arXiv subjects

Yi-Chao Li

Publications and source records attributed to Yi-Chao Li.

14 recordsLinked to original sources

arXiv2021

HI constraints from the cross-correlation of eBOSS galaxies and Green Bank Telescope intensity maps

We present the joint analysis of Neutral Hydrogen (HI) Intensity Mapping observations with three galaxy samples: the Luminous Red Galaxy (LRG) and Emission Line Galaxy (ELG) samples from the eBOSS survey, and the WiggleZ Dark Energy Survey sample. The HI intensity maps are Green Bank Telescope observations of the redshifted 21cm emission on 100deg2 covering the redshift range $0.6<z<1.0$. We process the data by separating and removing the foregrounds with FastICA, and construct a transfer function to correct for the effects of foreground removal on the HI signal. We cross-correlate the cleaned HI data with the galaxy samples and study the overall amplitude as well as the scale-dependence of the power spectrum. We also qualitatively compare our findings with the predictions by a semi-analytic galaxy evolution simulation. The cross-correlations constrain the quantity $Ω_{HI} b_{HI} r_{{HI},{opt}}$ at an effective scale $k_{eff}$, where $Ω_{HI}$ is the HI density fraction, $b_{HI}$ is the HI bias, and $r_{{HI},{opt}}$ the galaxy-hydrogen correlation coefficient, which is dependent on the HI content of the optical galaxy sample. At $k_{eff}=0.31 \, h/{Mpc}$ we find $Ω_{HI} b_{HI} r_{{HI},{Wig}} = [0.58 \pm 0.09 \, {(stat) \pm 0.05 \, {(sys)}}] \times 10^{-3}$ for GBT-WiggleZ, $Ω_{HI} b_{HI} r_{HI,{ELG}} = [0.40 \pm 0.09 \, {(stat) \pm 0.04 \, {(sys)}}] \times 10^{-3}$ for GBT-ELG, and $Ω_{HI} b_{HI} r_{{HI},{LRG}} = [0.35 \pm 0.08 \, {(stat) \pm 0.03 \, {(sys)}}] \times 10^{-3}$ for GBT-LRG, at $z\simeq 0.8$. We also report results at $k_{eff}=0.24 \, h/{Mpc}$ and $k_{eff}=0.48 \, h/{Mpc}$. With little information on HI parameters beyond our local Universe, these are amongst the most precise constraints on neutral hydrogen density fluctuations in an underexplored redshift range.

astro-ph.CO↗

arXiv2020

Reconstructing the radial velocity profile of cosmic voids with kinematic Sunyaev-Zeldovich Effect

We develop an estimator to extract the mean radial velocity profile of cosmic voids via the kinematic Sunyaev-Zeldovich effect of pairs of galaxies surrounding them. The estimator is tested with simulated pure kSZ map and void catalogue data from the same simulation. The results show that the recovered signal could be attenuated by low angular resolution of the map or large aperture photometry filter radius size, but the mean radial velocity profile can be fully recovered with our estimator. By applying the estimator to the Planck 2D-ILC CMB map, with galaxy and void catalogues from BOSS DR12, we find that the estimated void velocity profile is $3.31σ$ apart from null detection for for voids with continuously rising density profiles asymptoting to the mean density; and $1.75σ$ for voids with positive density contrast shell surrounded. By fitting the reconstructed data to the theoretical profile, we find the reduced $χ^{2}$ to be $1.19$ and $0.62$ for the two types of void, respectively, indicating a good fit of the model to the data. We then forecast the detectability of the radial velocity profile of cosmic voids with future CMB surveys, including SPT-3G, AdvACT, and Simons Observatory. We find that the contamination effect from CMB residuals is negligible with survey area over $2,000~{\rm deg}^2$, especially with aperture photometry size less than $1\,{\rm arcmin}$. But the effect from instrumental noise is non-negligible. For future SPT-3G, AdvACT and Simons Observatory, the detection is potentially achievable from $3σ$ to $10σ$ C.L., depending on specific instrumental parameters. This opens a new window of probing dynamics of the cosmic structures from the kinematic Sunyaev-Zeldovich effect.

astro-ph.CO↗

arXiv2019

Forecasts of cosmological constraints from HI intensity mapping with FAST, BINGO & SKA-I

We forecast the cosmological constraints of the neutral hydrogen (HI) intensity mapping (IM) technique with radio telescopes by assuming 1-year of observational time. The current and future radio telescopes we consider here are FAST (Five hundred meter Aperture Spherical Telescope), BINGO (Baryon acoustic oscillations In Neutral Gas Observations), and SKA-I (Square Kilometre Array phase I) single-dish experiment. We also forecast the combined constraints of the three radio telescopes with Planck. We find that, the $1 σ$ errors of $(w_{0}, w_{a})$ for BINGO, FAST and SKA-I with respect to the fiducial values are respectively, $(0.9293, 3.5792), (0.4083, 1.5878), (0.3158, 0.4622)$. This is equivalent to $(56.04\%, 55.64\%)$ and $(66.02\%, 87.09\%)$ improvements in constraining $(w_{0}, w_{a})$ for FAST and SKA-I relative to BINGO. Simulations further show that SKA-I will put more stringent constraints than both FAST and BINGO when each of the experiment is combined with Planck measurement. For the $9$ cosmological parameters in consideration, we find that, there is a trade-off between SKA-I and FAST in constraining cosmological parameters, with each experiment being more superior in constraining a particular set of parameters.

astro-ph.CO↗

arXiv2019

Searching for HI imprints in cosmic web filaments with 21-cm intensity mapping

We investigate the possible presence of neutral hydrogen (HI) in intergalactic filaments at very low redshift ($z\sim 0.08$), by stacking a set of 274,712 2dFGRS galaxy pairs over 21-cm maps obtained with dedicated observations conducted with the Parkes radio telescope, over a total sky area of approximately 1,300 square degrees covering two patches in the northern and in the southern Galactic hemispheres. The stacking is performed by combining local maps in which each pair is brought to a common reference frame; the resulting signal from the edge galaxies is then removed to extract the filament residual emission. We repeat the analysis on maps cleaned removing either 10 or 20 foreground modes in a principal component analysis. Our study does not reveal any clear HI excess in the considered filaments in either case; we determine upper limits on the total filament HI brightness temperature at $T_{\rm b} \lesssim 10.3 \,μ\text{K}$ for the 10-mode and at $T_{\rm b} \lesssim 4.8 \,μ\text{K}$ for the 20-mode removed maps at the 95% confidence level. These estimates translate into upper limits for the local filament HI density parameter, $Ω_{\rm HI}^{\rm (f)} \lesssim 7.0\times10^{-5}$ and $Ω_{\rm HI}^{\rm (f)} \lesssim 3.2\times10^{-5}$ respectively, and for the HI column density, $N_{\rm HI} \lesssim 4.6\times10^{15}\,\text{cm}^{-2}$ and $N_{\rm HI} \lesssim 2.1\times10^{15}\,\text{cm}^{-2}$ respectively. These column density constraints are consistent with previous detections of HI in the warm-hot intergalactic medium obtained observing broad Ly $α$ absorption systems. The present work shows for the first time how such constraints can be achieved using the stacking of galaxy pairs on 21-cm maps.

astro-ph.CO↗

arXiv2018

Qubit gates with simultaneous transport in double quantum dots

A single electron spin in a double quantum dot in a magnetic field is considered in terms of a four-level system. By describing the electron motion between the potential minima by spin-conserving tunneling and spin flip caused by a spin-orbit coupling, we inversely engineer faster-than-adiabatic state manipulation operations based on the geometry of four-dimensional (4D) rotations. In particular, we show how to transport a qubit among the quantum dots performing simultaneously a required spin rotation.

quant-ph↗

arXiv2018

Measurement of the pairwise kinematic Sunyaev-Zeldovich effect with Planck and BOSS data

We present a new measurement of the kinetic Sunyaev-Zeldovich effect (kSZ) using Planck cosmic microwave background (CMB) and Baryon Oscillation Spectroscopic Survey (BOSS) data. Using the `LowZ North/South' galaxy catalogue from BOSS DR12, and the group catalogue from BOSS DR13, we evaluate the mean pairwise kSZ temperature associated with BOSS galaxies. We construct a `Central Galaxies Catalogue' (CGC) which consists of isolated galaxies from the original BOSS data set, and apply the aperture photometry (AP) filter to suppress the primary CMB contribution. By constructing a halo model to fit the pairwise kSZ function, we constrain the mean optical depth to be $\barτ=(0.53\pm0.32)\times10^{-4}(1.65\,σ)$ for `LowZ North CGC', $\barτ=(0.30\pm0.57)\times10^{-4}(0.53\,σ)$ for `LowZ South CGC', and $\barτ=(0.43\pm0.28)\times10^{-4}(1.53\,σ)$ for `DR13 Group'. In addition, we vary the radius of the AP filter and find that the AP size of $7\,{\rm arcmin}$ gives the maximum detection for $\barτ$. We also investigate the dependence of the signal with halo mass and find $\barτ=(0.32\pm0.36)\times10^{-4}(0.8\,σ)$ and $\barτ=(0.67\pm0.46)\times10^{-4}(1.4\,σ)$ for `DR13 Group' with halo mass restricted to, respectively, less and greater than its median halo mass, $10^{12}\, h^{-1}{\rm M}_{\odot}$. For the `LowZ North CGC' sample restricted to $M_{\rm h} \gtrsim 10^{14}\, h^{-1}{\rm M}_\odot$ there is no detection of the kSZ signal because these high mass halos are associated with the high-redshift galaxies of the LowZ North catalogue, which have limited contribution to the pairwise kSZ signals.

astro-ph.CO↗

arXiv2017

Constraints on Primordial non-Gaussianity from Future HI Intensity Mapping Experiments

The primordial non-Gaussianity induces scale-dependent bias of the \hi with respect to the underlying dark matter, which exhibits features on the very large scales of the 21-cm power spectrum potentially observable with \hi intensity mapping observations. We forecast the prospective constraints on the four fundamental shapes of primordial non-Gaussianity (local, equilateral, orthogonal, and enfolded), with the current and future \hi intensity mapping experiments, BINGO, FAST, and SKA-I. With the current configuration of the experiments and assumed one-year observation time, we find that the SKA-I will provide tighter constraints on the local shape of primoridal non-Gaussianity than Planck. The results are $(σ_{f^{\rm local}_{\rm NL}},σ_{f^{\rm equil}_{\rm NL}},σ_{f^{\rm orth}_{\rm NL}},σ_{f^{\rm enfold}_{\rm NL}})_{\rm SKA-I}=(0.54, 86, 25, 43)$, $(σ_{f^{\rm local}_{\rm NL}},σ_{f^{\rm equil}_{\rm NL}},σ_{f^{\rm orth}_{\rm NL}},σ_{f^{\rm enfold}_{\rm NL}})_{\rm BINGO}=(17, 100, 128, 164)$, $(σ_{f^{\rm local}_{\rm NL}},σ_{f^{\rm equil}_{\rm NL}},σ_{f^{\rm orth}_{\rm NL}},σ_{f^{\rm enfold}_{\rm NL}})_{\rm FAST}=(9.5, 44, 75, 94)$. If the lower frequency band of FAST can be used, the constraint on local-type primordial non-Gaussianity will be $σ_{f_\mathrm{NL}}\sim1.62$ which is better than Planck. In addition, if the observation time for FAST could be extended to two years, the constraint on the equilateral shape of primordial non-Gaussianity would be improved to $σ_{f_\mathrm{NL}}\sim32$. Similarly, if the observational time of SKA-I could be extended to two years, the constraint on local and orthogonal shapes could be improved to $0.43$ and $20$, respectively, achieving better constraints than Planck.

astro-ph.CO↗

arXiv2016

Shortcut to adiabatic population transfer in quantum three-level systems: effective two-level problems and feasible counter-diabatic driving

Shortcut to adiabaticity in various quantum systems has attracted much attention with the wide applications in quantum information processing and quantum control. In this paper, we concentrate on stimulated Raman shortcut-to-adiabatic passage in quantum three-level systems. To implement counter-diabatic driving but without additional coupling, we first reduce the quantum three-level systems to effective two-level problems at large intermediate-level detuning, or on resonance, apply counter-diabatic driving along with the unitary transformation, and eventually modify the pump and Stokes pulses for achieving fast and high-fidelity population transfer. The required laser intensity and stability against parameter variation are further discussed, to demonstrate the advantage of shortcuts to adiabaticity.

quant-ph↗

arXiv2016

Experimental realization of stimulated Raman shortcut-to-adiabatic passage with cold atoms

Accurate control of a quantum system is a fundamental requirement in many areas of modern science ranging from quantum information processing to high-precision measurements. A significantly important goal in quantum control is to prepare a desired state as fast as possible with sufficiently high fidelity allowed by available resources and experimental constraints. Stimulated Raman adiabatic passage (STIRAP) is a robust way to realize high-fidelity state transfer but it requires a sufficiently long operation time to satisfy the adiabatic criteria. We here theoretically propose and then experimentally demonstrate a shortcut-to-adiabatic protocol to speed up the STIRAP. By modifying the shapes of the Raman pulses, we experimentally realize a fast and high-fidelity stimulated Raman shortcut-to-adiabatic passage that is robust against control parameter variations. The all-optical, robust, and fast protocol demonstrated here provides an efficient and practical way to control quantum systems.

quant-ph↗

arXiv2015

Dense magnetized plasma associated with a fast radio burst

Fast Radio Bursts are bright, unresolved, non-repeating, broadband, millisecond flashes, found primarily at high Galactic latitudes, with dispersion measures much larger than expected for a Galactic source. The inferred all-sky burst rate is comparable to the core-collapse supernova rate out to redshift 0.5. If the observed dispersion measures are assumed to be dominated by the intergalactic medium, the sources are at cosmological distances with redshifts of 0.2 to 1. These parameters are consistent with a wide range of source models. One fast radio burst showed circular polarization [21(7)%] of the radio emission, but no linear polarization was detected, and hence no Faraday rotation measure could be determined. Here we report the examination of archival data revealing Faraday rotation in a newly detected burst - FRB 110523. It has radio flux at least 0.6 Jy and dispersion measure 623.30(5) pc cm$^{-3}$. Using Galactic contribution 45 pc cm$^{-3}$ and a model of intergalactic electron density, we place the source at a maximum redshift of 0.5. The burst has rotation measure -186.1(1.4) rad m$^{-2}$, much higher than expected for this line of sight through the Milky Way and the intergalactic medium, indicating magnetization in the vicinity of the source itself or within a host galaxy. The pulse was scattered by two distinct plasma screens during propagation, which requires either a dense nebula associated with the source or a location within the central region of its host galaxy. Keeping in mind that there may be more than one type of fast radio burst source, the detection in this instance of source-local magnetization and scattering favours models involving young stellar populations such as magnetars over models involving the mergers of older neutron stars, which are more likely to be located in low density regions of the host galaxy.

astro-ph.HE↗

arXiv2015

Cosmological constraint on Brans-Dicke Model

We combine new Cosmic Microwave Background (CMB) data from Planck with Baryon Acoustic Oscillation (BAO) data to constrain the Brans-Dicke (BD) theory, in which the gravitational constant $G$ evolves with time. Observations of type Ia supernovae (SNeIa) provide another important set of cosmological data, as they may be regarded as standard candles after some empirical corrections. However, in theories that include modified gravity like the BD theory, there is some risk and complication when using the SNIa data because their luminosity may depend on $G$. In this paper, we assume a power law relation between the SNIa luminosity and $G$, but treat the power index as a free parameter. We then test whether the difference in distances measured with SNIa data and BAO data can be reduced in such a model. We also constrain the BD theory and cosmological parameters by making a global fit with the CMB, BAO and SNIa data set. For the CMB+BAO+SNIa data set, we find $0.08\times10^{-2} < ζ<0.33\times10^{-2} $ at the 68\% confidence level (CL) and $-0.01\times10^{-2} <ζ<0.43\times 10^{-2} $ at the 95\% CL, where $ζ$ is related to the {BD} parameter $ω$ by $ζ=\ln(1+1/ω)$.

astro-ph.CO↗

arXiv2015

Pulse design without rotating wave approximation

We design realizable time-dependent semiclassical pulses to invert the population of a two-level system faster than adiabatically when the rotating-wave approximation cannot be applied. Different approaches, based on the counterdiabatic method or on invariants, may lead to singularities in the pulse functions. Ways to avoid or cancel the singularities are put forward when the pulse spans few oscillations. For many oscillations an alternative numerical minimization method is proposed and demonstrated.

quant-ph↗

arXiv2014

Reducing the Tension Between the BICEP2 and the Planck Measurements: A Complete Exploration of the Parameter Space

A large inflationary tensor-to-scalar ratio $r_\mathrm{0.002} = 0.20^{+0.07}_{-0.05}$ is reported by the BICEP2 team based on their B-mode polarization detection, which is outside of the $95\%$ confidence level of the Planck best fit model. We explore several possible ways to reduce the tension between the two by considering a model in which $α_\mathrm{s}$, $n_\mathrm{t}$, $n_\mathrm{s}$ and the neutrino parameters $N_\mathrm{eff}$ and $Σm_\mathrmν$ are set as free parameters. Using the Markov Chain Monte Carlo (MCMC) technique to survey the complete parameter space with and without the BICEP2 data, we find that the resulting constraints on $r_\mathrm{0.002}$ are consistent with each other and the apparent tension seems to be relaxed. Further detailed investigations on those fittings suggest that $N_\mathrm{eff}$ probably plays the most important role in reducing the tension. We also find that the results obtained from fitting without adopting the consistency relation do not deviate much from the consistency relation. With available Planck, WMAP, BICEP2 and BAO datasets all together, we obtain $r_{0.002} = 0.14_{-0.11}^{+0.05}$, $n_\mathrm{t} = 0.35_{-0.47}^{+0.28}$, $n_\mathrm{s}=0.98_{-0.02}^{+0.02}$, and $α_\mathrm{s}=-0.0086_{-0.0189}^{+0.0148}$; if the consistency relation is adopted, we get $r_{0.002} = 0.22_{-0.06}^{+0.05}$.

astro-ph.CO↗

arXiv2013

Constraints on the Brans-Dicke gravity theory with the Planck data

Based on the new cosmic CMB temperature data from the Planck satellite, the 9 year polarization data from the WMAP, the BAO distance ratio data from the SDSS and 6dF surveys, we place a new constraint on the Brans-Dicke theory. We adopt a parametrization $ζ=\ln(1+1/ω})$, where the general relativity (GR) limit corresponds to $ζ= 0$. We find no evidence of deviation from general relativity. At 95% probability, $-0.00246 < ζ< 0.00567$, correspondingly, the region $-407.0 < ω<175.87$ is excluded. If we restrict ourselves to the $ζ>0$ (i.e. $ω>0$) case, then the 95% probability interval is $ζ<0.00549$, corresponding to $ω> 181.65$. We can also translate this result to a constraint on the variation of gravitational constant, and find the variation rate today as $\dot{G}=-1.42^{+2.48}_{-2.27} \times 10^{-13} $yr$^{-1} $ ($1σ$ error bar), the integrated change since the epoch of recombination is $δG/G = 0.0104^{+0.0186}_{-0.0067} $ ($1σ$ error bar). These limits on the variation of gravitational constant are comparable with the precision of solar system experiments.

astro-ph.CO↗