- 标题
- 摘要
- 关键词
- 实验方案
- 产品
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UV optical measurements of the Nozomi spacecraft interpreted with a two-component LIC-flow model <i>(Corrigendum)</i>
摘要： We found a typographical error regarding the uncertainty of the helium flow direction in our published paper Nakagawa et al. (2008). The helium flow direction should be (258.7 ± 8.0°, 3.4 ± 8.0°) instead of (258.7 ± 3.4°). As a consequence, the description for the helium flow direction in page 39 has to be replaced by “Residuals of simulated intensities with respect to observations attained minimum values for a downwind direction of (78.78 ± 8.0°, ?3.48 ± 8.0°), corresponding to an upwind direction of (258.78 ± 8.0°, 3.48 ± 8.0°).” All conclusions of the original paper remain unaffected. H. Nakagawa is grateful to Priscilla Frisch for pointing out this error.
关键词： ISM: atoms,ultraviolet: ISM,Sun: UV radiation,addenda,errata
更新于2025-09-23 15:23:52
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Absolute parameters for AI Phoenicis using WASP photometry <i>(Corrigendum)</i>
摘要： An error has been noted in the linear ephemeris for AI Phe, shown in Eq. (2) of the paper. The correct ephemeris is This is typographical error and has no effect on any of the timing analysis presented in the paper. HJD Pri. Min. = 2 455 805.24370(21) + 24.592483(17) E.
关键词： stars: fundamental parameters,errata,binaries: eclipsing,stars: evolution,addenda,stars: solar-type
更新于2025-09-23 15:22:29
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The extragalactic background light revisited and the cosmic photon–photon opacity ( <i>Corrigendum</i> )
摘要： For some unexplained reasons, all tables in the Franceschini & Rodighiero (2017) paper have been mixed up. Tables 1–3 reported there were identical to those published in Franceschini et al. (2008). We report here in Tables 1, 2, and 4 the corresponding correct values in terms of photon proper number densities and photon–photon optical depths as a function of photon energy. We also took this occasion to add a new table (Table 3) including the predicted extragalactic background light values at redshifts between 2 and 3.5, as requested by some readers of the Franceschini & Rodighiero (2017) paper. Both photon number densities and photon–photon optical depths are calculated including the contributions of the cosmic microwave background assumed as a black-body with T = 2.728 K. Except for the numerical values in the tables, all the rest of the Franceschini & Rodighiero (2017) paper is unaffected by the problem.
关键词： addenda,gamma rays: galaxies,diffuse radiation,errata,cosmic background radiation,BL Lacertae objects: general
更新于2025-09-23 15:22:29
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SEPIA – a new single pixel receiver at the APEX telescope ( <i>Corrigendum</i> )
摘要： A mistake occurred in the first paragraph of Sect. 2.1 during the production process. One should read the following sentences. One of the major challenges of bringing the SEPIA receiver with installed ALMA cartridges to the APEX telescope is the necessity to implement tertiary optics, which should not only provide the required and frequency independent illumination of the secondary but also be compatible with the existing optical layout of the APEX Cabin A where all single-pixel heterodyne receivers are installed. Another serious constraint is a clearance of the APEX Cabin A Nasmyth tube, whose rim is limited by the elevation encoder down to 150 mm in diameter requiring precision alignment possibilities to avoid Band 5 receiver beam truncation. ALMA receiver cartridges have built-in cold optics optimized for their respective position inside the ALMA Front-End (FE) receiver cryostat place at the antenna focal plane. In particular, depending on the cartridge position offset from the FE center, the beam tilt offset compensating is different for, for example, ALMA Band 5 – 2.38 degree and for ALMA Band 9 cartridges – 0.93 degree. SEPIA tertiary optics shall accommodate all these constrains and differences with minimum number of reflecting surfaces (thus minimizing the reflecting loss) and fit a very confined volume within the APEX Cabin A. Specific for SEPIA and in contrast to ALMA FE, we use a rotating cartridge-selection mirror. Such an optical switch addresses limitations of the Nasmyth layout when one receiver channel has access to the sky at a time (Fig. 1). The cartridge-selection mirror (NMF3, Fig. 1) with its precision computer-controlled rotating mechanism facilitates the accommodation of different ALMA cartridges having specific differences in the incoming beam positioning as outlined above.
关键词： errata,techniques: spectroscopic,addenda,instrumentation: detectors
更新于2025-09-23 15:22:29
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Beating the diffraction limit in astronomy via quantum cloning <i>(Corrigendum)</i>
摘要： In Sect. 3.3 of Kellerer (2014) I suggested detector read-out times below the coherence time of photons. If one assumes, instead, read-out times not less than the coherence time, Δt = λ2/(c Δλ), the spontaneous photons exceed, even for a very small ?eld-of-view, the number of stimulated photons per incoming photon. With the notation employed in Kellerer (2014) the mean number of cloned photons per incoming photon is: N ? 1 = σ S I (1) where I is the number of excited atoms, σ is the cross-section of excited atoms and S is the aperture- and ampli?er-area. A ?eld of angular diameter θ = 2.44 λ/D – where D is the aperture diameter – corresponds to the Airy disc up to its ?rst minimum. Within the read-out time Δt = λ2/(c Δλ), equal to the photon coherence time, this “di?raction area” receives a mean number of spontaneous photons: M = π θ2 4 · 1 4π · A Δt (2) A is the spontaneous emission rate. From these relations one obtains the average ?uence ratio of spontaneous and stimulated photons on the di?raction area: M N ? 1 = 0.74 π2 ～ 7.3 (3) in line with calculations by Prasad (1994) and his conclusions that the spontaneous emissions dominate the stimulated ones. On the other hand, on average 0.64 N cloned photons end up on the central standard deviation range of diameter 1/3 of the Airy disc. This area is 9 times smaller than the Airy disc considered above. Thus the ratio of spontaneous to stimulated ?uence is not 7.3 but merely 7.3/(9 × 0.64) ～ 1.3 in this region around the centre of the cloned photons. The spontaneous photons will prevent a large improvement of resolution as long as our set-up lacks a stage to recognize events where the stimulated emissions dominate. Such a stage is in principle possible, see notably the probabilistic noiseless ampli?cation processes discussed by Duan & Guo (1998), Ralph & Lund (2009). The main message of my article remains: it is fundamentally possible to improve the resolution of a telescope beyond the di?raction limit at the price of sensitivity, i.e. it is possible to trade sensitivity against resolution. The set-up that I have suggested will be incomplete unless it is given a suitable heralding stage.
关键词： instrumentation: high angular resolution,errata, addenda,telescopes
更新于2025-09-23 15:19:57
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Abundances of disk and bulge giants from high-resolution optical spectra
摘要： An error occurred during the production process. The subtitle of the article in the published version was "II. O, Mg, Co, and Ti in the bulge sample". Here, we correct this to "II. O, Mg, Ca, and Ti in the bulge sample".
关键词： Galaxy: evolution,Galaxy: bulge,errata, addenda,stars: abundances
更新于2025-09-19 17:15:36
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Integrated spectroscopy of the <i>Herschel</i> Reference Survey ( <i>Corrigendum</i> )
摘要： We noticed an error in the bisector fitting procedure adopted in our paper. Because of this error, there are some erroneous values in the slopes and intercepts given in Table 6 and in the best fit shown in Figs. 14 and 16. The corrected values and figures are given below. The updated C(Hβ) vs. βGALEX relations (bisector fit) are: C(Hβ) = 1.25 × βGALEX + 1.87; Spearman coefficient ρ = 0.56, shared by HI-deficient and HI-normal galaxies (solid line). A very similar relation is obtained excluding those galaxies hosting an AGN (C(Hβ) = 1.32 × βGALEX + 1.91; Spearman coefficient ρ = 0.61). These errors do not change the major conclusions of the paper.
关键词： galaxies: spiral,galaxies: ISM,dust, extinction,errata, addenda
更新于2025-09-10 09:29:36
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The Penn State – Toruń Centre for Astronomy Planet Search stars <i>(Corrigendum)</i>
摘要： Table 2 in our recent paper (Niedzielski et al. 2016) erroneously includes 20 stars that were finally adopted for detailed spectroscopic analysis (including 11 SB1s mentioned in the text) and are listed in Table 1 as well. Consequently, the corrected Table 2 (available in electronic version) contains 33 rather than 53 stars. They are 18 SB2 stars, 14 ones with variable CCFs (possibly SB2) and one with a weak CCF.
关键词： stars: atmospheres,stars: late-type,stars: general,stars: fundamental parameters,errata, addenda
更新于2025-09-04 15:30:14