2025MNRAS.536....1H


Query : 2025MNRAS.536....1H

2025MNRAS.536....1H - Mon. Not. R. Astron. Soc., 536, 1-26 (2025/January-1)

Measurements of the thermal and ionization state of the intergalactic medium during the cosmic afternoon.

HU T., KHAIRE V., HENNAWI J.F., TRIPP T.M., ONORBE J., WALTHER M. and LUKIC Z.

Abstract (from CDS):

We perform the first measurement of the thermal and ionization state of the intergalactic medium (IGM) across $0.9 \lt z \lt 1.5$ using 301 Ly $\,\alpha$ absorption lines fitted from 12 archival Hubble Space Telescope Space Telescope Imaging Spectrograph quasar spectra. We employ the machine-learning-based inference method that uses joint Doppler parameter-column density ($b{-}N_{{\rm {H\,{\small I}}}{}}$) distributions obtained from Ly$\,\alpha$ forest decomposition. Our results show that the H I photoionization rates, $\Gamma _{{\rm {H\,{\small I}}}{}}$, agree with recent ultraviolet background synthesis models, with $\log (\Gamma _{{\rm{H\,{\small I}}}}/\text{s}^{-1})={-11.79}^{+0.18}_{-0.15}$, ${-11.98}^{+0.09}_{-0.09}$, and ${-12.32}^{+0.10}_{-0.12}$ at $z=1.4$, 1.2, and 1, respectively. We obtain the IGM temperature at the mean density, $T_0$, and the adiabatic index, $\gamma$, as $[\log (T_0/\text{K}), \gamma ]=$ [${4.13}^{+0.12}_{-0.10}$, ${1.34}^{+0.10}_{-0.15}$], $[{3.79}^{+0.11}_{-0.11}$, ${1.70}^{+0.09}_{-0.09}]$, and $[{4.12}^{+0.15}_{-0.25}$, ${1.34}^{+0.21}_{-0.26}]$ at $z=1.4$, 1.2, and 1. Our measurements of $T_0$ at $z=1.4$ and 1.2 are consistent with the trend predicted from previous $z\lt 3$ temperature measurements and theoretical expectations, where the IGM cools down after He II reionization in the absence of any non-standard heating. However, our $T_0$ measurement at $z=1$ shows unexpectedly high IGM temperature. Given the relatively large uncertainty in these measurements, where $\sigma _{T_0} \sim 5000$ K, mostly emanating from the limited size of our data set, we cannot conclude whether the IGM cools down as expected. Lastly, we generate mock data sets to test the constraining power of future measurement with larger data sets. The results demonstrate that, with redshift path-length $\Delta z \sim 2$ for each redshift bin, three times the current data set, we can constrain the $T_0$ of IGM within 1500 K, which would be sufficient to constrain the IGM thermal history at $z \lt 1.5$ conclusively.

Abstract Copyright: © 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.

Journal keyword(s): intergalactic medium - quasars: absorption lines

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 QSO B0117+2118 QSO 01 20 17.2642359528 +21 33 46.197696168     16.1     ~ 130 0
2 4C -04.06 QSO 02 35 07.3418452008 -04 02 05.317096956   16.61 16.46 16.2   ~ 222 1
3 HE 0515-4414 QSO 05 17 07.6238702856 -44 10 55.579731312 14.74 15.49 15.16     ~ 129 0
4 QSO J1208+4540 QSO 12 08 58.0107013896 +45 40 35.421692952   16.00 15.70     ~ 194 0
5 QSO J1244+1721B QSO 12 44 10.8247089768 +17 21 04.508869464   16.40 16.09     ~ 159 1
6 QSO B1248+401 QSO 12 50 48.3268288080 +39 51 39.458894760   16.62 16.19     ~ 139 0
7 Ton 153 QSO 13 19 56.2320886176 +27 28 08.186323080   16.12 15.98     ~ 156 0
8 LBQS 1435-0134 QSO 14 37 48.2855255136 -01 47 10.816509804   16.11 15.78 16.39   ~ 88 1
9 QSO B1521+1009 QSO 15 24 24.5234088744 +09 58 29.087917572   15.74 16.2     ~ 145 0
10 QSO B1630+3744 QSO 16 32 01.1117931960 +37 37 49.980505332   16.50 16.30     ~ 183 0
11 QSO B1634+7037 QSO 16 34 28.9917184368 +70 31 32.393436960   14.90 14.66     ~ 273 0
12 QSO J1719+4804 Bla 17 19 38.2496454120 +48 04 12.247659408   15.33 14.60 14.25   ~ 186 1

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