195 research outputs found
Lensing power spectrum of the Cosmic Microwave Background with deep polarization experiments
Precise reconstruction of the cosmic microwave background lensing potential
can be achieved with deep polarization surveys by iteratively removing
lensing-induced modes. We introduce a lensing spectrum estimator and its
likelihood for such optimal iterative reconstruction. Our modelling share
similarities to the state-of-the-art likelihoods for quadratic estimator-based
(QE) lensing reconstruction. In particular, we generalize the and
lensing biases, and design a realization-dependent spectrum debiaser,
making this estimator robust to uncertainties in the data modelling. We
demonstrate unbiased recovery of the cosmology using map-based reconstructions.
For a CMB-S4 survey, this spectrum estimator and likelihood can double the
constraints on the lensing amplitude compared to the QE on a wide range of
scales, while keeping numerical cost under control and being robust to errors.Comment: 8 pages, 4 figure
Robust and efficient CMB lensing power spectrum from polarization surveys
Deep surveys of the CMB polarization have more information on the lensing
signal than the quadratic estimators (QE) can capture. We showed in a recent
work that a CMB lensing power spectrum built from a single optimized CMB
lensing mass map, working in close analogy to state-of-the-art QE techniques,
can result in an essentially optimal spectrum estimator at reasonable numerical
cost. We extend this analysis here to account for real-life non-idealities
including masking and realistic instrumental noise maps. As in the QE case, it
is necessary to include small corrections to account for the estimator response
to these anisotropies, which we demonstrate can be estimated easily from
simulations. The realization-dependent debiasing of the spectrum remains
robust, allowing unbiased recovery of the band powers even in cases where the
statistical model used for the lensing map reconstruction is grossly wrong.
This allows now robust and at the same time optimal CMB lensing constraints
from CMB data, on all scales relevant for the inference of the neutrino mass,
or other parameters of our cosmological model.Comment: 12 pages, 8 figures, comments are welcom
Cluster profiles from beyond-the-QE CMB lensing mass maps
Clusters of galaxies, being the largest collapsed structures in the universe,
offer valuable insights into the nature of cosmic evolution. Precise
calibration of the mass of clusters can be obtained by extracting their
gravitational lensing signal on the Cosmic Microwave Background (CMB)
fluctuations. We extend and test here the performance achieved on cluster
scales by the parameter-free, maximum a posteriori (MAP) CMB lensing
reconstruction method, which has been shown to be optimal in the broader
context of CMB lensing mass map and power spectrum estimation. In the context
of cluster lensing, the lensing signal of other large-scale structures acts as
an additional source of noise. We show here that by delensing the CMB
fluctuations around each and every cluster, this noise variance is reduced
according to expectations. We also demonstrate that the well-known bias in the
temperature quadratic estimator in this regime, sourced by the strong
non-Gaussianity of the signal, is almost entirely mitigated without any scale
cuts. Being statistically speaking an optimal and blind lensing mass map
reconstruction, the MAP estimator is a promising tool for the calibration of
the masses of clusters.Comment: 11 pages, 4 figures, prepared for PRD submissio
Occipital nerve block is effective in craniofacial neuralgias but not in idiopathic persistent facial pain
Occipital nerve block (ONB) has been used in several primary headache syndromes with good results. Information on its effects in facial pain is sparse. In this chart review, the efficacy of ONB using lidocaine and dexamethasone was evaluated in 20 patients with craniofacial pain syndromes comprising 8 patients with trigeminal neuralgia, 6 with trigeminal neuropathic pain, 5 with persistent idiopathic facial pain and 1 with occipital neuralgia. Response was defined as an at least 50% reduction of original pain. Mean response rate was 55% with greatest efficacy in trigeminal (75%) and occipital neuralgia (100%) and less efficacy in trigeminal neuropathic pain (50%) and persistent idiopathic facial pain (20%). The effects lasted for an average of 27 days with sustained benefits for 69, 77 and 107 days in three patients. Side effects were reported in 50%, albeit transient and mild in nature. ONBs are effective in trigeminal pain involving the second and third branch and seem to be most effective in craniofacial neuralgias. They should be considered in facial pain before more invasive approaches, such as thermocoagulation or vascular decompression, are performed, given that side effects are mild and the procedure is minimally invasive
The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and its Implications for Structure Growth
We present new measurements of cosmic microwave background (CMB) lensing over
sq. deg. of the sky. These lensing measurements are derived from the
Atacama Cosmology Telescope (ACT) Data Release 6 (DR6) CMB dataset, which
consists of five seasons of ACT CMB temperature and polarization observations.
We determine the amplitude of the CMB lensing power spectrum at
precision ( significance) using a novel pipeline that minimizes
sensitivity to foregrounds and to noise properties. To ensure our results are
robust, we analyze an extensive set of null tests, consistency tests, and
systematic error estimates and employ a blinded analysis framework. The
baseline spectrum is well fit by a lensing amplitude of
relative to the Planck 2018 CMB power spectra
best-fit CDM model and relative to
the best-fit model. From our lensing power
spectrum measurement, we derive constraints on the parameter combination
of
from ACT DR6 CMB lensing alone and
when combining ACT DR6 and Planck NPIPE
CMB lensing power spectra. These results are in excellent agreement with
CDM model constraints from Planck or
CMB power spectrum measurements. Our lensing measurements from redshifts
-- are thus fully consistent with CDM structure growth
predictions based on CMB anisotropies probing primarily . We find no
evidence for a suppression of the amplitude of cosmic structure at low
redshiftsComment: 45+21 pages, 50 figures. Prepared for submission to ApJ. Also see
companion papers Madhavacheril et al and MacCrann et a
The Athena X-ray Integral Field Unit: a consolidated design for the system requirement review of the preliminary definition phase
The Athena X-ray Integral Unit (X-IFU) is the high resolution X-ray
spectrometer, studied since 2015 for flying in the mid-30s on the Athena space
X-ray Observatory, a versatile observatory designed to address the Hot and
Energetic Universe science theme, selected in November 2013 by the Survey
Science Committee. Based on a large format array of Transition Edge Sensors
(TES), it aims to provide spatially resolved X-ray spectroscopy, with a
spectral resolution of 2.5 eV (up to 7 keV) over an hexagonal field of view of
5 arc minutes (equivalent diameter). The X-IFU entered its System Requirement
Review (SRR) in June 2022, at about the same time when ESA called for an
overall X-IFU redesign (including the X-IFU cryostat and the cooling chain),
due to an unanticipated cost overrun of Athena. In this paper, after
illustrating the breakthrough capabilities of the X-IFU, we describe the
instrument as presented at its SRR, browsing through all the subsystems and
associated requirements. We then show the instrument budgets, with a particular
emphasis on the anticipated budgets of some of its key performance parameters.
Finally we briefly discuss on the ongoing key technology demonstration
activities, the calibration and the activities foreseen in the X-IFU Instrument
Science Center, and touch on communication and outreach activities, the
consortium organisation, and finally on the life cycle assessment of X-IFU
aiming at minimising the environmental footprint, associated with the
development of the instrument. Thanks to the studies conducted so far on X-IFU,
it is expected that along the design-to-cost exercise requested by ESA, the
X-IFU will maintain flagship capabilities in spatially resolved high resolution
X-ray spectroscopy, enabling most of the original X-IFU related scientific
objectives of the Athena mission to be retained. (abridged).Comment: 48 pages, 29 figures, Accepted for publication in Experimental
Astronomy with minor editin
The Athena X-ray Integral Field Unit: a consolidated design for the system requirement review of the preliminary definition phase
The Athena X-ray Integral Unit (X-IFU) is the high resolution X-ray spectrometer studied since 2015 for flying in the mid-30s on the Athena space X-ray Observatory. Athena is a versatile observatory designed to address the Hot and Energetic Universe science theme, as selected in November 2013 by the Survey Science Committee. Based on a large format array of Transition Edge Sensors (TES), X-IFU aims to provide spatially resolved X-ray spectroscopy, with a spectral resolution of 2.5 eV (up to 7 keV) over a hexagonal field of view of 5 arc minutes (equivalent diameter). The X-IFU entered its System Requirement Review (SRR) in June 2022, at about the same time when ESA called for an overall X-IFU redesign (including the X-IFU cryostat and the cooling chain), due to an unanticipated cost overrun of Athena. In this paper, after illustrating the breakthrough capabilities of the X-IFU, we describe the instrument as presented at its SRR (i.e. in the course of its preliminary definition phase, so-called B1), browsing through all the subsystems and associated requirements. We then show the instrument budgets, with a particular emphasis on the anticipated budgets of some of its key performance parameters, such as the instrument efficiency, spectral resolution, energy scale knowledge, count rate capability, non X-ray background and target of opportunity efficiency. Finally, we briefly discuss the ongoing key technology demonstration activities, the calibration and the activities foreseen in the X-IFU Instrument Science Center, touch on communication and outreach activities, the consortium organisation and the life cycle assessment of X-IFU aiming at minimising the environmental footprint, associated with the development of the instrument. Thanks to the studies conducted so far on X-IFU, it is expected that along the design-to-cost exercise requested by ESA, the X-IFU will maintain flagship capabilities in spatially resolved high resolution X-ray spectroscopy, enabling most of the original X-IFU related scientific objectives of the Athena mission to be retained. The X-IFU will be provided by an international consortium led by France, The Netherlands and Italy, with ESA member state contributions from Belgium, Czech Republic, Finland, Germany, Poland, Spain, Switzerland, with additional contributions from the United States and Japan.The French contribution to X-IFU is funded by CNES, CNRS and CEA. This work has been also supported by ASI (Italian Space Agency) through the Contract 2019-27-HH.0, and by the ESA (European Space Agency) Core Technology Program (CTP) Contract No. 4000114932/15/NL/BW and the AREMBES - ESA CTP No.4000116655/16/NL/BW. This publication is part of grant RTI2018-096686-B-C21 funded by MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe”. This publication is part of grant RTI2018-096686-B-C21 and PID2020-115325GB-C31 funded by MCIN/AEI/10.13039/501100011033
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