Preliminary analysis of an ultraviolet Hubble Space Telescope faint object camera image of the center of M31

1992 ◽  
Vol 397 ◽  
pp. L35 ◽  
Author(s):  
I. R. King ◽  
J. M. Deharveng ◽  
R. Albrecht ◽  
C. Barbieri ◽  
J. C. Blades ◽  
...  
Keyword(s):  
Preliminary Analysis ◽  
Hubble Space Telescope ◽  
Space Telescope ◽  
Camera Image ◽  
Faint Object

scholarly journals Preliminary analysis of a Hubble FOS spectrum of VW Hyi in quiescence: A DAZQ white dwarf and accretion belt/ring

1996 ◽  
Vol 158 ◽  
pp. 249-250
Author(s):  
E. M. Sion ◽  
M. Huang ◽  
F. H. Cheng ◽  
I. Hubeny ◽  
P. Szkody
Keyword(s):  
White Dwarf ◽  
Preliminary Analysis ◽  
Hubble Space Telescope ◽  
Uv Spectrum ◽  
Space Telescope ◽  
Dwarf Nova ◽  
Faint Object ◽  
Faint Object Spectrograph

AbstractWe present a preliminary analysis of the UV spectrum of the dwarf nova VW Hyi during early quiescence, obtained with the Faint Object Spectrograph (FOS) on the Hubble Space Telescope (HST). The data were obtained approximately one day after the end of a normal outburst.

scholarly journals Hubble Space Telescope Images of Four Magellanic Cloud Planetary Nebulae

1993 ◽  
Vol 155 ◽  
pp. 213-213
Author(s):  
M. J. Barlow ◽  
J. C. Blades ◽  
S. Osmer ◽  
Keyword(s):  
Hubble Space Telescope ◽  
Planetary Nebulae ◽  
Circular Ring ◽  
Uniform Structure ◽  
Full Description ◽  
Type I ◽  
Space Telescope ◽  
Ring Shape ◽  
Faint Object ◽  
Northern Edge

Using the Faint Object Camera on-board the Hubble Space Telescope, we have obtained images of four planetary nebulae in the Magellanic Clouds, namely N2 and N5 in the SMC and N66 and N201 in the LMC. Each nebula was imaged through narrow-band filters isolating [O III] λ5007 and Hβ, for a nominal exposure time of 1000 seconds in each filter. The f/96 optical chain of the FOC was used, yielding 512×512 0.022 arcsec square pixels. Considerable detail is evident on the raw images and after deconvolution using the Richardson-Lucy algorithm, structures as small as 0.06 arcsec are easily discernible. Figure 1 shows NS and EW intensity cross-cuts through the deconvolved [O III] λ5007 images of SMC N2 and SMC N5. SMC N2 is a slightly ellleptical ringlike nebula, with its greatest elongation in the EW direction. The peak-to-peak dimensions of the ring are 0.21×0.26 arcsec2. SMC N5 has a circular ring shape, with the [O III] λ5007 image showing a clearly defined, nearly uniform structure, apart from a bright patch at the northern edge. The peak-to-peak diameter of the ring is 0.26 arcsec and the ring itself is significantly narrower than that of SMC N2, with a width as small as 0.06 arcsec (FWHM) in some places. LMC N201 is very compact, with a FWHM of 0.21 arcsec in the Hβ image. The Type I PN LMC N66 is a multi-polar nebula, with the brightest part having an extent of about 2 arcsec. Its structure is extremely complex, with several bright knots and faint loops visible outside the two bright lobes. A full description of our results can be found in Blades et al., ApJ,398, L41–44.

In-flight performance of the faint object camera of the Hubble Space Telescope

1991 ◽  
Author(s):  
Perry E. Greenfield ◽  
Francesco Paresce ◽  
David A. Baxter ◽  
Philip Hodge ◽  
Richard N. Hook ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Flight Performance ◽  
Space Telescope ◽  
Faint Object

scholarly journals High Speed UV Photometry of the AM Her Systems AM Her, VV Pup And V834 Cen, with the Hubble Space Telescope

1996 ◽  
Vol 158 ◽  
pp. 223-224
Author(s):  
K. Schaefer ◽  
H. Bond ◽  
G. Chanmugam
Keyword(s):  
Preliminary Analysis ◽  
High Speed ◽  
Hubble Space Telescope ◽  
Cataclysmic Variables ◽  
Low Frequency ◽  
Gabor Transform ◽  
Periodic Oscillations ◽  
Space Telescope ◽  
Uv Photometry ◽  
Magnetic Cataclysmic Variables

We have used the High Speed Photometer (HSP) aboard the Hubble Space Telescope to observe the magnetic cataclysmic variables VV Pup, AM Her, and V834 Cen in the UV (1400…3300 Å) with 0.01 s time resolution. We detected low frequency flickering in all three systems, and compare the time-scales with the predictions of King (1989). At higher frequencies we searched for shock oscillations from the accretion column(s) in these systems. The data were analyzed using the Gabor transform wavelet-like technique (Heil & Walnut 1989) to search for frequency evolution throughout each observation. Preliminary analysis suggests the detection of rapid UV quasi-periodic oscillations (QPOs) in VV Pup at 0.74 Hz, and at 4.4 Hz in V834 Cen. As in ground based observations, our observations failed to yield any rapid QPOs in AM Her itself.

Hubble Space Telescope Faint Object Camera calculated point-spread functions

1997 ◽  
Vol 36 (8) ◽  
pp. 1752 ◽  
Author(s):  
R. G. Lyon ◽  
J. E. Dorband ◽  
J. M. Hollis
Keyword(s):  
Hubble Space Telescope ◽  
Point Spread Functions ◽  
Space Telescope ◽  
Point Spread ◽  
Faint Object

Faint object camera: European contribution to the Hubble Space Telescope

1992 ◽  
Vol 26 (11) ◽  
pp. 827-834 ◽  
Author(s):  
H.W. Kröger ◽  
G.K. Schmidt ◽  
N. Pailer
Keyword(s):  
Hubble Space Telescope ◽  
Space Telescope ◽  
Faint Object
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