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A Bright Ultraviolet Excess in the Transitional 02es-like Type Ia Supernova 2019yvq

Jamison BurkeLas Cumbres Observatory, 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USAD. A. HowellLas Cumbres Observatory, 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USASumit K. SarbadhicaryCenter for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USADavid SandSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USAR. AmaroSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USADaichi HiramatsuLas Cumbres Observatory, 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USACurtis McCullyDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USAC. PellegrinoDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USAJennifer E. AndrewsSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USAPeter J. BrownGeorge P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A & M University, College Station, TX 77843, USAKoichi 公一 Itagaki 板垣Melissa ShahbandehDepartment of Physics, Florida State University, Tallahassee, FL 32306, USAO. FoxDepartment of Physics and Astronomy, University of California, 1 Shields Avenue, Davis, CA 95616-5270, USALaura ChomiukCenter for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USAE. Y. HsiaoDepartment of Physics, Florida State University, Tallahassee, FL 32306, USANathan SmithSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USAStefano ValentiDepartment of Physics and Astronomy, University of California, 1 Shields Avenue, Davis, CA 95616-5270, USA

2021en

ABI

Аннотация

We present photometric and spectroscopic observations of the nearby Type Ia SN 2019yvq, from its discovery $\sim$1 day after explosion to $\sim$100 days after its peak brightness. This SN exhibits several unusual features, most notably an extremely bright UV excess seen within $\sim$5 days of its explosion. As seen in Swift UV data, this early excess outshines its "peak" brightness, making this object more extreme than other SNe with early UV/blue excesses (e.g. iPTF14atg and SN 2017cbv). In addition, it was underluminous ($M_B=-18.4$), relatively quickly declining ($\Delta m_{15}(B)=1.35$), and shows red colors past its early blue bump. Unusual (although not unprecedented) spectral features include extremely broad-lined and high-velocity Si absorption. Despite obvious differences in peak spectra, we classify SN 2019yvq as a transitional member of the 02es-like subclass due to its similarities in several respects (e.g. color, peak luminosity, peak Ti, nebular [Ca II]). We model this dataset with a variety of published models, including SN ejecta - companion shock interaction and sub-Chandrasekhar mass WD double detonation models. Radio constraints from the VLA place an upper limit of $(4.5 - 20) \times 10^{-8}$ M$_{\odot}$/yr on the mass-loss rate from a symbiotic progenitor, which does not exclude a red giant or main sequence companion. Ultimately we find that no one model can accurately replicate all aspects of the dataset, and further we find that the ubiquity of early excesses in 02es-like SNe Ia requires a progenitor system that is capable of producing isotropic UV flux, ruling out some models for this class of objects.

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DOI: 10.3847/1538-4357/ac126b

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