Cosmic expansion history from SNe Ia data via information field theory

A&A 2017

Authors:

Natalia Porqueres, Torsten A. Enßlin, Maksim Greiner, Vanessa Böhm, Sebastian Dorn, Pilar Ruiz-Lapuente, Alberto Manrique

Abstract:

We present charm (cosmic history agnostic reconstruction method), a novel inference algorithm that reconstructs the cosmic expansion history as encoded in the Hubble parameter H(z) from SNe Ia data. The novelty of the approach lies in the usage of information field theory, a statistical field theory that is very well suited for the construction of optimal signal recovery algorithms. The charm algorithm infers non-parametrically s(a)=ln(ρ(a)/ρcrit0), the density evolution which determines H(z), without assuming an analytical form of ρ(a) but only its smoothness with the scale factor a=(1+z)−1. The inference problem of recovering the signal s(a) from the data is formulated in a fully Bayesian way. In detail, we have rewritten the signal as the sum of a background cosmology and a perturbation. This allows us to determine the maximum a posteriory estimate of the signal by an iterative Wiener filter method. Applying charm to the Union2.1 supernova compilation, we have recovered a cosmic expansion history that is fully compatible with the standard ΛCDM cosmological expansion history with parameter values consistent with the results of the Planck mission.

NIFTy 3 - Numerical Information Field Theory - A Python framework for multicomponent signal inference on HPC clusters

Annalen der Physik 2017

Authors:

Theo Steininger, Jait Dixit, Philipp Frank, Maksim Greiner, Sebastian Hutschenreuter, Jakob Knollmüller, Reimar Leike, Natalia Porqueres, Daniel Pumpe, Martin Reinecke, Matevž Šraml, Csongor Varady, Torsten Enßlin

Abstract:

NIFTy, "Numerical Information Field Theory", is a software framework designed to ease the development and implementation of field inference algorithms. Field equations are formulated independently of the underlying spatial geometry allowing the user to focus on the algorithmic design. Under the hood, NIFTy ensures that the discretization of the implemented equations is consistent. This enables the user to prototype an algorithm rapidly in 1D and then apply it to high-dimensional real-world problems. This paper introduces NIFTy 3, a major upgrade to the original NIFTy framework. NIFTy 3 allows the user to run inference algorithms on massively parallel high performance computing clusters without changing the implementation of the field equations. It supports n-dimensional Cartesian spaces, spherical spaces, power spaces, and product spaces as well as transforms to their harmonic counterparts. Furthermore, NIFTy 3 is able to treat non-scalar fields. The functionality and performance of the software package is demonstrated with example code, which implements a real inference algorithm from the realm of information field theory.

SDSS IV MaNGA: Discovery of an Ha Blob Associated with a Dry Galaxy Pair-Ejected Gas or a "Dark" Galaxy Candidate?

ASTROPHYSICAL JOURNAL 837:1 (2017) ARTN 32

Authors:

L Lin, J-H Lin, C-H Hsu, H Fu, S Huang, SF Sanchez, S Gwyn, JD Gelfand, E Cheung, K Masters, S Peirani, W Rujopakarn, DV Stark, F Belfiore, MS Bothwell, K Bundy, A Hagen, L Hao, S Huang, D Law, C Li, C Lintott, R Maiolino, A Roman-Lopes, W-H Wang, T Xiao, F Yuan, D Bizyaev, E Malanushenko, N Drory, JG Fernandez-Trincado, Z Pace, K Pan, D Thomas

Complementing the ground-based CMB-S4 experiment on large scales with the PIXIE satellite

Physical Review D 95:6 (2017)

Authors:

E Calabrese, D Alonso, J Dunkley

The XXL survey: First results and future

Astronomische Nachrichten Wiley 338:2-3 (2017) 334-341

Authors:

M Pierre, C Adami, M Birkinshaw, L Chiappetti, S Ettori, A Evrard, L Faccioli, F Gastaldello, P Giles, C Horellou, A Iovino, E Koulouridis, C Lidman, A Le Brun, B Maughan, S Maurogordato, I McCarthy, S Miyazaki, F Pacaud, S Paltani, M Plionis, T Reiprich, T Sadibekova, V Smolcic, S Snowden, J Surdej, M Tsirou, C Vignali, J Willis, S Alis, B Altieri, N Baran, C Benoist, A Bongiorno, M Bremer, A Butler, A Cappi, C Caretta, P Ciliegi, N Clerc, PS Corasaniti, J Coupon, J Delhaize, I Delvecchio, J Democles, Desai Sh, J Devriendt, Y Dubois, D Eckert, A Elyiv, A Farahi, C Ferraril, S Fotopoulou, W Forman, I Georgantopoulos, V Guglielmo, M Huynh, N Jerlin, Jones Ch, S Lavoie, Le Fevre J‐P, M Lieu, M Kilbinger, F MaruIli, A Mantz, S McGee, J‐B Melin, O Melnyk, L Moscardini, M Novak, E Piconcelli, B Poggianti, D Pomarede, E Pompei, T Ponman, ME Ramos Ceja, P Rana, D Rapetti, S Raychaudhury, M Ricci, H Rottgering, M Sahlen, J‐L Sauvageot, C Schimd, M Sereno, GP Smith, K Umetsu, P Valageas, A Valotti, I Valtchanov, A Veropalumbo, B Ascaso, D Barnes, M De Petris, F Durret, M Donahue, M Ithana, M Jarvis, M Johnston‐Hollitt, E Kalfountzou, S Kay, F La Franca, N Okabe, A Muzzin, A Rettura, F Ricci, J Ridl, G Risaliti, M Takizawa, P Thomas, N Truong

Abstract:

The XXL survey currently covers two 25 deg2 patches with XMM observations of ∼10 ks. We summarize the scientific results associated with the first release of the XXL dataset, which occurred in mid‐2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X‐ray (z < 2) cluster, (z < 4) active galactic nuclei (AGN), and cosmic background survey science will then benefit from an extraordinary data reservoir. This, combined with deep multi‐λ observations, will lead to solid standalone cosmological constraints and provide a wealth of information on the formation and evolution of AGN, clusters, and the X‐ray background. In particular, it will offer a unique opportunity to pinpoint the z > 1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions.