Table of Contents |
---|
Goals
- NDS Share(d) datasets: present online the below datasets so that users can find and obtain them. Highlight DOI's of both paper and dataset.
- Provide analysis tools along with each dataset (ideally deployable data-side to avoid having to copy the data).
Presentation Logistics
- Booth demos: NCSA, SDSC, ...
- SCinet late breaking news talk
Technology
- Globus Publish (https://github.com/globus/globus-publish-dspace)
- Modified DSpace with Globus Authentication, Groups, and Transfer
- Example instance: Materials Data Facility
- Requires a Globus endpoint on each resource (not available for Swift stores, e.g. SDSC Cloud)
- Analysis currently not supported
- yt Hub
- Built on Girder for data presentation, Jupyter for analysis, ...
- Example instance: yt Hub (https://docs.hub.yt/girder.html)
- Example skinned instance: Galaxy Cluster Merger Catalog
- Would need allocation on BlueWaters to run tools there. May need to move Moesta dataset elsewhere...
- ...
Datasets
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: ??
...
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. ?? - Matthew Turk can you fill this in?
Authors: ??
Paper URL: ??
Paper DOI: ??
Data URL: ??
Data DOI: ??
Size: ??
Code & Tools: ??
??
Description?
4. ...