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  • Other Sources  (10)
  • 2010-2014  (2)
  • 1985-1989  (5)
  • 1965-1969  (3)
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  • 1
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    Colors of reflection nebulae. III - Ultraviolet scattering by small particles in reflection nebulae associated with 17, 20, and 23 Tauri (1986)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: New surface brightness measurements in the reflection nebulae associated with the Pleiades stars 17, 20, and 23 Tau have been carried out with the IUE satellite. Each nebula was observed at two angular offsets south of the respective illuminating star. At the larger offsets (40, 40, and 60 arcsec respectively) each nebula exhibits a flux distribution which rises much more steeply with decreasing wavelengths than the corresponding stellar spectrum. At the smaller offsets (20 arcsec) the nebular spectra are more similar to those of the stars and fail to show the steep rise at wavelengths less than 2200 A. Independent observations of interstellar absorption lines as well as theoretical arguments by several previous authors lead to a model wherein the reflection nebulosity near the Pleiades stars is caused by a thin sheet of interstellar matter in front of the stars, at an approximate distance of a few x 10 to the -2nd pc. In the context of such a model the nebular spectra obtained near 17, 20, and 23 Tau can be understood only if the phase-function asymmetry of scattering declines with decreasing wavelengths throughout the spectral range. This result indicates that the role of scattering in the UV by particles in the 10 to the -6th cm size range appears more important than is generally recognized by current models.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 302; 421-431
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  • 2
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    Images in the rocket ultraviolet - The stellar population in the central bulge of M31 (1985)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: Imagery of the bulge of M31 obtained with a rocket-borne telescope in two broad bands centered at 1460 A and 2380 A is discussed. The UV spatial profiles over a region about 200 arcsec wide are identical with those at visible wavelengths. The absence of detectable point sources indicates that main-sequence stars hotter than B0 V are not present in the bulge. It is suggested that the far-UV flux in old stellar populations originates in post-AGB stars. The UV flux from such stars is extremely sensitive to age and the physics of their previous mass loss.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X); 298; L37-L40
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  • 3
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    Images in the rocket ultraviolet - The initial helium abundance and distance modulus of the globular cluster M5 from photometry of horizontal-branch stars (1985)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: A natural laboratory for the study of postmain-sequence evolution of low-mass (less than one solar mass) metal-poor stars is provided by globular clusters. These clusters are, therefore, a critical aid for developing an understanding of advanced stages of stellar evolution and of the chemical evolution of the Galaxy. Bohlin et al. (1983) have described a study of the postasymptotic branch star near the center of M5. The present investigation is concerned with the fainter horizontal-branch stars. The observations were made with the aid of a rocket-borne 38 cm f/9.0 Ritchey-Chretien telescope. Attention is given to payload and flight data, preflight bandpass calibration, the reduction of flight data, star selection, position measurement, photometry, the minimum observed horizontal-branch mass and inferences on mass loss, and individual UV-bright stars.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 292; 687-695
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  • 4
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    The Responses of the University of Iowa Charged Particle Detectors on Explorer 12 Graphic Summary (1966)
    In:  CASI
    Details
    Publication Date: 2019-05-29
    Description: Graphs of charged particle detectors responses on Explorer XII satellite
    Keywords: SPACE VEHICLES
    Type: NASA-CR-75227
    Format: application/pdf
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  • 5
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    Rocket observations of Orion stars with an all-reflective ultraviolet spectrograph. (1968)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Far UV spectra of O and B stars in Orion photographed from Aerobee rocket, describing wavelength measurements and line identifications
    Keywords: SPACE SCIENCES
    Type: ; ADEMIE DES SCIENCES
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  • 6
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    Graphic summary of the responses of the University of Iowa charged particle detectors on Explorer 14 (1966)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Graphs of Explorer XIV charged particle detectors responses
    Keywords: INSTRUMENTATION AND PHOTOGRAPHY
    Type: NASA-CR-81141 , REPT.-66-40
    Format: text
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  • 7
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    Detection of scattering in the 2175 A interstellar band (1986)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: Spectrophotometric observations of two reflection nebulae and their illuminating stars obtained with the International Ultraviolet Explorer Satellite have provided the first evidence for the presence of a scattering contribution to the 2175 A interstellar extinction band. Lower than normal far-UV extinction for the stars embedded in the nebulae indicates that the nebulae have a dust particle size distribution that is dominated by larger particles. The strength of the 2175 A band is larger than normal in both cases. The scattering is found to dominate the long-wavelength wing of the band, without shifting the central wavelength of the band by more than 20 A toward longer wavelengths. These observations are taken to indicate that the solid particles responsible for the 2175 A band can be considerably larger than the Rayleigh limit in some interstellar locations. The absence of a notable shift in the central wavelength of the band in such large particles presents a new severe constraint for models of interstellar grains.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X); 305; L23-L27
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  • 8
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    The unusual dust-scattering properties in the reflection nebula CED 201 (1987)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: Spectrophotometric data available from ground-based and IUE observations of the reflection nebula CED 201 and its illuminating star BD + 69.1231 deg are analyzed to deduce the most likely star-nebula geometry and the wavelength dependence of the scattering characteristics of the nebular grains. The dust albedo is found to decline from 0.72 at V to probably less than 0.2 at lambda less than 2000 A, explaining the unusual red color of this reflection nebula. The wavelength dependence of the optical depth and of the phase function asymmetry in the visible suggests the existence of a narrow size distribution of grains, skewed toward larger than normal particle sizes. CED 201 is one of two reflection nebulae with positive evidence for enhanced scattering in the long-wavelength wing of the 2175 A dust extinction feature, also pointing toward larger than average grains.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 321; 912-920
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  • 9
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    Performance of the Space Telescope Imaging Spectrograph after SM4 (2010)
    In:  CASI
    Details
    Publication Date: 2019-08-14
    Description: On May 17, 2009, during the fourth EVA of SM4, astronauts Michael Good and Mike Massimino replaced the failed LVPS-2 circuit board on the Space Telescope Imaging Spectrograph (STIS), restoring this HST instrument to operation after a nearly 6 year hiatus. STIS after this 2009 repair operates in much the same way as it did during the 2001-2004 period of operations with the Side-2 electronics. Internal and external alignments of the instrument are similar to what they had been in 2004, and most changes in performance are modest. The STIS CCD detector continued to experience radiation damage during the hiatus in operations, leading to decreased charge transfer efficiency (CTE) and an increased number of hot pixels. The sensitivities for most modes are surprisingly close to what was expected from simple extrapolation of the 2003-2004 trends, although the echelle modes show somewhat more complex behavior. The biggest surprise was that the dark count rate for the NUV MAMA detector after SM4 has been much larger than had been expected; it is currently about 2.5 times bigger than it was in 2004 and is only slowly decreasing. We discuss how these changes will affect science with STIS now and in the future.
    Keywords: Optics
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  • 10
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    Status of the STIS Instrument After Repair During Sm4 (2010)
    In:  Other Sources
    Details
    Publication Date: 2019-07-19
    Description: The Space Telescope Imaging Spectrograph (STIS) was installed in the Hubble Space Telescope (HST) in February of 1997, and operated until August of 2004, when an electrical malfunction in a power supply forced cessation of operations. On May 17,2009, during the fourth EVA of SM4, astronauts Michael Good and Mike Massimino undertook an eight-hour spacewalk, during which they replaced the STIS LVPS-2 circuit board containing the failed component, successfully repairing STIS. We will review the scientific capabilities and operational status of STIS after this repair. In most respects, STIS after the 2009 repair operates in much the same way as it did prior to the 2004 failure. Most changes in performance are close to what had been expected. The degradation of the STIS CCD due to radiation damage and the modest changes in optical throughput are consistent with extrapolation of previously-observed trends. Internal and external alignments of the instrument are also similar to what they were in 2004. The biggest surprise is that the dark current for the NUV MAMA detector is several times larger than had been expected and is only slowly decreasing towards its expected range. We discuss how these changes will affect science with STIS now and in the future.
    Keywords: Astronomy
    Type: 215th American Astronomical Society Conference; Jan 03, 2010 - Jan 07, 2010; Washington, DC; United States
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