Nebular Hα Limits for Fast Declining SNe Ia

D. J. Sand, R. C. Amaro, M. Moe, M. L. Graham, J. E. Andrews, J. Burke, R. Cartier, Y. Eweis, L. Galbany, D. Hiramatsu, D. A. Howell, S. W. Jha, M. Lundquist, T. Matheson, C. McCully, P. Milne, Nathan Smith, S. Valenti, S. Wyatt

Research output: Contribution to journalArticle

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Abstract

One clear observational prediction of the single-degenerate progenitor scenario as the origin of type Ia supernovae (SNe) is the presence of relatively narrow (≈1000 km s-1) Hα emission at nebular phases, although this feature is rarely seen. We present a compilation of nebular phase Hα limits for SN Ia in the literature and demonstrate that this heterogenous sample has been biased toward SN Ia with relatively high luminosities and slow decline rates, as parameterized by Δm 15(B), the difference in B-band magnitude between maximum light and 15 days afterward. Motivated by the need to explore the full parameter space of SN Ia and their subtypes, we present two new and six previously published nebular spectra of SN Ia with Δm 15(B) > 1.3 mag (including members of the transitional and SN1991bg-like subclasses) and measure nondetection limits of L < 0.85-9.9 × 1036 erg s-1, which we confirmed by implanting simulated Hα emission into our data. Based on the latest models of swept-up material stripped from a nondegenerate companion star, these L values correspond to hydrogen mass limits of M H lsim; 1-3 × 10-4 M o, which are roughly three orders of magnitude below that expected for the systems modeled, although we note that no simulations of Hα nebular emission in such weak explosions have yet been performed. Despite the recent detection of strong Hα in ASASSN-18tb (SN 2018fhw; Δm 15(B) = 2.0 mag), we see no evidence that fast-declining systems are more likely to have late time Hα emission, although a larger sample is needed to confirm this result.

Original languageEnglish (US)
Article numberL4
JournalAstrophysical Journal Letters
Volume877
Issue number1
DOIs
StatePublished - May 20 2019

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supernovae
companion stars
erg
explosions
explosion
luminosity
hydrogen
prediction
predictions
simulation

Keywords

  • supernovae: general

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Sand, D. J., Amaro, R. C., Moe, M., Graham, M. L., Andrews, J. E., Burke, J., ... Wyatt, S. (2019). Nebular Hα Limits for Fast Declining SNe Ia. Astrophysical Journal Letters, 877(1), [L4]. https://doi.org/10.3847/2041-8213/ab1eaf

Nebular Hα Limits for Fast Declining SNe Ia. / Sand, D. J.; Amaro, R. C.; Moe, M.; Graham, M. L.; Andrews, J. E.; Burke, J.; Cartier, R.; Eweis, Y.; Galbany, L.; Hiramatsu, D.; Howell, D. A.; Jha, S. W.; Lundquist, M.; Matheson, T.; McCully, C.; Milne, P.; Smith, Nathan; Valenti, S.; Wyatt, S.

In: Astrophysical Journal Letters, Vol. 877, No. 1, L4, 20.05.2019.

Research output: Contribution to journalArticle

Sand, DJ, Amaro, RC, Moe, M, Graham, ML, Andrews, JE, Burke, J, Cartier, R, Eweis, Y, Galbany, L, Hiramatsu, D, Howell, DA, Jha, SW, Lundquist, M, Matheson, T, McCully, C, Milne, P, Smith, N, Valenti, S & Wyatt, S 2019, 'Nebular Hα Limits for Fast Declining SNe Ia', Astrophysical Journal Letters, vol. 877, no. 1, L4. https://doi.org/10.3847/2041-8213/ab1eaf
Sand DJ, Amaro RC, Moe M, Graham ML, Andrews JE, Burke J et al. Nebular Hα Limits for Fast Declining SNe Ia. Astrophysical Journal Letters. 2019 May 20;877(1). L4. https://doi.org/10.3847/2041-8213/ab1eaf
Sand, D. J. ; Amaro, R. C. ; Moe, M. ; Graham, M. L. ; Andrews, J. E. ; Burke, J. ; Cartier, R. ; Eweis, Y. ; Galbany, L. ; Hiramatsu, D. ; Howell, D. A. ; Jha, S. W. ; Lundquist, M. ; Matheson, T. ; McCully, C. ; Milne, P. ; Smith, Nathan ; Valenti, S. ; Wyatt, S. / Nebular Hα Limits for Fast Declining SNe Ia. In: Astrophysical Journal Letters. 2019 ; Vol. 877, No. 1.
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abstract = "One clear observational prediction of the single-degenerate progenitor scenario as the origin of type Ia supernovae (SNe) is the presence of relatively narrow (≈1000 km s-1) Hα emission at nebular phases, although this feature is rarely seen. We present a compilation of nebular phase Hα limits for SN Ia in the literature and demonstrate that this heterogenous sample has been biased toward SN Ia with relatively high luminosities and slow decline rates, as parameterized by Δm 15(B), the difference in B-band magnitude between maximum light and 15 days afterward. Motivated by the need to explore the full parameter space of SN Ia and their subtypes, we present two new and six previously published nebular spectra of SN Ia with Δm 15(B) > 1.3 mag (including members of the transitional and SN1991bg-like subclasses) and measure nondetection limits of L Hα < 0.85-9.9 × 1036 erg s-1, which we confirmed by implanting simulated Hα emission into our data. Based on the latest models of swept-up material stripped from a nondegenerate companion star, these L Hα values correspond to hydrogen mass limits of M H lsim; 1-3 × 10-4 M o, which are roughly three orders of magnitude below that expected for the systems modeled, although we note that no simulations of Hα nebular emission in such weak explosions have yet been performed. Despite the recent detection of strong Hα in ASASSN-18tb (SN 2018fhw; Δm 15(B) = 2.0 mag), we see no evidence that fast-declining systems are more likely to have late time Hα emission, although a larger sample is needed to confirm this result.",
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AU - Burke, J.

AU - Cartier, R.

AU - Eweis, Y.

AU - Galbany, L.

AU - Hiramatsu, D.

AU - Howell, D. A.

AU - Jha, S. W.

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AU - Matheson, T.

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N2 - One clear observational prediction of the single-degenerate progenitor scenario as the origin of type Ia supernovae (SNe) is the presence of relatively narrow (≈1000 km s-1) Hα emission at nebular phases, although this feature is rarely seen. We present a compilation of nebular phase Hα limits for SN Ia in the literature and demonstrate that this heterogenous sample has been biased toward SN Ia with relatively high luminosities and slow decline rates, as parameterized by Δm 15(B), the difference in B-band magnitude between maximum light and 15 days afterward. Motivated by the need to explore the full parameter space of SN Ia and their subtypes, we present two new and six previously published nebular spectra of SN Ia with Δm 15(B) > 1.3 mag (including members of the transitional and SN1991bg-like subclasses) and measure nondetection limits of L Hα < 0.85-9.9 × 1036 erg s-1, which we confirmed by implanting simulated Hα emission into our data. Based on the latest models of swept-up material stripped from a nondegenerate companion star, these L Hα values correspond to hydrogen mass limits of M H lsim; 1-3 × 10-4 M o, which are roughly three orders of magnitude below that expected for the systems modeled, although we note that no simulations of Hα nebular emission in such weak explosions have yet been performed. Despite the recent detection of strong Hα in ASASSN-18tb (SN 2018fhw; Δm 15(B) = 2.0 mag), we see no evidence that fast-declining systems are more likely to have late time Hα emission, although a larger sample is needed to confirm this result.

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