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Microwave Spectro-Polarimetry of Matter and Radiation across Space and Time
PSL Research University1, Université Paris-Saclay2, University of Oxford3, New York University4, Cardiff University5, Lawrence Berkeley National Laboratory6, University of California, Berkeley7, California Institute of Technology8, Delft University of Technology9, Netherlands Institute for Space Research10, University of Bonn11, Cornell University12, INAF13, University of Barcelona14, Centre national de la recherche scientifique15, University of Manchester16, University of Paris17, University of Toronto18, University of Science and Technology of China19, Chinese Academy of Sciences20, Max Planck Society21, Sapienza University of Rome22, University of New South Wales23, Kavli Institute of Nanoscience24, University of Maryland, College Park25, Imperial College London26, Harvard University27, Goddard Space Flight Center28, Ben-Gurion University of the Negev29, RWTH Aachen University30, Perimeter Institute for Theoretical Physics31, University of Ferrara32, University of Porto33, University of Geneva34, European Southern Observatory35, Yale University36, University of California, Los Angeles37, University of La Laguna38, University of British Columbia39, Johns Hopkins University40, University of Oslo41, Indian Institute of Science Education and Research, Pune42, National Institutes of Natural Sciences, Japan43, University of Cambridge44
TL;DR: In this article, the authors proposed a spectro-polarimetric survey of the microwave sky using a broadband polarised imager and a moderate resolution spectroimager at the focus of a 3.5m aperture telescope actively cooled to about 8K.
Abstract: This paper discusses the science case for a sensitive spectro-polarimetric survey of the microwave sky. Such a survey would provide a tomographic and dynamic census of the three-dimensional distribution of hot gas, velocity flows, early metals, dust, and mass distribution in the entire Hubble volume, exploit CMB temperature and polarisation anisotropies down to fundamental limits, and track energy injection and absorption into the radiation background across cosmic times by measuring spectral distortions of the CMB blackbody emission. In addition to its exceptional capability for cosmology and fundamental physics, such a survey would provide an unprecedented view of microwave emissions at sub-arcminute to few-arcminute angular resolution in hundreds of frequency channels, a data set that would be of immense legacy value for many branches of astrophysics. We propose that this survey be carried-out with a large space mission featuring a broad-band polarised imager and a moderate resolution spectro-imager at the focus of a 3.5m aperture telescope actively cooled to about 8K, complemented with absolutely-calibrated Fourier Transform Spectrometer modules observing at degree-scale angular resolution in the 10-2000 GHz frequency range. We propose two observing modes: a survey mode to map the entire sky as well as a few selected wide fields, and an observatory mode for deeper observations of regions of specific interest.
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28,685 citations
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TL;DR: In this article, a review of the teleparallel gravity literature is presented, focusing on the open questions in this regime of physics, and the cosmological consequences for the various formulations of the proposed theories.
Abstract: Teleparallel gravity has significantly increased in popularity in recent decades, bringing attention to Einstein's other theory of gravity. In this Review, we relate this form of geometry to the broader metric-affine approach to forming gravitational theories where we describe a systematic way of constructing consistent teleparallel theories that respect certain physical conditions such as local Lorentz invariance. We first use teleparallel gravity to formulate a teleparallel equivalent of general relativity which is dynamically equivalent to general relativity but which may have different behaviors for other scenarios, such as quantum gravity. After setting this foundation, we describe the plethora of modified teleparallel theories of gravity that have been proposed in the literature. In the second part of the Review, we first survey works in teleparallel astrophysics literature where we focus on the open questions in this regime of physics. We then discuss the cosmological consequences for the various formulations of teleparallel gravity. We do this at background level by exploring works using various approaches ranging from dynamical systems to Noether symmetries, and more. Naturally, we then discuss perturbation theory, firstly by giving a concise approach in which this can be applied in teleparallel gravity theories and then apply it to a number of important theories in the literature. Finally, we examine works in observational and precision cosmology across the plethora of proposal theories. This is done using some of the latest observations and is used to tackle cosmological tensions which may be alleviated in teleparallel cosmology. We also introduce a number of recent works in the application of machine learning to gravity, we do this through deep learning and Gaussian processes, together with discussions about other approaches in the literature.
60 citations
TL;DR: In this paper, the authors compute the distortion signals from decaying particles that convert directly into photons at different epochs during cosmic history, focusing on injection energies $E_\mathrm{inj}\lesssim 20\,\mathm{keV}$.
Abstract: Spectral distortions (SDs) of the cosmic microwave background (CMB) provide a powerful tool for studying particle physics. Here we compute the distortion signals from decaying particles that convert directly into photons at different epochs during cosmic history, focusing on injection energies $E_\mathrm{inj}\lesssim 20\,\mathrm{keV}$. We deliver a comprehensive library of SD solutions that can be used to study a wide range of particle physics scenarios. We use {\tt CosmoTherm} to compute the SD signals, including effects on the ionization history and opacities of the Universe. We also consider the effect of blackbody-induced stimulated decay, which can modify the injection history significantly. Then, we use data from COBE/FIRAS and EDGES to constrain the properties of the decaying particles. We explore scenarios where these provide a dark matter (DM) candidate or constitute only a small fraction of DM. We complement the SD constraints with CMB anisotropy constraints, highlighting new effects from injections at very-low photon energies ($h
u\lesssim 10^{-4}\,\mathrm{eV}$). Our model-independent constraints exhibit rich structures in the lifetime-energy domain, covering injection energies $E_\mathrm{inj}\simeq 10^{-10}\mathrm{eV}-10\mathrm{keV}$ and lifetimes $\tau_X\simeq 10^5\,\mathrm{s}-10^{33}\mathrm{s}$. We discuss the constraints on axions and axion-like particles that convert directly into two photons, revising existing SD constraints in the literature. Our limits are competitive with other constraints for axion masses $m_a c^2\gtrsim 27\,\mathrm{eV}$ and we find that simple estimates based on the overall energetics are generally inaccurate. Future CMB spectrometers could significantly improve the obtained constraints, thus providing an important complementary probe of early-universe particle physics.
45 citations
Cites background from "Microwave Spectro-Polarimetry of Ma..."
...…photon conversion mediated by magnetic fields inside our galaxy and galaxy clusters can lead to anisotropic spectral distortions (both polarized and unpolarized, e.g., Mukherjee et al. 2019, 2020), providing exciting targets for future CMB imagers (Delabrouille et al. 2019; Chluba et al. 2019a)....
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TL;DR: In this paper, a precision analytic fitting formula for the exact numerical results of the relativistic corrections to the thermal Sunyaev-Zeldovich effect for clusters of galaxies was obtained.
Abstract: We have succeeded in obtaining a precision analytic fitting formula for the exact numerical results of the relativistic corrections to the thermal Sunyaev-Zeldovich effect for clusters of galaxies which has a 1% accuracy for the crossover frequency region where the thermal thermal Sunyaev-Zeldovich effect signal changes from negative to positive sign. The fitting has been carried out for the ranges 0.020 < theta < 0.035 and 0 < X < 15, where theta= kTe/mc^{2}, X = omega/kT0, Te is the electron temperature, omega is the angular frequency of the photon, and T0 is the temperature of the cosmic microwave background radiation. The overall accuracy of the fitting is better than 0.1%. The present analytic fitting formula will be useful for accurate analyses of the thermal Sunyaev-Zeldovich effect for clusters of galaxies.
43 citations
TL;DR: In this article, the authors present a detection of molecular gas emission at 1-5 GHz using line intensity mapping using a pair of 3 mm interferometric data sets, the first from the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field (ASPECS), and the second from a series of Atacama Compact Array (ACA) observations conducted between 2016 and 2018, targeting the COSMOS field.
Abstract: We present a detection of molecular gas emission at $z\sim1-5$ using the technique of line intensity mapping. We make use of a pair of 3 mm interferometric data sets, the first from the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field (ASPECS), and the second from a series of Atacama Compact Array (ACA) observations conducted between 2016 and 2018, targeting the COSMOS field. At 100 GHz, we measure non-zero power at 97.8% and 99.9% confidence in the ACA and ALMA data sets, respectively. In the joint result, we reject the zero-power hypothesis at 99.99% confidence, finding $\tilde{I}^{2}_{s}(
u)=770\pm210\ \mu\textrm{K}^2\ \textrm{Hz}\ \textrm{sr}$. After accounting for sample variance effects, the estimated spectral shot power is $\tilde{I}^{2}_{s}(
u)=1010_{-390}^{+550}\ \mu\textrm{K}^2\ \textrm{Hz}\ \textrm{sr}$. We derive a model for the various line species our measurement is expected to be sensitive to, and estimate the shot power to be $120_{-40}^{+80}\ \mu\textrm{K}^2\ h^{-3}\,\textrm{Mpc}^{3}$, $200^{+120}_{-70}\ \mu\textrm{K}^2\ h^{-3}\,\textrm{Mpc}^{3}$, and $90^{+70}_{-40}\ \mu\textrm{K}^2\ h^{-3}\,\textrm{Mpc}^{3}$ for CO(2-1) at $z=1.3$, CO(3-2) at $z=2.5$, and CO(4-3) at $z=3.6$, respectively. Using line ratios appropriate for high-redshift galaxies, we find these results to be in good agreement with those from the CO Power Spectrum Survey (COPSS). Adopting $\alpha_{\rm CO}=3.6\ M_{\odot}\ (\textrm{K}\ \textrm{km}\ \textrm{s}^{-1}\ \textrm{pc}^{2})^{-1}$, we estimate a cosmic molecular gas density of $\rho_{\textrm{H}_2}(z)\sim 10^{8}\ M_{\odot}\ \textrm{Mpc}^{-3}$ between $z=1-3$.
35 citations
Cites methods from "Microwave Spectro-Polarimetry of Ma..."
...Such experiments are likely to benefit from the decades of significant technical and observational studies of the CMB, and may be highly compatible with future experiments targeting the CMB (e.g, Switzer 2017; Moradinezhad Dizgah & Keating 2019; Delabrouille et al. 2019)....
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References
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01 Jan 2012
139,059 citations
"Microwave Spectro-Polarimetry of Ma..." refers background in this paper
...As a by-product of our systematic search for protoclusters, we expect to identify tens of thousands of strongly lensed dusty starbursts [39] out to z ' 7 or even higher....
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Journal Article•
28,685 citations
"Microwave Spectro-Polarimetry of Ma..." refers background in this paper
...Filter-bank spectrometer: l i t t t : s r r r l i : The recently demonstrated on-chip filter-bank spectrometer is an ideal candidate to provide spectral filtering and radiation detection over large bandwidths with minimal weight and complexity [177]....
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...On the same platform (or on an independent spacecraft) absolute spectroscopy across the entire frequency range will be performed by a Fourier-transform spectrometer (FTS) consisting of one or a few independent FTS modules, covering the full 10–2000 GHz band with spectral resolution ranging from 2.5 to 60 GHz, angular resolution ranging from a fraction of a degree to a few degrees, and overall sensitivity 1 Jy sr−1, 4 to 5 orders of magnitude better than that of COBE-FIRAS....
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...The proposed survey requires an L-class space mission, featuring three instruments that observe within the 10–2000 GHz frequency range, at varying spectral and angular resolutions....
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...7 Requirements and goals for mapping CMB lensing to trace the distribution of mass Full-sky CMB sensitivity ∆T per ' 1′ pixel between ' 1µK (requirement) and ' 0.6µK (goal); Deep-patch CMB sensitivity ∆T per ' 1′ pixel of ' 0.3µK; Angular resolution between 1.4′ (requirement) and 1′ (goal); Observations from ' 50 to ' 800 GHz with ' 20 frequency channels....
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...These channels should cover the frequency range where the SZ signals are the strongest relative to other emissions (between 100 and 400 GHz), with channels around the tSZ minimum, null, and maximum (150, 220, and 350 GHz), and extra channels at lower and higher frequencies to characterize low- and high-frequency foregrounds....
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TL;DR: The Virgo Consortium's EAGLE project as discussed by the authors is a suite of hydrodynamical simulations that follow the formation of galaxies and black holes in representative volumes, where thermal energy is injected into the gas, allowing winds to develop without predetermined speed or mass loading factors.
Abstract: We introduce the Virgo Consortium's EAGLE project, a suite of hydrodynamical simulations that follow the formation of galaxies and black holes in representative volumes. We discuss the limitations of such simulations in light of their finite resolution and poorly constrained subgrid physics, and how these affect their predictive power. One major improvement is our treatment of feedback from massive stars and AGN in which thermal energy is injected into the gas without the need to turn off cooling or hydrodynamical forces, allowing winds to develop without predetermined speed or mass loading factors. Because the feedback efficiencies cannot be predicted from first principles, we calibrate them to the z~0 galaxy stellar mass function and the amplitude of the galaxy-central black hole mass relation, also taking galaxy sizes into account. The observed galaxy mass function is reproduced to ≲0.2 dex over the full mass range, 108
2,828 citations
Case Western Reserve University1, University of Wisconsin-Madison2, Imperial College London3, South Dakota School of Mines and Technology4, University of Maryland, College Park5, University of California, Berkeley6, Lawrence Livermore National Laboratory7, University of Coimbra8, University of South Dakota9, Yale University10, University of California, Santa Barbara11, Brown University12, University of California, Davis13, Lawrence Berkeley National Laboratory14, University College London15, University of Rochester16, SLAC National Accelerator Laboratory17, Texas A&M University18, State University of New York System19, University of Edinburgh20
TL;DR: This search yields no evidence of WIMP nuclear recoils and constraints on spin-independent weakly interacting massive particle (WIMP)-nucleon scattering using a 3.35×10^{4} kg day exposure of the Large Underground Xenon experiment are reported.
Abstract: We report constraints on spin-independent weakly interacting massive particle (WIMP)-nucleon scattering using a 3.35×10^{4} kg day exposure of the Large Underground Xenon (LUX) experiment. A dual-phase xenon time projection chamber with 250 kg of active mass is operated at the Sanford Underground Research Facility under Lead, South Dakota (USA). With roughly fourfold improvement in sensitivity for high WIMP masses relative to our previous results, this search yields no evidence of WIMP nuclear recoils. At a WIMP mass of 50 GeV c^{-2}, WIMP-nucleon spin-independent cross sections above 2.2×10^{-46} cm^{2} are excluded at the 90% confidence level. When combined with the previously reported LUX exposure, this exclusion strengthens to 1.1×10^{-46} cm^{2} at 50 GeV c^{-2}.
1,844 citations
Columbia University1, University of Amsterdam2, University of California, Los Angeles3, University of Coimbra4, University of Zurich5, University of Mainz6, University of Münster7, University of Nantes8, Weizmann Institute of Science9, Shanghai Jiao Tong University10, University of Bologna11, Max Planck Society12, Purdue University13, Rice University14
TL;DR: A search for particle dark matter with the XENON100 experiment, operated at the Laboratori Nazionali del Gran Sasso for 13 months during 2011 and 2012, has yielded no evidence for dark matter interactions.
Abstract: We report on a search for particle dark matter with the XENON100 experiment, operated at the Laboratori Nazionali del Gran Sasso (LNGS) for 13 months during 2011 and 2012. XENON100 features an ultra-low electromagnetic background of (5.3\pm0.6)\times10^-3 events (kg day keVee)^-1 in the energy region of interest. A blind analysis of 224.6 live days \times 34 kg exposure has yielded no evidence for dark matter interactions. The two candidate events observed in the pre-defined nuclear recoil energy range of 6.6-30.5 keVnr are consistent with the background expectation of (1.0 \pm 0.2) events. A Profile Likelihood analysis using a 6.6-43.3 keVnr energy range sets the most stringent limit on the spin-independent elastic WIMP-nucleon scattering cross section for WIMP masses above 8 GeV/c^2, with a minimum of 2 \times 10^-45 cm^2 at 55 GeV/c^2 and 90% confidence level.
1,624 citations