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1. MHD Turbulence in Core-Collapse Supernovae
Authors: Philipp Moesta (pmoesta@berkeley.edu), Christian Ott (cott@tapir.caltech.edu)
Paper URL: http://www.nature.com/nature/journal/v528/n7582/full/nature15755.html
Paper DOI: dx.doi.org/10.1038/nature15755
Data URL: https://go-bluewaters.ncsa.illinois.edu/globus-app/transfer?origin_id=8fc2bb2a-9712-11e5-9991-22000b96db58&origin_path=%2F
Data DOI: ??
Size: 90 TB
Code & Tools: Einstein Toolkit, see this page for list of available vis tools for this format
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Citation: Mösta, P., Ott, C. D., Radice, D., Roberts, L. F., Schnetter, E., & Haas, R. (2015). A large-scale dynamo and magnetoturbulence in rapidly rotating core-collapse supernovae. Nature, 528(7582), 376–379. http://dx.doi.org/10.1038/nature15755
Paper URL: http://www.nature.com/nature/journal/v528/n7582/full/nature15755.html
Paper DOI: dx.doi.org/10.1038/nature15755
Data Citation: ??
Data URL: https://go-bluewaters.ncsa.illinois.edu/globus-app/transfer?origin_id=8fc2bb2a-9712-11e5-9991-22000b96db58&origin_path=%2F
Data DOI: http://dx.doi.org/doi:10.21970/N9RP4P
Data Location: Blue Waters (/projects/sciteam/jr6/share/)
Size: 205 TB
Code & Tools: Einstein Toolkit, see this page for list of available vis tools for this format
Jupyter Notebook: ??
The dataset is a series of snapshots in time from 4 ultra-high resolution 3D magnetohydrodynamic simulations of rapidly rotating stellar core-collapse. The 3D domain for all simulations is in quadrant symmetry with dimensions 0 < x,y < 66.5km, -66.5km < z < 66.5km. It covers the newly born neutron star and it's shear layer with a uniform resolution. The simulations were performed at 4 different resolutions [500m,200m,100m,50m]. There are a total of 350 snapshots over the simulated time of 10ms with 10 variables capturing the state of the magnetofluid. For the highest resolution simulation, a single 3D output variable for a single time is ~26GB in size. The entire dataset is ~205TB in size. The highest resolution simulation used 60 million CPU hours on BlueWaters. The dataset may be used to analyze the turbulent state of the fluid and perform analysis going beyond the published results in Nature doi:10.1038/nature15755.
2. Probing the Ultraviolet Luminosity Function of the Earliest Galaxies with the Renaissance Simulations
Authors: Brian O'Shea (oshea@msu.edu), John Wise, Hao Xu, Michael Norman
Paper Citation: Norman, B. W. O. and J. H. W. and H. X. and M. L. (2015). Probing the Ultraviolet Luminosity Function of the Earliest Galaxies with the Renaissance Simulations. The Astrophysical Journal Letters, 807(1), L12.
Paper URL: http://iopscience.iop.org/article/10.1088/2041-8205/807/1/L12/meta;jsessionid=40CF566DDA56AD74A99FE108F573F445.c1.iopscience.cld.iop.org
Paper DOI: dx.doi.org/10.1088/2041-8205/807/1/L12
Data URL:
Data Citation: ??
Data DOI: ??
Size: 89 TB
Code & Tools: Enzo
Jupyter Notebook: http://yt-project.org/docs/dev/cookbook/cosmological_analysis.html
In this paper, we present the first results from the Renaissance Simulations, a suite of extremely high-resolution and physics-rich AMR calculations of high-redshift galaxy formation performed on the Blue Waters supercomputer. These simulations contain hundreds of well-resolved galaxies at z ~ 25–8, and make several novel, testable predictions. Most critically, we show that the ultraviolet luminosity function of our simulated galaxies is consistent with observations of high-z galaxy populations at the bright end of the luminosity function (M1600 ⩽ -17), but at lower luminosities is essentially flat rather than rising steeply, as has been inferred by Schechter function fits to high-z observations, and has a clearly defined lower limit in UV luminosity. This behavior of the luminosity function is due to two factors: (i) the strong dependence of the star formation rate (SFR) on halo virial mass in our simulated galaxy population, with lower-mass halos having systematically lower SFRs and thus lower UV luminosities; and (ii) the fact that halos with virial masses below ~2 x 10^8 M do not universally contain stars, with the fraction of halos containing stars dropping to zero at ~7 x 10^6 M . Finally, we show that the brightest of our simulated galaxies may be visible to current and future ultra-deep space-based surveys, particularly if lensed regions are chosen for observation.
3. Dark Sky Simulation
Authors: Michael Warren, Alexandar Friedland, Daniel Holz, Samuel Skillman, Paul Sutter, Matthew Turk (mjturk@illinois.edu), Risa Wechsler
Paper Citation: Warren, M. S., Friedland, A., Holz, D. E., Skillman, S. W., Sutter, P. M., Turk, M. J., & Wechsler, R. H. (2014). Dark Sky Simulations Collaboration. Zenodo. https://doi.org/10.5281/zenodo.10777
Paper URL: https://zenodo.org/record/10777#.V_VvKtwcK1M, https://arxiv.org/abs/1407.2600
Paper DOI: http://dx.doi.org/10.5281/zenodo.10777
Data Citation: Warren, M. S., Friedland, A., Holz, D. E., Skillman, S. W., Sutter, P. M., Turk, M. J., & Wechsler, R. H. (2014). Dark Sky Simulations Collaboration. Zenodo. https://
2. Probing the Ultraviolet Luminosity Function of the Earliest Galaxies with the Renaissance Simulations
Authors: Brian O'Shea (oshea@msu.edu), John Wise, Hao Xu, Michael Norman
Paper URL: http://iopscience.iop.org/article/10.1088/2041-8205/807/1/L12/meta;jsessionid=40CF566DDA56AD74A99FE108F573F445.c1.iopscience.cld.iop.org
Paper DOI: dx.doi.org/10.1088/2041-8205/807/1/L12
Data URL:
Data DOI: ??
Size: 89 TB
Code & Tools: Enzo
In this paper, we present the first results from the Renaissance Simulations, a suite of extremely high-resolution and physics-rich AMR calculations of high-redshift galaxy formation performed on the Blue Waters supercomputer. These simulations contain hundreds of well-resolved galaxies at z ~ 25–8, and make several novel, testable predictions. Most critically, we show that the ultraviolet luminosity function of our simulated galaxies is consistent with observations of high-z galaxy populations at the bright end of the luminosity function (M1600 ⩽ -17), but at lower luminosities is essentially flat rather than rising steeply, as has been inferred by Schechter function fits to high-z observations, and has a clearly defined lower limit in UV luminosity. This behavior of the luminosity function is due to two factors: (i) the strong dependence of the star formation rate (SFR) on halo virial mass in our simulated galaxy population, with lower-mass halos having systematically lower SFRs and thus lower UV luminosities; and (ii) the fact that halos with virial masses below ~2 x 10^8 M do not universally contain stars, with the fraction of halos containing stars dropping to zero at ~7 x 10^6 M . Finally, we show that the brightest of our simulated galaxies may be visible to current and future ultra-deep space-based surveys, particularly if lensed regions are chosen for observation.
3. Dark Sky Simulation
Authors: Michael Warren, Alexandar Friedland, Daniel Holz, Samuel Skillman, Paul Sutter, Matthew Turk (mjturk@illinois.edu), Risa Wechsler
Paper URL: https://zenodo.org/record/10777#.V_VvKtwcK1M, https://arxiv.org/abs/1407.2600
Paper DOI: http://dx.doi.org/10.5281/zenodo.10777
Data URL:
Data DOI: ?? https://doi.org/10.5281/zenodo.10777 (Although this is classified as a report in Zenodo, the authors intended this to be the DOI for the dataset)
Size: 31 TB
Code & Tools& Tools: https://bitbucket.org/darkskysims/darksky_tour/
Jupyter Notebook: https://bitbucket.org/darkskysims/darksky_tour/girder.hub.yt/#user/570bd8fc2f2b14000176822c/folder/5820b9c09ea95c00014c71a1
The cosmological N-body simulation designed to provide a quantitative and accessible model of the evolution of the large-scale Universe.
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- Transfer (if necessary) each dataset to existing cloud architecture - in progress?
- Spin up a Docker-enabled host and mount nearby datasets (NFS, direct mount, etc.) - in progress?
- Federated model
- Using docker-compose, bring up provided girder-dev environment on each Docker host - pending
- Develop the "resolver" REST API to to
- Receive site metadata - in progressin - done => POST to /datasets
- Delegate tmpnb requests to remote Girder instances using existing /notebook API endpoint - done => POST to /resolve/:id
- Add authentication:
- We simply need to collect an e-mail address (identity) to run things on their behalf
- Could possibly import existing users from Girder using their API? probably not, due to security
- We could callback to Girder when sites push their metadata (assuming this can be done as Girder comes online)
- Extend UI to list off collections in connected Girder instance - doneish... very primitive, but styling it is trivial
- Add a "Launch Notebook" button next to each dataset where no notebook is runningdataset where no notebook is running - doneish... prototype is working, once real metadata is in place this is trivial
- Add a "Stop Notebook" button next to each dataset where a notebook has been launched - TBD
- this is a slightly tougher problem, as we now need to call out to every Girder's /notebook endpoint
- Modify girder-dev to POST site metadata on startup (feder8)- in progress
- Run a centralized resolver instance on Nebula for the purposes of the demo
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Here is my PPT version of my napkin sketch for the SC demo. Also context on where the demo product fits in the story. Comments, please!
Presentation v1
Please give me your feedback! Graphics executed to the edge of my abilities and patience. See presentation notes for script written so far.