Issue |
A&A
Volume 667, November 2022
|
|
---|---|---|
Article Number | A4 | |
Number of page(s) | 21 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/202244393 | |
Published online | 28 October 2022 |
Forbidden hugs in pandemic times
III. Observations of the luminous red nova AT 2021biy in the nearby galaxy NGC 4631⋆
1
Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, PR China
e-mail: yzcai789@163.com, wang_xf@mail.tsinghua.edu.cn
2
INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
3
School of Physics, O’Brien Centre for Science North, University College Dublin, Belfield, Dublin 4, Ireland
4
Beijing Planetarium, Beijing Academy of Science and Technology, Beijing 100044, PR China
5
Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA
6
Departamento de Ciencias Fisicas, Universidad Andres Bello, Fernandez Concha 700, Las Condes, Santiago, Chile
7
Millennium Institute of Astrophysics (MAS), Nuncio Monsenor Sòtero Sanz 100, Providencia, Santiago 8320000, Chile
8
Nagaraj-Noll-Otelline Graduate Fellow, University of California, Berkeley, CA 94720, USA
9
Sternberg Astronomical Institute of the Moscow State University, Moscow 119234, Russia
10
Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz 369167, Russia
11
Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain
12
The Department of Physics, The University of Auckland, Private Bag 92019, Auckland, New Zealand
13
Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, BT7 1NN Northern Ireland, UK
14
Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
15
Department of Astronomy, The Ohio State University, 140 W. 18th Avenue, Columbus, OH 43210, USA
16
Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, 191 W.Woodruff Avenue, Columbus, OH 43210, USA
17
Las Cumbres Observatory, 6740 Cortona Dr. Suite 102, Goleta, CA 93117, USA
18
Department of Physics, University of California, Santa Barbara, CA 93106, USA
19
Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138-1516, USA
20
The NSF AI Institute for Artificial Intelligence and Fundamental Interactions, Cambridge, USA
21
School of Physics and Astronomy, University of Minnesota, 116 Church Street SE, Minneapolis, MN 55455, USA
22
Department of Physics and Astronomy, University of Turku, 20014 Turku, Finland
23
Turku Collegium for Science, Medicine and Technology, University of Turku, 20014 Turku, Finland
24
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, PR China
25
School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 101408, PR China
26
The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, Sweden
27
Faculty of Physics, Moscow State University, 1 bldg. 2, Leninskie Gory, Moscow 119991, Russia
28
Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK
29
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild Str. 1, 85741 Garching, Germany
30
Niels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200 København N, Denmark
31
Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark
32
Università degli Studi di Padova, Dipartimento di Fisica e Astronomia, Vicolo dell’Osservatorio 2, 35122 Padova, Italy
33
Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, PR China
34
Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, PR China
35
Institut d’Estudis Espacials de Catalunya (IEEC), 08034 Barcelona, Spain
36
Hiroshima Astrophysical Science Centre, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan
37
University of Chinese Academy of Sciences, Beijing 100049, PR China
38
Finnish Centre for Astronomy with ESO (FINCA), 20014 University of Turku, Finland
39
Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital 263 001, India
40
School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, PR China
41
Department of Physics, College of Physical Sciences and Technology, Hebei University, Baoding 071002, PR China
42
Key Laboratory of High-precision Computation and Application of Quantum Field Theory of Hebei Province, Hebei University, Baoding 071002, PR China
Received:
1
July
2022
Accepted:
12
August
2022
We present an observational study of the luminous red nova (LRN) AT 2021biy in the nearby galaxy NGC 4631. The field of the object was routinely imaged during the pre-eruptive stage by synoptic surveys, but the transient was detected only at a few epochs from ∼231 days before maximum brightness. The LRN outburst was monitored with unprecedented cadence both photometrically and spectroscopically. AT 2021biy shows a short-duration blue peak, with a bolometric luminosity of ∼1.6 × 1041 erg s−1, followed by the longest plateau among LRNe to date, with a duration of 210 days. A late-time hump in the light curve was also observed, possibly produced by a shell-shell collision. AT 2021biy exhibits the typical spectral evolution of LRNe. Early-time spectra are characterised by a blue continuum and prominent H emission lines. Then, the continuum becomes redder, resembling that of a K-type star with a forest of metal absorption lines during the plateau phase. Finally, late-time spectra show a very red continuum (TBB ≈ 2050 K) with molecular features (e.g., TiO) resembling those of M-type stars. Spectropolarimetric analysis indicates that AT 2021biy has local dust properties similar to those of V838 Mon in the Milky Way Galaxy. Inspection of archival Hubble Space Telescope data taken on 2003 August 3 reveals a ∼20 M⊙ progenitor candidate with log (L/L⊙) = 5.0 dex and Teff = 5900 K at solar metallicity. The above luminosity and colour match those of a luminous yellow supergiant. Most likely, this source is a close binary, with a 17–24 M⊙ primary component.
Key words: binaries: close / stars: winds, outflows / stars: individual: AT 2021biy
Photometric tables are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/667/A4
© Y.-Z. Cai et al. 2022
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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