6 code implementations • 16 Jan 2014 • M. Betoule, R. Kessler, J. Guy, J. Mosher, D. Hardin, R. Biswas, P. Astier, P. El-Hage, M. Konig, S. Kuhlmann, J. Marriner, R. Pain, N. Regnault, C. Balland, B. A. Bassett, P. J. Brown, H. Campbell, R. G. Carlberg, F. Cellier-Holzem, D. Cinabro, A. Conley, C. B. D'Andrea, D. L. Depoy, M. Doi, R. S. Ellis, S. Fabbro, A. V. Filippenko, R. J. Foley, J. A. Frieman, D. Fouchez, L. Galbany, A. Goobar, R. R. Gupta, G. J. Hill, R. Hlozek, C. J. Hogan, I. M. Hook, D. A. Howell, S. W. Jha, L. Le Guillou, G. Leloudas, C. Lidman, J. L. Marshall, A. Möller, A. M. Mourão, J. Neveu, R. Nichol, M. D. Olmstead, N. Palanque-Delabrouille, S. Perlmutter, J. L. Prieto, C. J. Pritchet, M. Richmond, A. G. Riess, V. Ruhlmann-Kleider, M. Sako, K. Schahmaneche, D. P. Schneider, M. Smith, J. Sollerman, M. Sullivan, N. A. Walton, C. J. Wheeler
We have followed the methods and assumptions of the SNLS 3-year data analysis except for the following important improvements: 1) the addition of the full SDSS-II spectroscopically-confirmed SN Ia sample in both the training of the SALT2 light curve model and in the Hubble diagram analysis (\nsdssc SNe), 2) inter-calibration of the SNLS and SDSS surveys and reduced systematic uncertainties in the photometric calibration, performed blindly with respect to the cosmology analysis, and 3) a thorough investigation of systematic errors associated with the SALT2 modeling of SN Ia light-curves.
Cosmology and Nongalactic Astrophysics
2 code implementations • 2 Oct 2017 • D. M. Scolnic, D. O. Jones, A. Rest, Y. C. Pan, R. Chornock, R. J. Foley, M. E. Huber, R. Kessler, G. Narayan, A. G. Riess, S. Rodney, E. Berger, D. J. Brout, P. J. Challis, M. Drout, D. Finkbeiner, R. Lunnan, R. P. Kirshner, N. E. Sanders, E. Schlafly, S. Smartt, C. W. Stubbs, J. Tonry, W. M. Wood-Vasey, M. Foley, J. Hand, E. Johnson, W. S. Burgett, K. C. Chambers, P. W. Draper, K. W. Hodapp, N. Kaiser, R. P. Kudritzki, E. A. Magnier, N. Metcalfe, F. Bresolin, E. Gall, R. Kotak, M. McCrum, K. W. Smith
When the SN and CMB constraints are combined with constraints from BAO and local H0 measurements, the analysis yields the most precise measurement of dark energy to date: $w0 = -1. 007\pm 0. 089$ and $wa = -0. 222 \pm0. 407$ for the w0waCDM model.
Cosmology and Nongalactic Astrophysics
1 code implementation • 12 Apr 2015 • D. A. Goldstein, C. B. D'Andrea, J. A. Fischer, R. J. Foley, R. R. Gupta, R. Kessler, A. G. Kim, R. C. Nichol, P. Nugent, A. Papadopoulos, M. Sako, M. Smith, M. Sullivan, R. C. Thomas, W. Wester, R. C. Wolf, F. B. Abdalla, M. Banerji, A. Benoit-Lévy, E. Bertin, D. Brooks, A. Carnero Rosell, F. J. Castander, L. N. da Costa, R. Covarrubias, D. L. Depoy, S. Desai, H. T. Diehl, P. Doel, T. F. Eifler, A. Fausti Neto, D. A. Finley, B. Flaugher, P. Fosalba, J. Frieman, D. Gerdes, D. Gruen, R. A. Gruendl, D. James, K. Kuehn, N. Kuropatkin, O. Lahav, T. S. Li, M. A. G. Maia, M. Makler, M. March, J. L. Marshall, P. Martini, K. W. Merritt, R. Miquel, B. Nord, R. Ogando, A. A. Plazas, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, I. Sevilla-Noarbe, R. C. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E. C. Swanson, G. Tarle, J. Thaler, A. R. Walker
We describe an algorithm for identifying point-source transients and moving objects on reference-subtracted optical images containing artifacts of processing and instrumentation.
Instrumentation and Methods for Astrophysics
no code implementations • 19 May 2020 • T. de Jaeger, L. Galbany, S. González-Gaitán, R. Kessler, A. V. Filippenko, F. Förster, M. Hamuy, P. J. Brown, T. M. Davis, C. P. Gutiérrez, C. Inserra, G F. Lewis, A. Möller, D. Scolnic, M. Smith, D. Brout, D. Carollo, R. J. Foley, K. Glazebrook, S. R. Hinton, E. Macaulay, B. Nichol, M. Sako, N. E. Sommer, B. E. Tucker, T. M. C. Abbott, M. Aguena, S. Allam, J. Annis, S. Avila, E. Bertin, S. Bhargava, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, M. Crocce, L. N. da Costa, J. De Vicente, S. Desai, H. T. Diehl, P. Doel, A. Drlica-Wagner, T. F. Eifler, J. Estrada, S. Everett, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, W. G. Hartley, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, N. Kuropatkin, T. S. Li, M. Lima, M. A. G. Maia, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. A. Plazas, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, D. L. Tucker, T. N. Varga, A. R. Walker, J. Weller, R. Wilkinson
Despite vast improvements in the measurement of the cosmological parameters, the nature of dark energy and an accurate value of the Hubble constant (H$_0$) in the Hubble-Lema\^itre law remain unknown.
High Energy Astrophysical Phenomena Cosmology and Nongalactic Astrophysics
no code implementations • 14 Dec 2020 • J. D. R. Pierel, D. O. Jones, M. Dai, D. Q. Adams, R. Kessler, S. Rodney, M. R. Siebert, R. J. Foley, W. D. Kenworthy, D. Scolnic
By using BYOSED for SN Ia cosmology simulations, future analyses (e. g., Rubin and Roman SN Ia samples) will have greater flexibility to constrain or reduce such SN Ia modeling uncertainties.
Cosmology and Nongalactic Astrophysics
no code implementations • 21 Dec 2020 • K. Paterson, M. J. Lundquist, J. C. Rastinejad, W. Fong, D. J. Sand, J. E. Andrews, R. C. Amaro, O. Eskandari, S. Wyatt, P. N. Daly, H. Bradley, S. Zhou-Wright, S. Valenti, S. Yang, E. Christensen, A. R. Gibbs, F. Shelly, C. Bilinski, L. Chomiuk, A. Corsi, M. R. Drout, R. J. Foley, P. Gabor, P. Garnavich, C. J. Grier, E. Hamden, H. Krantz, E. Olszewski, V. Paschalidis, D. Reichart, A. Rest, N. Smith, J. Strader, D. Trilling, C. Veillet, R. M. Wagner, A. Zabludoff
In addition to triggered events within 24~hours, our transient search encompassed a time interval following GW events of $<120$~hrs, providing observations on $\sim$ 1/2 of the events accessible to the Mt Lemmon 1. 5 m telescope.
High Energy Astrophysical Phenomena
