Reconciling volumetric and individual galaxy type Ia supernova rates

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Reconciling volumetric and individual galaxy type Ia supernova rates. / Andersen, P.; Hjorth, J.

In: Monthly Notices of the Royal Astronomical Society, Vol. 480, No. 1, 2018, p. 68-74.

Research output: Contribution to journalJournal articleResearchpeer-review

Harvard

Andersen, P & Hjorth, J 2018, 'Reconciling volumetric and individual galaxy type Ia supernova rates', Monthly Notices of the Royal Astronomical Society, vol. 480, no. 1, pp. 68-74. https://doi.org/10.1093/mnras/sty1837

APA

Andersen, P., & Hjorth, J. (2018). Reconciling volumetric and individual galaxy type Ia supernova rates. Monthly Notices of the Royal Astronomical Society, 480(1), 68-74. https://doi.org/10.1093/mnras/sty1837

Vancouver

Andersen P, Hjorth J. Reconciling volumetric and individual galaxy type Ia supernova rates. Monthly Notices of the Royal Astronomical Society. 2018;480(1):68-74. https://doi.org/10.1093/mnras/sty1837

Author

Andersen, P. ; Hjorth, J. / Reconciling volumetric and individual galaxy type Ia supernova rates. In: Monthly Notices of the Royal Astronomical Society. 2018 ; Vol. 480, No. 1. pp. 68-74.

Bibtex

@article{f4bd7f24b0624a3d9cab99625e309e18,
title = "Reconciling volumetric and individual galaxy type Ia supernova rates",
abstract = "Significant observational effort has been devoted to determining volumetric type Ia supernova rates at high redshifts, leading to clues about the nature of Ia supernova progenitors and constraints on the iron production in the universe. A complementary approach is to investigate type Ia supernova rates in individual, more nearby, galaxies. The popular A + B model for the specific supernova rate, while reliable for a wide range of galaxy properties, diverges for large specific star formation rates. Applying it outside its range of validity could lead to the prediction of excessive type Ia supernova rates. Moreover, the A + B model it is not directly derived from a delay time distribution. We here introduce a new model which is explicitly motivated by a simple delay time distribution composed of a prompt and a delayed component. The model is in remarkably good agreement with current observational constraints. It yields a prompt fraction of f p = 0.11 -0.06 +0.10 in agreement with results based on volumetric rates of type Ia supernovae at high redshift. The model is tested against realistic star formation rates from the Illustris-1 simulation and is found to be self-consistent in the asymptotic limits. An analytic function that encapsulates the features of the new model is shown to be in excellent agreement with the data. In terms of goodness of fit, the new model is strongly preferred over the A + Bmodel. At log (sSFR) ≳-9 there are no constraints from observations. Observations in this regime will further constrain the delay time distribution of type Ia supernovae at short delay times.",
keywords = "Cosmology: observations, Cosmology: theory, Dark energy, Large-scale structure of Universe",
author = "P. Andersen and J. Hjorth",
year = "2018",
doi = "10.1093/mnras/sty1837",
language = "English",
volume = "480",
pages = "68--74",
journal = "Royal Astronomical Society. Monthly Notices",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",

}

RIS

TY - JOUR

T1 - Reconciling volumetric and individual galaxy type Ia supernova rates

AU - Andersen, P.

AU - Hjorth, J.

PY - 2018

Y1 - 2018

N2 - Significant observational effort has been devoted to determining volumetric type Ia supernova rates at high redshifts, leading to clues about the nature of Ia supernova progenitors and constraints on the iron production in the universe. A complementary approach is to investigate type Ia supernova rates in individual, more nearby, galaxies. The popular A + B model for the specific supernova rate, while reliable for a wide range of galaxy properties, diverges for large specific star formation rates. Applying it outside its range of validity could lead to the prediction of excessive type Ia supernova rates. Moreover, the A + B model it is not directly derived from a delay time distribution. We here introduce a new model which is explicitly motivated by a simple delay time distribution composed of a prompt and a delayed component. The model is in remarkably good agreement with current observational constraints. It yields a prompt fraction of f p = 0.11 -0.06 +0.10 in agreement with results based on volumetric rates of type Ia supernovae at high redshift. The model is tested against realistic star formation rates from the Illustris-1 simulation and is found to be self-consistent in the asymptotic limits. An analytic function that encapsulates the features of the new model is shown to be in excellent agreement with the data. In terms of goodness of fit, the new model is strongly preferred over the A + Bmodel. At log (sSFR) ≳-9 there are no constraints from observations. Observations in this regime will further constrain the delay time distribution of type Ia supernovae at short delay times.

AB - Significant observational effort has been devoted to determining volumetric type Ia supernova rates at high redshifts, leading to clues about the nature of Ia supernova progenitors and constraints on the iron production in the universe. A complementary approach is to investigate type Ia supernova rates in individual, more nearby, galaxies. The popular A + B model for the specific supernova rate, while reliable for a wide range of galaxy properties, diverges for large specific star formation rates. Applying it outside its range of validity could lead to the prediction of excessive type Ia supernova rates. Moreover, the A + B model it is not directly derived from a delay time distribution. We here introduce a new model which is explicitly motivated by a simple delay time distribution composed of a prompt and a delayed component. The model is in remarkably good agreement with current observational constraints. It yields a prompt fraction of f p = 0.11 -0.06 +0.10 in agreement with results based on volumetric rates of type Ia supernovae at high redshift. The model is tested against realistic star formation rates from the Illustris-1 simulation and is found to be self-consistent in the asymptotic limits. An analytic function that encapsulates the features of the new model is shown to be in excellent agreement with the data. In terms of goodness of fit, the new model is strongly preferred over the A + Bmodel. At log (sSFR) ≳-9 there are no constraints from observations. Observations in this regime will further constrain the delay time distribution of type Ia supernovae at short delay times.

KW - Cosmology: observations

KW - Cosmology: theory

KW - Dark energy

KW - Large-scale structure of Universe

U2 - 10.1093/mnras/sty1837

DO - 10.1093/mnras/sty1837

M3 - Journal article

AN - SCOPUS:85052552769

VL - 480

SP - 68

EP - 74

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 0035-8711

IS - 1

ER -

ID: 221671325