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A new method for measuring the global magnetic field structure of theGalactic plane is presented. We have determined the near-infrared polarizationof field stars around 52 Cepheids found in recent surveys toward the Galacticplane. The Cepheids are located at the galactic longitudes $-10^{\circ}\leq \,l\, \leq +10.5^{\circ}$ and latitudes $-0.22^{\circ}\leq \, l\, \leq+0.45^{\circ}$, and their distances are mainly in the range of 10 to 15 kpcfrom the Sun. Simple classification of the sightlines is made with thepolarization behavior vs. $H-K_{\mathrm S}$ color of field stars, and typicalexamples of three types are presented. Then, division of the field stars ineach line of sight into (a) foreground, (b) bulge, and (c) background is madewith the $Gaia$ DR2 catalog, the peak of the $H-K_{\mathrm S}$ color histogram,and $H-K_{\mathrm S}$ colors consistent with the distance of the Cepheid in thecenter, respectively. Differential analysis between them enables us to examinethe magnetic field structure more definitely than just relying on the$H-K_{\mathrm S}$ color difference. In one line of sight, the magnetic field isnearly parallel to the Galactic plane and well aligned all the way from the Sunto the Cepheid position on the other side of the Galactic center. Contrary toour preconceived ideas, however, sightlines having such well-aligned magneticfields in the Galactic plane are rather small in number. At least 36 Cepheidfields indicate random magnetic field components are significant. Two Cepheidfields indicate that the magnetic field orientation changes more than 45 in theline of sight. The polarization increase per color change $P$/ ($H-K_{\mathrmS}$) varies from region to region, reflecting the change in the ratio of themagnetic field strength and the turbulence strength.

Magnetic field structure of the Galactic plane from differential analysis of interstellar polarization