%0 Generic %1 vasiliev2019probing %A Vasiliev, Evgenii O. %A Sethi, Shiv K. %A Shchekinov, Yuri A. %D 2019 %K tifr %T Probing primordial $^3$He from hyperfine line afterglows around supercritical black holes %U http://arxiv.org/abs/1910.08622 %X We consider the possibility of the detection of $^3$HeII hyperfine line (rest frequency, $8.67 \, GHz$) emission from ionized zones around accreting black holes (BHs) formed at high redshifts, $z=15--30$. We show that the brightness temperature in 8.67GHz line increases and reaches a peak value after the accretion onto the BH exhausts and HeIII recombines into HeII. This period of brightening last up to 40~million years. We find that during this period the maximum brightness temperature reaches $0.2--0.5 \mu$K, depending on the epoch when such a black hole starts growing. The maximum angular size of the region emitting in the hyperfine line is around $0.5'$. The flux from such a region ($0.3 \, nJy$) is too small to be detected by SKA1-MID. The RMS of the collective flux from many emitting regions from a volume bounded by the synthesized beam and the band-width of SKA1-MID might reach 100~nJy, which is potentially detectable by SKA1-MID.

@misc{vasiliev2019probing, abstract = {We consider the possibility of the detection of $^3$HeII hyperfine line (rest frequency, $8.67 \, \rm GHz$) emission from ionized zones around accreting black holes (BHs) formed at high redshifts, $z=15\hbox{--}30$. We show that the brightness temperature in 8.67GHz line increases and reaches a peak value after the accretion onto the BH exhausts and HeIII recombines into HeII. This period of brightening last up to 40~million years. We find that during this period the maximum brightness temperature reaches $\simeq 0.2\hbox{--}0.5 \mu$K, depending on the epoch when such a black hole starts growing. The maximum angular size of the region emitting in the hyperfine line is around $0.5'$. The flux from such a region ($\simeq 0.3 \, \rm nJy$) is too small to be detected by SKA1-MID. The RMS of the collective flux from many emitting regions from a volume bounded by the synthesized beam and the band-width of SKA1-MID might reach 100~nJy, which is potentially detectable by SKA1-MID.}, added-at = {2019-10-22T07:54:11.000+0200}, author = {Vasiliev, Evgenii O. and Sethi, Shiv K. and Shchekinov, Yuri A.}, biburl = {https://www.bibsonomy.org/bibtex/2193f13fa4bd19eb51bb5c175427042e5/citekhatri}, description = {Probing primordial $^3$He from hyperfine line afterglows around supercritical black holes}, interhash = {d3d4f07b3848befe5a7f0dc9c75d85f8}, intrahash = {193f13fa4bd19eb51bb5c175427042e5}, keywords = {tifr}, note = {cite arxiv:1910.08622Comment: 7 pages, 2 figures, accepted in MNRAS}, timestamp = {2019-10-22T07:54:11.000+0200}, title = {Probing primordial $^3$He from hyperfine line afterglows around supercritical black holes}, url = {http://arxiv.org/abs/1910.08622}, year = 2019 }