(Please distribute this call to any colleagues who might be interested)
We extend an invitation for proposals for the use of the Arecibo Observatory HF facility with a deadline of August 12, 2016 (17:00 AST, 21:00 UTC). These petitions should be for usage of the HF facility and Incoherent Scatter Radar, as well for the passive and active optical instruments. Once the request is submitted and accepted, it is valid for scheduling until August 11, 2017, after which it will need to be re-submitted to maintain validity. This call will cover at least two campaigns of 5-to-6 days around new moon periods, the number might vary depending on the number of proposals awarded.
Information about observing proposals and policies can be found at http://www.naic.edu/~astro/proposals/proposal.shtml. Proposals must be submitted using the web-based cover form, which can be found online at http://www.naic.edu/~astro/proposals/hfprop.php. For this deadline we have enabled direct uploading of the PDF containing the main body of your proposal via the proposal website. If you do not upload your PDF, you should send it by separate email to email@example.com.
Technical information about our facilities and instrumentation as well as the contacts for specific support are found below. For any further information not addressed in this communication you can contact Christiano Brum (firstname.lastname@example.org).
We hope to obtain your proposals real soon and continue to do outstanding research during the upcoming year as we have done in the past.
The HF facility at Arecibo consists of six 100 KW HF transmitters that feed the 300 m dish using a Cassegrain feed. This feed consists of crossed dipoles located near the center of the surface of the dish that transmit upward to a light wire grid sub reflector that is supported from the three main towers. This element illuminates the dish, which transmits a narrow beam vertically. There are three crossed dipoles centered at 5.1 MHz, giving 22 dB of gain, and three more at 8.175 MHz, for almost 26 dB. The first frequency has been used in two successful campaigns, and the second is expected to be ready for the coming campaign. The transmitter building is located in the maintenance area and twelve three inch coaxial lines feed the individual antenna elements. A system for setting the timing and phasing of the transmitters is located in a control room extending from the transmitter building. For further information you can contact Michael Sulzer (email@example.com).
The 430 MHz Incoherent Scatter Radar (ISR) is capable of extremely sensitive diagnostics for HF modification experiments. Power from the pulsed 2.5 MW (currently about 1.3 to 1.5 MW) transmitter can be split with arbitrary ratio into two beams, allowing sensing through the center of the modified region simultaneously with sensing outside of it or near its edge. Possible geometries are set by the locations of the two feeds on opposite sides of the rotatable azimuth arm, with the minimum zenith angle differences set by the physical sizes of the feeds. Raw data can be collected with a 25 MHz wide data taking system for later analysis while a narrower bandwidth system is used to provide on line monitoring. The current coding technique allows 300 m range resolution on the enhanced plasma line while ion line and natural plasma line data are also recorded from the same radar pulses. There some restrictions in simultaneous viewing resulting from the extremely high signal power in the enhanced plasma line. For further information you can contact Michael Sulzer (firstname.lastname@example.org).
At Arecibo we have a variety of airglow and lidar instrumentation. Presently, airglow sensing equipment includes two Tilting-Filter Photometers, three Fabry-Perot Interferometers, and two All-sky Imagers. These instruments are located about 1000 feet from the center of the incoherent scatter radar.
The "active" optical instruments (lidars) have the capability to monitor the upper stratosphere to lower thermosphere. We have three systems, two of which are configurable to monitor one each of the meteoric metals: Na, Fe, Ca, or Ca+. Alternatively, one of the two metal lidars can be configured as a Rayleigh lidar to measure temperature from the upper stratosphere to the mesosphere, from about 35 to 70 km. The third lidar is a Doppler-resonance lidar that measures temperatures within the metal layer by sensing the Doppler broadening in the D1 resonance line of K.
Request for optical instrument support for HF experiments must be included in the proposal. We encourage the PIs to contact our staff for special optical configurations and further information: Jonathan Friedman (email@example.com), Shikha Raizada (firstname.lastname@example.org), or Jens Lautenbach (email@example.com).
The AO-ROF is located on Culebra Island (18°18′18″N; 65°18′05″W), Puerto Rico, about 96 miles east of the Arecibo Observatory. The design of the facility enables it to host two optical instruments requiring large domes (5-ft diameter) and four optical instruments that require smaller domes (1-ft diameter). Exterior space is also available for the installation of radio receivers or other kinds of instrumentation.
For every campaign the SAS department will be providing the F2 peak parameters prediction in order to help the users to define the best way to conduct their experiments. These predictions will be accessible on our website at least a month prior of every campaign (link). The predictions will provide different scenarios depending on the solar activity, historical ionosonde and ISR registers. For further information you can contact Christiano Brum (firstname.lastname@example.org)
Please email any questions about this call for proposals to Christiano Brum (email@example.com).
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