Re-Envisioning Numerical Information Field Theory
(NIFTy.re): A Library for Gaussian Processes and Variational
Inference

Edenhofer, Gordian; Frank, Philipp; Roth, Jakob; Leike, Reimar H.; Guerdi, Massin; Scheel-Platz, Lukas I.; Guardiani, Matteo; Eberle, Vincent; Westerkamp, Margret; Enßlin, Torsten A.

doi:10.21105/joss.06593

JOSS

2024

DOI: 10.21105/joss.06593

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Re-Envisioning Numerical Information Field Theory (NIFTy.re): A Library for Gaussian Processes and Variational Inference

Gordian Edenhofer,

Philipp Frank,

Jakob Roth

et al.

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2024

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Cited by 9 publications

References 33 publications

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El Gordo needs El Anzuelo: Probing the structure of cluster members with multi-band extended arcs in JWST data

Galan,

Caminha,

Knollmüller

et al. 2024

A&A

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Gravitational lensing by galaxy clusters involves hundreds of galaxies over a large redshift range and increases the likelihood of rare phenomena (supernovae, microlensing, dark substructures, etc.). Characterizing the mass and light distributions of foreground and background objects often requires a combination of high-resolution data and advanced modeling techniques. We present the detailed analysis of a prominent quintuply imaged dusty star-forming galaxy ($ mainly lensed by three members of the massive galaxy cluster ACT-CL\,J0102$-$4915, also known as d =0.87$). We leverage JWST/NIRCam images, which contain lensing features that were unseen in previous HST images, using a Bayesian, multi-wavelength, differentiable and GPU-accelerated modeling framework that combines (lens modeling) and (field model and inference) software packages. For one of the deflectors, we complement lensing constraints with stellar kinematics measured from VLT/MUSE data. In our lens model, we explicitly include the mass distribution of the cluster, locally corrected by a constant shear field. We find that the two main deflectors (L1 and L2) have logarithmic mass density slopes steeper than isothermal, with $ L1 and $ L2 We argue that such steep density profiles can arise due to tidally truncated mass distributions, which we probe thanks to the cluster lensing boost and the strong asymmetry of the lensing configuration. Moreover, our three-dimensional source model captures most of the surface brightness of the lensed galaxy, revealing a clump with a maximum diameter of $400$ parsecs at the source redshift, visible at wavelengths $ rest mu m. Finally, we caution on using point-like features within extended arcs to constrain galaxy-scale lens models before securing them with extended arc modeling.

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El Gordo needs El Anzuelo: Probing the structure of cluster members with multi-band extended arcs in JWST data

Galan,

Caminha,

Knollmüller

et al. 2024

A&A

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Nonparametric Bayesian reconstruction of Galactic magnetic fields using information field theory

Tsouros,

Bendre,

Edenhofer

et al. 2024

A&A

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Ultrahigh-energy cosmic rays (UHECRs) are charged particles with energies surpassing $10^ $ eV. Their sources remain elusive because they are obscured by deflections caused by the Galactic magnetic field (GMF). This challenge is further complicated by our limited understanding of the 3D structure of the GMF because current GMF observations primarily consist of quantities that are integrated along the line of sight (LOS). Nevertheless, data from upcoming stellar polarization surveys along with Gaia stellar parallax data are expected to yield local GMF measurements. This study is the second entry in our exploration of a Bayesian inference approach to the local GMF that uses synthetic local GMF observations that emulate forthcoming local GMF measurements, and attempts to use them to reconstruct its $3$D structure. The ultimate aim is to trace back observed UHECRs and thereby update our knowledge about their possible origin. In this proof-of-concept work, we assumed as ground truth a magnetic field produced by a dynamo simulation of the Galactic ISM. We employed methods of Bayesian statistical inference in order to sample the posterior distribution of the GMF within part of the Galaxy. By assuming a known rigidity and arrival direction of an UHECR, we traced its trajectory back through various GMF configurations drawn from the posterior distribution. Our objective was to rigorously evaluate the performance of our algorithm in scenarios that closely mirror the setting of expected future applications. In pursuit of this, we conditioned the posterior to synthetically integrated LOS measurements of the GMF, in addition to synthetic local plane of sky-component measurements. Our results demonstrate that for all locations of the observed arrival direction on the plane of sky, our algorithm is able to substantially update our knowledge on the original arrival direction of UHECRs with a rigidity of $E/Z = 5 $ eV, even without any LOS information. When the integrated data are included in the inference, the regions of the celestial sphere in which the maximum error occurs are greatly reduced. The maximum error is diminished by a factor of about $3$ even in these regions in the specific setting we studied. Additionally, we are able to identify the regions in which the largest error is expected to occur.

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The “C”: The large Chameleon-Musca-Coalsack cloud

Edenhofer,

Alves,

Zucker

et al. 2024

A&A

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Recent advancements in 3D dust mapping have transformed our understanding of the Milky Way’s local interstellar medium, enabling us to explore its structure in three spatial dimensions for the first time. In this Letter, we use the most recent 3D dust map by Edenhofer et al. to study the well-known Chameleon, Musca, and Coalsack cloud complexes, located about 200 pc from the Sun. We find that these three complexes are not isolated but rather connect to form a surprisingly well-defined half-ring, constituting a single C-shaped cloud with a radius of about 50 pc, a thickness of about 45 pc, and a total mass of about 5 × 104 M⊙, or 9 × 104 M⊙ if including everything in the vicinity of the C-shaped cloud. Despite the absence of an evident feedback source at its center, the dynamics of young stellar clusters associated with the C structure suggest that a single supernova explosion about 4 Myr–10 Myr ago likely shaped this structure. Our findings support a single origin story for these cloud complexes, suggesting that they were formed by feedback-driven gas compression, and offer new insights into the processes that govern the birth of star-forming clouds in feedback-dominated regions, such as the Scorpius-Centaurus association.

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Re-Envisioning Numerical Information Field Theory (NIFTy.re): A Library for Gaussian Processes and Variational Inference

Cited by 9 publications

References 33 publications

El Gordo needs El Anzuelo: Probing the structure of cluster members with multi-band extended arcs in JWST data

El Gordo needs El Anzuelo: Probing the structure of cluster members with multi-band extended arcs in JWST data

Nonparametric Bayesian reconstruction of Galactic magnetic fields using information field theory

The “C”: The large Chameleon-Musca-Coalsack cloud

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