10 results on '"D. Scolnic"'
Search Results
2. Studying Type II supernovae as cosmological standard candles using the Dark Energy Survey
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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, and R Wilkinson
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- 2020
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3. STRIDES: a 3.9 per cent measurement of the Hubble constant from the strong lens system DES J0408−5354
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A J Shajib, S Birrer, T Treu, A Agnello, E J Buckley-Geer, J H H Chan, L Christensen, C Lemon, H Lin, M Millon, J Poh, C E Rusu, D Sluse, C Spiniello, G C-F Chen, T Collett, F Courbin, C D Fassnacht, J Frieman, A Galan, D Gilman, A More, T Anguita, M W Auger, V Bonvin, R McMahon, G Meylan, K C Wong, T M C Abbott, J Annis, S Avila, K Bechtol, D Brooks, D Brout, D L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, F J Castander, M Costanzi, L N da Costa, J De Vicente, S Desai, J P Dietrich, P Doel, A Drlica-Wagner, A E Evrard, D A Finley, B Flaugher, P Fosalba, J García-Bellido, D W Gerdes, D Gruen, R A Gruendl, J Gschwend, G Gutierrez, D L Hollowood, K Honscheid, D Huterer, D J James, T Jeltema, E Krause, N Kuropatkin, T S Li, M Lima, N MacCrann, M A G Maia, J L Marshall, P Melchior, R Miquel, R L C Ogando, A Palmese, F Paz-Chinchón, A A Plazas, A K Romer, A Roodman, M Sako, E Sanchez, B Santiago, V Scarpine, M Schubnell, D Scolnic, S Serrano, I Sevilla-Noarbe, M Smith, M Soares-Santos, E Suchyta, G Tarle, D Thomas, A R Walker, and Y Zhang
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- 2020
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4. The Dark Energy Survey Supernova Programme: Modelling Selection Efficiency and Observed Core-collapse Supernova Contamination
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M Vincenzi, M Sullivan, O Graur, D Brout, T M Davis, C Frohmaier, L Galbany, C P Gutierrez, S R Hinton, R Hounsell, L Kelsey, R Kessler, E Kovacs, S Kuhlmann, J Lasker, C Lidman, A Moller, R C Nichol, M Sako, D Scolnic, M Smith, E Swann, P Wiseman, J Asore, G F Lewis, R Sharp, B E Tucker, M Aguena, S Allam, S Avila, E Bertin, D Brooks, D L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, F J Castander, A Choi, M Costanzi, L N da Costa, M E S Pereira, J De Vicente, S Desai, H T Diehl, P Doel, S Everett, I Ferrero, P Fosalba, J Frieman, J Garcia-Bellido, E Gaztanaga, D W Gerdes, D Gruen, R A Gruendl, G Gutierrez, D L Hollowood, K Honscheid, B Hoyle, D J James, K Kuehn, N Kuropatkin, M A G Maia, P Martini, F Menanteau, R Miquel, R Morgan, A Palmese, F Paz-Chinchon, A A Plazas, A K Romer, E Sanchez, V Scarpine, S Serrano, I Sevilla-Noarbe, M Soares-Santos, E Suchyta, G Tarle, D Thomas, C To, T N Varga, A R Walker, and R D Wilkinson
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Astronomy - Abstract
The analysis of current and future cosmological surveys of Type Ia supernovae (SNe Ia) at high redshift depends on the accuratephotometric classification of the SN events detected. Generating realistic simulations of photometric SN surveys constitutes anessential step for training and testing photometric classification algorithms, and for correcting biases introduced by selectioneffects and contamination arising from core-collapse SNe in the photometric SN Ia samples. We use published SN time-seriesspectrophotometric templates, rates, luminosity functions, and empirical relationships between SNe and their host galaxies toconstruct a framework for simulating photometric SN surveys. We present this framework in the context of the Dark EnergySurvey (DES) 5-yr photometric SN sample, comparing our simulations of DES with the observed DES transient populations.We demonstrate excellent agreement in many distributions, including Hubble residuals, between our simulations and data.We estimate the core collapse fraction expected in the DES SN sample after selection requirements are applied and beforephotometric classification. After testing different modelling choices and astrophysical assumptions underlying our simulation,we find that the predicted contamination varies from 7.2 to 11.7 per cent, with an average of 8.8 per cent and an r.m.s. of 1.1 percent. Our simulations are the first to reproduce the observed photometric SN and host galaxy properties in high-redshift surveyswithout fine-tuning the input parameters. The simulation methods presented here will be a critical component of the cosmologyanalysis of the DES photometric SN Ia sample: correcting for biases arising from contamination, and evaluating the associatedsystematic uncertainty.
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- 2021
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5. First cosmological results using Type Ia supernovae from the Dark Energy Survey: measurement of the Hubble constant
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E Macaulay, R C Nichol, D Bacon, D Brout, T M Davis, B Zhang, B A Bassett, D Scolnic, A Möller, C B D’Andrea, S R Hinton, R Kessler, A G Kim, J Lasker, C Lidman, M Sako, M Smith, M Sullivan, T M C Abbott, S Allam, J Annis, J Asorey, S Avila, K Bechtol, D Brooks, P Brown, D L Burke, J Calcino, A Carnero Rosell, D Carollo, M Carrasco Kind, J Carretero, F J Castander, T Collett, M Crocce, C E Cunha, L N da Costa, C Davis, J De Vicente, H T Diehl, P Doel, A Drlica-Wagner, T F Eifler, J Estrada, A E Evrard, A V Filippenko, D A Finley, B Flaugher, R J Foley, P Fosalba, J Frieman, L Galbany, J García-Bellido, E Gaztanaga, K Glazebrook, S González-Gaitán, D Gruen, R A Gruendl, J Gschwend, G Gutierrez, W G Hartley, D L Hollowood, K Honscheid, J K Hoormann, B Hoyle, D Huterer, B Jain, D J James, T Jeltema, E Kasai, E Krause, K Kuehn, N Kuropatkin, O Lahav, G F Lewis, T S Li, M Lima, H Lin, M A G Maia, J L Marshall, P Martini, R Miquel, P Nugent, A Palmese, Y-C Pan, A A Plazas, A K Romer, A Roodman, E Sanchez, V Scarpine, R Schindler, M Schubnell, S Serrano, I Sevilla-Noarbe, R Sharp, M Soares-Santos, F Sobreira, N E Sommer, E Suchyta, E Swann, M E C Swanson, G Tarle, D Thomas, R C Thomas, B E Tucker, S A Uddin, V Vikram, A R Walker, and P Wiseman
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- 2019
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6. First cosmology results using Type IA supernovae from the dark energy survey: effects of chromatic corrections to supernova photometry on measurements of cosmological parameters
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J Lasker, R Kessler, D Scolnic, D Brout, D L Burke, C B D’Andrea, T M Davis, S R Hinton, A G Kim, T S Li, C Lidman, E Macaulay, A Möller, E S Rykoff, M Sako, M Smith, M Sullivan, E Swann, B E Tucker, W Wester, B A Bassett, T M C Abbott, S Allam, J Annis, S Avila, K Bechtol, E Bertin, D Brooks, A Carnero Rosell, M Carrasco Kind, J Carretero, F J Castander, J Calcino, D Carollo, L N da Costa, C Davis, J De Vicente, H T Diehl, P Doel, A Drlica-Wagner, B Flaugher, J Frieman, J García-Bellido, E Gaztanaga, D Gruen, R A Gruendl, J Gschwend, G Gutierrez, D L Hollowood, K Honscheid, J K Hoormann, D J James, S Kent, E Krause, R Kron, K Kuehn, N Kuropatkin, M Lima, M A G Maia, J L Marshall, P Martini, F Menanteau, C J Miller, R Miquel, A A Plazas, E Sanchez, V Scarpine, I Sevilla-Noarbe, R C Smith, M Soares-Santos, F Sobreira, E Suchyta, M E C Swanson, G Tarle, D L Tucker, and A R Walker
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- 2019
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7. First cosmology results using Type Ia supernova from the Dark Energy Survey: simulations to correct supernova distance biases
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R Kessler, D Brout, C B D’Andrea, T M Davis, S R Hinton, A G Kim, J Lasker, C Lidman, E Macaulay, A Möller, M Sako, D Scolnic, M Smith, M Sullivan, B Zhang, P Andersen, J Asorey, A Avelino, J Calcino, D Carollo, P Challis, M Childress, A Clocchiatti, S Crawford, A V Filippenko, R J Foley, K Glazebrook, J K Hoormann, E Kasai, R P Kirshner, G F Lewis, K S Mandel, M March, E Morganson, D Muthukrishna, P Nugent, Y-C Pan, N E Sommer, E Swann, R C Thomas, B E Tucker, S A Uddin, T M C Abbott, S Allam, J Annis, S Avila, M Banerji, K Bechtol, E Bertin, D Brooks, E Buckley-Geer, D L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, F J Castander, M Crocce, L N da Costa, C Davis, J De Vicente, S Desai, H T Diehl, P Doel, T F Eifler, B Flaugher, P Fosalba, J Frieman, J García-Bellido, E Gaztanaga, D W Gerdes, D Gruen, R A Gruendl, G Gutierrez, W G Hartley, D L Hollowood, K Honscheid, D J James, M W G Johnson, M D Johnson, E Krause, K Kuehn, N Kuropatkin, O Lahav, T S Li, M Lima, J L Marshall, P Martini, F Menanteau, C J Miller, R Miquel, B Nord, A A Plazas, A Roodman, E Sanchez, V Scarpine, R Schindler, M Schubnell, S Serrano, I Sevilla-Noarbe, M Soares-Santos, F Sobreira, E Suchyta, G Tarle, D Thomas, A R Walker, and Y Zhang
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- 2019
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8. Using host galaxy spectroscopy to explore systematics in the standardization of Type Ia supernovae
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M Dixon, C Lidman, J Mould, L Kelsey, D Brout, A Möller, P Wiseman, M Sullivan, L Galbany, T M Davis, M Vincenzi, D Scolnic, G F Lewis, M Smith, R Kessler, A Duffy, E N Taylor, C Flynn, T M C Abbott, M Aguena, S Allam, F Andrade-Oliveira, J Annis, J Asorey, E Bertin, S Bocquet, D Brooks, D L Burke, A Carnero Rosell, D Carollo, M Carrasco Kind, J Carretero, M Costanzi, L N da Costa, M E S Pereira, P Doel, S Everett, I Ferrero, B Flaugher, D Friedel, J Frieman, J García-Bellido, M Gatti, D W Gerdes, K Glazebrook, D Gruen, J Gschwend, G Gutierrez, S R Hinton, D L Hollowood, K Honscheid, D Huterer, D J James, K Kuehn, N Kuropatkin, U Malik, M March, F Menanteau, R Miquel, R Morgan, B Nichol, R L C Ogando, A Palmese, F Paz-Chinchón, A Pieres, A A Plazas Malagón, M Rodriguez-Monroy, A K Romer, E Sanchez, V Scarpine, I Sevilla-Noarbe, M Soares-Santos, E Suchyta, G Tarle, C To, B E Tucker, D L Tucker, T N Varga, Dixon, M., Lidman, C., Mould, J., Kelsey, L., Brout, D., Möller, A., Wiseman, P., Sullivan, M., Galbany, L., Davis, T. M., Vincenzi, M., Scolnic, D., Lewis, G. F., Smith, M., Kessler, R., Duffy, A., Taylor, E. N., Flynn, C., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Asorey, J., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gerdes, D. W., Glazebrook, K., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Kuropatkin, N., Malik, U., March, M., Menanteau, F., Miquel, R., Morgan, R., Nichol, B., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Tucker, B. E., Tucker, D. L., Varga, T. N., Australian Research Council, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Generalitat de Catalunya, European Commission, and European Research Council
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Galaxies: general ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmology: observations ,cosmology observations ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Surveys ,Astrophysics - Astrophysics of Galaxies ,Space and Planetary Science ,surveys ,galaxies general ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::Solar and Stellar Astrophysics ,survey ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
M. Dixon et al., We use stacked spectra of the host galaxies of photometrically identified Type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) to search for correlations between Hubble diagram residuals and the spectral properties of the host galaxies. Utilizing full spectrum fitting techniques on stacked spectra binned by Hubble residual, we find no evidence for trends between Hubble residuals and properties of the host galaxies that rely on spectral absorption features (, MD would like to acknowledge support through an Australian Government Research Training Program Scholarship. This research was supported by the Australian Research Council The Centre of Excellence for Dark Matter Particle Physics (CDM; project number CE200100008) and the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav; project number CE170100004). This project/publication was made possible through the support of a grant from the John Templeton Foundation. The authors gratefully acknowledge this grant ID 61807, Two Standard Models Meet. The opinions expressed in this publication are those of the author(s) and do not necessarily reflect the views of the John Templeton Foundation. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. Based on data acquired at the Anglo-Australian Telescope, under program A/2013B/012. We acknowledge the traditional custodians of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present.
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- 2022
9. Constraining RV variation using highly reddened Type Ia supernovae from the Pantheon+ sample
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B M Rose, B Popovic, D Scolnic, and D Brout
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Space and Planetary Science ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Type Ia supernovae (SNe Ia) are powerful tools for measuring the expansion history of the universe, but the impact of dust around SNe Ia remains unknown and is a critical systematic uncertainty. One way to improve our empirical description of dust is to analyse highly reddened SNe Ia ($E(B-V)>0.4$, roughly equivalent to the fitted SALT2 light-curve parameter $c>0.3$). With the recently released Pantheon+ sample, there are 57 SNe Ia that were removed because of their high colour alone (with colours up to $c=1.61$), which can provide enormous leverage on understanding line-of-sight $R_V$. Previous studies have claimed that $R_V$ decreases with redder colour, though it is unclear if this is due to limited statistics, selection effects, or an alternative explanation. To test this claim, we fit two separate colour-luminosity relationships, one for the main cosmological sample ($c0.3$) SNe Ia. We find the change in the colour-luminosity coefficient to be consistent with zero. Additionally, we compare the data to simulations with different colour models, and find that the data prefers a model with a flat dependence of $R_V$ on colour over a declining dependence. Finally, our results strongly support that line-of-sight $R_V$ to SNe Ia is not a single value, but forms a distribution., Accepted to MNRAS, updating to match accepted version. 11 pages, 9 figures, 5 tables
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- 2022
10. The dark energy survey 5-yr photometrically identified type Ia supernovae
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A Möller, M Smith, M Sako, M Sullivan, M Vincenzi, P Wiseman, P Armstrong, J Asorey, D Brout, D Carollo, T M Davis, C Frohmaier, L Galbany, K Glazebrook, L Kelsey, R Kessler, G F Lewis, C Lidman, U Malik, R C Nichol, D Scolnic, B E Tucker, T M C Abbott, M Aguena, S Allam, J Annis, E Bertin, S Bocquet, D Brooks, D L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, F J Castander, C Conselice, M Costanzi, M Crocce, L N da Costa, J De Vicente, S Desai, H T Diehl, P Doel, S Everett, I Ferrero, D A Finley, B Flaugher, D Friedel, J Frieman, J García-Bellido, D W Gerdes, D Gruen, R A Gruendl, J Gschwend, G Gutierrez, K Herner, S R Hinton, D L Hollowood, K Honscheid, D J James, K Kuehn, N Kuropatkin, O Lahav, M March, J L Marshall, F Menanteau, R Miquel, R Morgan, A Palmese, F Paz-Chinchón, A Pieres, A A Plazas Malagón, A K Romer, A Roodman, E Sanchez, V Scarpine, M Schubnell, S Serrano, I Sevilla-Noarbe, E Suchyta, G Tarle, D Thomas, C To, T N Varga, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, European Research Council, Generalitat de Catalunya, Consejo Superior de Investigaciones Científicas (España), Ministerio de Economía y Competitividad (España), UAM. Departamento de Física Teórica, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmology: observations ,Supernovae: general ,FOS: Physical sciences ,Física ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Surveys ,Methods: data analysis ,Space and Planetary Science ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,Astrophysics - Instrumentation and Methods for Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
As part of the cosmology analysis using Type Ia Supernovae (SN Ia) in the Dark Energy Survey (DES), we present photometrically identified SN Ia samples using multiband light curves and host galaxy redshifts. For this analysis, we use the photometric classification framework SUPERNNOVAtrained on realistic DES-like simulations. For reliable classification, we process the DES SN programme (DES-SN) data and introduce improvements to the classifier architecture, obtaining classification accuracies of more than 98 per cent on simulations. This is the first SN classification to make use of ensemble methods, resulting in more robust samples. Using photometry, host galaxy redshifts, and a classification probability requirement, we identify 1863 SNe Ia from which we select 1484 cosmology-grade SNe Ia spanning the redshift range of 0.07 < z < 1.14. We find good agreement between the light-curve properties of the photometrically selected sample and simulations. Additionally, we create similar SN Ia samples using two types of Bayesian Neural Network classifiers that provide uncertainties on the classification probabilities. We test the feasibility of using these uncertainties as indicators for out-of-distribution candidates and model confidence. Finally, we discuss the implications of photometric samples and classification methods for future surveys such as Vera C. Rubin Observatory Legacy Survey of Space and Time., This paper has gone through internal review by the DES collaboration. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule Zürich (ETH), Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This work was completed in part with Midway resources provided by the University of Chicago’s Research Computing Center. This work makes use of data acquired at the Anglo-Australian Telescope, under program A/2013B/012. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present. MS is funded by the European Reearch Council (ERC) under the European Union’s Horizon 2020 Research and Innovation program (grant agreement no 759194 - USNAC). LG acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and the European Social Fund (ESF) ‘Investing in your future under the 2019 Ramón y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project, and from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016. LK thanks the UKRI Future Leaders Fellowship for support through the grant MR/T01881X/1.
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