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47 results for “Astrophysics”
Performance of high-order Godunov-type methods in simulations of astrophysical low Mach number flows
<p>Supplementary materials for the paper "Performance of high-order Godunov-type methods in simulations of astrophysical low Mach number flows". The supplementary materials are split into two .zip archives (KH2D-plots.zip and 3D-TURBULENCE-WAVES-plots.zip) containing figures not shown in the paper.</p>
Observational Astrophysics II at Stockholm University
<p>Observing with the Nordic Optical Telescope has, for many years, been an integral part of the course Observational Astrophysics II (ObsII) offered to masters and Ph.D. students at Stockholm University. I will review the activities related to the course in Stockholm, which also includes observations with the 20m radio telescope at the Onsala Space Observatory.</p>
Chemistry in Astrophysics : Atoms and Molecules
<p>The presentation corresponds to a IUPAC WorldFair Chemistry Webinar. The presentation aims at presenting in 5mn the type of chemistry data that are used in astrophysics, how we annotate those data, how we manipulate those data, what are the challenges and the issues linked to FAIR implementation, and what could be the collaboration with IUPAC. The PDF are uploaded at DOI 10.5281/zenodo.7101252</p> <p>IUPAC : https://iupac.org/worldfair-global-cooperation-on-fair-data-policy-and-practice/ and https://iupac.org/project/2022-012-1-024/</p> <p>VAMDC: https://vamdc.org</p>
Center for Astrophysics Colloquia, 1999
<p>Public lectures given at the Harvard-Smithsonian Center for Astrophysics as part of their CfA Colloquium series. Originally recorded on videotape and audio cassette in 1999 and converted to digital files by EverPresent in 2017. </p>
Center for Astrophysics Colloquia, 1992-1998
<p>Talks given at the Harvard-Smithsonian Center for Astrophysics as part of their CfA Colloquium series. Originally recorded on videotape and audio cassette between 1992 and 1998 and converted to digital files by EverPresent in 2017. </p>
Input files and data for paper "Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation"
<p>This entry contains input files to reproduce the results of the paper:</p> <p>Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation.</p> <p>Each zip archive corresponds to a section of the paper, and includes README files in ASCII format with a description. Raw output data and plotting tools are also provided for some of the results.</p>
Inlists used for studying the astrophysical properties of the Sirius binary system
<p>Using mesa-r23.05.1 a study of the sirius system was performed, both as a non-interacting binary, as well as test suites that take sirius b up until the wd cooling phases in an attempt to better understand the age of the system and the limits of the progenitor mass. Additionally, we hope to put constraints on the temperature, luminosity, and white dwarf mass by comparing this simulation to HST data. Lastly, we use these models to calculate an initial to final mass relation for the system.</p> <p>The inlists used have been included as well as some mod files for different metallicities and initial masses. It is split into three sections pertaining to the binary suite, and single star evolutions where we create carbon and oxygen white dwarfs for lower initial masses of sirius b, as well as a test suite that creates a neon oxygen white dwarf for larger initial masses.</p> <p>The mesasdk version is from July of last year (version 23.7.3)</p>
MOBSTER - At the crossroads of stellar astrophysics in the upper HR Diagram
<p>Contrarily to low-mass stars, in which dynamo-generated surface magnetism is essentially ubiquitous, only about 10% of stars with radiative envelopes (O, B and A) exhibit detectable magnetic fields at their surfaces. Yet, this small magnetic subpopulation includes potential progenitors of exotic astronomical objects, such as high-mass stellar black holes (even at solar metallicity) and magnetars. Therefore, there is a strong motivation to learn more about the as-yet misunderstood formation of these stars, and what is currently lacking is a robust statistical basis to interpret their properties. In this talk, I will briefly review massive star magnetism and some of the critical gaps in knowledge that currently plague their study. I will then discuss the observational limitations that prevent us from learning more, and argue that all-sky broadband photometric missions such as the Transiting Exoplanet Survey Satellite (TESS) offer a valuable indirect method of addressing these limitations. Finally, I will present the MOBSTER (Magnetic OB[A] Stars with TESS: probing their Evolutionary and Rotational properties) collaboration, and highlight some of its early results, as well as offer a glimpse of the road that lies ahead.</p>
Center for Astrophysics Colloquia, 2000-2004
<p>Public talks given at the Harvard-Smithsonian Center for Astrophysics as part of their CfA Colloquium series. Originally recorded on videotape between 2000 and 2004, and converted to .mp4 digital files by EverPresent in 2017. </p>
Center for Astrophysics Colloquia, 2005
<p>Public talks given at the Harvard-Smithsonian Center for Astrophysics as part of their CfA Colloquium series. Originally recorded on videotape in 2005, and converted to .mp4 digital files by EverPresent in 2017. </p>
Center for Astrophysics Colloquia, 2006
<p>Public talks given at the Harvard-Smithsonian Center for Astrophysics as part of their CfA Colloquium series. Originally recorded on videotape in 2006, and converted to .mp4 digital files by EverPresent in 2017. </p>
Modules for Experiments in Stellar Astrophysics (MESA): Time-Dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure
<p>We update the capabilities of the open-knowledge software instrument Modules for Experiments in Stellar Astrophysics (MESA). The new auto_diff module implements automatic differentiation in MESA, an enabling capability that alleviates the need for hard-coded analytic expressions or finite difference approximations. We significantly enhance the treatment of the growth and decay of convection in MESA with a new model for time-dependent convection, which is particularly important during late-stage nuclear burning in massive stars and electron degenerate ignition events. We strengthen MESA's implementation of the equation of state, and we quantify continued improvements to energy accounting and solver accuracy through a discussion of different energy equation features and enhancements. To improve the modeling of stars in MESA we describe key updates to the treatment of stellar atmospheres, molecular opacities, Compton opacities, conductive opacities, element diffusion coefficients, and nuclear reaction rates. We introduce treatments of starspots, an important consideration for low-mass stars, and modifications for superadiabatic convection in radiation-dominated regions. We describe new approaches for increasing the efficiency of calculating monochromatic opacities and radiative levitation, and for increasing the efficiency of evolving the late stages of massive stars with a new operator split nuclear burning mode. We close by discussing major updates to MESA's software infrastructure that enhance source code development and community engagement.</p>
Datasets indexed in Data Citation Index in the Astronomy and Astrophysics category, 2010-2019
<p>The dataset comprises a single list of datasets exported from Data Citation Index (Web of Science, Clarivate Analytics) in the Astronomy and Astrophysics category, for the period 2010 - 2019, allowing to identify annual evolution, countries and institutions with higher productivity, main repositories and hosting platforms, use in publications indexed in Web of Science.</p>
Center for Astrophysics Colloquia, 2007
<p>Public talks given at the Harvard-Smithsonian Center for Astrophysics as part of their CfA Colloquium series. Originally recorded on videotape in 2006, and converted to .mp4 digital files by EverPresent in 2017. </p>
Inferring the Astrophysical Population of Gravitational Wave Sources in the Presence of Noise Transients Data Release
<p>Data release for paper "Inferring the Astrophysical Population of Gravitational Wave Sources in the Presence of Noise Transients."</p> <p>To read in one of the result files and obtain the posterior samples, type</p> <pre><code class="language-python">import bilby result = bilby.core.result.read_in_result(filename="contaminant_0_result.json") samples = result.posterior</code></pre> <p> </p>
Use and Abuse of Astrophysical Models in Gravitational-wave Population Analyses
<p>Accompanying dataset for Cheng et al. 2023</p>
Data release for "Consistent eccentricities for gravitational wave astronomy: Resolving discrepancies between astrophysical simulations and waveform models"
<div> <p>This is a data release to accompany <a href="https://arxiv.org/abs/2402.07892">arXiv:2402.07892</a> "Consistent eccentricities for gravitational wave astronomy: Resolving discrepancies between astrophysical simulations and waveform models".</p> <p>See also <a href="../doi/10.5281/zenodo.10974974">https://zenodo.org/doi/10.5281/zenodo.10974974</a>. Please cite the paper (<a href="https://ui.adsabs.harvard.edu/abs/2024arXiv240207892V/abstract">https://ui.adsabs.harvard.edu/abs/2024arXiv240207892V/abstract</a>) if you use this in a publication or any other scientific work.</p> <p><br>The file can be read in using<br><br>```<br>import pandas</p> <p>data = pandas.read_hdf("CMC_eccentricities_standardized.hdf5")<br>```<br><br>The description of the different keys in the file are as follows:<br><br>- `m1`: source-frame mass of the primary object in the binary in units of Msun<br>- `m2`: source-frame mass of the secondary object in the binary in units of Msun<br>- `chi1`: dimensionless spin of the primary object in the binary<br>- `chi2`: dimensionless spin of the secondary object in the binary<br>- `z`: cosmological redshift<br>- `a0`: Initial separation in AU. This typically corresponds to the stopping criterion in astrophysical simulations.<br>- `e0`: The eccentricity at the initial separation `a0`<br>- `f0`: 22 mode frequency corresponding to the initial separation.<br>- `channel`: Takes values between 1 and 5. <br> - 1: Ejected mergers <br> - 2: In-cluster (two-body) mergers<br> - 3: Binary-Single Encounters<br> - 4: Binary-Binary Encounters<br> - 5: Single-Single Encounters<br>- `cluster_weight`: Weight given to each binary based on cluster properties (mass and metallicity), assuming some initial mass function for the cluster and metallicity evolution as a function of redshift.<br>- `cosmo_weight`: Weight given to each binary based on the redshift, to account for cosmological volume.<br>- `e_W03_*Hz`: Eccentricities extracted from the Wen 2003 prescription at the reference peak frequency specified.<br>- `e_t_2PN_10Hz`: Eccentricities extracted from the prescription in Vijaykumar et. al. 2024 at reference 22 mode frequency of 10 Hz. <br>- `e_t_2PN_Mf_1000HzMsun`: Eccentricities extracted from the prescription in Vijaykumar et. al. 2024 at reference 22 mode frequency corresponding to `M \times f = 1000 Hz Msun`. This ensures that eccentricity is defined at a fixed number of cycles before merger, independent of the cosmological redshift.<strong> We strongly recommend that all eccentricity estimates from astrophysical simulations are quoted at a reference frequency corresponding to fixed `M \times f`.</strong><br>- `total_weight`: `cosmo_weight \times cluster_weight`<br><br><strong>NOTE</strong>: For mergers belonging to `channel=1`, we straightaway set the `e_t_*` estimates to zero. This is because mergers from this channel will not be eccentric at `f>10 Hz`, and due to its large initial separation is computationally intensive to evolve using the PN evolution equations.</p> <p> </p> </div>
High Energy Laboratory Astrophysics using an X-Ray Microcalorimeter with an Electron Beam Ion Trap Project
"Since the summer of 2000 we have successfully deployed a high resolution x-ray microcalorimeter spectrometer, based on the spaceflight XRS instrument, at the Electron Beam Ion Trap (EBIT) facility at the Lawrence Livermore National Laboratory. Over the last decade, this highly successful partnership has made fundamental measurements in laboratory astrophysics including the measurements of the absolute cross sections of all the Fe L shell transitions from Fe XVII to Fe XXIV, line ratios in Fe and Ni L shell transitions, measurements of Fe K shell emission over a wide range of electron energies, and direct measurements of charge exchange emission from highly ionized Fe, O, N, and most recently L shell S, using a variety of donor gases. This work has resulted in the publication of over 30 peer-reviewed articles with many more either submitted or in preparation. The newest addition to the facility, the ECS microcalorimeter spectrometer, developed under this program, has performed flawlessly as a facility-class instrument since 2007. We propose here to continue our highly successful partnership and deploy new technology to resolve lines in the important 1/4 keV band that encompasses the M-shell iron emission and the L shell emission, including charge exchange, of many of the lower-Z elements, such as Si, S, Mg, Ne, Ca, and Ar. We thus propose completing a new spectrometer that will bring substantially improved performance to the laboratory astrophysics program at EBIT and will enable fundamentally new measurements. Thus, in addition to maintaining the current spectrometers, which will begin this work, a significant component of this proposal is the completion of a new spectrometer leveraged off of the substantial progress in high-resolution x-ray detectors developed for the International X-ray Observatory mission. The spectrometer will be composed of a detector system with unparalleled spectral resolution: 2 eV resolution across the 0.05-10 keV band. This will allow
Magnetically-coupled microcalorimeter arrays for x-ray astrophysics with sub-eV spectral resolution and large format capability Project
"We propose to develop a revolutionary x-ray camera for astrophysical imaging spectroscopy. High-resolution x-ray spectroscopy is a powerful tool for studying the evolving universe. Emission line ratios (e.g. within the He-like triplet) provide density and temperature diagnostics. Emission and absorption line energies identify ions and determine their velocities, and the shape of the lines can be used to study turbulence or the relativistic effects of a supermassive black hole. The grating spectrometers on the XMM and Chandra satellites demonstrated the power of high-resolution x-ray spectroscopy for astrophysics, but there remains a need for instrumentation that can provide higher spectral resolution with high throughput in the Fe-K band and that can enable spatial/spectral investigations of extended sources, such as supernova remnants and galaxy clusters. The instrumentation needed is a broad-band imaging spectrometer - basically an x-ray camera that can precisely resolve x-ray energies and fluxes over a large field-of-view. While we do not claim that in 3 years we will have developed such detectors, we advocate developing the technology that has the greatest potential for achieving this. Theoretically, magnetically-coupled microcalorimeters are best equipped to achieve sub-eV energy resolution in very large formats. We propose to build upon the work carried out by our group on metallic magnetic calorimeters (MMC) in the antecedent program. The great promise of MMCs for sub-eV energy resolution has been recognized for years. During our current research program, an accident in detector fabrication produced devices that derived their sensitivity from a different operating principle - the temperature dependence of a superconduc
Superconducting Resonator Spectrometer for Millimeter- and Submillimeter-Wave Astrophysics Project
"We propose to develop a novel ultra-compact spectrograph-on-a-chip for the submillimeter and millimeter waveband. SuperSpec uses planar lithographed superconducting transmission-line filters to sort incident radiation by frequency to an array of direct detectors such as MKIDs. The system is naturally wideband and can be very low loss, enabling background-limited spectroscopy on the ground and in space, as is currently done with a diffraction grating spectrographs. But while moderate-resolution grating systems for the mm and submm bands have sizes measured in tens of centimeters, SuperSpec can have a size measured in millimeters. If successful, SuperSpec will pave the way for a new kind of astronomical instrument for the submm/mm: a 2-D array of hundreds to thousands of individual spectrometers, each simultaneously measuring a separate spectrum. With the possible exception of polarization, such an instrument extracts all available information from the light at a telescope focal plane. SuperSpec thus offers the potential to revolutionize astrophysics in the far-IR through millimeter, an important spectral regime for which the the Astro2010 Decadal Survey made two specific recommendations for this decade: 1) Participate in the Japanese-led SPICA space telescope with a spectrometer instrument such as BLISS, and 2) Construct CCAT and its associated instrumentation. Depending on SPICA's schedule, SuperSpec technology could be injected and would enhance and extend the long-wavelength capability of BLISS or a similar instrument. Whether or not SPICA moves ahead quickly, our demonstration will position SuperSpec to be used in on CCAT and suborbital platforms this decade, paving the way for optimal science return with future NASA-led cryogenic far-IR space missions on the drawing board for the next decade: CALISTO/SAFIR and SPIRIT. SuperSpec is based on propagation on a superconducting transmission line (TL). As radiation propagates along the line, it encounters a seri
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
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Annotated Behaviour and Observability Dataset (ABODe)
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DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.