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6 results on '"Bains, I."'

1. MALT90: The Millimetre Astronomy Legacy Team 90 GHz Survey

Author

Jackson, J. M., Rathborne, J. M., Foster, J. B., Whitaker, J. S., Sanhueza, P., Claysmith, C., Mascoop, J. L., Wienen, M., Breen, S. L., Herpin, F., Duarte-Cabral, A., Csengeri, T., Longmore, S., Contreras, Y., Indermuehle, B., Barnes, P. J., Walsh, A. J., Cunningham, M. R., Brooks, K. J., Britton, T. R., Voronkov, M. A., Urquhart, J. S., Alves, J., Jordan, C. H., Hill, T., Hoq, S., Finn, S., C., S., Bains, I., Bontemps, S., Bronfman, L., Caswell, J. L., Deharveng, L., Ellingsen, S. P., Fuller, G. A., Garay, G., Green, J. A., Hindson, L., Jones, P. A., Lenfestey, C., Lo, N., Lowe, V., Mardones, D., Menten, K. M., Minier, V., Morgan, L. K., Motte, F., Muller, E., Peretto, N., Purcell, C. R., Schilke, P., Schneider-Bontemps, N., Schuller, F., Titmarsh, A., Wyrowski, F., Zavagno, A., Max-Planck-Institut für Radioastronomie (MPIFR), FORMATION STELLAIRE 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Swinburne University of Technology (Hawthorn campus), Laboratoire de Probabilités et Modèles Aléatoires (LPMA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Australia Telescope National Facility (ATNF), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Instituto Dom Luiz, Universidade de Lisboa = University of Lisbon (ULISBOA), Departamento de Astronomia (DAS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, German Aerospace Center (DLR), Max Planck Institute for Radio Astronomy, I. Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), School of Physics, Australia Telescope National Facility, Universidade de Lisboa (ULISBOA), Universidad de Santiago de Chile [Santiago] (USACH), Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany, Univ Cologne, Inst Phys 1, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Universität zu Köln

Subjects
Data products, High resolution, FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, QB, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Star formation, Astronomy, Astronomy and Astrophysics, Galactic plane, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Large sample, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Millimeter, Galaxy Astrophysics, Data reduction
Abstract

The Millimetre Astronomy Legacy Team 90 GHz (MALT90) survey aims to characterise the physical and chemical evolution of high-mass star-forming clumps. Exploiting the unique broad frequency range and on-the-fly mapping capabilities of the Australia Telescope National Facility Mopra 22 m single-dish telescope, MALT90 has obtained 3' x 3' maps toward ~2000 dense molecular clumps identified in the ATLASGAL 870 um Galactic plane survey. The clumps were selected to host the early stages of high-mass star formation and to span the complete range in their evolutionary states (from prestellar, to protostellar, and on to HII regions and photodissociation regions). Because MALT90 mapped 16 lines simultaneously with excellent spatial (38") and spectral (0.11 km/s) resolution, the data reveal a wealth of information about the clump's morphologies, chemistry, and kinematics. In this paper we outline the survey strategy, observing mode, data reduction procedure, and highlight some early science results. All MALT90 raw and processed data products are available to the community. With its unprecedented large sample of clumps, MALT90 is the largest survey of its type ever conducted and an excellent resource for identifying interesting candidates for high resolution studies with ALMA., Comment: Accepted to PASA, 13 pages

Published
2013
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2. Observations and radiative transfer modelling of a massive dense cold core in g333

Author

Lo, N., Redman, M. P., Jones, P. A., Cunningham, M. R., Chhetri, R., Bains, I., and Burton, M. G.

Subjects
stars: formation, clumps, ism: jets and outflows, starless cores, cologne database, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, envelope, outflow, Astrophysics - Astrophysics of Galaxies, ism: individual objects: g333.125-0.562, ism: kinematics and dynamics, radiative transfer, Astrophysics of Galaxies (astro-ph.GA), emission, continuum observations, cloud, molecular-spectroscopy, Astrophysics::Galaxy Astrophysics, discovery
Abstract

Cold massive cores are one of the earliest manifestations of high mass star formation. Following the detection of SiO emission from G333.125-0.562, a cold massive core, further investigations of the physics, chemistry and dynamics of this object has been carried out. Mopra and NANTEN2 molecular line profile observations, Australia Telescope Compact Array (ATCA) line and continuum emission maps, and Spitzer 24 and 70 \mum images were obtained. These new data further constrain the properties of this prime example of the very early stages of high mass star formation. A model for the source was constructed and compared directly with the molecular line data using a 3D molecular line transfer code - MOLLIE. The ATCA data reveal that G333.125-0.562 is composed of two sources. One of the sources is responsible for the previously detected molecular outflow and is detected in the Spitzer 24 and 70 \mum band data. Turbulent velocity widths are lower than other more active regions of G333 which reflects the younger evolutionary stage and/or lower mass of this core. The molecular line modelling requires abundances of the CO isotopes that strongly imply heavy depletion due to freeze-out of this species onto dust grains. The principal cloud is cold, moderately turbulent and possesses an outflow which indicates the presence of a central driving source. The secondary source could be an even less evolved object as no apparent associations with continuum emissions at (far-)infrared wavelengths., Comment: 10 pages, accepted to MNRAS

Published
2011

4. ASKAP and MeerKAT surveys of the magellanic clouds

Author

Loon, J. Th, Arce, H., Bailey, A., Bains, I., Begum, A., Bekki, K., Bekhti, N. B., Bland-Hawthorn, J., Brooks, K., Brunt, C., Burton, M., Caswell, J., Cunningham, M., Dickey, J., Douglas, K., Ellingsen, S., English, J., Estalella, R., Ford, A., Foster, T., Gaensler, B., Gallagher, J., Gibson, S., Girart, J., Goldsmith, P., Gómez, J. F., Gómez, Y., Green, A., Green, J., Haffner, M., Heiles, C., Heitsch, F., Hennebelle, P., Hirota, T., Hoare, M., Imai, H., Izumiura, H., Joncas, G., Jones, P., Kalberla, P., Kang, J. -H, Kawamura, A., Kerp, J., Kerton, C., Koo, B. -C, Kothes, R., Kurtz, S., Masa Lakicevic, Landecker, T., Lazarian, A., Lo, N., Lockman, F., Magnani, L., Mcclure-Griffiths, N., Menten, K., Migenes, V., Miville-Deschênes, M. -A, Muller, E., Nakagawa, A., Nakanishi, H., Nakashima, J. -I, Nidever, D., Nigra, L., Peek, J., Pérez-Torres, M., Phillips, C., Putman, M., Remijan, A., Richter, P., Schilke, P., Sofue, Y., Stanimirović, S., Tafoya, D., Taylor, R., Tian, W. -W, Uscanga, L., Loon, J., Voronkov, M., Wakker, B., Walsh, A., Westmeier, T., Winkel, B., Zweibel, E., Bagheri, G., Barway, S., Beletsky, Y., Bernard, J. -P, Bietenholz, M., Booth, R., Bot, C., Brinks, E., Cioni, M. -R, Blok, E., Evans, C., Gibson, B., Goedhart, S., Gómez, J., Gordon, K., Haverkorn, M., Holwerda, B., Indebetouw, R., Israel, F., Koribalski, B., Krumholz, M., Lakićević, M., Meixner, M., Oliveira, J., Sarre, P., Sewiło, M., Sibbons, L., Smith, K., Vlemmings, W., Walter, F., Whitelock, P., and Zijlstra, A.

Abstract

The Magellanic Clouds are a stepping stone from the overwhelming detail of the Milky Way in which we are immersed, to the global characteristics of galaxies both in the nearby and distant universe. They are interacting, gas-rich dwarf galaxies of sub-solar metallicity, not unlike the building blocks that assembled the large galaxies that dominate groups and clusters, and representative of the conditions at the height of cosmic star formation. The Square Kilometre Array (SKA) can make huge strides in understanding galactic metabolism and the ecological processes that govern star formation, by observations of the Magellanic Clouds and other, nearby Magellanic-type irregular galaxies. Two programmes with SKA Pathfinders attempt to pave the way: the approved Galactic ASKAP Spectral Line Survey (GASKAP) includes a deep survey in H I and OH of the Magellanic Clouds, whilst MagiKAT is proposed to perform more detailed studies of selected regions within the Magellanic Clouds - also including Faraday rotation measurements and observations at higher frequencies. These surveys also close the gap with the revolutionizing surveys at far-IR wavelengths with the Spitzer Space Telescope and Herschel Space Observatory.

5. Maser misto: Overlap in circumstellar envelopes

Author

Richards, A. M. S., Bains, I., Anna Bartkiewicz, Diamond, P. J., Etoka, S., Gray, M. D., Lekht, E. E., Mendoza-Torres, E., Masheder, M. R. W., Murakawa, K., Rosa-Gonzalez, D., Szymczak, M., Langevelde, H. J., Verhoelst, T., Vlemmings, W., and Yates, J. A.

6. Maser Misto

Author

Richards, A., Bains, I., Bartkiewicz, A., Diamond, P., Etoka, S., Gray, M. D., Lekht, E. E., Masheder, M. R. W., Mendoza-Torres, E., Murakawa, K., Rosa-Gonzalez, D., Szymczak, M., Huib Jan van Langevelde, Verhoelst, T., Vlemmings, W., and Yates, J. A.

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