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T. Takahashi

Publications and source records attributed to T. Takahashi.

At least 235 records · Page 13Linked to original sources
arXiv2002

An unidentified TeV source in the vicinity of Cygnus OB2

Deep observation (~113 hrs) of the Cygnus region at TeV energies using the HEGRA stereoscopic system of air Cerenkov telescopes has serendipitously revealed a signal positionally inside the core of the OB association Cygnus OB2, at the edge of the 95% error circle of the EGRET source 3EG J2033+4118, and ~0.5deg north of Cyg X-3. The centre of gravity of the source is RA (J2000): 20hr 32m 07s +-9.2s (stat) +-2.2s (sys), Dec (J2000): +41deg 30' 30" +-2.0' (stat) +-0.4' (sys). The source is steady, has a post-trial significance of +4.6 sigma, indication for extension with radius 5.6' at the ~3sigma level, and has a differential power-law flux with hard photon index of -1.9 +-0.3 (stat) +-0.3 (sys). The integral flux above 1 TeV amounts ~3% that of the Crab. No counterpart for the TeV source at other wavelengths is presently identified, and its extension would disfavour an exclusive pulsar or AGN origin. If associated with Cygnus OB2, this dense concentration of young, massive stars provides an environment conducive to multi-TeV particle acceleration and likely subsequent interaction with a nearby gas cloud. Alternatively, one could envisage gamma-ray production via a jet-driven termination shock.

astro-ph↗
arXiv2002

Single Photon X-Ray Imaging with Si- and CdTe-Sensors

Studies of a single photon counting hybrid pixel detector for X-ray imaging applications are presented. A silicon- and a CdTe-sensor were bump bonded onto the MPEC pixel readout chip and could be successfully operated. A new USB based readout system was used for data acquisition. Measurements of the performance on the latest MPEC chip and imaging characterization of the sensors are presented.

hep-ex↗
arXiv2002

Flat Spectrum X-ray Emission from the Direction of a Molecular Cloud Associated with SNR RX J1713.7-3946

We report on the discovery of a hard X-ray source with ASCA from a molecular cloud in the vicinity of the SNR RX J1713.7-3946. The energy spectrum (1--10 keV) shows a flat continuum which is described by a power-law with photon index 1.0 +-0.4. We argue that this unusually flat spectrum can be best interpreted in terms of characteristic bremsstrahlung emission from the ionization-loss-flattened distribution of either sub-relativistic protons or mildly-relativistic electrons. The strong shock of the SNR RX J1713.7-3946, which presumably interacts with the molecular cloud, as evidenced by observations of CO-lines, seems to be a natural site of acceleration of such sub- or mildly-relativistic nonthermal particles. However, the observed X-ray luminosity of 1.7 10^35 erg/s (for 6 kpc distance) requires that a huge kinetic energy of about 10^50 erg be released in the form of nonthermal particles to illuminate the cloud. The shock-acceleration at RX J1713.7-3946 can barely satisfy this energetic requirement, unless (i) the source is located much closer than 6 kpc and/or (ii) the mechanical energy of the explosion essentially exceeds 10^51 erg. Another possibility would be that an essential part of the "lost" energy is somehow converted to plasma waves, which return this energy to nonthermal particles through their turbulent reacceleration on plasma waves. Irrespective of mechanisms responsible for production of high-energy particles, the flat X-ray emission seems to be a signature of a new striking energetic phenomenon in molecular clouds.

astro-ph↗
arXiv2001

Relativistic Electron Facility for Education and Research at Hiroshima University

The Relativistic Electron Facility for Education and Research (REFER) at Hiroshima University accepts a 150 MeV electron beam from a microtron, the injector to the 700 MeV storage ring of the Hiroshima Synchrotron Research Center, and keep it circulating for 2.5ms without a RF acceleration. It acts as a beam stretcher and has been used for the following researches: 1) X-ray generation from an internal multiple foil crystalline target due to the parametric X-radiation (PXR) and the resonant transition radiation (RTR). 2) Laser backward Compton scattering. 3) Coherent pair creation from Si crystal by 150 MeV bremsstrahlung. 4) Study of the Ter-Mikaelian effect in the low energy part of the bremsstrahlung in an extracted electron line. 5) A novel scheme of beam stabilization by the induction coil. This paper reports the experimental results and the current status of the REFER electron ring.

physics.acc-ph↗
arXiv2001

Quasiparticles and Energy Scaling in Bi$_2$Sr$_2$Ca$_{n-1}$Cu$_n$O$_{2n+4}$ ($\it{n}$=1-3): Angle-Resolved Photoemission Spectroscopy

Angle-resolved photoemission spectroscopy (ARPES) has been performed on the single- to triple-layered Bi-family high-{\it T$_c$} superconductors (Bi$_2$Sr$_2$Ca$_{n-1}$Cu$_n$O$_{2n+4}$, $\it{n}$=1-3). We found a sharp quasiparticle peak as well as a pseudogap at the Fermi level in the triple-layered compound. Comparison among three compounds has revealed a universal rule that the characteristic energies of superconducting and pseudogap behaviors are scaled with the maximum {\it T$_c$}.

cond-mat.supr-con↗
arXiv2001

Five-year Monitorings of TeV Blazars with ASCA and RXTE

We study the temporal/spectral variability of two extragalactic TeV sources, Mrk 421 and Mrk 501, based on 5-year observations with the ASCA and RXTE satellites. We found that the peak of the synchrotron emission exists just in the X-ray band and its position shifted from lower to higher energy when the source became brighter. Relationship between the peak energy and peak luminosity showed quite different behavior in the two sources; Mrk 421 showed very little change in the peak position (0.5-2 keV), while Mrk 501 revealed the largest shift ever observed in blazars (1-100 keV). We analyze these X-ray data with the flux changes in TeV band, which are obtained from 35 truly simultateneous observations. Very different spectral evolution of both objects indicates some differences in the electron acceleration mechanism at work during the flares. We argue that the flux variability of Mrk 421 is associated with an increase in the number of electrons, while the flare of Mrk 501 is mostly due to the large changes in maximum energy of electrons. We also discuss the characteristic temporal variability of TeV sources, and implications for the X-ray emitting site in the relativistic jet.

astro-ph↗
arXiv2001

High-Resolution Photoemission Study of MgB2

We have performed high-resolution photoemission spectroscopy on MgB2 and observed opening of a superconducting gap with a narrow coherent peak. We found that the superconducting gap is s-like with the gap value of 4.5 meV at 15 K. The temperature dependence (15 - 40 K) of gap value follows well the BCS form, suggesting that 2Delta/kBTc at T=0 is about 3. No pseudogap behavior is observed in the normal state. The present results strongly suggest that MgB2 is categorized into a phonon-mediated BCS superconductor in the weak-coupling regime.

cond-mat.str-el↗
arXiv2001

Gold-plated processes at photon colliders

We review the most important topics and objectives of the physics program of the gamma-gamma, gamma-electron collider (photon collider) option for an e+e- linear collider.

hep-ph↗
arXiv2001

On the determination of the Fermi surface in high-Tc superconductors by angle-resolved photoemission spectroscopy

We study the normal state electronic excitations probed by angle resolved photoemission spectroscopy (ARPES) in Bi2201 and Bi2212. Our main goal is to establish explicit criteria for determining the Fermi surface from ARPES data on strongly interacting systems where sharply defined quasiparticles do not exist and the dispersion is very weak in parts of the Brillouin zone. Additional complications arise from strong matrix element variations within the zone. We present detailed results as a function of incident photon energy, and show simple experimental tests to distinguish between an intensity drop due to matrix element effects and spectral weight loss due to a Fermi crossing. We reiterate the use of polarization selection rules in disentangling the effect of umklapps due to the BiO superlattice in Bi2212. We conclude that, despite all the complications, the Fermi surface can be determined unambiguously: it is a single large hole barrel centered about (pi,pi) in both materials.

cond-mat.supr-con↗
arXiv2000

Complex Spectral Variability from Intensive Multi-wavelength Monitoring of Mrk421 in 1998

We conducted a multi-frequency campaign for the TeV blazar Mrk~421 in 1998 April. The campaign started from a pronounced high amplitude flare recorded by SAX and Whipple; ASCA observation started three days later. In the X-ray data, we detected multiple flares, occuring on time scales of about one day. ASCA data clearly reveal spectral variability. The comparison of the data from ASCA, EUVE and RXTE indicates that the variability amplitudes in the low energy synchrotron component are larger at higher photon energies. In TeV Gamma-rays, large intra-day variations -- which were correlated with the X-ray flux -- were observed when results from three Cherenkov telescopes are combined. The RMS variability of TeV Gamma--rays was similar to that observed in hard X-rays, above 10 keV. The X-ray light curve reveals flares which are almost symmetric for most of cases, implying the dominant time scale is the light crossing time through the emitting region. The structure function analysis based on the continuous X-ray light curve of seven days indicates that the characteristic time scale is ~0.5 day. The analysis of ASCA light curves in various energy bands appears to show both soft (positive) and hard (negative) lags. These may not be real, as systematic effects could also produce these lags, which are all much smaller than an orbit. If the lags of both signs are real, these imply that the particle acceleration and X-ray cooling time scales are similar.

astro-ph↗
arXiv2000

Renormalization of spectral lineshape and dispersion below Tc in Bi2Sr2CaCu2O8+d

Angle-resolved photoemission (ARPES) data in the superconducting state of Bi2Sr2CaCu2O8+d show a kink in the dispersion along the zone diagonal, which is related via a Kramers-Kronig analysis to a drop in the low-energy scattering rate. As one moves towards (pi,0), this kink evolves into a spectral dip. The occurrence of these anomalies in the dispersion and lineshape throughout the zone indicate the presence of a new energy scale in the superconducting state.

cond-mat.supr-con↗
arXiv2000

Coherent quasiparticle weight and its connection to high-T_c superconductivity from angle-resolved photoemission

In conventional superconductors, the pairing energy gap (Δ) and superconducting phase coherence go hand-in-hand. As the temperature is lowered, both the energy gap and phase coherence appear at the transition temperature T_c. In contrast, in underdoped high-T_c superconductors (HTSCs), a pseudogap appears at a much higher temperature T^*, smoothly evolving into the superconducting gap at T_c. Phase coherence on the other hand is only established at T_c, signaled by the appearance of a sharp quasiparticle (QP) peak in the excitation spectrum. Another important difference between the two types of superconductors is in the ratio of 2Δ/ T_c=R. In BCS theory, R~3.5, is constant. In the HTSCs this ratio varies widely, continuing to increase in the underdoped region, where the gap increases while T_c decreases. Here we report that in HTSCs it is the ratio z_AΔ_m/T_c which is approximately constant, where Δ_m is the maximum value of the d-wave gap, and z_A is the weight of the coherent excitations in the spectral function. This is highly unusual, since in nearly all phase transitions, T_c is determined by an energy scale alone. We further show that in the low-temperature limit, z_{\it A} increases monotonically with increasing doping x. The growth is linear, i.e. z_A(x)\propto x, in the underdoped to optimally doped regimes, and slows down in overdoped samples. The reduction of z_A with increasing temperature resembles that of the c-axis superfluid density.

cond-mat.supr-con↗
arXiv2000

Rapid Synchrotron Flares from BL Lacertae Detected by ASCA and RXTE

We report the variable X-ray emission from BL Lacertae detected in the ASCA ToO observation conducted during the EGRET and RXTE pointings, coincident with the 1997 July outburst. The source showed a historically high state of X-ray, optical, and gamma-ray emission, with its 2-10 keV flux peaking at ~3.3 E-11 erg/cm2/s. This is more than 3 times higher than the value measured by ASCA in 1995. We detected two rapid flares which occured only in the soft X-ray band, while the hard X-ray flux also increased, but decayed with a much longer time scale. Together with the requirement of a very steep and varying power law dominating the soft X-ray band in addition to the hard power law, we suggest that both the high energy end of the synchrotron spectrum and the hard inverse Compton spectrum were visible in this source during the outburst. We discuss the possible origins of the observed variability time scales, and interpret the short time scales of the soft X-ray variability as reflecting the size of the emission region.

astro-ph↗
arXiv2000

Optical Identification of the ASCA Large Sky Survey

We present results of optical identification of the X-ray sources detected in the ASCA Large Sky Survey. Optical spectroscopic observations were done for 34 X-ray sources which were detected with the SIS in the 2-7 keV band above 3.5 sigma. The sources are identified with 30 AGNs, 2 clusters of galaxies, and 1 galactic star. Only 1 source is still unidentified. The flux limit of the sample corresponds to 1 x 10^{-13} erg s^{-1} cm^{-2} in the 2-10 keV band. Based on the sample, the paper discusses optical and X-ray spectral properties of the AGNs, contribution of the sources to the Cosmic X-ray Background, and redshift and luminosity distributions of the AGNs. An interesting result is that the redshift distribution of the AGNs suggests a deficiency of high-redshift (0.5 < z < 2) and luminous (Lx(2-10 keV) > 10^{44} erg s^{-1}) absorbed narrow-line AGNs (so called type 2 QSOs).

astro-ph↗
arXiv1999

The Fermi surface of Bi2Sr2CaCu2O8

We study the Fermi surface of Bi2Sr2CaCu2O8 (Bi2212) using angle resolved photoemission (ARPES) with a momentum resolution of ~ 0.01 of the Brillouin zone. We show that, contrary to recent suggestions, the Fermi surface is a large hole barrel centered at (pi,pi), independent of the incident photon energy.

cond-mat.supr-con↗
arXiv1999

X-ray Observations of Optically-Selected, Radio-Quiet Quasars I: The ASCA results

We present the result of 27 ASCA observations of 26 radio-quiet quasars (RQQs) from the PG survey. All the RQQs were detected except 2 BALQSOs. We find the variability characteristics of the sources to be consistent with Seyf-1s. A powerlaw offers an acceptable description of the time-averaged spectra in the 2-10 keV (RQQ-frame) band for all but 1 dataset. The photon indices vary from object to object over the range 1.5~<Gamma(2-10 keV)~<3 with a mean Gamma(2-10keV)~2 and dispersion ~=0.25. The distribution of Gamma(2-10 keV is therefore similar to that observed in other RQ AGN, and seems unrelated to X-ray luminosity. No single model adequately describes the full 0.6-10 keV (obs-frame) continuum of all the RQQs. ~50% of the sources can be described by a single powerlaw (or with only very subtle deviations). All but one of the remaining datasets have convex spectra (flattening to higher energies). The exception is PG 1411+442, in which a substantial column density obscures ~98% of the continuum. We find only 5 (or 6) of 14 objects with z<~0.25 to have a 'soft excess' at energies <~1 keV, but find no universal shape for these spectral components. The spectrum of PG 1244+026 contains an emission feature at ~1 keV. The detection rate of absorption due to ionized material in these RQQs is lower than in Seyf-1s. In part, this may be due to selection effects. However, when detected, the absorbers in the RQQs exhibit a similar range of column density and ionization parameter as Seyf-1s. We find evidence of Fe K-shell emission in at least 8 RQQs. These are all low-luminosity objects, and the line parameters are consistent with other low-luminosity RQ AGN. However we find a trend whereby the profile and strength of the Fe K-shell emission changes as a function of luminosity.

astro-ph↗