2006
DOI: 10.1103/physrevlett.96.209602
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Cited by 13 publications
(13 citation statements)
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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%
“…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%
“…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%
“…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%