Search NASA⌕ Search
Home/Archive/DOE OSTI

DOE OSTI · 1894963

SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements

Pierel, J. D. R. (ORCID:0000000223617201)·Jones, D. O. (ORCID:0000000262300151)·Kenworthy, W. D. (ORCID:0000000251535983)·Dai, M. (ORCID:0000000259959692)·Kessler, R. (ORCID:0000000332210419)·Ashall, C. (ORCID:0000000252217557)·Do, A. (ORCID:0000000334297845)·Peterson, E. R. (ORCID:0000000185964746)·Shappee, B. J. (ORCID:0000000346311149)·Siebert, M. R. (ORCID:0000000324453891)·Barna, T. (ORCID:000000024843345X)·Brink, T. G. (ORCID:0000000159552502)·Burke, J. (ORCID:0000000300356659)·Calamida, A. (ORCID:0000000208827702)·Camacho-Neves, Y. (ORCID:0000000298303880)·Jaeger, T. de (ORCID:0000000160691139)·Filippenko, A. V. (ORCID:0000000334600103)·Foley, R. J. (ORCID:0000000224455275)·Galbany, L. (ORCID:0000000212966887)·Fox, O. D. (ORCID:0000000322381572)·Gomez, S. (ORCID:0000000163956702)·Hiramatsu, D. (ORCID:0000000211259187)·Hounsell, R. (ORCID:0000000204764206)·Howell, D. A. (ORCID:000000034253656X)·Jha, S. W. (ORCID:0000000187386011)·Kwok, L. A. (ORCID:0000000331081328)·Pérez-Fournon, I. (ORCID:0000000228076459)·Poidevin, F. (ORCID:0000000253915568)·Rest, A. (ORCID:0000000244105387)·Rubin, D. (ORCID:0000000154024647)·Scolnic, D. M. (ORCID:0000000249345849)·Shirley, R. (ORCID:0000000211140135)·Strolger, L. G. (ORCID:0000000277564440)·Tinyanont, S. (ORCID:0000000214814676)·Wang, Q. (ORCID:0000000152336989)
View original source ↗Export metadata ↓

Abstract

Abstract A large fraction of Type Ia supernova (SN Ia) observations over the next decade will be in the near-infrared (NIR), at wavelengths beyond the reach of the current standard light-curve model for SN Ia cosmology, SALT3 (∼2800–8700 Å central filter wavelength). To harness this new SN Ia sample and reduce future light-curve standardization systematic uncertainties, we train SALT3 at NIR wavelengths (SALT3-NIR) up to 2 μ m with the open-source model-training software SALTshaker , which can easily accommodate future observations. Using simulated data, we show that the training process constrains the NIR model to ∼2%–3% across the phase range (−20 to 50 days). We find that Hubble residual (HR) scatter is smaller using the NIR alone or optical+NIR compared to optical alone, by up to ∼30% depending on filter choice (95% confidence). There is significant correlation between NIR light-curve stretch measurements and luminosity, with stretch and color corrections often improving HR scatter by up to ∼20%. For SN Ia observations expected from the Roman Space Telescope, SALT3-NIR increases the amount of usable data in the SALT framework by ∼20% at redshift z ≲ 0.4 and by ∼50% at z ≲ 0.15. The SALT3-NIR model is part of the open-source SNCosmo and SNANA SN Ia cosmology packages.

Explore related subjects

79 ASTRONOMY AND ASTROPHYSICSAstronomical modelsAstronomy & AstrophysicsCosmologyNear infrared astronomyType Ia supernovae

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Pierel, J. D. R. (ORCID:0000000223617201), Jones, D. O. (ORCID:0000000262300151), Kenworthy, W. D. (ORCID:0000000251535983), Dai, M. (ORCID:0000000259959692), Kessler, R. (ORCID:0000000332210419), Ashall, C. (ORCID:0000000252217557), Do, A. (ORCID:0000000334297845), Peterson, E. R. (ORCID:0000000185964746), Shappee, B. J. (ORCID:0000000346311149), Siebert, M. R. (ORCID:0000000324453891), Barna, T. (ORCID:000000024843345X), Brink, T. G. (ORCID:0000000159552502), Burke, J. (ORCID:0000000300356659), Calamida, A. (ORCID:0000000208827702), Camacho-Neves, Y. (ORCID:0000000298303880), Jaeger, T. de (ORCID:0000000160691139), Filippenko, A. V. (ORCID:0000000334600103), Foley, R. J. (ORCID:0000000224455275), Galbany, L. (ORCID:0000000212966887), Fox, O. D. (ORCID:0000000322381572), Gomez, S. (ORCID:0000000163956702), Hiramatsu, D. (ORCID:0000000211259187), Hounsell, R. (ORCID:0000000204764206), Howell, D. A. (ORCID:000000034253656X), Jha, S. W. (ORCID:0000000187386011), Kwok, L. A. (ORCID:0000000331081328), Pérez-Fournon, I. (ORCID:0000000228076459), Poidevin, F. (ORCID:0000000253915568), Rest, A. (ORCID:0000000244105387), Rubin, D. (ORCID:0000000154024647), Scolnic, D. M. (ORCID:0000000249345849), Shirley, R. (ORCID:0000000211140135), Strolger, L. G. (ORCID:0000000277564440), Tinyanont, S. (ORCID:0000000214814676), Wang, Q. (ORCID:0000000152336989). 2022-10-27. SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements. https://doi.org/10.3847/1538-4357%2Fac93f9

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related reports

DOE OSTI2026

Dust Survival in Galactic Winds

This repository contains three-dimensional volumetric data from an Eulerian hydrodynamical simulation (conducted on a uniform Cartesian grid) generated by the Cholla hydrodynamics code. The datasets contain snapshots (full-grid, projections, and slices) in the HDF5 format of a multi-phase medium in which a hot, diffuse, dust-free background wind accelerates a cool, dense cloud of gas and dust. This scenario is intended to represent a supernova-driven galactic outflow, in which hot supernova winds are thought to accelerate cool interstellar medium material out of the galactic disk into the surrounding circumgalactic medium. There are three separate datasets for simulations corresponding to three cloud evolutionary scenarios: long-term cloud survival (surv), marginal cloud survival (disr), and cloud destruction (dest). Projection and slice images of the simulations are also included in this repository.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2026

Unraveling TeV halos with the Cherenkov Telescope Array

Pulsars are observed to emit bright and spatially extended gamma-ray emission at multi-TeV energies. These so-called "TeV halos" are now understood to be a nearly universal feature of middle-aged pulsars. However, many of the key physical processes that govern these systems, particularly those affecting particle diffusion, remain poorly constrained. We aim to evaluate the ability of the Cherenkov Telescope Array (CTA) to probe the physical properties of TeV halos, with a focus on the nearby and well-studied case of the Geminga pulsar. We simulate gamma-ray emission from various TeV halo models, incorporating different assumptions for the injected electron spectrum, spin-down evolution, and energy-dependent diffusion. These models are then used to forecast CTA's sensitivity to spectral and spatial differences, based on realistic mock observations and instrument response simulations. We find that CTA will be able to distinguish between a wide range of TeV halo models that are currently consistent with existing data. In particular, CTA observations can constrain the normalization, energy dependence, and spatial extent of the diffusion coefficient surrounding Geminga, as well as the spectral shape of the injected electron population.

79 ASTRONOMY AND ASTROPHYSICS↗