%0 Generic %1 mauch2019meerkat %A Mauch, T. %A Cotton, W. D. %A Condon, J. J. %A Matthews, A. M. %A Abbott, T. D. %A Adam, R. M. %A Aldera, M. A. %A Asad, K. M. B. %A Bauermeister, E. F. %A Bennett, T. G. H. %A Bester, H. %A Botha, D. H. %A Brederode, L. R. S. %A Brits, Z. B. %A Buchner, S. J. %A Burger, J. P. %A Camilo, F. %A Chalmers, J. M. %A Cheetham, T. %A de Villiers, D. %A de Villiers, M. S. %A Dikgale-Mahlakoana, M. A. %A Toit, L. J. du %A Esterhuyse, S. W. P. %A Fadana, G. %A Fanaroff, B. L. %A Fataar, S. %A February, S. %A Frank, B. S. %A Gamatham, R. R. G. %A Geyer, M. %A Goedhart, S. %A Gounden, S. %A Gumede, S. C. %A Heywood, I. %A Hlakola, M. J. %A Horrell, J. M. G. %A Hugo, B. %A Isaacson, A. R. %A Józsa, G. I. G. %A Jonas, J. L. %A Julie, R. P. M. %A Kapp, F. B. %A Kasper, V. A. %A Kenyon, J. S. %A Kotzé, P. P. A. %A Kriek, N. %A Kriel, H. %A Kusel, T. W. %A Lehmensiek, R. %A Loots, A. %A Lord, R. T. %A Lunsky, B. M. %A Madisa, K. %A Magnus, L. G. %A Main, J. P. L. %A Malan, J. A. %A Manley, J. R. %A Marais, S. J. %A Martens, A. %A Merry, B. %A Millenaar, R. %A Mnyandu, N. %A Moeng, I. P. T. %A Mokone, O. J. %A Monama, T. E. %A Mphego, M. C. %A New, W. S. %A Ngcebetsha, B. %A Ngoasheng, K. J. %A Ockards, M. T. O. %A Oozeer, N. %A Otto, A. J. %A Patel, A. A. %A Peens-Hough, A. %A Perkins, S. J. %A Ramaila, A. J. T. %A Ramudzuli, Z. R. %A Renil, R. %A Richter, L. L. %A Robyntjies, A. %A Salie, S. %A Schollar, C. T. G. %A Schwardt, L. C. %A Serylak, M. %A Siebrits, R. %A Sirothia, S. K. %A Smirnov, O. M. %A Sofeya, L. %A Stone, G. %A Taljaard, B. %A Tasse, C. %A Theron, I. P. %A Tiplady, A. J. %A Toruvanda, O. %A Twum, S. N. %A van Balla, T. J. %A van der Byl, A. %A van der Merwe, C. %A Van Tonder, V. %A Wallace, B. H. %A Welz, M. G. %A Williams, L. P. %A Xaia, B. %D 2019 %K library %T The 1.28 GHz MeerKAT DEEP2 Image %U http://arxiv.org/abs/1912.06212 %X We present the confusion-limited 1.28 GHz MeerKAT DEEP2 image covering one $68'$ FWHM primary beam area with $7.6''$ FWHM resolution and $0.55 \pm 0.01$ $\mu$Jy/beam rms noise. Its J2000 center position $\alpha=04^h 13^m 26.4^s$, $\delta=-80^00' 00''$ 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 $-5 łesssim łogS(Jy) -4$.

@misc{mauch2019meerkat, 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 $-5 \lesssim \log[S(\mathrm{Jy})] \lesssim -4$.}, added-at = {2019-12-16T04:00:39.000+0100}, author = {Mauch, T. and Cotton, W. D. and Condon, J. J. and Matthews, A. M. and Abbott, T. D. and Adam, R. M. and Aldera, M. A. and Asad, K. M. B. and Bauermeister, E. F. and Bennett, T. G. H. and Bester, H. and Botha, D. H. and Brederode, L. R. S. and Brits, Z. B. and Buchner, S. J. and Burger, J. P. and Camilo, F. and Chalmers, J. M. and Cheetham, T. and de Villiers, D. and de Villiers, M. S. and Dikgale-Mahlakoana, M. A. and Toit, L. J. du and Esterhuyse, S. W. P. and Fadana, G. and Fanaroff, B. L. and Fataar, S. and February, S. and Frank, B. S. and Gamatham, R. R. G. and Geyer, M. and Goedhart, S. and Gounden, S. and Gumede, S. C. and Heywood, I. and Hlakola, M. J. and Horrell, J. M. G. and Hugo, B. and Isaacson, A. R. and Józsa, G. I. G. and Jonas, J. L. and Julie, R. P. M. and Kapp, F. B. and Kasper, V. A. and Kenyon, J. S. and Kotzé, P. P. A. and Kriek, N. and Kriel, H. and Kusel, T. W. and Lehmensiek, R. and Loots, A. and Lord, R. T. and Lunsky, B. M. and Madisa, K. and Magnus, L. G. and Main, J. P. L. and Malan, J. A. and Manley, J. R. and Marais, S. J. and Martens, A. and Merry, B. and Millenaar, R. and Mnyandu, N. and Moeng, I. P. T. and Mokone, O. J. and Monama, T. E. and Mphego, M. C. and New, W. S. and Ngcebetsha, B. and Ngoasheng, K. J. and Ockards, M. T. O. and Oozeer, N. and Otto, A. J. and Patel, A. A. and Peens-Hough, A. and Perkins, S. J. and Ramaila, A. J. T. and Ramudzuli, Z. R. and Renil, R. and Richter, L. L. and Robyntjies, A. and Salie, S. and Schollar, C. T. G. and Schwardt, L. C. and Serylak, M. and Siebrits, R. and Sirothia, S. K. and Smirnov, O. M. and Sofeya, L. and Stone, G. and Taljaard, B. and Tasse, C. and Theron, I. P. and Tiplady, A. J. and Toruvanda, O. and Twum, S. N. and van Balla, T. J. and van der Byl, A. and van der Merwe, C. and Van Tonder, V. and Wallace, B. H. and Welz, M. G. and Williams, L. P. and Xaia, B.}, biburl = {https://www.bibsonomy.org/bibtex/23513f7db7c3a8c231aefb2f15ae10592/gpkulkarni}, description = {The 1.28 GHz MeerKAT DEEP2 Image}, interhash = {c01c71fbdf1671c6fbe695f8a1cde8b1}, intrahash = {3513f7db7c3a8c231aefb2f15ae10592}, keywords = {library}, note = {cite arxiv:1912.06212Comment: 20 pages, 18 figures. Accepted for publication in ApJ}, timestamp = {2019-12-16T04:00:39.000+0100}, title = {The 1.28 GHz MeerKAT DEEP2 Image}, url = {http://arxiv.org/abs/1912.06212}, year = 2019 }