UV–OPTICAL OBSERVATION OF TYPE Ia SUPERNOVA SN 2013dy IN NGC 7250

Zhai, Qingfeng; Zhang, Jujia; Zhang, Tianmeng; Liu, Zheng-Wei; Brown, P. J.; Huang, Fan; Zhao, Xulin; Chang, Liang; Yi, Weimin; Wang, Chuanjun; Xin, Yuxin; Wang, Jianguo; Lun, Bao-Li; Zhang, Xiliang; Fan, Yufeng; Zheng, Xu-Chang; Bai, J. M.

doi:10.3847/0004-6256/151/5/125

Cited by 21 publications

(13 citation statements)

References 73 publications

(110 reference statements)

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“…The HVFs of both SiII λ6355 Figure 12. Spectra of SN 2018oh at t∼−9, −4, 0, and +8 days and +1 month after B maximum, along with the comparable-phase spectra of SNe 2002fk (Blondin et al 2012), 2003du (Stanishev et al 2007), 2005cf (Garavini et al 2007Wang et al 2009a), 2011fe (Mazzali et al 2014;Zhang et al 2016), 2012cg (Marion et al 2016), and 2013dy (Zheng et al 2013;Pan et al 2015;Zhai et al 2016). All spectra have been corrected for reddening and the redshift of the host galaxy.…”

Section: Ejecta Velocitymentioning

confidence: 99%

Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

Li¹,

Wang²,

Vinkó³

et al. 2018

ApJ

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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 interesting constraints on its progenitor system. Here we present extensive optical, ultraviolet, and nearinfrared photometry, as well as dense sampling of optical spectra, for this object. SN 2018oh is relatively normal in its photometric evolution, with a rise time of 18.3±0.3 days and Δm 15 (B)=0.96±0.03 mag, but it seems to have bluer B−V colors. We construct the "UVOIR" bolometric light curve having a peak luminosity of 1.49×10 43 erg s −1 , from which we derive a nickel mass as 0.55±0.04 M e by fitting radiation diffusion models powered by centrally located 56 Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of 56 Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a nondegenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia but is characterized by prominent and persistent carbon absorption features. The CII features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in an SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers.

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Section: Ejecta Velocitymentioning

confidence: 99%

Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

Li¹,

Wang²,

Vinkó³

et al. 2018

ApJ

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“…There is no evidence of circumstellar material in any of SN2013dy, SN 2016coj, SN 2018gv, SN 2018pv, and SN 2019np. The most well-studied of them is SN2013dy (Zheng et al 2013;Pan et al 2015;Zhai et al 2016). It was detected ∼2.4 hr after first light and had an abundance of unburned material in its envelope.…”

mentioning

confidence: 99%

The Deepest Radio Observations of Nearby SNe Ia: Constraining Progenitor Types and Optimizing Future Surveys

Lundqvist

Kundu

Pérez-Torres

et al. 2020

ApJ

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We report deep radio observations of nearby Type Ia supernovae (SNe Ia) with the electronic Multi-Element Radio Linked Interferometer Network and the Australia Telescope Compact Array. No detections were made. With standard assumptions for the energy densities of relativistic electrons going into a power-law energy distribution and the magnetic field strength (ò e =ò B =0.1), we arrive at upper limits on mass-loss rate for the progenitor system of SN2013dy(SN 2016coj, SN 2018gv, SN 2018pv, SN 2019np) of-()  . We compare those limits with the expected mass-loss rates in different single-degenerate progenitor scenarios. We also discuss how information on ò e and ò B can be obtained from late observations of SNeIa and the youngest SNIa remnant detected in radio, G1.9+0.3, as well as strippedenvelope core-collapse SNe. We highlight SN2011dh and argue for ò e ≈0.1 and ò B ≈0.0033. Finally, we discuss strategies to observe at radio frequencies to maximize the chance of detection, given the time since explosion, the distance to the SN, and the telescope sensitivity.

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“…Moreover, the H-band break is observed around 1.5µm in the NIR spectra of SN 2019np, which is related to the dramatic shift in the amount of line blanketing from IGEs (Wheeler et al 1998). Similar to other SNe Ia (Sand et al 2018) (Zheng et al 2013;Pan et al 2015;Zhai et al 2016), 2017cbv (Hosseinzadeh et al 2017) and 2018oh (Li et al 2019).…”

Section: Nir Spectramentioning

confidence: 51%

Observations of the Very Young Type Ia Supernova 2019np with Early-excess Emission

Sai,

Wang,

Elias-Rosa

et al. 2022

Preprint

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UV–OPTICAL OBSERVATION OF TYPE Ia SUPERNOVA SN 2013dy IN NGC 7250

Cited by 21 publications

References 73 publications

Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

The Deepest Radio Observations of Nearby SNe Ia: Constraining Progenitor Types and Optimizing Future Surveys

Observations of the Very Young Type Ia Supernova 2019np with Early-excess Emission

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