Session H12: Mini-Symposium: Physics of the Cosmos

Physics of the Cosmos and PhysPAG Overview

The Physics of the Cosmos (PhysCOS) Program lies at the intersection of physics and astronomy. Its purpose is to explore some of the most fundamental questions regarding the physical forces and laws of the universe: the validity of Einstein's General Theory of Relativity and the nature of spacetime, the behavior of matter and energy in extreme environments, the cosmological parameters governing inflation and the evolution of the universe, and the nature of dark matter and dark energy. 

Located at the Goddard Space Flight Center, the PhysCOS Program Office supports, tracks, and studies a suite of science missions and enabling technologies that focus on specific aspects of these topics.

Please refer to the PhysCOS webpage for additional details for this session [https://pcos.gsfc.nasa.gov/physpag/meetings/APS_2024/APS2024-agenda.php]   

The Gravitational Wave Science Interest Group of the NASA Physics of the Cosmos Program

Among the Science Interest Groups (SIGs) of the NASA Physics of the Cosmos Program Analysis Group (PhysPAG) is the GW Science Interest Group (GW-SIG). One of the key goals of the GW-SIG is to advocate for the brand-new field of gravitational wave astronomy, build a vibrant community of gravitational wave astronomers, and promote the discovery space in this new field to the wider scientific community and to the public. In this talk, we summarize some of the most exciting recent scientific results in the field of GW physics and astronomy, provide an update on the GW-SIG activities and plans, and solicit community feedback on future GW-SIG activities.   

Community efforts in gamma-ray astrophysics: Insights from the GR SIG

The NASA Gamma Ray Science Interest Group (GR SIG) serves as a central hub and platform for the hard X-ray and gamma-ray astrophysics communities. It convenes monthly virtual meetings to discuss recent scientific results, technological progress, and current and future missions. Additionally, the group curates a list of technological requirements for future hard X-ray and gamma-ray missions and gathers community feedback to formulate recommendations for supporting the unique needs of these scientific communities, encompassing organizational aspects and scientific funding.

This presentation will provide an overview of the current activities of the GR SIG, highlighting the recent launch of the Future Innovations in Gamma-ray Science Analysis Group (FIG SAG) taskforce. We will also outline various avenues and opportunities for community involvement, empowering individuals to contribute actively to the evolution of hard X-ray and gamma-ray astrophysics.   

Future Innovations in Gamma Rays: A New Science Analysis Group

The Future Innovations in Gamma rays Science Analysis Group (FIGSAG) began in January, to study science justifications and associated mission requirements for future space-based gamma-ray facilities. The chairs have begun facilitating conversations among those with a stake in the future of gamma-ray missions, especially high-energy and multimessenger astrophysicists. At the conclusion of the project, we will author a report for consideration by NASA, which we hope will lay the scientific groundwork for discussions about investments in gamma-ray technologies and facilities in the next Astrophysics Decadal. You are invited to learn more and join the conversation.   

The Probe of Inflation and Cosmic Origins - Capabilities of a Next Generation $1B CMB Space Mission

We describe the capabilities of the Probe of Inflation and Cosmic Origins (PICO), a prototype for a next generation $1B-scale space mission. We present quantitative constraints on inflation in the presence of a wide range of foreground models. We demonstrate the value of a broad frequency coverage between 20 and 800 GHz, and of large sky coverage, which enables critical systematic cross-checks.   

Future CMB observations from space: CORE, PRISM and Voyage 2050 proposals and science programs

I will review the scientific rationale and mission design drivers for CORE, PRISM, and potential future science topics for missions to be launched in the context of the Voyage 2050 ESA programme.   

Complementing future CMB ground-based data sets with balloon observations

Future CMB ground-based missions, like CMB-S4, have ambitious plans of constraining models of inflation by measuring the tensor-to-scalar ratio, r, with an uncertainty of 5×10^-4. A key challenge for measuring r is separating the CMB and Galactic foregrounds. Specifically, polarized dust emission is the major contaminant, and it is best characterized by observations at higher frequencies in the range of 300 to 3000 GHz. The CMB-S4 frequency bands extend up to 270 GHz. We explore the added value of complementary balloon observations at higher frequencies to assist with foreground cleaning for CMB-S4. We describe two possible instruments: an imager with frequency coverage from 150 to 360 GHz and a spectrometer with frequency coverage from 100 to 800 GHz. In both cases, we demonstrate the impact of these complementary balloon observations on the uncertainty and bias in the measurement of r when added to the CMB-S4 dataset.