Lick Observatory, long the primary astronomical facility for the entire University of California system, is where I did my graduate training, and much of my dissertation research. Given its modest altitude of only about 4200 feet, the mountaintop views are unusually spectacular, including San Francisco Bay as far north as Mt. Tamalpais, Monterey Bay, and on a clear day looking across the Central Valley, the Sierra Nevada from near Mt. Whitney to well north of Yosemite (that's Half Dome in the picture below). Of course, I was most taken with the night-time views, especially when San Jose was covered with fog. In the night-time view of the main building with the 36-inch dome, that illumination isn't moonlight - it's named after a newspaper, San Jose Mercury (the picture having been taken in about 1980, just as the switch to low-pressure sodium lighting was beginning). The sunset picture with crescent Moon is pretty spectacular, but the city lights in foreground can be alarming if you're trying to look deep into the Universe.
The overall view includes the main building with the original 36" refractor and 1m Nickel reflector at far right, the 3m dome in the center, and (in the distance) the Crossley dome to its left. The former home of the 60-cm Boller and Chivens reflector (now occupied by the Katzman Automatic Imaging Telescope) is at extreme left, much closer than the others in this view from the east. The Carnegie astrograph is hidden from this vantage point.
There is an overhead view from Google maps. Many of the same features are seen in the following view from the window of an American Airlines Boeing 727 (the relevance being that 727s didn't have the engine exhaust blurring the view behind each wing at low altitude). This is a view looking to the northwest in early morning, including one of the frequent fogs that settle below the summit of Mt. Hamilton. The domes of the original 36" refractor (left, in the main building) and 120" Shane reflector (right) are most prominent, with the Crossley telescope on the ridge to the lower left of the main building and the double astrograph to the immediate left of the Shane telescope.
Mt. Hamilton is a popular tourist destinction, especially for sunset watching. I couldn't resist this slightly impressionistic picture of some viewers and their transportation in front of the Lick main building one evening in the summer of 1980:
Telescopes sure can last. The Crossley was moved to Mount Hamilton from England before 1895, and its "new" mounting dates to 1919. Still, I can't recall any observing in which I took greater pleasure than direct photography at the Crossley. The camera is at the f/5 prime focus with a guiding eyepiece at the top of the tube, fed by a prism. You're right out there at the top of the telescope on a platform in the middle of the open dome slit, with half the sky (and all too frequently, all of San Francisco Bay) spread out before you. Of course, in winter when it gets below freezing even near San Jose, I can't recall any more miserable observing either.
One major program I did at the Crossley was photographic monitoring of variations in the lensed double QSO 0957+561 over the couple of years after its discovery - which led to my first solo paper in the Astrophysical Journal, fittingly enough in the April 1, 1982 issue. I also did lots of galaxy photography, for such purposes as astrometry to register optical and radio structures (which was a bigger deal before the Digitized Sky Survey became available, and each field had to be individually measured and a separate plate solution computed for every time the plate went on and off the measuring machine). The early photographic archive (going back to 1895) allowed an unusual project, comparing pictures of QSOs seen close to nearby galaxies with much older pictures to look for the long-term variations in QSO brightness that some gravitational lensing models would predict. Here are a few blue-light Crossley photographs of galaxies, vintage 1980-1982, plus an art shot of M17 in red light to fill the time as the summer Milky Way interrupted the galaxy list. Exposures for the galaxies were 20-30 minutes on 103a-O plates, while M17 was an hour on 103a-F red-sensitive emulsion.
|Double quasar||NGC 4192||Arp 220||NGC 4800||M17|
For a few special purposes, the original Wampler single-channel spectrum scanner was around, which was one of the few instruments at the time which could measure spectra just longward of one micron. As an example, here are some spectral features of NGC 1068 in this region, including reddening-sensitive [S II] emission lines.
I arrived at UCSC just in time to follow the construction of the Nickel telescope, from being part of a grad course which made some minor changes to the design (if you've been there, the elbows in the northern yoke supports were our contribution), through preliminary mechanical assembly in the shops on campus, to pointing tests, and jumped right in to be the first full-fledged Ph.D. project done on the telescope. This telescope was based on an f/5 primary mirror originally planned as a replacement for the Crossley's mirror, but ended up in its own instrument, completely built in the Lick shops at UCSC and pushed financially upon a bequest by Anna Nickel. In all, I measured something like 700 spectra of about 200 galaxies, plus a library of giant and main-sequence stars for spectral synthesis. The 1-m telescope was installed in the dome formerly occupied by the first permanent telescope at Lick, the original 12-inch Clark refractor, at the north end of the same building best known for the 36-inch refractor. By the time I left UCSC in 1982, I had used about 10% of the dark time ever allocated on this telescope (something I'm unlikely ever to manage again on an instrument that I didn't pay for). I did make a point of patting the mirror cell goodbye that final morning. This plot compares the spectrum of galactic nucleus with a synthetic spectrum composed of nearby stellar a examples, and the difference shows weak emission lines that are nearly lost in the fine structure of the ordinary starlight spectrum.
Update: In late 2010, Elie Gates showed me around some of my old haunts at Lick. The Nickel telecope remains a workhorse with a wider slate of instruments, including a high-speed detector to look for laser communiticion from extraterrestrial civilizations. As a result, it has a lot more accessories and onboard wiring. The sign of a busy telecope, but not nearly as clean as its original lines were. I am pleased that there is now an electrically-operated cover so the obsever doesn't need to throw a 10-meter plastic sheet over it and pull the telecope up while hoping it doesn't slide off.
This telescope, starting from a glass blank used in testing the 200" Palomar primary mirror, kept the University of California competitive in optical and infrared astronomy with their neighbors to the south up until the design of what became the Keck telescopes. As far as I know, this is the smallest instrument in which observers routinely worked in a prime-focus cage. Okay, so the official UC policy at the time was that no grad students could be listed on the 120" schedule as the observers. I did manage a half-night in the prime focus cage during the first checkout of a CCD spectrograph. The [O III] emission lines really are an unearthly green, as I found when finishing the night with a calibration spectrum of NGC 7027 and telling the operator that I wasn't quite ready to move the telescope until Nebula Appreciation class was over. That very dim blob through the acquisition eyepiece really was Cygnus A, as we could tell when the spectrum came in. Ski Antonucci and I did end up with a night of our very own - which was snowed in, as photographically documented here.
Update - December 2010. I visited Lick again for an observing run at the Shane telescope, which now looks like this:
With colleagues from UCSB, we were using the Kast double spectrograph to follow up candidate giant ionized clouds around AGN, found by participants in the Galaxy Zoo project. As an example, this spectrum of SDSS J100507.88+283038.5 is show over the wavelength range 4500-5300 Angstroms. The lower galaxy spectrum shows ionized gas to about 10 kiloparsecs from the core - left to right, the emission is from He II, Hβ, and [O III]. The strength of [O III] and especially He II show that this gas is ionized by the hard continuum of an AGN rather than local star formation.
The Carnegie double astrograph was built for a single dedicated project - a long-term astrometric study of vast numbers of stars, using distant, faint galaxies as an inertial reference frame. This would yield newly accurate information on galactic rotation and stellar populations. The two objective lenses are best corrected for blue and yellow light, so that both wavelengths can be observed simultaneously. The first epoch of the survey began about 1947, with the second epoch of identical exposures completed in the 1980s. The blue lens has an image structure which grows rapidly to brighter magnitudes, which allows quite accurate photometry, while the yellow lens gives very sharp Schmidt-like star images. The survey observations used a wire grating over each objective, giving a short set of diffracted spectral images to the north and south of bright stars. This means that the positions of bright stars could be measured precisely by averaging the diffracted images, instead of finding the center of a huge overexposed blob. Since the survey exposures were long - two hours - tracking was important, so the astrometrists at Lick would re-adjust the polar axis to point at the appropriate refracted pole for each declination band being observed. Furthermore, they also had to adjust its pointing after each major earthquake in the area, to compensate for the slight rotation of Mt. Hamilton as the two sides of the San Andreas fault complex slide past each other.
As part of the graduate course on observing techniques, we each did practice plates with the astrograph. These included pictures of M31 (1 hour on 103a-O emulsion, blue astrograph - stick with the classics, we thought), and later a field around the double QSO 0957+561 including the edge-on spiral NGC 3079 (1 hour on 103a-G with the yellow lens through cirrus), showing the multiple images produced by the objective gratings. The double quasar is near the upper right corner of this excerpt, with NGC 3079 and its companion Markarian 131 near the bottom. These were scanned from contact prints made from the original 8x10" plates. Normal survey data were taken on still larger-format plates, 20 inches square and 1/4 inch thick. Only three astrometrists were allowed to handle these.
Update: the astrograph is now officialy retired, having served honorably for its original purpose plus the Shane-Wirtanen galaxy counts, some of the first evidence for truly large-scale cosmic structure. Its location is now largely overshadowed by the Automated Plan`et Finder dome nearby.
The former location of a Boller & Chivens 0.6 telescope has now been taken over by this compact robotic telescope, masterminded by Alex Filippenko and colleagues at Berkeley. Its program is dedicated to the search for nearby supernovae, by repeated imaging of thousands of galaxies. With only a single small instrument package, and no need for manual access to an eyepiece or anything, such a telescope can be made remarkably compact. The KAIT sits on a base which is basically a reinforced metal table. At this size, as much as I disbelieve I'm typing the word, the telescope can only be described as "cute".
Last changes: 9/2014 © 1999-2014