SXDF–ALMA 2-arcmin2 deep survey: 1.1-mm number counts

Hatsukade, Bunyo; Kohno, Kotaro; Umehata, Hideki; Aretxaga, I.; Caputi, K.; Dunlop, James; Ikarashi, Soh; Iono, Daisuke; Ivison, R. J.; Lee, Minju; Makiya, Ryu; Matsuda, Yoshihisa; Motohara, Kentaro; Nakanishi, Koichiro; Ohta, Kouji; Tadaki, K.; Tamura, Motohide; Wang, Wei-Hao; Wilson, Grant; Yamaguchi, Yuki; Yun, Min S.

doi:10.1093/pasj/psw026

Cited by 60 publications

(51 citation statements)

References 39 publications

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“…We also show the counts using seven SMGs that do not have z spec =3.09. Previous ALMA results (Karim et al 2013;Ono et al 2014;Simpson et al 2015a;Fujimoto et al 2016;Hatsukade et al 2016;Oteo et al 2016) are also shown. The flux density of the counts are scaled to 1.1mm flux density, assuming a modified black body (similar with Figure 9; S 1.1mm /S 870μm = 0.56, S 1.1mm /S 1.2mm =1.29, S 1.1mm /S 1.3mm =1.48).…”

Section: Size Measurement and Star Formation Rate Surface Densitymentioning

confidence: 58%

“…We briefly describe the method below (for more detail, see Hatsukade et al 2016). Model sources created by scaling the synthesized beam are injected into the image map corrected for primary beam attenuation.…”

Section: Completeness and Flux Boostingmentioning

confidence: 99%

“…The advent of the Atacama Large Millimeter/submillimeter Array (ALMA) allows us to break through these limitations. Contiguous ALMA mosaic imaging is able to open a window for submm/ mm deep surveys with sub-arcsec resolution (e.g., Tadaki et al 2015;Aravena et al 2016;Dunlop et al 2016;Hatsukade et al 2016;Walter et al 2016). 15 We utilized ALMA to conduct a deep imaging survey toward a well-studied protocluster at z = 3.09 in the SSA22 field.…”

Section: Introductionmentioning

confidence: 99%

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ALMA Deep Field in SSA22: Source Catalog and Number Counts

Umehata

Tamura

Kohno

et al. 2017

ApJ

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110

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We present results from a deep 2′×3′ (comoving scale of 3.7 Mpc×5.5 Mpc at z = 3) survey at 1.1mm, taken with the Atacama Large Millimeter/submillimeter Array (ALMA) in the SSA22 field. We observe the core region of a z = 3.09 protocluster, achieving a typical rms sensitivity of 60 μJy beam −1 at a spatial resolution of 0 7. We detect 18 robust ALMA sources at a signal-to-noise ratio (S/N)>5. Comparison between the ALMA map and a 1.1mm map, taken with the AzTEC camera on the Atacama Submillimeter Telescope Experiment (ASTE), indicates that three submillimeter sources discovered by the AzTEC/ASTE survey are resolved into eight individual submillimeter galaxies (SMGs) by ALMA. At least 10 of our 18 ALMA SMGs have spectroscopic redshifts of z;3.09, placing them in the protocluster. This shows that a number of dusty starburst galaxies are forming simultaneously in the core of the protocluster. The nine brightest ALMA SMGs with S/N>10 have a median intrinsic angular size of  -+ 0. 32 0.06 0.13 ( -+ 2.4 0.4 1.0 physical kpc at z = 3.09), which is consistent with previous size measurements of SMGs in other fields. As expected, the source counts show a possible excess compared to the counts in the general fields at S 1.1mm 1.0 mJy, due to the protocluster. Our contiguous mm mapping highlights the importance of large-scale structures on the formation of dusty starburst galaxies.

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Section: Size Measurement and Star Formation Rate Surface Densitymentioning

confidence: 58%

Section: Completeness and Flux Boostingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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ALMA Deep Field in SSA22: Source Catalog and Number Counts

Umehata

Tamura

Kohno

et al. 2017

ApJ

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110

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“…Its significantly higher angular resolution compared to single-dish telescopes (<  3 ) and the unparalleled sensitivity allow us to reach flux density levels in (sub)millimeter continuum maps even deeper than those achieved by studies of galaxy cluster fields or based on stacking analysis. Several recent studies have individually pinpointed (sub)millimeter sources down to 0.1 mJy in the 1 mm band (Hatsukade et al 2013;Ono et al 2014;Carniani et al 2015;Oteo et al 2016;Dunlop et al 2016;Hatsukade et al 2016). Some of these surveys have used clever approaches by taking advantage of archival data (Ono et al 2014;Carniani et al 2015;Fujimoto et al 2016), including ALMA calibration fields (Oteo et al 2016).…”

Section: Introductionmentioning

confidence: 99%

THE ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: CONTINUUM NUMBER COUNTS, RESOLVED 1.2 mm EXTRAGALACTIC BACKGROUND, AND PROPERTIES OF THE FAINTEST DUSTY STAR-FORMING GALAXIES

Aravena

Decarli

Walter

et al. 2016

ApJ

128

117

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We present an analysis of a deep (1σ=13 μJy) cosmological 1.2 mm continuum map based on ASPECS, the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field. In the 1 arcmin 2 covered by ASPECS we detect nine sources at s >3.5 significance at 1.2 mm. Our ALMA-selected sample has a median redshift of =  z 1.6 0.4, with only one galaxy detected at z>2 within the survey area. This value is significantly lower than that found in millimeter samples selected at a higher flux density cutoff and similar frequencies. Most galaxies have specific star formation rates (SFRs) similar to that of main-sequence galaxies at the same epoch, and we find median values of stellar mass and SFRs of , respectively. Using the dust emission as a tracer for the interstellar medium (ISM) mass, we derive depletion times that are typically longer than 300 Myr, and we find molecular gas fractions ranging from ∼0.1 to 1.0. As noted by previous studies, these values are lower than those using CO-based ISM estimates by a factor of ∼2. The 1 mm number counts (corrected for fidelity and completeness) are in agreement with previous studies that were typically restricted to brighter sources. With our individual detections only, we recover 55%±4% of the extragalactic background light (EBL) at 1.2 mm measured by the Planck satellite, and we recover 80% ±7% of this EBL if we include the bright end of the number counts and additional detections from stacking. The stacked contribution is dominated by galaxies at -z 1 2, with stellar masses of (1-3)×10 10 M  . For the first time, we are able to characterize the population of galaxies that dominate the EBL at 1.2 mm.

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“…The number density of the brightest SMGs with apparent submm flux in excess of 10 mJy at 850µm is ∼ 5 deg −2 (Hatsukade et al 2016), and the intrinsic Star Formation Rate (SFR) can exceed 1000 M ⊙ yr −1 if the submillimeter flux arises entirely from star formation. Although they are rare, these SMGs host the most intense starbursts in the entire universe and may represent the formation sites of massive elliptical galaxies.…”

Section: Introductionmentioning

confidence: 99%

Clumpy and Extended Starbursts in the Brightest Unlensed Submillimeter Galaxies

Iono

Yun

Aretxaga

et al. 2016

ApJL

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The central structure in three of the brightest unlensed z = 3 − 4 submillimeter galaxies are investigated through 0.′′ 015 -0. ′′ 05 (120 -360 pc) 860µm continuum images obtained using the Atacama Large Millimeter/submillimeter Array (ALMA). The distribution in the central kpc in AzTEC1 and AzTEC8 are extremely complex, and they are composed of multiple ∼ 200 pc clumps. AzTEC4 consists of two sources that are separated by ∼ 1.5 kpc, indicating a mid-stage merger. The peak star formation rate densities in the central clumps are ∼ 300 − 3000 M ⊙ yr −1 kpc −2 , suggesting regions with extreme star formation near the Eddington Limit. By comparing the flux obtained by ALMA and Submillimeter Array (SMA), we find that 68−90% of the emission is extended ( 1 kpc) in AzTEC 4 and 8. For AzTEC1, we identify at least 11 additional compact (∼ 200 pc) clumps in the extended 3 -4 kpc region. Overall, the data presented here suggest that the luminosity surface densities observed at 150 pc scales are roughly similar to that observed in local ULIRGs, as in the eastern nucleus of Arp 220. Between 10 to 30% of the 860µm continuum is concentrated in clumpy structures in the central kpc while the remaining flux is distributed over 1 kpc regions, some of which could also be clumpy. These sources can be explained by a rapid inflow of gas such as a merger of gas-rich galaxies, surrounded by extended and clumpy starbursts. However, the cold mode accretion model is not ruled out.

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SXDF–ALMA 2-arcmin2 deep survey: 1.1-mm number counts

Cited by 60 publications

References 39 publications

ALMA Deep Field in SSA22: Source Catalog and Number Counts

ALMA Deep Field in SSA22: Source Catalog and Number Counts

THE ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: CONTINUUM NUMBER COUNTS, RESOLVED 1.2 mm EXTRAGALACTIC BACKGROUND, AND PROPERTIES OF THE FAINTEST DUSTY STAR-FORMING GALAXIES

Clumpy and Extended Starbursts in the Brightest Unlensed Submillimeter Galaxies

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