ALMACAL VII: first interferometric number counts at 650 μm

Klitsch, Anne; Smail, Ian; Péroux, Céline; Biggs, A. D.; Chen, Chian-Chou; Ivison, R. J.; Popping, Gergö; Lagos, Claudia del P.; Béthermin, M.; Swinbank, A. M.; Hamanowicz, A.; Dutta, Rajeshwari

doi:10.1093/mnras/staa1315

Cited by 4 publications

(10 citation statements)

References 84 publications

(96 reference statements)

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“…We detected residual signals from the calibrator in some fields, so we masked the central part of each map to a radius of 2 arcsec. This radius is 2× larger than the masking used in band 8 (Klitsch et al 2020) but the loss is small for the larger fields of view (FoV) at the longer wavelengths explored here. To improve the reliability of the source detection in ALMACAL, we applied the source-finding algorithm in the two tapered images simultaneously.…”

Section: Source Detectionmentioning

confidence: 86%

“…Following our two earlier number counts papers, Oteo et al (2016) and Klitsch et al (2020), we performed the source detection using sextractor as it can deal easily with complex source structures (Bertin & Arnouts 1996). The search for detections is made in the images before primary beam correction, corresponding to a signalto-noise image.…”

Section: Source Detectionmentioning

confidence: 99%

“…By comparison, ALMACAL offers a good balance between sensitivity and effective area, and will continue to be an essential complement to blind surveys. Klitsch et al (2020) estimated the cosmic variance of band 8 footprints from ALMACAL following the methodology described in Driver & Robotham (2010). They found the cosmic variance is less than 5 per cent level in ALMACAL band 8 observations.…”

Section: Effective Areamentioning

confidence: 99%

“…Since then, both the number of calibrators and their on-source integration times have grown by more than an order of magnitude. Using the new data, Klitsch et al (2020) reported the first number counts in ALMA band 8, at 650 µm. Besides number counts, searches for molecular absorption or emission lines have put constrains on the evolution of molecular gas density over cosmic time (Klitsch et al 2019;Hamanowicz et al 2022, submitted).…”

mentioning

confidence: 99%

“…Besides number counts, searches for molecular absorption or emission lines have put constrains on the evolution of molecular gas density over cosmic time (Klitsch et al 2019;Hamanowicz et al 2022, submitted). In this work, we extend the number counts of Oteo et al (2016) and Klitsch et al (2020) to the most up-to-date ALMACAL dataset, covering ALMA bands 3, 4, 5, 6 and 7, at wavelengths from 3 mm down to 870 µm, respectively.…”

mentioning

confidence: 99%

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ALMACAL IX: Multiband ALMA survey for dusty star-forming galaxies and the resolved fractions of the cosmic infrared background

Chen

Ivison

Smail

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Wide, deep, blind continuum surveys at submillimetre/millimetre (submm/mm) wavelengths are required to provide a full inventory of the dusty, distant Universe. However, conducting such surveys to the necessary depth, with sub-arcsec angular resolution, is prohibitively time-consuming, even for the most advanced submm/mm telescopes. Here, we report the most recent results from the ALMACAL project, which exploits the ‘free’ calibration data from the Atacama Large Millimetre/submillimetre Array (ALMA) to map the lines of sight towards and beyond the ALMA calibrators. ALMACAL has now covered 1,001 calibrators, with a total sky coverage around 0.3 deg2, distributed across the sky accessible from the Atacama desert, and has accumulated more than 1,000 h of integration. The depth reached by combining multiple visits to each field makes ALMACAL capable of searching for faint, dusty, star-forming galaxies (DSFGs), with detections at multiple frequencies to constrain the emission mechanism. Based on the most up-to-date ALMACAL database, we report the detection of 186 DSFGs with flux densities down to S870μm ∼ 0.2 mJy, comparable with existing ALMA large surveys but less susceptible to cosmic variance. We report the number counts at five wavelengths between 870 μm and 3 mm, in ALMA bands 3, 4, 5, 6 and 7, providing a benchmark for models of galaxy formation and evolution. By integrating the observed number counts and the best-fitting functions, we also present the resolved fraction of the cosmic infrared background (CIB) and the CIB spectral shape. Combining existing surveys, ALMA has currently resolved about half of the CIB in the submm/mm regime.

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Section: Source Detectionmentioning

confidence: 86%

Section: Source Detectionmentioning

confidence: 99%

Section: Effective Areamentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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ALMACAL IX: Multiband ALMA survey for dusty star-forming galaxies and the resolved fractions of the cosmic infrared background

Chen

Ivison

Smail

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Licking the plate: Dusty star-forming galaxies buried in the ALMA calibration data

Chen,

Ivison,

Zwaan

et al. 2024

EPJ Web Conf.

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Deep, unbiased surveys are essential to decipher the cosmic evolution of galaxies. The submillimetre (submm) and millimetre (mm) windows complement the UV/optical waveband and are key to revealing the cold and dusty Universe. Traditional ways of conducting deep surveys resort to either lensed fields or target small areas for ultra-long integrations. These surveys have greatly advanced our understanding of dusty star-forming galaxies (DSFGs), but are susceptible to lensing uncertainties and cosmic variance and will be expensive to expand. Here, we summarise our recent multi-wavelength survey of DSFGs in the vicinity of ALMA’s calibrators: the ALMACAL survey. These fields have accumulated many hundreds of hours of on-source time, reaching depths and effective areas that are competitive with bespoke cosmological surveys. We summarise the multi-wavelength number counts from ALMACAL and the resolved fraction of the Cosmic Infrared Background (CIB) from submm to mm wave-lengths. Meanwhile, combining all available ALMA observations in each field results in impressive frequency coverage, which often yields the redshifts of these DSFGs. The ALMACAL survey has demonstrated the scientific value of calibration scans for all submm/mm and radio telescopes, existing and planned.

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Physical properties and evolution of (sub-)millimetre-selected galaxies in the galaxy formation simulation shark

Lagos

Cunha

Robotham

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We thoroughly explore the properties of (sub)-millimeter (mm) selected galaxies (SMGs) in the Shark semi-analytic model of galaxy formation. Compared to observations, the predicted number counts at wavelengths (λ) 0.6 − 2mm and redshift distributions at 0.1 − 2mm, agree well. At the bright end (≳ 1 mJy), Shark galaxies are a mix of mergers and disk instabilities. These galaxies display a stacked FUV-to-FIR spectrum that agrees well with observations. We predict that current optical/NIR surveys are deep enough to detect bright (>1 mJy) λ = 0.85 − 2mm-selected galaxies at z ≲ 5, but too shallow to detect counterparts at higher redshift. A James Webb Space Telescope 10,000s survey should detect all counterparts for galaxies with S0.85mm ≳ 0.01 mJy. We predict SMG’s disks contribute significantly (negligibly) to the rest-frame UV (IR). We investigate the 0 ≤ z ≤ 6 evolution of the intrinsic properties of >1 mJy λ = 0.85 − 2mm-selected galaxies finding their: (i) stellar masses are $>10^{10.2}\rm \, M_{\odot }$, with the 2mm ones tracing the most massive galaxies ($>10^{11}\rm \, M_{\odot }$); (ii) specific star formation rates (SFR) are mildly (≈3 − 10 ×) above the main sequence (MS); (iii) host halo masses are $\gtrsim 10^{12.3}\, \rm M_{\odot }$, with 2mm galaxies tracing the most massive halos (proto-clusters); (iv) SMGs have lower dust masses ($\approx 10^{8}\, \rm M_{\odot }$), higher dust temperatures (≈40 − 45 K) and higher rest-frame V-band attenuation (>1.5) than MS galaxies; (v) sizes decrease with redshift, from 4 kpc at z = 1 to ≲ 1 kpc at z = 4; (vi) the Carbon Monoxide line spectra of S0.85mm ≳ 1 mJy sources peak at 4 → 3. Finally, we study the contribution of SMGs to the molecular gas and cosmic SFR density at 0 ≤ z ≤ 10, finding that >1 mJy sources make a negligible contribution at z ≳ 3 and z ≳ 5, respectively, suggesting current observations have unveiled the majority of the star formation at 0 ≤ z ≤ 10.

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ALMACAL VII: first interferometric number counts at 650 μm

Cited by 4 publications

References 84 publications

ALMACAL IX: Multiband ALMA survey for dusty star-forming galaxies and the resolved fractions of the cosmic infrared background

ALMACAL IX: Multiband ALMA survey for dusty star-forming galaxies and the resolved fractions of the cosmic infrared background

Licking the plate: Dusty star-forming galaxies buried in the ALMA calibration data

Physical properties and evolution of (sub-)millimetre-selected galaxies in the galaxy formation simulation shark

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