A comprehensive study of Modulation effects on CMB Polarization

This article does the most general treatment of modulation in Polarization fields. We have considered both linear polarization fields Q and U & also scalar polarization modes E and B. We have shown that any arbitrary modulation in Q and U is allowed but the same can't be done in case of E and B fields. This result also gives a mathematical justification that the masking can only be applied to the Q and U fields and never to E and B fields.Comment: 10 pages, 2 figures, minor corrections, to be submitte

A geometrical interpretation of foreground filters for HI intensity

We give a new geometrical interpretation of HI intensity mapping foreground filters in harmonic space, for both single-dish and interferometer mode surveys. We derive the foreground-filtered HI auto power spectrum and then extend this to the cross-power spectrum of HI with CMB lensing. Foreground filtering leads to a loss of isotropy in Fourier space, resulting in harmonic space non-diagonal correlations, which we show are small compared to the diagonal ones. On large scales, foreground filters lead to a major loss of power in the HI$\,\times\,$CMB lensing correlations.Comment: 10 Pages + 4 Figures + 1 Appendix + References. (Version 2 with slight modifications

Prosthesis for a Case of Subtotal Orbital Exenteration

Aims and objectives: To rehabilitate a patient with subtotal orbital exenteration defect. Case description: A 32 year old male with history of carcinoma of ethmoid, treated surgically with subtotal orbital exenteration presented with a defect communicating with the pharynx. He was rehabilitated with a prosthetic eye. Conclusion: A two piece cast with a removable part containing the defect made it very easy to fabricate the prosthesis. Patient was happy with the appearance and expressed satisfaction.&nbsp

A study of Dipolar Signal in distant Quasars with various observables

We study the signal of anisotropy in AGNs/quasars of CatWISE2020 catalogue using different observables. It has been reported earlier that this data shows a strong signal of dipole anisotropy in the source number counts. We test this claim using two independent data analysis procedures and find our number count dipole consistent with the earlier results. In addition to number counts, we test for the anisotropy signal in two other observables -- mean spectral index $\bar{\alpha}$ and mean flux density $\bar{B}$. We find a dipole signal of considerable strength both in the mean spectral index and the mean flux density. The dipole in mean flux density points towards the galactic center and becomes very weak after imposing a flux cut to remove sources with flux greater than 1 mJy. This can be attributed to the presence of some bright sources. The signal in mean spectral index, however, is relatively stable as a function of both flux and galactic cuts. The dipole in this observable points roughly opposite to the galactic center and hence most likely arises due to galactic bias. Hence, the signal in both the mean spectral index and mean flux density appears to be consistent with isotropy.Comment: 19 pages, 5 figures, 5 tables. All comments are welcome

Superhorizon Perturbations: A Possible Explanation of the Hubble–Lemaître Tension and the Large-scale Anisotropy of the Universe.

Current cosmological observations point to a serious discrepancy between the observed Hubble parameter obtained using direct versus cosmic microwave background radiation measurements. Besides this so-called Hubble– Lemaître tension, we also find considerable evidence in diverse cosmological observables that indicate violation of the cosmological principle. In this paper, we suggest that both these discrepancies are related and can be explained by invoking superhorizon perturbations in the universe. We implement this by considering a single superhorizon mode and showing that it leads to both a dipole in large-scale structures and a shift in the Hubble–Lemaître parameter. Furthermore, the shift is found to be independent of redshift up to a certain distance. This is nicely consistent with the data

Separating Quantum Communication and Approximate Rank

One of the best lower bound methods for the quantum communication complexity of a function H (with or without shared entanglement) is the logarithm of the approximate rank of the communication matrix of H. This measure is essentially equivalent to the approximate gamma-2 norm and generalized discrepancy, and subsumes several other lower bounds. All known lower bounds on quantum communication complexity in the general unbounded-round model can be shown via the logarithm of approximate rank, and it was an open problem to give any separation at all between quantum communication complexity and the logarithm of the approximate rank. In this work we provide the first such separation: We exhibit a total function H with quantum communication complexity almost quadratically larger than the logarithm of its approximate rank. We construct H using the communication lookup function framework of Anshu et al. (FOCS 2016) based on the cheat sheet framework of Aaronson et al. (STOC 2016). From a starting function F, this framework defines a new function H=F_G. Our main technical result is a lower bound on the quantum communication complexity of F_G in terms of the discrepancy of F, which we do via quantum information theoretic arguments. We show the upper bound on the approximate rank of F_G by relating it to the Boolean circuit size of the starting function F