A1 Alkuperäisartikkeli tieteellisessä aikakauslehdessä
Forbidden hugs in pandemic times: I. Luminous red nova AT 2019zhd, a new merger in M 31
Julkaisun tekijät: Pastorello A, Fraser M, Valerin G, Reguitti A, Itagaki K, Ochner P, Williams SC, Jones D, Munday J, Smartt SJ, Smith KW, Srivastav S, Elias-Rosa N, Kankare E, Karamehmetoglu E, Lundqvist P, Mazzali PA, Munari U, Stritzinger MD, Tomasella L, Anderson JP, Chambers KC, Rest A, Rest A
Kustantaja: EDP SCIENCES S A
Julkaisuvuosi: 2021
Journal: Astronomy and Astrophysics
Tietokannassa oleva lehden nimi: ASTRONOMY & ASTROPHYSICS
Lehden akronyymi: ASTRON ASTROPHYS
Volyymi: 646
Sivujen määrä: 12
ISSN: 0004-6361
eISSN: 1432-0746
DOI: http://dx.doi.org/10.1051/0004-6361/202039952
We present the follow-up campaign of the luminous red nova (LRN) AT 2019zhd, the third event of this class observed in M 31. The object was followed by several sky surveys for about five months before the outburst, during which it showed a slow luminosity rise. In this phase, the absolute magnitude ranged from M-r=-2.8 +/- 0.2 mag to M-r=-5.6 +/- 0.1 mag. Then, over a four to five day period, AT 2019zhd experienced a major brightening, reaching a peak of M-r=-9.61 +/- 0.08 mag and an optical luminosity of 1.4x10(39) erg s(-1). After a fast decline, the light curve settled onto a short-duration plateau in the red bands. Although less pronounced, this feature is reminiscent of the second red maximum observed in other LRNe. This phase was followed by a rapid linear decline in all bands. At maximum, the spectra show a blue continuum with prominent Balmer emission lines. The post-maximum spectra show a much redder continuum, resembling that of an intermediate-type star. In this phase, H alpha becomes very weak, H beta is no longer detectable, and a forest of narrow absorption metal lines now dominate the spectrum. The latest spectra, obtained during the post-plateau decline, show a very red continuum (T-eff approximate to 3000 K) with broad molecular bands of TiO, similar to those of M-type stars. The long-lasting, slow photometric rise observed before the peak resembles that of LRN V1309 Sco, which was interpreted as the signature of the common-envelope ejection. The subsequent outburst is likely due to the gas outflow following a stellar merging event. The inspection of archival HST images taken 22 years before the LRN discovery reveals a faint red source (M-F555W=0.21 +/- 0.14 mag, with F555W-F814W=2.96 +/- 0.12 mag) at the position of AT 2019zhd, which is the most likely quiescent precursor. The source is consistent with expectations for a binary system including a predominant M5-type star.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
