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375 results on '"Mullan, B. P."'

1. The \^G Infrared Search for Extraterrestrial Civilizations with Large Energy Supplies. II. Framework, Strategy, and First Result

Author

Wright, J. T., Griffith, R., Sigurðsson, S., Povich, M. S., and Mullan, B.

Subjects
Physics - Popular Physics, Astrophysics - Astrophysics of Galaxies
Abstract

We describe the framework and strategy of the \^G infrared search for extraterrestrial civilizations with large energy supplies, which will use the wide-field infrared surveys of WISE and Spitzer to search for these civilizations' waste heat. We develop a formalism for translating mid-infrared photometry into quantitative upper limits on extraterrestrial energy supplies. We discuss the likely sources of false positives, how dust can and will contaminate our search, and prospects for distinguishing dust from alien waste heat. We argue that galaxy-spanning civilizations may be easier to distinguish from natural sources than circumstellar civilizations (i.e., Dyson spheres), although Gaia will significantly improve our capability to identify the latter. We present a "zeroth order" null result of our search based on the WISE all-sky catalog: we show, for the first time, that Kardashev Type III civilizations (as Kardashev originally defined them) are very rare in the local universe. More sophisticated searches can extend our methodology to smaller waste heat luminosities, and potentially entirely rule out (or detect) both Kardashev Type III civilizations and new physics that allows for unlimited "free" energy generation., Comment: 15 pages, 4 figures, accepted for publication in the Astrophysical Journal

Published
2014
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2. The \^G Infrared Search for Extraterrestrial Civilizations with Large Energy Supplies. I. Background and Justification

Author

Wright, J. T., Mullan, B., Sigurðsson, S., and Povich, M. S.

Subjects
Physics - Popular Physics, Astrophysics - Astrophysics of Galaxies
Abstract

We motivate the \^G infrared search for extraterrestrial civilizations with large energy supplies. We discuss some philosophical difficulties of SETI, and how communication SETI circumvents them. We review "Dysonian SETI", the search for artifacts of alien civilizations, and find that it is highly complementary to traditional communication SETI; the two together might succeed where either one, alone, has not. We discuss the argument of Hart (1975) that spacefaring life in the Milky Way should be either galaxy-spanning or non-existent, and examine a portion of his argument that we dub the "monocultural fallacy". We discuss some rebuttals to Hart that invoke sustainability and predict long Galaxy colonization timescales. We find that the maximum Galaxy colonization timescale is actually much shorter than previous work has found ($< 10^9$ yr), and that many "sustainability" counter-arguments to Hart's thesis suffer from the monocultural fallacy. We extend Hart's argument to alien energy supplies, and argue that detectably large energy supplies can plausibly be expected to exist because life has potential for exponential growth until checked by resource or other limitations, and intelligence implies the ability to overcome such limitations. As such, if Hart's thesis is correct then searches for large alien civilizations in other galaxies may be fruitful; if it is incorrect, then searches for civilizations within the Milky Way are more likely to succeed than Hart argued. We review some past Dysonian SETI efforts, and discuss the promise of new mid-infrared surveys, such as that of WISE., Comment: 18 pages, accepted for publication in the Astrophysical Journal

Published
2014
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3. Under Pressure: Star Clusters and the Neutral Hydrogen Medium of Tidal Tails

Author

Mullan, B., Kepley, A. A., Maybhate, A., English, J., Knierman, K., Hibbard, J. E., Bastian, N., Charlton, J. C., Durrell, P. R., Gronwall, C., Elmegreen, D., and Konstantopoulos, I. S.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using archival data from ATCA, WSRT, and the VLA, we have analyzed the HI emission of 22 tidal tail regions of the Mullan et al. sample of pairwise interacting galaxies. We have measured the column densities, line-of-sight velocity dispersions, and kinetic energy densities on ~kpc scales. We also constructed a tracer of the line-of-sight velocity gradient over ~10 kpc scales. We compared the distributions of these properties between regions that do and do not contain massive star cluster candidates (M_V < -8.5; ~10^4--10^6 M_(sun) as observed in HST WFPC2 VI data). In agreement with Maybhate et al., we find that a local, ~kpc-scale column density of log N_(HI) = 20.6 cm^(-2) is frequently required for detecting clustered star formation. This HI gas also tends to be turbulent, with line-of-sight velocity dispersions ~10--75 km/s, implying high kinetic energy densities (>46 erg pc^(-2)). Thus, high HI densities and pressures, partly determined by the tail dynamical age and other interaction characteristics, are connected to large-scale cluster formation in tidal tails overall. Lastly, we find that the high mechanical energy densities of the gas are likely not generally due to feedback from star formation. Rather, these properties are more likely to be a cause of star formation than a result., Comment: Accepted for publication in the Astrophysical Journal (online figure sets to appear in the electronic edition). 44 pages, 11 figures, 5 tables

Published
2013
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4. Gemini Spectroscopic Survey of Young Star Clusters in Merging/Interacting Galaxies. IV. Stephan's Quintet

Author

Trancho, G., Konstantopoulos, I., Bastian, N., Fedotov, K., Gallagher, S., Mullan, B., and Charlton, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a spectroscopic survey of 21 young massive clusters and complexes and one tidal dwarf galaxy candidate (TDG) in Stephan's Quintet, an interacting compact group of galaxies. All of the selected targets lie outside the main galaxies of the system and are associated with tidal debris. We find clusters with ages between a few and 125 Myr and confirm the ages estimated through HST photometry by Fedotov et al. (2011), as well as their modelled interaction history of the Quintet. Many of the clusters are found to be relatively long-lived, given their spectrosopically derived ages, while their high masses suggest that they will likely evolve to eventually become intergalactic clusters. One cluster, T118, is particularly interesting, given its age (\sim 125 Myr), high mass (\sim 2\times10^6 M\odot) and position in the extreme outer end of the young tidal tail. This cluster appears to be quite extended (Reff \sim 12 - 15 pc) compared to clusters observed in galaxy disks (Reff \sim 3 - 4 pc), which confirms an effect we previously found in the tidal tails of NGC 3256, where clusters are similarly extended. We find that star and cluster formation can proceed at a continuous pace for at least \sim 150 Myr within the tidal debris of interacting galaxies. The spectrum of the TDG candidate is dominated by a young population (\sim 7 Myr), and assuming a single age for the entire region, has a mass of at least 10^6 M\odot., Comment: 37 pages, 10 Figures, 7 Table

Published
2012
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5. NEOWISE Observations of Near-Earth Objects: Preliminary Results

Author

Mainzer, A., Grav, T., Bauer, J., Masiero, J., McMillan, R. S., Cutri, R. M., Walker, R., Wright, E., Eisenhardt, P., Tholen, D. J., Spahr, T., Jedicke, R., Denneau, L., DeBaun, E., Elsbury, D., Gautier, T., Gomillion, S., Hand, E., Mo, W., Watkins, J., Wilkins, A., Bryngelson, G. L., Molina, A. Del Pino, Desai, S., Camus, M. Go'mez, Hidalgo, S. L., Konstantopoulos, I., Larsen, J. A., Maleszewski, C., Malkan, M. A., Mauduit, J. -C., Mullan, B. L., Olszewski, E. W., Pforr, J., Saro, A., Scotti, J. V., and Wasserman, L. H.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

With the NEOWISE portion of the \emph{Wide-field Infrared Survey Explorer} (WISE) project, we have carried out a highly uniform survey of the near-Earth object (NEO) population at thermal infrared wavelengths ranging from 3 to 22 $\mu$m, allowing us to refine estimates of their numbers, sizes, and albedos. The NEOWISE survey detected NEOs the same way whether they were previously known or not, subject to the availability of ground-based follow-up observations, resulting in the discovery of more than 130 new NEOs. The survey's uniformity in sensitivity, observing cadence, and image quality have permitted extrapolation of the 428 near-Earth asteroids (NEAs) detected by NEOWISE during the fully cryogenic portion of the WISE mission to the larger population. We find that there are 981$\pm$19 NEAs larger than 1 km and 20,500$\pm$3000 NEAs larger than 100 m. We show that the Spaceguard goal of detecting 90% of all 1 km NEAs has been met, and that the cumulative size distribution is best represented by a broken power law with a slope of 1.32$\pm$0.14 below 1.5 km. This power law slope produces $\sim13,200\pm$1,900 NEAs with $D>$140 m. Although previous studies predict another break in the cumulative size distribution below $D\sim$50-100 m, resulting in an increase in the number of NEOs in this size range and smaller, we did not detect enough objects to comment on this increase. The overall number for the NEA population between 100-1000 m are lower than previous estimates. The numbers of near-Earth comets will be the subject of future work., Comment: Accepted to ApJ

Published
2011
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6. Star Clusters in the Tidal Tails of Interacting Galaxies: Cluster Populations Across a Variety of Tail Environments

Author

Mullan, B., Konstantopoulos, I. S., Kepley, A. A., Lee, K. H., Charlton, J. C., Knierman, K., Bastian, N., Chandar, R., Durrell, P. R., Elmegreen, D., English, J., Gallagher, S. C., Gronwall, C., Hibbard, J. E., Hunsberger, S., Johnson, K. E., Maybhate, A., Palma, C., Trancho, G., and Vacca, W. D.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We have searched for compact stellar structures within 17 tidal tails in 13 different interacting galaxies using F606W- and F814W- band images from the Wide Field Planetary Camera 2 (WFPC2) on the Hubble Space Telescope (HST). The sample of tidal tails includes a diverse population of optical properties, merging galaxy mass ratios, HI content, and ages. Combining our tail sample with Knierman et al. (2003), we find evidence of star clusters formed in situ with Mv < -8.5 and V-I < 2.0 in 10 of 23 tidal tails; we are able to identify cluster candidates to Mv = -6.5 in the closest tails. Three tails offer clear examples of "beads on a string" star formation morphology in V-I color maps. Two tails present both tidal dwarf galaxy (TDG) candidates and cluster candidates. Statistical diagnostics indicate that clusters in tidal tails may be drawn from the same power-law luminosity functions (with logarithmic slopes ~ -2 - -2.5) found in quiescent spiral galaxies and the interiors of interacting systems. We find that the tail regions with the largest number of observable clusters are relatively young (< 250 Myr old) and bright (V < 24 mag arcsec^(-2)), probably attributed to the strong bursts of star formation in interacting systems soon after periapse. Otherwise, we find no statistical difference between cluster-rich and cluster-poor tails in terms of many observable characteristics, though this analysis suffers from complex, unresolved gas dynamics and projection effects., Comment: Accepted for publication in the Astrophysical Journal. 27 pages, 8 figures

Published
2011
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7. Tidal Tails in Interacting Galaxies: Formation of Compact Stellar Structures

Author

Mullan, B., Charlton, J. C., Konstantopoulos, I. S., Bastian, N., Chandar, R., Durrell, P. R., Elmegreen, D., English, J., Gallagher, S. C., Gronwall, C., Hibbard, J. E., Hunsberger, S., Johnson, K. E., Kepley, A., Knierman, K., Koribalski, B., Lee, K. H., Maybhate, A., Palma, C., and Vacca, W. D.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics, Astrophysics - Galaxy Astrophysics
Abstract

We have used V- and I- band images from the Hubble Space Telescope (HST) to identify compact stellar clusters within the tidal tails of twelve different interacting galaxies. The seventeen tails within our sample span a physical parameter space of HI/stellar masses, tail pressure and density through their diversity of tail lengths, optical brightnesses, mass ratios, HI column densities, stage on the Toomre sequence, and tail kinematics. Our preliminary findings in this study indicate that star cluster demographics of the tidal tail environment are compatible with the current understanding of star cluster formation in quiescent systems, possibly only needing changes in certain parameters or normalization of the Schechter cluster initial mass function (CIMF) to replicate what we observe in color-magnitude diagrams and a brightest absolute magnitude -- log N plot., Comment: To appear in the Proceedings of the Galaxy Wars: Stellar Populations and Star Formation in Interacting Galaxies Conference

Published
2009

8. Using the health action process approach to predict and improve health outcomes in individuals with type 2 diabetes mellitus

Author

MacPhail M, Mullan B, Sharpe L, MacCann C, and Todd J

Subjects
Specialties of internal medicine, RC581-951
Abstract

Mariana MacPhail,1 Barbara Mullan,2 Louise Sharpe,1 Carolyn MacCann,1 Jemma Todd1 1School of Psychology, University of Sydney, Sydney, NSW, Australia; 2School of Psychology and Speech Pathology, Curtin University, Bentley, WA, Australia Background: The purpose of this study was to explore the predictive utility of the Health Action Process Approach (HAPA) and test a HAPA-based healthy eating intervention, in adults with type 2 diabetes mellitus. Materials and methods: The study employed a prospective, randomized, controlled trial design. The 4-month intervention consisted of self-guided HAPA-based workbooks in addition to two telephone calls to assist participants with the program implementation, and was compared to “treatment as usual”. Participants (n=87) completed health measures (diet, body mass index [BMI], waist circumference, blood pressure, blood glucose levels, lipid levels, and diabetes distress) and HAPA measures prior to the intervention and again upon completion 4 months later. Results: The overall HAPA model predicted BMI, although only risk awareness and recovery self-efficacy were significant independent contributors. Risk awareness, intentions, and self-efficacy were also independent predictors of health outcomes; however, the HAPA did not predict healthy eating. No significant time × condition interaction effects were found for diet or any HAPA outcome measures. Conclusion: Despite the success of HAPA in predicting health outcomes for those with type 2 diabetes mellitus, the intervention was unsuccessful in changing healthy eating or any of the other measured variables, and alternative low-cost health interventions for those with type 2 diabetes mellitus should be explored. Keywords: intervention, healthy eating, theory, risk awareness, self-efficacy

Published
2014

11. Poster display IV experimental and instrumentation

Author

Masoli, O. Osvaldo, Redruello, M., Ogresta, F., Collaud, C., Koslowski, P., Baliño, N. Perez, Eleta, M., Arce, P., Vidal, L., Kardash, O., Maroz-Vadalajskaya, N. Natalia, Vanhove, C. Christian, Lahoutte, T., Defrise, M., Andreyev, A., Bossuyt, A., Franken, P. R., Franken, P. R. Philippe, Lahoutte, T., Maskali, F., Vanhove, C., Nloga, J., Tran, N., Marie, P. Y., Peix, A. Amalia, Garcia-Barreto, D., Ponce, F., Cabrera, L. O., Valiente, J., Tornes, F., Guerrero, I., Heres, F., Garcia, E. J., Cabale, B., Bindslev, L. Lene, Bisgaard, K. B. Kirsten, Haack-Soerensen, M. H. S. Mandana, Mortensen, S. M. Steen, Kragh, L. K. Linda, Kjaer, A. K. Andreas, Kastrup, J. K. Jens, Hesse, B. H. Birger, Aboul-Enein, F. Fatma, Battah, A., Fattah, A. Abdel, Atty, A. Abdel, Allam, A., Riou, L. Laurent, Broisat, A., Ghezzi, C., Lartizien, C., Berthonneche, C., Toufektsian, M. C., Maitrejean, S., Janier, M., Vanzetto, G., Fagret, D., Rouzet, F. Francois, Daou, D., Lebtahi, R., Frank, R., Leenhardt, A., Slama, M., Guludec, D. Le, Sarda-Mantel, L. Laure, Michel, J. B., Rouzet, F., Martet, G., Meulemans, A., Vrigneaud, J. M., Guludec, D. Le, Daou, D. Doumit, Coaguila, C., Benada, A., Razzouk, M., Idy-Peretti, I., Guludec, D. Le, Vilain, D., Lebtahi, R., Guludec, D. Le, Stegger, L. Lars, Schäfers, K., Flögel, U., Schrader, J., Schober, O., Levkau, B., Schäfers, M., Kies, P. Peter, Wichter, T., Schäfers, K. P., Schäfers, M., Wielepp, J. P. Peter, Baller, D., Pulawski, E., Weise, R., Fricke, E., Horstkotte, D., Burchert, W., Eckert, S., Dongas, A., Horstkotte, D., Burchert, W., Nekolla, S. G. Stephan, Martinez, M. J., Howe, W., Kehren, F., Ziegler, S. I., Vassiliadis, I. Ioannis, Souretis, G., Komporozos, C., Fountos, A., Papademetriou, A., Spanos, A., Antoniou, A., Strembelas, P., Moralidis, E. Efstratios, Arsos, G., Boundas, D., Georga, S., Karatzas, N., Karakatsanis, K., Prassopoulos, V. Vassilios, Parthenakis, F., Patrianakos, A., Koukouraki, S., Velidaki, A., Karkavitsas, N., Vardas, P., Velidaki, A. Antigone, Perisinakis, K., Koukouraki, S., Koutsikos, J., Prassopoulos, V., Vardas, P., Karkavitsas, N., Sundaraiya, S. Sumati, Sumati, S., Sambhasivam, KA., David, S., Zakavi, S. R. Seyed Rasoul, Kakhki, V. R. Dabagh, Jabari, H., Zingerman, B., Bendayan, D., Sagie, A., Solodky, A., Mats, I., Shapira, Y., Kremer, M. R., Zafrir, N. Nili, Rimini, M. L. Maria Luisa De, Catalano, M., Bonzani, G., Scalzone, A., Merenda, R., Monteforte, I., Monda, V., Muto, P., Carboni, G. P. Gian Piero, Miglionico, M., Tavolozza, M., Marcassa, C. Claudio, Campini, R., Calza, P., Giannuzzi, P., Eleuteri, E., Marcassa, C. Claudio, Campini, R., Scapellato, F., Temporelli, P. L., Giannuzzi, P., Pellegrino, T., Storto, G., Sorrentino, A. R., Silvestri, A., Filardi, P. Perrone, Brevetti, G., Cuocolo, A. Alberto, Cho, K. Keiichi, Kumita, S., Seino, K., Nakajo, H., Toba, M., Kumazaki, T., Muramatsu, T. Toshihiro, Yamazaki, T., Seki, K., Kawanami, J., Nakajima, T., Yamada, Y., Suga, T., Matsumoto, K., Nishimura, S., Taki, J. Junichi, Higuchi, T., Kawashima, A., Nakajima, K., Muramori, A., Matsunari, I., Tait, J. F., Vanderheyden, J. L., Strauss, H. W., Tonami, N., Adachi, I. Itaru, Shimomura, H., Kintaka, T., Komori, T., Ogura, Y., Kitaura, Y., Narabayashi, I., Iida, H. Hidehiro, Zeniya, T., Kim, K. M., Watabe, H., Teramoto, N., Yamamichi, Y., Alexanderson, E. Erick, Ricalde, A., Vargas, A., Meave, A., Amigo, M. C., Misko, J., Dziuk, M. Miroslaw, Warczynska, A., Skrobowska, E., Vasconcelos, M. Mariana, Martins, E., Faria, T., Oliveira, A., Pardal, N., Macedo, F., Pereira, J., Rocha-Gonçalves, F., Cantinho, G. Guilhermina, Pena, H., Freire, L., Veiga, A., Gonçalves, P., Godinho, F., Chua, T. Terrance, Lee, C. Y., Keng, F., Ding, Z. P., Koh, T. H., Awamleh, P. Paula, Talavera, P., Torres, V., Balsa, M. A., González, O., Alberca, M. T., Miguel, R., Cosío, F. G., Lomsky, M. Milan, Richter, J., Johansson, L., El-Ali, H., Åström, K., Ljungberg, M., Edenbrandt, L., Hung, G. U. Guang-Uei, Lee, K. W., Chen, C. P., Yang, K. T., Pekindil, G., Sarikaya, A. Ali, Ege, T., Salihoglu, S., Entok, E. Emre, Cavusoglu, Y., Ak, I., Vardareli, E., Timuralp, B., Tout, D. Deborah, Loong, C. Y., Naidoo, V. V., Aswegen, A. Van, Underwood, S. R., Thorley, P. J. Penelope, Goris, M. Michael, ZHU, H. J., Clements, I. P. Ian, Mullan, B. P., O’Connor, M. K., Breen, J. F., McGregor, C. G. A., Liu, Y. H. Yi-Hwa, Li, S., Bourke, B., Weyman, C., Sinusas, A. J., Ramakrishna, G. Gautam, Miller, T. D., O’Connor, M. K., Gibbons, R. J., Tsatkin, V., Wackers, F. J. T. H., Liu, Y. H. Yi-Hwa, Tsatkin, V., Prior, J. O. John, Facta, A. D., Schindler, T. H., Oxilia-Estigarribia, M. A., Hernandez-Pampaloni, M., Campisi, R., Zhang, X., Bischof-Delaloye, A., Nathan, L., Schelbert, H. R., Gullberg, G. T. Grant, Huesman, R. H., Reutter, B. W., Sitek, A., Veress, A. I., Weiss, J. A., Qi, J., Yang, Y., Gordi, T. Toufigh, Olmsted, A., Lieu, H., and Belardinelli, L.

Published
2005
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12. Poster display I clinical general

Author

Gurgenyan, S. V. Svetlana, Vatinyan, S. K. H., Nicogosyan, K. G., Edilyan, L. B., Chobanyan, B. G., Graf, S., Beheshti, M., Kienast, O., Oezer, S., Angelberger, P., Dudczak, R., Li, S. Shuren, Azevedo, J. C. Jader, Félix, R. C., Corrêa, P. L., Barbirato, G. B., Mesquita, E. T., Volschan, A., Dohmann, H. F., Mesquita, C. T., Peix, A. Amalia, Hidalgo, J., Dorticos, E., Llerena, L., Paredes, A., Macias, C., Valle, L. Del, Cortinas, L., Torres, M., Ponce, F., Petersen, C. L. Claus Leth, Appel, J., Kjaer, A., Awadalla, H. Hany, Hamed, R., Jamal, M., Rayan, M., Mahmoodi, A., Awaad, O., Demerdash, S. El, Adel, A., Kader, M. Abdel, Sarda-Mantel, L. Laure, Michel, J. B., Rouzet, F., Martet, G., Louedec, L., Raguin, O., Vrigneaud, J. M., Saumon, G., Khaw, B. A., Guludec, D. Le, Delahaye, N. Nicolas, Dinanian, S., Slama, M. S., Sarda, L., Tamas, C., Samuel, D., Adams, D., Syrota, A., Moralidis, E. Efstratios, Spyridonidis, T., Arsos, G., Karatzas, N., Karakatsanis, K., Koutelou, M. Maria, Theodorakos, A., Kollaros, N., Manginas, A., Graphakos, S., Tsapaki, V., Kouzoumi, A., Cokkinos, D., Goussetis, E., Prassopoulos, V. Vassilios, Parthenakis, F., Patrianakos, A., Velidaki, A., Koukouraki, S., Papadimitriou, E., Diakakis, G., Maurakis, H., Karakavitsas, N., Vardas, P., Koszegi, Z. Zsolt, Jenei, C., Varga, J., Galuska, L., Edes, I., Ray, Soumendranath, Kundu Bijon, Sarma S K., Day N R., Skouse, D. Douglas, Florimonte, L., Maffioli, L., Piatti, L., Calegari, M., Mancini, R., Bossi, M., Carboni, G. P. Gian Piero, Toriyama, T., Takase, H. Hiroyuki, Okado, T, Tanaka, S., Dohi, Y., Yasuhi, W. Watanabe, Akihiro, S., Akio, Y., Yasunori, W., Kimio, T., Nariaki, E., Yasuhiko, T., Ryo, K., Kasama, S. Shu, Honjo, T., Ichikawa, S., Toyama, T., Kurabayashi, M., Furuhashi, T. Tatsuhiko, Moroi, M., Kunimasa, T., Fukuda, H., Sugi, K., Takeishi, Y. Yasuchika, Arimoto, T., Kubota, I., Kambara, N. Naoshige, Hosokawa, R., Ohba, M., Saito, K., Motomura, H., Kanoi, T., Kume, N., Saji, H., Kita, T., Nohara, R., Akashi, Y. J. Yoshihiro, Musha, H., Kida, K., Suzuki, K., Inoue, K., Kawasaki, K., Hashimoto, N., Miyake, F., Yokoyama, Y. Yasuhiro, Sato, A., Nozato, T., Takahashi, A., Isobe, M., Aonuma, K., Hiroe, M., Peovska, I. Irena, Bosevski, M., Pavlovic, J.Maksimovic, Vavlukis, M., Vallejo, E. Enrique, Rodriguez, G., Jimenez, L., Hernandez, S., Bialostozky, D., Orea, A. Arturo, Asensio, E., Castillo, L., Dorantes, J., Narvaez, R., Gonzalez, O., Zee, P. M. Marc Van der, Verberne, H. J., Straalen, J. P. Van, Fischer, J. C., Sanders, G. T. B., Eck-Smit, B. L. F. Van, Winter, R. J. De, Kostkiewicz, M. Magdalena, Szot, W., Mura, A., Lesniak-Sobelga, A., Olszowska, M., Tracz, W., Ferreira, M. J. Maria Joao, Ferrer-Antunes, A. I., Rodrigues, V., Santos, F., Lima, J., Cerqueira, M. D., Providencia, L. A., Rodrigues, V., Martins, E., Vasconcelos, M. Mariana, Faria, T., Oliveira, A., Garcia, M., Pereira, J., Rocha-Goncalves, F., Lourenço, C. Cândida, Ferrer-Antunes, A., Vieira, H., Martins, R., Franco, F., Providência, L. A., Flotats, A. Albert, Estorch, M., Estorch, M. Montserrat, Mena, E., Camacho, V., Fuertes, J., Rodriguez, A., Flotats, A., Hernandez, M. A., Kulisewsky, J., Carrio, I., Jose-Galcera, J., Caballero-Martínez, A., Jara-Perez, P., Villegas-Garcia, M., Iñigo-García, L., Rosa, J. A. Nuño de la, Florenciano-Sánchez, R., Castillo-Soria, J. F., Valentí-Aldeguer, J. A., Pico-Aracil, F., Martínez-Caballero, A., Villegas-García, M., Castillo-Soria, F., Sánchez-Villanueva, J. G., Rosa, J. A. Nuço de la, Içigo-García, L., Palop, R., Florenciano-Sanchez, R., Lopez-Martínez, I., Jara-Pñrez, P., Rosa, J. A. Nuno de la, Castillo-Soria, F. J., Jara-Pérez, P., Contreras, J., Villegas-Sánchez, M., Obrador, D., Puig, M., Serra-Grima, R., Santaló, M., Carrió, I., Sorensen, J. Jens, Frostfeldt, G., Lindahl, B., Valind, S., Wallentin, L., Somsen, G. A. Aernout, Burri, H., Zaza, S., Fleury, E., Righetti, A., Entok, E. Emre, Birdane, A., Cavusoglu, Y., Ak, I., Timuralp, B., Haworth, M. J., Mitchell, A. R. J. Andrew, Gardner, M. A., Ormerod, O. J. M., Clements, I. P. Ian, Mullan, B. P., MacGregor, C. G., Breen, J. F., Akinboboye, O. O., Nichols, K. J., Wang, Y., Dim, U. Uzodinma, Lachman, J., Nichols, K. J., Muratore, K. A., Aracely, N., Haag, E. S., Druz, R. S. Regina, Gopal, A. S., Borges, A., Ngai, K. C., Dim, U. R., Wiley, M., Freeman, J., Kitchen, S., Graham, D., Schindel, M., Clark, E., Speiser, D., Hackney, T., Feldkamp, M., and Rosamond, T. Thomas

Published
2005
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32. Determination of the optimum standardised ileal digestible sulphur amino acids to lysine ratio in weaned pigs challenged with enterotoxigenic Escherichia coli

Author

Capozzalo, M. M., Resink, J. W., Htoo, J. K., Kim, J. C., de Lange, F. M., Mullan, B. P., Hansen, C. F., Pluske, J. R., Capozzalo, M. M., Resink, J. W., Htoo, J. K., Kim, J. C., de Lange, F. M., Mullan, B. P., Hansen, C. F., and Pluske, J. R.

Abstract

This experiment tested the hypothesis that pigs challenged with an enterotoxigenic strain of E. coli (ETEC) would require a higher sulphur amino acids (SAA) to Lys ratio (SAA:Lys). Pigs (n = 120) weighing 7.4 ± 0.52 kg (mean ± SD) and weaned at 27 d (Pietrain genotype, mixed sex) were stratified into 1 of 6 treatments based on weaning weight, sex and genotype for the F4 fimbria receptor (n = 20). Five diets were formulated with increasing ratios of standardised ileal digestible (SID) sulphurSAA:Lys. Pigs were housed in pens of 4 during an adaptation period of 6 d after which time pigs were housed individually. Pigs fed different SID SAA:Lys levels were infected with ETEC (5 mL, 1.13 × 108 CFU/mL, serotype O149:K91:K88) on d 8, 9, and 10 after weaning. The sixth diet, which contained 0.55 SID SAA:Lys and corresponded to current NRC recommendations, was allocated to 2 groups of pigs either with or without ETEC infection, and was considered as the infected or non-infected control group respectively. Pigs were fed Phase 1 diets (10.2 MJ NE, 1.2% SID Lys) ad libitum until d 15 after weaning. Phase 2 diets (10.2 MJ NE, 1.1% SID Lys) were fed ad libitum for the following three weeks. Diets did not contain any antimicrobial compounds. Corrected SID SAA:Lys determined based on analyzed amino acid content and the respective standardised ileal digestibility of ingredients were found to be 0.47, 0.55, 0.61, 0.69 and 0.77 for Phase 1 diets, and 0.47, 0.55, 0.63, 0.71 and 0.78 for Phase 2 diets. Following infection, oedema disease was diagnosed in all groups including the non-infection control group, therefore data from non-infected pigs were combined with pigs infected and fed 0.55 SAA:Lys for analysis of production and plasma data. There were no dietary effects of SID SAA:Lys on days with diarrhoea or faecal shedding of F4 ETEC (P > 0.05). Overall, average daily gain (ADG), feed intake and G:F were optimised at 0.71 (SE = 0.073), 0.73 (SE = 0.065) and 0.68 (SE

Published
2017

34. Pigs experimentally infected with an enterotoxigenic strain of Escherichia coli have improved feed efficiency and indicators of inflammation with dietary supplementation of tryptophan and methionine in the immediate post-weaning period

Author

Capozzalo, M. M., primary, Kim, J. C., additional, Htoo, J. K., additional, de Lange, C. F. M., additional, Mullan, B. P., additional, Hansen, C. F., additional, Resink, J. W., additional, and Pluske, J. R., additional

Published
2017
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35. Population growth, energy use, and the implications for the search for extraterrestrial intelligence.

Author

Mullan, B. and Haqq-Misra, J.

Subjects
EXTRATERRESTRIAL beings, POPULATION, ENERGY consumption, SUSTAINABILITY, CLIMATE change, FERMI'S paradox, SPACE biology
Abstract

Highlights • We update calculations of population- and energy-related "doomsdays" from Von Hoerner (1975). • Current trends show "doomsdays" related to a population singularity or agricultural limitations may not occur. • "Doomsdays" may occur due to greenhouse gas emissions by 2300, and/or direct heating by 2300–2400. • Using ∼1016–1017 W may raise Earth's temperature by 12 K or require complete coverage by solar collectors by ∼2400 • If this also applies to extraterrestrial civilizations, it may support the "sustainability solution" to the Fermi Paradox. Abstract Von Hoerner ("Population Explosion and Interstellar Expansion," Journal of the British Interplanetary Society, 28, 691–712, 1975; hereafter VH75) examined the effects of human population growth and predicted agricultural, environmental, and other problems from observed growth rate trends. Using straightforward calculations, VH75 predicted the "doomsday" years for these scenarios (≈2020–2050), when we as a species should run out of space or food, or induce catastrophic anthropogenic climate change through thermodynamically unavoidable direct heating of the planet. Now that over four decades have passed, in this paper we update VH75. We perform similar calculations as that work, with improved data and trends in population growth, food production, energy use, and climate change. For many of the impacts noted in VH75 our work amounts to pushing the "doomsday" horizon back to the 2300 s–2400 s (or much further for population-driven interstellar colonization). This is largely attributable to using worldwide data that exhibit smaller growth rates of population and energy use in the last few decades. While population-related catastrophes appear less likely than in VH75, our continued growth in energy use provides insight into possible future issues. We find that, if historic trends continue, direct heating of the Earth will be a substantial contributor to climate change by ≈2260, regardless of the energy source used, coincident with our transition to a Kardashev type-I civilization. We also determine that either an increase of Earth's global mean temperature of ≈12 K will occur or an unreasonably high fraction of the planet will need to be covered by solar collectors by ∼2400 to keep pace with our growth in energy use. We further discuss the implications in terms of interstellar expansion, the transition to type II and III civilizations, SETI, and the Fermi Paradox. We conclude that the "sustainability solution" to the Fermi Paradox is a compelling possibility. [ABSTRACT FROM AUTHOR]

Published
2019
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49. Separate and combined effects of oligofructose and inulin on post-weaning colibacillosis and weight gain: a preliminary study

Author

Halas, D., Hansen, Christian Fink, Hampson, D. J., Kim, J. C., Mullan, B. P., Callesen, Jesper, Wilson, R. H., Pluske, J. R., Paterson, J. E., and Barker, J. A.

Subjects
Escherichia, experimental infections, Animal Nutrition (Production Responses) [LL520], Meat Producing Animals [LL120], liveweight gain, Sus scrofa, piglets, Escherichia coli infections, prokaryotes, Suidae, eukaryotes, Animal Nutrition (Physiology) [LL510], Enterobacteriaceae, Proteobacteria, Escherichia coli, mammals, Chordata, Artiodactyla, Enterobacteriales, inulin, Bacteria, weaning, pigs, Suiformes, pig feeding, Sus, diarrhoea, animals, feed supplements, bacterium. colibacteriosis. diarrhea. E. coli. gut flora. hogs. intestinal micro-organisms. liveweight gains. oligofructose. scouring. swine, diets, Prion, Viral, Bacterial and Fungal Pathogens of Animals [LL821], growth rate, vertebrates, Gammaproteobacteria, intestinal microorganisms
Published
2007

50. Gut health in the pig

Author

Pluske, J. R., Hansen, Christian Fink, Payne, H. G., Mullan, B. P., Kim, J. C., Hampson, D. J., Paterson, J. E., and Barker, J. A.

Subjects
liveweight gain, Sus scrofa, mineral supplements, digestive tract, antibiotics, Suidae, microbial flora, digestive disorders, enteritis, Chordata, Artiodactyla, OECD Countries, zinc, pigs, Suiformes, Sus, Commonwealth of Nations, EU regulations, animals, APEC countries, Feed Additives [RR130], intestinal microorganisms, disease control, salmonellosis, Meat Producing Animals [LL120], Oceania, Pesticides and Drugs, Animal Immunology [LL650], Microbial Ecology [ZZ333], dysentery, eukaryotes, Animal Nutrition (Physiology) [LL510], Control [HH405], mammals, Laws and Regulations [DD500], EC regulations. gastrointestinal tract. gut flora. hogs. ileitis. intestinal micro-organisms. intestine epithelium. jejunitis. liveweight gains. microflora. Salmonella infections. swine, creep feeding, feed additives, tylosin, animal health, Australasia, Developed Countries, Australia, immunity, lactic acid bacteria, carcass quality, intestinal mucosa, probiotics, Biochemistry and Physiology of Microorganisms [ZZ394], copper, gastrointestinal diseases, Prion, Viral, Bacterial and Fungal Pathogens of Animals [LL821], vertebrates
Abstract

Gastrointestinal disturbances can cause large economic losses in the pig industry. Diseases and conditions of the gastrointestinal tract (GIT) that can cause economic loss have generally been controlled by the use of dietary (and or in the water) antimicrobial compounds, such as antibiotic feed additives and (or) minerals such as zinc and copper. However the implementation of legislation in some parts of the world, for example the European Union, and a growing sentiment worldwide to reduce the use of dietary antimicrobial compounds, has caused a reassessment of measures to influence GIT 'health' and caused enormous interest in alternative means to control diseases and conditions of the GIT. There are now available a wide array of products and strategies available to the pig industry that influence 'gut health'. The products in the market place are characterised predominately not only by their (claimed) different modes of action, but also by the variation in responses seen when offered to pigs, and not only in the post-weaning period. This variation is presumably a consequence of the many different conditions of management that pigs are under, that in turn influences factors such as composition of the microbiota and mucosal immunity. Other strategies, such as the manipulation of particle size and changing the protein content of a diet, might also be adopted to influence the expression of enteric pathogens and the expression of disease. Ultimately, the cost-benefit of adopting such practices to influence gastrointestinal 'health' requires consideration.

Published
2007

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