Examinando por Autor "Palmese, A."

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    SOAR/Goodman Spectroscopic Assessment of Candidate Counterparts of the LIGO/Virgo Event GW190814
    (IOP Publishing Ltd, 2022-04-01) Tucker, D.L.; Wiesner, M.P.; Allam, S.S.; Soares-Santos, M.; Bom, C.R.; Butner, M.; Garcia, A.; Morgan, R.; Olivares, E. F.; Palmese, A.; Santana-Silva, L.; Shrivastava, A.; Annis, J.; García-Bellido, J.; Gill, M.S.S.; Herner, K.; Kilpatrick, C.D.; Makler, M.; Sherman, N.; Amara, A.; Lin, H.; Smith, M.; Swann, E.; Arcavi, I.; Bachmann, T.G.; Bechtol, K.; Berlfein, F.; Briceño, C.; Brout, D.; Butler, R.E.; Cartier, R.; Casares, J.; Chen, H.-Y.; Conselice, C.; Contreras, C.; Cook, E.; Cooke, J.; Dage, K.; D'Andrea, C.; Davis, T.M.; De Carvalho, R.; Diehl, H.T.; Dietrich, J.P.; Doctor, Z.; Drlica-Wagner, A.; Drout, M.; Farr, B.; Finley, D.A.; Fishbach, M.; Foley, R.J.; Förster-Burón, F.; Fosalba, P.; Friedel, D.; Frieman, J.; Frohmaier, C.; Gruendl, R.A.; Hartley, W.G.; Hiramatsu, D.; Holz, D.E.; Howell, D.A.; Kawash, A.; Kessler, R.; Kuropatkin, N.; Lahav, O.; Lundgren, A.; Lundquist, M.; Malik, U.; Mann, A.W.; Marriner, J.; Marshall, J.L.; Martínez-Vázquez, C.E.; McCully, C.; Menanteau, F.; Meza, N.; Narayan, G.; Neilsen, E.; Nicolaou, C.; Nichol, R.; Paz-Chinchón, F.; Pereira, M.E.S.; Pineda, J.; Points, S.; Quirola-Vásquez, J.; Rembold, S.; Rest, A.; Rodriguez, Ó.; Romer, A.K.; Sako, M.; Salim, S.; Scolnic, D.; Smith, J.A.; Strader, J.; Sullivan, M.; Swanson, M.E.C.; Thomas, D.; Valenti, S.; Varga, T.N.; Walker, A.R.; Weller, J.; Wood, M.L.; Yanny, B.; Zenteno, A.; Aguena, M.; Andrade-Oliveira, F.; Bertin, E.; Brooks, D.; Burke, D.L.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Costanzi, M.; Da Costa, L.N.; De Vicente, J.; Desai, S.; Everett, S.; Ferrero, I.; Flaugher, B.; Gaztanaga, E.; Gerdes, D.W.; Gruen, D.; Gschwend, J.; Gutierrez, G.; Hinton, S.R.; Hollowood, D.L.; Honscheid, K.; James, D.J.; Kuehn, K.; Lima, M.; Maia, M.A.G.; Miquel, R.; Ogando, R.L.C.; Pieres, A.; Plazas Malagón, A.A.; Rodriguez-Monroy, M.; Sanchez, E.; Scarpine, V.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I.; Suchyta, E.; Tarle, G.; To, C.; Zhang, Y.
    On 2019 August 14 at 21:10:39 UTC, the LIGO/Virgo Collaboration (LVC) detected a possible neutron star-black hole merger (NSBH), the first ever identified. An extensive search for an optical counterpart of this event, designated GW190814, was undertaken using the Dark Energy Camera on the 4 m Victor M. Blanco Telescope at the Cerro Tololo Inter-American Observatory. Target of Opportunity interrupts were issued on eight separate nights to observe 11 candidates using the 4.1 m Southern Astrophysical Research (SOAR) telescope's Goodman High Throughput Spectrograph in order to assess whether any of these transients was likely to be an optical counterpart of the possible NSBH merger. Here, we describe the process of observing with SOAR, the analysis of our spectra, our spectroscopic typing methodology, and our resultant conclusion that none of the candidates corresponded to the gravitational wave merger event but were all instead other transients. Finally, we describe the lessons learned from this effort. Application of these lessons will be critical for a successful community spectroscopic follow-up program for LVC observing run 4 (O4) and beyond. © 2022. The Author(s). Published by the American Astronomical Society.
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    The STRong lensing Insights into the dark energy survey (STRIDES) 2017/2018 follow-up campaign: Discovery of 10 lensed quasars and 10 quasar pairs
    (Oxford University Press, 2020) Lemon, C.; Auger, M.; Anguita, T.; McMahon, R.; Apostolovski, Y.; Chen, G.; Fassnacht, C.; Melo, A.; Motta, V.; Shajib, A.; Treu, T.; Agnello, A.; Buckley-Geer, E; Schechter, P.; Birrer, S.; Collett, T.; Courbin, F.; Rusu, C.; Abbott, T.; Allam, S.; Annis, J.; Avila, S.; Bertin, E.; Brooks, D.; Burke, D.; Carnero Rosell, A.; Carrasco Kind, M.; Carretero, J.; Costanzi, M.; Costa, L.; De Vicente, J.; Desai, S.; Eifler, T.; Flaugher, B.; Frieman, J.; Garcia-Bellido, J.; Gaztanaga, E.; Gerdes, D.; Gruen, D.; Gruendl, R.; Gschwend, J.; Gutierrez, G.; Honscheid, K.; James, D.; Kim, A.; Krause, E.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Lima, M.; Lin, H.; Maia, M.; March, M.; Marshall, J.; Menanteau, F.; Miquel, R.; Palmese, A.; Paz-Chinchon, F.; Plazas, A.; Roodman, A.; Sanchez, E.; Schubnell, M.; Serrano, S.; Smith, M.; Soares-Santos, M.; Suchyta, E.; Tarle, G.; Walker, A.
    We report the results of the STRong lensing Insights into the Dark Energy Survey (STRIDES) follow-up campaign of the late 2017/early 2018 season. We obtained spectra of 65 lensed quasar candidates with ESO Faint Object Spectrograph and Camera 2 on the NTT and Echellette Spectrograph and Imager onKeck, confirming 10 newlensed quasars and 10 quasar pairs. Eight lensed quasars are doubly imaged with source redshifts between 0.99 and 2.90, one is triply imaged (DESJ0345.2545, z = 1.68), and one is quadruply imaged (quad: DESJ0053.2012, z = 3.8). Singular isothermal ellipsoid models for the doubles, based on high-resolution imaging from SAMI on Southern Astrophysical Research Telescope or Near InfraRed Camera 2 on Keck, give total magnifications between 3.2 and 5.6, and Einstein radii between 0.49 and 1.97 arcsec. After spectroscopic follow-up, we extract multi-epoch grizY photometry of confirmed lensed quasars and contaminant quasar+star pairs from DES data using parametric multiband modelling, and compare variability in each system's components. By measuring the reduced χ2 associated with fitting all epochs to the samemagnitude, we find a simple cut on the less variable component that retains all confirmed lensed quasars, while removing 94 per cent of contaminant systems. Based on our spectroscopic follow-up, this variability information improves selection of lensed quasars and quasar pairs from 34-45 per cent to 51-70 per cent, with most remaining contaminants being star-forming galaxies. Using mock lensed quasar light curves we demonstrate that selection based only on variability will over-represent the quad fraction by 10 per cent over a complete DES magnitude-limited sample, explained by the magnification bias and hence lower luminosity/more variable sources in quads.