Constraining Type Ia Supernova Delay Time with Spatially Resolved Star Formation Histories

Chen, Xingzhuo; Hu, Lei; Wang, Lifan

doi:10.3847/1538-4357/ac178d

Cited by 10 publications

(11 citation statements)

References 55 publications

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“…To test the two probability density distributions in the horizontal direction, we perform the Wasserstein distance (Earth movers' distance) calculations (see Table 8). This test deduces the minimum work where one distribution is required to change into the other (Chen et al 2021;List 2021). To calculate the distance, we use the scipy.stats.wasserstein_distance 10 Python see a reasonable agreement in both distributions for the other rotations.…”

Section: Discussionmentioning

confidence: 99%

Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms

Arachchige

Cohen

Muñoz-Jaramillo

et al. 2022

ApJ

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The input of the solar wind models plays a significant role in accurate solar wind predictions at 1 au. This work introduces a synthetic magnetogram produced from a dynamo model as an input for magnetohydrodynamics simulations. We perform a quantitative study that compares the space weather modeling framework (SWMF) results for the observed and synthetic solar magnetogram input. For each case, we compare the results for extreme ultraviolet images and extract the simulation data along the Earth trajectory to compare with in situ observations. We initialize the SWMF using the real and synthetic magnetograms for a set of Carrington rotations within solar cycles 23 and 24. Our results help quantify the ability of dynamo models to be used as input to solar wind models and thus provide predictions for the solar wind at 1 au.

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Section: Discussionmentioning

confidence: 99%

Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms

Arachchige

Cohen

Muñoz-Jaramillo

et al. 2022

ApJ

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“…The redshifts of the VHZ SNe Ia are derived following the FLARE project (Wang et al 2017;Regős & Vinkó 2019) where the rates of SN Ia are based on an extrapolation of the local SN Ia rates out to z ∼ 6 based on the star formation rates at higher redshifts as recently derived in Chen et al (2021). Note that the rates given in Chen et al (2021) are in the observer time frame. The survey assumes an area of 0.05 deg 2 with a time span of 6 yr.…”

Section: Type Ia Sn Datamentioning

confidence: 99%

“…From a theoretical point of view, it is also likely that both the single degenerate (SD) and double degenerate (DD) models may be at work in the production of SNe Ia. In addition to the popular SD scenario, recent studies seem to indicate that most of the observed SNe Ia can be accounted for by a delay time distribution (DTD) that can be expected from the DD channel (Castrillo et al 2020;Chen et al 2021;Wiseman et al 2021). Wiseman et al (2021) found that there is a strong correlation between the DTD slope and the SN light-curve decline rate.…”

Section: Cosmological Parameters and Systematic Effectsmentioning

confidence: 99%

“…Riess and Livio (2006) show that at redshift from 1.5-3.0 the systematic evolution of SNe Ia can be the strongest if the delay time of SN Ia explosions from the formation of their progenitors is around 2-3 Gyr. However, a major portion of SNe Ia may explode with a delay time as short as 200 million yr (e.g., Castrillo et al 2020;Chen et al 2021;Wiseman et al 2021). It is thus important to observe SNe at even higher redshifts.…”

Section: Introductionmentioning

confidence: 99%

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Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST

Liu

Wang

Chen

et al. 2022

ApJ

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We investigate the potential of using a sample of very high-redshift (2 ≲ z ≲ 6) (VHZ) Type Ia supernovae (SNe Ia) attainable by JWST on constraining cosmological parameters. At such high redshifts, the age of the universe is young enough that the VHZ SN Ia sample comprises the very first SNe Ia of the universe, with progenitors among the very first generation of low-mass stars that the universe has made. We show that the VHZ SNe Ia can be used to disentangle systematic effects due to the luminosity distance evolution with redshifts intrinsic to SN Ia standardization. Assuming that the systematic evolution can be described by a linear or logarithmic formula, we found that the coefficients of this dependence can be determined accurately and decoupled from cosmological models. Systematic evolution as large as 0.15 mag and 0.45 mag out to z = 5 can be robustly separated from popular cosmological models for linear and logarithmic evolution, respectively. The VHZ SNe Ia will lay the foundation for quantifying the systematic redshift evolution of SN Ia luminosity distance scales. When combined with SN Ia surveys at comparatively lower redshifts, the VHZ SNe Ia allow for the precise measurement of the history of the expansion of the universe from z ∼ 0 to the epoch approaching reionization.

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“…Such a decreasing trend depends on the delay time distribution (DTD) for SN Ia. The DTD is usually expressed as a power-law function f D (t Ia ) ∝ t Ia s (t Ia,min ≈ 0.1 Gyr), where the slope index is negative and has been reported as s = −1 (Totani et al 2008;Maoz et al 2014) or s = −1.4 (Strolger et al 2020;Chen et al 2021). The t Ia -model is constrained by SNe Ia which appeared in low-redshift galaxies below z ∼ 1.5 and is extrapolated to higher redshift in this paper.…”

Section: Standard Chemical Evolution For Host Elliptical Galaxiesmentioning

confidence: 99%

Potential signature of Population III pair-instability supernova ejecta in the BLR gas of the most distant quasar at z = 7.54

Yoshii¹,

Sameshima²,

Tsujimoto³

et al. 2022

Preprint

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The search for Population III (Pop III) stars has fascinated and eluded astrophysicists for decades. One promising place for capturing evidence of their presence must be high-redshift objects; signatures should be recorded in their characteristic chemical abundances. We deduce the Fe and Mg abundances of the broad-line region (BLR) from the intensities of ultraviolet Mg II and Fe II emission lines in the near-infrared spectrum of UKIDSS Large Area Survey (ULAS) J1342+0928 at z = 7.54, by advancing our novel flux-to-abundance conversion method developed for z ∼ 1 quasars. We find that the BLR of this quasar is extremely enriched, by a factor of 20 relative to the solar Fe abundance, together with a very low Mg/Fe abundance ratio: [Fe/H] = +1.36 ± 0.19 and [Mg/Fe] = −1.11 ± 0.12, only 700 million years after the Big Bang. We conclude that such an unusual abundance feature cannot be explained by the standard view of chemical evolution that considers only the contributions from canonical supernovae. While there remains uncertainty in the high-mass end of the Pop III IMF, here we propose that the larger amount of iron in ULAS J1342+0928 was supplied by a pair-instability supernova (PISN) caused by the explosion of a massive Pop III star in the high-mass end of the possible range of 150-300 M . Chemical-evolution models based on initial PISN enrichment well explain the trend in [Fe/Mg]-z all the way from z < 3 to z = 7.54. We predict that stars with very low [Mg/Fe] at all metallicities are hidden in the Galaxy, and they will be efficiently discovered by ongoing new-generation photometric surveys.

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Constraining Type Ia Supernova Delay Time with Spatially Resolved Star Formation Histories

Cited by 10 publications

References 55 publications

Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms

Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms

Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST

Potential signature of Population III pair-instability supernova ejecta in the BLR gas of the most distant quasar at z = 7.54

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