Seeing the Outer Edge of the Infant Type Ia Supernova 2024epr in the Optical and Near Infrared
W. B. Hoogendam, D. O. Jones, C. Ashall, B. J. Shappee, R. J. Foley, M. A. Tucker, M. E. Huber, Katie Auchettl, D. Desai, A. Do, Jason T. Hinkle, S. Romagnoli, J. Shi, A. Syncatto, C. R. Angus, K. C. Chambers, D. A. Coulter, Kyle W. Davis, Thomas de Boer, Alexander Gagliano, M. Kong, Chien-Cheng Lin, T. Lowe, E. A. Magnier, P. Mínguez, Y. C. Pan, Kishore C. Patra, Scott Severson, K. Taggart, A. R. Wasserman, S. K. Yadavalli, Ping Chen, R. S. Post
Abstract
We present optical-to-near-infrared (NIR) photometry and spectroscopy of the Type Ia supernova (SN~Ia) 2024epr, including NIR spectra observed within two days of first light. The early-time optical spectra show strong, high-velocity Ca and Si features near rarely-observed velocities at $ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mn>0.1</mml:mn> </mml:math> c$, and the NIR spectra show a “knee.’’ Despite early-time, high-velocity features, SN~2024epr evolves into a normal SN~Ia, albeit with stronger peak-light Ca absorption than other SNe~Ia with the same light curve shape. Although we infer a normal decline rate, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mi>Δ</mml:mi> <mml:msub> <mml:mi>m</mml:mi> <mml:mn>15</mml:mn> </mml:msub> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mi>B</mml:mi> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo>=</mml:mo> <mml:mn>1.09</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.12</mml:mn> </mml:mrow> </mml:math> ~mag, from the light-curve rise, SN~2024epr is a Branch”cool’’ object and has red early-time colors ( <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mi>g</mml:mi> <mml:mo>−</mml:mo> <mml:mi>r</mml:mi> <mml:mo>≈</mml:mo> <mml:mn>0.15</mml:mn> </mml:mrow> </mml:math> ~mag at <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>10</mml:mn> </mml:mrow> </mml:math> ~days). The high velocities point to a density enhancement in the outer layers of the explosion, predicted by some models, but thick-shell He-detonation models do not match the smoothly rising light curve or apparent lack of He in our early-time NIR spectra. No current models (e.g., delayed detonation or thin He shell double detonation) appear to reproduce all observed properties, particularly the unusual early-time colors. Such constraints are only possible for SN~2024epr from the earliest optical and NIR observations, highlighting their importance for constraining SN~Ia models. Finally, we identify several literature SNe~Ia with intermediate mass elements at $ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mn>30</mml:mn> <mml:mspace width="0.167em"/> <mml:mn>000</mml:mn> <mml:mspace width="0.222em"/> <mml:mi>k</mml:mi> <mml:mi>m</mml:mi> <mml:mspace width="0.222em"/> <mml:mi>s</mml:mi> </mml:mrow> </mml:math> ^{-1}$ within days after the explosion that evolve into otherwise normal SNe~Ia at peak light, suggesting the early-time spectra of SNe~Ia may hide a broad diversity of observational characteristics.