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WMAP's Introduction to Cosmology

Planck 353 GHz 𝜏 = ± (Planck 2013 XV) Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 7 Brief history of t measurementsWMAP 9yrs: 𝜏 = ± (Hinshaw+ 2013) WMAP 9yrs + Planck 353 GHz 𝜏 = ± (Planck 2013 XV) WMAP 9yrs + Planck 353 GHz 𝜏 = ± (Planck 2018 V in pr.) Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 8 Brief history of t measurementsWMAP 9yrs: 𝜏 = ± (Hinshaw+ 2013) WMAP 9yrs + Planck 353 GHz 𝜏 = ± (Planck 2013 XV) WMAP 9yrs + Planck 353 GHz 𝜏 = ± (Planck 2018 V in pr.) Planck lowTEB (LFI) (Planck 2015 XIII) 𝜏 = ± 0.023 Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 9 Brief history of t measurementsWMAP 9yrs: 𝜏 = ± (Hinshaw+ 2013) WMAP 9yrs + Planck 353 GHz 𝜏 = ± (Planck 2013 XV) WMAP 9yrs + Planck 353 GHz 𝜏 = ± (Planck 2018 V in pr.) Planck lowTEB (LFI) (Planck 2015 XIII) 𝜏 = ± 0.023 Planck lowTEB (LFI) (Planck 2018 V in pr.) 𝜏 = ± 0.020 Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 10 Brief history of t measurementsWMAP 9yrs: 𝜏 = ± (Hinshaw+ 2013) WMAP 9yrs + Planck 353 GHz 𝜏 = ± (Planck 2013 XV) WMAP 9yrs + Planck 353 GHz 𝜏 = ± (Planck 2018 V in pr.) Planck lowTEB (LFI) (Planck 2015 XIII) 𝜏 = ± 0.023 Planck lowTEB (LFI) (Planck 2018 V in pr.) 𝜏 = ± 0.020 Planck lowE (HFI) (Planck XLVI) 𝜏 = ± 0.009 Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 11 Brief history of t measurementsWMAP 9yrs: 𝜏 = ± (Hinshaw+ 2013) WMAP 9yrs + Planck 353 GHz 𝜏 = ± (Planck 2013 XV) WMAP 9yrs + Planck 353 GHz 𝜏

WMAP- Content of the Universe

– LiteBIRD Kick Off Meeting - JAXS 1 July 2019 21 A joint map from LFI and WMAPPreliminary LFI+WMAP The WMAP low-ell polarization likelihood can be analyzed using a map-based formalism similar for LFI. Good consistency already at the level of angular power spectrum This enables use of a joint (weighted-average by pixel) dataset U. Natale et al. in prep. Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 22 The LFI+WMAP dataset Good consistency across different Galactic masksPreliminary Good consistency across different Galactic masks Dt scatter by mask compared to simulations U. Natale et al. in prep. Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 23 t from LFI and WMAP from LFI+WMAP PreliminaryNull test is map-based, estimate has ~20% error on t (from low ell only) Includes TE (and, potentially, BB, TB, EB...) But from a pixel-based likelihood. Can be used to constrain models for which an EE spectrum-based likelihood (as HFI) in unsuited, e.g. non-isotropic cosmologies (CMB anomalies) Cosmological birefringence Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 24 Joint view of existing constraints on tL. Pagano Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 25 Conclusions and lessons learnedIn low ell polarization, LFI has provided constraints based on 70 GHz, used as baseline in 2015 and as consistency in 2018. Low ell polarization is an hard measurement. The Planck experience shows that systematic errors can arise at the level of data processing, in the interplay between calibration, map-making and component separation Validation through end-to-end simulations is an extremely important step Solving problems requires time. LFI could benefit from a well integrated team, thanks to strong links between Science Ground Segment and Science exploitation teams. Post-legacy analysis is delivering a joint pixel based dataset for LFI and WMAP, competitive in terms of noise and suitable for many non-standard analyses. Paolo Natoli – LFI Systematics

WMAP- Expansion of the Universe

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WMAP's Introduction to Cosmology - NASA

In the universe is crucial for figuring out its geometry and its fate.Let's explore three possibilities for the geometry of the universe: open, closed or flat. If the density of matter in the universe is greater than the critical density, then we say our universe is closed and has a positive curvature. In a closed universe, you could set out on a journey across space, traveling in a straight line, and you'd eventually loop around and arrive back at your starting point. The positive curvature is convex rather than concave, and it would imply a universe shaped like the surface of a sphere. In a sphere, two parallel lines would not remain parallel forever; first they would diverge, and then they would converge back onto their point of origin and cross over each other.If the density of matter in the universe is less than the critical density, the geometry of the universe is described as being open and negatively curved, like the concave shape of a saddle, and quite possibly infinite in extent.But if the universe is keenly balanced so that the density of matter is equal to the critical density, then the geometry of the universe is described as being flat. A flat geometry is a Euclidean geometry, named after the ancient Greek mathematician Euclid, wherein parallel lines remain parallel and the angles of a triangle add up to 180 degrees.So which is it? NASA's Wilkinson Microwave Anisotropy Probe (WMAP) and the European Space Agency's Planck mission have measured the matter-energy density of the universe, and both have found omega to be equal to the critical density. In other words, the universe seems to have a flat geometry.What are some possible shapes of our universe?By studying the density of matter on the cosmic microwave background (snapshots of which we can see in the squares), astronomers can determine whether the universe is open (not enough matter), flat (just enough matter), or closed (too much matter). (Image credit: NASA/WMAP Science Team)WMAP and Planck measured omega with a great deal of precision, and cosmologists are very confident that the universe is flat.

web vulnerabilities scan with WMAP

And Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 26 Extra Slides Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 27 Post legacy analysis PreliminarySeveral, ongoing post legacy activities on LFI Timeline reprocessing and improved calibration with component separation interplay is eventual goal: will take some time. Optimization of the procedure on existing timelines is already yielding results, e.g. in terms of consistency across masking U. Natale et al, in preparation Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 28 WMAP 9 year dataset The WMAP large-angle polarization likelihood can be analyzed using a map-based formalism similar for LFI Using weighted average for Ka, Q and V for CMB K-band and HFI 353 for synchrotron and dust cleaning As opposed to LFI 30 GHz and HFI 353 GHz for LFI, with CMB only from 70 GHz Good consistency already at the level of angular power spectrum This enables use of a joint (weighted-average by pixel) dataset Preliminary Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 29 With and without TE Dt = t(TT+TE+EE) – t(TT+EE)Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019

WMAP- Life in the Universe - NASA

Chosen different paths to interrogate our universe's beginnings.In a 2020 study, researchers did so by investigating the split between matter and antimatter. In the study, not yet peer-reviewed, they proposed that the imbalance in the amount of matter and antimatter in the universe is related to the universe's vast quantities of dark matter, an unknown substance that exerts influence over gravity and yet doesn't interact with light. They suggested that in the crucial moments immediately after the Big Bang, the universe may have been pushed to make more matter than its inverse, antimatter, which then could have led to the formation of dark matter.The age of the universeArtist's impression of the European Space Agency's Planck spacecraft. Planck's main goal is to study the Cosmic Microwave Background — the relic radiation left over from the Big Bang. (Image credit: ESA/C. Carreau)The CMB has been observed by many researchers now and with many spacecraft missions. One of the most famous space-faring missions to do so was NASA's Cosmic Background Explorer (COBE) satellite, which mapped the sky in the 1990s.Several other missions have followed in COBE's footsteps, such as the BOOMERanG experiment (Balloon Observations of Millimetric Extragalactic Radiation and Geophysics), NASA's Wilkinson Microwave Anisotropy Probe (WMAP) and the European Space Agency's Planck satellite.Planck's observations mapped the CMB in unprecedented detail. Planck was turned off on Oct. 23, 2013, but the data gathered by the observatory is continually explored.Related: How old is the universe?The maps give rise to new mysteries, however, such as why the Southern Hemisphere appears slightly redder (warmer) than the Northern Hemisphere. The Big Bang Theory says that the CMB would be mostly the same, no matter where you look.Examining the CMB also gives astronomers clues as to the composition of the universe. Researchers think most of the cosmos is made up of matter and energy that cannot be "sensed" with our conventional instruments, leading to the names "dark matter" and "dark energy." It is thought that only 5% of the universe is made up of matter such as planets, stars and galaxies.This graphic shows a timeline of the universe based on the Big Bang theory and inflation models. (Image credit: NASA / WMAP Science Team)Was the Big Bang an explosion?Although the Big Bang is often described as an "explosion", that's a misleading image. In an explosion, fragments are flung out from a central point into a pre-existing space. If you were at the central point, you'd see all the fragments moving away from you at roughly the same speed.But the Big Bang wasn't like that. It was an expansion of space itself — a concept that comes out of Einstein's equations of general relativity but has no counterpart in the

WMAP- Age of the Universe - NASA

This graphic shows a timeline of the universe based on the Big Bang theory and inflation models.(Image credit: NASA/WMAP)Big Bang DiagramNASA The Big Bang theory proposes that the universe began as an extremely hot and dense dot only a few millimeters wide. It since grew over 13.7 billion years into the vast and cooler expanding cosmos that presently exists. An extension of the Big Bang model, inflation, poses that the universe initially expanded far faster than the speed of light and grew from a subatomic size to a golf-ball size almost instantaneously, shown in this diagram. It took quite a bit more than seven days to create the universe as we know it today. SPACE.com looks at the mysteries of the heavens in our series: The History & Future of the Cosmos. This is Part 2 in that series.Astronomers Detect First Split-Second of the UniverseNASA/WMAP The Wilkinson Microwave Anisotropy Probe (WMAP) has produced a new, more detailed picture of the infant universe. Colors indicate "warmer" (red) and "cooler" (blue) spots. The white bars show the "polarization" direction of the oldest light. This new information helps to pinpoint when the first stars formed and provides new clues about events that transpired in the first trillionth of a second of the universe.After Big Bang Came Moment of Pure Chaos, Study FindsESO Snapshot from a computer simulation of the formation of large-scale structures in the universe, showing a patch of 100 million light-years and the resulting coherent motions of galaxies flowing toward the highest mass concentration in the center.Star Observations Could Solve Cosmic RiddleEuropean Southern Observatory The globular cluster NGC 6397 contains around 400,000 stars and is located about 7,200 light years away in the southern constellation Ara. With an estimated age of 13.5 billion years, it is likely among the first objects of the galaxy to form after the Big Bang.New Model of the Early UniverseAlvaro Orsi, Institute for Computational Cosmology, Durham University. The universe, 590 million years after the Big Bang, may have looked like this, according to computer simulations, with some stretches of dark matter (green) and galaxies with varying luminosity of star formation (yellow is brightest).Hubble Lifts Fog on Early UniverseNASA, ESA, R. Windhorst (Arizona State University) and H. Yan (Spitzer Science Center, Caltech) This image shows primordial dwarf galaxy candidates circled in green. Three enlargements at right show several dwarf objects that are at the limits of Hubble's present instrument capabilities in September 2004. The Hubble UDF is a small region of sky in the direction of the southern constellation Fornax. The faintest objects are less than one four-billionth the brightness of stars that can be seen with the naked eye.Explanation of Dark Matter Might Lie in Origin of Stars Science One scenario envisioning the creation of the earliest stars suggests that dark matter particles are very light and can zip through space more quickly. These warm dark matter models predict that dark matter formed long filamentary structures along which stars appeared like pearls on a string. In. WMap 3.0.3 APK download for Android. Create beautiful, minimal, custom map wallpapers and backgrounds with WMap.

WMAP- Fate of the Universe - NASA

Presentation on theme: "LFI systematics and impact on science"— Presentation transcript: 1 LFI systematics and impact on sciencePaolo Natoli Università di Ferrara and INFN on behalf of the Planck collaboration and of the LFI Data Processing Center Special credits: L. Colombo, A. Gruppuso, M. Lattanzi, M. Migliaccio, D. Molinari, U. Natale, L. Pagano 2 The Low Frequency Instrument on PlanckLFI was the Low Frequency Instrument on Planck Radiometric detectors like WMAP, but total power Frequency range: 30 – 70 GHz Science Ground Segment in Trieste (INAF-OATs), Italy Planck built to be a component separation machine, LFI provided the low frequency end Hard to disentangle systematics impact on science from LFI But there are interesting exceptions: Large-angle (low-ell) polarization analysis is one Analysis pipelines from the two instruments "almost" independent in terms of data content and methodology Provides nice consistency checks Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 3 Large-angle polarizationChallenging measurement (Jean-Loup Puget's talk) Of some science importance Optical depth t is the worst constrained parameter of the six LCDM (14% relative error in Planck legacy) A full-sky cosmic variance limited measurement of E-mode polarization is still awaited LiteBIRD: will likely provide this “definitive” measurement at large scales It will be crucial to get: Accurate reionization history Neutrino parameters (esp. masses) Large-scale anomalies getting tensor-to-scalar ratio in B-mode reionization peak Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 4 CMB and cosmic reionizationOptical depth to reionization: Second major change of ionization state of H Damps temperature and polarization fluctuations inside horizon Generates new polarization at large angular scales Sunyaev and Chluba 2006 Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 5 Brief history of t measurementsWMAP 9yrs: 𝜏 = ± (Hinshaw+ 2013) Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 6 Brief history of t measurementsWMAP 9yrs: 𝜏 = ± (Hinshaw+ 2013) WMAP 9yrs +

WMAP - The Inflatable Universe - NASA

= ± (Planck 2018 V in pr.) Planck lowTEB (LFI) (Planck 2015 XIII) 𝜏 = ± 0.023 Planck lowTEB (LFI) (Planck 2018 V in pr.) 𝜏 = ± 0.020 Planck lowE (HFI) (Planck XLVI) 𝜏 = ± 0.009 Planck lowE (HFI) (Planck 2018 V in pr.) 𝜏 = ± WMAP LFI HFI Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 12 Foreground mitigation: LFI and HFIMap-based template fitting procedure to mitigate foreground contamination, using low and high channels as tracers of polarized synchrotron and dust. Same methodology for LFI and HFI Template cleaning of maps m = [Q, U] for the channels= 70, 100, 143 GHz 353 GHz 30 GHz 30 GHz: tracer of synchrotron emission 353 GHz: tracer of thermal dust emission Foreground coefficients fitted by minimising, on about 70% of the sky: Where the rescaled covariance matrix is: Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 13 Pixel-based likelihood modellingWhile HFI uses a cross-spectrum based likelihood driven by simulations, LFI uses a map-based formalism Based on cleaned 70 GHz map Statistically efficient Sensitive to full TEB (HFI is EE-only) Provided CMB signal covariance is adapted, can probe non-isotropic models But prone to map-level systematics Requires accurate estimation of the underlying covariance matrix fSKY = 86% fSKY = 62.4% Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 14 Correcting for noise mismatchEstimating the noise covariance matrix is hard: It is a by-product of the map-making scheme, but exact computation is prohibitive Have to resort to approximations. This works reasonably well for LFI (less well for HFI) Still, noise mismatches arise. This can be measured from half-ring half-difference maps, and the noise matrix properly debiased EE noise bias BB noise bias 1s shade HRHD bias Rescaled noise matrix bias Original noise matrix bias L. Colombo Paolo Natoli – LFI Systematics and Impact on Science – LiteBIRD Kick Off Meeting - JAXS 1 July 2019 15 The LFI. WMap 3.0.3 APK download for Android. Create beautiful, minimal, custom map wallpapers and backgrounds with WMap. WMAP PRODUCES NEW RESULTS WMAP 7-year Results Released. The WMAP team has reported the first direct detection of pre-stellar helium, providing an important test of the big bang prediction.

WMAP- Content of the Universe - NASA

Episode of "Star Talk."BibliographyChristopher S. Baird, 'Where is the Edge of the Universe?', West Texas A&M University, (2016) D. Linde, 'Chaotic Inflation', Physics Letters B, Vol 129, issues 3–4 (1983) Pease, 'Brane New World', Nature, 411 (2001) Density', Swinburne Encyclopedia of Astronomy, 'History of Cosmic Structure Formation', Observe the Effect of Dark Matter on the Evolution of the Galaxies', Instituto de Astrofísica de Canarias (2024) 'Universe 101: Will the Universe Expand Forever?' (2024), Schombe, 'Geometry of the Universe', University of Oregon, L. Bennett et al, 'First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Preliminary Maps and Basic Results', The Astrophysical Journal Supplement Series, Vol 148, No. 1 (2003) Collaboration, 'Planck 2018 results VI: Cosmological Parameters', Astronomy & Astrophysics, 641, A6, (2020) Akrami et al, 'Promise of Future Searches for Cosmic Topology', Physical Review Letters, 132 (2024) Wolfram MathWorld, Merali, 'Doughnut-Shaped Universe Bites Back', Nature (2008), Lacièze-Rey and Jean-Pierre Luminet, 'Cosmic Topology', Physics Reports, Vol 254, Issue 3, (1995) J. Cornish et al, 'Constraining the Topology of the Universe', Physical Review Letters, 92 (2004) R. Eskilt, 'Cosmic Topology, Part IIa: Eigenmodes, Correlation Matrices and Detectability of Orientable Euclidean Manifolds', Journal of Cosmology and Astroparticle Physics, Vol 2024 (2024), Guth, 'Inflation', Carnegie Observatories Astrophysics Series, Vol 2: Measuring and Modeling the Universe (2004) Lehners, 'Ekpyrotic and Cyclic Cosmology', Physics Reports, Vol 465, issue 6 (2008) Perlmutter, 'Supernovae, Dark Energy and the Accelerating Universe', Physics Today, Vol 56, Issue 4 (2003) the Universe Last Forever?' CSIRO Parkes Observatory, Caldwell and Marc Kamionkowski, 'The Physics of Cosmic Acceleration' Annual Review of Nuclear and Particle Science, Vol 59 (2009) Wang et al, 'Current Observational Constraints on Cosmic Doomsday', Journal of Cosmology and Astroparticle Physics, Vol 2004 (2004) R. Caldwell, Rahul Dave, Paul J. Steinhardt, 'Cosmological Imprint of an Energy Component with General Equation of State', Physical Review Letters, Vol 80, No 1582 (1998) our Space Forums to keep talking space on the latest missions, night sky and more! And if you have a news tip, correction or comment, let us know at: [email protected] space news, the latest updates on rocket launches, skywatching events and more!Keith