Understanding the extreme luminosity of DES14X2fna

DES Collaboration; M. Grayling; C. P. Gutiérrez; M. Sullivan; P. Wiseman; M. Vincenzi; S. González-Gaitán; B. E. Tucker; L. Galbany; L. Kelsey; C. Lidman; E. Swann; M. Smith; C. Frohmaier; D. Carollo; K. Glazebrook; G. F. Lewis; A. Möller; S. R. Hinton; S. A. Uddin; T. M. C. Abbott; M. Aguena; S. Avila; E. Bertin; S. Bhargava; D. Brooks; A. Carnero Rosell; M. Carrasco Kind; J. Carretero; M. Costanzi; L. N. da Costa; J. De Vicente; S. Desai; H. T. Diehl; P. Doel; S. Everett; Bruno Ferrero; P. Fosalba; J. Frieman; J. García-Bellido; E. Gaztanaga; D. Gruen; R. A. Gruendl; J. Gschwend; G. Gutierrez; B. Hoyle; K. Kuehn; N. Kuropatkin; M. Lima; N. MacCrann; J. L. Marshall; P. Martini; R. Miquel; R. Morgan; A. Palmese; F. Paz-Chinchón; A. A. Plazas; A. K. Romer; C. Sánchez; E. Sanchez; V. Scarpine; S. Serrano; I. Sevilla-Noarbe; M. Soares-Santos; E. Suchyta; G. Tarle; D. Thomas; C. To; T. N. Varga; A. R. Walker; R. D. Wilkinson

doi:10.1093/mnras/stab1478

Understanding the extreme luminosity of DES14X2fna

DES Collaboration, M. Grayling^*, C. P. Gutiérrez, M. Sullivan, P. Wiseman, M. Vincenzi, S. González-Gaitán, B. E. Tucker, L. Galbany, L. Kelsey, C. Lidman, E. Swann, M. Smith, C. Frohmaier, D. Carollo, K. Glazebrook, G. F. Lewis, A. Möller, S. R. Hinton, S. A. UddinT. M. C. Abbott, M. Aguena, S. Avila, E. Bertin, S. Bhargava, D. Brooks, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, J. De Vicente, S. Desai, H. T. Diehl, P. Doel, S. Everett, Bruno Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, B. Hoyle, K. Kuehn, N. Kuropatkin, M. Lima, N. MacCrann, J. L. Marshall, P. Martini, R. Miquel, R. Morgan, A. Palmese, F. Paz-Chinchón, A. A. Plazas, A. K. Romer, C. Sánchez, E. Sanchez, V. Scarpine, S. Serrano, I. Sevilla-Noarbe, M. Soares-Santos, E. Suchyta, G. Tarle, D. Thomas, C. To, T. N. Varga, A. R. Walker, R. D. Wilkinson

^*Corresponding author for this work

Australian Astronomical Optics

Research output: Contribution to journal › Article › peer-review

4 Citations (Scopus)

800 Downloads (Pure)

Abstract

We present DES14X2fna, a high-luminosity, fast-declining Type IIb supernova (SN IIb) at redshift z = 0.0453, detected by the Dark Energy Survey (DES). DES14X2fna is an unusual member of its class, with a light curve showing a broad, luminous peak reaching M_r ≃ -19.3 mag 20 d after explosion. This object does not show a linear decline tail in the light curve until ≃60 d after explosion, after which it declines very rapidly (4.30 ± 0.10 mag 100 d^-1 in the r band). By fitting semi-analytic models to the photometry of DES14X2fna, we find that its light curve cannot be explained by a standard ⁵⁶Ni decay model as this is unable to fit the peak and fast tail decline observed. Inclusion of either interaction with surrounding circumstellar material or a rapidly-rotating neutron star (magnetar) significantly increases the quality of the model fit. We also investigate the possibility for an object similar to DES14X2fna to act as a contaminant in photometric samples of SNe Ia for cosmology, finding that a similar simulated object is misclassified by a recurrent neural network (RNN)-based photometric classifier as an SN Ia in ∼1.1-2.4 percent of cases in DES, depending on the probability threshold used for a positive classification.

Original language	English
Pages (from-to)	3950-3967
Number of pages	18
Journal	Monthly Notices of the Royal Astronomical Society
Volume	505
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stab1478
Publication status	Published - Aug 2021

Bibliographical note

© 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

Keywords

supernovae: general
supernovae: individual: DES14X2fna

Access to Document

10.1093/mnras/stab1478Licence: CC BY

Publisher version (open access)Final published version, 5.66 MBLicence: CC BY

Cite this

DES Collaboration, Grayling, M., Gutiérrez, C. P., Sullivan, M., Wiseman, P., Vincenzi, M., González-Gaitán, S., Tucker, B. E., Galbany, L., Kelsey, L., Lidman, C., Swann, E., Smith, M., Frohmaier, C., Carollo, D., Glazebrook, K., Lewis, G. F., Möller, A., Hinton, S. R., ... Wilkinson, R. D. (2021). Understanding the extreme luminosity of DES14X2fna. Monthly Notices of the Royal Astronomical Society, 505(3), 3950-3967. https://doi.org/10.1093/mnras/stab1478

@article{d79131ade2ce432bb88a1dba392599f0,

title = "Understanding the extreme luminosity of DES14X2fna",

abstract = "We present DES14X2fna, a high-luminosity, fast-declining Type IIb supernova (SN IIb) at redshift z = 0.0453, detected by the Dark Energy Survey (DES). DES14X2fna is an unusual member of its class, with a light curve showing a broad, luminous peak reaching Mr ≃ -19.3 mag 20 d after explosion. This object does not show a linear decline tail in the light curve until ≃60 d after explosion, after which it declines very rapidly (4.30 ± 0.10 mag 100 d-1 in the r band). By fitting semi-analytic models to the photometry of DES14X2fna, we find that its light curve cannot be explained by a standard 56Ni decay model as this is unable to fit the peak and fast tail decline observed. Inclusion of either interaction with surrounding circumstellar material or a rapidly-rotating neutron star (magnetar) significantly increases the quality of the model fit. We also investigate the possibility for an object similar to DES14X2fna to act as a contaminant in photometric samples of SNe Ia for cosmology, finding that a similar simulated object is misclassified by a recurrent neural network (RNN)-based photometric classifier as an SN Ia in ∼1.1-2.4 percent of cases in DES, depending on the probability threshold used for a positive classification.",

keywords = "supernovae: general, supernovae: individual: DES14X2fna",

author = "{DES Collaboration} and M. Grayling and Guti{\'e}rrez, {C. P.} and M. Sullivan and P. Wiseman and M. Vincenzi and S. Gonz{\'a}lez-Gait{\'a}n and Tucker, {B. E.} and L. Galbany and L. Kelsey and C. Lidman and E. Swann and M. Smith and C. Frohmaier and D. Carollo and K. Glazebrook and Lewis, {G. F.} and A. M{\"o}ller and Hinton, {S. R.} and Uddin, {S. A.} and Abbott, {T. M. C.} and M. Aguena and S. Avila and E. Bertin and S. Bhargava and D. Brooks and Rosell, {A. Carnero} and Kind, {M. Carrasco} and J. Carretero and M. Costanzi and {da Costa}, {L. N.} and {De Vicente}, J. and S. Desai and Diehl, {H. T.} and P. Doel and S. Everett and Bruno Ferrero and P. Fosalba and J. Frieman and J. Garc{\'i}a-Bellido and E. Gaztanaga and D. Gruen and Gruendl, {R. A.} and J. Gschwend and G. Gutierrez and B. Hoyle and K. Kuehn and N. Kuropatkin and M. Lima and N. MacCrann and Marshall, {J. L.} and P. Martini and R. Miquel and R. Morgan and A. Palmese and F. Paz-Chinch{\'o}n and Plazas, {A. A.} and Romer, {A. K.} and C. S{\'a}nchez and E. Sanchez and V. Scarpine and S. Serrano and I. Sevilla-Noarbe and M. Soares-Santos and E. Suchyta and G. Tarle and D. Thomas and C. To and Varga, {T. N.} and Walker, {A. R.} and Wilkinson, {R. D.}",

note = "{\textcopyright} 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.",

year = "2021",

month = aug,

doi = "10.1093/mnras/stab1478",

language = "English",

volume = "505",

pages = "3950--3967",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

DES Collaboration, Grayling, M, Gutiérrez, CP, Sullivan, M, Wiseman, P, Vincenzi, M, González-Gaitán, S, Tucker, BE, Galbany, L, Kelsey, L, Lidman, C, Swann, E, Smith, M, Frohmaier, C, Carollo, D, Glazebrook, K, Lewis, GF, Möller, A, Hinton, SR, Uddin, SA, Abbott, TMC, Aguena, M, Avila, S, Bertin, E, Bhargava, S, Brooks, D, Rosell, AC, Kind, MC, Carretero, J, Costanzi, M, da Costa, LN, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Everett, S, Ferrero, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hoyle, B, Kuehn, K, Kuropatkin, N, Lima, M, MacCrann, N, Marshall, JL, Martini, P, Miquel, R, Morgan, R, Palmese, A, Paz-Chinchón, F, Plazas, AA, Romer, AK, Sánchez, C, Sanchez, E, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Suchyta, E, Tarle, G, Thomas, D, To, C, Varga, TN, Walker, AR & Wilkinson, RD 2021, 'Understanding the extreme luminosity of DES14X2fna', Monthly Notices of the Royal Astronomical Society, vol. 505, no. 3, pp. 3950-3967. https://doi.org/10.1093/mnras/stab1478

TY - JOUR

T1 - Understanding the extreme luminosity of DES14X2fna

AU - DES Collaboration

AU - Grayling, M.

AU - Gutiérrez, C. P.

AU - Sullivan, M.

AU - Wiseman, P.

AU - Vincenzi, M.

AU - González-Gaitán, S.

AU - Tucker, B. E.

AU - Galbany, L.

AU - Kelsey, L.

AU - Lidman, C.

AU - Swann, E.

AU - Smith, M.

AU - Frohmaier, C.

AU - Carollo, D.

AU - Glazebrook, K.

AU - Lewis, G. F.

AU - Möller, A.

AU - Hinton, S. R.

AU - Uddin, S. A.

AU - Abbott, T. M. C.

AU - Aguena, M.

AU - Avila, S.

AU - Bertin, E.

AU - Bhargava, S.

AU - Brooks, D.

AU - Rosell, A. Carnero

AU - Kind, M. Carrasco

AU - Carretero, J.

AU - Costanzi, M.

AU - da Costa, L. N.

AU - De Vicente, J.

AU - Desai, S.

AU - Diehl, H. T.

AU - Doel, P.

AU - Everett, S.

AU - Ferrero, Bruno

AU - Fosalba, P.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Hoyle, B.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Lima, M.

AU - MacCrann, N.

AU - Marshall, J. L.

AU - Martini, P.

AU - Miquel, R.

AU - Morgan, R.

AU - Palmese, A.

AU - Paz-Chinchón, F.

AU - Plazas, A. A.

AU - Romer, A. K.

AU - Sánchez, C.

AU - Sanchez, E.

AU - Scarpine, V.

AU - Serrano, S.

AU - Sevilla-Noarbe, I.

AU - Soares-Santos, M.

AU - Suchyta, E.

AU - Tarle, G.

AU - Thomas, D.

AU - To, C.

AU - Varga, T. N.

AU - Walker, A. R.

AU - Wilkinson, R. D.

N1 - © 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

PY - 2021/8

Y1 - 2021/8

N2 - We present DES14X2fna, a high-luminosity, fast-declining Type IIb supernova (SN IIb) at redshift z = 0.0453, detected by the Dark Energy Survey (DES). DES14X2fna is an unusual member of its class, with a light curve showing a broad, luminous peak reaching Mr ≃ -19.3 mag 20 d after explosion. This object does not show a linear decline tail in the light curve until ≃60 d after explosion, after which it declines very rapidly (4.30 ± 0.10 mag 100 d-1 in the r band). By fitting semi-analytic models to the photometry of DES14X2fna, we find that its light curve cannot be explained by a standard 56Ni decay model as this is unable to fit the peak and fast tail decline observed. Inclusion of either interaction with surrounding circumstellar material or a rapidly-rotating neutron star (magnetar) significantly increases the quality of the model fit. We also investigate the possibility for an object similar to DES14X2fna to act as a contaminant in photometric samples of SNe Ia for cosmology, finding that a similar simulated object is misclassified by a recurrent neural network (RNN)-based photometric classifier as an SN Ia in ∼1.1-2.4 percent of cases in DES, depending on the probability threshold used for a positive classification.

AB - We present DES14X2fna, a high-luminosity, fast-declining Type IIb supernova (SN IIb) at redshift z = 0.0453, detected by the Dark Energy Survey (DES). DES14X2fna is an unusual member of its class, with a light curve showing a broad, luminous peak reaching Mr ≃ -19.3 mag 20 d after explosion. This object does not show a linear decline tail in the light curve until ≃60 d after explosion, after which it declines very rapidly (4.30 ± 0.10 mag 100 d-1 in the r band). By fitting semi-analytic models to the photometry of DES14X2fna, we find that its light curve cannot be explained by a standard 56Ni decay model as this is unable to fit the peak and fast tail decline observed. Inclusion of either interaction with surrounding circumstellar material or a rapidly-rotating neutron star (magnetar) significantly increases the quality of the model fit. We also investigate the possibility for an object similar to DES14X2fna to act as a contaminant in photometric samples of SNe Ia for cosmology, finding that a similar simulated object is misclassified by a recurrent neural network (RNN)-based photometric classifier as an SN Ia in ∼1.1-2.4 percent of cases in DES, depending on the probability threshold used for a positive classification.

KW - supernovae: general

KW - supernovae: individual: DES14X2fna

UR - http://www.scopus.com/inward/record.url?scp=85124065723&partnerID=8YFLogxK

U2 - 10.1093/mnras/stab1478

DO - 10.1093/mnras/stab1478

M3 - Article

SN - 0035-8711

VL - 505

SP - 3950

EP - 3967

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Understanding the extreme luminosity of DES14X2fna

Abstract

Bibliographical note

Keywords

Access to Document

Other files and links

Fingerprint

Cite this