Supernova remnants and content in high mass stars of the giant Hii region NGC 604

An optical survey of NGC 604, the brightestHII complex in M33, has lead to the discovery of a single supernova remnant, in agreement with the predominantly thermal radio spectrum of the region. For the same NGC 604, we have derived from the H flux and the evolutionary tracks of the stars, the population and the birth-rates of Main Sequence, high-mass stars. The computation is in agreement with the observations of the upper part of the stellar luminosity function. From the stellar population one predicts in the region a number of remnants significantly larger than 1. To explain this discrepancy, it is suggested the presence in NGC 604 of at least one overluminous, hot star (M _B9), which contributes to a large fraction of the ionizations.On leave from the Asiago Observatory.On leave from Istituto di Fisica Generale, Università di Torino.     

Markarian 313: An intermediate object between a seyfert and a starburst galaxy

An ultraviolet-excess galaxy Markarian 313 (NGC 7465), which consists of a multiple system with NGC 7463 and NGC 7464, is studied using the low- and high-resolution optical spectrum. Emission lines of H, H, [NII], and [OIII] have conspicuous blueward asymmetrical wings or blue slanted profiles in the spectrum of the nuclear region of the galaxy. The width of these emission lines is as broad as 600 km s^–1 at the zero-intensity level, and the velocity difference between the narrow and broad components is estimated at around 80 km s^–1 from the two-component Gaussian profile fitting. This fact could be an evidence of a large-scale dynamical motion in or surrounding the nuclear region of the galaxy, implying that it bears an intermediate characteristic between a Seyfert and a starburst galaxy.     

Nebular complex in the region of Cas OB2 association; ring nebula Sh157

This paper presents the results of monochromatic [Oiii], [Nii], and [Sii] observations of ring nebula Sh157 around the star (WR + B0III) HD 219460 belonging to the Ba 3 cluster. A stratification of radiation typical for photoionization excitation has been revealed. The observations suggest that the Sh157 ring structure may arise as a result of the HD 219460 stellar wind blowing the surroundingHii region, and the bubble age is found to bet(2–5)×10⁵ yr. Three outer envelopes have been distinguished: a weaker extended emission shell apparently blown out by the wind from B-stars of the Ba 3 cluster, and two dust shells which are likely to be associated with NGC 7510 and Cas OB2. The paper is also concerned with the discussion of young star aggregates Ba 3, NGC 7510, Cas OB1, OB2, OB4, OB5, OB7, and Cep OBI and the associatedHii regions, shells and supershells of gas and dust, molecular clouds, and supernova remnants which may be probable members of a single giant stellar complex where the star formation process is in progress.     

Pseudo-resonance absorption lines in planetary nebulae: Discovery?

The possibility of the formation of pseudo-resonance absorption lines in planetary nebulae is predicted only theoretically. However, this has not been confirmed by direct observations. In the present article an attempt has been made to show, as a result of careful analysis of IUE spectral recordings for a group of planetary nebulae, that the existence of one pseudo-resonance line 1300 SiIII is without doubt at least in spectra of three planetary nebulae: NGC 2610, NGC 3587, and NGC 6891. The presence of this line in the spectra of the other three planetary nebulae, NGC 6210, IC 3568, and IC 4776, seems to be probable. The role of the interstellar selective absorption, the blending effect by the resonance lines of SiII,Oi, andSi in the formation of the pseudo-resonance line 1300 SiIII as well as the possibility of formation of this line in the photosphere of central star of nebula were analysed.     

The electron temperature distributions and internal kinematics of seven diffuse nebulae

A Fabry-Pérot spectrophotometer is used to derive values of the intensity ratio H/[Nii] at 98 points in the seven bright diffuse nebulae M8, M20, M16, M17, NGC7000, M42, IC434. The fraction of nitrogen in the singly ionized state is estimated in the different objects, and is found to be sufficiently constant within any one nebula so that the above intensity ratio may be used to derive accurate electron temperature distributions. The position of the peak of the nebular line, its excess non-thermal width, its shape and relative intensity are used to derive kinematical models of these objects.It is found that values of H/[Nii]1 are representative of the bright central cores of these nebulae. Temperatures between 7000K and 12000K were derived in the different objects. Although some of this apparent variation is due to the different conditions of excitation in the various nebulae, it is shown that a convincing progression of temperature in M8, M16, M17 is supported by radio recombination line results. The temperature variation within any one object was generally significantly less than 1500K.No evidence was found for velocities of mass motion at more than twice the speed of sound. Relative radial velocities of generally less than 15 km sec^–1 characterized the velocity fields of M8, M20, M16, M42. The velocities in M17 were measured as about 20 km sec^–1. Motions in NGC 7000 and IC 434 were much lower (5 km sec^–1) although here the number of points taken was too small to construct meaningful kinematical models.It is concluded that the internal motions of radiatively ionizedHii regions of Pop. I will not significantly affect the results of existing surveys for determining the rotation of the galaxy with radial velocities deduced from nebular emission lines.     

Observations des bords brillants dans NGC 281, IC 434 et M 16

Sommaire Les photographies monochromatiques en H, [Nii] 6584 et [Oiii] 5007 ont été obtenues sur NGC 281, IC 434 et M 16 eu vue de la détection et de l'étude des bords brillants. A partir de ces photos, on accède à la carte d'égal rapport [Nii]/H grâce à la méthode décrite par Louise et Sapin (1972). A l'exclusion des bords brillants, ce rapport varie très peu à l'intérieur d'une même nébuleuse. Par contre à l'approche des fronts d'ionisation, il augmente de façon spectaculaire et systématique.Le renforcement de la raie [Oiii] vers les bords brillants suggère la présence des inhomogénéités (globules ou/et filaments) et le rôle possible que jouent les mécanismes d'échange de charges étudiés par Aller et Keyes (1980).

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Observations of bright rims in NGC 281, IC 434 and M 16

Monochromatic plates are obtained in H, [Nii] 6584 and [Oiii] 5007 lines for three Hii regions: NGC 281, IC 434 and M 16. They allow both detection and physical studies of bright rims. Indeed, it is shown that bright rims appear most contrasted on [Nii] and [Oiii] plates. Furthermore, maps of ratio [Nii]/H are derived from the method described by Louise and Sapin (1972). This ratio remains practically constant within the nebula, except for bright rims where it increases. This may be understood by means of both increasing abundanceN(N⁺/N(H⁺) and temperature following to the model of Mallik (1975).The [Oiii] enhancement towards bright rims in M 16 suggests the presence of inhomogeneities (globules or/and filaments) and the possible role played by charge exchange mechanisms as pointed out by Aller and Keyes (1980).

     

Interferometric study of NGC 7793

Results of H interferometric observations of NGC 7793 are reported. This galaxy contains about 93 HII regions and a general emission background. Its radial velocity is 215 km s^–1.The total mass is low, 2–3×10⁹ solar masses, as well as the average density; the meanM/L is 0.4 suggesting a high proportion of young objects.     

Mesure des Raies de [Sii] dans Trois Nébuleuses planétaires de L'hémisphère Austral

Three southern planetary nebulae (NGC 2818, He 2-130, and NGC 3132) have been observed with the IDS (Image Dessector Scanner) combined with the Boller and Chivens spectrograph mounted at the Cassegrain focus of the 1.52 m telescope of the ESO in Chile. The spectrograph dispersion was 60 Å mm^–1 in the spectral range 6170–7298 Å. The slit aperture was 4×4. Spectra were obtained from an array of positions across each nebula along the E-W direction and/or N-S direction. The data reduction followed the standard IHAP routines for IDS observations. In order to derive electron density, only the [Sii] lines (6617 Å–6731 Å) are given in this paper. The results are in agreement with a shell structure for the observed nebulae.

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Toutes les observations ont été faites à l'Observatoire européen Austral (ESO) au Chili.     

The baryon-symmetric domain cosmology and the cosmic X-ray background

The baryon-symmetric domain cosmology (BSDC) of Steckeret al. (1971) have explained the diffuse -ray background. However, evidence has shown that active galactic nuclei (AGNs) are likely contributors to the diffuse -ray background, so there are some problems with the original formulations. We have reviewed the original formulations and have modified the expressions for the matter temperature and the redshifts at which the cosmic radiation from the BSDC becomes significantly absorbed. In this way, we show that the cosmic radiation from the BSDC agrees remarkably with the cosmic X-ray background from 1 keV to 100 keV. We have also shown that AGNs contribute significantly to the cosmic background beyond 100 keV. Therefore, we have arrived at a consistent model in which the BSDC model and AGN model together can explain the cosmic background from 1 keV to 1 MeV.     

Type I supernova 1974g in NGC 4414

Photographic image-tube spectra (150 Å mm^–1, 4500 Å-7000 Å) of the type I supernova (1974g) in the Sc galaxy NGC 4414 obtained at phases+ 14 days and + 40 days past maximum light have been reduced to absolute flux. The positions of various spectral features and the overall appearance of the spectra of SN 1974g closely match previously observed type I SN spectra at similar phases. An electronographic isophotal map of NGC 4414 is presented, and an accurate position of SN 1974g given. A distance to NGC 4414 of 15 Mpc was determined from the recessional velocities and the diameters of Hii regions; while the absolute magnitude at maximum light of SN 1974g was found to beM _B(max)=–19.0. Estimates of the radius of the expanding photosphere of SN 1974g, cetermined by two independent methods, giveR10¹⁵ cm in the early post-maximum phases. The time of outburst,t=–25 days, has been estimated for SN 1974g. By assuming the broad emission feature observed at 6480 Å to be H, very rough estimates of the electron density and the mass of ionized hydrogen in the expanding supernova envelope are given. The total (observed) luminous energy of SN 1974g was 10⁵¹ erg.     

Observations of the planetary nebula NGC 6853 at [Nii] 6584 Å

New Observations of the [Nii]6584 Å line have been made over the surface of the Dumbell nebula (NGC 6853). The observed lines at the centre of the nebula disc exhibited line splitting of 54.3 km s^–1. The lines appeared double at the centre of the nebula and became single at the boundary. These observations are discussed and compared with those obtained by previous workers.     

Evidence for supernova-induced star formation in the monoceros OB2 association

The Monoceros ring, a circular optical nebulosity 3°.5 in diameter and centred at R.A.=6^h37^m, Dec.=6°30 (l ⁱⁱ =205°.5,b ⁱⁱ =0°.2) is in good structural agreement with radio observations. A neutral hydrogen shell is also accurately projected on the ring. These observations are consistent with the Monoceros ring being a supernova remnant 90–100 pc in diameter expanding at about 45 km s^–1 and having an age of the order of a million years. Bright Hii regions containing early-type stars (e.g., galactic cluster NGC 2244 in the Rosette nebula) and extremely young stars of the OB association Mon OB2 lie at the edges of the ring. The positional and temporal coincidence of the Mon OB2 association with a supernova remnant suggests that probably the star formation in this region is induced or speeded up by the passage of a supernova shock wave through the clumpy interstellar medium.     

On peculiarities of the H and K Ca ii lines of quiescent prominences

A study of the metallic lines in bright quiescent prominences indicates that the optical thickness in the K line of Ca ii may reach values as high as 10³. This is about 10 times larger than the optical thickness in the H line and may explain some peculiarities of the H and K lines in solar prominences.     

The structure of a typical double-ring planetary nebula NGC 2392

Monochromatic photographs in H, [Nii] 6584 and [Oiii] 5007 Å show many different details in the morphological structure of the Eskimo Nebula (NGC 2392). H and [Nii] images show, in a first approximation, similar structure (elliptical inner ring and broken outer ring) whereas both rings in [Oiii] are quite circular and regular in brightness. A photometric study using the method described by Louise (1974) gives various geometrical parameters of both rings which are practically the same for the observed lines. In other words, the classical stratification structure in planetary nebulae is not clearly observed in NGC 2392, in good agreement with previous observations (Wilson, 1950). This fact is probably a consequence of the peculiar structure in the geometry of the nebula. A model consisting of an inner toroid surrounded by a spherical shell is proposed to account for both photometric and spectroscopic observations.     

Star formation in NGC5471

We present a study of the star formation in the giant Hii region NGC5471 in the outskirts of M101. We have performed integrated photometry of the mean emission knots. Stellar population analysis with the code chorizos is compatible with the hypothesis that these regions have at least two different populations. The color–magnitude diagram of the region as derived from Hubble Space Telescope/WPFC2 stellar photometry shows that star formation has been going on for the last 70 Myr.     

Une étude morphologique de NGC 650-1

Résumé L'apparence plus diffuse en H qu'en [Nii] 6584 des arches filamentaires de NGC 650-1 est bien visible sur les photographies obtenues par Louise (1982).Cet auteur suggère que ceci est peut être le résultat de la diffusion plus rapide des ions H⁺ par rapport aux ions N⁺, ces derniers étant 14 fois plus lourds.Nous montrons cependant dans cet article que la diffusion relative des divers types d'ions est négligeable dans les nébuleuses planétaires.Les observations de Louise (1982) peuvent cependant être interprétées par un effet de structure d'ionisation, l'azote se présentant à l'état N⁺⁺ dans la région la plus interne des arches filamentaires. Dans un autre domaine, les observations de Sabbadin et Hamzaoglu (1981) suggèrent que NGC 650-1 n'as pas de symétrie axiale.Nous montrons que deux causes physiques distinctes sont nécessaires pour expliquer ce résultat: la rotation du noyau qui a éjecté la nébuleuse planétaire et le champ magnétique intranébulaire, l'axe de rotation stellaire n'étant pas exactement parallèle à l'axe magnétique.

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A morphological study of NGC 650-1

Long-exposure plates have been made on NGC 650-1 by Louise (1982). One of the typical features is the filamentary structure which appears sharper in [Nii] than in H.This author suggests that the H image is fuzzy because the hydrogen ions diffuse more rapidly than nitrogen ions. We show, however, that the relative diffusion of various ions is negligible in planetary nebulae. Therefore, Louise's suggestion must be rejected.The observations of this author can be interpreted by means of an ionization effect, nitrogen being present in N⁺⁺ state within the most internal part of filamentary arches.On the other hand, observations made by Sabbadin and Hamzoglu (1981) suggest that NGC 650-1 does not possess axial symmetry. We show that two physical mechanisms are necessary to explain it: rotation of nucleus which has ejected the planetary nebulae, and intranebular magnetic field; the magnetic axis being not parallel to the rotation axis.

     

Radio emission of the NGC 1499 nebula at decametric wavelengths

Observations of the ionized hydrogen region NGC 1499 have been carried out with the radio telescope UTR-2 at frequencies 12.6, 14.7, 16.7, 20 and 25 MHz. The half-power resolution of the instrument to zenith is 28×34 at 25 MHz. The average volume density of the non-thermal radio emission between the Sun and the nebula (1.75×10^–40 W m^–3 Hz^–1 ster^–1 at 25 MHz), the electron temperature of the HII nebula (T _e =4400 K), the measure of emission (ME=1500 cm^–6 pc) and other parameters have been obtained. Maps of brightness distribution over the source are presented for each observation frequency. The results are compared with previously obtained data.     

Hii region statistics in spirals

From high-resolution maps of the spiral galaxies NGC 3992 and NGC 4321, obtained with the TAURUS camera at the 4.2 m William Herschel Telescope, we have inferred: (a) The total number of separately identifiableHii regions in their discs classified according to their membership of a spiral arm or the interarm disc, (b) the radial distribution ofHii regions, (c) the frequency distribution of diameters ofHii regions, (d) the luminosity function; each parameter rpesented separately for theHii regions in the arms and in the interarm region, showing the differences between them. From these observations we have also derived the radial dependence of the product of the filling factor, the electron density, and the ionized hydrogen density, which does not appear to change between arm and interarm disc.Paper presented at the 11th European Regional Astronomical Meetings of the IAU on New Windows to the Universe, held 3–8 July, 1989, Tenerife, Canary Islands, Spain.     

Physical conditions in NGC 6164-5

From spectroscopic observations of the emission lines H, 4959 and 5007[Oiii], H, 6584[Nii], 6717 and 6731[Sii] and some interferometric data in H and [Nii] it was established that NGC 6164 and NGC 6165 have characteristics of normal Hii regions for Ne and Te. They are embedded in a very tenuous medium nearly coincident with the Strömgren sphere of the central star HD 148937, corresponding to the outer peripheral structure described by Westerlund. Variations of the relative abundances of N, O, and S are discussed.     

Local interstellar medium

This paper reviews and analyses various observational data about the local interstellar medium (LISM)-a volume with a radius of about 200 pc near the Sun. There are collected radio, IR, optical, UV, and X-ray observations of the ISM and data on the Sco-Cen association. All available information confirms Weaver's (1979) conclusions that the Sun is located near an edge of a giant cavern with a radius of about 180 pc and the cavern center coincides with the Sco-Cen associated center. The outer rim of the cavern is observed as numerous, very longHi flaments, filaments of the interstellar polarization, and soft X-rays radiated by coronal gas with a temperature of about 10⁶K. Close environment (from 10^–4 to 2–5 pc) of the Sun is filled by warm (about 10⁴ K)Hi with the number density 0.1–0.2 cm^–3, which is a corona of the local cloud of the ISM. The central part of the cloud is observed to the galactical center direction at a distance of 10–20 pc as Sancini and van Woerden's (1970)Hi filament. The cloud blown round by stellar winds has a horseshoe-like shape, bordering the Sun. Tinbergen's (1982) patch of polarization is observational evidence of the shape.Several arguments are given to show that the bright spots of soft X-rays (130–284 eV) near the galactic poles are produced by an interaction of stellar winds with outer edge of the local cloud near the ends of the patch of polarization. Lyman continuum radiation from Sco-Cen stars was shown to be probably the main source of ionization of extendedHii regions of low density in the LISM. Various data evidence that the North Polar Spur is a SNR in the local cavern with the age of about 10⁵ years. Interaction of the local cavern with an interstellar absorption-free tunnel stretched for more than 1 kpc along the galactical longitudel=240° is discussed. In conclusion several actual problems of investigation of the LISM were formulated.