DiRAC Institute in GeekWire

How number crunchers could help crack the cosmological mystery of dark energy

BY ALAN BOYLE on May 15, 2018 at 9:08 pm

Big data just might give astronomers a better grip on the answer to one of the biggest questions in physics: Exactly what’s behind the mysterious acceleration in the expansion rate of the universe, also known as dark energy?

Read the full article here.

Visitors: Petar Zečević

April 15th-May 5th, 2018. 

Petar Zečević is a PhD student from University of Zagreb, Croatia. He has been working in the software industry for more than 15 years, as a full-stack developer, consultant, analyst, and team leader. Petar is the author of Spark in Action book (Manning, September 2016). He also gives talks on Apache Spark, organizes monthly Apache Spark Zagreb meetups, and has several Apache Spark projects behind him.


DIRAC Institute Open House, May 14th, 2018

We would like to thank all of you who attended the lecture by Nobel Laureate Saul Perlmutter to celebrate the opening of our DiRAC Institute.
It was a wonderful and inspiring evening that demonstrated how our understanding of the universe might change as a result of the data from a new generation of telescopes and satellites that will come on line over the next few years. We were very happy that you could join us and share this excitement and hope that, over the coming months, you will follow the work and discoveries that will come from the DiRAC Institute.
If you would like to hear about some of the research going on at DiRAC Institute you can watch our team describe some of their research highlights or check the news on our site. We would also welcome your support of the students and researchers at the DiRAC Institute.

Thank you again for participating in the inaugural DIRAC Institute Open House!

2011 Nobel Laureate, Dr. Saul Perlmutter inspired us by his lecture
“What We Learn When We Learn the Universe is Accelerating”.

In his talk, Dr. Perlmutter described how supernova observations led to the Nobel-prize winning discovery of dark energy and the acceleration of the universe, and how modern methods for collecting data are changing the ways we ask questions, conduct research, and make discoveries in astronomy and astrophysics. 
About the Speaker 

Saul Perlmutter is a 2011 Nobel Laureate, sharing the prize in Physics for the discovery of the accelerating expansion of the Universe. He is a professor of physics at the University of California, Berkeley, where he holds the Franklin W. and Karen Weber Dabby Chair, and a senior scientist at Lawrence Berkeley National Laboratory. He is the leader of the international Supernova Cosmology Project, and director of both the Berkeley Institute for Data Science and the Berkeley Center for Cosmological Physics. His undergraduate degree was from Harvard and his PhD from UC Berkeley. In addition to other awards and honors, he is a member of the National Academy of Sciences and the American Academy of Arts and Sciences and a fellow of the American Physical Society and the American Association for the Advancement of Science. Perlmutter has also written popular articles, and has appeared in numerous PBS, Discovery Channel, and BBC documentaries. His interest in teaching scientific approaches to problem-solving for non-scientists led to Berkeley courses on Sense and Sensibility and Science and Physics & Music.

What We Learn When We Learn that the Universe is Accelerating 

The 1998 discovery that the universe’s expansion is accelerating was not only unexpected, but also led to the idea of a previously-unknown “dark energy” forming almost three-quarters of the “stuff” that makes up the universe. How was this discovery made? How did new ways of thinking about the collection of data make this discovery possible? What has been the progress since in understanding this dark energy, the accelerating universe, and potentially the fate of the universe? In this illuminating and provoking talk Dr. Saul Perlmutter, Nobel Laureate, will describe the observations that led to the discovery of “dark energy” and how our ability to collect data at ever increasing rates is changing the way we undertake science and and the discoveries we can make. 


2018-02-20 Seminar: Jean-Charles Cuillandre, CEA-Saclay/Observatoire de Paris

When: February 20, 2018 @ 12:30 – 1:30pm
Where: PAB, B305, 3rd floor

The challenge of the distributed Euclid survey:

The ESA Euclid space mission core science goals rely on complementary deep ground-based surveys covering both the northern and southern galactic caps. This talk will present an overview of the space survey design and the current status of the ground-based survey campaign, with a focus on its first element, CFHT’s Canada-France Imaging Survey.


Visitors: Eddie Schlafly

Brown Bag on February 14-16, 2018.

Eddie is a Hubble Fellow working at Lawrence Berkeley National Laboratory, trying to understand the structure of the Galaxy, and especially its dust, using observations of stars. His most recent work uses the DECam instrument on the Blanco 4-m telescope to image the southern Galactic plane, to understand its stars, gas, and dust. He also uses APOGEE spectroscopy to understand how dust properties vary, and the PS1 survey to infer the three-dimensional structure of the dust in the Milky Way.

Visitors: Naoki Yoshida

Seminar on Feb 12, 2018.

Naoki Yoshida is a Professor of Astrophysics in the Department of Physics at the University of Tokyo, as well as a  Senior Research Scientist at the Kavli Institute for the Physics and Mathematics of the Universe.

2018-02-14 Brown Bag: Eddie Schlafly, Lawrence Berkeley National Laboratory

When: February 14, 2018 @ 2:00-3:00pm 
Where: PAB, WRF Data Science Studio, Seminar Room, 6th floor

The DECam Plane Survey: Optical Photometry of Two Billion Objects in the Southern Galactic PlaneThe DECam

Plane Survey is a five-band optical and near-infrared survey of the southern Galactic plane with the Dark Energy Camera at Cerro Tololo. The survey is designed to reach past the main-sequence turn-off of old populations at the distance of the Galactic center through a reddening E(B − V ) of 1.5 mag. Typical single-exposure depths are 23.7, 22.8, 22.3, 21.9, and 21.0 mag (AB) in the grizY bands, with seeing around 1″. The footprint covers the Galactic plane with |b| < 4 degrees, 5 degrees > l > −120 degrees. The survey pipeline simultaneously solves for the positions and fluxes of tens of thousands of sources in each image, delivering positions and fluxes of roughly two billion stars with better than 10 mmag precision. Most of these objects are highly reddened and deep in the Galactic disk, probing the structure and properties of the Milky Way and its interstellar medium. The fully processed images and derived catalogs are publicly available.

Read more about Eddie here.

2018-02-12 Lunch Seminar: Naoki Yoshida, Kavli IPMU, University of Tokyo

When: February 12, 2018 @ 12:30 – 1:30pm 
Where: PAB, WRF Data Science Studio, 6th floor

Big Data Cosmology with Subaru HSC Survey

Subaru HSC is ongoing and is planned to survey a total of ~1200 square degrees by 2019. We have already conducted 180-nights observation, and collected about 65% of the total. We use the data to detect and classify distant supernovae and to reconstruct the large-scale cosmic density field in 3D. To this end, we have developed a new “machine” adopting AUC boosting and pAUC methods, as well as commonly used Random Forest and DNN. The machine detected ~1500 supernovae including faint ones down to 26-th magnitude. We have also developed a multi-label classifier  (Type Ia, Ibc, IIP, IIN, IIL) and used it successfully to extract a few tens high-redshift Type Ia supernovae, which have been sent for spectroscopic observations by HST. For cosmological parameter estimation, we have developed a fast, machine-learned “emulator” that calculates statistical quantities of weak lensing. We run 200 supercomputer simulations of cosmic structure formation and use the outputs to train and develop the emulator (effectively a python package). Cross-validation study shows that the emulator predicts the gravitational lensing effects on the matter distribution and on the clustering of galaxies with an accuracy of 3 percent.  We will integrate the emulator in our Markov-Chain Monte-Carlo program to infer the main cosmological parameters such as the matter density and the density fluctuation amplitude. Finally, we are developing a CNN that can calculate basic strong lensing parameters such as Einstein radius and lens ellipticity from observed multi-band images. I discuss the future prospects for LSST.



2018-02-05: Seminar: Melissa Graham

When: February 5, 2018 @ 12:30-1:30pm 
Where: PAB, WRF Data Science Studio, 6th floor

Mini-Workshop: Alert Stream Filters for Your ZTF Science Goals

The seminar will start with a brief presentation of some of the main ZTF science drivers that require Alert Stream filters, and then we will add our own ZTF science goals and, as a group, create a Filter Wish List. Another brief presentation of the current Alert Packet contents will be provided, with a focus on the schema keys that are most likely to be used in a filter. We will then break into small groups and attempt to write conceptual-level algorithms for the filters on our wish list, and collect these into a single document. We will finish with a group discussion of the main problems/questions faced in our filter-writing attempts. The compiled Filter Wish List document and common issues faced will be used in the near future by the local UW ZTF alert stream team. If you’re not yet sure what kind of time-domain science you might do with ZTF, please do join us — hopefully one of the topics will be inspiring! Should you want to review the basics of the ZTF survey prior to this workshop, see Bellm et al. (2014): http://adsabs.harvard.edu/abs/2014htu..conf…27B

Visitors: Andreas A. Berlind

February 1-2, 2018.

Seminar on February 2, 2018 @ 1:00pm

I am currently an associate professor in the Astronomy Group in the Physics and Astronomy Department at Vanderbilt University. My research interests lie in the areas of large-scale structure and galaxy formation, as well as ultra-high energy cosmic rays. I completed my Ph.D. degree in Astronomy at the Ohio State University, and my A.B. degree inAstrophysical Sciences at Princeton University. Before that, I lived in Athens, Greece where I attended Athens College.