Table 1 The atmospheric parameters for each spectroscopic dataset

From: A super-Chandrasekhar mass type Ia supernova progenitor at 49 pc set to detonate in 23 Gyr

Telescope/instrument

VLT/UVES

WHT/ISIS

HST/COS

Adopted

Teff,1 (K)

17,230 ± 710

\(16,50{0}_{-300}^{+400}\)

18,630 ± 80

\(17,26{0}_{-880}^{+1,380}\)

log g1 (dex)

8.408 ± 0.027

8.35 ± 0.05

8.307 ± 0.020

\(8.35{0}_{-0.052}^{+0.066}\)

M1 (M)

0.871 ± 0.018

0.83 ± 0.03

0.810 ± 0.013

0.834 ± 0.039

Teff,2 (K)

20,190 ± 280

20,200 ± 300

18,010 ± 70

\(2,000{0}_{-2,000}^{+400}\)

log g2 (dex)

8.151 ± 0.021

8.16 ± 0.04

8.178 ± 0.018

\(8.16{4}_{-0.030}^{+0.027}\)

M2 (M)

0.713 ± 0.014

0.72 ± 0.03

0.727 ± 0.013

0.721 ± 0.020

MT (M)

1.584 ± 0.022

1.55 ± 0.04

1.537 ± 0.018

1.555 ± 0.044

  1. Hybrid fitting was performed in all cases using Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) photometry. A systematic difference between the ultraviolet spectroscopy and the optical photometry was considered in the fitting (Methods). Masses are inferred by interpolation of evolutionary sequences61 and MT is the total mass of the system. The final adopted values were obtained by concatenating the distributions obtained for each parameter to quote the median and 68% confidence interval on the Teff and log g, and then interpolating to find masses. The more/less massive star is labelled with subscript 1/2, respectively. The WHT/ISIS solution is quoted from a previous result26.