González-López, Jorge and Novak, Mladen and Decarli, Roberto and Walter, Fabian and Aravena, Manuel and Carilli, Chris and Boogaard, Leindert and Popping, Gergö and Weiss, Axel and Assef, Roberto J. and Bauer, Franz Erik and Bouwens, Rychard and Cortes, Paulo C. and Cox, Pierre and Daddi, Emanuele and Cunha, Elisabete da and Díaz-Santos, Tanio and Ivison, Rob and Magnelli, Benjamin and Riechers, Dominik and Smail, Ian and Werf, Paul van der and Wagg, Jeff (2020) 'The ALMA Spectroscopic Survey in the HUDF : deep 1.2 mm continuum number counts.', Astrophysical journal., 897 (1). p. 897.
We present the results from the 1.2 mm continuum image obtained as part of the Atacama Large Millimeter/ submillimeter Array Spectroscopic Survey in the Hubble Ultra Deep Field. The 1.2 mm continuum image has a size of 2.9 (4.2) arcmin2 within a primary beam response of 50% (10%) and an rms value of m - 9.3 Jy beam 1. We detect 35 sources at high significance (Fidelity 0.5); 32 have well-characterized near-infrared Hubble Space Telescope counterparts. We estimate the 1.2 mm number counts to flux levels of <30 Jy m in two different ways: we first use the detected sources to constrain the number counts and find a significant flattening of the counts below Sν ∼ 0.1 mJy. In a second approach, we constrain the number counts using a probability of deflection statistics (P(D)) analysis. For this latter approach, we describe new methods to accurately measure the noise in interferometric imaging (employing jackknifing in the cube and in the visibility plane). This independent measurement confirms the flattening of the number counts. Our analysis of the differential number counts shows that we are detecting ∼93% (∼100% if we include the lower fidelity detections) of the total continuum dust emission associated with galaxies in the Hubble Ultra Deep Field. The ancillary data allow us to study the dependence of the 1.2 mm number counts on redshift (z = 0−4), galaxy dust mass (M M dust = 10 10 – 7 9 ), stellar mass (M M = 10 10 – 9 12* ), and star formation rate ( = - M - SFR 1 1000 yr 1). In an accompanying paper we show that the number counts are crucial to constrain galaxy evolution models and the understanding of star-forming galaxies at high redshift.
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|Publisher Web site:||https://doi.org/10.3847/1538-4357/ab765b|
|Publisher statement:||© 2020. The American Astronomical Society. All rights reserved.|
|Date accepted:||11 February 2020|
|Date deposited:||29 July 2020|
|Date of first online publication:||06 July 2020|
|Date first made open access:||29 July 2020|
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