2020ApJ...888...61M

Query : 2020ApJ...888...61M

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 θb~68′ FWHM primary-beam area with θ = 7.''6 FWHM resolution and σn=0.55±0.01µJybeam–1 rms noise. Its J2000 center position α = 04h 13m 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.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

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

Simbad objects: 2

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Number of rows : 2
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 PKS 0252-712 rG 02 52 46.15578 -71 04 35.2742   19.0 19.0     ~ 104 1
2 ICRF J193925.0-634245 Sy2 19 39 25.0245304992 -63 42 45.640373400   18.87 18.37 17.64   ~ 1332 2

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