三个发光的红色Novae的全球演化：大流行时期的禁止拥抱-IV

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三个发光的红色Novae的全球演化：大流行时期的禁止拥抱-IV

Panchromatic evolution of three luminous red novae: Forbidden hugs in pandemic times -- IV

论文作者

Pastorello, A., Valerin, G., Fraser, M., Reguitti, A., Elias-Rosa, N., Filippenko, A. V., Rojas-Bravo, C., Tartaglia, L., Reynolds, T. M., Valenti, S., Andrews, J. E., Ashall, C., Bostroem, K. A., Brink, T. G., Burke, J., Cai, Y. -Z., Cappellaro, E., Coulter, D. A., Dastidar, R., Davis, K. W., Dimitriadis, G., Fiore, A., Foley, R. J., Fugazza, D., Galbany, L., Gangopadhyay, A., Geier, S., Gutierrez, C. P., Haislip, J., Hiramatsu, D., Holmbo, S., Howell, D. A., Hsiao, E. Y., Hung, T., Jha, S. W., Kankare, E., Karamehmetoglu, E., Kilpatrick, C. D., Kotak, R., Kouprianov, V., Kravtsov, T., Kumar, S., Li, Z. -T., Lundquist, M. J., Lundqvist, P., Matilainen, K., Mazzali, P. A., McCully, C., Misra, K., Morales-Garoffolo, A., Moran, S., Morrell, N., Newsome, M., Gonzalez, E. Padilla, Pan, Y. -C., Pellegrino, C., Phillips, M. M., Pignata, G., Piro, A. L., Reichart, D. E., Rest, A., Salmaso, I., Sand, D. J., Siebert, M. R., Smartt, S. J., Smith, K. W., Srivastav, S., Stritzinger, M. D., Taggart, K., Tinyanont, S., Yan, S. -Y., Wang, L., Wang, X. -F., Williams, S. C., Wyatt, S., Zhang, T. -M., de Boer, T., Chambers, K., Gao, H., Magnier, E.

论文摘要

我们介绍了三个外层状红色Novae（LRNE）的光度和光谱数据：AT2018BWO，AT2021AFY和AT2021BLU。爆发发作几周后，在NGC45（6.8 MPC）中发现了AT2018BWO。在监测期间，瞬态达到了10^40 ERG/s的峰值光度。由UGC10043（49.2 MPC）托管的AT2021AFY显示出双峰光曲线，两个峰达到相似的光度为2.1（+-0.6）X10^41 ERG/s。对于UGC5829中的AT2021BLU（8.6 MPC），前爆发阶段受到了几个光度测量的监控，并且该物体在爆发前显示出缓慢的发光度。用空前的节奏对AT2021BLU的光曲线进行采样，直到物体消失在太阳后面，然后在后期恢复。 AT2021BLU的光曲线显示出双峰，突出的早期最大值达到6.5x10^40 ERG/s，是AT2021AFY的一半。 AT2021AFY和AT2021BLU的光谱显示了LRNE的预期演化：在第一个峰期间发射中突出的Balmer线所主导的蓝色连续体，并且在第二个具有狭窄的吸收金属线的K型恒星一致的红色连续体中，第二次峰值的蓝色连续体。 AT2018BWO的光谱明显不同，其红色连续体在吸收中以广泛的分子特征为主。由于这些光谱在第二个峰后与LRNE的光谱非常相似，因此在非常晚期的进化阶段发现了AT2018BWO。这将解释其快速演化和与M型恒星兼容的光谱特性。从对爆发前几年的LRN站点的深框架进行分析，以及对光曲线的考虑，这三个LRNE的静态祖细胞系统可能是巨大的，初选范围为AT2018BWO的13MO，从AT2021BLU的AT2018BWO到13-18MO，AT2021BLU以及超过40mo的AT202111afy。

We present photometric and spectroscopic data on three extragalactic luminous red novae (LRNe): AT2018bwo, AT2021afy, and AT2021blu. AT2018bwo was discovered in NGC45 (at 6.8 Mpc) a few weeks after the outburst onset. During the monitoring period, the transient reached a peak luminosity of 10^40 erg/s. AT2021afy, hosted by UGC10043 (49.2 Mpc), showed a double-peaked light curve, with the two peaks reaching a similar luminosity of 2.1(+-0.6)x10^41 erg/s. For AT2021blu in UGC5829, (8.6 Mpc), the pre-outburst phase was well-monitored by several photometric surveys, and the object showed a slow luminosity rise before the outburst. The light curve of AT2021blu was sampled with an unprecedented cadence until the object disappeared behind the Sun, and it was then recovered at late phases. The light curve of AT2021blu shows a double peak, with a prominent early maximum reaching a luminosity of 6.5x10^40 erg/s, which is half of that of AT2021afy. The spectra of AT2021afy and AT2021blu display the expected evolution for LRNe: a blue continuum dominated by prominent Balmer lines in emission during the first peak, and a redder continuum consistent with that of a K-type star with narrow absorption metal lines during the second, broad maximum. The spectra of AT2018bwo are markedly different, with a very red continuum dominated by broad molecular features in absorption. As these spectra closely resemble those of LRNe after the second peak, AT2018bwo was probably discovered at the very late evolutionary stages. This would explain its fast evolution and the spectral properties compatible with that of an M-type star. From the analysis of deep frames of the LRN sites years before the outburst, and considerations of the light curves, the quiescent progenitor systems of the three LRNe were likely massive, with primaries ranging from 13Mo for AT2018bwo, to 13-18Mo for AT2021blu, and over 40Mo for AT2021afy.

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