Now showing items 1-4 of 4

    • Phillips, M. M.; Contreras, Carlos; Hsiao, E. Y.; Morrell, Nidia; Burns, Christopher R.; Stritzinger, Maximilian; Ashall, C.; Freedman, Wendy L.; Hoeflich, P.; Persson, S. E.; Piro, Anthony L.; Suntzeff, Nicholas B.; Uddin, Syed A.; Anais, Jorge; Baron, E.; Busta, Luis; (Institute of Physics Publishing, 2019)
      © 2018. The Astronomical Society of the Pacific. All rights reserved. Printed in the U.S.A.The Carnegie Supernova Project-II (CSP-II) was an NSF-funded, four-year program to obtain optical and near-infrared observations ...
    • Hsiao, E. Y.; Phillips, M. M.; Marion, G. H.; Kirshner, R. P.; Morrell, N.; Sand, D. J.; Burns, C. R.; Contreras, C.; Hoeflich, P.; Stritzinger, M. D.; Valenti, S.; Anderson, J. P.; Ashall, C.; Baltay, C.; Baron, E.; Banerjee, D. P.K.; Davis, S.; Diamond, T. R.; Folatelli, Gastón (Institute of Physics Publishing, 2019)
      Shifting the focus of Type Ia supernova (SN Ia) cosmology to the near infrared (NIR) is a promising way to significantly reduce the systematic errors, as the strategy minimizes our reliance on the empirical width-luminosity ...
    • Li, W.; Wang, X.; Vinkó, J.; Mo, J.; Hosseinzadeh, G.; Sand, D. J.; Zhang, J.; Lin, H.; Zhang, T.; Wang, L.; Zhang, J.; Chen, Z.; Xiang, D.; Rui, L.; Huang, F.; Li, X.; Zhang, X.; Li, L.; Baron, E.; Derkacy, J. M.; Zhao, X.; Sai, H.; Zhang, K.; Wang, L.; Howell, D. A.; McCully, C.; Arcavi, I.; Valenti, S.; Hiramatsu, D.; Burke, J.; Rest, A.; Garnavich, P.; Tucker, B. E.; Narayan, G.; Shaya, E.; Margheim, S.; Zenteno, A.; Villar, A.; Dimitriadis, G.; Foley, R. J.; Pan, Y.-C.; Coulter, D. A.; Fox, O. D.; Jha, S. W.; Jones, D. O.; Kasen, N. D.; Kilpatrick, C. D.; Piro, A. L.; Riess, A. G.; Rojas Bravo, C.; Shappee, B. J.; Holoien, T. W.-S.; Stanek, K. Z.; Drout, M. R.; Auchettl, K.; Kochanek, C. S.; Brown, J. S.; Bose, S.; Bersier, D.; Brimacombe, J.; Chen, P.; Dong, S.; Holmbo, S.; Muñoz, J. A.; Mutel, R. L.; Post, R. S.; Prieto, J. L.; Shields, J.; Tallon, D.; Thompson, T. A.; Vallely, P. J.; Villanueva, S.; Smartt, S. J.; Smith, K. W.; Chambers, K. C.; Flewelling, H. A.; Huber, M. E.; Magnier, E. A.; Waters, C. Z.; Schultz, A. S. B.; Bulger, J.; Lowe, T. B.; Willman, M.; Sárneczky, K.; Pál, A.; Wheeler, J. C.; Bódi, A.; Bognár, Zs.; Csák, B.; Cseh, B.; Csörnyei, G.; Hanyecz, O.; Ignácz, B.; Kalup, Cs.; Könyves-Tóth, R.; Kriskovics, L.; Ordasi, A.; Rajmon, I.; Sódor, A.; Szabó, R.; Szakáts, R.; Zsidi, G.; Milne, P.; Andrews, J. E.; Smith, N.; Bilinski, C.; Brown, P. J.; Nordin, J.; Williams, S. C.; Galbany, Lluis; Palmerio, J.; Hook, I. M.; Inserra, C.; Maguire, K.; Cartier, Régis; Razza, A.; Gutiérrez, C. P.; Hermes, J. J.; Reding, J. S.; Kaiser, B. C.; Tonry, J. L.; Heinze, A. N.; Denneau, L.; Weiland, H.; Stalder, B.; Barentsen, G.; Dotson, J.; Barclay, T.; Gully-Santiago, M.; Hedges, C.; Cody, A. M.; Howell, S.; Coughlin, J.; Van Cleve, J. E.; Vinícius de Miranda Cardoso, J.; Larson, K. A.; McCalmont-Everton, K. M.; Peterson, C. A.; Ross, S. E.; Reedy, L. H.; Osborne, D.; McGinn, C.; Kohnert, L.; Migliorini, L.; Spencer, B.; Labonde, C.; Castillo, G.; Beerman, G.; Steward, K.; Hanley, M.; Larsen, R.; Gangopadhyay, R.; Kloetzel, R.; Weschler, T.; Nystrom, V.; Moffatt, J.; Redick, M.; Griest, K.; Packard, M.; Muszynski, M.; Kampmeier, J.; Bjella, R.; Flynn, S.; Elsaesser, B. (IOP Publishing, 2019)
      Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically confirmed Type Ia supernova (SN Ia) observed in the Kepler field. The Kepler data revealed an excess emission in its early light curve, allowing us to place ...
    • Vallely, Patrick; Vallely, Patrick; Moreno Raya, M. E.; Baron, E.; Ruiz Lapuente, Pilar; Domínguez, I.; Galbany, Lluis; González Hernández, J. I.; Méndez, J.; Hamuy Wackenhut, Mario; López Sánchez, Ángel R.; Catalan, S.; Cooke, E.; Farina, C.; Génova Santos, R.; Karjalainen, R.; Lietzen, H.; McCormac, J.; Riddick, F.; Rubino Martin, J. A.; Skillen, I.; Tudor, V.; Vaduvescu, O. (Oxford Univ. Press Inc., 2016)
      We analyse a time series of optical spectra of SN 2014J from almost two weeks prior to maximum to nearly four months after maximum. We perform our analysis using the synow code, which is well suited to track the distribution ...