Lin and Chiang Reply:

Lin, Deng-Sung; Chiang, TC

doi:10.1103/physrevlett.96.209602

Cited by 13 publications

(13 citation statements)

References 8 publications

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“…4(c)), our experimental results in the same figure lack that spectral feature, in agreement with previous photoemission studies [1,6]. For example, to resolve this disagreement between the DFT results and photoemission, Lin et al [49] proposed that, with increasing oxygen doping in the BiO layer, the BiO band shifts above E F at the M point, which also is consistent with a scanning tunneling microscopic and spectroscopic study [50]. The excess oxygen atoms are believed to be responsible for the δ in the common designation Bi 2 Sr 2 CaCu 2 O 8+δ .…”

Section: Discussionsupporting

confidence: 92%

Atomic-layer-resolved composition and electronic structure of the cuprate Bi2Sr2CaCu2
Kuo
¹
,
Lin
²
,
Conti
³

et al. 2018
Phys. Rev. B

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A major remaining challenge in the superconducting cuprates is the unambiguous differentiation of the composition and electronic structure of the CuO 2 layers and those of the intermediate layers. The large c axis for these materials permits employing soft x-ray (930.3 eV) standing wave (SW) excitation in photoemission that yields atomic layer-byatomic layer depth resolution of these properties. Applying SW photoemission to Bi 2 Sr 2 CaCu 2 O 8+δ yields the depth distribution of atomic composition and the layerresolved densities of states. We detect significant Ca presence in the SrO layers and oxygen bonding to three different cations. The layer-resolved valence electronic structure is found to be strongly influenced by the atomic supermodulation structure--as determined by comparison to density functional theory calculations, by Ca-Sr intermixing, and by correlation effects associated with the Cu 3d-3d Coulomb interaction, further clarifying the complex interactions in this prototypical cuprate. Measurements of Proposal No. 20161205) for access to Beamline CASSIOPEE that contributed to the results presented here.

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Section: Discussionsupporting

confidence: 92%

Atomic-layer-resolved composition and electronic structure of the cuprate Bi2Sr2CaCu2
Kuo
¹
,
Lin
²
,
Conti
³

et al. 2018
Phys. Rev. B

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show abstract

“…In order to quantity the tension it is useful to consider the posterior of equation (25), where the degeneracy is removed by considering the combination r d h. The result is given in Figure 3. Using now the Index of Inconsistency of Lin & Ishak (2017), we find a 4.5σ tension between Planck 2018 and angular BAO (SNe+θ BAO ), while Planck 2018 and anisotropic BAO are in good agreement (1.7σ tension). See Table 4 for the numerical summary.…”

Section: Resultsmentioning

confidence: 78%

A new method to build the (inverse) distance ladder

Camarena

Marra

2020

Monthly Notices of the Royal Astronomical Society

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The cosmic distance ladder is the succession of techniques by which it is possible to determine distances to astronomical objects. Here, we present a new method to build the cosmic distance ladder, going from local astrophysical measurements to the CMB. Instead of relying on cosmography in order to model the luminosity-distance relation and calibrate supernovae with BAO, we exploit the distance-duality relation d L = (1 + z) 2 d A -valid if photon number is conserved and gravity is described by a metric theory. The advantage is that the results will not depend on the parametrization of the luminosity-distance relation: no model is adopted in order to calibrate BAO with supernovae. This method yields measurements of the Hubble constant and deceleration parameter that only use local observations. Furthermore, it can directly assess the impact of BAO observations on the strong 4-5σ tension between local and global H 0 . Using the latest supernova, BAO and CMB observations, we found a consistently low value of q 0 and strong inconsistency between angular and anisotropic BAO measurements, which are, or not, in agreement with CMB depending on the kind of analysis. We conclude that, in order to understand the reasons behind the H 0 crisis, a first step should be clarifying the tension between angular and anisotropic BAO as this will help understanding if new physics is required at the pre-recombination epoch or/and during the dark energy era.

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“…In this paper, the focus is on the interpretation of the jet environments of AGN, in particular on the specific subset known as blazars, which exhibit flares with short timescale variations in radio, optical, X-ray and γ-ray wavebands. The class of blazars was identified following the discovery (Hartmann et al 1992;Lin et al 1992) of transient gamma-ray emission in 3C 279 and Mrk 421 by the EGRET instrument on the Compton Gamma-Ray Observatory in the 100 MeV -1 GeV range. This was around the same time that the Whipple atmosphericČerenkov telescope (ACT) discerned that Mrk 421 also emitted at TeV energies (Punch et al 1992).…”

Section: Introductionmentioning

confidence: 99%

Probing acceleration and turbulence at relativistic shocks in blazar jets

Baring

Böttcher

Summerlin

2016

Mon. Not. R. Astron. Soc.

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Diffusive shock acceleration (DSA) at relativistic shocks is widely thought to be an important acceleration mechanism in various astrophysical jet sources, including radio-loud active galactic nuclei such as blazars. Such acceleration can produce the non-thermal particles that emit the broadband continuum radiation that is detected from extragalactic jets. An important recent development for blazar science is the ability of Fermi-LAT spectroscopy to pin down the shape of the distribution of the underlying non-thermal particle population. This paper highlights how multi-wavelength spectra spanning optical to X-ray to gamma-ray bands can be used to probe diffusive acceleration in relativistic, oblique, magnetohydrodynamic (MHD) shocks in blazar jets. Diagnostics on the MHD turbulence near such shocks are obtained using thermal and non-thermal particle distributions resulting from detailed Monte Carlo simulations of DSA. These probes are afforded by the characteristic property that the synchrotron νF ν peak energy does not appear in the gamma-ray band above 100 MeV. We investigate self-consistently the radiative synchrotron and inverse Compton signatures of the simulated particle distributions. Important constraints on the diffusive mean free paths of electrons, and the level of electromagnetic field turbulence are identified for three different case study blazars, Mrk 501, BL Lacertae and AO 0235+164. The X-ray excess of AO 0235+164 in a flare state can be modelled as the signature of bulk Compton scattering of external radiation fields, thereby tightly constraining the energy-dependence of the diffusion coefficient for electrons. The concomitant interpretations that turbulence levels decline with remoteness from jet shocks, and the probable significant role for non-gyroresonant diffusion, are posited.

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Lin and Chiang Reply:

Cited by 13 publications

References 8 publications

Atomic-layer-resolved composition and electronic structure of the cuprate Bi2Sr2CaCu2
Kuo
¹
,
Lin
²
,
Conti
³

et al. 2018
Phys. Rev. B

Atomic-layer-resolved composition and electronic structure of the cuprate Bi2Sr2CaCu2
Kuo
¹
,
Lin
²
,
Conti
³

et al. 2018
Phys. Rev. B

A new method to build the (inverse) distance ladder

Probing acceleration and turbulence at relativistic shocks in blazar jets

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Lin and Chiang Reply:

Cited by 13 publications

References 8 publications

Atomic-layer-resolved composition and electronic structure of the cuprate Bi2Sr2CaCu2Kuo1, Lin2, Conti3 et al. 2018Phys. Rev. B

Atomic-layer-resolved composition and electronic structure of the cuprate Bi2Sr2CaCu2Kuo1, Lin2, Conti3 et al. 2018Phys. Rev. B

A new method to build the (inverse) distance ladder

Probing acceleration and turbulence at relativistic shocks in blazar jets

Contact Info

Product

Resources

About

Atomic-layer-resolved composition and electronic structure of the cuprate Bi2Sr2CaCu2
Kuo
¹
,
Lin
²
,
Conti
³

et al. 2018
Phys. Rev. B

Atomic-layer-resolved composition and electronic structure of the cuprate Bi2Sr2CaCu2
Kuo
¹
,
Lin
²
,
Conti
³

et al. 2018
Phys. Rev. B