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- Hagentoft, Carl-Eric, 1958, et al.
(författare)
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Annex 55, Reliability of Energy Efficient Building Retrofitting - Probability Assessment of Performance and Cost, (RAP-RETRO): Probabilistic Tools
- 2015
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Rapport (övrigt vetenskapligt/konstnärligt)abstract
- The International Energy AgencyThe International Energy Agency (IEA) was established in 1974 within the framework of the Organisation forEconomic Co-operation and Development (OECD) to implement an international energy programme. A basicaim of the IEA is to foster international co-operation among the 28 IEA participating countries and to increaseenergy security through energy research, development and demonstration in the fields of technologies forenergy efficiency and renewable energy sources.The IEA Energy in Buildings and Communities ProgrammeThe IEA co-ordinates research and development in a number of areas related to energy. The mission of theEnergy in Buildings and Communities (EBC) Programme is to develop and facilitate the integration oftechnologies and processes for energy efficiency and conservation into healthy, low emission, andsustainable buildings and communities, through innovation and research. (Until March 2013, the IEA-EBCProgramme was known as the Energy in Buildings and Community Systems Programme, ECBCS.)The research and development strategies of the IEA-EBC Programme are derived from research drivers,national programmes within IEA countries, and the IEA Future Buildings Forum Think Tank Workshops. Theresearch and development (R&D) strategies of IEA-EBC aim to exploit technological opportunities to saveenergy in the buildings sector, and to remove technical obstacles to market penetration of new energy efficienttechnologies. The R&D strategies apply to residential, commercial, office buildings and community systems,and will impact the building industry in five focus areas for R&D activities: Integrated planning and building design Building energy systems Building envelope Community scale methods Real building energy use
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| 3. |
- Rey, Martin P., et al.
(författare)
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EDGE – Dark matter or astrophysics? Breaking dark matter heating degeneracies with H I rotation in faint dwarf galaxies
- 2024
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Ingår i: Monthly Notices of the Royal Astronomical Society. - 0035-8711. ; 529:3, s. 2379-2398
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Tidskriftsartikel (refereegranskat)abstract
- Low-mass dwarf galaxies are expected to reside within dark matter haloes that have a pristine, ‘cuspy’ density profile within their stellar half-light radii. This is because they form too few stars to significantly drive dark matter heating through supernova-driven outflows. Here, we study such simulated faint systems (104 ≤ M* ≤ 2 × 106 M) drawn from high-resolution (3 pc) cosmological simulations from the ‘Engineering Dwarf Galaxies at the Edge of galaxy formation’ (EDGE) project. We confirm that these objects have steep and rising inner dark matter density profiles at z = 0, little affected by galaxy formation effects. But five dwarf galaxies from the suite also showcase a detectable H I reservoir (MH I ≈ 105 − 106 M), analogous to the observed population of faint, H I-bearing dwarf galaxies. These reservoirs exhibit episodes of ordered rotation, opening windows for rotation curve analysis. Within actively star-forming dwarfs, stellar feedback easily disrupts the tenuous H I discs (vφ,g ≈ 10 km s−1), making rotation short-lived (≪ 150 Myr) and more challenging to interpret for dark matter inferences. In contrast, we highlight a long-lived (≥ 500 Myr) and easy-to-interpret H I rotation curve extending to ≈ 2 r1/2,3D in a quiescent dwarf, that has not formed new stars since z = 4. This stable gas disc is supported by an oblate dark matter halo shape that drives high-angular momentum gas flows. Our results strongly motivate further searches for H I in rotation curves in the observed population of H I-bearing low-mass dwarfs, that provide a key regime to disentangle the respective roles of dark matter microphysics and galaxy formation effects in driving dark matter heating.
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| 4. |
- Rey, Martin P., et al.
(författare)
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EDGE : What shapes the relationship between H i and stellar observables in faint dwarf galaxies?
- 2022
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Ingår i: Monthly Notices of the Royal Astronomical Society. - : Oxford University Press (OUP). - 0035-8711 .- 1365-2966. ; 511:4, s. 5672-5681
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Tidskriftsartikel (refereegranskat)abstract
- We show how the interplay between feedback and mass-growth histories introduces scatter in the relationship between stellar and neutral gas properties of field faint dwarf galaxies (M∗ 106, M⊙). Across a suite of cosmological, high-resolution zoomed simulations, we find that dwarf galaxies of stellar masses 105 ≤ M∗ ≤ 106, M⊙ are bimodal in their cold gas content, being either H i-rich or H i-deficient. This bimodality is generated through the coupling between (i) the modulation of H i contents by the background of ultraviolet radiation (UVB) at late times and (ii) the significant scatter in the stellar-to-halo mass relationship induced by reionization. Furthermore, our H i-rich dwarfs exhibit disturbed and time-variable neutral gas distributions primarily due to stellar feedback. Over the last four billion years, we observe order-of-magnitude changes around the median M H,\small I, factor-of-a-few variations in H i spatial extents, and spatial offsets between H i and stellar components regularly exceeding the galaxies' optical sizes. Time variability introduces further scatter in the M∗-M H, small I relation and affects a galaxy's detectability in H i at any given time. These effects will need to be accounted for when interpreting observations of the population of faint, H i-bearing dwarfs by the combination of optical and radio wide, deep surveys.
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