Abstract
At the beginning of the nineteenth century one of the scientific issues driving the research of astronomers, like the Herschels, was to test if all the nebulæ can be resolved into stars.
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Notes
- 1.
The 140 ft telescope was initially planned to be the first major instrument of NRAO. Because it was feared that computers would not be able to effectively point a large alt-az telescope, the 140 ft was designed to have a (very expensive) equatorial mounting. In late 1960, it was realized that parts of the mount design were vulnerable to brittle fracture. The redesign would impose a delay of years; hence it was decided that a large, but cheap 300 ft transit telescope with a surface of high enough quality for operation at a wavelength of 21 cm should be built, and built fast. Less than 2 years later, the 300 ft telescope designed by John Findlay was completed and NRAO’s image, affected by the 140 ft delay, was restored. According to Findlay, a brilliant scientist/engineer with a sharp sense of humour, the 300 ft was built “for the price of sugar: 68 cents per pound” (Burke 2005). The 140 ft was eventually inaugurated in 1965. On the night of November 15, 1988, the 300 ft telescope collapsed, after one quarter of a century of fine service. On that day, in the course of the annual meeting of the Arecibo Observatory Board of Trustees, I was addressing the Board and representatives of the National Science Foundation on the need to allocate funds for an engineering inspection of the telescope’s focal platform structural health. On the following day, after hearing news of the 300 ft collapse, the decision to inspect and the funds to do it were unanimously approved.
- 2.
I will refer as Ultraviolet (UV) to the wavelength range shortwards of ∼ 3300 Å, which is often divided in far-UV (FUV) and near-UV (NUV) at ∼ 2000 Å. The range shortwards of Ly α is usually termed Extreme-UV (EUV).
- 3.
There were other UV instruments: the USSR ASTRON station, GLAZAR on MIR, S201 on Apollo 16, FAUST on Spacelab, the GSFC camera, SCAP 2000, FOCA, FUVCAM, NUVIEWS,…Rocket and balloon experiments continue today, as an economical and fast way to test new technology.
- 4.
The first discovery of broad absorptions in UV resonance lines of massive stars, with velocities of a few thousand km s−1, from Aerobee rocket data of B stars in Orion, was reported by Morton and Spitzer (1966) who correctly interpreted them as evidence of mass loss.
- 5.
H α and HeII 4686 are also wind diagnostics but only in high luminosity stars with high \(\dot{M}\); instead, resonance lines in UV and EUV trace winds also at low L bol, low \(\dot{M}\), high T eff [even in the hottest evolved stars, when all other diagnostics fade Bianchi (2012)]. UV lines also allow us to measure wind velocity, and momentum injected by the stellar wind into the interstellar medium.
- 6.
The instruments mentioned so far had resolution of tens of arcminutes or worse, flux limit ∼ 11–12 mag, except for balloons which can lift larger telescopes, but cannot access FUV due to the limited heights they can reach.
- 7.
With UIT, two other UV instruments were flown: the Hopkins Ultraviolet Telescope (HUT) performing spectrophotometry in the 425–1850 Å range, and the Wisconsin Ultraviolet Photopolarimetry Experiment (WUPPE spectrapolarimeter, covering the range from 1250 to 3200 Å).
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Rampazzo, R. et al. (2016). Extragalactic Astronomy: From Pioneers to Big Science. In: D'Onofrio, M., Rampazzo, R., Zaggia, S. (eds) From the Realm of the Nebulae to Populations of Galaxies. Astrophysics and Space Science Library, vol 435. Springer, Cham. https://doi.org/10.1007/978-3-319-31006-0_1
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