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3,600 results on '"Sharp, R."'

305. OzDES multifibre spectroscopy for the Dark Energy Survey: 3-yr results and first data release

Author

Childress, MJ, Lidman, C, Davis, TM, Tucker, BE, Asorey, J, Yuan, F, Abbott, TMC, Abdalla, FB, Allam, S, Annis, J, Banerji, M, Benoit-Lévy, A, Bernard, SR, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carollo, D, Carrasco Kind, M, Carretero, J, Castander, FJ, Cunha, CE, da Costa, LN, D'Andrea, CB, Doel, P, Eifler, TF, Evrard, AE, Flaugher, B, Foley, RJ, Fosalba, P, Frieman, J, García-Bellido, J, Glazebrook, K, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gupta, RR, Gutierrez, G, Hinton, SR, Hoormann, JK, James, DJ, Kessler, R, Kim, AG, King, AL, Kovacs, E, Kuehn, K, Kuhlmann, S, Kuropatkin, N, Lagattuta, DJ, Lewis, GF, Li, TS, Lima, M, Lin, H, Macaulay, E, Maia, MAG, Marriner, J, March, M, Marshall, JL, Martini, P, McMahon, RG, Menanteau, F, Miquel, R, Moller, A, Morganson, E, Mould, J, Mudd, D, Muthukrishna, D, Nichol, RC, Nord, B, Ogando, RLC, Ostrovski, F, Parkinson, D, Plazas, AA, Reed, SL, Reil, K, Romer, AK, Rykoff, ES, Sako, M, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Scolnic, D, Sevilla-Noarbe, I, Seymour, N, Sharp, R, Smith, M, Soares-Santos, M, Sobreira, F, Sommer, NE, Spinka, H, Suchyta, E, Sullivan, M, Swanson, MEC, Tarle, G, Uddin, SA, Walker, AR, and Wester, W

Subjects
astro-ph.GA, astro-ph.CO, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, dark energy, general [supernovae], Astrophysics::Galaxy Astrophysics, Astronomical and Space Sciences
Abstract

We present results for the first three years of OzDES, a six year programme to obtain redshifts for objects in the Dark Energy Survey (DES) supernova fields using the 2dF fibre positioner and AAOmega spectrograph on the Anglo-Australian Telescope. OzDES is a multi-object spectroscopic survey targeting multiple types of targets at multiple epochs over a multiyear baseline and is one of the first multi-object spectroscopic surveys to dynamically include transients into the target list soon after their discovery. At the end of three years, OzDES has spectroscopically confirmed almost 100 supernovae, and has measured redshifts for 17 000 objects, including the redshifts of 2566 supernova hosts. We examine how our ability to measure redshifts for targets of various types depends on signal-to-noise ratio (S/N), magnitude and exposure time, finding that our redshift success rate increases significantly at a S/N of 2-3 per 1-Å bin. We also find that the change in S/N with exposure time closely matches the Poisson limit for stacked exposures as long as 10 h. We use these results to predict the redshift yield of the full OzDES survey, as well as the potential yields of future surveys on other facilities such as (i.e. the 4-m Multi-Object Spectroscopic Telescope, the Subaru Prime Focus Spectrograph and the Maunakea Spectroscopic Explorer). This work marks the first OzDES data release, comprising 14 693 redshifts. OzDES is on target to obtain over 30 000 redshifts over the 6-yr duration of the survey, including a yield of approximately 5700 supernova host-galaxy redshifts.

Published
2017

306. Studies of solute distribution at solid-liquid interfaces

Author

Sharp, R

Abstract

An attempt has been made in this thesis to put on a sound basis, the relation between interface morphology and distribution of solute in alloys solidifying in a cellular or dendritic manner. Specimens have been grown under precisely known and regulated conditions and quenching by rapid withdrawal into water has ensured that the solute distribution existing in the liquid has been retained in the solid. Electron microprobe analysis coupled with optical microscopy studies have then been used to give information concerning the effect of growth variables on the nature of the interface. The results of this work fall into two distinct parts. First, data are presented which relate to the tips of the cells or dendrites solidified under conditions involving convective flow or transport by diffusion only, and with both heavy and light solutes. Second, extensive annealing of the initial structure behind the tips has been investigated to establish the mechanism involved in post-solidification ripening. It has been found that over the range of experimental conditions used, the amount of lateral segregation produced by cells and dendrites increases with increasing growth velocity and concentration and with a decrease in the value of the imposed temperature gradient. The results suggest that the solute segregation adjusts until the average gradient of liquidus temperature normal to the interface is equal to the imposed temperature gradient. At the same time as lateral segregation increases, there is a gradual change in morphology from simple cells to cells with branches and finally to crystallographic dendrites which have well-developed side arms. Increasing growth rate was found to cause a decrease in the size of branched cells and dendrites, However, the size of simple cells appears to be independent of growth velocity and alloy concentration but is linked to the magnitude of the concentration gradient at the tips. In specimens in which there is convection in the melt, a boundary layer exists, inside which there is no stirring. Outside this layer the liquid is fully mixed. The thickness of the layer was found to depend on alloy concentration, and temperature gradient, both variables which affect the magnitude of the density inversion. Annealing of the cellular structure behind the growth front was found to occur by removal of solute-rich liquid from the cell walls to the cell corners. When the interface plane is (100) or (111) this takes place randomly, but if it is (110), then cell walls disappear preferentially in one direction. The reason for this has been discussed and the conclusion reached that the mechanism causing changes in cell structure is the reduction in surface area of the solute-rich liquid films. Annealing in the branched cell and dendrite specimens takes place by the disappearance of branches or secondary arms behind the interface, the rate of disappearance depending on concentration and being essentially different for the two morphologies involved. The results presented give the spacing of arms as a function of time allowed for annealing.

Published
2017

307. OzDES multifibre spectroscopy for the Dark Energy Survey: Three year results and first data release

Author

Childress, M. J., Lidman, C., Davis, T. M., Tucker, B. E., Asorey, J., Yuan, F., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Banerji, M., Benoit-Levy, A., Stephanie Bernard, Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Castander, F. J., Cunha, C. E., Da Costa, L. N., D Andrea, C. B., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Foley, R. J., Fosalba, P., Frieman, J., Garcia-Bellido, J., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, R. R., Gutierrez, G., Hinton, S. R., Hoormann, J. K., James, D. J., Kessler, R., Kim, A. G., King, A. L., Kovacs, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lagattuta, D. J., Lewis, G. F., Li, T. S., Lima, M., Lin, H., Macaulay, E., Maia, M. A. G., Marriner, J., March, M., Marshall, J. L., Martini, P., Mcmahon, R. G., Menanteau, F., Miquel, R., Moller, A., Morganson, E., Mould, J., Mudd, D., Muthukrishna, D., Nichol, R. C., Nord, B., Ogando, R. L. C., Ostrovski, F., Parkinson, D., Plazas, A. A., Reed, S. L., Reil, K., Romer, A. K., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Seymour, N., Sharp, R., Smith, M., Soares-Santos, M., Sobreira, F., Sommer, N. E., Spinka, H., Suchyta, E., Sullivan, M., Swanson, M. E. C., Tarle, G., Uddin, S. A., Walker, A. R., Wester, W., and Zhang, B. R.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present results for the first three years of OzDES, a six-year programme to obtain redshifts for objects in the Dark Energy Survey (DES) supernova fields using the 2dF fibre positioner and AAOmega spectrograph on the Anglo-Australian Telescope. OzDES is a multi-object spectroscopic survey targeting multiple types of targets at multiple epochs over a multi-year baseline, and is one of the first multi-object spectroscopic surveys to dynamically include transients into the target list soon after their discovery. At the end of three years, OzDES has spectroscopically confirmed almost 100 supernovae, and has measured redshifts for 17,000 objects, including the redshifts of 2,566 supernova hosts. We examine how our ability to measure redshifts for targets of various types depends on signal-to-noise, magnitude, and exposure time, finding that our redshift success rate increases significantly at a signal-to-noise of 2 to 3 per 1-Angstrom bin. We also find that the change in signal-to-noise with exposure time closely matches the Poisson limit for stacked exposures as long as 10 hours. We use these results to predict the redshift yield of the full OzDES survey, as well as the potential yields of future surveys on other facilities such as the 4m Multi-Object Spectroscopic Telescope (4MOST), the Subaru Prime Focus Spectrograph (PFS), and the Maunakea Spectroscopic Explorer (MSE). This work marks the first OzDES data release, comprising 14,693 redshifts. OzDES is on target to obtain over a yield of approximately 5,700 supernova host-galaxy redshifts., Accepted for publication in MNRAS. Redshift data release is available at http://www.mso.anu.edu.au/ozdes/DR1

Published
2017

308. Galaxy and Mass Assembly (GAMA): galaxies at the faint end of the Hα luminosity function

Author

Brough, S., Hopkins, A. M., Sharp, R. G., Gunawardhana, M., Wijesinghe, D., Robotham, A. S. G., Driver, S. P., Baldry, I. K., Bamford, S. P., Liske, J., Loveday, J., Norberg, P., Peacock, J. A., Bland-Hawthorn, J., Brown, M. J. I., Cameron, E., Croom, S. M., Frenk, C. S., Foster, C., Hill, D. T., Jones, D. H., Kelvin, L. S., Kuijken, K., Nichol, R. C., Parkinson, H. R., Pimbblet, K., Popescu, C. C., Prescott, M., Sutherland, W. J., Taylor, E., Thomas, D., Tuffs, R. J., and van Kampen, E.

Subjects
Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present an analysis of the properties of the lowest Hα-luminosity galaxies (LHα≤ 4 × 1032 W; SFR < 0.02 M⊙ yr−1, with SFR denoting the star formation rate) in the Galaxy And Mass Assembly survey. These galaxies make up the rise above a Schechter function in the number density of systems seen at the faint end of the Hα luminosity function. Above our flux limit, we find that these galaxies are principally composed of intrinsically low stellar mass systems (median stellar mass = 2.5 × 108 M⊙) with only 5/90 having stellar masses M > 1010 M⊙. The low-SFR systems are found to exist predominantly in the lowest-density environments (median density ∼0.02 galaxy Mpc−2) with none in environments more dense than ∼1.5 galaxy Mpc−2. Their current specific SFRs (SSFRs; −8.5 < log [SSFR (yr −1)] < −12) are consistent with their having had a variety of star formation histories. The low-density environments of these galaxies demonstrate that such low-mass, star-forming systems can only remain as low mass and form stars if they reside sufficiently far from other galaxies to avoid being accreted, dispersed through tidal effects or having their gas reservoirs rendered ineffective through external processes

Published
2017

309. Multi-messenger Observations of a Binary Neutron Star Merger

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S. D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, Markus, Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calder, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, Ximeng, Chen, Y., Cheng, H. P., Chia, H., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, A. K. W., Chung, S., Ciani, G., Ciolfi, R., Cirelli, C. E., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. F., Cohen, D., Colla, A., Collette, C. G., Cominsky, L. R., Jr., M. Constancio, Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Dálya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Da Silva Costa, C. F., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Day, B., De, S., DeBra, D., Degallaix, J., De Laurentis, M., Deléglise, S., Pozzo, W. Del, Demos, N., Denker, T., Dent, T., De Pietri, R., Dergachev, V., De Rosa, R., DeRosa, R. T., De Rossi, C., DeSalvo, R., De Varona, O., Devenson, J., Dhurandhar, S., Díaz, M. C., Fiore, L. Di, Giovanni, M. Di, Girolamo, T. Di, Lieto, A. Di, Pace, S. Di, Palma, I. Di, Renzo, F. Di, Doctor, Z., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Douglas, R., Álvarez, M. Dovale, Downes, T. P., Drago, M., Dreissigacker, C., Driggers, J. C., Du, Z., Ducrot, M., Dupej, P., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenstein, R. A., Essick, R. C., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M. M., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finstad, D., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J. A., Forsyth, P. W. F., Forsyth, S. S., Fournier, J. D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E. M., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glover, L., Goetz, E., Goetz, R., Gomes, S., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Gretarsson, E. M., Griswold, B., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Haster, C. J., Haughian, K., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Houston, E. A., Howell, E. J., Hreibi, A., Hu, Y. M., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Indik, N., Inta, R., Intini, G., Isa, H. N., Isac, J. M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kasprzack, M., Katolik, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Kéfélian, F., Keitel, D., Kemball, A. J., Kennedy, R., Kent, C., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. M., Kimbrell, S. J., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Krämer, C., Kringel, V., Krishnan, B., Królak, A., Kuehn, G., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Landry, M., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Larson, S. L., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, K., Lehmann, J., Lenon, A., Leonardi, M., Leroy, N., Letendre, N., Levin, Y., Li, T. G. F., Linker, S. D., Littenberg, T. B., Liu, J., Lo, R. K. L., Lockerbie, N. A., London, L. T., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lück, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Machenschalk, B., MacInnis, M., Macleod, D. M., Hernandez, I. Maga, Magaña-Sandoval, F., Zertuche, L. Maga, Magee, R. M., Majorana, E., Maksimovic, I., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsh, P., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McNeill, L., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Mejuto-Villa, E., Melatos, A., Mendell, G., Mercer, R. A., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, B. B., Miller, Julian Sebastian, Millhouse, M., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Ming, J., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moffa, D., Moggi, A., Mogushi, K., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mours, B., Mow-Lowry, C. M., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Napier, K., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Nevin, L., Newport, J. M., Newton, G., Ng, K. K. Y., Nguyen, P., Nguyen, Thank Thank, Nichols, D., Nielsen, A. B., Nissanke, S., Nitz, A., Noack, A., Nocera, F., Nolting, D., North, C., Nuttall, L. K., Oberling, J., O'Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard, O'Reilly, B., Ormiston, R., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Page, J., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Howard, Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. 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A., Hampel-Arias, Z., Harding, J. P., Hernandez, S., Hernandez-Almada, A., Hona, B., Hüntemeyer, P., Iriarte, A., Jardin-Blicq, A., Joshi, V., Kaufmann, S., Kieda, D., Lara, A., Lauer, R. J., Lennarz, D., Linnemann, J. T., Longinotti, A. L., Luna-García, R., López-Coto, R., Malone, K., Marinelli, S. S., Martinez, O., Martinez-Castellanos, I., Martínez-Castro, J., Martínez-Huerta, H., Matthews, J. A., Miranda-Romagnoli, P., Moreno, E., Mostafá, M., Nellen, L., Newbold, M., Nisa, M. U., Noriega-Papaqui, R., Pelayo, R., Pretz, J., Pérez-Pérez, E. G., Ren, Z., Rho, C. D., Rivière, C., Rosa-González, D., Rosenberg, M., Ruiz-Velasco, E., Salazar, H., Sandoval, A., Schneider, M., Schoorlemmer, H., Sinnis, G., Smith, A. J., Springer, R. W., Surajbali, P., Tibolla, O., Tollefson, K., Torres, I., Ukwatta, T. N., Weisgarber, T., Westerhoff, S., Wisher, I. G., Wood, J., Yapici, T., Yodh, G. B., Younk, P. W., Zhou, H., Álvarez, J. D., Aab, A., Abreu, P., Aglietta, M., Albuquerque, I. F. M., Albury, J. M., Allekotte, I., Almela, A., Alvarez-Muñiz, J., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Arsene, N., Asorey, H., Assis, P., Avila, G., Badescu, A. M., Balaceanu, A., Barbato, F., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Biteau, J., Blaess, S. G., Blanco, A., Blazek, J., Bleve, C., Boháčová, M., Bonifazi, C., Borodai, N., Botti, A. M., Brack, J., Brancus, I., Bretz, Thomas Günther, Bridgeman, A., Briechle, Florian, Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caccianiga, L., Cancio, A., Canfora, F., Caruso, R., Castellina, A., Catalani, F., Cataldi, G., Cazon, L., Chavez, A. G., Chinellato, J. A., Chudoba, J., Clay, R. W., Colalillo, R., Coleman, A., Collica, L., Coluccia, M. R., Conceição, R., Consolati, G., Contreras, F., Cooper, M. J., Coutu, S., Covault, C. E., Cronin, J., D'Amico, Stefano, Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., Day, J. A., De Almeida, R. M., De Jong, S., De Mauro, G., De Mello Neto, J. R. T., De Mitri, Ivan, De Oliveira, J., De Souza, V., Debatin, J., Deligny, O., Diogo, F., Dobrigkeit, C., D'Olivo, Juan Carlos, Dorosti, Q., Dova, M. T., Dundovic, A., Ebr, J., Engel, R., Erdmann, Martin, Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Farmer, J., Farrar, G., Fauth, A. C., Fazzini, N., Feldbusch, F., Fenu, F., Fick, B., Figueira, J. M., Freire, M. M., Fujii, T., Fuster, A., Gaïor, R., García, B., Gemmeke, H., Gherghel-Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, Jens Christian, Golup, G., González, N., Gorgi, A., Gottowik, M., Grillo, A. F., Grubb, T. D., Guarino, F., Guedes, G. P., Halliday, R., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Harvey, V. M., Haungs, A., Hebbeker, Thomas, Heck, D., Heimann, P., Herve, A. E., Hojvat, C., Holt, E. W., Homola, P., Hörandel, J. R., Horvath, P., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Jandt, I., Johnsen, J. A., Josebachuili, M., Jurysek, J., Kääpä, A., Kampert, K. H., Keilhauer, B., Kemmerich, N., Kemp, Julian, Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, Rafael, Krohm, N., Kuempel, D., Kunka, N., Lago, B. L., LaHurd, D., Lang, R. G., Lauscher, Markus, Legumina, R., Letessier-Selvon, A., Lhenry-Yvon, I., Link, K., Lopes, L., López, R., Lorek, R., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Marsella, G., Martello, D., Martinez, H., Mathes, H. J., Mathys, S., Matthews, J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina, C., Medina-Tanco, G., Melo, D., Menshikov, A., Merenda, K. D., Michal, S., Micheletti, M. I., Middendorf, Lukas, Miramonti, L., Mitrica, B., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Morlino, G., Müller, A. L., Müller, Gero, Muller, M. A., Müller, S., Mussa, R., Naranjo, I., Nguyen, P. H., Niculescu-Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, Tim, Nitz, D., Nosek, D., Novotny, V., Nožka, L., Núñez, L. A., Oikonomou, F., Olinto, A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pȩkala, J., Peña-Rodriguez, J., Pereira, L. A. S., Perlin, M., Perrone, L., Peters, Christine Jutta, Petrera, S., Phuntsok, J., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Plum, Matthias, Poh, J., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos-Pollan, Raúl, Rautenberg, J., Ravignani, D., Ridky, J., Riehn, F., Risse, M., Ristori, P., Rizi, V., Roncoroni, M. J., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salamida, F., Saleh, A., Salina, G., Sánchez, F., Sanchez-Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schröder, S., Schumacher, Johannes Christian, Sciutto, S. J., Segreto, A., Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Soriano, J. F., Squartini, R., Stanca, D., Stasielak, J., Stassi, P., Stolpovskiy, M., Strafella, F., Streich, A., Suarez, F., Suarez-Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Šupík, J., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Timmermans, C., Tomankova, L., Tomé, B., Travnicek, P., Trini, M., Tueros, M., Ulrich, R., Unger, M., Urban, Martin, Valiño, I., Valore, L., Van Aar, G., Van Bodegom, Patrick, Van Den Berg, A. M., Van Vliet, A., Varela, E., Vargas Cárdenas, Bernardo, Vázquez, R. A., Ventura, C., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, David Simon, Watson, A. A., Weber, M., Weindl, A., Wiedeński, M., Wiencke, L., Wilczyński, H., Wirtz, Marcus, Wittkowski, D., Wundheiler, B., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Kim, S., Schulze, S., Corral-Santana, J. M., González-López, J., Hartmann, D. H., Ishwara-Chandra, C. H., Martín, S., Mehner, A., Misra, K., Michałowski, M. J., Resmi, L., Paragi, Z., Agudo, I., An, T., Beswick, R., Casadio, C., Frey, S., Jonker, P., Kettenis, M., Marcote, B., Moldon, J., Szomoru, A., Langevelde, H. J., Cwiek, A., Cwiok, M., Czyrkowski, H., Dabrowski, R., Kasprowicz, G., Mankiewicz, L., Nawrocki, K., Opiela, R., Piotrowski, L. W., Wrochna, G., Zaremba, M., Żarnecki, A. F., Haggard, D., Nynka, M., Ruan, J. J., Bland, P. A., Booler, T., Devillepoix, H. A. R., De Gois, J. S., Hancock, P. J., Howie, R. M., Paxman, J., Sansom, E. K., Towner, M. C., Tonry, J., Coughlin, M., Stubbs, C. W., Denneau, L., Heinze, A., Stalder, B., Weiland, H., Eatough, R. P., Kramer, M., Kraus, A., Piro, L., González, J. Becerra, Butler, N. R., Khandrika, H. G., Kutyrev, A., Lee, W. H., Ricci, R., Sanchez-Ramirez, R., Veilleux, S., Watson, A. M., Wieringa, M. H., Burgess, J. M., Van Eerten, H., Fontes, C. J., Korobkin, O., Wollaeger, R. T., Camilo, F., Foley, A. R., Goedhart, S., Makhathini, S., Oozeer, N., Smirnov, O. M., and Woudt, P. A.

Abstract

59 Seiten : Illustrationen, Tabellen, Diagramme (2017).

Published
2017
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310. Orbit-orbit branching rules

Author

Gingras, F, Patera, J, and Sharp, R. T

Subjects
Thermodynamics And Statistical Physics
Abstract

It is shown how the derivation of group-subgroup (IR to IR) branching rules is facilitated by the use of the much simpler (Weyl) orbit-orbit branching rules.

Published
1993

313. Man-Machine Communication

Author

Sharp, R. W.

Abstract

The author argues that programs to prepare the casual computer user are needed. Too much emphasis has been placed on thorough understanding of the working of the machine, and not enough on general principles of man-machine interaction. (SD)

Published
1974

315. Cover Image

Author

Kers, Johan A., primary, Sharp, R. Eryl, additional, Muley, Sheela, additional, Mayo, Melissa, additional, Colbeck, Jeffrey, additional, Zhu, Yihui, additional, DeFusco, Anthony W., additional, Park, Jae H., additional, and Handfield, Martin, additional

Published
2018
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318. The SAMI Galaxy Survey: gas content and interaction as the drivers of kinematic asymmetry

Author

Bloom, J V, primary, Croom, S M, additional, Bryant, J J, additional, Schaefer, A L, additional, Bland-Hawthorn, J, additional, Brough, S, additional, Callingham, J, additional, Cortese, L, additional, Federrath, C, additional, Scott, N, additional, van de Sande, J, additional, D'Eugenio, F, additional, Sweet, S, additional, Tonini, C, additional, Allen, J T, additional, Goodwin, M, additional, Green, A W, additional, Konstantopoulos, I S, additional, Lawrence, J, additional, Lorente, N, additional, Medling, A M, additional, Owers, M S, additional, Richards, S N, additional, and Sharp, R, additional

Published
2018
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321. Disección sub-mucosa endoscópica en cáncer gástrico incipiente

Author

Allan Sharp R, Andrés Donoso D, Fernando Pimentel M, Alex Scalona P, Adolfo Parra B, José Gellona V, and Osvaldo Llanos L

Subjects
medicine.medical_specialty, Cáncer gástrico incipiente, business.industry, disección endoscópica submucosa, cáncer gástrico, Cancer, Endoscopic submucosal dissection, medicine.disease, Surgery, Early Gastric Cancer, Dissection, medicine.anatomical_structure, Submucosa, medicine, Stage (cooking), business, Survival rate, Lymph node
Abstract

Introducción: El cáncer gástrico es la primera causa de muerte por cáncer en Chile y la sobrevida se encuentra en directa relación con la etapa de la enfermedad. El cáncer gástrico incipiente se define como aquel cáncer limitado a la mucosa o sub-mucosa independiente del compromiso ganglionar y se caracteriza por su excelente pronóstico, con sobrevida mayor a 90% a 10 años de seguimiento. La disección sub-mucosa endoscópica es una técnica descrita y desarrollada en Japón que permite la resección en bloque y con márgenes negativos de tumores incipientes mayores a 2 cm por vía endoscópica. Método: Se realizó una búsqueda en las bases de datos (Pubmed, EBSCO, Cochrane) bajo las palabras clave: "gastric cáncer", "early gastric cáncer", "endoscopic submucosal dissection". Resultados: Los resultados de grandes series demuestran una sobrevida comparable a la cirugía clásica, con menor morbilidad y sin mortalidad asociada. La presente revisión describe la técnica de disección sub-mucosa endoscópica en cáncer gástrico incipiente, sus indicaciones, los resultados, el análisis de las piezas resecadas, las complicaciones y el modo de seguimiento de los pacientes. Conclusión: La disección sub-mucosa endoscópica es una alternativa válida, con buenos resultados a largo plazo en pacientes debidamente seleccionados.

Published
2013
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327. The SAMI Galaxy Survey: Spatially resolving the environmental quenching of star formation in GAMA galaxies

Author

Schaefer, AL, Croom, SM, Allen, JT, Brough, S, Medling, AM, Ho, IT, Scott, N, Richards, SN, Pracy, MB, Gunawardhana, MLP, Norberg, P, Alpaslan, M, Bauer, AE, Bekki, K, Bland-Hawthorn, J, Bloom, JV, Bryant, JJ, Couch, WJ, Driver, SP, Fogarty, LMR, Foster, C, Goldstein, G, Green, AW, Hopkins, AM, Konstantopoulos, IS, Lawrence, JS, López-Sánchez, AR, Lorente, NPF, Owers, MS, Sharp, R, Sweet, SM, Taylor, EN, van de Sande, J, Walcher, CJ, Wong, OI, Schaefer, AL, Croom, SM, Allen, JT, Brough, S, Medling, AM, Ho, IT, Scott, N, Richards, SN, Pracy, MB, Gunawardhana, MLP, Norberg, P, Alpaslan, M, Bauer, AE, Bekki, K, Bland-Hawthorn, J, Bloom, JV, Bryant, JJ, Couch, WJ, Driver, SP, Fogarty, LMR, Foster, C, Goldstein, G, Green, AW, Hopkins, AM, Konstantopoulos, IS, Lawrence, JS, López-Sánchez, AR, Lorente, NPF, Owers, MS, Sharp, R, Sweet, SM, Taylor, EN, van de Sande, J, Walcher, CJ, and Wong, OI

Abstract

We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of Ha emission, we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M*; 108.1-1010.95M⊙) and in fifth nearest neighbour local environment density (∑5; 10-1.3-102.1 Mpc-2). We show that star formation rate gradients in galaxies are steeper in dense (log10(∑5/Mpc2) > 0.5) environments by 0.58 ± 0.29 dex re-1 in galaxies with stellar masses in the range 1010 < M*/M⊙ < 1011 and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density, the star formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scale-radius ratio (r50,Hα/r50,cont), which compares the extent of ongoing star formation to previous star formation. With this metric, we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from ~5 ± 4 per cent in low-density environments (log10(∑5/Mpc2) < 0.0) to 30 ± 15 per cent in the highest density environments (log10(∑5/Mpc2) > 1.0). These lines of evidence strongly suggest that with increasing local environment density, the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.

Published
2017

328. Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes

Author

Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J. R., Anderson, G. E., Ashley, M. C. B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M. S., Bian, F., Bland, P. A., Boer, M., Booler, T., Brandeker, Alexis, Brown, I. S., Buckley, D. A. H., Chang, S. -W., Coward, D. M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupak, M., de Gois, J. S., Deller, A., Devillepoix, H. A. R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T. J., Franzen, T., Gaensler, B. M., Galloway, D. K., Gendre, B., Giblin, T., Goobar, Ariel, Green, J., Hancock, P. J., Hartig, B. A. D., Howell, E. J., Horsley, L., Hotan, A., Howie, R. M., Hu, L., Hu, Y., James, C. W., Johnston, S., Johnston-Hollitt, M., Kaplan, D. L., Kasliwal, M., Keane, E. F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L. C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D. E., McCully, C., Moller, A., Morales, M. F., Morris, D., Murphy, T., Noysena, K., Onken, C. A., Orange, N. B., Oslowski, S., Pallot, D., Paxman, J., Potter, S. B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E. M., Sansom, E. K., Scalzo, R. A., Schmidt, B. P., Scott, S. M., Seghouani, N., Shang, Z., Shannon, R. M., Shao, L., Shara, M. M., Sharp, R., Sokolowski, M., Sollerman, Jesper, Staff, J., Steele, K., Sun, T., Suntzeff, N. B., Tao, C., Tingay, S., Towner, M. C., Thierry, P., Trott, C., Tucker, B. E., Vaisanen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., Zovaro, H., Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J. R., Anderson, G. E., Ashley, M. C. B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M. S., Bian, F., Bland, P. A., Boer, M., Booler, T., Brandeker, Alexis, Brown, I. S., Buckley, D. A. H., Chang, S. -W., Coward, D. M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupak, M., de Gois, J. S., Deller, A., Devillepoix, H. A. R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T. J., Franzen, T., Gaensler, B. M., Galloway, D. K., Gendre, B., Giblin, T., Goobar, Ariel, Green, J., Hancock, P. J., Hartig, B. A. D., Howell, E. J., Horsley, L., Hotan, A., Howie, R. M., Hu, L., Hu, Y., James, C. W., Johnston, S., Johnston-Hollitt, M., Kaplan, D. L., Kasliwal, M., Keane, E. F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L. C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D. E., McCully, C., Moller, A., Morales, M. F., Morris, D., Murphy, T., Noysena, K., Onken, C. A., Orange, N. B., Oslowski, S., Pallot, D., Paxman, J., Potter, S. B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E. M., Sansom, E. K., Scalzo, R. A., Schmidt, B. P., Scott, S. M., Seghouani, N., Shang, Z., Shannon, R. M., Shao, L., Shara, M. M., Sharp, R., Sokolowski, M., Sollerman, Jesper, Staff, J., Steele, K., Sun, T., Suntzeff, N. B., Tao, C., Tingay, S., Towner, M. C., Thierry, P., Trott, C., Tucker, B. E., Vaisanen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., and Zovaro, H.

Abstract

The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early- to late-time multi-wavelength observations, including optical imaging and spectroscopy, mid-infrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source emission cooled from approximately 6 400 K to 2 100 K over a 7-d period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (similar to 2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor.

Published
2017
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329. The SAMI Galaxy Survey: The Low-Redshift Stellar Mass Tully-Fisher Relation

Author

Bloom, J. V., Croom, S. M., Bryant, J. J., Callingham, J. R., Schaefer, A. L., Cortese, L., Hopkins, A. M., DEugenio, F., Scott, N., Glazebrook, K., Tonini, C., McElroy, R. E., Clark, H., Catinella, B., Allen, J. T., Bland-Hawthorn, J., Goodwin, M., Green, A. W., Konstantopoulos, I. S., Lawrence, J., Lorente, N., Medling, A. M., Owers, M. S., Richards, S. N., Sharp, R., Bloom, J. V., Croom, S. M., Bryant, J. J., Callingham, J. R., Schaefer, A. L., Cortese, L., Hopkins, A. M., DEugenio, F., Scott, N., Glazebrook, K., Tonini, C., McElroy, R. E., Clark, H., Catinella, B., Allen, J. T., Bland-Hawthorn, J., Goodwin, M., Green, A. W., Konstantopoulos, I. S., Lawrence, J., Lorente, N., Medling, A. M., Owers, M. S., Richards, S. N., and Sharp, R.

Abstract

We investigate the Tully-Fisher Relation (TFR) for a morphologically and kine- matically diverse sample of galaxies from the SAMI Galaxy Survey using 2 dimensional spatially resolved Halpha velocity maps and find a well defined relation across the stellar mass range of 8.0 < log(M*) < 11.5. We use an adaptation of kinemetry to parametrise the kinematic Halpha asymmetry of all galaxies in the sample, and find a correlation between scatter (i.e. residuals off the TFR) and asymmetry. This effect is pronounced at low stellar mass, corresponding to the inverse relationship between stellar mass and kinematic asymmetry found in previous work. For galaxies with log(M*) < 9.5, 25 +/- 3% are scattered below the root mean square (RMS) of the TFR, whereas for galaxies with log(M*) > 9.5 the fraction is 10 +/- 1% We use 'simulated slits' to directly compare our results with those from long slit spectroscopy and find that aligning slits with the photometric, rather than the kinematic, position angle, increases global scatter below the TFR. Further, kinematic asymmetry is correlated with misalignment between the photometric and kinematic position angles. This work demonstrates the value of 2D spatially resolved kinematics for accurate TFR studies; integral field spectroscopy reduces the underestimation of rotation velocity that can occur from slit positioning off the kinematic axis.

Published
2017
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330. Capability of Detecting Ultra-Violet Counterparts of Gravitational Waves with GLUV

Author

Ridden-Harper, R., Tucker, B., Sharp, R., Gilbert, J., Petkovic, M., Ridden-Harper, R., Tucker, B., Sharp, R., Gilbert, J., and Petkovic, M.

Abstract

With the discovery of gravitational waves (GW), attention has turned towards detecting counterparts to these sources. In discussions on counterpart signatures and multi-messenger follow-up strategies to GW detections, ultra-violet (UV) signatures have largely been neglected, due to UV facilities being limited to SWIFT, which lacks high-cadence UV survey capabilities. In this paper, we examine the UV signatures from merger models for the major GW sources, highlighting the need for further modelling, while presenting requirements and a design for an effective UV survey telescope. Using $u'$-band models as an analogue, we find that a UV survey telescope requires a limiting magnitude of m$_{u'}\rm (AB)\approx 24$ to fully complement the aLIGO range and sky localisation. We show that a network of small, balloon-based UV telescopes with a primary mirror diameter of 30~cm could be capable of covering the aLIGO detection distance from $\sim$60--100\% for BNS events and $\sim$40\% for BHNS events. The sensitivity of UV emission to initial conditions suggests that a UV survey telescope would provide a unique dataset, that can act as an effective diagnostic to discriminate between models., Comment: 12 pages, 10 figures, 1 table, comments are welcome

Published
2017
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331. Dark Energy Survey Year 1 Results: Redshift distributions of the weak lensing source galaxies

Author

Hoyle, B., Gruen, D., Bernstein, G. M., Rau, M. M., De Vicente, J., Hartley, W. G., Gaztanaga, E., DeRose, J., Troxel, M. A., Davis, C., Alarcon, A., MacCrann, N., Prat, J., Sánchez, C., Sheldon, E., Wechsler, R. H., Asorey, J., Becker, M. R., Bonnett, C., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Castander, F. J., Cawthon, R., Chang, C., Childress, M., Davis, T. M., Drlica-Wagner, A., Gatti, M., Glazebrook, K., Gschwend, J., Hinton, S. R., Hoormann, J. K., Kim, A. G., King, A., Kuehn, K., Lewis, G., Lidman, C., Lin, H., Macaulay, E., Maia, M. A. G., Martini, P., Mudd, D., Möller, A., Nichol, R. C., Ogando, R. L. C., Rollins, R. P., Roodman, A., Ross, A. J., Rozo, E., Rykoff, E. S., Samuroff, S., Sevilla-Noarbe, I., Sharp, R., Sommer, N. E., Tucker, B. E., Uddin, S. A., Varga, T. N., Vielzeuf, P., Yuan, F., Zhang, B., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Busha, M. T., Capozzi, D., Carretero, J., Crocce, M., D'Andrea, C. B., da Costa, L. N., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kirk, D., Krause, E., Kuhlmann, S., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Nord, B., O'Neill, C. R., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Schubnell, M., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., Weller, J., Wester, W., Wolf, R. C., Yanny, B., Zuntz, J., Hoyle, B., Gruen, D., Bernstein, G. M., Rau, M. M., De Vicente, J., Hartley, W. G., Gaztanaga, E., DeRose, J., Troxel, M. A., Davis, C., Alarcon, A., MacCrann, N., Prat, J., Sánchez, C., Sheldon, E., Wechsler, R. H., Asorey, J., Becker, M. R., Bonnett, C., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Castander, F. J., Cawthon, R., Chang, C., Childress, M., Davis, T. M., Drlica-Wagner, A., Gatti, M., Glazebrook, K., Gschwend, J., Hinton, S. R., Hoormann, J. K., Kim, A. G., King, A., Kuehn, K., Lewis, G., Lidman, C., Lin, H., Macaulay, E., Maia, M. A. G., Martini, P., Mudd, D., Möller, A., Nichol, R. C., Ogando, R. L. C., Rollins, R. P., Roodman, A., Ross, A. J., Rozo, E., Rykoff, E. S., Samuroff, S., Sevilla-Noarbe, I., Sharp, R., Sommer, N. E., Tucker, B. E., Uddin, S. A., Varga, T. N., Vielzeuf, P., Yuan, F., Zhang, B., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Busha, M. T., Capozzi, D., Carretero, J., Crocce, M., D'Andrea, C. B., da Costa, L. N., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kirk, D., Krause, E., Kuhlmann, S., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Nord, B., O'Neill, C. R., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Schubnell, M., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., Weller, J., Wester, W., Wolf, R. C., Yanny, B., and Zuntz, J.

Abstract

We describe the derivation and validation of redshift distribution estimates and their uncertainties for the galaxies used as weak lensing sources in the Dark Energy Survey (DES) Year 1 cosmological analyses. The Bayesian Photometric Redshift (BPZ) code is used to assign galaxies to four redshift bins between z=0.2 and 1.3, and to produce initial estimates of the lensing-weighted redshift distributions $n^i_{PZ}(z)$ for bin i. Accurate determination of cosmological parameters depends critically on knowledge of $n^i$ but is insensitive to bin assignments or redshift errors for individual galaxies. The cosmological analyses allow for shifts $n^i(z)=n^i_{PZ}(z-\Delta z^i)$ to correct the mean redshift of $n^i(z)$ for biases in $n^i_{\rm PZ}$. The $\Delta z^i$ are constrained by comparison of independently estimated 30-band photometric redshifts of galaxies in the COSMOS field to BPZ estimates made from the DES griz fluxes, for a sample matched in fluxes, pre-seeing size, and lensing weight to the DES weak-lensing sources. In companion papers, the $\Delta z^i$ are further constrained by the angular clustering of the source galaxies around red galaxies with secure photometric redshifts at 0.15

Published
2017
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332. The SAMI Galaxy Survey: Disk-halo interactions in radio-selected star-forming galaxies

Author

Leslie, S. K., Bryant, J. J., Ho, I. -T., Sadler, E. M., Medling, A. M., Groves, B., Kewley, L. J., Bland-Hawthorn, J., Croom, S. M., Wong, O. I., Brough, S., Tescari, E., Sweet, S. M., Sharp, R., Green, A. W., López-Sánchez, A. R., Allen, J. T., Fogarty, L. M. R., Goodwin, M., Lawrence, J. S., Konstantopoulos, I. S., Owers, M. S., Richards, S. N., Leslie, S. K., Bryant, J. J., Ho, I. -T., Sadler, E. M., Medling, A. M., Groves, B., Kewley, L. J., Bland-Hawthorn, J., Croom, S. M., Wong, O. I., Brough, S., Tescari, E., Sweet, S. M., Sharp, R., Green, A. W., López-Sánchez, A. R., Allen, J. T., Fogarty, L. M. R., Goodwin, M., Lawrence, J. S., Konstantopoulos, I. S., Owers, M. S., and Richards, S. N.

Abstract

In this paper, we compare the radio emission at 1.4 GHz with optical outflow signatures of edge-on galaxies. We report observations of six edge-on star-forming galaxies in the Sydney-AAO Multi-object Integral-field spectrograph (SAMI) Galaxy Survey with 1.4 GHz luminosities $> 1\times10^{21}$ W Hz$^{-1}$. Extended minor axis optical emission is detected with enhanced \nii/H$\alpha$ line ratios and velocity dispersions consistent with galactic winds in three of six galaxies. These galaxies may host outflows driven by a combination of thermal and cosmic ray processes. We find that galaxies with the strongest wind signatures have extended radio morphologies. Our results form a baseline for understanding the driving mechanisms of galactic winds., Comment: 16 pages, 5 figures. Published in MNRAS July 2017

Published
2017
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333. The SAMI Galaxy Survey: The cluster redshift survey, target selection and cluster properties

Author

Owers, M. S., Allen, J. T., Baldry, I., Bryant, J. J., Cecil, G. N., Cortese, L., Croom, S. M., Driver, S. P., Fogarty, L. M. R., Green, A. W., Helmich, E., de Jong, J. T. A., Kuijken, K., Mahajan, S., McFarland, J., Pracy, M. B., Robotham, A. G. S., Sikkema, G., Sweet, S., Taylor, E. N., Kleijn, G. Verdoes, Bauer, A. E., Bland-Hawthorn, J., Brough, S., Colless, M., Couch, W. J., Davies, R. L, Drinkwater, M. J., Goodwin, M., Hopkins, A. M., Konstantopoulos, I. S., Foster, C., Lawrence, J. S., Lorente, N. P. F, Medling, A. M., Metcalfe, N., Richards, S. N., van de Sande, J., Scott, N., Shanks, T., Sharp, R., Thomas, A. D., Tonini, C., Owers, M. S., Allen, J. T., Baldry, I., Bryant, J. J., Cecil, G. N., Cortese, L., Croom, S. M., Driver, S. P., Fogarty, L. M. R., Green, A. W., Helmich, E., de Jong, J. T. A., Kuijken, K., Mahajan, S., McFarland, J., Pracy, M. B., Robotham, A. G. S., Sikkema, G., Sweet, S., Taylor, E. N., Kleijn, G. Verdoes, Bauer, A. E., Bland-Hawthorn, J., Brough, S., Colless, M., Couch, W. J., Davies, R. L, Drinkwater, M. J., Goodwin, M., Hopkins, A. M., Konstantopoulos, I. S., Foster, C., Lawrence, J. S., Lorente, N. P. F, Medling, A. M., Metcalfe, N., Richards, S. N., van de Sande, J., Scott, N., Shanks, T., Sharp, R., Thomas, A. D., and Tonini, C.

Abstract

We describe the selection of galaxies targeted in eight low redshift clusters (APMCC0917, A168, A4038, EDCC442, A3880, A2399, A119 and A85; $0.029 < z < 0.058$) as part of the Sydney-AAO Multi-Object integral field Spectrograph Galaxy Survey (SAMI-GS). We have conducted a redshift survey of these clusters using the AAOmega multi-object spectrograph on the 3.9m Anglo-Australian Telescope. The redshift survey is used to determine cluster membership and to characterise the dynamical properties of the clusters. In combination with existing data, the survey resulted in 21,257 reliable redshift measurements and 2899 confirmed cluster member galaxies. Our redshift catalogue has a high spectroscopic completeness ($\sim 94\%$) for $r_{\rm petro} \leq 19.4$ and clustercentric distances $R< 2\rm{R}_{200}$. We use the confirmed cluster member positions and redshifts to determine cluster velocity dispersion, $\rm{R}_{200}$, virial and caustic masses, as well as cluster structure. The clusters have virial masses $14.25 \leq {\rm log }({\rm M}_{200}/\rm{M}_{\odot}) \leq 15.19$. The cluster sample exhibits a range of dynamical states, from relatively relaxed-appearing systems, to clusters with strong indications of merger-related substructure. Aperture- and PSF-matched photometry are derived from SDSS and VST/ATLAS imaging and used to estimate stellar masses. These estimates, in combination with the redshifts, are used to define the input target catalogue for the cluster portion of the SAMI-GS. The primary SAMI-GS cluster targets have $R< \rm{R}_{200}$, velocities $|v_{\rm pec}| < 3.5\sigma_{200}$ and stellar masses $9.5 \leq {\rm log(M}^*_{approx}/\rm{M}_{\odot}) \leq 12$. Finally, we give an update on the SAMI-GS progress for the cluster regions., Comment: 28 pages, 15 figures, 3 tables, accepted for publication in MNRAS

Published
2017
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334. THE SAMI GALAXY SURVEY: REVISITING GALAXY CLASSIFICATION THROUGH HIGH-ORDER STELLAR KINEMATICS

Author

Van De Sande, J, Bland-Hawthorn, J, Fogarty, LMR, Cortese, L, D'Eugenio, F, Croom, SM, Scott, N, Allen, JT, Brough, S, Bryant, JJ, Cecil, G, Colless, M, Couch, WJ, Davies, R, Elahi, PJ, Foster, C, Goldstein, G, Goodwin, M, Groves, B, Ho, IT, Jeong, H, Jones, DH, Konstantopoulos, IS, Lawrence, JS, Leslie, SK, López-Sánchez, ÁR, McDermid, RM, McElroy, R, Medling, AM, Oh, S, Owers, MS, Richards, SN, Schaefer, AL, Sharp, R, Sweet, SM, Taranu, D, Tonini, C, Walcher, CJ, Yi, SK, Van De Sande, J, Bland-Hawthorn, J, Fogarty, LMR, Cortese, L, D'Eugenio, F, Croom, SM, Scott, N, Allen, JT, Brough, S, Bryant, JJ, Cecil, G, Colless, M, Couch, WJ, Davies, R, Elahi, PJ, Foster, C, Goldstein, G, Goodwin, M, Groves, B, Ho, IT, Jeong, H, Jones, DH, Konstantopoulos, IS, Lawrence, JS, Leslie, SK, López-Sánchez, ÁR, McDermid, RM, McElroy, R, Medling, AM, Oh, S, Owers, MS, Richards, SN, Schaefer, AL, Sharp, R, Sweet, SM, Taranu, D, Tonini, C, Walcher, CJ, and Yi, SK

Abstract

Recent cosmological hydrodynamical simulations suggest that integral field spectroscopy can connect the high-order stellar kinematic moments h3 (∼skewness) and h4 (∼kurtosis) in galaxies to their cosmological assembly history. Here, we assess these results by measuring the stellar kinematics on a sample of 315 galaxies, without a morphological selection, using two-dimensional integral field data from the SAMI Galaxy Survey. Proxies for the spin parameter (λRe) and ellipticity (∈e) are used to separate fast and slow rotators; there exists a good correspondence to regular and non-regular rotators, respectively, as also seen in earlier studies. We confirm that regular rotators show a strong h3 versus V/σ anti-correlation, whereas quasi-regular and non-regular rotators show a more vertical relation in h3 and V/σ. Motivated by recent cosmological simulations, we develop an alternative approach to kinematically classify galaxies from their individual h3 versus V/σ signatures. Within the SAMI Galaxy Survey, we identify five classes of high-order stellar kinematic signatures using Gaussian mixture models. Class 1 corresponds to slow rotators, whereas Classes 2-5 correspond to fast rotators. We find that galaxies with similar λRe - ∈e values can show distinctly different h3 - V/σ signatures. Class 5 objects are previously unidentified fast rotators that show a weak h3 versus V/σ anti-correlation. From simulations, these objects are predicted to be disk-less galaxies formed by gas-poor mergers. From morphological examination, however, there is evidence for large stellar disks. Instead, Class 5 objects are more likely disturbed galaxies, have counter-rotating bulges, or bars in edge-on galaxies. Finally, we interpret the strong anti-correlation in h3 versus V/σ as evidence for disks in most fast rotators, suggesting a dearth of gas-poor mergers among fast rotators.

Published
2017

335. A STUDY of CENTRAL GALAXY ROTATION with STELLAR MASS and ENVIRONMENT

Author

Oliva-Altamirano, P, Brough, S, Tran, KV, Jimmy, Miller, C, Bremer, MN, Phillipps, S, Sharp, R, Colless, M, Lara-López, MA, López-Sánchez, ÁR, Pimbblet, K, Kafle, PR, Couch, WJ, Oliva-Altamirano, P, Brough, S, Tran, KV, Jimmy, Miller, C, Bremer, MN, Phillipps, S, Sharp, R, Colless, M, Lara-López, MA, López-Sánchez, ÁR, Pimbblet, K, Kafle, PR, and Couch, WJ

Abstract

We present a pilot analysis of the influence of galaxy stellar mass and cluster environment on the probability of slow rotation in 22 central galaxies at mean redshift z = 0.07. This includes new integral-field observations of five central galaxies selected from the Sloan Digital Sky Survey, observed with the SPIRAL integral-field spectrograph on the Anglo-Australian Telescope. The composite sample presented here spans a wide range of stellar masses, 10.9 < log(M∗/M⊙)lt; 12.0, and are embedded in halos ranging from groups to clusters, 12.9 < log(M200 Ṁ) < 15.6. We find a mean probability of slow rotation in our sample of P(SR) = 54 ± 7%. Our results show an increasing probability of slow rotation in central galaxies with increasing stellar mass. However, when we examine the dependence of slow rotation on host cluster halo mass, we do not see a significant relationship. We also explore the influence of cluster dominance on slow rotation in central galaxies. Clusters with low dominance are associated with dynamically younger systems. We find that cluster dominance has no significant effect on the probability of slow rotation in central galaxies. These results conflict with a paradigm in which halo mass alone predetermines central galaxy properties.

Published
2017

336. The SAMI Galaxy Survey: A new method to estimate molecular gas surface densities from star formation rates

Author

Federrath, C, Salim, DM, Medling, AM, Davies, RL, Yuan, T, Bian, F, Groves, BA, Ho, IT, Sharp, R, Kewley, LJ, Sweet, SM, Richards, SN, Bryant, JJ, Brough, S, Croom, S, Scott, N, Konstantopoulos, I, Goodwin, M, Federrath, C, Salim, DM, Medling, AM, Davies, RL, Yuan, T, Bian, F, Groves, BA, Ho, IT, Sharp, R, Kewley, LJ, Sweet, SM, Richards, SN, Bryant, JJ, Brough, S, Croom, S, Scott, N, Konstantopoulos, I, and Goodwin, M

Abstract

Stars form in cold molecular clouds. However, molecular gas is difficult to observe because the most abundant molecule (H2) lacks a permanent dipole moment. Rotational transitions of CO are often used as a tracer of H2, but CO is much less abundant and the conversion from CO intensity to H2 mass is often highly uncertain. Here we present a new method for estimating the column density of cold molecular gas (gas) using optical spectroscopy. We utilize the spatially resolved Ha maps of flux and velocity dispersion from the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey. We derive maps of gas by inverting the multi-freefall star formation relation, which connects the star formation rate surface density (SFR) with gas and the turbulent Mach number (M). Based on the measured range of SFR = 0.005 1.5 M yr-1 kpc-2 and M = 18 130, we predict gas = 7 200 M pc-2 in the star-forming regions of our sample of 260 SAMI galaxies. These values are close to previously measured gas obtained directly with unresolved CO observations of similar galaxies at low redshift. We classify each galaxy in our sample as 'star-forming' (219) or 'composite/AGN/shock' (41), and find that in 'composite/AGN/shock' galaxies the average SFR, M and gas are enhanced by factors of 2.0, 1.6 and 1.3, respectively, compared to star-forming galaxies. We compare our predictions of gas with those obtained by inverting the Kennicutt Schmidt relation and find that our new method is a factor of 2 more accurate in predicting gas, with an average deviation of 32 per cent from the actual gas.

Published
2017

337. The SAMI Galaxy Survey: Asymmetry in gas kinematics and its links to stellar mass and star formation

Author

Bloom, JV, Fogarty, LMR, Croom, SM, Schaefer, A, Bryant, JJ, Cortese, L, Richards, S, Bland-Hawthorn, J, Ho, IT, Scott, N, Goldstein, G, Medling, A, Brough, S, Sweet, SM, Cecil, G, López-Sánchez, A, Glazebrook, K, Parker, Q, Allen, JT, Goodwin, M, Green, AW, Konstantopoulos, IS, Lawrence, JS, Lorente, N, Owers, MS, Sharp, R, Bloom, JV, Fogarty, LMR, Croom, SM, Schaefer, A, Bryant, JJ, Cortese, L, Richards, S, Bland-Hawthorn, J, Ho, IT, Scott, N, Goldstein, G, Medling, A, Brough, S, Sweet, SM, Cecil, G, López-Sánchez, A, Glazebrook, K, Parker, Q, Allen, JT, Goodwin, M, Green, AW, Konstantopoulos, IS, Lawrence, JS, Lorente, N, Owers, MS, and Sharp, R

Abstract

We study the properties of kinematically disturbed galaxies in the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey using a quantitative criterion, based on kinemetry (Krajnović et al.). The approach, similar to the application of kinemetry by Shapiro et al., uses ionized gas kinematics, probed by Ha emission. By this method, 23 ± 7 per cent of our 360-galaxy sub-sample of the SAMI Galaxy Survey are kinematically asymmetric. Visual classifications agree with our kinemetric results for 90 per cent of asymmetric and 95 per cent of normal galaxies.We find that stellar mass and kinematic asymmetry are inversely correlated and that kinematic asymmetry is both more frequent and stronger in low-mass galaxies. This builds on previous studies that found high fractions of kinematic asymmetry in low-mass galaxies using a variety of different methods. Concentration of star formation and kinematic disturbance are found to be correlated, confirming results found in previous work. This effect is stronger for high-mass galaxies (log(M*) > 10) and indicates that kinematic disturbance is linked to centrally concentrated star formation. Comparison of the inner (within 0.5Re) and outer Ha equivalent widths of asymmetric and normal galaxies shows a small but significant increase in inner equivalent width for asymmetric galaxies.

Published
2017

338. The SAMI Galaxy Survey: The cluster redshift survey, target selection and cluster properties

Author

Owers, MS, Allen, JT, Baldry, I, Bryant, JJ, Cecil, GN, Cortese, L, Croom, SM, Driver, SP, Fogarty, LMR, Green, AW, Helmich, E, de Jong, JTA, Kuijken, K, Mahajan, S, McFarland, J, Pracy, MB, Robotham, AGS, Sikkema, G, Sweet, S, Taylor, EN, Verdoes Kleijn, G, Bauer, AE, Bland-Hawthorn, J, Brough, S, Colless, M, Couch, WJ, Davies, RL, Drinkwater, MJ, Goodwin, M, Hopkins, AM, Konstantopoulos, IS, Foster, C, Lawrence, JS, Lorente, NPF, Medling, AM, Metcalfe, N, Richards, SN, van de Sande, J, Scott, N, Shanks, T, Sharp, R, Thomas, AD, Tonini, C, Owers, MS, Allen, JT, Baldry, I, Bryant, JJ, Cecil, GN, Cortese, L, Croom, SM, Driver, SP, Fogarty, LMR, Green, AW, Helmich, E, de Jong, JTA, Kuijken, K, Mahajan, S, McFarland, J, Pracy, MB, Robotham, AGS, Sikkema, G, Sweet, S, Taylor, EN, Verdoes Kleijn, G, Bauer, AE, Bland-Hawthorn, J, Brough, S, Colless, M, Couch, WJ, Davies, RL, Drinkwater, MJ, Goodwin, M, Hopkins, AM, Konstantopoulos, IS, Foster, C, Lawrence, JS, Lorente, NPF, Medling, AM, Metcalfe, N, Richards, SN, van de Sande, J, Scott, N, Shanks, T, Sharp, R, Thomas, AD, and Tonini, C

Abstract

We describe the selection of galaxies targeted in eight low-redshift clusters (APMCC0917, A168, A4038, EDCC442, A3880, A2399, A119 and A85; 0.029 < z < 0.058) as part of the Sydney-AAO Multi-Object Integral field spectrograph Galaxy Survey (SAMI-GS). We have conducted a redshift survey of these clusters using the AAOmega multi-object spectrograph on the 3.9-m Anglo-Australian Telescope. The redshift survey is used to determine cluster membership and to characterize the dynamical properties of the clusters. In combination with existing data, the survey resulted in 21 257 reliable redshift measurements and 2899 confirmed cluster member galaxies. Our redshift catalogue has a high spectroscopic completeness (~94 per cent) for rpetro ≤ 19.4 and cluster-centric distances R < 2R200. We use the confirmed cluster member positions and redshifts to determine cluster velocity dispersion, R200, virial and caustic masses, as well as cluster structure. The clusters have virial masses 14.25 ≤ log(M200/M·) ≤ 15.19. The cluster sample exhibits a range of dynamical states, from relatively relaxed-appearing systems, to clusters with strong indications of merger-related substructure. Aperture- and point spread function matched photometry are derived from Sloan Digital Sky Survey and VLT Survey Telescope/ATLAS imaging and used to estimate stellar masses. These estimates, in combination with the redshifts, are used to define the input target catalogue for the cluster portion of the SAMI-GS. The primary SAMI-GS cluster targets have R

Published
2017

339. Galaxy and Mass Assembly (GAMA): the red fraction and radial distribution of satellite galaxies

Author

Prescott, Matthew, Baldry, I. K., James, P. A., Bamford, S. P., Bland-Hawthorn, J., Brough, S., Brown, M. J. I., Cameron, E., Conselice, C. J., Croom, S. M., Driver, S. P., Frenk, C. S., Gunawardhana, M., Hill, D. T., Hopkins, A. M., Jones, D. H., Kelvin, L. S., Kuijken, K., Liske, J., Loveday, J., Nichol, R. C., Norberg, P., Parkinson, H. R., Peacock, J. A., Phillipps, S., Pimbblet, K. A., Popescu, C. C., Robotham, A. S. G., Sharp, R. G., Sutherland, W. J., Taylor, E. N., Tuffs, R. J., van Kampen, E., Wijesinghe, D., Prescott, Matthew, Baldry, I. K., James, P. A., Bamford, S. P., Bland-Hawthorn, J., Brough, S., Brown, M. J. I., Cameron, E., Conselice, C. J., Croom, S. M., Driver, S. P., Frenk, C. S., Gunawardhana, M., Hill, D. T., Hopkins, A. M., Jones, D. H., Kelvin, L. S., Kuijken, K., Liske, J., Loveday, J., Nichol, R. C., Norberg, P., Parkinson, H. R., Peacock, J. A., Phillipps, S., Pimbblet, K. A., Popescu, C. C., Robotham, A. S. G., Sharp, R. G., Sutherland, W. J., Taylor, E. N., Tuffs, R. J., van Kampen, E., and Wijesinghe, D.

Abstract

We investigate the properties of satellite galaxies that surround isolated hosts within the redshift range 0.01 < z < 0.15, using data taken as part of the Galaxy And Mass Assembly survey. Making use of isolation and satellite criteria that take into account stellar mass estimates, we find 3514 isolated galaxies of which 1426 host a total of 2998 satellites. Separating the red and blue populations of satellites and hosts, using colour-mass diagrams, we investigate the radial distribution of satellite galaxies and determine how the red fraction of satellites varies as a function of satellite mass, host mass and the projected distance from their host. Comparing the red fraction of satellites to a control sample of small neighbours at greater projected radii, we show that the increase in red fraction is primarily a function of host mass. The satellite red fraction is about 0.2 higher than the control sample for hosts with , while the red fractions show no difference for hosts with . For the satellites of more massive hosts, the red fraction also increases as a function of decreasing projected distance. Our results suggest that the likely main mechanism for the quenching of star formation in satellites hosted by isolated galaxies is strangulation

Published
2017

340. Galaxy and Mass Assembly (GAMA): ugriz galaxy luminosity functions

Author

Loveday, J., Norberg, P., Baldry, I. K., Driver, S. P., Hopkins, A. M., Peacock, J. A., Bamford, S. P., Liske, J., Bland-Hawthorn, J., Brough, S., Brown, M. J. I., Cameron, E., Conselice, C. J., Croom, S. M., Frenk, C. S., Gunawardhana, M., Hill, D. T., Jones, D. H., Kelvin, L. S., Kuijken, K., Nichol, R. C., Parkinson, H. R., Phillipps, S., Pimbblet, K. A., Popescu, C. C., Prescott, M., Robotham, A. S. G., Sharp, R. G., Sutherland, W. J., Taylor, E. N., Thomas, D., Tuffs, R. J., van Kampen, E., Wijesinghe, D., Loveday, J., Norberg, P., Baldry, I. K., Driver, S. P., Hopkins, A. M., Peacock, J. A., Bamford, S. P., Liske, J., Bland-Hawthorn, J., Brough, S., Brown, M. J. I., Cameron, E., Conselice, C. J., Croom, S. M., Frenk, C. S., Gunawardhana, M., Hill, D. T., Jones, D. H., Kelvin, L. S., Kuijken, K., Nichol, R. C., Parkinson, H. R., Phillipps, S., Pimbblet, K. A., Popescu, C. C., Prescott, M., Robotham, A. S. G., Sharp, R. G., Sutherland, W. J., Taylor, E. N., Thomas, D., Tuffs, R. J., van Kampen, E., and Wijesinghe, D.

Abstract

Galaxy and Mass Assembly (GAMA) is a project to study galaxy formation and evolution, combining imaging data from ultraviolet to radio with spectroscopic data from the AAOmega spectrograph on the Anglo-Australian Telescope. Using data from Phase 1 of GAMA, taken over three observing seasons, and correcting for various minor sources of incompleteness, we calculate galaxy luminosity functions (LFs) and their evolution in the ugriz passbands. At low redshift, z < 0.1, we find that blue galaxies, defined according to a magnitude-dependent but non-evolving colour cut, are reasonably well fitted over a range of more than 10 magnitudes by simple Schechter functions in all bands. Red galaxies, and the combined blue plus red sample, require double power-law Schechter functions to fit a dip in their LF faintwards of the characteristic magnitude M* before a steepening faint end. This upturn is at least partly due to dust-reddened disc galaxies. We measure the evolution of the galaxy LF over the redshift range 0.002 < z < 0.5 both by using a parametric fit and by measuring binned LFs in redshift slices. The characteristic luminosity L* is found to increase with redshift in all bands, with red galaxies showing stronger luminosity evolution than blue galaxies. The comoving number density of blue galaxies increases with redshift, while that of red galaxies decreases, consistent with prevailing movement from blue cloud to red sequence. As well as being more numerous at higher redshift, blue galaxies also dominate the overall luminosity density beyond redshifts z≃ 0.2. At lower redshifts, the luminosity density is dominated by red galaxies in the riz bands, and by blue galaxies in u and g

Published
2017

341. Galaxy and Mass Assembly (GAMA): survey diagnostics and core data release

Author

Driver, S. P., Hill, D. T., Kelvin, L. S., Robotham, A. S. G., Liske, J., Norberg, P., Baldry, I. K., Bamford, S. P., Hopkins, A. M., Loveday, J., Peacock, J. A., Andrae, E., Bland-Hawthorn, J., Brough, S., Brown, M. J. I., Cameron, E., Ching, J. H. Y., Colless, M., Conselice, C. J., Croom, S. M., Cross, N. J. G., De Propris, R., Dye, S., Drinkwater, M. J., Ellis, S., Graham, Alister W., Grootes, M. W., Gunawardhana, M., Jones, D. H., van Kampen, E., Maraston, C., Nichol, R. C., Parkinson, H. R., Phillipps, S., Pimbblet, K., Popescu, C. C., Prescott, M., Roseboom, I. G., Sadler, E. M., Sansom, A. E., Sharp, R. G., Smith, D. J. B., Taylor, E., Thomas, D., Tuffs, R. J., Wijesinghe, D., Dunne, L., Frenk, C. S., Jarvis, M. J., Madore, B. F., Meyer, M. J., Seibert, M., Staveley-Smith, L., Sutherland, W. J., Warren, S. J., Driver, S. P., Hill, D. T., Kelvin, L. S., Robotham, A. S. G., Liske, J., Norberg, P., Baldry, I. K., Bamford, S. P., Hopkins, A. M., Loveday, J., Peacock, J. A., Andrae, E., Bland-Hawthorn, J., Brough, S., Brown, M. J. I., Cameron, E., Ching, J. H. Y., Colless, M., Conselice, C. J., Croom, S. M., Cross, N. J. G., De Propris, R., Dye, S., Drinkwater, M. J., Ellis, S., Graham, Alister W., Grootes, M. W., Gunawardhana, M., Jones, D. H., van Kampen, E., Maraston, C., Nichol, R. C., Parkinson, H. R., Phillipps, S., Pimbblet, K., Popescu, C. C., Prescott, M., Roseboom, I. G., Sadler, E. M., Sansom, A. E., Sharp, R. G., Smith, D. J. B., Taylor, E., Thomas, D., Tuffs, R. J., Wijesinghe, D., Dunne, L., Frenk, C. S., Jarvis, M. J., Madore, B. F., Meyer, M. J., Seibert, M., Staveley-Smith, L., Sutherland, W. J., and Warren, S. J.

Abstract

The Galaxy and Mass Assembly (GAMA) survey has been operating since 2008 February on the 3.9-m Anglo-Australian Telescope using the AAOmega fibre-fed spectrograph facility to acquire spectra with a resolution of R≈ 1300 for 120 862 Sloan Digital Sky Survey selected galaxies. The target catalogue constitutes three contiguous equatorial regions centred at 9h (G09), 12h (G12) and 14.5h (G15) each of 12 × 4 deg2 to limiting fluxes of rpet < 19.4, rpet < 19.8 and rpet < 19.4 mag, respectively (and additional limits at other wavelengths). Spectra and reliable redshifts have been acquired for over 98 per cent of the galaxies within these limits. Here we present the survey footprint, progression, data reduction, redshifting, re-redshifting, an assessment of data quality after 3 yr, additional image analysis products (including ugrizYJHK photometry, Sérsic profiles and photometric redshifts), observing mask and construction of our core survey catalogue (GamaCore). From this we create three science-ready catalogues: GamaCoreDR1 for public release, which includes data acquired during year 1 of operations within specified magnitude limits (2008 February to April); GamaCoreMainSurvey containing all data above our survey limits for use by the GAMA Team and collaborators; and GamaCoreAtlasSV containing year 1, 2 and 3 data matched to Herschel-ATLAS science demonstration data. These catalogues along with the associated spectra, stamps and profiles can be accessed via the GAMA website: http://www.gama-survey.org

Published
2017

342. Galaxy and Mass Assembly (GAMA): the star formation rate dependence of the stellar initial mass function

Author

Gunawardhana, M. L. P., Hopkins, A. M., Sharp, R. G., Brough, S., Taylor, E., Bland-Hawthorn, J., Maraston, C., Tuffs, R. J., Popescu, C. C., Wijesinghe, D., Jones, D. H., Croom, S., Sadler, E., Wilkins, S., Driver, S. P., Liske, J., Norberg, P., Baldry, I. K., Bamford, S. P., Loveday, J., Peacock, J. A., Robotham, A. S. G., Zucker, D. B., Parker, Q. A., Conselice, C. J., Cameron, E., Frenk, C. S., Hill, D. T., Kelvin, L. S., Kuijken, K., Madore, B. F., Nichol, B., Parkinson, H. R., Pimbblet, K. A., Prescott, M., Sutherland, W. J., Thomas, D., van Kampen, E., Gunawardhana, M. L. P., Hopkins, A. M., Sharp, R. G., Brough, S., Taylor, E., Bland-Hawthorn, J., Maraston, C., Tuffs, R. J., Popescu, C. C., Wijesinghe, D., Jones, D. H., Croom, S., Sadler, E., Wilkins, S., Driver, S. P., Liske, J., Norberg, P., Baldry, I. K., Bamford, S. P., Loveday, J., Peacock, J. A., Robotham, A. S. G., Zucker, D. B., Parker, Q. A., Conselice, C. J., Cameron, E., Frenk, C. S., Hill, D. T., Kelvin, L. S., Kuijken, K., Madore, B. F., Nichol, B., Parkinson, H. R., Pimbblet, K. A., Prescott, M., Sutherland, W. J., Thomas, D., and van Kampen, E.

Abstract

The stellar initial mass function (IMF) describes the distribution in stellar masses produced from a burst of star formation. For more than 50 yr, the implicit assumption underpinning most areas of research involving the IMF has been that it is universal, regardless of time and environment. We measure the high-mass IMF slope for a sample of low-to-moderate redshift galaxies from the Galaxy and Mass Assembly survey. The large range in luminosities and galaxy masses of the sample permits the exploration of underlying IMF dependencies. A strong IMF-star formation rate dependency is discovered, which shows that highly star-forming galaxies form proportionally more massive stars (they have IMFs with flatter power-law slopes) than galaxies with low star formation rates. This has a significant impact on a wide variety of galaxy evolution studies, all of which rely on assumptions about the slope of the IMF. Our result is supported by, and provides an explanation for, the results of numerous recent explorations suggesting a variation of or evolution in the IMF

Published
2017

343. Multi-messenger observations of a binary neutron star merger

Author

Abbott, B., Abbott, R., Abbott, T., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R., Adya, V., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P., Amato, A., Ananyeva, A., Anderson, S., Anderson, W., Angelova, S., Antier, S., Appert, S., Arai, K., Araya, M., Areeda, J., Arnaud, N., Arun, K., Ascenzi, S., Ashton, G., Ast, M., Aston, S., Astone, P., Atallah, D., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M., Bae, S., Baker, P., Baldaccini, F., Ballardin, G., Ballmer, S., Banagiri, S., Barayoga, J., Barclay, S., Barish, B., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J., Bawaj, M., Bayley, J., Bazzan, M., Becsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A., Berger, B., Bergmann, G., Bero, J., Berry, C., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I., Billingsley, G., Billman, C., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M., Blackburn, J., Blackman, J., Blair, C., Blair, D., Blair, R., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P., Branchesi, M., Brau, J., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J., Brooks, A., Brown, D., Brunett, S., Buchanan, C., Buikema, A., Bulik, T., Bulten, H., Buonanno, A., Buskulic, D., Buy, C., Byer, R., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J., Callister, T., Calloni, E., Camp, J., Canepa, M., Canizares, P., Cannon, K., Cao, H., Cao, J., Capano, C., Capocasa, E., Carbognani, F., Caride, S., Carney, M., Diaz, J., Casentini, C., Caudill, S., Cavagli, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cerd-Durn, P., Cerretani, G., Cesarini, E., Chamberlin, S., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B., Chen, H., Chen, X., Chen, Y., Cheng, H., Chia, H., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H., Cho, M., Chow, J., Christensen, N., Chu, Q., Chua, A., Chua, S., Chung, A., Chung, S., Ciani, G., Ciolfi, R., Cirelli, C., Cirone, A., Clara, F., Clark, J., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P., Cohen, D., Colla, A., Collette, C., Cominsky, L., Constancio, M., Conti, L., Cooper, S., Corban, P., Corbitt, T., Cordero-Carrion, I., Corley, K., Cornish, N., Corsi, A., Cortese, S., Costa, C., Coughlin, M., Coughlin, S., Coulon, J., Countryman, S., Couvares, P., Covas, P., Cowan, E., Coward, D., Cowart, M., Coyne, D., Coyne, R., Creighton, J., Creighton, T., Cripe, J., Crowder, S., Cullen, T., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Dlya, G., Danilishin, S., D'Antonio, S., Danzmann, K., Dasgupta, A., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E., Day, B., De, S., Debra, D., Degallaix, J., De laurentis, M., Deleglise, S., Del Pozzo, W., Demos, N., Denker, T., Dent, T., De Pietri, R., Dergachev, V., De Rosa, R., DeRosa, R., De Rossi, C., DeSalvo, R., De Varona, O., Devenson, J., Dhurandhar, S., Diaz, M., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., Doctor, Z., Dolique, V., Donovan, F., Dooley, K., Doravari, S., Dorrington, I., Douglas, R., Alvarez, M., Downes, T., Drago, M., Dreissigacker, C., Driggers, J., Du, Z., Ducrot, M., Dupej, P., Dwyer, S., Edo, T., Edwards, M., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S., Eisenstein, R., Essick, R., Estevez, D., Etienne, Z., Etzel, T., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W., Fauchon-Jones, E., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M., Fernandez-Galiana, A., Ferrante, I., Ferreira, E., Ferrini, F., Fidecaro, F., Finstad, D., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J., Forsyth, P., Forsyth, S., Fournier, J., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E., Fritschel, P., Frolov, V., Fulda, P., Fyffe, M., Gabbard, H., Gadre, B., Gaebel, S., Gair, J., Gammaitoni, L., Ganija, M., Gaonkar, S., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, A., Ghosh, S., Giaime, J., Giardina, K., Giazotto, A., Gill, K., Glover, L., Goetz, E., Goetz, R., Gomes, S., Goncharov, B., Gonzlez, G., Castro, J., Gopakumar, A., Gorodetsky, M., Gossan, S., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A., Gretarsson, E., Griswold, B., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G., Guo, X., Gupta, A., Gupta, M., Gushwa, K., Gustafson, E., Gustafson, R., Halim, O., Hall, B., Hall, E., Hamilton, E., Hammond, G., Haney, M., Hanke, M., Hanks, J., Hanna, C., Hannam, M., Hannuksela, O., Hanson, J., Hardwick, T., Harms, J., Harry, G., Harry, I., Hart, M., Haster, C., Haughian, K., Healy, J., Heidmann, A., Heintze, M., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I., Hennig, J., Heptonstall, A., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hofman, D., Holt, K., Holz, D., Hopkins, P., Horst, C., Hough, J., Houston, E., Howell, E., Hreibi, A., Hu, Y., Huerta, E., Huet, D., Hughey, B., Husa, S., Huttner, S., Huynh-Dinh, T., Indik, N., Inta, R., Intini, G., Isa, H., Isac, J., Isi, M., Iyer, B., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jimenez-Forteza, F., Johnson, W., Jones, D., Jones, R., Jonker, R., Ju, L., Junker, J., Kalaghatgi, C., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J., Kapadia, S., Karki, S., Karvinen, K., Kasprzack, M., Katolik, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Kefelian, F., Keitel, D., Kemball, A., Kennedy, R., Kent, C., Key, J., Khalili, F., Khan, I., Khan, S., Khan, Z., Khazanov, E., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, W., Kim, Y., Kimbrell, S., King, E., King, P., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J., Kleybolte, L., Klimenko, S., Knowles, T., Koch, P., Koehlenbeck, S., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W., Kowalska, I., Kozak, D., Krmer, C., Kringel, V., Krishnan, B., Krlak, A., Kuehn, G., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B., Lai, K., Landry, M., Lang, R., Lange, J., Lantz, B., Lanza, R., Larson, S., Lartaux-Vollard, A., Lasky, P., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lee, C., Lee, H., Lee, K., Lehmann, J., Lenon, A., Leonardi, M., Leroy, N., Letendre, N., Levin, Y., Li, T., Linker, S., Littenberg, T., Liu, J., Lo, R., Lockerbie, N., London, L., Lord, J., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J., Lousto, C., Lovelace, G., Lck, H., Lumaca, D., Lundgren, A., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Machenschalk, B., MacInnis, M., Macleod, D., Hernandez, I., Magaa-Sandoval, F., Zertuche, L., Magee, R., Majorana, E., Maksimovic, I., Man, N., Mandic, V., Mangano, V., Mansell, G., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Mrka, S., Mrka, Z., Markakis, C., Markosyan, A., Markowitz, A., Maros, E., Marquina, A., Marsh, P., Martelli, F., Martellini, L., Martin, I., Martin, R., Martynov, D., Mason, K., Massera, E., Masserot, A., Massinger, T., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCarthy, R., McClelland, D., McCormick, S., McCuller, L., McGuire, S., McIntyre, G., McIver, J., McManus, D., McNeill, L., Mcrae, T., McWilliams, S., Meacher, D., Meadors, G., Mehmet, M., Meidam, J., Mejuto-Villa, E., Melatos, A., Mendell, G., Mercer, R., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P., Miao, H., Michel, C., Middleton, H., Mikhailov, E., Milano, L., Mueller, A., Mueller, B., Miller, J., Millhouse, M., Milovich-Goff, M., Minazzoli, O., Minenkov, Y., Ming, J., Mishra, C., Mitra, S., Mitrofanov, V., Mitselmakher, G., Mittleman, R., Moffa, D., Moggi, A., Mogushi, K., Mohan, M., Mohapatra, S., Montani, M., Moore, C., Moraru, D., Moreno, G., Morriss, S., Mours, B., Mow-Lowry, C., Mueller, G., Muir, A., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muniz, E., Muratore, M., Murray, P., Napier, K., Nardecchia, I., Naticchioni, L., Nayak, R., Neilson, J., Nelemans, G., Nelson, T., Nery, M., Neunzert, A., Nevin, L., Newport, J., Newton, G., Ng, K., Nguyen, P., Nguyen, T., Nichols, D., Nielsen, A., Nissanke, S., Nitz, A., Noack, A., Nocera, F., Nolting, D., North, C., Nuttall, L., Oberling, J., O'Dea, G., Ogin, G., Oh, J., Oh, S., Ohme, F., Okada, M., Oliver, M., Oppermann, P., Oram, R., O'Reilly, B., Ormiston, R., Ortega, L., O'Shaughnessy, R., Ossokine, S., Ottaway, D., Overmier, H., Owen, B., Pace, A., Page, J., Page, M., Pai, A., Pai, S., Palamos, J., Palashov, O., Palomba, C., Pal-Singh, A., Pan, H., Pang, B., Pang, P., Pankow, C., Pannarale, F., Pant, B., Paoletti, F., Paoli, A., Papa, M., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perez, C., Perreca, A., Perri, L., Pfeiffer, H., Phelps, M., Piccinni, O., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I., Pirello, M., Pitkin, M., Poe, M., Poggiani, R., Popolizio, P., Porter, E., Post, A., Powell, J., Prasad, J., Pratt, J., Pratten, G., Predoi, V., Prestegard, T., Price, L., Prijatelj, M., Principe, M., Privitera, S., Prodi, G., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Prrer, M., Qi, H., Quetschke, V., Quintero, E., Quitzow-James, R., Raab, F., Rabeling, D., Radkins, H., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K., Ramos-Buades, A., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D., Ren, W., Reyes, S., Ricci, F., Ricker, P., Rieger, S., Riles, K., Rizzo, M., Robertson, N., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J., Roma, V., Romano, R., Romel, C., Romie, J., Rosinska, D., Ross, M., Rowan, S., Rdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sampson, L., Sanchez, E., Sanchez, L., Sanchis-Gual, N., Sandberg, V., Sanders, J., Sassolas, B., Sathyaprakash, B., Saulson, P., Sauter, O., Savage, R., Sawadsky, A., Schale, P., Scheel, M., Scheuer, J., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R., Schonbeck, A., Schreiber, E., Schuette, D., Schulte, B., Schutz, B., Schwalbe, S., Scott, J., Scott, S., Seidel, E., Sellers, D., Sengupta, A., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D., Shaffer, T., Shah, A., Shahriar, M., Shaner, M., Shao, L., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A., Singer, L., Singh, A., Singhal, A., Sintes, A., Slagmolen, B., Smith, B., Smith, J., Smith, R., Somala, S., Son, E., Sonnenberg, J., Sorazu, B., Sorrentino, F., Souradeep, T., Spencer, A., Srivastava, A., Staats, K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S., Stone, R., Stops, D., Strain, K., Stratta, G., Strigin, S., Strunk, A., Sturani, R., Stuver, A., Summerscales, T., Sun, L., Sunil, S., Suresh, J., Sutton, P., Swinkels, B., Szczepanczyk, M., Tacca, M., Tait, S., Talbot, C., 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Abstract

© 2017. The American Astronomical Society. All rights reserved. On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma -ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40 8 8-+ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nu

Published
2017

344. Discovery of a z=0.65 post-starburst BAL quasar in the DES supernova fields

Author

Mudd, D., Martini, P., Tie, S., Lidman, C., McMahon, R., Banerji, M., Davis, T., Peterson, B., Sharp, R., Seymour, Nick, Childress, M., Lewis, G., Tucker, B., Yuan, F., Abbot, T., Abdalla, F., Allam, S., Benoit-Levy, A., Bertin, E., Brooks, D., Camero Rosell, A., Kind, M., Carretero, J., da Costa, L., Desai, S., Diehl, T., Eifler, T., Finley, D., Flaugher, B., Glazebrook, K., Gruen, D., Gruendl, R., Gutierrez, G., Hinton, S., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Macaulay, E., Maia, M., Miquel, R., Ogando, R., Plazas, A., Riel, K., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, R., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., Uddin, S., Walker, A., Zhang, B., Mudd, D., Martini, P., Tie, S., Lidman, C., McMahon, R., Banerji, M., Davis, T., Peterson, B., Sharp, R., Seymour, Nick, Childress, M., Lewis, G., Tucker, B., Yuan, F., Abbot, T., Abdalla, F., Allam, S., Benoit-Levy, A., Bertin, E., Brooks, D., Camero Rosell, A., Kind, M., Carretero, J., da Costa, L., Desai, S., Diehl, T., Eifler, T., Finley, D., Flaugher, B., Glazebrook, K., Gruen, D., Gruendl, R., Gutierrez, G., Hinton, S., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Macaulay, E., Maia, M., Miquel, R., Ogando, R., Plazas, A., Riel, K., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, R., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., Uddin, S., Walker, A., and Zhang, B.

Abstract

We present the discovery of a z = 0.65 low-ionization broad absorption line (LoBAL) quasar in a post-starburst galaxy in data from the Dark Energy Survey (DES) and spectroscopy from the Australian Dark Energy Survey (OzDES). LoBAL quasars are a minority of all BALs, and rarer still is that this object also exhibits broad Fe ii (an FeLoBAL) and Balmer absorption. This is the first BAL quasar that has signatures of recently truncated star formation, which we estimate ended about 40 Myr ago. The characteristic signatures of an FeLoBAL require high column densities, which could be explained by the emergence of a young quasar from an early, dust-enshrouded phase, or by clouds compressed by a blast wave. The age of the starburst component is comparable to estimates of the lifetime of quasars, so if we assume the quasar activity is related to the truncation of the star formation, this object is better explained by the blast wave scenario.

Published
2017

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