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

Konkoly; ePESSTO; University of Arizona; K2 Mission Team; Kegs; Kepler Spacecraft Team; Pan-STARRS; Decam; Asas-Sn; Ptss/tnts; Las Cumbres Observatory; ATLAS

doi:10.3847/2041-8213/aaedb0

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

Konkoly, ePESSTO, University of Arizona, K2 Mission Team, Kegs, Kepler Spacecraft Team, Pan-STARRS, Decam, Asas-Sn, Ptss/tnts, Las Cumbres Observatory, ATLAS

Astronomy

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87 Scopus citations

Abstract

We present an exquisite 30 minute 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 Panoramic Survey Telescope (Pan-STARRS1) and Rapid Response System 1 and Cerro Tololo Inter-American Observatory 4 m Dark Energy Camera (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 supernovae (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 ± 0.04 days after explosion, has a FWHM of 3.12 ± 0.04 days, a blackbody temperature of K, a peak luminosity of , and a total integrated energy of . 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 ∼ 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.

Original language	English (US)
Article number	L1
Journal	Astrophysical Journal Letters
Volume	870
Issue number	1
DOIs	https://doi.org/10.3847/2041-8213/aaedb0
State	Published - Jan 1 2019

Keywords

supernovae: general
supernovae: individual (SN 2018oh)

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.3847/2041-8213/aaedb0

Cite this

@article{65148df729b84e5eba5c3c8eeb739521,

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

abstract = "We present an exquisite 30 minute 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 Panoramic Survey Telescope (Pan-STARRS1) and Rapid Response System 1 and Cerro Tololo Inter-American Observatory 4 m Dark Energy Camera (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 supernovae (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 ± 0.04 days after explosion, has a FWHM of 3.12 ± 0.04 days, a blackbody temperature of K, a peak luminosity of , and a total integrated energy of . 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 ∼ 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 = "supernovae: general, supernovae: individual (SN 2018oh)",

author = "Konkoly and ePESSTO and {University of Arizona} and {K2 Mission Team} and Kegs and {Kepler Spacecraft Team} and Pan-STARRS and Decam and Asas-Sn and Ptss/tnts and {Las Cumbres Observatory} and ATLAS and 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 Pan, {Y. C.} 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 Cleve, {J. E.Van} and {De Miranda Cardoso}, {J. Vin{\'i}cius} 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 Sand, {D. J.} and N. Smith",

year = "2019",

month = jan,

day = "1",

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

language = "English (US)",

volume = "870",

journal = "Astrophysical Journal Letters",

issn = "2041-8205",

publisher = "American Astronomical Society",

number = "1",

}

TY - JOUR

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

AU - Konkoly

AU - ePESSTO

AU - University of Arizona

AU - K2 Mission Team

AU - Kegs

AU - Kepler Spacecraft Team

AU - Pan-STARRS

AU - Decam

AU - Asas-Sn

AU - Ptss/tnts

AU - Las Cumbres Observatory

AU - ATLAS

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 - Cleve, J. E.Van

AU - De Miranda Cardoso, J. Vinícius

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 - Sand, D. J.

AU - Smith, N.

PY - 2019/1/1

Y1 - 2019/1/1

N2 - We present an exquisite 30 minute 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 Panoramic Survey Telescope (Pan-STARRS1) and Rapid Response System 1 and Cerro Tololo Inter-American Observatory 4 m Dark Energy Camera (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 supernovae (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 ± 0.04 days after explosion, has a FWHM of 3.12 ± 0.04 days, a blackbody temperature of K, a peak luminosity of , and a total integrated energy of . 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 ∼ 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 minute 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 Panoramic Survey Telescope (Pan-STARRS1) and Rapid Response System 1 and Cerro Tololo Inter-American Observatory 4 m Dark Energy Camera (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 supernovae (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 ± 0.04 days after explosion, has a FWHM of 3.12 ± 0.04 days, a blackbody temperature of K, a peak luminosity of , and a total integrated energy of . 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 ∼ 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 - supernovae: general

KW - supernovae: individual (SN 2018oh)

UR - http://www.scopus.com/inward/record.url?scp=85059854261&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85059854261&partnerID=8YFLogxK

U2 - 10.3847/2041-8213/aaedb0

DO - 10.3847/2041-8213/aaedb0

M3 - Article

AN - SCOPUS:85059854261

SN - 2041-8205

VL - 870

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 1

M1 - L1

ER -

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

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K2 observations of type Ia supernova SN 2018oh

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

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ASJC Scopus subject areas

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K2 observations of type Ia supernova SN 2018oh

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