K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova

Physics

Electronic data

Dimitriadis_1811.10061
Rights statement: © Copyright 2019 IOP Publishing
Accepted author manuscript, 3.96 MB, PDF document
Available under license: CC BY-NC: Creative Commons Attribution-NonCommercial 4.0 International License

Text available via DOI:

https://doi.org/10.3847/2041-8213/aaedb0
Final published version

Keywords

Astrophysics - High Energy Astrophysical Phenomena

View graph of relations

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Published

Standard

K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova. / Dimitriadis, G.; Foley, R. J.; Rest, A. et al.
In: Astrophysical Journal Letters, Vol. 870, L1, 01.01.2019.

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Harvard

Dimitriadis, G, Foley, RJ, Rest, A, Kasen, D, Piro, AL, Polin, A, Jones, DO, Villar, A, Narayan, G, Coulter, DA, Kilpatrick, CD, Pan, Y-C, Rojas-Bravo, C, Fox, OD, Jha, SW, Nugent, PE, Riess, AG, Scolnic, D, Drout, MR, Barentsen, G, Dotson, J, Gully-Santiago, M, Hedges, C, Cody, AM, Barclay, T, Howell, S, Garnavich, P, Tucker, BE, Shaya, E, Mushotzky, R, Olling, RP, Margheim, S, Zenteno, A, Coughlin, J, Van Cleve, JE, Cardoso, JVDM, Larson, KA, McCalmont-Everton, KM, Peterson, CA, Ross, SE, Reedy, LH, Osborne, D, McGinn, C, Kohnert, L, Migliorini, L, Wheaton, A, Spencer, B, Labonde, C, Castillo, G, Beerman, G, Steward, K, Hanley, M, Larsen, R, Gangopadhyay, R, Kloetzel, R, Weschler, T, Nystrom, V, Moffatt, J, Redick, M, Griest, K, Packard, M, Muszynski, M, Kampmeier, J, Bjella, R, Flynn, S, Elsaesser, B, Chambers, KC, Flewelling, HA, Huber, ME, Magnier, EA, Waters, CZ, Schultz, ASB, Bulger, J, Lowe, TB, Willman, M, Smartt, SJ, Smith, KW, Points, S, Strampelli, GM, Brimacombe, J, Chen, P, Munoz, JA, Mutel, RL, Shields, J, Vallely, PJ, Villanueva, SJ, Li, W, Wang, X, Zhang, J, Lin, H, Mo, J, Zhao, X, Sai, H, Zhang, X, Zhang, K, Zhang, T, Wang, L, Zhang, J, Baron, E, DerKacy, JM, Li, L, Chen, Z, Xiang, D, Rui, L, Wang, L, Huang, F, Li, X, Hosseinzadeh, G, Howell, DA, Arcavi, I, Hiramatsu, D, Burke, J, Valenti, S, Tonry, JL, Denneau, L, Heinze, AN, Weiland, H, Stalder, B, Vinko, J, Sarneczky, K, Pa, A, Bodi, A, Bognar, Z, Csak, B, Cseh, B, Csornyei, G, Hanyecz, O, Ignacz, B, Kalup, C, Konyves-Toth, R, Kriskovics, L, Ordasi, A, Rajmon, I, Sodor, A, Szabo, R, Szakats, R, Zsidi, G, Williams, SC, Nordin, J, Cartier, R, Frohmaier, C, Galbany, L, Gutierrez, CP, Hook, I, Inserra, C, Smith, M, Sand, DJ, Andrews, JE, Smith, N & Bilinski, C 2019, 'K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova', Astrophysical Journal Letters, vol. 870, L1. https://doi.org/10.3847/2041-8213/aaedb0

APA

Dimitriadis, G., Foley, R. J., Rest, A., Kasen, D., Piro, A. L., Polin, A., Jones, D. O., Villar, A., Narayan, G., Coulter, D. A., Kilpatrick, C. D., Pan, Y-C., Rojas-Bravo, C., Fox, O. D., Jha, S. W., Nugent, P. E., Riess, A. G., Scolnic, D., Drout, M. R., ... Bilinski, C. (2019). K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova. Astrophysical Journal Letters, 870, Article L1. https://doi.org/10.3847/2041-8213/aaedb0

Vancouver

Dimitriadis G, Foley RJ, Rest A, Kasen D, Piro AL, Polin A et al. K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova. Astrophysical Journal Letters. 2019 Jan 1;870:L1. Epub 2018 Dec 28. doi: 10.3847/2041-8213/aaedb0

Author

Dimitriadis, G. ; Foley, R. J. ; Rest, A. et al. / K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova. In: Astrophysical Journal Letters. 2019 ; Vol. 870.

Bibtex

@article{7ee66f220b2e4548887f6c9adc3c4e8e,

title = "K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova",

abstract = "We present an exquisite, 30-min cadence Kepler (K2) light curve of the Type Ia supernova (SN Ia) 2018oh (ASASSN-18bt), starting weeks before explosion, covering the moment of explosion and the subsequent rise, and continuing past peak brightness. These data are supplemented by multi-color Pan-STARRS1 and CTIO 4-m DECam observations obtained within hours of explosion. The K2 light curve has an unusual two-component shape, where the flux rises with a steep linear gradient for the first few days, followed by a quadratic rise as seen for typical SNe Ia. This {"}flux excess{"} relative to canonical SN Ia behavior is confirmed in our $i$-band light curve, and furthermore, SN 2018oh is especially blue during the early epochs. The flux excess peaks 2.14$\pm0.04$ days after explosion, has a FWHM of 3.12$\pm0.04$ days, a blackbody temperature of $T=17,500^{+11,500}_{-9,000}$ K, a peak luminosity of $4.3\pm0.2\times10^{37}\,{\rm erg\,s^{-1}}$, and a total integrated energy of $1.27\pm0.01\times10^{43}\,{\rm erg}$. We compare SN 2018oh to several models that may provide additional heating at early times, including collision with a companion and a shallow concentration of radioactive nickel. While all of these models generally reproduce the early K2 light curve shape, we slightly favor a companion interaction, at a distance of $\sim$$2\times10^{12}\,{\rm cm}$ based on our early color measurements, although the exact distance depends on the uncertain viewing angle. Additional confirmation of a companion interaction in future modeling and observations of SN 2018oh would provide strong support for a single-degenerate progenitor system.",

keywords = "Astrophysics - High Energy Astrophysical Phenomena",

author = "G. Dimitriadis and Foley, {R. J.} and A. Rest and D. Kasen and Piro, {A. L.} and A. Polin and Jones, {D. O.} and A. Villar and G. Narayan and Coulter, {D. A.} and Kilpatrick, {C. D.} and Y.-C. Pan and C. Rojas-Bravo and Fox, {O. D.} and Jha, {S. W.} and Nugent, {P. E.} and Riess, {A. G.} and D. Scolnic and Drout, {M. R.} and G. Barentsen and J. Dotson and M. Gully-Santiago and C. Hedges and Cody, {A. M.} and T. Barclay and S. Howell and P. Garnavich and Tucker, {B. E.} and E. Shaya and R. Mushotzky and Olling, {R. P.} and S. Margheim and A. Zenteno and J. Coughlin and {Van Cleve}, {J. E.} and Cardoso, {J. Vinicius de Miranda} and Larson, {K. A.} and McCalmont-Everton, {K. M.} and Peterson, {C. A.} and Ross, {S. E.} and Reedy, {L. H.} and D. Osborne and C. McGinn and L. Kohnert and L. Migliorini and A. Wheaton and B. Spencer and C. Labonde and G. Castillo and G. Beerman and K. Steward and M. Hanley and R. Larsen and R. Gangopadhyay and R. Kloetzel and T. Weschler and V. Nystrom and J. Moffatt and M. Redick and K. Griest and M. Packard and M. Muszynski and J. Kampmeier and R. Bjella and S. Flynn and B. Elsaesser and Chambers, {K. C.} and Flewelling, {H. A.} and Huber, {M. E.} and Magnier, {E. A.} and Waters, {C. Z.} and Schultz, {A. S. B.} and J. Bulger and Lowe, {T. B.} and M. Willman and Smartt, {S. J.} and Smith, {K. W.} and S. Points and Strampelli, {G. M.} and J. Brimacombe and P. Chen and Munoz, {J. A.} and Mutel, {R. L.} and J. Shields and Vallely, {P. J.} and Villanueva, {S., Jr} and W. Li and X. Wang and J. Zhang and H. Lin and J. Mo and X. Zhao and H. Sai and X. Zhang and K. Zhang and T. Zhang and L. Wang and J. Zhang and E. Baron and DerKacy, {J. M.} and L. Li and Z. Chen and D. Xiang and L. Rui and L. Wang and F. Huang and X. Li and G. Hosseinzadeh and Howell, {D. A.} and I. Arcavi and D. Hiramatsu and J. Burke and S. Valenti and Tonry, {J. L.} and L. Denneau and Heinze, {A. N.} and H. Weiland and B. Stalder and J. Vinko and K. Sarneczky and A. Pa and A. Bodi and Zs. Bognar and B. Csak and B. Cseh and G. Csornyei and O. Hanyecz and B. Ignacz and Cs. Kalup and R. Konyves-Toth and L. Kriskovics and A. Ordasi and I. Rajmon and A. Sodor and R. Szabo and R. Szakats and G. Zsidi and Williams, {S. C.} and J. Nordin and R. Cartier and C. Frohmaier and L. Galbany and Gutierrez, {C. P.} and I. Hook and C. Inserra and M. Smith and Sand, {D. J.} and Andrews, {J. E.} and N. Smith and C. Bilinski",

year = "2019",

month = jan,

day = "1",

doi = "10.3847/2041-8213/aaedb0",

language = "English",

volume = "870",

journal = "Astrophysical Journal Letters",

issn = "2041-8205",

publisher = "IOP Publishing Ltd",

}

RIS

TY - JOUR

T1 - K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova

AU - Dimitriadis, G.

AU - Foley, R. J.

AU - Rest, A.

AU - Kasen, D.

AU - Piro, A. L.

AU - Polin, A.

AU - Jones, D. O.

AU - Villar, A.

AU - Narayan, G.

AU - Coulter, D. A.

AU - Kilpatrick, C. D.

AU - Pan, Y.-C.

AU - Rojas-Bravo, C.

AU - Fox, O. D.

AU - Jha, S. W.

AU - Nugent, P. E.

AU - Riess, A. G.

AU - Scolnic, D.

AU - Drout, M. R.

AU - Barentsen, G.

AU - Dotson, J.

AU - Gully-Santiago, M.

AU - Hedges, C.

AU - Cody, A. M.

AU - Barclay, T.

AU - Howell, S.

AU - Garnavich, P.

AU - Tucker, B. E.

AU - Shaya, E.

AU - Mushotzky, R.

AU - Olling, R. P.

AU - Margheim, S.

AU - Zenteno, A.

AU - Coughlin, J.

AU - Van Cleve, J. E.

AU - Cardoso, J. Vinicius de Miranda

AU - Larson, K. A.

AU - McCalmont-Everton, K. M.

AU - Peterson, C. A.

AU - Ross, S. E.

AU - Reedy, L. H.

AU - Osborne, D.

AU - McGinn, C.

AU - Kohnert, L.

AU - Migliorini, L.

AU - Wheaton, A.

AU - Spencer, B.

AU - Labonde, C.

AU - Castillo, G.

AU - Beerman, G.

AU - Steward, K.

AU - Hanley, M.

AU - Larsen, R.

AU - Gangopadhyay, R.

AU - Kloetzel, R.

AU - Weschler, T.

AU - Nystrom, V.

AU - Moffatt, J.

AU - Redick, M.

AU - Griest, K.

AU - Packard, M.

AU - Muszynski, M.

AU - Kampmeier, J.

AU - Bjella, R.

AU - Flynn, S.

AU - Elsaesser, B.

AU - Chambers, K. C.

AU - Flewelling, H. A.

AU - Huber, M. E.

AU - Magnier, E. A.

AU - Waters, C. Z.

AU - Schultz, A. S. B.

AU - Bulger, J.

AU - Lowe, T. B.

AU - Willman, M.

AU - Smartt, S. J.

AU - Smith, K. W.

AU - Points, S.

AU - Strampelli, G. M.

AU - Brimacombe, J.

AU - Chen, P.

AU - Munoz, J. A.

AU - Mutel, R. L.

AU - Shields, J.

AU - Vallely, P. J.

AU - Villanueva, S., Jr

AU - Li, W.

AU - Wang, X.

AU - Zhang, J.

AU - Lin, H.

AU - Mo, J.

AU - Zhao, X.

AU - Sai, H.

AU - Zhang, X.

AU - Zhang, K.

AU - Zhang, T.

AU - Wang, L.

AU - Zhang, J.

AU - Baron, E.

AU - DerKacy, J. M.

AU - Li, L.

AU - Chen, Z.

AU - Xiang, D.

AU - Rui, L.

AU - Wang, L.

AU - Huang, F.

AU - Li, X.

AU - Hosseinzadeh, G.

AU - Howell, D. A.

AU - Arcavi, I.

AU - Hiramatsu, D.

AU - Burke, J.

AU - Valenti, S.

AU - Tonry, J. L.

AU - Denneau, L.

AU - Heinze, A. N.

AU - Weiland, H.

AU - Stalder, B.

AU - Vinko, J.

AU - Sarneczky, K.

AU - Pa, A.

AU - Bodi, A.

AU - Bognar, Zs.

AU - Csak, B.

AU - Cseh, B.

AU - Csornyei, G.

AU - Hanyecz, O.

AU - Ignacz, B.

AU - Kalup, Cs.

AU - Konyves-Toth, R.

AU - Kriskovics, L.

AU - Ordasi, A.

AU - Rajmon, I.

AU - Sodor, A.

AU - Szabo, R.

AU - Szakats, R.

AU - Zsidi, G.

AU - Williams, S. C.

AU - Nordin, J.

AU - Cartier, R.

AU - Frohmaier, C.

AU - Galbany, L.

AU - Gutierrez, C. P.

AU - Hook, I.

AU - Inserra, C.

AU - Smith, M.

AU - Sand, D. J.

AU - Andrews, J. E.

AU - Smith, N.

AU - Bilinski, C.

PY - 2019/1/1

Y1 - 2019/1/1

N2 - We present an exquisite, 30-min cadence Kepler (K2) light curve of the Type Ia supernova (SN Ia) 2018oh (ASASSN-18bt), starting weeks before explosion, covering the moment of explosion and the subsequent rise, and continuing past peak brightness. These data are supplemented by multi-color Pan-STARRS1 and CTIO 4-m DECam observations obtained within hours of explosion. The K2 light curve has an unusual two-component shape, where the flux rises with a steep linear gradient for the first few days, followed by a quadratic rise as seen for typical SNe Ia. This "flux excess" relative to canonical SN Ia behavior is confirmed in our $i$-band light curve, and furthermore, SN 2018oh is especially blue during the early epochs. The flux excess peaks 2.14$\pm0.04$ days after explosion, has a FWHM of 3.12$\pm0.04$ days, a blackbody temperature of $T=17,500^{+11,500}_{-9,000}$ K, a peak luminosity of $4.3\pm0.2\times10^{37}\,{\rm erg\,s^{-1}}$, and a total integrated energy of $1.27\pm0.01\times10^{43}\,{\rm erg}$. We compare SN 2018oh to several models that may provide additional heating at early times, including collision with a companion and a shallow concentration of radioactive nickel. While all of these models generally reproduce the early K2 light curve shape, we slightly favor a companion interaction, at a distance of $\sim$$2\times10^{12}\,{\rm cm}$ based on our early color measurements, although the exact distance depends on the uncertain viewing angle. Additional confirmation of a companion interaction in future modeling and observations of SN 2018oh would provide strong support for a single-degenerate progenitor system.

AB - We present an exquisite, 30-min cadence Kepler (K2) light curve of the Type Ia supernova (SN Ia) 2018oh (ASASSN-18bt), starting weeks before explosion, covering the moment of explosion and the subsequent rise, and continuing past peak brightness. These data are supplemented by multi-color Pan-STARRS1 and CTIO 4-m DECam observations obtained within hours of explosion. The K2 light curve has an unusual two-component shape, where the flux rises with a steep linear gradient for the first few days, followed by a quadratic rise as seen for typical SNe Ia. This "flux excess" relative to canonical SN Ia behavior is confirmed in our $i$-band light curve, and furthermore, SN 2018oh is especially blue during the early epochs. The flux excess peaks 2.14$\pm0.04$ days after explosion, has a FWHM of 3.12$\pm0.04$ days, a blackbody temperature of $T=17,500^{+11,500}_{-9,000}$ K, a peak luminosity of $4.3\pm0.2\times10^{37}\,{\rm erg\,s^{-1}}$, and a total integrated energy of $1.27\pm0.01\times10^{43}\,{\rm erg}$. We compare SN 2018oh to several models that may provide additional heating at early times, including collision with a companion and a shallow concentration of radioactive nickel. While all of these models generally reproduce the early K2 light curve shape, we slightly favor a companion interaction, at a distance of $\sim$$2\times10^{12}\,{\rm cm}$ based on our early color measurements, although the exact distance depends on the uncertain viewing angle. Additional confirmation of a companion interaction in future modeling and observations of SN 2018oh would provide strong support for a single-degenerate progenitor system.

KW - Astrophysics - High Energy Astrophysical Phenomena

U2 - 10.3847/2041-8213/aaedb0

DO - 10.3847/2041-8213/aaedb0

M3 - Journal article

VL - 870

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

SN - 2041-8205

M1 - L1

ER -

Research

Electronic data

Links

Text available via DOI:

Keywords