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25 April 2024

» arxiv » 1912.6212

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The 1.28 GHz MeerKAT DEEP2 Image
T. Mauch ; W. D. Cotton ; J. J. Condon ; A. M. Matthews ; T. D. Abbott ; R. M. Adam ; M. A. Aldera ; K. M. B. Asad ; E. F. Bauermeister ; T. G. H. Bennett ; H. Bester ; D. H. Botha ; L. R. S. Brederode ; Z. B. Brits ; S. J. Buchner ; J. P. Burger ; F. Camilo ; J. M. Chalmers ; T. Cheetham ; D. de Villiers ; M. S. de Villiers ; M. A. Dikgale-Mahlakoana ; L. J. du Toit ; S. W. P. Esterhuyse ; G. Fadana ; B. L. Fanaroff ; S. Fataar ; S. February ; B. S. Frank ; R. R. G. Gamatham ; M. Geyer ; S. Goedhart ; S. Gounden ; S. C. Gumede ; I. Heywood ; M. J. Hlakola ; J. M. G. Horrell ; B. Hugo ; A. R. Isaacson ; G. I. G. Józsa ; J. L. Jonas ; R. P. M. Julie ; F. B. Kapp ; V. A. Kasper ; J. S. Kenyon ; P. P. A. Kotzé ; N. Kriek ; H. Kriel ; T. W. Kusel ; R. Lehmensiek ; A. Loots ; R. T. Lord ; B. M. Lunsky ; K. Madisa ; L. G. Magnus ; J. P. L. Main ; J. A. Malan ; J. R. Manley ; S. J. Marais ; A. Martens ; B. Merry ; R. Millenaar ; N. Mnyandu ; I. P. T. Moeng ; O. J. Mokone ; T. E. Monama ; M. C. Mphego ; W. S. New ; B. Ngcebetsha ; K. J. Ngoasheng ; M. T. O. Ockards ; N. Oozeer ; A. J. Otto ; A. A. Patel ; A. Peens-Hough ; S. J. Perkins ; A. J. T. Ramaila ; Z. R. Ramudzuli ; R. Renil ; L. L. Richter ; A. Robyntjies ; S. Salie ; C. T. G. Schollar ; L. C. Schwardt ; M. Serylak ; R. Siebrits ; S. K. Sirothia ; O. M. Smirnov ; L. Sofeya ; G. Stone ; B. Taljaard ; C. Tasse ; I. P. Theron ; A. J. Tiplady ; O. Toruvanda ; S. N. Twum ; T. J. van Balla ; A. van der Byl ; C. van der Merwe ; V. Van Tonder ; B. H. Wallace ; M. G. Welz ; L. P. Williams ; B. Xaia ;
Date:	12 Dec 2019
Abstract:	We present the confusion-limited 1.28 GHz MeerKAT DEEP2 image covering one $approx 68’$ FWHM primary beam area with $7.6’’$ FWHM resolution and $0.55 pm 0.01$ $mu$Jy/beam rms noise. Its J2000 center position $alpha=04^h 13^m 26.4^s$, $delta=-80^circ 00’ 00’’$ was selected to minimize artifacts caused by bright sources. We introduce the new 64-element MeerKAT array and describe commissioning observations to measure the primary beam attenuation pattern, estimate telescope pointing errors, and pinpoint $(u,v)$ coordinate errors caused by offsets in frequency or time. We constructed a 1.4 GHz differential source count by combining a power-law count fit to the DEEP2 confusion $P(D)$ distribution from $0.25$ to $10$ $mu$Jy with counts of individual DEEP2 sources between $10$ $mu$Jy and $2.5$ mJy. Most sources fainter than $S sim 100$ $mu$Jy are distant star-forming galaxies obeying the FIR/radio correlation, and sources stronger than $0.25$ $mu$Jy account for $sim93\%$ of the radio background produced by star-forming galaxies. For the first time, the DEEP2 source count has reached the depth needed to reveal the majority of the star formation history of the universe. A pure luminosity evolution of the 1.4 GHz local luminosity function consistent with the Madau & Dickinson (2014) model for the evolution of star-forming galaxies based on UV and infrared data underpredicts our 1.4 GHz source count in the range $-5 lesssim log[S(mathrm{Jy})] lesssim -4$.
Source:	arXiv, 1912.6212
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