CCERA and Carleton University begin collaboration

CCERA and the Physics department at Carleton University have begun a collaborative effort in support of their undergraduate astrophysics program.

In this program, 3rd-year astrophysics students will gain remote access to CCERA’s instrumentation and data-feeds in support of a lab-based radio astronomy segment in the 3rd-year astrophysics program.

The program is coordinated for Carleton University by Etienne Rollin and Penka Matanska, both instructors in the physics department at Carleton.

First of two 21cm “binocular” dishes brought on-line

The first of two 1.2m dishes for rapid surveys of the 21cm line has been brought on-line, and is currently observing at the declination of the galactic center (declination of -29 degrees).

The second dish will be brought on-line soon, which will allow spectral surveys do be completed at twice the rate of a single dish of the same size.

Stay “tuned” for more announcements….

A donated 12ft Andrew Dish!

John Blais, of Almonte, Ontario, very kindly donated a 12ft Andrew solid-aluminum dish to us. The long-term plan is to incorporate it into our pulsar work.

Here it is in the truck, ready to go off to the lab:

We’ll make up a very-simple fixed-pointing mount, which will have the dish pointed nearly-vertical, with a 9 degree tilt to the North.

Successful observations of Virgo A using 611-MHz interferometer

Using CCERA’s “insanely small array” radio telescope, we have successfully completed a 4-day “study” of the extragalactic radio source Virgo A. Show below are both the complex-correlator outputs, and the brightness derivation. Virgo A, also known as M87, is a massive galaxy some 54 million light-years from earth. It plays host to a super-massive black hole at the center, which produces a super-luminal (apparently-faster-than-light) gas “jet” of ejected material.

Its radio flux at 611MHz (our observing frequency) is approximately 500 Jansky, or 5×10^-24 Watts/M^2/Hz of bandwidth. Since our antenna are roughly 1 M^2 in area, That means that we’re intercepting a few pico-watts of power from this source!

Lab/office move complete, UHF interferometer operational

Our lab/office has successful moved downstairs, to Suite 104. We’re still working on bringing back some data services, like the 21cm spectrometer feed.

IN the last week, we’ve had success in making our UHF “pathfinder” interferometer operational, at a frequency of 611MHz, with a baseline of 33.5m. A “first light” interferogram from Virgo A is shown below. Virgo A, also known as M87, is a super massive elliptical galaxy roughly 54M light-years from earth. It is very luminous, making it easy to “see” with CCERA’s modest instrumentation.

CCERA lab/office moves

We’re nearing completion of the move of our office/lab space one floor down, from suite 204 to suite 104. This was necessitated by some “reconfiguration” required by our landlord.

One side effect of this move is that we’ll not be providing the 21cm data products for a few days as we rebuild our IT environment.

The move *may* also have the desirable side-effect of reducing self-interference from our computers, since we’ll be both further away from the antenna, and also have another layer of *thick* concrete and terra-cotta block floor between our lab and the antennae on the roof.

Pulsar array changes shape

We’ve re-jigged the pulsar array again, changing it from a 3 x 3 array to a 2 x 4 array. This geometry is much easier to manage, and it has allowed us to build a better reflector screen under the array, hopefully reducing the amount of ground radiation “seen” by the array elements.

Pulsar array upgrades

We’ve been working to improve the functionality of the pulsar array in order to enhance the reliability and verifiability of ongoing observations of PSRB0329+54.

Gary Atkins and Marcus Leech re-engineered the pulsar array support structure, and have been working on adding a “fence” around the array, to exclude low-angle RFI, which is where most terrestrial interference will be coming from. More work needs to be done to extend the fence around the entire array, but the array is now better-balanced on the support structure.

In addition the front-end electronics have been replaced to improve up-front filtering, using a custom UHF filter provided by Jan Jency in Slovakia. Further versions of this filter will allow us to observe on any of the 3 radio astronomy frequencies in the North American UHF band, while suppressing others.

A peak inside the new front end shows a noise injector, and a new 1/4-wave filter/protector

The noise injector hasn’t been connected yet, but will allow us to do a quick “sanity test” of the entire pulsar system from the comfort of the lab.

Stay tuned 🙂 🙂

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