For the September 7, 2017 proposal deadline.
- Proposal policies, submission details, and a web-based cover
sheet, can be found linked from the
- New users should read the Guide
for New Arecibo Users
- Other user-related information is to be found on the
- Radio sources with declinations in the range -1° < Dec <
+37.5° are visible from Arecibo, and can be tracked over zenith angles
between 1.1° and 19.7°.
- Available receivers in the (frequency-agile) Gregorian Dome, their
frequency coverage, typical System Temperature, Telescope Gain and
current status are listed in the
table of receivers.
- Pulsar, spectral-line, VLBI, and continuum backends are available to
exploit all of these receivers. Details are available on the Radio Astronomy Backends page.
- The PUPPI pulsar backend provides a maximum bandwidth of 800 MHz, up to 4096 spectral channels, and 40.96 µs minimum sampling time in search mode. In addition, 20.48 µs sampling is possible in on-line folding mode. For more details, potential users can refer to the PUPPI observing and support guide. PUPPI is now available for all receivers, including those above 3 GHz.
- As part of their data management plan, PUPPI users should include details
of how they will ensure their data is removed from the PUPPI drives in a
- The 2 x 7, dual-polarization, 300-MHz bandwidth, "Mock"
spectrometers are available to all ALFA users. For details see
Mock Spectrometers for ALFA users.
- A SINGLE-PIXEL MODE for the Mock spectrometers
is available. This can provide up to 1 GHz of contiguous spectral
coverage. On-line pulsar folding is not yet supported. For
use of the Mock spectrometers with a single-pixel receiver, see
Specifics for Mock Single-Pixel mode .
- The WAPP spectrometer provides an 8-band, dual-polarization,
single-pixel observing capability for spectral lines or pulsars.
This device can be used to place 8 independent bands over a 1-GHz range,
each band having up to 100-MHz bandwidth. A contiguous 680-MHz
spectral coverage can be obtained after allowing for filter
roll-off. For an overview of WAPP capabilities, see
WAPP spectrometer information.
- Mk-5A and Mk-5C disc-based recorders for Very Long Baseline
Interferometry (VLBI) are available for use with the HSA, EVN and
Global networks at all bands up to 10 GHz. Those wishing to include
the ultra-high sensitivity of Arecibo in their VLBI observations should
submit proposals directly to these networks rather than to Arecibo, but
include justification for usage of the 305-m telescope. The maximum data
recording rate at Arecibo is 2 Gbps with the Mk-5C, and 1 Gbps with the
Mk-5A. eVLBI science observations with the EVN can be made up to 512 Mbps.
- The new C-Band Wide receiver, covering the full 4-8 GHz frequency range, is
currently being commissioned and is expected to become available for
observations during the 2018A semester. This receiver is expected
to have a Tsys in the range 25–35 K and will be circularly
- The new C-Band Wide receiver has replaced the 6-8 GHz C-High receiver,
which is no longer available for observations. The 4-6 GHz C-band receiver
remains available at this time.
- A plan to incorporate a wider-band signal path than the current 1-GHz limit
is in development, but is unlikely to be available for the 2018A