. Stringhetti, A. Szalay, L. Tresse, M. Trifoglio, M. Urry, L. Valenziano, F. Villa, I. Villo Perez, F. Walter, M. Ward, R. White, S. White, E. Wright, R. Wyse, G. Zamorani, A. Zacchei, W. W. Zeilinger, F. Zerbi, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Space Telescope Science Institute (STScI), Institute for Computational Cosmology, Department of Physics, Durham University, Durham (ICC), Centre for Advanced Instrumentation, Department of Physics, Durham University (CfAI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Max-Planck-Institut für Astrophysik (MPA), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), Brera, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), INAF-Osservatorio Astronomico di Trieste (INAF-OATs), European Southern Observatory (ESO), Università di Milano, University of Oklahoma, Instituto de Astrofísica de Canarias (IAC), Rheinische Friedrich-Wilhelms-Universität Bonn, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Bologna), Department of Earth Atmospheric and Planetary Sciences, MIT, The Royal Observatory (ROE), Goddard Space Flight Center, NASA, Astrophysics Science Division, INAF-Osservatorio Astronomico di Bologna (OABO), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad Politecnica de Cartagena (UPCT), University of Maryland, University of Arizona, Scuola Internazionale Superiore di Studi Avanzati (SISSA), Università degli Studi di Padova = University of Padua (Unipd), University of Leiden, California Institute of Technology, Department of Astronomy (CALTECH), OpSys Project Consulting, University of Hertfordshire [Hatfield] (UH), Institute of Astronomy, University of Cambridge (IoA), Research and Scientific Support Department, ESA-ESTEC (RSSD), University of California, Santa Cruz (UCSC), Steward Observatory, University of Arizona, UC Riverside, INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), University of Bucharest, Institute for Astronomy, University of Hawaii, INAF-Osservatorio Astronomico di Padova, Princeton, Ecole Polytechnique Fédérale de Lausanne (EPFL), University of Oxford, Johns Hopkins University (JHU), Yale University, University of California, Los Angeles (UCLA), University of Vienna, Cimatti A., Robberto M., Baugh C., Beckwith S. V. W., Content R., Daddi E., De Lucia G., Garilli B., Guzzo L., Kauffmann G., Lehnert M., Maccagni D., Martínez-Sansigre A., Pasian F., Reid I. N., Rosati P., Salvaterra R., Stiavelli M., Wang Y., Osorio M. Zapatero, Balcells M., Bersanelli M., Bertoldi F., Blaizot J., Bottini D., Bower R., Bulgarelli A., Burgasser A., Burigana C., Butler R. C., Casertano S., Ciardi B., Cirasuolo M., Clampin M., Cole S., Comastri A., Cristiani S., Cuby J.-G., Cuttaia F., de Rosa A., Sanchez A. Diaz, di Capua M., Dunlop J., Fan X., Ferrara A., Finelli F., Franceschini A., Franx M., Franzetti P., Frenk C., Gardner Jonathan P., Gianotti F., Grange R., Gruppioni C., Gruppuso A., Hammer F., Hillenbrand L., Jacobsen A., Jarvis M., Kennicutt R., Kimble R., Kriek M., Kurk J., Kneib J.-P., Le Fevre O., Macchetto D., MacKenty J., Madau P., Magliocchetti M., Maino D., Mandolesi N., Masetti N., McLure R., Mennella A., Meyer M., Mignoli M., Mobasher B., Molinari E., Morgante G., Morris S., Nicastro L., Oliva E., Padovani P., Palazzi E., Paresce F., Garrido A. Perez, Pian E., Popa L., Postman M., Pozzetti L., Rayner J., Rebolo R., Renzini A., Röttgering H., Schinnerer E., Scodeggio M., Saisse M., Shanks T., Shapley A., Sharples R., Shea H., Silk J., Smail I., Spanó P., Steinacker J., Stringhetti L., Szalay A., Tresse L., Trifoglio M., Urry M., Valenziano L., Villa F., Perez I. Villo, Walter F., Ward M., White R., White S., Wright E., Wyse R., Zamorani G., Zacchei A., Zeilinger W., Zerbi F., Cimatti, A., Robberto, M., Baugh, C., Beckwith, S. V. W., Content, R., Daddi, E., De, Lucia, G., Garilli, B., Guzzo, L., Kauffmann, Ferrara, Andrea, and 113, Coauthors

Subjects
Observational cosmology, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Space (mathematics), law.invention, Telescope, law, Dark energy, Spectral resolution, media_common, Physics, COSMIC cancer database, Astronomical and space-research instrumentation, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Billion years, Galaxy, Redshift, Space and Planetary Science, Sky, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We describe the scientific motivations, the mission concept and the instrumentation of SPACE, a class-M mission proposed for concept study at the first call of the ESA Cosmic-Vision 2015-2025 planning cycle. SPACE aims to produce the largest three-dimensional evolutionary map of the Universe over the past 10 billion years by taking near-IR spectra and measuring redshifts for more than half a billion galaxies at 0, Comment: 27 pages, Experimental Astronomy, in press. The SPACE team complete list is available at http://urania.bo.astro.it/cimatti/space . The article with full resolution figures is available at http://urania.bo.astro.it/cimatti/space/publications.htm

Published
2008
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4. Computer visualization techniques (CVTs) foster evidence-based target delineation

Author

M. Smiedala, John E. McGary, Bin S. Teh, V. Shukla, H. Hsin Lu, Walter H. Grant, J. Kurk, E. Brian Butler, Ryan Butler, and Arnold dela Cruz Paulino

Subjects
Multimodal imaging, Cancer Research, Creative visualization, Evidence-based practice, Emerging technologies, business.industry, Computer science, media_common.quotation_subject, Radiotherapy Planning, Computer-Assisted, General Medicine, Machine learning, computer.software_genre, Oncology, Neoplasms, Image Processing, Computer-Assisted, Radiation Oncology, Humans, Artificial intelligence, Intensity modulated radiotherapy, Outcome data, business, computer, media_common
Abstract

Computer visualization techniques (CVTs) are an emerging technology that can organize all cancer specialists. This article describes CVTs' ability to maximize the currently untapped advantages of intensity modulated radiotherapy (IMRT). The visual speed and dynamic strategies inherent in CVTs improves IMRT by distilling vast amounts of anatomic, multimodal imaging, textual/meaning, and surgical/outcome data into a large, rigorous, standardized evidence base of storable target delineation plans. This ability to standardize strategies will allow the collection of meaningful evidence based outcome data.

Published
2007

5. zCOSMOS: A Large VLT/VIMOS redshift survey covering 0 < z < 3 in the COSMOS field

Author

S. J. Lilly, O. Le Fevre, A. Renzini, G. Zamorani, M. Scodeggio, T. Contini, C. M. Carollo, G. Hasinger, J.‐P. Kneib, A. Iovino, V. Le Brun, C. Maier, V. Mainieri, M. Mignoli, J. Silverman, L. A. M. Tasca, M. Bolzonella, A. Bongiorno, D. Bottini, P. Capak, K. Caputi, A. Cimatti, O. Cucciati, E. Daddi, R. Feldmann, P. Franzetti, B. Garilli, L. Guzzo, O. Ilbert, P. Kampczyk, K, Kovac, F. Lamareille, A. Leauthaud, J.‐F. Le Borgne, H. J. McCracken, C. Marinoni, R. Pello, E. Ricciardelli, C. Scarlata, D. Vergani, D. B. Sanders, E. Schinnerer, N. Scoville, Y. Taniguchi, S. Arnouts, H. Aussel, S. Bardelli, M. Brusa, A. Cappi, P. Ciliegi, A. Finoguenov, S. Foucaud, R. Franceschini, C. Halliday, C. Impey, C. Knobel, A. Koekemoer, J. Kurk, D. Maccagni, S. Maddox, B. Marano, G. Marconi, B. Meneux, B. Mobasher, C. Moreau, J. A. Peacock, C. Porciani, L. Pozzetti, R. Scaramella, D. Schiminovich, P. Shopbell, I. Smail, D. Thompson, L. Tresse, G. Vettolani, A. Zanichelli, E. Zucca, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy, Department of Physics, ETH Zürich, Università degli Studi di Padova = University of Padua (Unipd), INAF-Osservatorio Astronomico di Bologna (OABO), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestriche Physik (MPE), INAF-Osservatorio Astronomico di Brera, Cahill Center for Astronomy and Astrophysics, California Institute of Technology, INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), National Optical Astronomy Observatory, Tucson (NOAO), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy, University of Hawaii, Max-Planck-Institut für Astronomie (MPIA), Tohoku University, Nottingham University, University of Arizona (UoA), Space Telescope Science Institute (STScI), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), European Southern Observatory (ESO), University of Edinburgh, Istituto Nazionale di Astrofisica (INAF), Columbia University, New York, Institute for Computational Cosmology, Department of Physics, Durham University, Durham (ICC), IRA-INAF, Bologna, Beaussier, Catherine, Lilly S. J., Le Fèvre O., Renzini A., Zamorani G., Scodeggio M., Contini T., Carollo C. M., Hasinger G., Kneib J.-P., Iovino A., Le Brun V., Maier C., Mainieri V., Mignoli M., Silverman J., Tasca L. A. M., Bolzonella M., Bongiorno A., Bottini D., Capak P., Caputi K., Cimatti A., Cucciati O., Daddi E., Feldmann R., Franzetti P., Garilli B., Guzzo L., Ilbert O., Kampczyk P., Kovac K., Lamareille F., Leauthaud A., Borgne J.-F. Le, McCracken H. J., Marinoni C., Pello R., Ricciardelli E., Scarlata C., Vergani D., Sanders D. B., Schinnerer E., Scoville N., Taniguchi Y., Arnouts S., Aussel H., Bardelli S., Brusa M., Cappi A., Ciliegi P., Finoguenov A., Foucaud S., Franceschini R., Halliday C., Impey C., Knobel C., Koekemoer A., Kurk J., Maccagni D., Maddox S., Marano B., Marconi G., Meneux B., Mobasher B., Moreau C., Peacock J. A., Porciani C., Pozzetti L., Scaramella R., Schiminovich D., Shopbell P., Smail I., Thompson D., Tresse L., Vettolani G., Zanichelli A., and Zucca E.

Subjects
Physics, Active galactic nucleus, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, Redshift survey, 01 natural sciences, Redshift, Spectral line, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, Galaxy group, 0103 physical sciences, Emission spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Spectrograph
Abstract

zCOSMOS is a large redshift survey that is being undertaken in the COSMOS field using 600 hours of observation with the VIMOS spectrograph on the 8-m VLT. The survey is designed to characterise the environments of COSMOS galaxies from the 100 kpc scales of galaxy groups up to the 100 Mpc scale of the cosmic web and to produce diagnostic information on galaxies and active galactic nuclei. The zCOSMOS survey consists of two parts: (a) zCOSMOS-bright, a magnitude-limited I-band IAB < 22.5 sample of about 20,000 galaxies with 0.1 < z < 1.2 covering the whole 1.7 deg2 COSMOS ACS field and designed to mimic the parameters of the 2dfGRS; and (b) zCOSMOS-deep, a survey of approximately 10,000 galaxies selected through colour-selection criteria to have 1.4 < z < 3.0, within the central 1 deg2. This paper describes the survey design and the construction of the target catalogues, and briefly outlines the observational program and the data pipeline. In the first observing season, spectra of 1303 zCOSMOS-bright targets and of 977 zCOSMOS-deep targets have been obtained. These are briefly analysed to demonstrate the characteristics that may be expected from zCOSMOS, and particularly zCOSMOS-bright, when it is finally completed between 2008-2009. The power of combining spectroscopic and photometric redshifts is demonstrated, especially in correctly identifying the emission line in single-line spectra and in determining which of the less reliable spectroscopic redshifts are correct and which are incorrect. Our zCOSMOS-deep spectra demonstrate the effectiveness of our selection techniques to isolate high redshift galaxies at 1.4 < z < 3.0 and of VIMOS to measure their redshifts using ultraviolet absorption lines., Comment: 24 pages plus 16 figures. Accepted, to appear in the ApJ Supplement COSMOS Special Issue

Published
2006
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6. EVALUATION OF SELECTED INSECTICIDES FOR CONTROL OF BOLLWORM (BW) AND TOBACCO BUDWORM (TBW) IN GEORGIA ON COTTON, 2004

Author

John N. All, Michelle Samuel-Foo, J. Kurk Lance, Phillip H. Jost, and Caleb V. Warrington

Subjects
Early season, Horticulture, Bollworm, Sprayer, Sowing, Square (unit), General Medicine, Upper third, Acre, Biology, Volume rate
Abstract

This test was conducted at the Southeastern Research and Education Center, Midville, GA. The test was set up in a RCB design with 4 replications and one untreated check per replication. The plots were 4 rows by 50 ft with an untreated border row on each side. The rows were planted on beds spaced 38 inches apart using a 4-row Max Emerge II John Deere planter. Temik 15G at 3.0 lb product/acre was placed in-furrow at planting for early season thrips control. Treatment applications began on 14 Jul when square damage was approaching a threshold of 5%. Treatments were applied with a CO2 spraying system mounted on a Powell high cycle sprayer. The sprayer traveled at a speed of 3.0 mph. Treatments were applied at a volume rate of 10 gpa, at 50 psi, with 3 nozzles per row using TX-3 hollow cone nozzles. Treatments were applied on 14, 20, 27 Jul, and 4 Aug. Weekly efficacy evaluations were done by randomly selecting 5 plants from the middle two rows of each plot and counting all the fruiting structures (squares and bolls) on the upper third of each plant. Fruiting structures were examined for feeding damage and the presence of larvae. The efficacy surveys were done on 20, 27 Jul, 4, and 11 Aug. On 5 Oct, yield was taken by mechanically harvesting the two middle rows of each plot. Means for percent square damage and yield were analyzed using ANOVA with means separation using LSD (P ≤ 0.05).

Published
2005
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11. EVALUATION OF SELECTED INSECTICIDES FOR CONTROL OF CORN EARWORM IN SWEET CORN, 2003

Author

John N. All and J. Kurk Lance

Subjects
Horticulture, Sprayer, Sowing, General Medicine, Biology
Abstract

Two tests were planted (28 Apr and 2 Jun) at the University of Georgia's Plant Sciences Farm, near Watkinsville, GA. The tests were set up in a RCB design with four replications. The plots were 2-row by 20 ft with 5 ft alleys between each block. The rows were planted on beds spaced 30 inches apart using a Max Emerge II John Deere planter. Treatment applications were initiated when silks began to appear. Treatments were applied with a backpack CO2 sprayer set at 30 psi delivering 25 gpa. The spray was directed on to the silks of all ears in the plot. The spray dates for the first planting were 27 and 30 Jun, 2,7,9, 11,14, and 16 Jul. The spray dates for the second planting were 18, 21, 23, 25, 28, and 30 Jul, 1 and 4 Aug. All ears in the middle 18 ft of each plot were collected and examined for feeding damage and larvae presence. The harvest dates were 18 Jul (first planting) and 6 Aug (second planting). All means derived from damaged ears and live larvae counts were analyzed using Tukey's Studentized range, with P ≤ 0.05.

Published
2004
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13. EVALUATION OF SELECTED INSECTICIDES FOR CONTROL OF VELVETBEAN CATERPILLAR AND SOYBEAN LOOPER ON SOYBEANS, 2002

Author

David Jenkins, J. Kurk Lance, K. Lohmeyer, and John N. All

Subjects
Horticulture, Sprayer, General Medicine, Biology, Caterpillar, biology.organism_classification, Row, Toward the head
Abstract

The test was conducted at the Southeastern Research and Education Center, Midville, GA. Soybeans were planted on 24 May on beds spaced 38 inch apart using a four row Max Emerge John Deere planter. The experimental design was RCB with four replications. The plot size was 32 x by 4 rows. Treatments were applied on 7 Aug when eight random plant shakes were averaged 5 larvae/ft of row and defoliation was approximately 8-10%. Treatments were applied with a CO2 spraying system mounted on a Powell high cycle sprayer. The sprayer traveled at a speed of 3 mph. Treatments were applied at a vol rate of 10 gpa, at 50 psi, with three nozzles/row. The nozzles were TX-3 hollow cone. Efficacy surveys were done on 14 Aug and 21 Aug. Plant shakes measuring 12 ft of row were done in the middle two rows of each plot. Larvae were counted and identified based on the following criteria. The VBC had four abdominal pro legs, smooth skin, and were a greenish-brown color. The SBL had two abdominal pro legs, body that tapered down toward the head, light green in color, and distinct looping movement. Percentage of plant defoliation rate was also assessed in each plot. Data analysis was done using ANOVA for RCB with means separation using Tukey's Studentized Range.

Published
2003
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36. THE SINS/zC-SINF SURVEY OF z ∼ 2 GALAXY KINEMATICS: REST-FRAME MORPHOLOGY, STRUCTURE, AND COLORS FROM NEAR-INFRARED HUBBLE SPACE TELESCOPE IMAGING.

Author

S. Tacchella, P. Lang, C. M. Carollo, N. M. Förster Schreiber, A. Renzini, A. E. Shapley, S. Wuyts, G. Cresci, R. Genzel, S. J. Lilly, C. Mancini, S. F. Newman, L. J. Tacconi, G. Zamorani, R. I. Davies, J. Kurk, and L. Pozzetti

Subjects
STAR formation, GALAXY formation, STELLAR evolution, OPTICAL resolution
Abstract

We present the analysis of Hubble Space Telescope (HST) J- and H-band imaging for 29 galaxies on the star-forming main sequence at z ∼ 2, which have adaptive optics Very Large Telescope SINFONI integral field spectroscopy from our SINS/zC-SINF program. The SINFONI Hα data resolve the ongoing star formation and the ionized gas kinematics on scales of 1–2 kpc; the near-IR images trace the galaxies’ rest-frame optical morphologies and distributions of stellar mass in old stellar populations at a similar resolution. The global light profiles of most galaxies show disk-like properties well described by a single Sérsic profile with , with only requiring a high Sérsic index, all more massive than . In bulge+disk fits, about 40% of galaxies have a measurable bulge component in the light profiles, with showing a substantial bulge-to-total ratio (B/T) . This is a lower limit to the frequency of z ∼ 2 massive galaxies with a developed bulge component in stellar mass because it could be hidden by dust and/or outshined by a thick actively star-forming disk component. The galaxies’ rest-optical half-light radii range between 1 and 7 kpc, with a median of 2.1 kpc, and lie slightly above the size–mass relation at these epochs reported in the literature. This is attributed to differences in sample selection and definitions of size and/or mass measurements. The color gradient and scatter within individual z ∼ 2 massive galaxies with are as high as in z = 0 low-mass, late-type galaxies and are consistent with the high star formation rates of massive z ∼ 2 galaxies being sustained at large galactocentric distances. [ABSTRACT FROM AUTHOR]

Published
2015
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37. Searching for large-scale structures around high-redshift radio galaxies with Herschel

Author

Bram Venemans, A. Saro, R. Herbonnet, E. E. Rigby, H. J. A. Röttgering, Helmut Dannerbauer, F. Maschietto, Nina A. Hatch, George K. Miley, Nick Seymour, Yi-Kuan Chiang, G. De Lucia, Jaron Kurk, Roderik Overzier, David L. Clements, C. De Breuck, Stefano Borgani, Bruce Sibthorpe, E. E., Rigby, N. A., Hatch, H. J. A., Rottgering, B., Sibthorpe, Y. K., Chiang, R., Overzier, R., Herbonnet, Borgani, Stefano, D. L., Clement, H., Dannerbauer, C., De Breuck, G., De Lucia, J., Kurk, F., Maschietto, G., Miley, A., Saro, N., Seymour, and B., Venemans

Subjects
Luminous infrared galaxy, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio galaxy, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics, galaxies: general, galaxies [infrared], galaxies: clusters: general, galaxies: high-redshift, infrared: galaxies, Redshift, Space observatory, Galaxy, Spire, Space and Planetary Science, clusters: general [galaxies], high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics, general [galaxies]
Abstract

This paper presents the first results of a far-infrared search for protocluster-associated galaxy overdensities using the SPIRE instrument on-board the {\it Herschel} Space Observatory. Large ($\sim$400 arcmin$^{2}$) fields surrounding 26 powerful high-redshift radio galaxies ($2.0 < z < 4.1$; $L_{\rm 500 MHz} > 10^{28.5}$ WHz$^{-1}$) are mapped at 250, 350 and 500\mic to give a unique wide-field sample. On average the fields have a higher than expected, compared to blank fields, surface density of 500\mic sources within 6 comoving Mpc of the radio galaxy. The analysis is then restricted to potential protocluster members only, which are identified using a far-infrared colour selection; this reveals significant overdensities of galaxies in 2 fields, neither of which are previously known protoclusters. The probability of finding 2 overdensities of this size by chance, given the number of fields observed is $5 \times 10^{-4}$. Overdensities here exist around radio galaxies with $L_{\rm 500 MHz} \gtrsim 10^{29}$ WHz$^{-1}$ and $z < 3$. The radial extent of the average far-infrared overdensity is found to be $\sim$6 comoving Mpc. Comparison with predictions from numerical simulations shows that the overdensities are consistent with having masses $> 10^{14}$Msolar. However, the large uncertainty in the redshift estimation means that it is possible that these far-infrared overdensities consist of several structures across the redshift range searched., 13 pages, 9 figures; Accepted for publication in MNRAS

Published
2014

38. Listening to galaxies tuning atz~ 2.5–3.0: The first strikes of the Hubble fork

Author

Alvio Renzini, Margherita Talia, Lucia Pozzetti, Claire Halliday, M. Mignoli, Jaron Kurk, Andrea Cimatti, M. Talia, A. Cimatti, M. Mignoli, L. Pozzetti, A. Renzini, J. Kurk, and C. Halliday

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Morphological type, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Rest frame, Redshift, Galaxy, Spectral line, Hubble sequence, Bimodality, symbols.namesake, galaxies: high-redshift, Space and Planetary Science, Morphological analysis, symbols, galaxies: structure, galaxies: formation, galaxies: evolution, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the morphological properties of 494 galaxies selected from the GMASS survey at z>1, primarily in their optical rest frame, using HST images, from the CANDELS survey. We propose that the Hubble sequence of galaxy morphologies takes shape at redshift 2.51, such that at redshifts z=2.5-2.7 and above, the Hubble types cannot be identified, and most galaxies are classified as irregular. The quantitative morphological analysis shows that, at 1, Comment: 27 pages, 16 figures, 5 tables. "Morphological atlas" in the appendix. Revised version accepted for publication in A&A

Published
2014
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39. ACTIVE GALACTIC NUCLEUS FEEDBACK AT z ∼ 2 AND THE MUTUAL EVOLUTION OF ACTIVE AND INACTIVE GALAXIES

Author

Alvio Renzini, C. Halliday, G. Rodighiero, E. Daddi, M. Mignoli, Margherita Talia, Paolo Cassata, Marcella Brusa, A. Cimatti, J. D. Kurk, A. Cimatti, M. Brusa, M. Talia, M. Mignoli, G. Rodighiero, J. Kurk, P. Cassata, C. Halliday, A. Renzini, and E. Daddi

Subjects
Physics, Active galactic nucleus, Stellar mass, 010308 nuclear & particles physics, Star formation, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Spectral line, Redshift, Luminosity, Interstellar medium, Space and Planetary Science, 0103 physical sciences, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The relationship between galaxies of intermediate stellar mass and moderate luminosity active galactic nuclei (AGNs) at 1 < z < 3 is investigated with a Galaxy Mass Assembly ultra-deep Spectroscopic Survey (GMASS) sample complemented with public data in the GOODS-South field. Using X-ray data, hidden AGNs are identified in unsuspected star-forming galaxies with no apparent signs of non-stellar activity. In the color-mass plane, two parallel trends emerge during the ~2 Gyr between the average redshifts z ~ 2.2 and z ~ 1.3: while the red sequence becomes significantly more populated by ellipticals, the majority of AGNs with L(2-10 keV) > 1042.3 erg s–1 disappear from the blue cloud/green valley where they were hosted predominantly by star-forming systems with disk and irregular morphologies. These results are even clearer when the rest-frame colors are corrected for dust reddening. At z ~ 2.2, the ultraviolet spectra of active galaxies (including two Type 1 AGNs) show possible gas outflows with velocities up to about –500 km s–1, which are observed neither in inactive systems at the same redshift, nor at lower redshifts. Such outflows indicate the presence of gas that can move faster than the escape velocities of active galaxies. These results suggest that feedback from moderately luminous AGNs (log LX < 44.5 erg s–1) played a key role at z >~ 2 by contributing to outflows capable of ejecting part of the interstellar medium and leading to a rapid decrease in star formation in host galaxies with stellar masses 10 < log({\cal M}/M_{\odot }) 11.

Published
2013
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40. Computer visualization techniques (CVTs) foster evidence-based target delineation.

Author

Butler EB, Shukla V, Paulino AC, Lu HH, Butler R, Smiedala M, Kurk J, Grant WH 3rd, McGary JE, and Teh BS

Subjects
Humans, Radiation Oncology instrumentation, Radiotherapy Planning, Computer-Assisted instrumentation, Image Processing, Computer-Assisted, Neoplasms radiotherapy, Radiation Oncology methods, Radiotherapy Planning, Computer-Assisted methods
Abstract

Computer visualization techniques (CVTs) are an emerging technology that can organize all cancer specialists. This article describes CVTs' ability to maximize the currently untapped advantages of intensity modulated radiotherapy (IMRT). The visual speed and dynamic strategies inherent in CVTs improves IMRT by distilling vast amounts of anatomic, multimodal imaging, textual/meaning, and surgical/outcome data into a large, rigorous, standardized evidence base of storable target delineation plans. This ability to standardize strategies will allow the collection of meaningful evidence based outcome data.

Published
2007
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41. Evaluation technique for bileaflet mechanical valves.

Author

Shipkowitz T, Ambrus J, Kurk J, and Wickramasinghe K

Subjects
Blood Flow Velocity physiology, Cross-Sectional Studies, Humans, Image Processing, Computer-Assisted methods, Models, Cardiovascular, Prosthesis Design methods, Pulsatile Flow physiology, Rheology methods, Stress, Mechanical, Video Recording methods, Heart Valve Prosthesis
Abstract

Background and Aims of the Study: Several techniques were utilized to evaluate the performance of bileaflet mechanical heart valves and improve upon current valve designs., Methods: Particle image velocimetry (PIV), computational fluid dynamics (CFD) and video analysis were used to evaluate St. Jude Medical (SJM) and ATS valves in an abrupt enlargement outlet chamber. Video analysis and PIV provided information on the opening angle of the leaflets and 2D velocity fields. PAM-FLOW CFD software was used to predict flow through the valves with leaflets in the fully open position, which corresponds to steady flow conditions in the experimental study. The ATS valve was also modeled at its reported incomplete leaflet opening angle, and with an orifice modification. Additional CFD techniques were employed to find the natural opening angle of the ATS valve., Results: In steady and pulsatile flow, the SJM leaflets opened completely. PIV showed three fairly uniform jets passing through the SJM valve. CFD analysis of the pressure distribution across the SJM valve showed a resultant moment in the open direction, indicating that the leaflets were held against the open stops at 85 degrees. In both steady and pulsatile flow, the leaflets in the ATS valve did not open to the designed opening angle. From video analysis, the ATS leaflet opening angle was estimated at 72-76 degrees. PIV showed that the incomplete opening angle of the ATS leaflets produced a large wake region behind the leaflets, and lateral jets that impinged on the side walls of the test chamber. CFD analysis showed a pressure distribution across the ATS valve which produced a moment causing the leaflets not to open to 85 degrees. The equilibrium position of the leaflet was approximately 75 degrees. The leaflets in the CFD model opened to the full 85 degrees when the orifice was increased by 2 mm on the outflow side., Conclusion: The combination of techniques used in this study provided a method that will be useful in evaluating new valve designs. It was learned that leaflet position, pivot location and orifice height influence pressure distribution across the leaflets, thereby affecting the opening angle.

Published
2002

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