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5 results on '"Dyrbye, S."'

1. How low can you go? SN 2018zd as a low-mass Fe core-collapse supernova

Author

Callis, E., Fraser, M., Pastorello, A., Dong, Subo, Brennan, S. J., Chen, P., Bose, S., Reynolds, T., Salmon, L., Jonker, P., Benetti, S., Berton, M., Cannizzaro, G., Cappellaro, E., Congiu, E., Dyrbye, S., Eappachen, D., Elias-Rosa, N., Gromadzki, M., Gutiérrez, C. P., Holmbo, S., Holoien, T. W. S., Itagaki, K., Kankare, E., Mattila, S., Mutel, R., Ochner, P., Post, R. S., Prieto, J., Reguitti, A., Roth, T., Ryon, J., Sagués-Carracedo, A., Shappee, B. J., Siviero, A., Stassun, K. G., Stritzinger, M., Tomasella, L., Villanueva Jr., S., Wevers, T., and Wiggins, P.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present spectroscopy and photometry of SN 2018zd, a Type IIP core-collapse supernova with signatures of interaction with circumstantial material in its earliest spectra. High ionization lines, the earmark of shock breakout, are not seen in the earliest spectral epoch, and are only seen in a single spectrum at 4.9 d after explosion. The strength and brevity of these features imply a confined circumstellar material shell in the immediate vicinity of the progenitor. Once the narrow emission lines disappear, SN 2018zd evolves similarly to a Type IIP SN, although the blue colour and enhanced plateau magnitude of SN 2018zd suggests an additional source of luminosity throughout the plateau phase. While SN 2018zd has previously been proposed as an electron-capture SN, we suggest that it is an Fe core-collapse from a low mass red supergiant progenitor. Differences in interpretation for SN 2018zd arise in part due to the large uncertainty on the distance to the host-galaxy NGC 2146, which we re-derive here to be $15.6^{+6.1}_{-3.0}$ Mpc. We find the ejected $^{56}$Ni mass for SN 2018zd to be 0.017 M$_{\odot}$, significantly higher than models of ECSNe predict. We also find the Ni/Fe ratio in SN 2018zd to be much lower that would be expected for an ECSN.

Published
2021

2. The Evolution of Luminous Red Nova AT 2017jfs in NGC 4470

Author

Pastorello, A., Chen, T. -W., Cai, Y. -Z., Morales-Garoffolo, A., Cano, Z., Mason, E., Barsukova, E. A., Benetti, S., Berton, M., Bose, S., Bufano, F., Callis, E., Cannizzaro, G., Cartier, R., Chen, Ping, Dong, Subo, Dyrbye, S., Elias-Rosa, N., Floers, A., Fraser, M., Geier, S., Goranskij, V. P., Kann, D. A., Kuncarayakti, H., Onori, F., Reguitti, A., Reynolds, T., Losada, I. R., Carracedo, A. Sagues, Schweyer, T., Smartt, S. J., Tatarnikov, A. M., Valeev, A. F., Vogl, C., Wevers, T., Postigo, A. de Ugarte, Izzo, L., Inserra, C., Kankare, E., Maguire, K., Smith, K. W., Stalder, B., Tartaglia, L., Thoene, C. C., Valerin, G., and Young, D. R.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present the results of our photometric and spectroscopic follow-up of the intermediate-luminosity optical transient AT 2017jfs. At peak, the object reaches an absolute magnitude of Mg=-15.46+-0.15 mag and a bolometric luminosity of 5.5x10^41 erg/s. Its light curve has the double-peak shape typical of Luminous Red Novae (LRNe), with a narrow first peak bright in the blue bands, while the second peak is longer lasting and more luminous in the red and near-infrared (NIR) bands. During the first peak, the spectrum shows a blue continuum with narrow emission lines of H and Fe II. During the second peak, the spectrum becomes cooler, resembling that of a K-type star, and the emission lines are replaced by a forest of narrow lines in absorption. About 5 months later, while the optical light curves are characterized by a fast linear decline, the NIR ones show a moderate rebrightening, observed until the transient disappeared in solar conjunction. At these late epochs, the spectrum becomes reminiscent of that of M-type stars, with prominent molecular absorption bands. The late-time properties suggest the formation of some dust in the expanding common envelope or an IR echo from foreground pre-existing dust. We propose that the object is a common-envelope transient, possibly the outcome of a merging event in a massive binary, similar to NGC4490-2011OT1., Comment: 7 pages, 4 figures, 2 Tables (incl. one on-line). Published in A&A Letters

Published
2019
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3. The evolution of luminous red nova AT 2017jfs in NGC 4470 [Letter to the editor]

Author

Pastorello, A., Chen, T.-W., Cai, Y.-Z., Morales-Garoffolo, A., Cano, Z., Mason, E., Barsukova, E. A., Benetti, S., Berton, M., Bose, S., Bufano, F., Callis, E., Cannizzaro, G., Cartier, R., Chen, Ping, Dong, Subo, Dyrbye, S., Elias-Rosa, N., Flörs, A., Fraser, M., Geier, S., Goranskij, V. P., Kann, D. A., Kuncarayakti, H., Onori, F., Reguitti, A., Reynolds, T., Losada, I. R., Sagués Carracedo, A., Schweyer, T., Smartt, S. J., Tatarnikov, A. M., Valeev, A. F., Vogl, C., Wevers, T., de Ugarte Postigo, A., Izzo, L., Inserra, C., Kankare, E., Maguire, K., Smith, K. W., Stalder, B., Tartaglia, L., Thöne, C. C., Valerin, G., and Young, D. R.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present the results of our photometric and spectroscopic follow-up of the intermediate-luminosity optical transient AT 2017jfs. At peak, the object reaches an absolute magnitude of Mg = −15.46 ± 0.15 mag and a bolometric luminosity of 5.5 × 1041 erg s−1. Its light curve has the double-peak shape typical of luminous red novae (LRNe), with a narrow first peak bright in the blue bands, while the second peak is longer-lasting and more luminous in the red and near-infrared (NIR) bands. During the first peak, the spectrum shows a blue continuum with narrow emission lines of H and Fe II. During the second peak, the spectrum becomes cooler, resembling that of a K-type star, and the emission lines are replaced by a forest of narrow lines in absorption. About 5 months later, while the optical light curves are characterized by a fast linear decline, the NIR ones show a moderate rebrightening, observed until the transient disappears in solar conjunction. At these late epochs, the spectrum becomes reminiscent of that of M-type stars, with prominent molecular absorption bands. The late-time properties suggest the formation of some dust in the expanding common envelope or an IR echo from foreground pre-existing dust. We propose that the object is a common-envelope transient, possibly the outcome of a merging event in a massive binary, similar to NGC 4490−2011OT1.

Published
2019

4. The evolution of luminous red nova AT 2017jfs in NGC 4470

Author

China Scholarship Council, Science Foundation Ireland, Ministerio de Ciencia e Innovación (España), European Commission, National Science Foundation (US), Istituto Nazionale di Astrofisica, Science and Technology Facilities Council (UK), European Research Council, European Southern Observatory, Lomonosov Moscow State University, Pastorello, Andrea, Chen, T. W., Cai, Yongzhi, Morales-Garoffolo, A., Cano, Z., Mason, E., Barsukova, E. A., Benetti, S., Berton, M., Bose, S., Bufano, F., Callis, E., Cannizzaro, G., Cartier, R., Chen, P., Dong, S. B., Dyrbye, S., Elias-Rosa, Nancy, Flors, A., Fraser, Morgan, Geier, Stefan, Goranskij, V. P., Kann, D. A., Kuncarayakti, Hanindyo, Onori, F., Reguitti, Andrea, Reynolds, Thomas M., Losada, I. R., Carracedo, A. S., Schweyer, T., Smartt, S. J., Tatarnikov, A. M., Valeev, A. F., Vogl, Christian, Wevers, T., Ugarte Postigo, Antonio de, Izzo, L., Inserra, Cosimo, Kankare, E, Maguire, Kate, Smith, Ken W., Stalder, B., Tartaglia, Leonardo, Thöne, Cristina Carina, Valerin, Giorgio, Young, D. R., China Scholarship Council, Science Foundation Ireland, Ministerio de Ciencia e Innovación (España), European Commission, National Science Foundation (US), Istituto Nazionale di Astrofisica, Science and Technology Facilities Council (UK), European Research Council, European Southern Observatory, Lomonosov Moscow State University, Pastorello, Andrea, Chen, T. W., Cai, Yongzhi, Morales-Garoffolo, A., Cano, Z., Mason, E., Barsukova, E. A., Benetti, S., Berton, M., Bose, S., Bufano, F., Callis, E., Cannizzaro, G., Cartier, R., Chen, P., Dong, S. B., Dyrbye, S., Elias-Rosa, Nancy, Flors, A., Fraser, Morgan, Geier, Stefan, Goranskij, V. P., Kann, D. A., Kuncarayakti, Hanindyo, Onori, F., Reguitti, Andrea, Reynolds, Thomas M., Losada, I. R., Carracedo, A. S., Schweyer, T., Smartt, S. J., Tatarnikov, A. M., Valeev, A. F., Vogl, Christian, Wevers, T., Ugarte Postigo, Antonio de, Izzo, L., Inserra, Cosimo, Kankare, E, Maguire, Kate, Smith, Ken W., Stalder, B., Tartaglia, Leonardo, Thöne, Cristina Carina, Valerin, Giorgio, and Young, D. R.

Abstract

We present the results of our photometric and spectroscopic follow-up of the intermediate-luminosity optical transient AT 2017jfs. At peak, the object reaches an absolute magnitude of Mg = -15:46 ± 0:15 mag and a bolometric luminosity of 5:5 × 1041 erg s-1. Its light curve has the doublepeak shape typical of luminous red novae (LRNe), with a narrow first peak bright in the blue bands, while the second peak is longer-lasting and more luminous in the red and near-infrared (NIR) bands. During the first peak, the spectrum shows a blue continuum with narrow emission lines of H and Fe II. During the second peak, the spectrum becomes cooler, resembling that of a K-type star, and the emission lines are replaced by a forest of narrow lines in absorption. About 5 months later, while the optical light curves are characterized by a fast linear decline, the NIR ones show a moderate rebrightening, observed until the transient disappears in solar conjunction. At these late epochs, the spectrum becomes reminiscent of that of M-type stars, with prominent molecular absorption bands. The late-time properties suggest the formation of some dust in the expanding common envelope or an IR echo from foreground pre-existing dust. We propose that the object is a common-envelope transient, possibly the outcome of a merging event in a massive binary, similar to NGC4490-2011OT1. © ESO 2019.

Published
2019

5. The evolution of luminous red nova at 2017jfs in NGC4470?

Author

Pastorello A., Chen T., Cai Y., Morales-Garoffolo A., Cano Z., Mason E., Barsukova E., Benetti S., Berton M., Bose S., Bufano F., Callis E., Cannizzaro G., Cartier R., Chen P., Dong S., Dyrbye S., Elias-Rosa N., Flörs A., Fraser M., Geier S., Goranskij V., Kann D., Kuncarayakti H., Onori F., Reguitti A., Reynolds T., Losada I., Sagués Carracedo A., Schweyer T., Smartt S., Tatarnikov A., Valeev A., Vogl C., Wevers T., De Ugarte Postigo A., Izzo L., Inserra C., Kankare E., Maguire K., Smith K., Stalder B., Tartaglia L., Thöne C., Valerin G., Young D., Pastorello A., Chen T., Cai Y., Morales-Garoffolo A., Cano Z., Mason E., Barsukova E., Benetti S., Berton M., Bose S., Bufano F., Callis E., Cannizzaro G., Cartier R., Chen P., Dong S., Dyrbye S., Elias-Rosa N., Flörs A., Fraser M., Geier S., Goranskij V., Kann D., Kuncarayakti H., Onori F., Reguitti A., Reynolds T., Losada I., Sagués Carracedo A., Schweyer T., Smartt S., Tatarnikov A., Valeev A., Vogl C., Wevers T., De Ugarte Postigo A., Izzo L., Inserra C., Kankare E., Maguire K., Smith K., Stalder B., Tartaglia L., Thöne C., Valerin G., and Young D.

Abstract

© ESO 2019. We present the results of our photometric and spectroscopic follow-up of the intermediate-luminosity optical transient AT 2017jfs. At peak, the object reaches an absolute magnitude of Mg = -15:46 ± 0:15 mag and a bolometric luminosity of 5:5 × 1041 erg s-1. Its light curve has the doublepeak shape typical of luminous red novae (LRNe), with a narrow first peak bright in the blue bands, while the second peak is longer-lasting and more luminous in the red and near-infrared (NIR) bands. During the first peak, the spectrum shows a blue continuum with narrow emission lines of H and Fe II. During the second peak, the spectrum becomes cooler, resembling that of a K-type star, and the emission lines are replaced by a forest of narrow lines in absorption. About 5 months later, while the optical light curves are characterized by a fast linear decline, the NIR ones show a moderate rebrightening, observed until the transient disappears in solar conjunction. At these late epochs, the spectrum becomes reminiscent of that of M-type stars, with prominent molecular absorption bands. The late-time properties suggest the formation of some dust in the expanding common envelope or an IR echo from foreground pre-existing dust. We propose that the object is a common-envelope transient, possibly the outcome of a merging event in a massive binary, similar to NGC4490-2011OT1.

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