The Ultraviolet Imaging Telescope - Design and performance

Stecher, T. P.; Baker, Gerald R.; Bartoe, Donna D.; Bauer, Frank; Blum, A.; Bohlin, R. C.; Butcher, H. R.; Chen, Peter C.; Collins, Nicholas R.; Cornett, R. H.; Deily, John J.; Greason, M. R.; Hennessy, G. S.; Hill, J. K.; Hill, Robert S.; Hintzen, P.; Isensee, J. E.; Kenny, Peter; Landsman, W. B.; Linard, D.; Maran, S. P.; Neff, Susan G.; Nichols, Granville R.; Novello, Joseph; O’Connell, R. W.; Offenberg, J. D.; Parise, R. A.; Pfarr, B.; Plummer, Thomas B.; Richardson, F. F.; Roberts, M. S.; Sitko, Susan D.; Smith, Andrew M.; Stober, A. K.; Stolarik, J. D.; Tebay, Jack C.

doi:10.1086/186474

Cited by 45 publications

(30 citation statements)

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“…Uncertainty in the absolute calibration can lead to uncertainties of up to 10 − 15 % in the FUV flux. A detailed discussion of the reduction of the UIT data to flux-calibrated arrays is given by Stecher et al (1992Stecher et al ( , 1997.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Star Formation Triggering Mechanisms in Dwarf Galaxies: The Far‐Ultraviolet, Hα, and HiMorphology of Holmberg II

Stewart

Fanelli

Byrd

et al. 2000

ApJ

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Section: Observations and Data Reductionmentioning

confidence: 99%

Star Formation Triggering Mechanisms in Dwarf Galaxies: The Far‐Ultraviolet, Hα, and HiMorphology of Holmberg II

Stewart

Fanelli

Byrd

et al. 2000

ApJ

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“…This paper uses the final version of the UIT Astro-2 data reduction pipeline, which is called by the name FLIGHT22. Detailed descriptions of the UIT instrument and data reduction are given elsewhere (Stecher et al 1997;Stecher et al 1992). The Astro-2 UIT calibration is based on 75 measurements of 49 stars that have been observed by IUE.…”

Section: Overviewmentioning

confidence: 99%

Ultraviolet Imaging of the Irregular Galaxy NGC 4449 with the Ultraviolet Imaging Telescope: Photometry and Recent Star Formation History

Hill

Fanelli

Smith

et al. 1998

ApJ

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The bright Magellanic irregular galaxy NGC 4449 was observed during the Astro-2 Space Shuttle mission by the Ultraviolet Imaging Telescope (UIT), which obtained images of a 40 ′ field centered on the galaxy in two broad far-ultraviolet (FUV) bands centered at 1520Å and 1620Å, with 3 ′′ − 5 ′′ spatial resolution. Together with Hα and Hβ fluxes from ground-based Fabry-Perot images, these data are analyzed in order to explore the recent star formation history of NGC 4449. Maps of the flux ratios Hα/FUV and FUV/blue continuum are presented and interpreted using evolutionary synthesis models. Photometry is presented both for 22 apertures containing large OB complexes and for 57 small apertures containing compact FUV-emitting knots. The OB complexes along the northern edge of the visible system have high Hα/FUV ratios, and thus appear to be more dominated by the current generation of stars than are other parts of the galaxy. However, young sources do exist elsewhere and are particularly conspicuous along the bar. The small aperture analysis shows three candidate regions for sequential star formation. Surface brightness profiles are consistent with an exponential disk in both the FUV and the optical continuum.

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“…There have been several efforts to obtain images of representative nearby galaxies. The FOCA balloon experiment at 2000Å has measured six UV images of local galaxies (Blecha et al 1990), the astro-1 (astro-2) mission measured 27 (45) UV images of objects using the Ultraviolet Imaging Telescope (Stecher et al 1992), and Maoz et al (1997) have recently compiled UV images of 110 galaxies using the FOC on HST (2300Å). Cognizant of the importance of these UV images for assessing galaxy evolution, researchers (Bohlin et al 1991;Giavalisco et al 1996a;Maoz 1997) have already used these data to comment on deep HST images.…”

Section: Introductionmentioning

confidence: 99%

Cloning Hubble Deep Fields. I. A Model‐independent Measurement of Galaxy Evolution

Bouwens¹,

Broadhurst²,

Silk³

1998

ApJ

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We present a model-independent method of quantifying galaxy evolution in high-resolution images, a method which we apply to the Hubble Deep Field (HDF). Our procedure is to k-correct all pixels belonging to the images of a complete set of bright galaxies and then to replicate each galaxy image to higher redshift by the product of its space density, and the cosmological volume. The set of 1/V max , bright galaxies is itself selected from the HDF, because presently the HDF provides the highest quality UV images of a redshift-complete sample of galaxies (31 galaxies with I \ 21.9, for which z6 \ 0.5, V /V max is spread fairly). These galaxies are bright enough to permit accurate pixel-by-pixel k-corrections into the rest frame UV (D2000 We match the shot noise, spatial sampling, and point-spread function smooth-Ó). ing of the HDF data, resulting in entirely empirical and parameter-free "" no-evolution ÏÏ deep Ðelds of galaxies for direct comparison with the HDF. In addition, the overcounting rate and the level of incompleteness can be accurately quantiÐed by this procedure. We obtain the following results. Faint HDF galaxies (I [ 24) are much smaller, more numerous, and less regular than our no-evolution extrapolation, for any interesting geometry. A higher proportion of HDF galaxies "" dropout ÏÏ in both U and B, indicating that some galaxies are brighter at higher redshifts than our "" cloned ÏÏ z D 0.5 population.

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The Ultraviolet Imaging Telescope - Design and performance

Cited by 45 publications

References 0 publications

Star Formation Triggering Mechanisms in Dwarf Galaxies: The Far‐Ultraviolet, Hα, and HiMorphology of Holmberg II

Star Formation Triggering Mechanisms in Dwarf Galaxies: The Far‐Ultraviolet, Hα, and HiMorphology of Holmberg II

Ultraviolet Imaging of the Irregular Galaxy NGC 4449 with the Ultraviolet Imaging Telescope: Photometry and Recent Star Formation History

Cloning Hubble Deep Fields. I. A Model‐independent Measurement of Galaxy Evolution

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