We present a new catalogue of spectrophotometric distances and line-of-sight systemic velocities to 103 H II regions between 90 • ≤ ℓ ≤ 195 • (longitude quadrants II and part of III). Two new velocities for each region are independently measured using 1-arcminute resolution 21 cm H I and 2.6 mm 12 CO line maps (from the Canadian Galactic Plane Survey and FCRAO Outer Galaxy Surveys) that show where gaseous shells are observed around the periphery of the ionized gas. Known and neighbouring O&B-type stars with published UBV photometry and MK classifications are overlaid onto 21 cm continuum maps, and those stars observed within the boundary of the H II emission (and whose distance is not more than 3 times the standard deviation of the others) are used to calculate new mean stellar distances to each of the 103 nebulae. Using this approach of excluding distance outliers from the mean distance to a group of many stars in each H II region lessens the impact of anomalous reddening for certain individuals. The standard deviation of individual stellar distances in a cluster is typically 20% per stellar distance, and the error in the mean distance to the cluster is typically ±10%. Final mean distances of 9 common objects with VLBI parallax distances show a 1:1 correspondence. Further, comparison with previous catalogues of H II regions in these quadrants shows a 50% reduction in scatter for the distance to Perseus spiral arm objects in the same region, and a reduction by ∼1/ √ 2 in scatter around a common angular velocity relative to the Sun Ω − Ω 0 (km s −1 kpc −1 ). The purpose of the catalogue is to provide a foundation for more detailed large-scale Galactic spiral structure and dynamics (rotation curve, density wave streaming) studies in the 2 nd and 3 rd quadrants, which from the Sun's location is the most favourably viewed section of the Galaxy.

Context. New and existing large-scale radio surveys of the Milky Way at centimetre wavelengths can play an important role in uncovering the hundreds of expected but missing supernova remnants in the Galaxy's interstellar medium. We report on the discovery of two supernova remnants (SNRs) designated G152.4−2.1 and G190.9−2.2, using Canadian Galactic Plane Survey data. Aims. The aims of this paper are, first, to present evidence that favours the classification of both sources as SNRs, and, second, to describe basic parameters (integrated flux density, spectrum, and polarization) as well as properties (morphology, line-of-sight velocity, distance and physical size) to facilitate and motivate future observations. Methods. Spectral and polarization parameters are derived from multiwavelength data from existing radio surveys carried out at wavelengths between 6 and 92 cm. In particular for the source G152.4−2.1 we also use new observations at 11 cm done with the Effelsberg 100 m telescope. The interstellar medium around the discovered sources is analyzed using 1-arcmin line data from neutral hydrogen (H i) and 45-arcsec 12 CO(J = 1 → 0).Results. G152.4−2.1 is a barrel shaped SNR with two opposed radio-bright polarized flanks on the north and south. The remnant, which is elongated along the Galactic plane is evolving in a more-or-less uniform medium. G190.9−2.2 is also a shell-type remnant with east and west halves elongated perpendicular to the plane, and is evolving within a low-density region bounded by dense neutral hydrogen in the north and south, and molecular ( 12 CO) clouds in the east and west. The integrated radio continuum spectral indices are −0.65 ± 0.05 and −0.66 ± 0.05 for G152.4−2.1 and G190.9−2.2 respectively. Both SNRs are approximately 1 kpc distant, with G152.4−2.1 being larger (32 × 30 pc in diameter) than G190.9−2.2 (18 × 16 pc). These two remnants are the lowest surface brightness SNRs yet catalogued at Σ 1 GHz < ∼ 5 × 10 −23 W m −2 Hz −1 sr −1 .

We report the discovery of the new pulsar wind nebula (PWN) G141.2+5.0 in data observed with the Dominion Radio Astrophysical Observatory's Synthesis Telescope at 1420 MHz. The new PWN has a diameter of about 3.5 ′ , which translates at a distance of 4.0 kpc to a spatial extent of about 4 pc. It displays a radio spectral index of α ≈ −0.7, similar to the PWN G76.9+1.1. G141.2+5.0 is highly polarized up to 40 % with an average of 15 % in the 1420 MHz data. It is located in the centre of a small spherical HI bubble, which is expanding at a velocity of 6 km s −1 . The bubble's systemic velocity is −53 km s −1 and could be the result of the progenitor star's mass loss or the shell-type SNR created by the same supernova explosion in a highly advanced stage. The systemic velocity of the bubble shares the velocity of H I associated with the Cygnus spiral arm, which is seen across the 2nd and 3rd quadrants and an active star-forming arm immediately beyond the Perseus arm. A kinematical distance of 4±0.5 kpc is found for G141.2+5.0, similar to the optical distance of the Cygnus arm (3.8±1.1 kpc). G141.2+5.0 represents the first radio PWN discovered in 17 years and the first SNR discovered in the Cygnus spiral arm, which is in stark contrast with the Perseus arm's overwhelming population of shell-type remnants.