arXiv subjects

J. S. Huang

Publications and source records attributed to J. S. Huang.

63 records · Page 4Linked to original sources

arXiv2010

High efficiency tomographic reconstruction of quantum states by quantum nondemolition measurements

We propose a high efficiency tomographic scheme to reconstruct an unknown quantum state of the qubits by using a series of quantum nondemolition (QND) measurements. The proposed QND measurements of the qubits are implemented by probing the the stationary transmissions of the dispersively-coupled resonator. It is shown that only one kind of QND measurements is sufficient to determine all the diagonal elements of the density matrix of the detected quantum state. The remaining non-diagonal elements of the density matrix can be determined by other spectral measurements by beforehand transferring them to the diagonal locations using a series of unitary operations. Compared with the pervious tomographic reconstructions based on the usual destructively projective (DP) measurements (wherein one kind of such measurements could only determine one diagonal element of the density matrix), the present approach exhibits significantly high efficiency for N-qubit (N > 1). Specifically, our generic proposal is demonstrated by the experimental circuit-quantumelectrodynamics (circuit-QED) systems with a few Josephson charge qubits.

quant-ph↗

arXiv2010

Quantum state engineering with flux-biased Josephson phase qubits by Stark-chirped rapid adiabatic passages

In this paper, the scheme of quantum computing based on Stark chirped rapid adiabatic passage (SCRAP) technique [L. F. Wei et al., Phys. Rev. Lett. 100, 113601 (2008)] is extensively applied to implement the quantum-state manipulations in the flux-biased Josephson phase qubits. The broken-parity symmetries of bound states in flux-biased Josephson junctions are utilized to conveniently generate the desirable Stark-shifts. Then, assisted by various transition pulses universal quantum logic gates as well as arbitrary quantum-state preparations could be implemented. Compared with the usual PI-pulses operations widely used in the experiments, the adiabatic population passage proposed here is insensitive the details of the applied pulses and thus the desirable population transfers could be satisfyingly implemented. The experimental feasibility of the proposal is also discussed.

quant-ph↗

arXiv2009

Jaynes-Cummings Models with trapped surface-state electrons in THz cavities

An electron floating on the liquid Helium is proposed to be trapped (by a micro-electrode set below the liquid Helium) in a high finesse cavity. Two lowest levels of the vertical motion of the electron acts as a two-level "atom", which could resonantly interact with the THz cavity. In the Lamb-Dicke regime, wherein the electron's in-plane activity region is much smaller than the wavelength of the cavity mode, the famous Jaynes-Cummings model (JCM) could be realized. By applying an additional external classical laser beam to the electron, a driven JCM could also be implemented. With such a driven JCM certain quantum states, e.g., coherent states and the Schrodinger cat states, of the THz cavity field could be prepared by one-step evolution. The numerical results show that, for the typical parameters of the cavity and electron on liquid Helium, a strong coupling between the artificial atom and the THz cavity could be obtained.

quant-ph↗

arXiv2008

Deterministic spatio-temporal control of nano-optical fields in optical antennas and nano transmission lines

We show that pulse shaping techniques can be applied to tailor the ultrafast temporal response of the strongly confined and enhanced optical near fields in the feed gap of resonant optical antennas (ROAs). Using finite-difference time-domain (FDTD) simulations followed by Fourier transformation, we obtain the impulse response of a nano structure in the frequency domain, which allows obtaining its temporal response to any arbitrary pulse shape. We apply the method to achieve deterministic optimal temporal field compression in ROAs with reduced symmetry and in a two-wire transmission line connected to a symmetric dipole antenna. The method described here will be of importance for experiments involving coherent control of field propagation in nanophotonic structures and of light-induced processes in nanometer scale volumes.

physics.optics↗

arXiv2007

Lyman Break Galaxies at z~1 and the evolution of the dust attenuation in star-forming galaxies with the redshift

Ultraviolet (UV) galaxies have been selected from GALEX. The presence of a FUV-dropout in their spectral energy distributions proved to be a very complete (83.3%) but not very efficient (21.4%) tool for identifying Lyman Break Galaxies (LBGs) at z~1. We divide the LBG sample into two sub-classes: red LBGs (RLBGs) detected at 24 micron which are mainly Luminous IR Galaxies (LIRGs) and blue LBGs (BLBGs) undetected at 24 microns down to 83 microJy. Two of the RLBGs are also detected at 70 micron. The median SED of the RLBGs is similar (above lambda~1 micron) to the dusty starburst HR10. However, unlike local (U)LIRGs, RLBGs are UV bright objects. We suggest that these objects contain a large amount of dust but that some bare stellar populations are also directly visible. The median SED of the BLBGs is consistent with their containing the same stellar population as the RLBGs but with a lower dust content. The luminosity function of our LBG sample at z~1 is similar to the luminosity function of NUV-selected galaxies at the same redshift. The integrated luminosity densities of z~1 LBGs and NUV-selected galaxies are very consistent. We show that star formation rates (SFRs) estimated from UV measurements and corrected using the IRX-beta method provide average total SFR_TOT in agreement with SFR_UV + SFR_dust. However, IRX-beta-based SFR_TOT shows a large dispersion. Summing up the detected UV (1150A rest-frame) and IR-based star formation rates of the detected objects, we find that only one third of the total (i.e. UV + dust) LBG SFR resides in BLBGs and two thirds in RLBGs, even though most LBGs at z~1 are BLBGs. On the other hand, the total SFR of LBGs accounts for only 11% of the total SFR at z~1. Finally, we observe a regular decrease of L_TIR / L_FUV from z=0 to z~2 for UV-selected samples.

astro-ph↗

arXiv2007

The Differences of Star Formation History Between Merging Galaxies and Field Galaxies in the EDR of the SDSS

Based on the catalog of merging galaxies in the Early Data Release (EDR) of the Sloan Digital Sky Survey (SDSS), the differences of star formation history between merging galaxies and field galaxies are studied statistically by means of three spectroscopic indicators the 4000-Å break strength, the Balmer absorption-line index, and the specific star formation rate. It is found that for early-type merging galaxies the interactions will not induce significant enhancement of the star-formation activity because of its stability and lack of cool gas. On the other hand, late-type merging galaxies always in general display more active star formation than field galaxies on different timescales within about 1Gyr. We also conclude that the mean stellar ages of late-type merging galaxies are younger than those of late-type field galaxies.

astro-ph↗

arXiv2007

Lyman Break Galaxies and Luminous IR Galaxies at z ~ 1

We use deep GALEX images of CDFS in UV to define the first large sample of 420 Lyman Break Galaxies at z~1. We use a PSF fitting to estimate UV magnitudes on these deep crowded images. Deep Spitzer IRAC and MIPS provide the first detection of a large sample of Lyman Break Galaxies in the mid- to far-infrared range. We are therefore able to study and compare the UV and TIR emission of Lyman Break Galaxies. We find that about 15% of the LBG sample are strong emitters at 24 microns (Red LBGs). Most of them are Luminous IR Galaxies (LIRGs) while the rest (Blue LBGs) are undetected at the 83 microJy level of MIPS GTO image. We find that Blue LBGs have a Spectral Energy Distribution similar to high redshift Lyman Break Galaxies. Finally, the dust-to-FUV ratio of this sample is compared with similar ratios at z=1 and z~2. This work suggests an evolution (decrease) of the dust-to-FUV ratio with the redshift.

astro-ph↗

arXiv2006

AEGIS: A Panchromatic Study of IRAC-selected Extremely Red Objects with Confirmed Spectroscopic Redshifts

We study 87 Extremely Red Objects (EROs), selected both to have color redder than R-[3.6] = 4.0, and to have confirmed spectroscopic redshifts. Together, these two constraints result in this sample populating a fairly narrow redshift range at 0.76 < z < 1.42. The key new ingredient included here is deep Spitzer Space Telescope InfraRed Array Camera (IRAC) data. Based on [3.6]-[8.0] color, we demonstrate that it is possible to classify EROs into early-type, dusty starburst, or power-law (AGN) types. We present ultraviolet to mid-infrared spectral energy distributions (SEDs) and Advanced Camera for Surveys (ACS) images, both of which support our simple IRAC color classification.

astro-ph↗

arXiv1998

Global Extinction in Spiral Galaxies

Magnitude-limited samples of spiral galaxies drawn from the Ursa Major and Pisces clusters are used to determine their extinction properties as a function of inclination. Imaging photometry is available for 87 spirals in B,R,I and K' bands. Extinction causes systematic scatter in color-magnitude plots. A strong luminosity dependence is found. Relative edge-on to face-on extinction of up to 1.7 mag is found at B for the most luminous galaxies but is unmeasurably small for faint galaxies. At R the differential absorption with inclination reaches 1.3 mag, at I it reaches 1.0 mag, and at K' the differential absorption can in the extreme be as great as 0.3 mag. The luminosity dependence of reddening can be translated into a dependence on rotation rate which is a distance-independent observable. Hence, corrections can be made that are useful for distance measurements. The strong dependence of the corrections on luminosity act to steepen luminosity-linewidth correlations. The effect is greatest toward the blue, with the consequence that luminosity-linewidth slope dependencies are now only weakly a function of color.

astro-ph↗