view Abstract Citations (8) References (4) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS First Results from the Faint Object Camera: High-Resolution Imaging of the Pluto-Charon System Albrecht, R. ; Barbieri, C. ; Blades, J. C. ; Boksenberg, A. ; Crane, P. ; Deharveng, J. M. ; Disney, M. J. ; Jakobsen, P. ; Kamperman, T. M. ; King, I. R. ; Macchetto, F. ; Mackay, C. D. ; Paresce, F. ; Weigelt, G. ; Baxter, D. ; Greenfield, P. ; Jedrzejewski, R. ; Nota, A. ; Sparks, W. B. Abstract The first observations of a solar system target with the Faint Object Camera of the HST are reported. Observations of the Pluto-Charon system were obtained in f/96 and f/288 mode. Pluto and Charon were clearly resolved, and the observed separation and diameters are in accordance with expectations. The f/96 data were astrometrically and photometrically analyzed; preliminary results are presented. Publication: The Astrophysical Journal Pub Date: June 1991 DOI: 10.1086/186073 Bibcode: 1991ApJ...374L..65A Keywords: Astrometry; Astronomical Photometry; Charon; Pluto (Planet); Diameters; Faint Object Camera; Astronomy; PLANETS: PLUTO full text sources ADS | data products MAST (1) ESA (1)
view Abstract Citations (49) References (48) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS PG 0832+676: an Apparently Normal B1 V Star 18 Kiloparsecs above the Galactic Plane Brown, Paul J. F. ; Dufton, Philip L. ; Keenan, Francis P. ; Boksenberg, Alec ; King, David L. ; Pettini, Max Abstract Stellar equivalent widths and line profiles, measured from optical spectra obtained with the 5 m Hale telescope and the 2.5 m Isaac Newton telescope, are used in conjunction with model atmosphere calculations to determine the atmospheric parameters and chemical composition of the faint, blue, high-galactic latitude star PG 0832 + 676. The effective temperature (Teff = 25,000 K), surface gravity (log g = 3.9), and abundances of He, C, N, O, Mg, Al, and Si are similar to those of Population I OB-type stars, from which it is concluded that PG 0832 + 676 is a normal star at a distance from the galactic plane of about 18 kpc. The star's kinematics and evolutionary age suggest that it formed in the halo, possibly from galactic fountain material. Publication: The Astrophysical Journal Pub Date: April 1989 DOI: 10.1086/167305 Bibcode: 1989ApJ...339..397B Keywords: B Stars; Blue Stars; Stellar Atmospheres; Stellar Spectra; Abundance; Chemical Composition; Spectral Line Width; Stellar Evolution; Astrophysics; ABUNDANCES; STARS: EARLY-TYPE; STARS: INDIVIDUAL ALPHANUMERIC: PG 0832; 676 full text sources ADS | data products SIMBAD (2)
view Abstract Citations (37) References (17) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Spectroscopy of the QSO pair Q0028+003 / Q0029+003. Shaver, P. A. ; Boksenberg, A. ; Robertson, J. G. Abstract It is hypothesized that a prominent, narrow absorption line system discovered in the spectrum of Q0029+003, at a redshift of 1.7334, and only 190 km/sec from the emission line redshift of Q0028+003, may be due to a galaxy located in a cluster containing the latter QSO. Alternatively, the absorption line system may arise in a halo associated with Q0028+003 and extending at least 520 kpc, which is the projected separation of the two QSOs at this redshift. Publication: The Astrophysical Journal Pub Date: October 1982 DOI: 10.1086/183879 Bibcode: 1982ApJ...261L...7S Keywords: Absorption Spectra; Astronomical Spectroscopy; Galactic Clusters; Line Spectra; Quasars; Red Shift; Calcium; Galactic Nuclei; Magnesium; Spectral Energy Distribution; Spectral Line Width; Astronomy full text sources ADS | data products NED (7) SIMBAD (1) MAST (1)
Observations with a spectral resolution of 0.01 nm have been made for several stars in the balloon ultraviolet. For the two coolest stars studied ((3 Ori and a Lyr) wavelengths of all observed spectral features in the range 273-288 nm are given with an accuracy of approximately ± 0.004 nm. Using these results the velocity field in the atmosphere of (3 Ori has been investigated and evidence is found for an outward motion in the higher layers and a pulsation-type motion in the deepest layers. The strength of the Mg+ resonance and subordinate lines near 280 nm for all the stars observed is compared with non-l.t.e. calculations. Good agreement between observation and theory is found for main sequence stars but the stronger lines in the supergiants imply microturbulent velocities >10 km s_1.
An optical counterpart of the radio/X-ray supernova remnant in 30 Dor B in the LMC has been detected by direct imaging and spectroscopic techniques. Interesting properties at X-ray, optical and radio wavelengths are considered. Because it has a non-thermal X-ray spectrum and a flat radio spectrum, it may be a Crab-like SNR, but more evolved.
view Abstract Citations (22) References (18) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS First Results from the Faint Object Camera: Imaging the Core of R Aquarii Paresce, F. ; Albrecht, R. ; Barbieri, C. ; Blades, J. C. ; Boksenberg, A. ; Crane, P. ; Deharveng, J. M. ; Disney, M. J. ; Jakobsen, P. ; Kamperman, T. M. ; King, I. R. ; Macchetto, F. ; Mackay, C. D. ; Weigelt, G. ; Baxter, D. ; Greenfield, P. ; Jedrzejewski, R. ; Nota, A. ; Sparks, W. B. Abstract The Faint Object Camera on the HST was pointed toward the symbiotic long-period M7e Mira variable R Aquarii, and very high resolution images of the inner core, mainly in the ionized oxygen emission lines in the optical, are reported. Both images show bright arcs, knots, and filaments superposed on a fainter, diffuse nebulosity extending in a general SW-NE direction from the variable to the edge of the field at 10 arcsec distance. The core is resolved in forbidden O III 5007 A and forbidden O II 3727 A into at least two bright knots of emission whose positions and structures are aligned with PA = 50 deg. The central knots appear to be the source of a continuous, well-collimated, stream of material extending out to 3-4 arcsec in the northern sector corresponding to a linear distance of about 1000 AU. The northern stream seems to bend around an opaque obstacle and form a spiral before breaking up into wisps and knots. The southern stream is composed of smaller, discrete parcels of emitting gas curving to the SE. Publication: The Astrophysical Journal Pub Date: March 1991 DOI: 10.1086/185960 Bibcode: 1991ApJ...369L..67P Keywords: Faint Object Camera; Mira Variables; Nebulae; Stellar Spectra; Symbiotic Stars; Emission Spectra; Forbidden Transitions; Oxygen Spectra; Astrophysics; NEBULAE: INDIVIDUAL NAME: R AQUARII; STARS: INDIVIDUAL CONSTELLATION NAME: R AQUARII; STARS: SYMBIOTIC full text sources ADS | data products SIMBAD (1) MAST (1) ESA (1)
Intermediate-resolution spectra of the QSOS MCS402, Q0347–383, Q0420–388, and Q2204–408 have been combined to yield average spectra of Lyα absorption systems with improved signal-to-noise ratios. Searches for absorption lines of a number of heavy elements were carried out with no positive detections. Limits on the heavy element ions' column densities have been determined which are in broad agreement with previous studies. The further usefulness of intermediate-resolution (∼ 1 Å) spectra for setting heavy clement abundance limits in Lyα systems is considered.
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