Towards 21-cm intensity mapping at z = 2.28 with uGMRT using the tapered gridded estimator – II. Cross-polarization power spectrum

Abstract

ABSTRACT Neutral hydrogen (H i) 21-cm intensity mapping (IM) offers an efficient technique for mapping the large-scale structures in the Universe. We introduce the ‘Cross’ Tapered Gridded Estimator (Cross TGE), which cross-correlates two cross-polarizations (RR and LL) to estimate the multifrequency angular power spectrum Cℓ(Δν). We expect this to mitigate several effects like noise bias, calibration errors, etc., which affect the ‘Total’ TGE that combines the two polarizations. Here, we apply the Cross TGE on $24.4 \text{-} \rm {MHz}$-bandwidth uGMRT (upgraded Giant Metrewave Radio Telescope) Band 3 data centred at $432.8 \, \rm {MHz}$ aiming H i IM at z = 2.28. The measured Cℓ(Δν) is modelled to yield maximum likelihood estimates of the foregrounds and the spherical power spectrum P(k) in several k bins. Considering the mean squared brightness temperature fluctuations, we report a 2σ upper limit $\Delta _{\mathrm{ UL}}^{2}(k) \le (58.67)^{2} \, {\rm mK}^{2}$ at $k=0.804 \, {\rm Mpc}^{-1}$, which is a factor of 5.2 improvement on our previous estimate based on the Total TGE. Assuming that the H i traces the underlying matter distribution, we have modelled Cℓ(Δν) to simultaneously estimate the foregrounds and $[\Omega _{\rm{ H}\, {\small {I}}} b_{\rm{ H}\, {\small {I}}}]$, where $\Omega _{\rm{ H}\, {\small {I}}}$ and $b_{\rm{ H}\, {\small {I}}}$ are the H i density and linear bias parameters, respectively. We obtain a best-fitting value of $[\Omega _{\rm{ H}\, {\small {I}}}b_{\rm{ H}\, {\small {I}}}]^2 = 7.51\times 10^{-4} \pm 1.47\times 10^{-3}$ that is consistent with noise. Although the 2σ upper limit $[\Omega _{\rm{ H}\, {\small {I}}}b_{\rm{ H}\, {\small {I}}}]_{\mathrm{ UL}} \le 0.061$ is ∼50 times larger than the expected value, this is a considerable improvement over earlier works at this redshift.