P200 Observer Information
Nightly operations of the Palomar 200-inch Hale Telescope (P200) are conducted from a data/control room, and facilitated by telescope operators and support astronomer personnel. Typically observations are conducted in the same data room; in limited circumstances remote observations are supported—see Palomar Remote Observing. Allocation of P200 observing time is handled through independent time allocation process within eligible constituencies, and the allocations are merged into an integrated observing schedule
P200 supports limited remote observing capabilities for DBSP, TSpec, LFC, and WIRC. Interested/eligible parties can find more information on Palomar Remote Observing at our COO Remote Observing page.
The Lead Observer (LO) identified for each P200 night is the single contact point for all scheduling and logistical matters associated with the observing run. If no distinct LO is designated, the program Principal Investigator serves as LO. Please see the on-line P200 Observing Schedule if you have questions about the LO-designation for an upcoming run.
LOs are responsible for identifying instrument settings at least two weeks before an observing run. Instrument settings (aka Palomar "green sheets") for instruments such as DBSP are defined through the on-line reservation form (available through the observer login portal, or through help request to the P200 Support Astronomer group).
The Hale Telescope instruments provide a wide range of imaging and spectroscopic capabilities in the optical and near-infrared. PALM-3000 is the new adaptive optics system. It works in conjunction with other instruments including the Palomar High Angular Resolution Observer (PHARO), the Oxford SWIFT integral field spectrograph, and the specialized coronograph Project 1640.
The Hale's seeing-limited imaging instruments include two wide-field cameras: the Large Format Camera (LFC) in the optical and the Wide-field Infrared Camera (WIRC) in the infrared, both mounted at the prime focus of the telescope and covering 24 and 8.9 arcminutes across, respectively. Additionally the new WaSP large-format CCD imager at prime focus will eventually replace LFC as the default prime focus optical imager. The Cosmic Web Imager (CWI) is an imaging spectrograph (integral-field unit) that images over a range of wavelengths simultaneously. Our traditional single-object spectrographs are the optical Double Spectrograph (DBSP) and the infrared Triple Spectrograph (TripleSpec), both mounting at the Cassegrain focus.
Instruments in development include the high-speed CHIMERA camera, and the AO-fed Stellar Double Coronagraph (SDC).
The following is a summary of P200 instrument information/resources:
Public instruments are those set up and maintained by the Palomar Observatory staff, and are available for all constituencies to use.
Private instruments are those built, set up, and maintained by individuals or groups for their own research. Other observers wishing to use these instruments must to arrange, in advance, a collaboration with the builder.
Semiprivate instruments are similar to the private instruments except that the builders have agreed to make them available to others without the need for a formal collaboration, although consultation may be advisable. Scheduling restrictions may apply, however.
Documentation on the Shepherd Autoguider.
A summary of technical specifications for the P200 CCDs is available here.
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