StaNdaRT: a repository of standardised test models and outputs for supernova radiative transfer

¹ Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
e-mail: stephane.blondin@lam.fr
² Unidad Mixta Internacional Franco-Chilena de Astronomía, CNRS/INSU UMI 3386 and Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile
³ NRC “Kurchatov institute”, Institute for Theoretical and Experimental Physics (ITEP), Moscow 117218, Russia
⁴ Sternberg Astronomical Institute, Moscow State University, Moscow 119234, Russia
⁵ Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
⁶ Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, Northern Ireland, UK
⁷ GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany
⁸ Institut d’Astrophysique de Paris, CNRS-Sorbonne Université, 98 bis boulevard Arago, 75014 Paris, France
⁹ Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
¹⁰ Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, 87545, USA
¹¹ Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48823, USA
¹² Department of Physics and Astronomy & Pittsburgh Particle Physics, Astrophysics, and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USA
¹³ The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden
¹⁴ Departments of Physics and Astronomy, University of California Berkeley and Lawrence Berkeley National Laboratory, USA
¹⁵ Department of Particle Phys. & Astrophys., Weizmann Institute of Science, Rehovot 76100, Israel
¹⁶ Department of Computational Mathematics, Science, and Engineering, Michigan State University, East Lansing, MI 48824, USA
¹⁷ Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, 85748 Garching bei München, Germany
¹⁸ Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, La Plata B1900, Argentina
¹⁹ Department of Astronomy and Theoretical Astrophysics Center, University of California, Berkeley, CA 94720, USA
²⁰ Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya St. 48, 119017 Moscow, Russia
²¹ Department of Physics, New York University, New York, NY 10003, USA
²² Computer, Computational, and Statistical Sciences Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
²³ Department of Physics & Astronomy, Louisiana State University, Baton Rouge, LA 70803, USA
²⁴ Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
²⁵ Department of Physics, NRCN, Beer-Sheva 84190, Israel
²⁶ ARTIS Collaboration  
²⁷ CMFGEN Collaboration  
²⁸ CRAB Collaboration  
²⁹ KEPLER Collaboration  
³⁰ SEDONA Collaboration  
³¹ STELLA Collaboration  
³² SUMO Collaboration  
³³ SuperNu Collaboration  
³⁴ TARDIS Collaboration  
³⁵ URILIGHT Collaboration  

Received: 27 May 2022
Accepted: 22 September 2022

Abstract

We present the first results of a comprehensive supernova (SN) radiative-transfer (RT) code-comparison initiative (StaNdaRT), where the emission from the same set of standardised test models is simulated by currently used RT codes. We ran a total of ten codes on a set of four benchmark ejecta models of Type Ia SNe. We consider two sub-Chandrasekhar-mass (M_tot = 1.0 M_⊙) toy models with analytic density and composition profiles and two Chandrasekhar-mass delayed-detonation models that are outcomes of hydrodynamical simulations. We adopt spherical symmetry for all four models. The results of the different codes, including the light curves, spectra, and the evolution of several physical properties as a function of radius and time are provided in electronic form in a standard format via a public repository. We also include the detailed test model profiles and several Python scripts for accessing and presenting the input and output files. We also provide the code used to generate the toy models studied here. In this paper, we describe the test models, radiative-transfer codes, and output formats in detail, and provide access to the repository. We present example results of several key diagnostic features.