Upcoming and Previous Seminars (Past months or Previous years)

Note that if the talk's pdf or ppt is available after the talk, you can get it by clicking on the talk title.

Physics/Astronomy C290C Cosmology and Cosmology-BCCP Seminar
The Physics/Astronomy C290C series consists of the Cosmology-BCCP LBNL-Physics-Astronomy Cosmology seminars held Tuesdays 1:10-2:00 pm .
in room 131 Campbell Hall or on ZOOM. It will vary from week to week. Please don't bring your lunch (it is hard to keep this room clean; this is a change).
Please mail Joanne Cohn to add to this list or to suggest speakers.

This seminar is intended for BCCP members and Berkeley graduate students pursuing their dissertation research in cosmology. Other LBL, Berkeley Astronomy and and Berkeley Physics Department members are welcome. If the talk is on ZOOM, members of the Berkeley Astronomy/Physics and Cosmology communities can email Joanne Cohn for information.

Speaker/Visitor Info is here.





BOSS and Nyx
(Image by C. Stark)

Note that there are also other talks which might be of interest, including:


August 2021
Aug 31, Tuesday
1:10 pm (BCCP/Cosmology)
One minute intros
131 Campbell Hall


September 2021
Sep 7, Tuesday
1:10 pm (BCCP/Cosmology)
Xiaohan Wu, Harvard
131 Campbell Hall
Potential new insights about reionization from the cosmic microwave background(?) and the Lyman alpha forest
Reionization of the intergalactic medium remains one of the most mysterious questions in the research of cosmology. While the first generation of stars (Pop-III) likely ionize the universe at 1-10% level at z>15, the second generation of stars are believed to drive the bulk of reionization at z<12 and complete the reionization process in a patchy pattern. In this talk I will discuss potential new insights into Pop-III reionization at z>15 using the large-scale polarization of the CMB and imprints of patchy reionization at z<12 on the post-reionization Lyman-alpha forest. I will show that although future CMB surveys will be able to measure the large-scale CMB EE power spectrum at higher signal-to-noise and constrain the optical depth at z>15 much better than Planck, the detailed shape of the EE power spectrum is unlikely to add in more constraining power on our understanding of Pop-III star formation. On the other hand, temperature fluctuations owing to patchy reionization likely induce excess power on the large scales of the Lyman-alpha forest flux power spectrum, indicating a potential future observational constraint on the patchiness of reionization. We also found negligible impact of temperature fluctuations on the small-scale shape of the forest flux power spectrum, implying that patchy reionization is unlikely to bias current IGM temperature measurements and WDM/FDM constraints using the forest flux power spectrum.
Sep 14, Tuesday
1:10 pm (BCCP/Cosmology)
Sihao Cheng, JHU
131 Campbell Hall, speaker via ZOOM
The scattering transform in cosmology, or, a CNN without training
Patterns and non-Gaussian textures are ubiquitous in astronomical data but challenging to quantify. I will present a new powerful statistical tool, called the “scattering transform”. It borrows ideas from convolutional neural nets (CNNs) while retaining the advantages of traditional statistics. As an example, I will demonstrate its application to weak lensing cosmology, where it outperforms classic statistics and is on a par with CNNs. I will also show interesting interpretations of the scattering statistics. I argue that the scattering transform provides a powerful new approach in cosmology and beyond.
Sep 16, Thursday
12:40 pm (Astronomy Colloquium)
Steven Furlanetto, UCLA
131 Campbell Hall
Hints About the Earliest Galaxies
The Cosmic Dawn - the era when the first stars and galaxies formed - is one of the frontiers of extragalactic astrophysics. In this talk, I will describe how surprisingly simple models of galaxy evolution provide insight into the basic processes driving these galaxies (and others) while simultaneously highlighting the many ways in which these early, tiny sources may differ from their descendants and ways in which we may observe their properties. In particular, I will show how measurements of the intergalactic medium already provide important insights into these galaxies. Finally, I will describe how a host of new telescopes, including the James Webb Space Telescope and the Hydrogen Epoch of Reionization Array, will provide insights into this era.
Sep 21, Tuesday
1:10 pm (BCCP/Cosmology)
Oliver Philcox, Princeton
131 Campbell Hall
Large Scale Structure Beyond the 2-Point Function
According to the standard paradigm, the distribution of matter in the early Universe obeys Gaussian statistics, and is thus fully described by its power spectrum. Thanks to gravitational evolution, the current Universe is far from Gaussian, yet large scale structure (LSS) analysis is almost always restricted to the two-point function. This begs the question: what information lies in higher-order statistics?
In this talk, I will discuss the benefits of non-Gaussian correlation functions, both in the context of tightening constraints on ΛCDM parameters, and probing new physics in the early and late Universe. A number of technical difficulties must be overcome before the full power of the statistics can be realized: these include the modeling of window functions for Fourier-space statistics, and efficient estimation of the real-space correlators themselves. I will present practical methods that can obviate these difficulties, such as quadratic algorithms for measuring N-point correlation functions, regardless of N. Such techniques will facilitate a number of exciting tests of the cosmological model.
Sep 28, Tuesday
1:10 pm (BCCP/Cosmology)
Huangyu Xiao, Washington
131 Campbell Hall
Axion Dark Matter in the Sky
The axion, a well-motivated particle from the theoretical point of view, is also a viable dark matter candidate. If the initial axion field is not homogenized by inflation, it can naturally imprint large isocurvature fluctuations at extremely small scales and form substructures with subplanetary masses. There have been proposals that appear capable of detecting substructures with such masses, which open the window to detect axions indirectly.
In this talk, I will discuss the evolution of axion minihalos based on N-body simulations. The present-day abundance and density profiles of axion minihalos in the Universe are obtained by extrapolating the simulation results analytically, suggesting that axion minihalos are detectable in future observations.

October 2021
Oct 5, Tuesday
1:10 pm (BCCP/Cosmology)
Boryana Hadzhiyska, Harvard
131 Campbell Hall, speaker via ZOOM

Oct 12, Tuesday
1:10 pm (BCCP/Cosmology)
Deaglan Barnett, Oxford
131 Campbell Hall, speaker via ZOOM

Oct 19, Tuesday
1:10 pm (BCCP/Cosmology)
Abhishek Maniyar, NYU
131 Campbell Hall, speaker via ZOOM

Oct 26, Tuesday
1:10 pm (BCCP/Cosmology)
Shivam Pandey, Penn
131 Campbell Hall, speaker via ZOOM


November 2021
Nov 2, Tuesday
1:10 pm (BCCP/Cosmology)
,
131 Campbell Hall

Nov 5, Friday
12 noon (LBL INPA)
Guochao (Jason) Sun, Caltech
LBL 50-5132 and ZOOM

Nov 9, Tuesday
1:10 pm (BCCP/Cosmology)
Huanqing Chen, Chicago
131 Campbell Hall

Nov 16, Tuesday
1:10 pm (BCCP/Cosmology)
,
131 Campbell Hall

Nov 30, Tuesday
1:10 pm (BCCP/Cosmology)
,
131 Campbell Hall






Past Months



June 2021
June 3, Thursday
4 pm (LBL RPM)
Julien Guy, LBL
The Dark Energy Spectroscopic Instrument (DESI): start of the five year survey.
The Dark Energy Spectroscopic Instrument (DESI) started its main survey on May 14. Over 5 years, it will measure the spectra and redshifts of about 30 millions galaxies and quasars over 14,000 square degrees. This 3D map will be used to reconstruct the expansion history of the universe up to z=3.5, and measure the growth rate of structure in the redshift range 0.7-1.6 with unequaled precision (< 1.5% per redshift bin of 0.1). The start of the survey marks the end of a successful survey validation period during which more than one million cosmological redshifts were measured. This data set, along with many commissioning studies, has demonstrated the project meets its science requirements written many years ago. I will present how we have validated the target selection, the instrument performance, the spectroscopic pipeline, operations, and the survey strategy.
June 8, Tuesday
1:10 pm (BCCP/Cosmology)--postponed April talk
Alexandra Amon, SLAC/Stanford
The Dark Energy Survey Year 3 Results from Weak Lensing and Clustering
I will present the cosmological weak lensing and clustering results from the Dark Energy Survey (DES) using its first three years of data taken using the Dark Energy Camera on the 4m Blanco telescope at CTIO. This analysis spans the full DES footprint, more than 4000 sq. deg. of sky, with the final shear catalogue containing more than 100 million galaxies, constituting the most powerful weak lensing dataset to date. The comparison of DES cosmological constraints on dark matter and dark energy from WL and LSS in the low-redshift Universe to CMB constraints provides an unprecedented test of the standard cosmological model, across high and low redshift. These DES results from the low-redshift Universe are consistent with those from the cosmic microwave background (CMB) and support the standard cosmological model, LCDM. I will mention the main challenges that our analysis is susceptible to, and the summarise the DES-Year 3 approach to account for these and deliver robust cosmological constraints.

July 2021
July 22, Thursday
4 pm (RPM LBL)
Anna Porredon, OSU By ZOOM
Dark Energy Survey Year 3 Results from Galaxy Clustering and Weak Lensing
The cosmological information extracted from photometric surveys is more robust when multiple probes of the large-scale structure of the universe are used. Two of the most sensitive probes are galaxy clustering and weak lensing. I will present cosmological results from the Dark Energy Survey first three years of observations combining those two probes, using an optimized lens sample of 11 million galaxies for the clustering measurements. The shear catalog used for weak lensing contains more than 100 million galaxies, constituting the largest dataset to date of this kind. I will show how we optimized the selection of this lens sample in terms of the forecasted cosmological constraints. Last, I will explain how we validated the analysis to deliver robust cosmological constraints.


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