ALMA constraints on the faint millimetre source number counts and their contribution to the cosmic infrared background

Carniani, Stefano; Maiolino, R.; Zotti, G. de; Negrello, M.; Marconi, A.; Bothwell, M. S.; Capak, P.; Carilli, Christopher L.; Castellano, M.; Cristiani, S.; Ferrara, Andrea; Fontana, A.; Gallerani, S.; Jones, G. C.; Ohta, Kouji; Ota, Kazuaki; Pentericci, L.; Santini, P.; Sheth, Kartik; Vallini, L.; Vanzella, E.; Wagg, Jeff; Williams, R. J.

doi:10.1051/0004-6361/201525780

Cited by 97 publications

(149 citation statements)

References 44 publications

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“…In Band 6 we re-observed the [Cii] emission in BDF − 3299 aiming at achieving the same sensitivity of previous observations obtained in Cycle 1 Carniani et al 2015), but with higher (×8) spatial resolution. ALMA Band-6 observations were carried out on 2015 June 30 and July 1 with a extended configuration (longest baseline = 1,570 m) and a precipitable water vapour of PWV = 0.8 mm.…”

Section: Observationsmentioning

confidence: 94%

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Carniani

Maiolino

Pallottini

et al. 2017

A&A

Self Cite

187

237

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We present new ALMA observations of the [Oiii]88µm line and high angular resolution observations of the [Cii]158µm line in a normal star forming galaxy at z=7.1. Previous [Cii] observations of this galaxy had detected [Cii] emission consistent with the Lyα redshift but spatially slightly offset relative to the optical (UV-rest frame) emission. The new [Cii] observations reveal that the [Cii] emission is partly clumpy and partly diffuse on scales larger than about 1kpc.[Oiii] emission is also detected at high significance, offset relative to the optical counterpart in the same direction as the [Cii] clumps, but mostly not overlapping with the bulk of the [Cii] emission. The offset between different emission components (optical/UV and different far-IR tracers) is similar to that which is observed in much more powerful starbursts at high redshift. We show that the [Oiii] emitting clump cannot be explained in terms of diffuse gas excited by the UV radiation emitted by the optical galaxy, but it requires excitation by in-situ (slightly dust obscured) star formation, at a rate of about 7 M yr −1 . Within 20 kpc from the optical galaxy the ALMA data reveal two additional [Oiii] emitting systems, which must be star forming companions. We discuss that the complex properties revealed by ALMA in the z∼7.1 galaxy are consistent with expectations by recent models and cosmological simulations, in which differential dust extinction, differential excitation and different metal enrichment levels, associated with different subsystems assembling a galaxy, are responsible for the various appearance of the system when observed with distinct tracers.

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Section: Observationsmentioning

confidence: 94%

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Carniani

Maiolino

Pallottini

et al. 2017

A&A

Self Cite

187

237

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“…The total flux density for this source is 0.150±0.014mJy, determined by fitting a pointsource model to the visibilities using the uvmodelfit task in CASA. Recent deep ALMA surveys have built up statistics on the number of faint background sources expected in a given field of view (Hatsukade et al 2013;Carniani et al 2015). Given these (sub)millimeter source counts, the number of sources with flux density of >0.15 mJy expected within our field of view is 2.6 1. the ALMA beam radius is ∼0 78 along R.A., it is likely that the ALMA source is the same background object as observed in optical data.…”

Section: Continuum Emissionmentioning

confidence: 99%

A Complete ALMA Map of the Fomalhaut Debris Disk

MacGregor

Matrà

Kalas

et al. 2017

ApJ

107

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We present ALMA mosaic observations at 1.3mm (223 GHz) of the Fomalhaut system with a sensitivity of 14μJy/beam. These observations provide the first millimeter map of the continuum dust emission from the complete outer debris disk with uniform sensitivity, enabling the first conclusive detection of apocenter glow. We adopt an MCMC modeling approach that accounts for the eccentric orbital parameters of a collection of particles within the disk. The outer belt is radially confined with an inner edge of 136.3±0.9au and width of 13.5±1.8au. We determine a best-fit eccentricity of 0.12±0.01. Assuming a size distribution power-law index of q=3.46±0.09, we constrain the dust absorptivity power-law index β to be 0.9<β<1.5. The geometry of the disk is robustly constrained with inclination 65°.6±0°. 3, position angle 337°.9±0°. 3, and argument of periastron 22°.5±4°.3. Our observations do not confirm any of the azimuthal features found in previous imaging studies of the disk with Hubble Space Telescope, SCUBA, and ALMA. However, we cannot rule out structures 10 au in size or that only affect smaller grains. The central star is clearly detected with a flux density of 0.75±0.02mJy, significantly lower than predicted by current photospheric models. We discuss the implications of these observations for the directly imaged Fomalhaut b and the inner dust belt detected at infrared wavelengths.

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“…In fact, Su et al (2015) suspected that the integrated submillimeter flux of the system is likely contaminated by background galaxies due to the excess emission detected at Herschel/SPIRE bands and APEX 870 µm compared to the disk SED model. Using the parameters of the Schechter function in Carniani et al (2015), the probability of a galaxy with an 1.3 mm flux of >0.81 mJy within 4 of the star is ∼0.5%, but increases to 5% and 14% chance within the FWHM and 10% of the primary beam, respectively. For the fainter source, the probability of having a source with an 1.3 mm flux of >0.1 mJy within 4 of the star is 11.4%.…”

Section: Alignment Of a Background Galaxymentioning

confidence: 99%

ALMA 1.3 mm Map of the HD 95086 System

Su¹,

MacGregor²,

Booth³

et al. 2017

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Planets and minor bodies such as asteroids, Kuiper-belt objects and comets are integral components of a planetary system. Interactions among them leave clues about the formation process of a planetary system. The signature of such interactions is most prominent through observations of its debris disk at millimeter wavelengths where emission is dominated by the population of large grains that stay close to their parent bodies. Here we present ALMA 1.3 mm observations of HD 95086, a young early-type star that hosts a directly imaged giant planet b and a massive debris disk with both asteroid-and Kuiper-belt analogs. The location of the Kuiper-belt analog is resolved for the first time. The system can be depicted as a broad (∆R/R ∼0.84), inclined (30• ±3• ) ring with millimeter emission peaked at 200±6 au from the star. The 1.3 mm disk emission is consistent with a broad disk with sharp boundaries from 106±6 to 320±20 au with a surface density distribution described by a power law with an index of -0.5±0.2. Our deep ALMA map also reveals a bright source located near the edge of the ring, whose brightness at 1.3 mm and potential spectral energy distribution are consistent with it being a luminous star-forming galaxy at high redshift. We set constraints on the orbital properties of planet b assuming co-planarity with the observed disk.

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ALMA constraints on the faint millimetre source number counts and their contribution to the cosmic infrared background

Cited by 97 publications

References 44 publications

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

A Complete ALMA Map of the Fomalhaut Debris Disk

ALMA 1.3 mm Map of the HD 95086 System

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