Publications of the Astronomical Society of Australia最新文献

{"title":"The host galaxy of FRB 20171020A revisited","authors":"K. Lee-Waddell, C. W. James, S. Ryder, E. Mahony, A. Bahramian, Baerbel Koribalski, Pravir Kumar, L. Marnoch, F. North-Hickey, E. Sadler, R. Shannon, N. Tejos, J. Thorne, J. Wang, R. Wayth","doi":"10.1017/pasa.2023.27","DOIUrl":"https://doi.org/10.1017/pasa.2023.27","url":null,"abstract":"Abstract The putative host galaxy of FRB 20171020A was first identified as ESO 601-G036 in 2018, but as no repeat bursts have been detected, direct confirmation of the host remains elusive. In light of recent developments in the field, we re-examine this host and determine a new association confidence level of 98%. At 37 Mpc, this makes ESO 601-G036 the third closest FRB host galaxy to be identified to date and the closest to host an apparently non-repeating FRB (with an estimated repetition rate limit of \u0000$<$\u0000 \u0000$0.011$\u0000 bursts per day above \u0000$10^{39}$\u0000 erg). Due to its close distance, we are able to perform detailed multi-wavelength analysis on the ESO 601-G036 system. Follow-up observations confirm ESO 601-G036 to be a typical star-forming galaxy with H i and stellar masses of \u0000$log_{10}!(M_{rm{H,{small I}}} / M_odot) sim 9.2$\u0000 and \u0000$log_{10}!(M_star / M_odot) = 8.64^{+0.03}_{-0.15}$\u0000 , and a star formation rate of \u0000$text{SFR} = 0.09 pm 0.01,{rm M}_odot,text{yr}^{-1}$\u0000 . We detect, for the first time, a diffuse gaseous tail ( \u0000$log_{10}!(M_{rm{H,{small I}}} / M_odot) sim 8.3$\u0000 ) extending to the south-west that suggests recent interactions, likely with the confirmed nearby companion ESO 601-G037. ESO 601-G037 is a stellar shred located to the south of ESO 601-G036 that has an arc-like morphology, is about an order of magnitude less massive, and has a lower gas metallicity that is indicative of a younger stellar population. The properties of the ESO 601-G036 system indicate an ongoing minor merger event, which is affecting the overall gaseous component of the system and the stars within ESO 601-G037. Such activity is consistent with current FRB progenitor models involving magnetars and the signs of recent interactions in other nearby FRB host galaxies.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":null,"pages":null},"PeriodicalIF":6.3,"publicationDate":"2023-05-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"82740750","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"HYPEREION—A precision system for the detection of the absorption profile centred at 78 MHz in the radio background spectrum","authors":"N. Patra, R. Wayth, M. Sokolowski, D. Price, B. McKinley, D. Kenney","doi":"10.1017/pasa.2023.25","DOIUrl":"https://doi.org/10.1017/pasa.2023.25","url":null,"abstract":"Abstract The report of a detection of an absorption profile centred at 78 MHz in the continuum radio background spectrum by the EDGES experiment and its interpretation as the redshifted 21 cm signal of cosmological origin has become one of the most debated results of observational cosmology in recent times. The cosmological 21 cm has long been proposed to be a powerful probe for observing the early Universe and tracing its evolution over cosmic time. Even though the science case is well established, measurement challenges posed on the technical ground are not fully understood to the level of claiming a successful detection. EDGES’s detection has naturally motivated a number of experimental attempts worldwide to corroborate the findings. In this paper, we present a precision cross-correlation spectrometer HYPEREION purpose-designed for a precision radio background measurement between 50–120 MHz to detect the absorption profile reported by the EDGES experiment. HYPEREION implements a pre-correlation signal processing technique that self-calibrates any spurious additive contamination from within the system and delivers a differential measurement of the sky spectrum and a reference thermal load internal to the system. This ensures an unambiguous ‘zero-point’ of absolute calibration of the purported absorption profile. We present the system design, measurement equations of the ideal system, systematic effects in the real system, and finally, an assessment of the real system output for the detection of the absorption profile at 78 MHz in the continuum radio background spectrum.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":null,"pages":null},"PeriodicalIF":6.3,"publicationDate":"2023-05-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73320569","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Hydra II: Characterisation of Aegean, Caesar, ProFound, PyBDSF, and Selavy source finders","authors":"M. Boyce, A. Hopkins, S. Riggi, L. Rudnick, M. Ramsay, C. Hale, J. Marvil, M. Whiting, P. Venkataraman, C. O’Dea, S. Baum, Y. Gordon, A. Vantyghem, M. Dionyssiou, H. Andernach, J. Collier, J. English, B. Koribalski, D. Leahy, M. Michałowski, S. Safi-Harb, M. Vaccari, Elaine L. Alexander, M. Cowley, A. Kapinska, A. Robotham, H. Tang","doi":"10.1017/pasa.2023.29","DOIUrl":"https://doi.org/10.1017/pasa.2023.29","url":null,"abstract":"Abstract We present a comparison between the performance of a selection of source finders (SFs) using a new software tool called Hydra. The companion paper, Paper I, introduced the Hydra tool and demonstrated its performance using simulated data. Here we apply Hydra to assess the performance of different source finders by analysing real observational data taken from the Evolutionary Map of the Universe (EMU) Pilot Survey. EMU is a wide-field radio continuum survey whose primary goal is to make a deep ( \u0000$20mu$\u0000 Jy/beam RMS noise), intermediate angular resolution ( \u0000$15^{primeprime}$\u0000 ), 1 GHz survey of the entire sky south of \u0000$+30^{circ}$\u0000 declination, and expecting to detect and catalogue up to 40 million sources. With the main EMU survey it is highly desirable to understand the performance of radio image SF software and to identify an approach that optimises source detection capabilities. Hydra has been developed to refine this process, as well as to deliver a range of metrics and source finding data products from multiple SFs. We present the performance of the five SFs tested here in terms of their completeness and reliability statistics, their flux density and source size measurements, and an exploration of case studies to highlight finder-specific limitations.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":null,"pages":null},"PeriodicalIF":6.3,"publicationDate":"2023-04-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"84645737","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Hydra I: An extensible multi-source-finder comparison and cataloguing tool","authors":"M. Boyce, A. Hopkins, S. Riggi, L. Rudnick, M. Ramsay, C. Hale, J. Marvil, M. Whiting, P. Venkataraman, C. O’Dea, S. Baum, Y. Gordon, A. Vantyghem, M. Dionyssiou, H. Andernach, J. Collier, J. English, B. Koribalski, D. Leahy, M. Michałowski, S. Safi-Harb, M. Vaccari, Elaine L. Alexander, M. Cowley, A. Kapinska, A. Robotham, H. Tang","doi":"10.1017/pasa.2023.24","DOIUrl":"https://doi.org/10.1017/pasa.2023.24","url":null,"abstract":"Abstract The latest generation of radio surveys are now producing sky survey images containing many millions of radio sources. In this context it is highly desirable to understand the performance of radio image source finder (SF) software and to identify an approach that optimises source detection capabilities. We have created Hydra to be an extensible multi-SF and cataloguing tool that can be used to compare and evaluate different SFs. Hydra, which currently includes the SFs Aegean, Caesar, ProFound, PyBDSF, and Selavy, provides for the addition of new SFs through containerisation and configuration files. The SF input RMS noise and island parameters are optimised to a 90% ‘percentage real detections’ threshold (calculated from the difference between detections in the real and inverted images), to enable comparison between SFs. Hydra provides completeness and reliability diagnostics through observed-deep ( \u0000$mathcal{D}$\u0000 ) and generated-shallow ( \u0000$mathcal{S}$\u0000 ) images, as well as other statistics. In addition, it has a visual inspection tool for comparing residual images through various selection filters, such as S/N bins in completeness or reliability. The tool allows the user to easily compare and evaluate different SFs in order to choose their desired SF, or a combination thereof. This paper is part one of a two part series. In this paper we introduce the Hydra software suite and validate its \u0000$mathcal{D/S}$\u0000 metrics using simulated data. The companion paper demonstrates the utility of Hydra by comparing the performance of SFs using both simulated and real images.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":null,"pages":null},"PeriodicalIF":6.3,"publicationDate":"2023-04-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77952160","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"M dwarfs found in the first Byurakan spectral sky survey database. Gaia EDR3 and TESS data. Some preliminary results","authors":"K. Gigoyan, A. Sarkissian, G. Kostandyan, K. Gigoyan, M. Meftah, S. Bekki, N. Azatyan, F. Zamkotsian","doi":"10.1017/pasa.2023.20","DOIUrl":"https://doi.org/10.1017/pasa.2023.20","url":null,"abstract":"Abstract In order to gain more information on the 236 M dwarfs identified in the First Byurakan Survey (FBS) low-resolution (lr) spectroscopic database, Gaia EDR3 high-accuracy astrometric and photometric data and Transiting Exoplanet Survey Satellite (TESS) data are used to characterise these M dwarfs and their possible multiplicity. Among the sample of 236 relatively bright \u0000$(7.3 < K_S < 14.4)$\u0000 M dwarfs, 176 are new discoveries. The Gaia EDR3 G broadband magnitudes are in the range \u0000$11.3 < G < 17.1$\u0000 . New distance information based on the EDR3 parallaxes are used to estimate the G-band absolute magnitudes. Nine FBS M dwarfs out of 176 newly discovered lie within 25 pc of the Sun. The FBS 0909-082 is the most distant \u0000$(r=780$\u0000 pc) M dwarf of the analysed sample, with a G-band absolute magnitude \u0000$M(G) = 9.18$\u0000 , \u0000$M = 0.59$\u0000 M \u0000$_{odot}$\u0000 , \u0000$L = 0.13597$\u0000 L \u0000$_{odot}$\u0000 , and \u0000$T_{eff}$\u0000 = 3844 K; it can be classified as M1 - M2 subtype dwarf. The nearest is FBS 0250+167, a M7 subtype dwarf located at 3.83 pc from the Sun with a very high proper motion (5.13 arcsec yr \u0000$^{-1}$\u0000 ). The TESS estimated masses lie in the range 0.095 ( \u0000$pm$\u0000 0.02) M \u0000$_{odot}leq$\u0000 \u0000$Mleq$\u0000 0.7 ( \u0000$pm$\u0000 0.1) M \u0000$_{odot}$\u0000 and \u0000$T_{eff}$\u0000 in the range 4000 K < \u0000$T_{eff}$\u0000 < 2790 K. We analyse colour-colour and colour-absolute magnitude diagram (CaMD) diagrams for the M dwarfs. Results suggest that 27 FBS M dwarfs are double or multiple systems. The observed spectral energy distribution (SED) for some of the M dwarfs can be used to classify potential infrared excess. Using TESS light curves, flares are detected for some FBS M dwarfs. Finally, for early and late sub-classes of the M dwarfs, the detection range for survey is estimated for the first time.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":null,"pages":null},"PeriodicalIF":6.3,"publicationDate":"2023-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74647154","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The role of impact parameter in typical close galaxy flybys","authors":"A. Mitrašinović, M. Micic","doi":"10.1017/pasa.2023.23","DOIUrl":"https://doi.org/10.1017/pasa.2023.23","url":null,"abstract":"Abstract Close galaxy flybys, interactions during which two galaxies inter-penetrate, are frequent and can significantly affect the evolution of individual galaxies. Equal-mass flybys are extremely rare and almost exclusively distant, while frequent flybys have mass ratios \u0000$q=0.1$\u0000 or lower, with a secondary galaxy penetrating deep into the primary. This can result in comparable strengths of interaction between the two classes of flybys and lead to essentially the same effects. To demonstrate this, emphasise and explore the role of the impact parameter further, we performed a series of N-body simulations of typical flybys with varying relative impact parameters \u0000$b/R_{mathrm{vir},1}$\u0000 ranging from \u0000$0.114$\u0000 to \u0000$0.272$\u0000 of the virial radius of the primary galaxy. Two-armed spirals form during flybys, with radii of origin correlated with the impact parameter and strengths well approximated with an inverted S-curve. The impact parameter does not affect the shape of induced spirals, and the lifetimes of a distinguished spiral structure appear to be constant, \u0000$T_mathrm{LF} sim 2$\u0000 Gyr. Bars, with strengths anti-correlated with the impact parameter, form after the encounter is over in simulations with \u0000$b/R_{mathrm{vir},1} leq 0.178$\u0000 and interaction strengths \u0000$Sgeq0.076$\u0000 , but they are short-lived except for the stronger interactions with \u0000$Sgeq0.129$\u0000 . We showcase an occurrence of multiple structures (ring-like, double bar) that survives for an exceptionally long time in one of the simulations. Effects on the pre-existing bar instability, that develops much later, are diverse: from an acceleration of bar formation, little to no effect, to even bar suppression. There is no uniform correlation between these effects and the impact parameter, as they are secondary effects, happening later in a post-flyby stage. Classical bulges are resilient to flyby interactions, while dark matter halos can significantly spin up in the amount anti-correlated with the impact parameter. There is an offset angle between the angular momentum vector of the dark matter halo and that of a disc, and it correlates linearly with the impact parameter. Thus, flybys remain an important pathway for structural evolution within galaxies in the local Universe.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":null,"pages":null},"PeriodicalIF":6.3,"publicationDate":"2023-04-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81879462","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The thermal history of the intergalactic medium at 3.9 ≤ z ≤ 4.3","authors":"T. Ondro, R. Gális","doi":"10.1017/pasa.2023.22","DOIUrl":"https://doi.org/10.1017/pasa.2023.22","url":null,"abstract":"Abstract A new determination of the temperature of the intergalactic medium (IGM) over \u0000$3.9 leq z leq 4.3$\u0000 is presented. We applied the curvature method on a sample of 10 high-resolution quasar spectra from the Ultraviolet and Visual Echelle Spectrograph on the VLT/ESO. We measured the temperature at mean density by determining the temperature at the characteristic overdensity, which is tight function of the absolute curvature irrespective of \u0000$unicode{x03B3}$\u0000 . Under the assumption of fiducial value of \u0000$unicode{x03B3} = 1.4$\u0000 , we determined the values of temperatures at mean density \u0000$T_{0} = 7893^{+1417}_{-1226}$\u0000 K and \u0000$T_{0} = 8153^{+1224}_{-993}$\u0000 K for redshift range of \u0000$3.9 leq z leq 4.1$\u0000 and \u0000$4.1 leq z leq 4.3$\u0000 , respectively. Even though the results show no strong temperature evolution over the studied redshift range, our measurements are consistent with an IGM thermal history that includes a contribution from He ii reionisation.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":null,"pages":null},"PeriodicalIF":6.3,"publicationDate":"2023-04-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74094128","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Hi in Ring Galaxies Survey (Hi-RINGS)—Effects of the bar on the Hi gas in ring galaxies","authors":"C. Murugeshan, R. Džudžar, R. Bagge, T. O'Beirne, O. I. Wong, V. Kilborn, M. Cluver, K. Lutz, A. Elagali","doi":"10.1017/pasa.2023.19","DOIUrl":"https://doi.org/10.1017/pasa.2023.19","url":null,"abstract":"Abstract We present a new high-resolution neutral atomic hydrogen (Hi) survey of ring galaxies using the Australia Telescope Compact Array (ATCA). We target a sample of 24 ring galaxies from the Buta (1995) Southern Ring Galaxy Survey Catalogue in order to study the origin of resonance-, collisional- and interaction-driven ring galaxies. In this work, we present an overview of the sample and study their global and resolved Hi properties. In addition, we also probe their star formation properties by measuring their star formation rates (SFR) and their resolved SFR surface density profiles. We find that a majority of the barred galaxies in our sample are Hi-deficient, alluding to the effects of the bar in driving their Hi deficiency. Furthermore, for the secularly evolving barred ring galaxies in our sample, we apply Lindblad’s resonance theory to predict the location of the resonance rings and find very good agreement between predictions and observations. We identify rings of Hi gas and/or star formation co-located at one or the other major resonances. Lastly, we measure the bar pattern speed ( \u0000$Omega_{textrm{bar}}$\u0000 ) for a sub-sample of our galaxies and find that the values range from 10–90 \u0000$textrm{km s}^{-1}$\u0000 kpc \u0000$^{-1}$\u0000 , in good agreement with previous studies.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":null,"pages":null},"PeriodicalIF":6.3,"publicationDate":"2023-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"78387711","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Classical novae in the ASKAP pilot surveys","authors":"Ashna Gulati, T. Murphy, D. Kaplan, R. Soria, J. Leung, Yuanming Wang, J. Pritchard, E. Lenc, S. Duchesne, A. O’Brien","doi":"10.1017/pasa.2023.21","DOIUrl":"https://doi.org/10.1017/pasa.2023.21","url":null,"abstract":"Abstract We present a systematic search for radio counterparts of novae using the Australian Square Kilometer Array Pathfinder (ASKAP). Our search used the Rapid ASKAP Continuum Survey, which covered the entire sky south of declination \u0000$+41^{circ}$\u0000 ( \u0000$sim$\u0000 \u0000$34000$\u0000 square degrees) at a central frequency of 887.5 MHz, the Variables and Slow Transients Pilot Survey, which covered \u0000$sim$\u0000 \u0000$5000$\u0000 square degrees per epoch (887.5 MHz), and other ASKAP pilot surveys, which covered \u0000$sim$\u0000 200–2000 square degrees with 2–12 h integration times. We crossmatched radio sources found in these surveys over a two–year period, from 2019 April to 2021 August, with 440 previously identified optical novae, and found radio counterparts for four novae: V5668 Sgr, V1369 Cen, YZ Ret, and RR Tel. Follow-up observations with the Australian Telescope Compact Array confirm the ejecta thinning across all observed bands with spectral analysis indicative of synchrotron emission in V1369 Cen and YZ Ret. Our light-curve fit with the Hubble Flow model yields a value of \u0000$1.65pm 0.17 times 10^{-4} rm :M_odot$\u0000 for the mass ejected in V1369 Cen. We also derive a peak surface brightness temperature of \u0000$250pm80$\u0000 K for YZ Ret. Using Hubble Flow model simulated radio lightcurves for novae, we demonstrate that with a 5 \u0000$sigma$\u0000 sensitivity limit of 1.5 mJy in 15-min survey observations, we can detect radio emission up to a distance of 4 kpc if ejecta mass is in the range \u0000$10^{-3}rm :M_odot$\u0000 , and upto 1 kpc if ejecta mass is in the range \u0000$10^{-5}$\u0000 – \u0000$10^{-3}rm :M_odot$\u0000 . Our study highlights ASKAP’s ability to contribute to future radio observations for novae within a distance of 1 kpc hosted on white dwarfs with masses \u0000$0.4$\u0000 – \u0000$1.25:rm M_odot$\u0000 , and within a distance of 4 kpc hosted on white dwarfs with masses \u0000$0.4$\u0000 – \u0000$1.0:rm M_odot$\u0000 .","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":null,"pages":null},"PeriodicalIF":6.3,"publicationDate":"2023-03-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"85237905","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"MWAX: A new correlator for the Murchison Widefield Array","authors":"I. Morrison, B. Crosse, G. Sleap, R. Wayth, A. Williams, M. Johnston-Hollitt, J. Jones, S. Tingay, M. Walker, L. Williams","doi":"10.1017/pasa.2023.15","DOIUrl":"https://doi.org/10.1017/pasa.2023.15","url":null,"abstract":"Abstract We describe the design, validation, and commissioning of a new correlator termed ‘MWAX’ for the Murchison Widefield Array (MWA) low-frequency radio telescope. MWAX replaces an earlier generation MWA correlator, extending correlation capabilities and providing greater flexibility, scalability, and maintainability. MWAX is designed to exploit current and future Phase II/III upgrades to MWA infrastructure, most notably the simultaneous correlation of all 256 of the MWA’s antenna tiles (and potentially more in future). MWAX is a fully software-programmable correlator based around an ethernet multicast architecture. At its core is a cluster of 24 high-performance GPU-enabled commercial-off-the-shelf compute servers that together process in real-time up to 24 coarse channels of 1.28 MHz bandwidth each. The system is highly flexible and scalable in terms of the number of antenna tiles and number of coarse channels to be correlated, and it offers a wide range of frequency/time resolution combinations to users. We conclude with a roadmap of future enhancements and extensions that we anticipate will be progressively rolled out over time.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":null,"pages":null},"PeriodicalIF":6.3,"publicationDate":"2023-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"87295041","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}