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NASA NTRS1983

Discovery of large radial velocities in the supernova remnant 3C 58

New spectroscopic observations of four filaments in 3C 58, three of which appear close to the remnant's radio center, are described. Observed line intensities and radial velocities are presented which indicate a high radial expansion velocity for the object and nearly zero radial velocities for filaments located along the remnant's edge. Large velocities are present nearer the remnant's center up to a maximum of about 900 km/s. These velocities strongly support the identification of 3C 58 as the remnant of the historical supernova seen in AD 1181. A crude estimate of the reddening of the object is made. The observed H-alpha/H-beta ratio of about six suggests only a modest amount of extinction. The object is unlikely to possess a mean expansion velocity of 10,000 km/s over 800 yr, and a previously estimated distance to the object of about 8 kpc is thus improbable.

Fesen, R. A.↗

NASA NTRS1983

cD galaxy dynamics and an aged ridge (jet) in 3C 338

The results of VLA observations and possible models for the peculiar structure of 3C 338, a two-arcmin radio source associated with the cD galaxy NGC 6166 in Abell 2199, are presented. The optical parameters for Abell 2199 and NGc 6166 are reviewed, and the VLA observations and reductions are described. The radio structure of 3C 338 including spectral index and polarization distributions are also discussed. Two possible origins for the ridge structure located to the south of the core which has some characteristics of a jet are proposed. The first involves a cooling accretion flow of ICM material onto the cD. The ram pressure of a highly asymmetric flow seems to be sufficient to confine the radio ridge using an accretion rate of 100 solar masses/yr. The second model presumes that the ridge is actually an aged radio jet. The radio engine would have to be intermittent with a period of about ten million years.

White, R. A.↗

NASA NTRS1983

Millimeter and submillimeter observations of 3C 273

The first detection of 3C 273 (1226 + 023) at wavelengths of 107, 240, and 400 microns together with contemporary measurements at 800 microns, 1.1, 1.9, 3.3, and 8.9 mm, is reported. These observations show that the continuum spectrum of 3C 273 can be extrapolated smoothly from the submillimeter to the infrared with a constant spectral index. There is no evidence of thermal emission from dust. It is shown that the spectrum is consistent with optically thin synchrotron emission from a relativistic beam at a small angle to the line of sight.

Glaccum, W.↗

NASA NTRS1984

What bends 3C 465?

This paper studies the interaction of the prototypical wide-angle tailed radio source 3C 465 with the ambient cluster gas. 3C 465 is attached to the dominant D galaxy NGC 7720 in the cluster Abell 2634. New VLA maps of the radio source are presented which reveal an inner jet and a rapid change of structure at the hot spots at the beginning of each tail. New X-ray maps of the cluster gas are also presented. It is shown that the sharp bend of the flowing radio-luminous plasma between the inner jets and the beginning of the tails cannot be explained by any of the conventional models. Neither galactic motion, buoyancy, gravitational bending, nor dynamic pressure can account for the bending of this source. Attention is also given to new possibilities for the dynamics of this type of radio tailed source: the effect of a current in the jets, and the interaction with cooling clouds in the cluster gas.

Eilek, J. A.↗

NASA NTRS1984

The dusty, luminous broad-line radio galaxy 3C 109

In the present optical polarimetry and IR photometry for the broad line radio galaxy 3C 109, the absence of variability, in conjunction with a polarization in H-alpha that is identical to that of the adjacent continuum, suggests that the strong polarization of this galaxy is due to extinction by aligned dust grains. This is the process which gives rise to interstellar polarization within the Galaxy. The energy output of 3C 109, from the optical to 20 microns, exceeds by a factor of 2-4 that of the Seyfert 1 galaxy Markarian 231. These observations, together with recent polarimetry of other broad line radio galaxies, indicate that their broad line regions are more heavily reddened than those of either the Seyfert 1 galaxies or quasars. Evidence for a gradual decrease in dust content with increasing source luminosity is discussed.

Rudy, R. J.↗

NASA NTRS1985

Characterization of X-ray sources detected in a deep Einstein exposure of the field around 3C 295

An extensive set of optical and radio observations is presented that characterize the X-ray sources detected in an extremely deep Einstein Observatory exposure of the 3C 295 region. A total of five X-ray sources was found. This number is consistent with the only previous log N - log S result published at these flux levels. One of the sources was a galactic star. The four extragalactic sources are active galactic nuclei (three Seyferts and one QSO). Two of the sources are Seyfert galaxies in the 3C 295 cluster, one of which was previously unknown. The number of Seyfert galaxies in the cluster that is found from this complete X-ray survey is inconsistent with that expected from the fraction of low-redshift active galactic nuclei in their clusters.

Henry, J. P.↗

NASA NTRS1986

Confining hot spots in 3C 196 - Implications for QSO-companion galaxies

VLBI observations of the extremely compact hot spot in the northern radio lobe of the QSO 3C 196 reveal the angular size of its smallest substructure to be 0.065 arcsec x 0.045 arcsec or about 300 pc at the redshift distance. The morphology of the hot spot and its orientation relative to the more diffuse radio emission suggest that it is formed by an oblique interaction between the nuclear QSO jet and circum-QSO cloud. The inferred density in this cloud, together with its apparent size, imply that the cloud contains a galactic mass, greater than a billion solar masses of gas. The effect of the jet will be to hasten gravitational collapse of the cloud. If many QSOs such as 3C 196 are formed or found in gas-rich environments, the QSO radio phase may commonly stimulate the metamorphosis of circum-QSO gas to QSO-companion galaxies or it may play a significant part in catalyzing star formation in existing companions.

Brown, R. L.↗

NASA NTRS1986

Detection of a 'rotating' gas cloud 100 kiloparsecs in diameter surrounding 3C 275.1, a quasar at the center of a rich cluster of galaxies

The distorted radio quasar 3C 275.1 (z = 0.55) is the first QSO found to lie at the center of a rich cluster of galaxies. The quasar is surrounded by an extremely large elliptical nebulosity whose major axis exceeds 100 kpc. Spectroscopic observations of this nebulosity were obtained, with the spectrograph slit aligned along the nebulosity's major axis. The spectrum of the nebulosity in the visible is dominated by O II and O III forbidden emission lines, which yield a well-defined 'solid-body rotation curve' extending 40 kpc from the quasar nucleus, a rotation curve very different from those of normal spiral galaxies. The 3C 275.1 nebulosity is both the largest yet discovered around a quasar and the first in which organized large-scale motions (rotation?) have been identified. The nebulosity may be residue from multiple tidal interactions with cluster members, or it may be accumulated material from a 'cooling flow' of the type seen in low-redshift clusters which are X-ray sources.

Hintzen, P.↗

NASA NTRS1990

The high energy source 3C 273

The properties of 3C 273 are reviewed and an attempt is made to find an answer to the question why 3C 273 is the only extragalactic source so far, which was detected at energies greater than or equal to 50 MeV.

Vonmontigny, Corinna↗

NASA NTRS1991

Controlled growth of 3C-SiC and 6H-SiC films on low-tilt-angle vicinal (0001) 6H-SiC wafers

It has been found that, with proper pregrowth surface treatment, 6H-SiC single-crystal films can be grown by chemical vapor deposition (CVD) at 1450 C on vicinal (0001) 6H-SiC with tilt angles as small as 0.1 deg. Previously, tilt angles of greater than 1.5 deg were required to achieve 6H on 6H at this growth temperature. In addition, 3C-SiC could be induced to grow within selected regions on the 6H substrate. the 3C regions contained few (or zero) double-positioning boundaries and a low density of stacking faults. A new growth model is proposed to explain the control of SiC polytype in this epitaxial film growth process.

Powell, J. A.↗

NASA NTRS1991

SATCOM antenna siting study on P-3C aircraft, volume 1

The NEC-BSC (Basic Scattering Code) was used to study the performance of a SATCOM antenna on a P-3C aircraft. After plate cylinder fields are added to version 3.1 of the NEC-BSC, it is shown that the NEC-BSC can be used to accurately predict the performance of a SATCOM antenna system on a P-3C aircraft. The study illustrates that the NEC-BSC gives good results when compared with scale model measurements provided by Boeing and Lockheed.

Bensman, D. A.↗

NASA NTRS1992

Mechanical properties of 3C silicon carbide

The residual stress and Young's modulus of 3C silicon carbide (SiC) epitaxial films deposited on silicon substrates were measured by load-deflection measurements using suspended SiC diaphragms fabricated with silicon micromachining techniques. The film's residual stress was tensile and averaged 274 MPa while the in-plane Young's modulus averaged 394 GPa. In addition, the bending moment due to the residual stress variation through the thickness of the film was determined by measuring the deflection of free-standing 3C-SiC cantilever beams. The bending moment was in the range of 2.6 x 10 exp -8 -4.2 x 10 exp-8 N m.

Tong, Lijun↗

NASA NTRS1992

Kinematics of the parsec-scale relativistic jet in 3C 345

The paper presents two 5 GHz most recently obtained VLBI images of the nucleus of the quasar 3C 345 (being observed since 1977), which were obtained in 1989 and 1990 with 4 pc resolution. The images show a variety of morphological features in the jet, which can help to understand the dynamics of the central energy source and the transport of energy along the jet. Also presented are the analysis of the images, temporal variations, and the jet profile. The jet speed and the orientation of 3C 345 were determined from various observational constraints, within the framework of the relativistic twin-jet model.

Unwin, Stephen C.↗

NASA NTRS1993

Observations of the gaseous Galactic halo toward 3C 273 with the Goddard High Resolution Spectrograph

An analysis of observations of 24 absorption lines produced near zero redshift by Milky Way disk and halo gas along the sight line to 3C 273 is presented. The reduced spectra have a resolution of about 20 km/s (FWHM) with broad wings and an SNR of 13 to 20. The species detected include C II, C II*, C IV, O I, Mg II, Si II, Si IV, S II, Mn II, Fe II, and Ni II. The O I absorption is blended with earth atmospheric emission, and one of the Si IV doublet lines is blended with an intergalactic Lyman-alpha line. Column densities are determined for C II*, C IV, Si II, Si IV, N V, S II, Mn II, and Ni II using standard curve-of-growth techniques and the apparent optical depth method. The column density for S II and a measure of N(H I) from FOS observations of Lyman-alpha reveal a 45-percent overabundance of sulfur compared with neutral hydrogen which is probably due to the presence of S II in ionized gas toward 3C 273.

Savage, Blair D.↗

NASA NTRS1993

EGRET observations of 3C 273

The quasar 3C 273 was detected by COS-B in the 1970's. EGRET observations of this sky region in June and October 1991 revealed a flux from 3C 273 lower than that measured by COS-B. The flux observed by EGRET in the June period is approximately 3 x 10 exp -7/sq cm s for energies greater than 100 MeV. During the October observation it appears to be even lower. For the first observation a preliminary spectrum which has a photon index of 2.4 has been derived.

Von Montigny, C.↗

NASA NTRS1993

Identification of the sigma source near 3C 273 - A new class of AGN?

The hard X-ray source detected with SIGMA at an offset of about 15 arcmin from 3C 273 may be identified with an uncataloged Einstein X-ray source detected in the deep Einstein HRI exposure of 3C 273 and in subsequent short IPC exposures. We have identified this source, within the SIGMA error circle, with a faint (mag 19-20) QSO at z = 0.57. Comparison of the SIGMA and Einstein fluxes with this optical object suggest it is highly self-absorbed, and possibly highly variable. The discovery of such a class of AGN would have important consequences for the cosmic X-ray background.

Grindlay, J. E.↗

NASA NTRS1993

CCD mosaic images of the supernova remnant 3C 400.2

We have constructed CCD mosaic images of the old Galactic supernova remnant 3C 400.2 in lines of H-alpha + forbidden N II, forbidden S II, and forbidden O III, plus a continuum band. These are the first CCD images covering the full extent of this remnant, and they reveal significantly more nebulosity than the deepest photographic plates. Comparison with radio and X-ray images indicates dramatically different morphology in the three regimes. The optical images both in H-alpha + forbidden N II and in forbidden S II show an almost complete, irregular shell of emission, with a diameter of about 16 arcmin, little over half that of the radio shell, while the X-ray structure is a centrally peaked ellipsoid. Approximate values for optical line fluxes are obtained; we estimate L(H-alpha) about 3 x 10 exp 35 ergs/s, roughly three times the X-ray luminosity. We also report a previously uncataloged planetary nebula southwest of 3C 400.2.

Winkler, P. F.↗

NASA NTRS1993

Optical and Hubble Space Telescope ultraviolet spectropolarimetry of 3C 273 and PG 1114+445

New optical spectropolarimetry and broad-band measurements, made during periods when the linear polarization of the quasar 3C 273 was no greater than 1 pct, are combined with ultraviolet polarization measurements made with the Faint Object Spectrograph of the Hubble Space Telescope. Very weak UV polarization during the time of observation is seen in the HST measurements, which is consistent with the completely unpolarized UV continuum and emission lines. Optical spectropolarimetry, however, reveals polarized light, the source of which is consistent with a nonthermal component, diluted by other unpolarized emission sources, such as the 'big blue bump'. Optical spectropolarimetry of the radio-quiet quasar PG 1114+445 is also presented. The polarization of this QSO is thought to result from scattering by dust external to the narrow-line region. 3C 273 and PG 1114+445 are useful in illustrating the range of polarizing mechanisms which can operate in low-polarization QSOs.

Smith, Paul S.↗