First detection of SO and SO2 in a B[e] supergiant ejecta, with chemical models reproducing high SO2 abundance in ~10^4 yr and low 32SO/33SO ratio attributed to photochemistry-driven fractionation.
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- background 10.3390/atoms13060052. [29] F.A. Jenkins, E. Segr` e. Phys. Rev.,55, 52 (1939). DOI: 10.1103/PhysRev.55.52. [30] L.I. Schiff, H. Snyder. Phys. Rev.,55, 59 (1939). DOI: 10.1103/PhysRev.55.59. [31] G.W. Preston. Astrophys. J.,160, L143 (1970). DOI: 10.1086/180547. [32] S.B. Kemic. Astrophysics and Space Science,36, 459 (1975). DOI: 10.1007/BF00645268. [33] C. Moran, T.R. Marsh, V.S. Dhillon. Monthly Notices of the Royal Astronomical Society,299, 218 (1998). DOI: 10.1046/j.1365-8711.1998.01763.x. 1
- background It is well known that capturing key physics in the synthetic models - from stellar energetics and spectra, and in particular the treatment of the thermally puls- ing asymptotic-giant-branch (TP-AGB) phase - is key to avoid systematic uncertainties in the derived galaxy physical parameters. TP-AGB stars dominate the NIR light of intermediate-age stellar populations (∼0.2-2 Gyr) in C. Maraston (1998, 2005) evolutionary population synthe- sis models, producing numerous NIR features, including molec
- background The characteristic granule lifetime is estimated as Tgra ≈ dgra σ1D ≈2.9m −1 22 σ1D 100 km s−1 −2 Myr.(27) The dynamical effects of these density fluctuations can be modeled by treating FDM granules as quasiparticles (Bar-Or et al. 2019; El-Zant et al. 2020; Cha- vanis 2021; Dutta Chowdhury et al. 2021). Assuming a Maxwellian velocity distribution, the effective particle mass is Mgra ≈ πρd3 6 ,(28) whereρdenotes the local dark matter density. The granule size remains approximately constant in
- background 2025). Moreover, under the same approximation, the baryonic inflow rate is expressed as ˙Mb ≃144M ⊙ yr−1fb,0.16T 3/2 vir,6 1 +z 10 ,(6) whereT vir,6 =T vir/(106 K) is the normalized halo virial temperature. Therefore, if the gas supply feeds the nu- clear region of a massive halo with a virial temperature ofT vir,6 ≃1, this rate corresponds to∼ O(100)× ˙MEdd for a BH withM BH ≲10 7 M⊙. Such an inflow is sufficient to confine ionizing radiation from the central AGN through efficient radiative
- method thusζhas to transform likeζ→ζ−αin order for the pro- jected shear to stay invariant. The polar angles transform like φi →φ i −αand therefore the coefficients need to satisfy the identitya 1 +a 2 +a 3 =1. The choice forζis arbitrary, as long as it meets the two conditions above. Choosing another projection angleζ ′ = a′ 1φ1 +a ′ 2φ2 +a ′ 3φ3 changes the 4PCF only by the phase factor e2i(ζ′−ζ) =e 2i[(a1−a′ 1)ϕ12+(a′ 3−a3)ϕ23]. Throughout the following work, Article number, page 4 of 19 Jonathan Oe
- background (a) Detected filaments around Abell 2744. The dashed green circles mark radii of 1, 2.2, and 3.4 Mpc, respectively. The red (cyan) arrows indicate the best-fit directions measured in the inner (outer) annulus. The shaded regions represent the 16th-84th percentile ranges from 1000 bootstrap realizations. The white contours show the reconstructed WL mass map atκ= [0.12,0.24,0.36,0.48,0.6,0.7]. The yellow circles mark cluster member galaxies. The magenta star denotes the reference point adopted for
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