  Since its formation 4.6 billion years ago, our solar system has most likely
crossed numerous magnetized interstellar clouds and bubbles of different sizes
and contents on its path through the Milky Way. Having a reference model for
how the heliosphere and interstellar winds interact is critical for
understanding our current Galactic environment, and it requires untangling the
roles of two major actors: the time-variable solar wind and the local
interstellar magnetic field. Numerical simulations predict a distortion of the
heliosphere caused by both solar wind anisotropy and interstellar magnetic
field orientation. However, model comparison to deep space probes' measurements
led to contradictory reports by Voyager 1 and Voyager 2 of both several
crossings of the solar wind's termination shock and of the strength of the
local interstellar field, with values ranging from 1.8 to 5.7 {\mu}G. Here, we
show that Voyager 1 & 2 plasma, fields, and Lyman-{\alpha} sky background
measurements, as well as space observations of high-energy particles of
heliospheric origin, may all be explained by a rather weak interstellar field
2.2 +/- 0.1 {\mu}G pointing from Galactic coordinates (l,b) \sim (28, 52)+/-
3{\deg}. For the 2000 epoch Ulysses-based helium parameters assumed thus far,
the interstellar bow shock must exist. By contrast, using the 2010 epoch
IBEX-based He parameters and a stronger magnetic field leads to a plasma
configuration that is not consistent with the Voyagers TS crossings. For the
newly proposed interstellar He parameters, more simulations are required before
one may determine whether the interstellar bow shock truly does disappear under
those assumptions.
