The ALMA Frontier Fields Survey

Laporte, Nicolas; Bauer, F. E.; Troncoso-Iribarren, P.; Huang, Xu; González-López, Jorge; Kim, S.; Anguita, T.; Aravena, M.; Barrientos, L. Felipe; Bouwens, Rychard; Bradley, Larry; Brammer, Gabriel; Carrasco, Mauricio; Carvajal, R.; Coe, Dan; Demarco, R.; Ellis, Richard S.; Ford, H. C.; Francke, Harold; Ibar, E.; Infante, L.; Kneißl, R.; Koekemoer, Anton M.; Messias, H.; Muñoz-Arancibia, A.; Nagar, Neil M.; Padilla, Nelson; Pelló, R.; Postman, Marc; Quénard, D.; Romero-Cañizales, C.; Treister, Ezequiel; Villard, Eric; Zheng, Wei; Zitrin, Adi

doi:10.1051/0004-6361/201730628

Cited by 30 publications

(33 citation statements)

References 73 publications

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“…4.5). For example, of the 12 galaxies presented by Laporte et al (2017), with fluxes measured using ALMA at 1.1 mm (González-López et al 2017), seven of them have a size measured by HST F140W/WFC3 similar to the size measured in the ALMA map. On the other hand, for the remaining five galaxies, their sizes are approximately two times more compact 0.6 0.8 1.0 1.2 1.4 1.6…”

Section: Completenessmentioning

confidence: 96%

GOODS-ALMA: 1.1 mm galaxy survey

Franco

Elbaz

Béthermin

et al. 2018

A&A

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219

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Aims. We present a 69 arcmin2 ALMA survey at 1.1 mm, GOODS-ALMA, matching the deepest HST-WFC3 H-band part of the GOODS-South field. Methods. We tapered the 0″24 original image with a homogeneous and circular synthesized beam of 0″60 to reduce the number of independent beams – thus reducing the number of purely statistical spurious detections – and optimize the sensitivity to point sources. We extracted a catalog of galaxies purely selected by ALMA and identified sources with and without HST counterparts down to a 5σ limiting depth of H = 28.2 AB (HST/WFC3 F160W). Results. ALMA detects 20 sources brighter than 0.7 mJy at 1.1 mm in the 0″60 tapered mosaic (rms sensitivity σ ≃ 0.18 mJy beam−1) with a purity greater than 80%. Among these detections, we identify three sources with no HST nor Spitzer-IRAC counterpart, consistent with the expected number of spurious galaxies from the analysis of the inverted image; their definitive status will require additional investigation. We detect additional three sources with HST counterparts either at high significance in the higher resolution map, or with different detection-algorithm parameters ensuring a purity greater than 80%. Hence we identify in total 20 robust detections. Conclusions. Our wide contiguous survey allows us to push further in redshift the blind detection of massive galaxies with ALMA with a median redshift of z = 2.92 and a median stellar mass of M⋆ = 1.1 × 1011 M⊙. Our sample includes 20% HST-dark galaxies (4 out of 20), all detected in the mid-infrared with Spitzer-IRAC. The near-infrared based photometric redshifts of two of them (z ∼ 4.3 and 4.8) suggest that these sources have redshifts z > 4. At least 40% of the ALMA sources host an X-ray AGN, compared to ∼14% for other galaxies of similar mass and redshift. The wide area of our ALMA survey provides lower values at the bright end of number counts than single-dish telescopes affected by confusion.

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Section: Completenessmentioning

confidence: 96%

GOODS-ALMA: 1.1 mm galaxy survey

Franco

Elbaz

Béthermin

et al. 2018

A&A

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219

295

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“…We also compare our measurements of the extended component with the median value of a sample of faint field galaxies in strongly lensed cluster in the Hubble Frontier Fields Survey (González-López et al 2017;Laporte et al 2017). These galaxies at z 1.0-2.9 are detected with Figure 8.…”

Section: What Is the Extended Dust Component?mentioning

confidence: 99%

An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: high-resolution dust continuum morphologies and the link between sub-millimetre galaxies and spheroid formation

Gullberg

Smail

Swinbank

et al. 2019

Monthly Notices of the Royal Astronomical Society

114

171

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We present an analysis of the morphology and profiles of the dust continuum emission in 153 bright sub-millimetre galaxies (SMGs) detected with ALMA at signal to noise ratios of > 8 in high-resolution 0. 18 (∼ 1 kpc) 870 µm maps. We measure sizes, shapes and light profiles for the rest-frame far-infrared emission from these luminous starforming systems and derive a median effective radius (R e ) of 0. 10 ± 0. 04 for our sample with a median flux of S 870 = 5.6 ± 0.2 mJy. We find that the apparent axial ratio (b/a) distribution of the SMGs peaks at b/a ∼ 0.63 ± 0.02 and is best described by triaxial morphologies, while their emission profiles are best fit by a Sérsic model with n 1.0 ± 0.1, similar to exponential discs. This combination of triaxiality and n ∼ 1 Sérsic index are characteristic of bars and we suggest that the bulk of the 870 µm dust continuum emission in the central ∼ 2 kpc of these galaxies arises from bar-like structures. As such we caution against using the orientation of shape of the bright dust continuum emission at resolution to assess either the orientation of any disc on the sky or tits inclination. By stacking our 870 µm maps we recover faint extended dust continuum emission on ∼ 4 kpc scales which contributes 13 ± 1% of the total 870 µm emission. The scale of this extended emission is similar to that seen for the molecular gas and rest-frame optical light in these systems, suggesting that it represents an extended dust and gas disc at radii larger than the more active bar component. Including this component in our estimated size of the sources we derive a typical effective radius of 0. 15 ± 0. 05 or 1.2 ± 0.4 kpc. Our results suggest that kpc-scale bars are ubiquitous features of high star-formation rate systems at z 1, while these systems also contain fainter and more extended gas and stellar envelopes. We suggest that these features, seen some 10-12 Gyrs ago, represent the formation phase of the earliest galactic-scale components: stellar bulges.

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“…Since we have accurate positions and deep HST imaging, we thus consider available spectroscopic and photometric redshift information. Laporte et al (2017; hereafter Paper II) determine photometric redshifts for all our S /N > 5 detections via SED fitting, finding a mean redshift of z = 1.99 ± 0.27. Five of these high-significance sources (A2744-ID01, A2744-ID02, MACS J0416-ID01, MACS J0416-ID02, and MACS J1149-ID03) have spectroscopic redshifts from the GLASS survey (Treu et al 2015), which are consistent with the photometric redshifts found.…”

Section: Source Redshiftsmentioning

confidence: 99%

The ALMA Frontier Fields Survey

Muñoz-Arancibia

González-López

Ibar

et al. 2018

A&A

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Context. Characterizing the number counts of faint (i.e., sub-mJy and especially sub-100 μJy), dusty star-forming galaxies is currently a challenge even for deep, high-resolution observations in the FIR-to-mm regime. They are predicted to account for approximately half of the total extragalactic background light at those wavelengths. Searching for dusty star-forming galaxies behind massive galaxy clusters benefits from strong lensing, enhancing their measured emission while increasing spatial resolution. Derived number counts depend, however, on mass reconstruction models that properly constrain these clusters. Aims. We aim to estimate the 1.1 mm number counts along the line of sight of three galaxy clusters, Abell 2744, MACS J0416.1–2403, and MACS J1149.5+2223, which are part of the ALMA Frontier Fields Survey. We have performed detailed simulations to correct these counts for lensing effects, probing down to the sub-mJy flux density level. Methods. We created a source catalog based on ALMA 1.1 mm continuum detections. We used several publicly available lensing models for the galaxy clusters to derive the intrinsic flux densities of these sources. We performed Monte Carlo simulations of the number counts for a detailed treatment of the uncertainties in the magnifications and adopted source redshifts. Results. We estimate lensing-corrected number counts at 1.1 mm using source detections down to S/N = 4.5. In each cluster field, we find an overall agreement among the number counts derived for the different lens models, despite their systematic variations regarding source magnifications and effective areas. Combining all cluster fields, our number counts span ∼2.5 dex in demagnified flux density, from several mJy down to tens of μJy. Both our differential and cumulative number counts are consistent with recent estimates from deep ALMA observations at a 3σ level. Below ≈0.1 mJy, however, our cumulative counts are lower by ≈1 dex, suggesting a flattening in the number counts. Conclusions. We derive 1.1 mm number counts around three well-studied galaxy clusters following a statistical approach. In our deepest ALMA mosaic, we estimate number counts for intrinsic flux densities ≈4 times fainter than the rms level. This highlights the potential of probing the sub-10 μJy population in larger samples of galaxy cluster fields with deeper ALMA observations.

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The ALMA Frontier Fields Survey

Cited by 30 publications

References 73 publications

GOODS-ALMA: 1.1 mm galaxy survey

GOODS-ALMA: 1.1 mm galaxy survey

An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: high-resolution dust continuum morphologies and the link between sub-millimetre galaxies and spheroid formation

The ALMA Frontier Fields Survey

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