Dark energy

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In physical cosmology, astronomy and celestial mechanics, dark energy is a hypothetical form of energy that permeates all of space and tends to increase the rate of expansion of the universe. Dark energy is the most accepted theory to explain recent observations that the universe appears to be expanding at an accelerating rate. In the standard model of cosmology, dark energy currently accounts for 73% of the total mass-energy of the universe. (Wikipedia.org)






Conferences related to Dark energy

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2019 IEEE 46th Photovoltaic Specialists Conference (PVSC)

Photovoltaic materials, devices, systems and related science and technology


2019 IEEE International Conference on Image Processing (ICIP)

The International Conference on Image Processing (ICIP), sponsored by the IEEE SignalProcessing Society, is the premier forum for the presentation of technological advances andresearch results in the fields of theoretical, experimental, and applied image and videoprocessing. ICIP 2019, the 26th in the series that has been held annually since 1994, bringstogether leading engineers and scientists in image and video processing from around the world.


2019 IEEE International Geoscience and Remote Sensing Symposium (IGARSS)

International Geosicence and Remote Sensing Symposium (IGARSS) is the annual conference sponsored by the IEEE Geoscience and Remote Sensing Society (IEEE GRSS), which is also the flagship event of the society. The topics of IGARSS cover a wide variety of the research on the theory, techniques, and applications of remote sensing in geoscience, which includes: the fundamentals of the interactions electromagnetic waves with environment and target to be observed; the techniques and implementation of remote sensing for imaging and sounding; the analysis, processing and information technology of remote sensing data; the applications of remote sensing in different aspects of earth science; the missions and projects of earth observation satellites and airborne and ground based campaigns. The theme of IGARSS 2019 is “Enviroment and Disasters”, and some emphases will be given on related special topics.


2019 IEEE Nuclear Science Symposium and Medical Imaging Conference (NSS/MIC)

This conference is the annual premier meeting on the use of instrumentation in the Nuclear and Medical fields. The meeting has a very long history of providing an exciting venue for scientists to present their latest advances, exchange ideas, renew existing collaboration and form new ones. The NSS portion of the conference is an ideal forum for scientists and engineers in the field of Nuclear Science, radiation instrumentation, software engineering and data acquisition. The MIC is one of the most informative venues on the state-of-the art use of physics, engineering, and mathematics in Nuclear Medicine and related imaging modalities, such as CT and increasingly so MRI, through the development of hybrid devices


2019 IEEE Photonics Conference (IPC)

The IEEE Photonics Conference, previously known as the IEEE LEOS Annual Meeting, offers technical presentations by the world’s leading scientists and engineers in the areas of lasers, optoelectronics, optical fiber networks, and associated lightwave technologies and applications. It also features compelling plenary talks on the industry’s most important issues, weekend events aimed at students and young photonics professionals, and a manufacturer’s exhibition.


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Periodicals related to Dark energy

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Applied Superconductivity, IEEE Transactions on

Contains articles on the applications and other relevant technology. Electronic applications include analog and digital circuits employing thin films and active devices such as Josephson junctions. Power applications include magnet design as well asmotors, generators, and power transmission


Audio, Speech, and Language Processing, IEEE Transactions on

Speech analysis, synthesis, coding speech recognition, speaker recognition, language modeling, speech production and perception, speech enhancement. In audio, transducers, room acoustics, active sound control, human audition, analysis/synthesis/coding of music, and consumer audio. (8) (IEEE Guide for Authors) The scope for the proposed transactions includes SPEECH PROCESSING - Transmission and storage of Speech signals; speech coding; speech enhancement and noise reduction; ...


Computing in Science & Engineering

Physics, medicine, astronomy—these and other hard sciences share a common need for efficient algorithms, system software, and computer architecture to address large computational problems. And yet, useful advances in computational techniques that could benefit many researchers are rarely shared. To meet that need, Computing in Science & Engineering (CiSE) presents scientific and computational contributions in a clear and accessible format. ...


Dielectrics and Electrical Insulation, IEEE Transactions on

Electrical insulation common to the design and construction of components and equipment for use in electric and electronic circuits and distribution systems at all frequencies.


Electron Device Letters, IEEE

Publishes original and significant contributions relating to the theory, design, performance and reliability of electron devices, including optoelectronic devices, nanoscale devices, solid-state devices, integrated electronic devices, energy sources, power devices, displays, sensors, electro-mechanical devices, quantum devices and electron tubes.


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Xplore Articles related to Dark energy

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Towards the most robust way of assigning numerical degrees to ordered labels, with possible applications to dark matter and dark energy

2016 Annual Conference of the North American Fuzzy Information Processing Society (NAFIPS), 2016

Experts often describe their estimates by using words from natural language, i.e., in effect, sorted labels. To efficiently represent the corresponding expert knowledge in a computer-based system, we need to translate these labels into a computer-understandable language, i.e., into numbers. There are many ways to translate labels into numbers. In this paper, we propose to select a translation which is ...


Technologies for the SNAP - SuperNova acceleration probe

2002 IEEE Nuclear Science Symposium Conference Record, 2002

The SuperNova/Acceleration Probe (SNAP) is a space-based experiment to measure the expansion history of the Universe, and is currently in the R&D phase. The experiment is motivated by the recent discovery that the expansion of the Universe is accelerating. Cosmologists believe that some unknown energy, called dark energy, permeates all of space and drives the acceleration. The SNAP conceptual design ...


A Short-Term Measure of Dark Energy in Sparse Atomic Estimations

2007 Conference Record of the Forty-First Asilomar Conference on Signals, Systems and Computers, 2007

A sparse atomic estimation involves finding a representation of a signal that uses terms with finite support drawn from an overcomplete dictionary. These terms can constructively and destructively interfere with each other in the reconstruction, and some may even disappear. For this reason, we refer to the interference between atoms in the sparse estimation as "dark energy" (DE). Building upon ...


Galaxy evolution simulation on basement of linguo-combinatorial approach with uncertainty

2016 XIX IEEE International Conference on Soft Computing and Measurements (SCM), 2016

The galaxy is seen as a complex cyber-physical system with a wide variety of elements. In the course of its development the galaxy interacts with the environment consisting of other galaxies and larger structures. In addition, the Galaxy is under the influence of external and internal control, which is realized through a hypothetical control unit. As a management tool is ...


Physical Insight of Space-Time and Modeling of Space-Time Dipoles, Gravity Waves and Gravitons: A Micro Space Antenna to Detect the Nature of Gravity Field

2006 International Conference on Advances in Space Technologies, 2006

This paper presents an interpretation of space-time and modeling of space-time tri-dipoles, gravity field waves, and gravity carriers (the gravitons). The approach in this proposed paper is based on geometric modeling of space-time as a phase fluid and the momentum generated by the time. In this modeling, the time is considered as a mechanical variable along with other variables and ...


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Educational Resources on Dark energy

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IEEE-USA E-Books

  • Towards the most robust way of assigning numerical degrees to ordered labels, with possible applications to dark matter and dark energy

    Experts often describe their estimates by using words from natural language, i.e., in effect, sorted labels. To efficiently represent the corresponding expert knowledge in a computer-based system, we need to translate these labels into a computer-understandable language, i.e., into numbers. There are many ways to translate labels into numbers. In this paper, we propose to select a translation which is the most robust, i.e., which preserves the order between the corresponding numbers under the largest possible deviations from the original translation. The resulting formulas are in good accordance with the translation coming from the Laplace's principle of sufficient reason, and - somewhat surprisingly - with the current estimates of the proportion of dark matter and dark energy in our Universe.

  • Technologies for the SNAP - SuperNova acceleration probe

    The SuperNova/Acceleration Probe (SNAP) is a space-based experiment to measure the expansion history of the Universe, and is currently in the R&D phase. The experiment is motivated by the recent discovery that the expansion of the Universe is accelerating. Cosmologists believe that some unknown energy, called dark energy, permeates all of space and drives the acceleration. The SNAP conceptual design consists of a wide-field (approximately one degree) diffraction limited telescope with a 2-meter primary. Its half-billion-pixel imaging system is comprised of state-of-the-art visible and infrared sensors sharing a large focal plane. SNAP will use thousands of supernovae as cosmic markers of the scale of the universe over time and thus construct a history of the universe's growth. Looking back over 10 billion years at the expansion history of the universe, SNAP will be able to distinguish among different theories of dark energy. In this presentation the development challenges, new technologies, and instrumentation will be described. This work is funded by the DOE Office of Science.

  • A Short-Term Measure of Dark Energy in Sparse Atomic Estimations

    A sparse atomic estimation involves finding a representation of a signal that uses terms with finite support drawn from an overcomplete dictionary. These terms can constructively and destructively interfere with each other in the reconstruction, and some may even disappear. For this reason, we refer to the interference between atoms in the sparse estimation as "dark energy" (DE). Building upon our previous work, we present a short-term measure of DE (STDE) that can be used to examine the distribution of interference in the signal estimation. We present results for several signals, and discuss some applications of this measure.

  • Galaxy evolution simulation on basement of linguo-combinatorial approach with uncertainty

    The galaxy is seen as a complex cyber-physical system with a wide variety of elements. In the course of its development the galaxy interacts with the environment consisting of other galaxies and larger structures. In addition, the Galaxy is under the influence of external and internal control, which is realized through a hypothetical control unit. As a management tool is considered manipulation of arbitrary coefficients in the structure equivalent equations, the imposition and lifting of restrictions on the variables of the system, the union in collective systems et al., which eventually forms the life cycles of galaxies. Galaxies are complex self-organizing systems so they are subject to identified patterns of development of complex systems [2, 5, 6].

  • Physical Insight of Space-Time and Modeling of Space-Time Dipoles, Gravity Waves and Gravitons: A Micro Space Antenna to Detect the Nature of Gravity Field

    This paper presents an interpretation of space-time and modeling of space-time tri-dipoles, gravity field waves, and gravity carriers (the gravitons). The approach in this proposed paper is based on geometric modeling of space-time as a phase fluid and the momentum generated by the time. In this modeling, the time is considered as a mechanical variable along with other variables and treated on an equal footing. This model suggests that the space-time has a polarity and is composed of dipoles which are responsible for forming the orbits and storing the space-time energy-momentum. The tri-dipoles can be unified into a solo space-time dipole with an angle of 45 degrees. Such a result shows that the space-time is not void, on the contrary, it is full of conserved and dynamic energy-momentum structure. Furthermore, the gravity field waves is modeled and assumed to be carried by the gravitons which move in the speed of light. The equivalent mass of the graviton is found to be equal to 0.707 of the equivalent mass of the light carrier (the photon). Such a result indicates that the lightest particle (up to the author's knowledge) in the nature is the graviton and has an equivalent mass equals to 2.5119 times 10-52 kg. Moreover, a micro space antenna is proposed to detect the gravity waves. Finally, simulation results are demonstrated to verify the analytical results.

  • Image processing challenges in weak gravitational lensing

    The field of weak gravitational lensing, which measures the basic properties of the Universe by studying the way that light from distant galaxies is perturbed as it travels towards us, is a very active field in astronomy. This short article presents a broad overview of the field, including some of the important questions that cosmologists are trying to address, such as understanding the nature of dark energy and dark matter. To do this, there is an increasing feeling within the weak lensing community that other disciplines, such as computer science, machine learning, signal processing and image processing, have the expertise that would bring enormous advantage if channelled into lensing studies. To illustrate this point, the article below outlines some of the key steps in a weak lensing analysis chain. The challenges are distinct at each step, but each could benefit from ideas developed in the signal processing domain. This article also gives a brief overview of current and planned lensing experiments that will soon bring about an influx of data sets that are substantially larger than those analysed to date. It is, therefore, inevitable that current techniques are likely to be insufficient, thus leading to an exciting era where new methods will become crucial for the continued success of the field.

  • Overview of the Canadian hydrogen intensity mapping experiment (CHIME)

    The Baryon Acoustic Oscillations (BAO) which occurred in the early universe have left a distinctive imprint in subsequent large-scale structure, thereby providing a standard, cosmological ruler. Measurements of the apparent diameter of BAO over an appreciable period of cosmic time thus reveal the expansion history of the universe and can provide valuable new data for constraining models of dark energy. Intensity mapping of hydrogen's 21 cm line over a broad range in frequencies is an exciting new prospect for determining the large scale, three-dimensional structure of the universe in pursuit of this goal.

  • Feedback calibration of the MOFF correlator

    Summary form only given. Proposed radio arrays to probe the Epoch of Reionization and dark energy through HI 21 cm measurements will require compact arrays with tens of thousands of antenna elements. The computation requirements of traditional XF or FX correlators for these arrays would easily reach the peta-flop regime, making the correlator a dominant cost. The MOFF (Modular Optimal Frequency Fourier) correlator has been developed as an alternative method for fully correlating these large numbers of elements. The MOFF shares the computational advantages of direct imaging or FFT correlators while making no constraints on the antenna arrangement or type. A major concern for this new correlator design is the calibration. In traditional data processing, self-cal or related algorithms use visibilities to determine the calibration during postprocessing. The MOFF correlator does not form visibilities, but rather forms the image directly. In addition the crucial software holography step of the MOFF requires the antenna power patterns to be known in real time to use as the gridding kernel. Fortunately it is possible to determine the calibration by correlating pixels of the electric field image with the antenna signal - feeding the correlator output back to the input. Through simulations we demonstrate this feedback calibration method for several realistic example arrays in the presence of noise and extraneous sources. We show that the calibration converges as expected for compact large-N arrays characteristic of future 21 cm cosmology experiments, allowing the correlator to form high quality dirty electric field images at a fraction of the computational cost for traditional correlator methods.

  • The Hydrogen Intensity and Real-Time Analysis Experiment

    The Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX [1], Table 1) is an intensity mapping project to be co-located with the Square Kilometer Array in South Africa. By making use of an 1024 element interferometer of low- cost 6m dishes arranged in a compact grid, HIRAX will map the low-frequency southern sky from 400-800 MHz, probing neutral hydrogen emission over the redshift range of 0.8-2.5. The principle goal of this survey is to accurately measure the observed baryon acoustic oscillation feature imprinted on large- scale structure through HI intensity mapping (See e.g. [2]). As this epoch spans the onset of the transition from matter-dominated to dark energy- dominated expansion, HIRAX will provide highly competitive constraints on cosmological parameters, particularly the equation of state of dark energy. Forecasts of these contraints using the methodology of [3] are shown in Figure 1. The final survey will map 15,000 square degrees of the southern sky, overlapping contemporary and forthcoming surveys such as those from the Large Synoptic Survey Telescope and the Dark Energy Survey, as well as ground based Cosmic Microwave Background surveys. HIRAX will therefore enable a wide range of HI cross-correlation studies with external large-scale structure probes. Additionally, HIRAX will be a powerful instrument for detecting and monitoring radio transients such as Fast Radio Bursts and pulsars.

  • A Xe detector for WIMP search

    For the ever-challenging dark matter direct detection, we have developed an optimized detector for over a decade. The ZEPLIN II detector with liquid Xe as a target material is now under construction at UCLA, which will be installed in the 1100-m deep UK Boulby salt mine in early 2002. Two-phase (liquid and gas) Xe scheme has been shown to be very promising for a superior dark matter particle identification. We present Monte Carlo simulation studies of light collection for the ZEPLIN II central detector. The simulation code includes absorption, reflection, and refraction at the interface between liquid and gas. The response of photopeaks to each energy level from 5-keV to 100-keV with the 5-keV bin is linear without any significant statistical fluctuations. The modified light collection efficiency (f/sub mod/ = recorded photoelectrons/incident photons) is uniform throughout the entire range of gamma energies in this study. We also discuss the need for signal amplification and a large-scale detector in order to cover the comprehensive SUSY-WIMP region with the lowest possible energy threshold.



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