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1. On the Interpretation of d o ( x )do(x)

   https://doi.org/10.1515/jci-2019-2002  

   Pearl, Judea (April 2019, Journal of Causal Inference)

   Abstract This paper provides empirical interpretation of the do(x) operator when applied to non-manipulable variables such as race, obesity, or cholesterol level. We view do(x) as an ideal intervention that provides valuable information on the effects of manipulable variables and is thus empirically testable. We draw parallels between this interpretation and ways of enabling machines to learn effects of untried actions from those tried. We end with the conclusion that researchers need not distinguish manipulable from non-manipulable variables; both types are equally eligible to receive the do(x) operator and to produce useful information for decision makers. 

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2. The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3

   https://doi.org/10.3847/2041-8213/aca486  

   Tsygankov, Sergey S.; Doroshenko, Victor; Poutanen, Juri; Heyl, Jeremy; Mushtukov, Alexander A.; Caiazzo, Ilaria; Di Marco, Alessandro; Forsblom, Sofia V.; González-Caniulef, Denis; Klawin, Moritz; et al (December 2022, The Astrophysical Journal Letters)

   Abstract The first X-ray pulsar, Cen X-3, was discovered 50 yr ago. Radiation from such objects is expected to be highly polarized due to birefringence of plasma and vacuum associated with propagation of photons in the presence of the strong magnetic field. Here we present results of the observations of Cen X-3 performed with the Imaging X-ray Polarimetry Explorer. The source exhibited significant flux variability and was observed in two states different by a factor of ∼20 in flux. In the low-luminosity state, no significant polarization was found in either pulse phase-averaged (with a 3 σ upper limit of 12%) or phase-resolved (the 3 σ upper limits are 20%–30%) data. In the bright state, the polarization degree of 5.8% ± 0.3% and polarization angle of 49.°6 ± 1.°5 with a significance of about 20 σ were measured from the spectropolarimetric analysis of the phase-averaged data. The phase-resolved analysis showed a significant anticorrelation between the flux and the polarization degree, as well as strong variations of the polarization angle. The fit with the rotating vector model indicates a position angle of the pulsar spin axis of about 49° and a magnetic obliquity of 17°. The detected relatively low polarization can be explained if the upper layers of the neutron star surface are overheated by the accreted matter and the conversion of the polarization modes occurs within the transition region between the upper hot layer and a cooler underlying atmosphere. A fraction of polarization signal can also be produced by reflection of radiation from the neutron star surface and the accretion curtain. 

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3. The BIG X-ray tail

   https://doi.org/10.1093/mnrasl/slab108  

   Ge, Chong; Sun, Ming; Yagi, Masafumi; Fossati, Matteo; Forman, William; Jáchym, Pavel; Churazov, Eugene; Zhuravleva, Irina; Boselli, Alessandro; Jones, Christine; et al (October 2021, Monthly Notices of the Royal Astronomical Society: Letters)

   ABSTRACT Galaxy clusters grow primarily through the continuous accretion of group-scale haloes. Group galaxies experience preprocessing during their journey into clusters. A star-bursting compact group, the Blue Infalling Group (BIG), is plunging into the nearby cluster A1367. Previous optical observations reveal rich tidal features in the BIG members, and a long H α trail behind. Here, we report the discovery of a projected ∼250 kpc X-ray tail behind the BIG using Chandra and XMM–Newton observations. The total hot gas mass in the tail is ∼7 × 1010 M⊙ with an X-ray bolometric luminosity of ∼3.8 × 1041 erg s−1. The temperature along the tail is ∼1 keV, but the apparent metallicity is very low, an indication of the multi-T nature of the gas. The X-ray and H α surface brightnesses in the front part of the BIG tail follow the tight correlation established from a sample of stripped tails in nearby clusters, which suggests the multiphase gas originates from the mixing of the stripped interstellar medium (ISM) with the hot intracluster medium (ICM). Because thermal conduction and hydrodynamic instabilities are significantly suppressed, the stripped ISM can be long lived and produce ICM clumps. The BIG provides us a rare laboratory to study galaxy transformation and preprocessing. 

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4. The Mellin moments and for the pion and kaon from lattice QCD

   Constantia Alexandrou, Simone Bacchio (January 2020, Physical review)

   null (Ed.)

   under Review 

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5. Accretion geometry of the neutron star low mass X-ray binary Cyg X-2 from X-ray polarization measurements

   https://doi.org/10.1093/mnras/stac3726  

   Farinelli, R; Fabiani, S; Poutanen, J; Ursini, F; Ferrigno, C; Bianchi, S; Cocchi, M; Capitanio, F; De Rosa, A; Gnarini, A; et al (January 2023, Monthly Notices of the Royal Astronomical Society)

   ABSTRACT We report spectro-polarimetric results of an observational campaign of the bright neutron star low-mass X-ray binary Cyg X-2 simultaneously observed by IXPE, NICER, and INTEGRAL. Consistently with previous results, the broad-band spectrum is characterized by a lower-energy component, attributed to the accretion disc with kTin ≈ 1 keV, plus unsaturated Comptonization in thermal plasma with temperature kTe = 3 keV and optical depth τ ≈ 4, assuming a slab geometry. We measure the polarization degree in the 2–8 keV band P = 1.8 ± 0.3 per cent and polarization angle ϕ = 140° ± 4°, consistent with the previous X-ray polarimetric measurements by OSO-8 as well as with the direction of the radio jet which was earlier observed from the source. While polarization of the disc spectral component is poorly constrained with the IXPE data, the Comptonized emission has a polarization degree P = 4.0 ± 0.7 per cent and a polarization angle aligned with the radio jet. Our results strongly favour a spreading layer at the neutron star surface as the main source of the polarization signal. However, we cannot exclude a significant contribution from reflection off the accretion disc, as indicated by the presence of the iron fluorescence line. 

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