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<jats:title>Abstract</jats:title> <jats:p>We augment the heliospheric network of galactic cosmic ray (GCR) monitors using 2012–2017 penetrating radiation measurements from the New Horizons (NH) Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI), obtaining intensities of ≳75 MeV particles. The new, predominantly GCR observations provide critical links between the Sun and Voyager 2 and Voyager 1 (V2 and V1), in the heliosheath and local interstellar medium (LISM), respectively. We provide NH, Advanced Composition Explorer (ACE), V2, and V1 GCR observations, using them to track solar cycle variations and short-term Forbush decreases from the Sun to the LISM, and to examine the interaction that results in the surprising, previously reported V1 LISM anisotropy episodes. To investigate these episodes and the hitherto unexplained lagging of associated in situ shock features at V1, propagating disturbances seen at ACE, NH, and V2 were compared to V1. We conclude that the region where LISM magnetic field lines drape around the heliopause is likely critical for communicating solar disturbance signals upstream of the heliosheath to V1. We propose that the anisotropy-causing physical process that suppresses intensities at ∼90° pitch angles relies on GCRs escaping from a single compression in the draping region, not on GCRs trapped between two compressions. We also show that NH suprathermal and energetic particle data from PEPSSI are consistent with the interpretation that traveling shocks and corotating interaction region (CIR) remnants can be distinguished by the existence or lack of Forbush decreases, respectively, because turbulent magnetic fields at local shocks inhibit GCR transport while older CIR structures reaching the outer heliosphere do not.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We report on the results of a new spectroscopic monitoring campaign of the quasar PG 0026+129 at the Calar Alto Observatory 2.2 m telescope from 2017 July to 2020 February. Significant variations in the fluxes of the continuum and broad emission lines, including H<jats:italic>β</jats:italic> and He <jats:sc>ii</jats:sc>, were observed in the first and third years, and clear time lags between them are measured. The broad H<jats:italic>β</jats:italic> line profile consists of two Gaussian components: an intermediate-width H<jats:inline-formula> <jats:tex-math> <?CDATA ${\beta }_{\mathrm{IC}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn1.gif" xlink:type="simple" /> </jats:inline-formula> with an FWHM of 1964 ± 18 <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{km}\,{{\rm{s}}}^{-1}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn2.gif" xlink:type="simple" /> </jats:inline-formula> and another very broad H<jats:inline-formula> <jats:tex-math> <?CDATA ${\beta }_{\mathrm{VBC}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn3.gif" xlink:type="simple" /> </jats:inline-formula> with an FWHM of 7570 ± 83 <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{km}\,{{\rm{s}}}^{-1}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn4.gif" xlink:type="simple" /> </jats:inline-formula>. H<jats:inline-formula> <jats:tex-math> <?CDATA ${\beta }_{\mathrm{IC}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn5.gif" xlink:type="simple" /> </jats:inline-formula> has long time lags of ∼40–60 days in the rest frame, while H<jats:inline-formula> <jats:tex-math> <?CDATA ${\beta }_{\mathrm{VBC}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn6.gif" xlink:type="simple" /> </jats:inline-formula> shows nearly zero time delay with respect to the optical continuum at 5100 Å. The velocity-resolved delays show consistent results: lags of ∼30–50 days at the core of the broad H<jats:italic>β</jats:italic> line and roughly zero lags at the wings. H<jats:inline-formula> <jats:tex-math> <?CDATA ${\beta }_{\mathrm{IC}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn7.gif" xlink:type="simple" /> </jats:inline-formula> has a redshift of ∼400 <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{km}\,{{\rm{s}}}^{-1}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn8.gif" xlink:type="simple" /> </jats:inline-formula>, which seems to be stable for nearly 30 yr by comparing with archived spectra, and may originate from an infall. The rms spectrum of H<jats:inline-formula> <jats:tex-math> <?CDATA ${\beta }_{\mathrm{VBC}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn9.gif" xlink:type="simple" /> </jats:inline-formula> shows a double-peaked profile with brighter blue peak and extended red wing in the first year, which matches the signature of a thin disk. Both the double-peaked profile and the near-zero lag suggest that H<jats:inline-formula> <jats:tex-math> <?CDATA ${\beta }_{\mathrm{VBC}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn10.gif" xlink:type="simple" /> </jats:inline-formula> comes from a region associated with the part of the accretion disk that emits the optical continuum. Adopting the FWHM (in the rms spectrum) and the time lag measured for the total H<jats:italic>β</jats:italic> line, and a virial factor of 1.5, we obtain a virial mass of <jats:inline-formula> <jats:tex-math> <?CDATA ${2.89}_{-0.69}^{+0.60}\times {10}^{7}\,{M}_{\odot }$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabc2daieqn11.gif" xlink:type="simple" /> </jats:inline-formula> for the central black hole in this quasar.</jats:p>