SIMBAD references

2020ApJ...888...61M - Astrophys. J., 888, 61-61 (2020/January-2)

The 1.28 GHz MeerKAT DEEP2 image.

MAUCH T., COTTON W.D., CONDON J.J., MATTHEWS A.M., ABBOTT T.D., ADAM R.M., ALDERA M.A., ASAD K.M.B., BAUERMEISTER E.F., BENNETT T.G.H., BESTER H., BOTHA D.H., BREDERODE L.R.S., BRITS Z.B., BUCHNER S.J., BURGER J.P., CAMILO F., CHALMERS J.M., CHEETHAM T., DE VILLIERS D., DE VILLIERS M.S., DIKGALE-MAHLAKOANA M.A., DU TOIT L.J., ESTERHUYSE S.W.P., FADANA G., FANAROFF B.L., FATAAR S., FEBRUARY S., FRANK B.S., GAMATHAM R.R.G., GEYER M., GOEDHART S., GOUNDEN S., GUMEDE S.C., HEYWOOD I., HLAKOLA M.J., HORRELL J.M.G., HUGO B., ISAACSON A.R., JOZSA G.I.G., JONAS J.L., JULIE R.P.M., KAPP F.B., KASPER V.A., KENYON J.S., KOTZE P.P.A., KRIEK N., KRIEL H., KUSEL T.W., LEHMENSIEK R., LOOTS A., LORD R.T., LUNSKY B.M., MADISA K., MAGNUS L.G., MAIN J.P.L., MALAN J.A., MANLEY J.R., MARAIS S.J., MARTENS A., MERRY B., MILLENAAR R., MNYANDU N., MOENG I.P.T., MOKONE O.J., MONAMA T.E., MPHEGO M.C., NEW W.S., NGCEBETSHA B., NGOASHENG K.J., OCKARDS M.T.O., OOZEER N., OTTO A.J., PATEL A.A., PEENS-HOUGH A., PERKINS S.J., RAMAILA A.J.T., RAMUDZULI Z.R., RENIL R., RICHTER L.L., ROBYNTJIES A., SALIE S., SCHOLLAR C.T.G., SCHWARDT L.C., SERYLAK M., SIEBRITS R., SIROTHIA S.K., SMIRNOV O.M., SOFEYA L., STONE G., TALJAARD B., TASSE C., THERON I.P., TIPLADY A.J., TORUVANDA O., TWUM S.N., VAN BALLA T.J., VAN DER BYL A., VAN DER MERWE C., VAN TONDER V., WALLACE B.H., WELZ M.G., WILLIAMS L.P. and XAIA B.

Abstract (from CDS):

We present the confusion-limited 1.28 GHz MeerKAT DEEP2 image covering one θ_b~68^′ FWHM primary-beam area with θ = 7.''6 FWHM resolution and σ_n=0.55±0.01µJybeam^–1 rms noise. Its J2000 center position α = 04^h 13^m 26.s4, δ = -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 µJy with counts of individual DEEP2 sources between 10 µJy and 2.5 mJy. Most sources fainter than S ∼ 100 µJy are distant star-forming galaxies (SFGs) obeying the far-IR/radio correlation, and sources stronger than 0.25 µJy account for ∼93% of the radio background produced by SFGs. 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 model for the evolution of SFGs based on UV and infrared data underpredicts our 1.4 GHz source count in the range -5≲log[S(Jy)]≲-4.

Journal keyword(s): Radio telescopes - Galaxy counts - Star formation

Simbad objects: 2

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