An ultra-wide bandwidth (704 to 4 032 MHz) receiver for the Parkes radio telescope

Hobbs, G.; Manchester, R. N.; Dunning, Alex; Jameson, A.; Roberts, P.; George, D.; Green, James; Tuthill, J.; Toomey, Lawrence; Kaczmarek, Jane; Mader, Stacy; Marquarding, M.; Ahmed, Azeem; Amy, S. W.; Bailes, M.; Beresford, Ron; Bhat, N. D. R.; Bock, Douglas C.-J.; Bourne, Michael; Bowen, Mark; Brothers, M.; Cameron, Andrew D.; Carretti, E.; Carter, Nick; Castillo, Santy; Chekkala, R.; Cheng, Wan; Chung, Y.; Craig, Daniel A.; Dai, Shi; Dawson, J. R.; Dempsey, James; Doherty, Paul; Dong, Bin; Edwards, P. G.; Ergesh, T.; Gao, X.; Han, J. L.; Hayman, Douglas B.; Indermuehle, B.; Jeganathan, K.; Johnston, S.; Kanoniuk, Henry; Kesteven, Michael; Krämer, M.; Leach, M.; McIntyre, Vince; Moss, V. A.; Osłowski, S.; Phillips, Chris; Pope, Nathan; Preisig, Brett; Price, D. C.; Reeves, Ken; Reilly, Les; Reynolds, John; Robishaw, Timothy; Roush, Peter; Ruckley, Tim; Sadler, E. M.; Sarkissian, John; Severs, Sean; Shannon, R. M.; Smart, Ken; Smith, Malcolm R.; Smith, Stephanie; Sobey, C.; Staveley‐Smith, L.; Tzioumis, A. K.; Straten, W. van; Wang, Na; Wen, L.; Whiting, M. T.

doi:10.1017/pasa.2020.2

Cited by 167 publications

(100 citation statements)

References 41 publications

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“…As a point of comparison, evaluating (14) for a Gaussian beam yields a survey speed of 0.721 G S 2 max , where G is the half power field of view of the Gaussian beam. Using this measure, the survey speed of ASKAP at 1.4 GHz is 245 times faster than the Parkes 64 m dish with a cryogenic single-pixel receiver having T sys /η of 40 k (Hobbs et al 2020).…”

Section: Survey Speedmentioning

confidence: 99%

Australian square kilometre array pathfinder: I. system description

Hotan

Bunton

Chippendale

et al. 2021

Publ. Astron. Soc. Aust.

214

159

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In this paper, we describe the system design and capabilities of the Australian Square Kilometre Array Pathfinder (ASKAP) radio telescope at the conclusion of its construction project and commencement of science operations. ASKAP is one of the first radio telescopes to deploy phased array feed (PAF) technology on a large scale, giving it an instantaneous field of view that covers $31\,\textrm{deg}^{2}$ at $800\,\textrm{MHz}$ . As a two-dimensional array of 36 $\times$ 12 m antennas, with baselines ranging from 22 m to 6 km, ASKAP also has excellent snapshot imaging capability and 10 arcsec resolution. This, combined with 288 MHz of instantaneous bandwidth and a unique third axis of rotation on each antenna, gives ASKAP the capability to create high dynamic range images of large sky areas very quickly. It is an excellent telescope for surveys between 700 and $1800\,\textrm{MHz}$ and is expected to facilitate great advances in our understanding of galaxy formation, cosmology, and radio transients while opening new parameter space for discovery of the unknown.

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Section: Survey Speedmentioning

confidence: 99%

Australian square kilometre array pathfinder: I. system description

Hotan

Bunton

Chippendale

et al. 2021

Publ. Astron. Soc. Aust.

214

159

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“….7-4.0 GHz) at at least one of our facilities in the near future (see Ransom et al 2019). Indeed, large fractional-bandwidth receivers have already been deployed by the PPTA (Hobbs et al 2020) and the EPTA (Freire 2012) for high-precision pulsar timing, and largefractional bandwidth or multi-band sub-arraying capabilities are either planned or are implemented in all of the aforementioned efforts.…”

Section: ∼0mentioning

confidence: 99%

The NANOGrav 12.5 yr Data Set: Observations and Narrowband Timing of 47 Millisecond Pulsars

Alam¹,

Arzoumanian²,

Baker³

et al. 2020

ApJS

134

109

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We present a new analysis of the profile data from the 47 millisecond pulsars comprising the 12.5year data set of the North American Nanohertz Observatory for Gravitational Waves (NANOGrav), which is presented in a parallel paper (Alam et al. 2020, NG12.5). Our reprocessing is performed using "wideband" timing methods, which use frequency-dependent template profiles, simultaneous time-of-arrival (TOA) and dispersion measure (DM) measurements from broadband observations, and novel analysis techniques. In particular, the wideband DM measurements are used to constrain the DM portion of the timing model. We compare the ensemble timing results to NG12.5 by examining the timing residuals, timing models, and noise model components. There is a remarkable level of agreement across all metrics considered. Our best-timed pulsars produce encouragingly similar results to those from NG12.5. In certain cases, such as high-DM pulsars with profile broadening, or sources that are weak and scintillating, wideband timing techniques prove to be beneficial, leading to more precise timing model parameters by 10 − 15%. The high-precision, multi-band measurements of several pulsars indicate frequency-dependent DMs. Compared to the narrowband analysis in NG12.5, the TOA volume is reduced by a factor of 33, which may ultimately facilitate computational speed-ups for complex pulsar timing array analyses. This first wideband pulsar timing data set is a stepping stone, and its consistent results with NG12.5 assure us that such data sets are appropriate for gravitational wave analyses.

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“…Additionally, we note that Ziurys & Turner (1985) quote a velocity resolution 1.4 km s -1 , whereas our observations have a velocity resolution of 0.25 km s -1 . With the Parkes 64-m Telescope fitted with the new Ultra-wideband receiver (Hobbs et al 2020), we detected CH in the eastern lobe (IRS1) at 3.264 GHz in a 10min snapshot image. Therefore, we know the molecule to exist in the region, and more observing time should yield a detection of the low-frequency transitions.…”

Section: Results and Limits For Detectionmentioning

confidence: 99%

“…The CSIRO Parkes 64-m Telescope, an SKA technology pathfinder, has a new ultra-wide band receiver (Hobbs et al 2020), which covers the frequency range of 704-4 000 MHz, allowing simultaneous studies of the 724.788 MHz and ∼3.3 GHz CH transitions. Rydbeck et al (1973) observed CH ground state transitions at 3.264 GHz in 17 HII regions.…”

Section: Implications For Future Studiesmentioning

confidence: 99%

First search for low-frequency CH with a Square Kilometre Array precursor telescope

Tremblay

Green

Mader

et al. 2020

Publ. Astron. Soc. Aust.

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The diatomic free radical methylidyne (CH) is an important tracer of the interstellar medium, and the study of it was critical to our earliest understanding of star formation. Although it is detectable across the electromagnetic spectrum, observations at radio frequencies allow for a study of the kinematics of the diffuse and dense gas in regions of new star formation. There is only two published (single-dish) detections of the low-frequency hyperfine transitions between 700 and 725 MHz, despite the precise frequencies being known. These low-frequency transitions are of particular interest as they are shown in laboratory experiments to be more sensitive to magnetic fields than their high-frequency counterparts (with more pronounced Zeeman splitting). In this work, we take advantage of the radio quiet environment and increased resolution of the Australian Square Kilometre Array Pathfinder (ASKAP) over previous searches to make a pilot interferometric search for CH at 724.7883 MHz (the strongest of the hyperfine transitions) in RCW 38. We found the band is clean of radio frequency interference, but we did not detect the signal from this transition to a five-sigma sensitivity limit of 0.09 Jy, which corresponds to a total column density upper limit of 1.9 $\times 10^{18}$ cm–2 for emission and 1.3 $\times 10^{14}$ cm–2 for absorption with an optical depth limit of 0.95. Achieved within 5 h of integration, this column density sensitivity should have been adequate to detect the emission or absorption in RCW 38, if it had similar properties to the only previous reported detections in W51.

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An ultra-wide bandwidth (704 to 4 032 MHz) receiver for the Parkes radio telescope

Cited by 167 publications

References 41 publications

Australian square kilometre array pathfinder: I. system description

Australian square kilometre array pathfinder: I. system description

The NANOGrav 12.5 yr Data Set: Observations and Narrowband Timing of 47 Millisecond Pulsars

First search for low-frequency CH with a Square Kilometre Array precursor telescope

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