Carniani, S. and Maiolino, R. and De Zotti, G. and Negrello, M. and Marconi, A. and Bothwell, M. S. and Capak, P. and Carilli, C. and Castellano, M. and Cristiani, S. and Ferrara, A. and Fontana, A. and Gallerani, S. and Jones, G. and Ohta, K. and Ota, K. and Pentericci, L. and Santini, P. and Sheth, K. and Vallini, L. and Vanzella, E. and Wagg, J. and Williams, R. J. (2015) ALMA constraints on the faint millimetre source number counts and their contribution to the cosmic infrared background. Astronomy and Astrophysics, 584 . Art. No. A78. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20160115-165135620
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We have analysed 18 ALMA continuum maps in Bands 6 and 7, with rms down to 7.8 μJy, to derive differential number counts down to 60 μJy and 100 μJy at λ = 1.3 mm and λ = 1.1 mm, respectively. Furthermore, the non-detection of faint sources in the deepest ALMA field enabled us to set tight upper limits on the number counts down to 30 μJy. This is a factor of four deeper than the currently most stringent upper limit. The area covered by the combined fields is 9.5 × 10^(-4) deg^2 at 1.1 mm and 6.6 × 10^(-4) deg^2 at 1.3 mm. With respect to previous works, we improved the source extraction method by requiring that the dimension of the detected sources be consistent with the beam size. This method enabled us to remove spurious detections that have plagued the purity of the catalogues in previous studies. We detected 50 faint sources (at fluxes <1 mJy) with signal-to-noise (S/N) >3.5 down to 60 μJy, hence improving the statistics by a factor of four relative to previous studies. The inferred differential number counts are dN/ d(Log_(10)S) = 1 × 10^5 deg^2 at a 1.1 mm flux S_λ = 1.1 mm = 130 μJy, and dN/ d(Log_(10)S) = 1.1 × 10^5 deg^2 at a 1.3 mm flux S_λ = 1.3 mm = 60 μJy. At the faintest flux limits probed by our data, i.e. 30 μJy and 40 μJy, we obtain upper limits on the differential number counts of dN/ d(Log_(10)S) < 7 × 10^5 deg^2 and dN/ d(Log_(10)S) < 3 × 10^5 deg^2, respectively. Determining the fraction of cosmic infrared background (CIB) resolved by the ALMA observations was hampered by the large uncertainties plaguing the CIB measurements (a factor of four in flux). However, our results provide a new lower limit to CIB intensity of 17.2 Jy deg^(-2) at 1.1 mm and of 12.9 Jy deg^(-2) at 1.3 mm. Moreover, the flattening of the integrated number counts at faint fluxes strongly suggests that we are probably close to the CIB intensity. Our data imply that galaxies with star formation rate (SFR) < 40 M_⊙/yr certainly contribute less than 50% to the CIB (and probably a much lower percentage) while more than 50% of the CIB must be produced by galaxies with SFR> 40 M_⊙/yr. The differential number counts are in nice agreement with recent semi-analytical models of galaxy formation even as low as our faint fluxes. Consequently, this supports the galaxy evolutionary scenarios and assumptions made in these models.
|Additional Information:||© ESO, 2015. Received 1 February 2015 / Accepted 2 September 2015. We thank the anonymous referee for comments and suggestions that improved the paper. We thank Paola Andreani, Matthew Auger and Valentina Calvi for comments and discussions. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.1.00115.S, ADS/JAO.ALMA#2011.1.00243.S, ADS/JAO.ALMA#2011.1.00767.S, ADS/JAO.ALMA#2012.1.00142.S, ADS/JAO.ALMA#2012.1.00374.S, ADS/JAO.ALMA#2012.1.00523.S, ADS/JAO.ALMA#2012.1.00719.S and ADS/JAO.ALMA#2012.A.00040.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. G.D.Z. and M.N. acknowledge financial support from ASI/INAF Agreement 2014-024-R.0 for the Planck LFI activity of Phase E2.|
|Group:||Infrared Processing and Analysis Center (IPAC), COSMOS|
|Subject Keywords:||galaxies: evolution – galaxies: high-redshift – galaxies: formation|
|Official Citation:||ALMA constraints on the faint millimetre source number counts and their contribution to the cosmic infrared background S. Carniani, R. Maiolino, G. De Zotti, M. Negrello, A. Marconi, M. S. Bothwell, P. Capak, C. Carilli, M. Castellano, S. Cristiani, A. Ferrara, A. Fontana, S. Gallerani, G. Jones, K. Ohta, K. Ota, L. Pentericci, P. Santini, K. Sheth, L. Vallini, E. Vanzella, J. WaggS. Carniani, R. Maiolino, G. De Zotti, M. Negrello, A. Marconi, M. S. Bothwell, P. Capak, C. Carilli, M. Castellano, S. Cristiani, A. Ferrara, A. Fontana, S. Gallerani, G. Jones, K. Ohta, K. Ota, L. Pentericci, P. Santini, K. Sheth, L. Vallini, E. Vanzella, J. Wagg and R. J. Williams A&A, 584 (2015) A78 DOI: http://dx.doi.org/10.1051/0004-6361/201525780|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||George Porter|
|Deposited On:||19 Jan 2016 15:42|
|Last Modified:||19 Jan 2016 15:42|
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