The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

T. -W. Chen; M. Nicholl; S. J. Smartt; P. A. Mazzali; R. M. Yates; T. J. Moriya; C. Inserra; N. Langer; T. Krühler; Y. -C. Pan; R. Kotak; L. Galbany; P. Schady; P. Wiseman; J. Greiner; S. Schulze; A. W. S. Man; A. Jerkstrand; K. W. Smith; M. Dennefeld; C. Baltay; J. Bolmer; E. Kankare; F. Knust; K. Maguire; D. Rabinowitz; S. Rostami; M. Sullivan; D. R. Young

doi:10.1051/0004-6361/201630163

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

T. -W. Chen, M. Nicholl, S. J. Smartt, P. A. Mazzali, R. M. Yates, T. J. Moriya, C. Inserra, N. Langer, T. Krühler, Y. -C. Pan, R. Kotak, L. Galbany, P. Schady, P. Wiseman, J. Greiner, S. Schulze, A. W. S. Man, A. Jerkstrand, K. W. Smith, M. DennefeldC. Baltay, J. Bolmer, E. Kankare, F. Knust, K. Maguire, D. Rabinowitz, S. Rostami, M. Sullivan, D. R. Young

Physics and Astronomy

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Abstract

We present and analyse an extensive dataset of the superluminous supernova (SLSN) LSQ14mo (z = 0.256), consisting of a multi-colour light curve from -30 d to +70 d in the rest-frame (relative to maximum light) and a series of six spectra from PESSTO covering -7 d to +50 d. This is among the densest spectroscopic coverage, and best-constrained rising light curve, for a fast-declining hydrogen-poor SLSN. The bolometric light curve can be reproduced with a millisecond magnetar model with 4 M_☉ ejecta mass, and the temperature and velocity evolution is also suggestive of a magnetar as the power source. Spectral modelling indicates that the SN ejected 6 M_☉ of CO-rich material with a kinetic energy of 7 × 10⁵¹ erg, and suggests a partially thermalised additional source of luminosity between -2 d and +22 d. This may be due to interaction with a shell of material originating from pre-explosion mass loss. We further present a detailed analysis of the host galaxy system of LSQ14mo. PESSTO and GROND imaging show three spatially resolved bright regions, and we used the VLT and FORS2 to obtain a deep (five-hour exposure) spectra of the SN position and the three star-forming regions, which are at a similar redshift. The FORS2 spectrum at + 300 days shows no trace of SN emission lines and we place limits on the strength of [O I] from comparisons with other Ic supernovae. The deep spectra provides a unique chance to investigate spatial variations in the host star-formation activity and metallicity. The specific star-formation rate is similar in all three components,as is the presence of a young stellar population. However, the position of LSQ14mo exhibits a lower metallicity, with 12 + log (O/H) = 8.2 in both the R₂₃ and N2 scales (corresponding to 0.3 Z_☉ ). We propose that the three bright regions in the host system are interacting, which could induce gas flows triggering star formation in low-metallicity regions.

Based on observations at ESO, Program IDs: 191.D-0935, 094.D-0645, 096.A-9099....

Original language	English
Journal	Astronomy and Astrophysics
DOIs	https://doi.org/10.1051/0004-6361/201630163
Publication status	Published - Jun 2017

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Chen, T. -W., Nicholl, M., Smartt, S. J., Mazzali, P. A., Yates, R. M., Moriya, T. J., Inserra, C., Langer, N., Krühler, T., Pan, Y. -C., Kotak, R., Galbany, L., Schady, P., Wiseman, P., Greiner, J., Schulze, S., Man, A. W. S., Jerkstrand, A., Smith, K. W., ... Young, D. R. (2017). The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system. Astronomy and Astrophysics. https://doi.org/10.1051/0004-6361/201630163

@article{0de48c7212224e91b21e2fd6259766de,

title = "The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system",

abstract = "We present and analyse an extensive dataset of the superluminous supernova (SLSN) LSQ14mo (z = 0.256), consisting of a multi-colour light curve from -30 d to +70 d in the rest-frame (relative to maximum light) and a series of six spectra from PESSTO covering -7 d to +50 d. This is among the densest spectroscopic coverage, and best-constrained rising light curve, for a fast-declining hydrogen-poor SLSN. The bolometric light curve can be reproduced with a millisecond magnetar model with 4 M☉ ejecta mass, and the temperature and velocity evolution is also suggestive of a magnetar as the power source. Spectral modelling indicates that the SN ejected 6 M☉ of CO-rich material with a kinetic energy of 7 × 1051 erg, and suggests a partially thermalised additional source of luminosity between -2 d and +22 d. This may be due to interaction with a shell of material originating from pre-explosion mass loss. We further present a detailed analysis of the host galaxy system of LSQ14mo. PESSTO and GROND imaging show three spatially resolved bright regions, and we used the VLT and FORS2 to obtain a deep (five-hour exposure) spectra of the SN position and the three star-forming regions, which are at a similar redshift. The FORS2 spectrum at + 300 days shows no trace of SN emission lines and we place limits on the strength of [O I] from comparisons with other Ic supernovae. The deep spectra provides a unique chance to investigate spatial variations in the host star-formation activity and metallicity. The specific star-formation rate is similar in all three components,as is the presence of a young stellar population. However, the position of LSQ14mo exhibits a lower metallicity, with 12 + log (O/H) = 8.2 in both the R23 and N2 scales (corresponding to 0.3 Z☉ ). We propose that the three bright regions in the host system are interacting, which could induce gas flows triggering star formation in low-metallicity regions. Based on observations at ESO, Program IDs: 191.D-0935, 094.D-0645, 096.A-9099....",

author = "Chen, {T. -W.} and M. Nicholl and Smartt, {S. J.} and Mazzali, {P. A.} and Yates, {R. M.} and Moriya, {T. J.} and C. Inserra and N. Langer and T. Kr{\"u}hler and Pan, {Y. -C.} and R. Kotak and L. Galbany and P. Schady and P. Wiseman and J. Greiner and S. Schulze and Man, {A. W. S.} and A. Jerkstrand and Smith, {K. W.} and M. Dennefeld and C. Baltay and J. Bolmer and E. Kankare and F. Knust and K. Maguire and D. Rabinowitz and S. Rostami and M. Sullivan and Young, {D. R.}",

year = "2017",

month = jun,

doi = "10.1051/0004-6361/201630163",

language = "English",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Chen, T-W, Nicholl, M, Smartt, SJ, Mazzali, PA, Yates, RM, Moriya, TJ, Inserra, C, Langer, N, Krühler, T, Pan, Y-C, Kotak, R, Galbany, L, Schady, P, Wiseman, P, Greiner, J, Schulze, S, Man, AWS, Jerkstrand, A, Smith, KW, Dennefeld, M, Baltay, C, Bolmer, J, Kankare, E, Knust, F, Maguire, K, Rabinowitz, D, Rostami, S, Sullivan, M & Young, DR 2017, 'The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system', Astronomy and Astrophysics. https://doi.org/10.1051/0004-6361/201630163

TY - JOUR

T1 - The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

AU - Chen, T. -W.

AU - Nicholl, M.

AU - Smartt, S. J.

AU - Mazzali, P. A.

AU - Yates, R. M.

AU - Moriya, T. J.

AU - Inserra, C.

AU - Langer, N.

AU - Krühler, T.

AU - Pan, Y. -C.

AU - Kotak, R.

AU - Galbany, L.

AU - Schady, P.

AU - Wiseman, P.

AU - Greiner, J.

AU - Schulze, S.

AU - Man, A. W. S.

AU - Jerkstrand, A.

AU - Smith, K. W.

AU - Dennefeld, M.

AU - Baltay, C.

AU - Bolmer, J.

AU - Kankare, E.

AU - Knust, F.

AU - Maguire, K.

AU - Rabinowitz, D.

AU - Rostami, S.

AU - Sullivan, M.

AU - Young, D. R.

PY - 2017/6

Y1 - 2017/6

N2 - We present and analyse an extensive dataset of the superluminous supernova (SLSN) LSQ14mo (z = 0.256), consisting of a multi-colour light curve from -30 d to +70 d in the rest-frame (relative to maximum light) and a series of six spectra from PESSTO covering -7 d to +50 d. This is among the densest spectroscopic coverage, and best-constrained rising light curve, for a fast-declining hydrogen-poor SLSN. The bolometric light curve can be reproduced with a millisecond magnetar model with 4 M☉ ejecta mass, and the temperature and velocity evolution is also suggestive of a magnetar as the power source. Spectral modelling indicates that the SN ejected 6 M☉ of CO-rich material with a kinetic energy of 7 × 1051 erg, and suggests a partially thermalised additional source of luminosity between -2 d and +22 d. This may be due to interaction with a shell of material originating from pre-explosion mass loss. We further present a detailed analysis of the host galaxy system of LSQ14mo. PESSTO and GROND imaging show three spatially resolved bright regions, and we used the VLT and FORS2 to obtain a deep (five-hour exposure) spectra of the SN position and the three star-forming regions, which are at a similar redshift. The FORS2 spectrum at + 300 days shows no trace of SN emission lines and we place limits on the strength of [O I] from comparisons with other Ic supernovae. The deep spectra provides a unique chance to investigate spatial variations in the host star-formation activity and metallicity. The specific star-formation rate is similar in all three components,as is the presence of a young stellar population. However, the position of LSQ14mo exhibits a lower metallicity, with 12 + log (O/H) = 8.2 in both the R23 and N2 scales (corresponding to 0.3 Z☉ ). We propose that the three bright regions in the host system are interacting, which could induce gas flows triggering star formation in low-metallicity regions. Based on observations at ESO, Program IDs: 191.D-0935, 094.D-0645, 096.A-9099....

AB - We present and analyse an extensive dataset of the superluminous supernova (SLSN) LSQ14mo (z = 0.256), consisting of a multi-colour light curve from -30 d to +70 d in the rest-frame (relative to maximum light) and a series of six spectra from PESSTO covering -7 d to +50 d. This is among the densest spectroscopic coverage, and best-constrained rising light curve, for a fast-declining hydrogen-poor SLSN. The bolometric light curve can be reproduced with a millisecond magnetar model with 4 M☉ ejecta mass, and the temperature and velocity evolution is also suggestive of a magnetar as the power source. Spectral modelling indicates that the SN ejected 6 M☉ of CO-rich material with a kinetic energy of 7 × 1051 erg, and suggests a partially thermalised additional source of luminosity between -2 d and +22 d. This may be due to interaction with a shell of material originating from pre-explosion mass loss. We further present a detailed analysis of the host galaxy system of LSQ14mo. PESSTO and GROND imaging show three spatially resolved bright regions, and we used the VLT and FORS2 to obtain a deep (five-hour exposure) spectra of the SN position and the three star-forming regions, which are at a similar redshift. The FORS2 spectrum at + 300 days shows no trace of SN emission lines and we place limits on the strength of [O I] from comparisons with other Ic supernovae. The deep spectra provides a unique chance to investigate spatial variations in the host star-formation activity and metallicity. The specific star-formation rate is similar in all three components,as is the presence of a young stellar population. However, the position of LSQ14mo exhibits a lower metallicity, with 12 + log (O/H) = 8.2 in both the R23 and N2 scales (corresponding to 0.3 Z☉ ). We propose that the three bright regions in the host system are interacting, which could induce gas flows triggering star formation in low-metallicity regions. Based on observations at ESO, Program IDs: 191.D-0935, 094.D-0645, 096.A-9099....

U2 - 10.1051/0004-6361/201630163

DO - 10.1051/0004-6361/201630163

M3 - Article

SN - 0004-6361

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

ER -

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

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