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1. First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A

   https://doi.org/10.3847/2041-8213/ae0c04  

   Cortés, P C; Pineda, J E; Hsieh, T-H; Tobin, J J; Saha, P; Girart, J M; Le_Gouellec, V_J M; Stephens, I W; Looney, L W; Koumpia, E; et al (October 2025, The Astrophysical Journal Letters)

   Abstract We present the first results from the Atacama Large Millimeter/submillimeter Array Perseus Polarization Survey, focusing on the magnetic field in the SVS 13A circumbinary disk. The data set includes full Stokes dust continuum observations at $\sim 0\stackrel{″}{.}3$ and 870μm, as well as molecular line emission from C¹⁷O(J = 3 → 2) at $\sim 0\stackrel{″}{.}3$ , C¹⁸O(J = 2 → 1) at $\sim 0\stackrel{″}{.}2$ , and DCN(J = 3 → 2) at $\sim 0\stackrel{″}{.}1$ angular resolution. Our observations resolve both a previously identified dust spiral and an infalling streamer, capturing their spatial and kinematic structures. The streamer is traced from scales >300 au down to the circumbinary disk. Using alignment measure (AM) maps and histograms that compare the orientations of the plane-of-sky magnetic field with local intensity and velocity gradients, we find that the AM distribution peaks at a value of 1. This AM peak strongly suggests alignment between the field and the dust total intensity emission, as well as between the field and the gas velocity, which in turn suggests grain alignment by magnetic fields. From our data, we derive a magnetic field strength,B_pos ∼ 1.1 ± 0.6 mG, and a kinetic-to-magnetic energy ratio of 0.5 ± 0.4, suggesting magnetic dominance. We also produced a map of the Alfvénic Mach number, finding ${\mathcal{M}}_{\mathrm{A}}<1$ along the streamer, consistent with sub-Alfvénic infalling motions. Therefore, the field is likely facilitating the inflow of material from the envelope onto the disk by constraining movement across the field lines. This represents the first detection of a magnetically sub-Alfvénic infalling streamer in a protostellar system. 

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2. Multi-scale Physical Properties of NGC 6334 as Revealed by Local Relative Orientations between Magnetic Fields, Density Gradients, Velocity Gradients, and Gravity

   https://doi.org/10.3847/1538-4357/acb540  

   Liu, Junhao; Zhang, Qizhou; Koch, Patrick M.; Liu, Hauyu Baobab; Li, Zhi-Yun; Li, Shanghuo; Girart, Josep Miquel; Chen, Huei-Ru Vivien; Ching, Tao-Chung; Ho, Paul T.; et al (March 2023, The Astrophysical Journal)

   Abstract We present ALMA dust polarization and molecular line observations toward four clumps (I(N), I, IV, and V) in the massive star-forming region NGC 6334. In conjunction with large-scale dust polarization and molecular line data from JCMT, Planck, and NANTEN2, we make a synergistic analysis of relative orientations between magnetic fields (θ_B), column density gradients (θ_NG), local gravity (θ_LG), and velocity gradients (θ_VG) to investigate the multi-scale (from ∼30 to 0.003 pc) physical properties in NGC 6334. We find that the relative orientation betweenθ_Bandθ_NGchanges from statistically more perpendicular to parallel as column density ( $N_{{\mathrm{H}}_2}$ ) increases, which is a signature of trans-to-sub-Alfvénic turbulence at complex/cloud scales as revealed by previous numerical studies. Becauseθ_NGandθ_LGare preferentially aligned within the NGC 6334 cloud, we suggest that the more parallel alignment betweenθ_Bandθ_NGat higher $N_{{\mathrm{H}}_2}$ is because the magnetic field line is dragged by gravity. At even higher $N_{{\mathrm{H}}_2}$ , the angle betweenθ_Bandθ_NGorθ_LGtransits back to having no preferred orientation, or statistically slightly more perpendicular, suggesting that the magnetic field structure is impacted by star formation activities. A statistically more perpendicular alignment is found betweenθ_Bandθ_VGthroughout our studied $N_{{\mathrm{H}}_2}$ range, which indicates a trans-to-sub-Alfvénic state at small scales as well, and this signifies that magnetic field has an important role in the star formation process in NGC 6334. The normalized mass-to-flux ratio derived from the polarization-intensity gradient (KTH) method increases with $N_{{\mathrm{H}}_2}$ , but the KTH method may fail at high $N_{{\mathrm{H}}_2}$ due to the impact of star formation feedback. 

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3. Search for Neutrino Emission from Hard X-Ray AGN with IceCube

   https://doi.org/10.3847/1538-4357/ada94b  

   Abbasi, R; Ackermann, M; Adams, J; Agarwalla, S K; Aguilar, J A; Ahlers, M; Alameddine, JM; Amin, N M; Andeen, K; Argüelles, C; et al (March 2025, The Astrophysical Journal)

   Abstract Active galactic nuclei (AGN) are promising candidate sources of high-energy astrophysical neutrinos, since they provide environments rich in matter and photon targets where cosmic-ray interactions may lead to the production of gamma rays and neutrinos. We searched for high-energy neutrino emission from AGN using the Swift-BAT Spectroscopic Survey catalog of hard X-ray sources and 12 yr of IceCube muon track data. First, upon performing a stacked search, no significant emission was found. Second, we searched for neutrinos from a list of 43 candidate sources and found an excess from the direction of two sources, the Seyfert galaxies NGC 1068 and NGC 4151. We observed NGC 1068 at flux ${\varphi }_{{\nu }_{\mu }+{\overline{\nu }}_{\mu }}$ = $4.02_{-1.52}^{+1.58}\times 10^{-11}$ TeV⁻¹cm⁻²s⁻¹normalized at 1 TeV, with a power-law spectral indexγ= 3.10 ${}_{-0.22}^{+0.26}$ , consistent with previous IceCube results. The observation of a neutrino excess from the direction of NGC 4151 is at a posttrial significance of 2.9σ. If interpreted as an astrophysical signal, the excess observed from NGC 4151 corresponds to a flux ${\varphi }_{{\nu }_{\mu }+{\overline{\nu }}_{\mu }}$ = $1.51_{-0.81}^{+0.99}\times 10^{-11}$ TeV⁻¹cm⁻²s⁻¹normalized at 1 TeV andγ= 2.83 ${}_{-0.28}^{+0.35}$ . 

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4. Connection between f-electron correlations and magnetic excitations in UTe2

   https://doi.org/10.1038/s41535-024-00720-9  

   Halloran, Thomas; Czajka, Peter; Saucedo_Salas, Gicela; Frank, Corey E; Kang, Chang-Jong; Rodriguez-Rivera, J A; Lass, Jakob; Mazzone, Daniel G; Janoschek, Marc; Kotliar, Gabriel; et al (December 2025, npj Quantum Materials)

   Abstract The detailed anisotropic dispersion of the low-temperature, low-energy magnetic excitations of the candidate spin-triplet superconductor UTe₂is revealed using inelastic neutron scattering. The magnetic excitations emerge from the Brillouin zone boundary at the high symmetryYandTpoints and disperse along the crystallographic$$\hat{b}$$ $\hat{b}$ -axis. In applied magnetic fields to at leastμ₀H= 11 T along the$$\hat{c}-{\rm{axis}}$$ $\hat{c}-\mathrm{axis}$ , the magnetism is found to be field-independent in the (hk0) plane. The scattering intensity is consistent with that expected from U³⁺/U⁴⁺ f-electron spins with preferential orientation along the crystallographic$$\hat{a}$$ $\hat{a}$ -axis, and a fluctuating magnetic moment ofμ_eff=1.7(5)μ_B. We propose interband spin excitons arising fromf-electron hybridization as a possible origin of the magnetic excitations in UTe₂. 

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5. ALMA-IMF. IX. Catalog and Physical Properties of 315 SiO Outflow Candidates in 15 Massive Protoclusters

   https://doi.org/10.3847/1538-4357/ad0786  

   Towner, A. P.; Ginsburg, A.; Dell’Ova, P.; Gusdorf, A.; Bontemps, S.; Csengeri, T.; Galván-Madrid, R.; Louvet, F. K.; Motte, F.; Sanhueza, P.; et al (December 2023, The Astrophysical Journal)

   Abstract We present a catalog of 315 protostellar outflow candidates detected in SiOJ= 5 − 4 in the ALMA-IMF Large Program, observed with ∼2000 au spatial resolution, 0.339 km s⁻¹velocity resolution, and 2–12 mJy beam⁻¹(0.18–0.8 K) sensitivity. We find median outflow masses, momenta, and kinetic energies of ∼0.3M_⊙, 4M_⊙km s⁻¹, and 10⁴⁵erg, respectively. Median outflow lifetimes are 6000 yr, yielding median mass, momentum, and energy rates of $\dot{M}$ = 10^−4.4M_⊙yr⁻¹, $\dot{P}$ = 10^−3.2M_⊙km s⁻¹yr⁻¹, and $\dot{E}$ = 1L_⊙. We analyze these outflow properties in the aggregate in each field. We find correlations between field-aggregated SiO outflow properties and total mass in cores (∼3σ–5σ), and no correlations above 3σwith clump mass, clump luminosity, or clump luminosity-to-mass ratio. We perform a linear regression analysis and find that the correlation between field-aggregated outflow mass and total clump mass—which has been previously described in the literature—may actually be mediated by the relationship between outflow mass and total mass in cores. We also find that the most massive SiO outflow in each field is typically responsible for only 15%–30% of the total outflow mass (60% upper limit). Our data agree well with the established mechanical force−bolometric luminosity relationship in the literature, and our data extend this relationship up toL≥ 10⁶L_⊙and $\dot{P}$ ≥ 1M_⊙km s⁻¹yr⁻¹. Our lack of correlation with clumpL/Mis inconsistent with models of protocluster formation in which all protostars start forming at the same time. 

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