Based on our Hα interferometric observations and CO data, we analyze the structure and kinematics of the gas in an extended region of the Cygnus arm around the recently discovered star WR 142a. We have established that WR 142a and the ionized hydrogen in its immediate neighborhood are associated with the complex of molecular clouds observed in a region with l ∼ 78°–80°30′, b ∼ 2°–3°20′, and V LSR ∼ 4–16 km s −1 . Traces of the action of the stellar wind from WR 142a on the ambient gas have been found to the northeast of the star in a region devoid of dense absorbing foreground clouds. These include very weak thin gas and dust filaments as well as high-velocity components of the Hα profile, which can be interpreted as a possible expansion of the shell swept up by the wind with a velocity as high as 50–80 km s −1 . Giant regions of reduced CO emission dominated by high-velocity motions of ionized hydrogen have been detected. Stars of the Cyg OB2 association and the cluster NGC 6910 can be responsible for these motions.

We investigated the kinematics of ionized gas in an extended (20°×15°) region containing the X-ray Superbubble in Cygnus with the aim of finding the shell swept up by a strong wind from Cyg OB2. Hα observations were carried out with high angular and spectral resolutions using a Fabry-Perot interferometer attached to the 125-cm telescope at the Crimean Observatory of the Sternberg Astronomical Institute. We detected high-velocity gas motions, which could result from the expansion of the hypothetical shell at a velocity of 25–50 km s−1. Given the number of OB stars increased by Knödlseder (2000) by an order of magnitude, Cyg OB2 is shown to possess a wind that is strong enough [L w ≃ (1–2) × 1039 erg s−1] to produce a shell comparable in size to the X-ray Superbubble and to a giant system of optical filaments. Based on our measurements and on X-ray and infrared observations, we discuss possible observational manifestations of the shell swept up by the wind.

The radial velocity fields of molecular clouds, OB stars, and ionized hydrogen in the Cygnus arm ( l ∼ 72°–8°) are analyzed. A gradientΔ V LSR /Δ l in the mean line-of-sight velocities of molecular clouds and ionized hydrogen due to differential Galactic rotation is detected, and two groups of physically and genetically associated objects moving with different line-of-sight velocities are identified. One of the two molecular-cloud complexes ( l ∼77.3°–80°) is located within 1 kpc of the Sun, closer to the inner edge of the arm, whereas the other complex ( l ∼78.5°–85°) lies 1–1.5 kpc from the Sun and is farther from the inner edge of the arm. The residual azimuthal velocities of the objects in both groups are analyzed. The residual azimuthal velocities of the first molecular-cloud complex are directed opposite to the Galactic rotation ( V Θ ∼ −7 km/s), while those of the second complex are near zero or in the direction of Galactic rotation, independent of the distance to the complex ( V Θ ≥ 1 km/s). Like the molecular clouds, stars of the Cygnus arm form two kinematic groups with similar azimuthal velocities. On the whole, the mean azimuthal velocities V Θ for the ionized hydrogen averaged over large areas agree with the velocities of either the first or second molecular-cloud complex. In terms of density-wave theory, the observed differences between the magnitudes and directions of the azimuthal velocities of the kinematic groups considered could be due to their different locations within the arm.

New optical and X-ray observations of the supernova remnant (SNR) G78.2+2.1 are presented. CCD Hα observations with a Fabry-Perot interferometer attached to the 125-cm reflector at the Crimean Station of the Sternberg Astronomical Institute are used to obtain the radial-velocity field toward the SNR and in its vicinity. The brightness distribution and X-ray spectrum of the SNR are obtained from archival ROSAT and ASCA X-ray data. The X-ray image of G78.2+2.1 exhibits a shell structure (ΔR/R≃0.3) and is generally similar to its radio image; a comparison with the radio map at ν=1.4 GHz constructed from archival VLA data reveals the coincidence of features on scales of several arcminutes at the eastern boundary of G78.2+2.1. Weak X-ray emission (an outer shell or a halo of size ≃2°) has been identified for the first time far outside G78.2+2.1. The X-ray emission from G78.2+2.1 is shown to characterize a young adiabatic SNR [MX-ray ≃ 100 M⊙, Vs≃103km s−1, t≃(5–6)×103 years], which probably expands inside the cavity swept up by the progenitor's stellar wind. Searches for the corresponding radio structure are required to elucidate the nature of the outer X-ray shell or halo.

The HI distribution in the region of the radio source Cygnus X and the supernova remnant G78.2+2.1 has been investigated using observations in the 21-cm radio line with an angular resolution of 2.4' obtained on the RATAN-600 radio telescope. Two HI shells can be distinguished: the first (diameter approximate to 7 degrees) surrounds the entire extended thermal radio source Cygnus X, while the second, smaller, one (diameter approximate to 2 degrees) envelops the supernova remnant. Both shells display expansion with velocities exceeding 10 km/s. To compare the HI and ionized-gas velocities, the region was observed in the H-alpha line with a Fabry-Perot interferometer and CCD array on the 125-cm telescope of the Crimean Laboratory of the Sternberg Astronomical Institute. The molecular-gas distribution around Cygnus X is considered on the basis of the CO line emission. The physical parameters of HI shells are determined, and their nature is discussed. The presence of a large HI shell and a cavity in the molecular-gas distribution around Cygnus X indicates that the radio source may form a single structure. The smaller HI shell around G78.2+2.1 could have been created by either the supernova explosion or the stellar wind of the precursor star.

Interferometric H-alpha observations of the system of shells in the region of the Cyg OB1 and Cyg OB3 associations are presented. The ionized-hydrogen radial-velocity field is studied in the region I similar to 725 degrees-79 degrees, b similar to 1 degrees-4 degrees. The main component in the line profile is observed in the radial-velocity interval Delta V-LSR = 2-20 km/s. A decrease in the radial velocity of the main component with longitude is noted, due to the differential rotation of the Galaxy. A comparison of the observed run of mean velocity with that expected for various distances suggests that most of the radiating ionized gas in the direction of Cyg OB1 is at a distance of 1.5-2 kpc. This is consistent with the mean photometric distance to stars in this association. In some regions, a secondary line maximum is observed at high positive or negative velocities, at a level no less than 30-35% of the maximum intensity of the main component. High-velocity motions at negative velocities up to V-LSR = -85 km/s have been observed on multiple occasions, including in interstellar absorption lines in the spectra of the stars of Cyg OB1 and Cyg OB3. The widespread presence of regions with high positive velocities V-LSR = 30-55 km/s is reported here for the first time. The relation between the spatial distributions of the molecular and ionized components of the shell complex is discussed. It is concluded that the multiple-shell system formed as the result of an interaction between the stars of the Cyg OB1 association and a dense molecular complex. At the western edge of the multiple-shell system, there is some contribution from the stars of the Cyg OB3 association, and, at the eastern edge, there is a significant contribution from the stars of Cyg OB9 and from two WR stars at a distance of about 900 pc.

The results of a complex program of research on the extended infrared shell around the nebula NGC 6888 and the star WR 136 are presented. We performed H-alpha observations with a Fabry-Perot interferometer mounted at the focus of the 125-cm telescope and radio continuum (2.7 to 31 cm) and 21-cm H I observations with the RATAN-BOO radio telescope. A thick expanding shell of neutral hydrogen 120 pc in diameter that immediately surrounds the extended infrared shell was detected. This suggests that the infrared shell is a single structure rather than a chance projection of physically unrelated objects. The radial velocity of the H I shell is 11 +/- 1 km s(-1), the expansion velocity is 10 +/- 3 km s(-1), and the mass of the neutral hydrogen in the shell is 10(4)M(.). The bright radio features that we detected in the region of the infrared shell all exhibit a flat spectrum typical of thermal emission from optically thin H II regions, The same inference is probably also true for the nebula Simeiz 55. Our observations are consistent with the assumption of A,P. Marston that the extended shell was formed by the stellar wind from the precursor of WR 136, but they do not rule out the identification with a very old supernova remnant proposed by J. Nichols-Bohlin and R.A. Fesen, either. A revision of the distance to the pulsar PSR J2013+3845 with inhomogeneity of the interstellar medium taken into account allows for its formation during the same supernova explosion some 4 x 10(5) years ago.

We present H alpha interferometric observations of the northwestern part of the gas and dust complex associated with the Cyg OB1 and OB3 associations. The radial-velocity field of ionized hydrogen in the region l similar to 73.5 degrees-77 degrees and b similar to 1.5 degrees-4 degrees is studied. Most of the H alpha-line profiles exhibit the main peak and weak features in the blue wings; in individual regions, a secondary peak with an intensity that reaches 15-30% of the intensity of the main component is observed. The mean radial velocity of the main component systematically decreases from V-LSR = 18-20 km s(-1) in the south of the region to V-LSR = 4-11 km s(-1) in the north. As in our previous studies, we associate the motion of ionized hydrogen at a radial velocity of 4-12 km s(-1), which is determined from the brightest component of the Ha profile, with the differential Galactic rotation. The radial velocities of the weak features in the H alpha-line profile are distributed over the range -100 to -20 km s(-1). In the direction of the nebulae Simeiz 55, G75.6+3.2, and G74.5+2.2, the distribution of secondary peaks in the line profile makes it possible to reliably identify gas flows at mean velocities V-LSR similar to -55, -35, and -33 km s(-1), respectively. We use our decade-long studies of-the kinematics of ionized gas in the multishell complex associated with Cyg OB1 and OB3 to compile an electronic database of radial velocities in the H alpha line. By now we have obtained more than 1000 interference-filter images and measured the radial velocities at more than 9000 points.

We carried out interferometric H alpha observations of the extended IR shell around NGC 6888 and WR 136 in the northwestern part of the gas and dust complex associated with Cyg OB1 and Cyg OB3. High-velocity motions were detected in a small region at the boundary of the IR shell, which we associate with the spherically symmetric shell nebula Simeiz 55. The processing of archival IUE data also revealed interstellar absorption lines in the spectrum of the star HD 228519 (B0.5 V), lying at the center of Simeiz 55, at least in the plane of the sky, at the largest negative velocities encountered in the shell complex. The radial-velocity field in the nebula can be interpreted as an asymmetric expansion of the shell with a velocity of 75 km s(-1). The possibility that the nebula is an unrecognized supernova remnant in the radiative phase is not ruled out.

Interferometric observations of the emission nebulas near the stars WR 141 and WR 142, lying in the southern part of the supershell surrounding the Cyg OB1 association, have been conducted in the H(alpha) line. The radial-velocity field of a sky area about 1 degree2 in size was investigated using a folding optical system, which comprised a Fabry-Perot interferometer and an image intensifier, attached to the 125-cm and 60-cm reflectors. The ionized hydrogen in the filament surrounding the star WR 142 was shown to emit at about 10 km s-1, whereas its emission near the star WR 141 was found to occur in the velocity range 0 to 12 km s-1. A weaker H(alpha) emission was also detected at high negative (V(LSR) approximately 50 km s-1) and positive (V(LSR) approximately 20 - 45 km s-1) velocities. In the sky area under study, low-brightness regions around both stars were identified at velocities of 7.5 to 10 km s-1 (WR 141) and of 10 to 12.5 km s-1 (WR 142), which are close to the velocity of the main H(alpha)-line component, using the available distribution of CO emission. These velocities correspond to the far edge of the molecular-cloud complex. High-velocity motions in the H(alpha) line and cavities in the distribution of CO emission are likely to be caused by the ionizing radiation and wind arising from the stars WR 141 and WR 142.

Monochromatic [OIII] and [NII] observations and interferometric H(alpha) observations of the HII nebula, connected with stars WR 134 and WR 135, have been carried out. The radial velocity field of this nebula was investigated. Basing on nebula morphology and kinematics, we supposed that the closed elliptical emission shell, including the nebula Anon MR 100, was formed by WR 134 stellar wind action. The investigated shell is a part of the hierarchical shell system in the region of the associations Cyg OB1 and OB3, at least, in the sky plane. It is shown that the star WR 134 has blown a shell al the edge of the parent molecular cloud, emitting at the velocity 5-7 km/s. Because of the inhomogeneous density distribution in the surrounding medium, the shell's expansion was not the same in the different directions: inside the cloud at a velocity close to 20 km/s, and outward in the northern direction at a velocity about 50 km/s.

A faint shell-like nebula has been identified as a possible optical counterpart of the radio supernova remnant G73.9 + O.9. The interferometric observations of the nebula in the H(alpha) line have been carried out using Fabry - Perot plates and an image converter with a focus reducing camera on the 125-cm and 60-cm telescopes. The results of our interferometric observations confirm the identification of the SNR's optical emission. The FWHM of the H(alpha) line in the nebula was found to be around 100-120 km/s as compared with 50-100 km/s outside the radio source G73.9+ + 0.9. An upper limit of expansion velocity or the nebula is found to be about 50 km/s. A genetical relation between the hierarchical system of the shells around Cyg OBI and the SNR is possible, being supported by the kinematic distance of about 0,5-2 kpc, as it follows from the mean radial velocity of the nebula v(LSR) = 4 +/- 3 km/s.