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University of Cambridge > Talks.cam > Galaxies Discussion Group > Probing the Post to Early Stage of Cosmic Reionization using JWST and Subaru
Probing the Post to Early Stage of Cosmic Reionization using JWST and SubaruAdd to your list(s) Download to your calendar using vCal
If you have a question about this talk, please contact Sandro Tacchella. Lya damping wing absorption measurement is a useful tool to constrain the key cosmic reionization parameters including neutral hydrogen fraction xHI, but the measurement had been limited only to the small number of extremely UV-continuum bright sources such as QSO /GRBs. For the first time, we constrain xHI and ionized bubble radii Rb by measuring Lya damping wing absorptions using bright galaxy spectra detected in JWST observations. We combine JWST /NIRSpec spectra taken by CEERS , GO-1433, DDT -2750, and JADES programs, and obtain 27 bright (M_UV<-18.5) UV-continuum galaxies at 7 < z < 12. We construct 4 composite spectra binned by redshift and find the clear transition from sharp to soft spectral break towards high redshift at the restframe 1216 Å suggesting the increase of Lyα damping wing absorption. We estimate Lya damping wing absorption in the galaxy spectra with a state-of-art stellar population synthesis model including Lya emission and host HI absorptions. Assuming the standard inside-out reionization picture having an ionized bubble with Rb around a galaxy in the intergalactic medium of xHI, we obtain xHI (Rb) values monotonically increasing (decreasing) trend from xHI = 0.54 to 0.95 (log Rb = 1.89 to -0.68 comoving Mpc) at redshift 7.12 to 9.91. We also estimate xHI at z 5.7 Subaru LAE catalog consists of 8182 galaxies, and we estimate xHI from Lya luminosity function and LAE clustering properties using a prediction based on semi-numerical simulation 21cmFAST. The redshift evolution of xHI between z=6 to 12 inferred from JWST and Subaru result indicate a very rapid reionization scenario progressing mainly at z=7-8. This talk is part of the Galaxies Discussion Group series. This talk is included in these lists:
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