Supernovae and their host galaxies – IV. The distribution of supernovae relative to spiral arms

Aramyan, L. S.; Hakobyan, A. A.; Петросян, А. Р.; Lapparent, V. de; Bertin, E.; Mamon, G. A.; Kunth, D.; Nazaryan, T. A.; Adibekyan, V.; Turatto, M.

doi:10.1093/mnras/stw873

Cited by 33 publications

(39 citation statements)

References 70 publications

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“…In practice, in rotationally-supported galaxies much of this motion is epicyclic within the disk, thus extending the dispersal time. The recent study by Aramyan et al (2016) finds that ∼ 66% of SNe Ia in spirals are associated with spiral arms, where most star-formation takes place. Given that in the local universe roughly 60% of SNe Ia occur in spirals (Li et al 2011), this implies that ∼ 40% of all SNe Ia are associated with spiral arms.…”

Section: Categorizing Sne Ia By Agementioning

confidence: 99%

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Strong dependence of Type Ia supernova standardization on the local specific star formation rate

Rigault

Brinnel

Aldering

et al. 2020

A&A

142

146

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As part of an ongoing effort to identify, understand and correct for astrophysics biases in the standardization of Type Ia supernovae (SN Ia) for cosmology, we have statistically classified a large sample of nearby SNe Ia into those located in predominantly younger or older environments. This classification is based on the specific star formation rate measured within a projected distance of 1 kpc from each SN location, (LsSFR). This is an important refinement compared to using the local star formation rate directly (Rigault et al. 2013; 2015), as it provides a normalization for relative numbers of available SN progenitors and is more robust against extinction by dust. We find that the SNe Ia in predominantly younger environments are ∆ Y = 0.163 ± 0.029 mag (5.7 σ) fainter than those in predominantly older environments after conventional light-curve standardization. This is the strongest standardized SN Ia brightness systematic connected to host-galaxy environment measured to date. The well-established step in standardized brightnesses between SNe Ia in hosts with lower or higher total stellar masses is smaller, at ∆ M = 0.119 ± 0.032 mag (4.5 σ), for the same set of SNe Ia. When fit simultaneously, the environment age offset remains very significant, with ∆ Y = 0.129 ± 0.032 mag (4.0 σ), while the global stellar mass step is reduced to ∆ M = 0.064 ± 0.029 mag (2.2 σ). Thus, approximately 70% of the variance from the stellar mass step is due to an underlying dependence on environment-based progenitor age. Also, we verify that using the local star formation rate alone is not as powerful as LsSFR at sorting SNe Ia into brighter and fainter subsets. Standardization using only the SNe Ia in younger environments reduces the total dispersion from 0.142 ± 0.008 mag to 0.120 ± 0.010 mag. We show that as environment ages evolve with redshift, a strong bias, especially on measurement of the derivative of the dark energy equation of state, can develop. Fortunately, data to measure and correct for this effect using our local specific star formation rate indicator is likely to be available for many next-generation SN Ia cosmology experiments.

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Section: Categorizing Sne Ia By Agementioning

confidence: 99%

“…Such local coherence in stellar properties has long been exploited in estimating relative ages of supernovae (e.g. Moore 1973;van Dyk 1992;Bartunov et al 1994;Aramyan et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Strong dependence of Type Ia supernova standardization on the local specific star formation rate

Rigault

Brinnel

Aldering

et al. 2020

A&A

142

146

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“…The NE2001 model has been used to investigate 3D CR distributions in the ISM by Werner et al (2015), but so far not to calculate IEMs with 3D ISM target density distributions. Studies of other nearby spiral galaxies can also guide the construction of suitable source density distributions for the bulge/bar and arms (e.g., Hakobyan et al 2016;Aramyan et al 2016). In addition the production of an optimised ISRF model is a key ingredient that will require further work: better determination of arm model parameters including distributing dust in them as well as stars, and whether or not stellar/dust arms are co-aligned (e.g., Vallée 2014), the description of the nonaxisymmetric structures across the inner Galaxy (e.g., López-Corredoira et al 2005;Babusiaux & Gilmore 2005;Green et al 2011;Zoccali & Valenti 2016), warps and flaring in the stellar disc (e.g.…”

Section: Interstellar Radiation Fieldmentioning

confidence: 99%

High-energy Gamma Rays from the Milky Way: Three-dimensional Spatial Models for the Cosmic-Ray and Radiation Field Densities in the Interstellar Medium

Porter

Jóhannesson

Moskalenko

2017

ApJ

145

215

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High-energy γ-rays of interstellar origin are produced by the interaction of cosmic-ray (CR) particles with the diffuse gas and radiation fields in the Galaxy. The main features of this emission are well understood and are reproduced by existing CR propagation models employing 2D Galactocentric cylindrically symmetrical geometry. However, the high-quality data from instruments like the Fermi Large Area Telescope reveal significant deviations from the model predictions on few to tens of degree scales indicating the need to include the details of the Galactic spiral structure and thus require 3D spatial modelling. In this paper the high-energy interstellar emissions from the Galaxy are calculated using the new release of the GALPROP code employing 3D spatial models for the CR source and interstellar radiation field (ISRF) densities. Three models for the spatial distribution of CR sources are used that are differentiated by their relative proportion of input luminosity attributed to the smooth disc or spiral arms. Two ISRF models are developed based on stellar and dust spatial density distributions taken from the literature that reproduce local near-to far-infrared observations. The interstellar emission models that include arms and bulges for the CR source and ISRF densities provide plausible physical interpretations for features found in the residual maps from high-energy γ-ray data analysis. The 3D models for CR and ISRF densities provide a more realistic basis that can be used for the interpretation of the non-thermal interstellar emissions from the Galaxy.

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“…Compared to other SN types, SE SNe are most associated with leading edges of spiral arms, where compression triggers star formation (e.g. Aramyan et al, 2016;Karapetyan et al 2018). Galaxy interactions and mergers can also trigger extensive local star formation activity.…”

Section: Absence Of Se Sne In Galaxy Outskirtsmentioning

confidence: 99%

The radial distribution of supernovae compared to star formation tracers

Audcent-Ross

Meurer

Audcent

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Given the limited availability of direct evidence (pre-explosion observations) for supernova (SN) progenitors, the location of supernovae (SNe) within their host galaxies can be used to set limits on one of their most fundamental characteristics, their initial progenitor mass. We present our constraints on SN progenitors derived by comparing the radial distributions of 80 SNe in the SINGG and SUNGG surveys to the R-band, Hα, and UV light distributions of the 55 host galaxies. The strong correlation of Type Ia SNe with R-band light is consistent with models containing only low mass progenitors, reflecting earlier findings. When we limit the analysis of Type II SNe to apertures containing 90 per cent of the total flux, the radial distribution of these SNe best traces far ultraviolet (FUV) emission, consistent with recent direct detections indicating Type II SNe have moderately massive red supergiant progenitors. Stripped Envelope (SE) SNe have the strongest correlation with Hα fluxes, indicative of very massive progenitors (M * 20 M ). This result contradicts a small, but growing, number of direct detections of SE SN progenitors indicating they are moderately massive binary systems. Our result is consistent, however, with a recent population analysis suggesting binary SE SN progenitor masses are regularly underestimated. SE SNe are centralised with respect to Type II SNe and there are no SE SNe recorded beyond half the maximum disc radius in the optical and one third the disc radius in the ultraviolet. The absence of SE SNe beyond these distances is consistent with reduced massive star formation efficiencies in the outskirts of the host galaxies.

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Supernovae and their host galaxies – IV. The distribution of supernovae relative to spiral arms

Cited by 33 publications

References 70 publications

Strong dependence of Type Ia supernova standardization on the local specific star formation rate

Strong dependence of Type Ia supernova standardization on the local specific star formation rate

High-energy Gamma Rays from the Milky Way: Three-dimensional Spatial Models for the Cosmic-Ray and Radiation Field Densities in the Interstellar Medium

The radial distribution of supernovae compared to star formation tracers

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