Abstract
Many present-day galaxies are known to harbor supermassive, ≥106 M☉, black holes. These central black holes must have grown through accretion from less massive seeds in the early universe. The molecules CO and H2 can be used to trace this young population of accreting massive black holes through the X-ray irradiation of ambient gas. The X-rays drive a low-metallicity ion-molecule chemistry that leads to the formation and excitation of CO and H2 in 100 K 15 and H2 S(0) and S(1) emission is found that allows one to constrain ambient conditions. Comparable line strengths cannot be produced by FUV or cosmic-ray irradiation. Weak, but perhaps detectable, H+3 (2, 2) → (1, 1) emission is found and discussed. The models predict that black hole masses larger than 105 M☉ can be detected with ALMA, over a redshift range of 5-20, provided that the black holes radiate close to Eddington.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
