COSMOGLOBE: Simulating zodiacal emission with ZodiPy

San, M.; Herman, D.; Erikstad, G. B.; Galloway, M.; Watts, Duncan J.

doi:10.1051/0004-6361/202244133

Cited by 5 publications

(2 citation statements)

References 23 publications

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“…The predicted zodiacal light is then obtained by evaluating a sequence of line-of-sight integrals from the position of the observer and through a model of the three-dimensional interplanetary dust distribution. For implementation details and examples of how to apply ZodiPy to a real-world dataset, see San et al (2022).…”

Section: Statement Of Needmentioning

confidence: 99%

ZodiPy: A Python package for zodiacal light simulations

San

2024

JOSS

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ZodiPy is an Astropy-affiliated Python package for zodiacal light simulations. Its purpose is to provide the astrophysics and cosmology communities with an accessible and easy-to-use Python interface to existing zodiacal light models, assisting in the analysis of infrared astrophysical data and enabling quick and easy zodiacal light forecasting for future experiments. ZodiPy implements the Kelsall et al. (1998) and the Planck Collaboration et al. (2014) interplanetary dust models, which allow for zodiacal light simulations between 1.25−240𝜇m and 30−857GHz, respectively, with the possibility of extrapolating the models to other frequencies.

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Section: Statement Of Needmentioning

confidence: 99%

ZodiPy: A Python package for zodiacal light simulations

San

2024

JOSS

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“…However, ZL at both 1.25 µm and optical wavelength (ONC-T wide-band) is the scattered sunlight component, and the spectral shape is the same irrespective of ecliptic latitude (Tsumura et al 2010). Therefore, the model ZL brightness at 1.25 µm observed from the Hayabusa2 position was calculated using the ZodiPy code (San et al 2022), and then ZL brightness at the optical wavelength (ONC-T wide-band) was estimated by extrapolating from 1.25 µm using the Solar spectrum (Gueymard et al 2002) as shown in Figure 16 (red). The Gegenschein appears in the antisolar direction, and the Kelsall model does not include the Gegenschein.…”

Section: Absolute Zl Brightnessmentioning

confidence: 99%

Initial Result of Heliocentric Distance Dependence of Zodiacal Light Observed by Hayabusa2#

Tsumura

Matsuura

Sano

et al. 2023

Preprint

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The zodiacal light (ZL) is sunlight scattered by interplanetary dust (IPD) in the optical wavelengths. The spatial distribution of IPD in the Solar system may hold an important key to understanding the evolution of the Solar system and material transportation within it. The IPD number density can be expressed as [[EQUATION]] , and the result of [[EQUATION]] was obtained by the previous observations from the interplanetary space by Helios 1/2 and Pioneer 10/11 in the 1970s and 1980s. However, no direct measurements of [[EQUATION]] based on the ZL observation from the interplanetary space outside the Earth's orbit have been conducted since then. Here we introduce the initial result of the ZL radial profile at optical wavelengths observed at 0.76-1.06 au by ONC-T with Hayabusa2# mission in 2021-2022. The obtained ZL brightness is well reproduced by the model brightness, but there is a small excess of the observed ZL brightness over the model brightness at around 0.9 au. The obtained radial power-law index is [[EQUATION]] , which is consistent with the previous results based on the ZL observations. The dominant uncertainty source arises from the uncertainty in the Diffuse Galactic Light estimation.

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Beyondplanck

Andersen¹,

Aurlien²,

Banerji³

et al. 2023

A&A

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We describe the BEYONDPLANCK project in terms of our motivation, methodology, and main products, and provide a guide to a set of companion papers that describe each result in more detail. Building directly on experience from ESA’s Planck mission, we implemented a complete end-to-end Bayesian analysis framework for the Planck Low Frequency Instrument (LFI) observations. The primary product is a full joint posterior distribution P(ω ∣ d), where ω represents the set of all free instrumental (gain, correlated noise, bandpass, etc.), astrophysical (synchrotron, free-free, thermal dust emission, etc.), and cosmological (cosmic microwave background – CMB – map, power spectrum, etc.) parameters. Some notable advantages of this approach compared to a traditional pipeline procedure are seamless end-to-end propagation of uncertainties; accurate modeling of both astrophysical and instrumental effects in the most natural basis for each uncertain quantity; optimized computational costs with little or no need for intermediate human interaction between various analysis steps; and a complete overview of the entire analysis process within one single framework. As a practical demonstration of this framework, we focus in particular on low-ℓ CMB polarization reconstruction with Planck LFI. In this process, we identify several important new effects that have not been accounted for in previous pipelines, including gain over-smoothing and time-variable and non-1/f correlated noise in the 30 and 44 GHz channels. Modeling and mitigating both previously known and newly discovered systematic effects, we find that all results are consistent with the ΛCDM model, and we constrained the reionization optical depth to τ = 0.066 ± 0.013, with a low-resolution CMB-based χ2 probability to exceed of 32%. This uncertainty is about 30% larger than the official pipelines, arising from taking a more complete instrumental model into account. The marginal CMB solar dipole amplitude is 3362.7 ± 1.4 μK, where the error bar was derived directly from the posterior distribution without the need of any ad hoc instrumental corrections. We are currently not aware of any significant unmodeled systematic effects remaining in the Planck LFI data, and, for the first time, the 44 GHz channel is fully exploited in the current analysis. We argue that this framework can play a central role in the analysis of many current and future high-sensitivity CMB experiments, including LiteBIRD, and it will serve as the computational foundation of the emerging community-wide COSMOGLOBE effort, which aims to combine state-of-the-art radio, microwave, and submillimeter data sets into one global astrophysical model.

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COSMOGLOBE: Simulating zodiacal emission with ZodiPy

Cited by 5 publications

References 23 publications

ZodiPy: A Python package for zodiacal light simulations

ZodiPy: A Python package for zodiacal light simulations

Initial Result of Heliocentric Distance Dependence of Zodiacal Light Observed by Hayabusa2#

Beyondplanck

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