The ALMA Spectroscopic Survey in the HUDF: Deep 1.2 mm Continuum Number Counts

González-López, Jorge; Novak, Mladen; Decarli, Roberto; Walter, Fabian; Aravena, M.; Carilli, C. L.; Boogaard, Leindert; Popping, Gergö; Weiß, A.; Assef, Roberto J.; Bauer, F. E.; Bouwens, Rychard; Cortés, Paulo C.; Cox, P.; Daddi, Emanuele; Cunha, Elisabete da; Díaz-Santos, T.; Ivison, R. J.; Magnelli, B.; Riechers, Dominik A.; Smail, Ian; Werf, P. van der; Wagg, Jeff

doi:10.3847/1538-4357/ab765b

Cited by 82 publications

(143 citation statements)

References 89 publications

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“…For ALPS.1 and 3, our 1.3 mm continuum flux density measurements are consistent with the measurements of Dunlop et al (2017), whereas our value for ALPS.2 is (50±20)% larger. Conversely, the 1.3 mm flux density measured here for ALPS.1 is (55±20)% lower than the continuum flux density measured based on the ASPECS LP data in González-López et al (2020), whereas the flux density measured for ALPS.3 is consistent within the errors. The 1.3 mm flux density measured here for ALPS.2 is consistent with the value in González-López et al (2020).…”

Section: Deriving Dust and Gas Masses From The Alma Mapscontrasting

confidence: 53%

“…Conversely, the 1.3 mm flux density measured here for ALPS.1 is (55±20)% lower than the continuum flux density measured based on the ASPECS LP data in González-López et al (2020), whereas the flux density measured for ALPS.3 is consistent within the errors. The 1.3 mm flux density measured here for ALPS.2 is consistent with the value in González-López et al (2020). The difference between the flux densities measured by Dunlop et al (2017) and González-López et al (2020) can be mostly attributed to the different spectral setups, with the Dunlop et al (2017) covering longer wavelengths.…”

Section: Deriving Dust and Gas Masses From The Alma Mapscontrasting

confidence: 53%

“…We required the sources to be CO-bright in order to resolve their emission, at ∼0 5, within five hours of integration time, with ALMA, and select galaxies that are extended in the rest-frame optical to increase the chances of observing extended dust and CO emission. In Figure 1, we compare the properties of the three galaxies studied here to the parent sample of ASPECS LP 1.2 mm candidates (listed in Table 1 of González-López et al 2020) and the full set of galaxies in the HUDF (see Aravena et al 2020). Our ALPS sources have large stellar masses (   M 10 11 ) and high FIR luminosities compared with the majority of the sources in the field, because of our selection of CO-and 1 mm-bright targets.…”

Section: Galaxy Selectionmentioning

confidence: 99%

“…We analyze two Band 6 (211-275 GHz; 1.1-1.4 mm) surveys of the HUDF, taken at different depths and resolutions. We use the unresolved observations from the ASPECS LP (project code: 2016.1.00324, described in González-López et al 2020) and the 1.3 mm observations of Dunlop et al (2017) (project code: 2012.1.00173.S), which provide a higher spatial resolution. The source IDs from the ASPECS LP and HUDF data of Dunlop et al (2017) are provided in Table 1.…”

Section: Dust-continuum (Band 6) Observationsmentioning

confidence: 99%

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A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

Kaasinen

Walter

Novak

et al. 2020

ApJ

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We compare the extent of the dust, molecular gas, and stars in three star-forming galaxies, at z=1.4, 1.6, and 2.7, selected from the Hubble Ultra Deep Field based on their bright carbon monoxide (CO) and dust-continuum emission as well as their large rest-frame optical sizes. The galaxies have high stellar masses,  > M M 10 11 * , and reside on, or slightly below, the main sequence of star-forming galaxies at their respective redshifts. We probe the dust and molecular gas using subarcsecond Atacama Large Millimeter/submillimeter Array observations of the 1.3 mm continuum and CO line emission, respectively, and probe the stellar distribution using Hubble Space Telescope observations at 1.6 μm. We find that for all three galaxies the CO emission appears 30% more compact than the stellar emission. For the z=1.4 and 2.7 galaxies, the dust emission is also more compact, by 50%, than the stellar emission, whereas for the z=1.6 galaxy, the dust and stellar emission have similar spatial extents. This similar spatial extent is consistent with observations of local disk galaxies. However, most high-redshift observations show more compact dust emission, likely because of the ubiquity of central starbursts at high redshift and the limited sensitivity of many of these observations. Using the CO emission line, we also investigate the kinematics of the cold interstellar medium in the galaxies, and find that all three have kinematics consistent with a rotation-dominated disk.

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Section: Deriving Dust and Gas Masses From The Alma Mapscontrasting

confidence: 53%

Section: Deriving Dust and Gas Masses From The Alma Mapscontrasting

confidence: 53%

Section: Galaxy Selectionmentioning

confidence: 99%

Section: Dust-continuum (Band 6) Observationsmentioning

confidence: 99%

See 2 more Smart Citations

A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

Kaasinen

Walter

Novak

et al. 2020

ApJ

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“…The coverage of ASPECS (Band 3 and Band 6) provides simultaneous constraints on multiple lines from CO, [ ] C I for most sources, depending on the redshift (as well as any other species in the frequency range). Furthermore, the multiple tunings scanning through the entire ALMA frequency bands give a high continuum sensitivity, providing a deep (9.3 μJy beam −1 , Section 2.1), contiguous continuum map at 1.2 mm in the Hubble Ultra Deep Field (HUDF; Aravena et al 2020;González-López et al 2020). Using earlier data from the ASPECS-Pilot program on a smaller area of the sky, Decarli et al (2016b) studied a sample of seven galaxies at z=1-3 (a subset of the sources studied in this paper), finding that the CO excitation conditions were overall lower than those typically found in starbursts, SMGs, and QSO environments. This paper studies the CO excitation, atomic carbon emission and ISM conditions in a flux-limited sample of 22 CO and/or dust-continuum detected galaxies at z=1-3 from the ASPECS Large Program (LP), supplemented by follow-up CO(1-0) observations from VLASPECS (Riechers et al 2020).…”

Section: Introductionmentioning

confidence: 99%

The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: CO Excitation and Atomic Carbon in Star-forming Galaxies at z = 1–3

Boogaard

Werf

Weiß

et al. 2020

ApJ

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114

153

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We investigate the CO excitation and interstellar medium (ISM) conditions in a cold gas mass-selected sample of 22 star-forming galaxies at z=0.46-3.60, observed as part of the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field (ASPECS). Combined with Very Large Array follow-up observations, we detect a total of 34 CO -J J 1 transitions with J=1 up to 8 (and an additional 21 upper limits, up to J=10) and 6 [ ] C I  P P 10 5 , comparable to the Milky Way and main-sequence galaxies at similar redshifts, and fairly high densities (10 4 cm −3), consistent with the low-J CO excitation. Our results imply a decrease in the cosmic molecular gas mass density at z2 compared to previous ASPECS measurements.

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GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxies

Franco

Elbaz

Zhou

et al. 2020

A&A

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In this paper, we extend the source detection in the GOODS-ALMA field (69 arcmin2, 1σ ≃ 0.18 mJy beam−1) to deeper levels than presented in our previous work. Using positional information at 3.6 and 4.5 μm (from Spitzer-IRAC) as well as the Very Large Array (VLA) at 3 GHz, we explore the presence of galaxies detected at 1.1 mm with ALMA below our original blind detection limit of 4.8-σ, at which the number of spurious sources starts to dominate over that of real sources. In order to ensure the most reliable counterpart association possible, we have investigated the astrometry differences between different instruments in the GOODS–South field. In addition to a global offset between the Atacama Large Millimeter/submillimeter Array (ALMA) and the Hubble Space Telescope (HST) already discussed in previous studies, we have highlighted a local offset between ALMA and the HST that was artificially introduced in the process of building the mosaic of the GOODS–South image. We created a distortion map that can be used to correct for these astrometric issues. In this Supplementary Catalog, we find a total of 16 galaxies, including two galaxies with no counterpart in HST images (also known as optically dark galaxies), down to a 5σ limiting depth of H = 28.2 AB (HST/WFC3 F160W). This brings the total sample of GOODS-ALMA 1.1 mm sources to 35 galaxies. Galaxies in the new sample cover a wider dynamic range in redshift (z = 0.65−4.73), are on average twice as large (1.3 vs 0.65 kpc), and have lower stellar masses (M⋆SC = 7.6 × 1010 M⊙ vs M⋆MC = 1.2 × 1011 M⊙). Although exhibiting larger physical sizes, these galaxies still have far-infrared sizes that are significantly more compact than inferred from their optical emission.

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The ALMA Spectroscopic Survey in the HUDF: Deep 1.2 mm Continuum Number Counts

Cited by 82 publications

References 89 publications

A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: CO Excitation and Atomic Carbon in Star-forming Galaxies at z = 1–3

GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxies

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