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Astrophsyics

PCOS Science Goals

Understand the formation and growth of massive black holes and their role in the evolution of galaxies

The massive black holes (~109 solar masses) ubiquitous in the Universe today are thought to stem from seed black holes formed early in the Reionization era. The origin of these seeds is uncertain. They may have formed from either large stellar mass black holes (~100 solar masses) left over from the first stars or intermediate mass black holes (~104–5 solar masses) formed directly by the collapse of supermassive gas clouds. Whether supermassive black holes grow through mergers or accretion, their host galaxies appear to have co-evolved with them. A strong correlation has become evident between the properties and evolution of galaxies and the growth of their central supermassive black holes. The energetic processes around SMBHs result in huge radiative andmechanical outputs that could potentially have a profound effect on their larger scale environment in galaxies, clusters and the intergalactic medium. But quantitative descriptions of the interaction between massive black hole growth and galaxy growth are lacking. Understanding the formation of galaxies, and their subsequent evolution, will be coupled to intensive study of the evolution of supermassive black holes.



PCOS News

Program News and Announcements

1 June 2018
MMA SAG analyzing the benefits of multimessenger observations made possible by NASA observatories in the 2020 decade and beyond launched! Join the kickoff telecon Friday, 8 June, and sign up today! »  Full details
18 May 2018
Gamma-ray SIG Workshop for Decadal Survey Science White Papers, 23–24 May 2018, George Washington University »  Workshop Sign-up
26 Feb 2018
LISA Preparatory Science is a new program element in ROSES 2018 to provide support for U.S. investigators involved in analysis and interpretation of simulated LISA data. Mandatory NOIs are due 19 Mar 2018 and full proposals are due 14 Jun 2018.

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  • NASA Official: Phil Newman
  • Web Curator: Pat Tyler
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