ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
We present a statistical study of 180 dust continuum sources identified in 33 massive cluster fields by the Atacama Large Millimeter/submillimeter Array Lensing Cluster Survey (ALCS) over a total of 133 arcmin ^2 area, homogeneously observed at 1.2 mm. ALCS enables us to detect extremely faint milli...
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2024-01-01
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| author | Seiji Fujimoto Kotaro Kohno Masami Ouchi Masamune Oguri Vasily Kokorev Gabriel Brammer Fengwu Sun Jorge González-López Franz E. Bauer Gabriel B. Caminha Bunyo Hatsukade Johan Richard Ian Smail Akiyoshi Tsujita Yoshihiro Ueda Ryosuke Uematsu Adi Zitrin Dan Coe Jean-Paul Kneib Marc Postman Keiichi Umetsu Claudia del P. Lagos Gergö Popping Yiping Ao Larry Bradley Karina Caputi Miroslava Dessauges-Zavadsky Eiichi Egami Daniel Espada R. J. Ivison Mathilde Jauzac Kirsten K. Knudsen Anton M. Koekemoer Georgios E. Magdis Guillaume Mahler A. M. Muñoz Arancibia Timothy Rawle Kazuhiro Shimasaku Sune Toft Hideki Umehata Francesco Valentino Tao Wang Wei-Hao Wang |
| author_facet | Seiji Fujimoto Kotaro Kohno Masami Ouchi Masamune Oguri Vasily Kokorev Gabriel Brammer Fengwu Sun Jorge González-López Franz E. Bauer Gabriel B. Caminha Bunyo Hatsukade Johan Richard Ian Smail Akiyoshi Tsujita Yoshihiro Ueda Ryosuke Uematsu Adi Zitrin Dan Coe Jean-Paul Kneib Marc Postman Keiichi Umetsu Claudia del P. Lagos Gergö Popping Yiping Ao Larry Bradley Karina Caputi Miroslava Dessauges-Zavadsky Eiichi Egami Daniel Espada R. J. Ivison Mathilde Jauzac Kirsten K. Knudsen Anton M. Koekemoer Georgios E. Magdis Guillaume Mahler A. M. Muñoz Arancibia Timothy Rawle Kazuhiro Shimasaku Sune Toft Hideki Umehata Francesco Valentino Tao Wang Wei-Hao Wang |
| author_sort | Seiji Fujimoto |
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| description | We present a statistical study of 180 dust continuum sources identified in 33 massive cluster fields by the Atacama Large Millimeter/submillimeter Array Lensing Cluster Survey (ALCS) over a total of 133 arcmin ^2 area, homogeneously observed at 1.2 mm. ALCS enables us to detect extremely faint millimeter sources by lensing magnification, including near-infrared (NIR) dark objects showing no counterparts in existing Hubble Space Telescope and Spitzer images. The dust continuum sources belong to a blind sample ( N = 141) with signal-to-noise ratio (S/N) ≳ 5.0 (a purity of >0.99) or a secondary sample ( N = 39) with S/N = 4.0–5.0 screened by priors. With the blind sample, we securely derive 1.2 mm number counts down to ∼7 μ Jy, and find that the total integrated 1.2 mm flux is ${20.7}_{-6.5}^{+8.5}$ Jy deg ^−2 , resolving ≃80% of the cosmic infrared background light. The resolved fraction varies by a factor of 0.6–1.1 due to the completeness correction depending on the spatial size of the millimeter emission. We also derive infrared (IR) luminosity functions (LFs) at z = 0.6–7.5 with the $1/{V}_{\max }$ method, finding the redshift evolution of IR LFs characterized by positive luminosity and negative density evolution. The total (= UV + IR) cosmic star formation rate density (SFRD) at z > 4 is estimated to be ${161}_{-21}^{+25}$ % of the Madau and Dickinson measurements mostly based on rest-frame UV surveys. Although our general understanding of the cosmic SFRD is unlikely to change beyond a factor of 2, these results add to the weight of evidence for an additional (≈60%) SFRD component contributed by the faint millimeter population, including NIR-dark objects. |
| format | Article |
| id | doaj-art-025b919c44a348a690b146d5af20ce04 |
| institution | Kabale University |
| issn | 0067-0049 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal Supplement Series |
| spelling | doaj-art-025b919c44a348a690b146d5af20ce042024-11-27T05:56:26ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492024-01-0127523610.3847/1538-4365/ad5ae2ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8Seiji Fujimoto0https://orcid.org/0000-0001-7201-5066Kotaro Kohno1https://orcid.org/0000-0002-4052-2394Masami Ouchi2https://orcid.org/0000-0002-1049-6658Masamune Oguri3https://orcid.org/0000-0003-3484-399XVasily Kokorev4https://orcid.org/0000-0002-5588-9156Gabriel Brammer5https://orcid.org/0000-0003-2680-005XFengwu Sun6https://orcid.org/0000-0002-4622-6617Jorge González-López7https://orcid.org/0000-0003-3926-1411Franz E. Bauer8https://orcid.org/0000-0002-8686-8737Gabriel B. Caminha9https://orcid.org/0000-0001-6052-3274Bunyo Hatsukade10https://orcid.org/0000-0001-6469-8725Johan Richard11https://orcid.org/0000-0001-5492-1049Ian Smail12https://orcid.org/0000-0003-3037-257XAkiyoshi Tsujita13https://orcid.org/0000-0002-0498-5041Yoshihiro Ueda14https://orcid.org/0000-0001-7821-6715Ryosuke Uematsu15https://orcid.org/0000-0001-6653-779XAdi Zitrin16https://orcid.org/0000-0002-0350-4488Dan Coe17https://orcid.org/0000-0001-7410-7669Jean-Paul Kneib18https://orcid.org/0000-0002-4616-4989Marc Postman19https://orcid.org/0000-0002-9365-7989Keiichi Umetsu20https://orcid.org/0000-0002-7196-4822Claudia del P. Lagos21https://orcid.org/0000-0003-3021-8564Gergö Popping22https://orcid.org/0000-0003-1151-4659Yiping Ao23https://orcid.org/0000-0003-3139-2724Larry Bradley24https://orcid.org/0000-0002-7908-9284Karina Caputi25https://orcid.org/0000-0001-8183-1460Miroslava Dessauges-Zavadsky26https://orcid.org/0000-0003-0348-2917Eiichi Egami27https://orcid.org/0000-0003-1344-9475Daniel Espada28https://orcid.org/0000-0002-8726-7685R. J. Ivison29https://orcid.org/0000-0001-5118-1313Mathilde Jauzac30https://orcid.org/0000-0003-1974-8732Kirsten K. Knudsen31https://orcid.org/0000-0002-7821-8873Anton M. Koekemoer32https://orcid.org/0000-0002-6610-2048Georgios E. Magdis33https://orcid.org/0000-0002-4872-2294Guillaume Mahler34https://orcid.org/0000-0003-3266-2001A. M. Muñoz Arancibia35https://orcid.org/0000-0002-8722-516XTimothy Rawle36https://orcid.org/0000-0002-7028-5588Kazuhiro Shimasaku37https://orcid.org/0000-0002-2597-2231Sune Toft38https://orcid.org/0000-0003-3631-7176Hideki Umehata39https://orcid.org/0000-0003-1937-0573Francesco Valentino40https://orcid.org/0000-0001-6477-4011Tao Wang41https://orcid.org/0000-0002-2504-2421Wei-Hao Wang42https://orcid.org/0000-0003-2588-1265Department of Astronomy, The University of Texas at Austin , Austin, TX, USA ; fujimoto@utexas.edu; Cosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK2200 Copenhagen N, DenmarkInstitute of Astronomy, Graduate School of Science, The University of Tokyo , 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan; Research Center for the Early Universe, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Institute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo , Kashiwa, Chiba 277-8583, JapanCenter for Frontier Science, Chiba University , 1-33 Yayoi-cho, Inage-ku, Chiba 263-8522, Japan; Department of Physics, Graduate School of Science, Chiba University , 1-33 Yayoi-Cho, Inage-Ku, Chiba 263-8522, JapanCosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK2200 Copenhagen N, Denmark; Kapteyn Astronomical Institute, University of Groningen , Postbus 800, 9700 AV Groningen, The NetherlandsCosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK2200 Copenhagen N, DenmarkSteward Observatory, University of Arizona , 933 N. Cherry Ave., Tucson, AZ 85721, USANúcleo de Astronomía de la Facultad de Ingeniería y Ciencias, Universidad Diego Portales , Av. Ejército Libertador 441, Santiago, Chile; Las Campanas Observatory, Carnegie Institution of Washington , Casilla 601, La Serena, ChileInstituto de Astrofísica , Facultad de Física, Pontificia Universidad Católica de Chile, Campus San Joaquín, Av. Vicuña Mackenna 4860, Macul Santiago, 7820436, Chile; Centro de Astroingeniería, Facultad de Física, Pontificia Universidad Católica de Chile , Campus San Joaquín, Av. Vicuña Mackenna 4860, Macul Santiago, 7820436, Chile; Millennium Institute of Astrophysics , Nuncio Monseñor Sótero Sanz 100, Of 104, Providencia, Santiago, ChileKapteyn Astronomical Institute, University of Groningen , Postbus 800, 9700 AV Groningen, The NetherlandsInstitute of Astronomy, Graduate School of Science, The University of Tokyo , 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Graduate Institute for Advanced Studies , SOKENDAI, Osawa, Mitaka, Tokyo 181-8588, JapanUniv Lyon, Univ Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574 , F-69230, Saint-Genis-Laval, FranceCentre for Extragalactic Astronomy, Department of Physics, Durham University , Durham DH1 3LE, UKInstitute of Astronomy, Graduate School of Science, The University of Tokyo , 2-21-1 Osawa, Mitaka, Tokyo 181-0015, JapanDepartment of Astronomy, Kyoto University , Kyoto 606-8502, JapanDepartment of Astronomy, Kyoto University , Kyoto 606-8502, JapanPhysics Department, Ben-Gurion University of the Negev , P.O. Box 653, Be’er-sheva 8410501, IsraelSpace Telescope Science Institute (STScI) , 3700 San Martin Dr., Baltimore, MD 21218, USA; Association of Universities for Research in Astronomy (AURA) , Inc. for the European Space Agency (ESA), USA; Center for Astrophysical Sciences, Department of Physics and Astronomy, The Johns Hopkins University , 3400 N Charles St., Baltimore, MD 21218, USALaboratoire dÁstrophysique , Ecole Polytechnique Fédérale de Lausanne, Observatoire de Sauverny, CH-1290 Versoix, SwitzerlandSpace Telescope Science Institute (STScI) , 3700 San Martin Dr., Baltimore, MD 21218, USAInstitute of Astronomy and Astrophysics , Academia Sinica (ASIAA), AS/NTU Astronomy-Mathematics Building, No. 1, Sec. 4, Roosevelt Rd., Taipei 10617, TaiwanCosmic Dawn Center (DAWN) , Denmark; International Centre for Radio Astronomy Research (ICRAR), M468, University of Western Australia , 35 Stirling Hwy, Crawley, WA 6009, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , AustraliaEuropean Southern Observatory , Karl-Schwarzschild-Str. 2, D-85748, Garching, GermanyPurple Mountain Observatory and Key Laboratory for Radio Astronomy, Chinese Academy of Sciences , Nanjing, People's Republic of ChinaSpace Telescope Science Institute (STScI) , 3700 San Martin Dr., Baltimore, MD 21218, USACosmic Dawn Center (DAWN) , Denmark; Kapteyn Astronomical Institute, University of Groningen , Postbus 800, 9700 AV Groningen, The NetherlandsDépartement d'Ástronomie, Université de Genève , Chemin Pegasi 51, 1290 Versoix, SwitzerlandSteward Observatory, University of Arizona , 933 N. Cherry Ave., Tucson, AZ 85721, USADepartamento de Física Teórica y del Cosmos, Campus de Fuentenueva, Edificio Mecenas, Universidad de Granada , E-18071, Granada, Spain; Instituto Carlos I de Física Teórica y Computacional , Facultad de Ciencias, E-18071, Granada, SpainEuropean Southern Observatory , Karl-Schwarzschild-Strasse 2, D-85748 Garching, GermanyCentre for Extragalactic Astronomy, Department of Physics, Durham University , Durham DH1 3LE, UK; Institute for Computational Cosmology, Durham University , South Road, Durham DH1 3LE, UKDepartment of Space, Earth and Environment, Chalmers University of Technology , SE-412 96 Gothenburg, SwedenSpace Telescope Science Institute (STScI) , 3700 San Martin Dr., Baltimore, MD 21218, USACosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK2200 Copenhagen N, Denmark; DTU-Space, Technical University of Denmark , Elektrovej 327, 2800, Kgs. Lyngby, DenmarkCentre for Extragalactic Astronomy, Department of Physics, Durham University , Durham DH1 3LE, UK; Institute for Computational Cosmology, Durham University , South Road, Durham DH1 3LE, UKMillennium Institute of Astrophysics , Nuncio Monseñor Sótero Sanz 100, Of 104, Providencia, Santiago, Chile; Center for Mathematical Modeling (CMM), Universidad de Chile , Beauchef 851, Santiago, ChileEuropean Space Agency (ESA), ESA Office, Space Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USAResearch Center for the Early Universe, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan; Department of Astronomy, School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanCosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK2200 Copenhagen N, DenmarkInstitute for Advanced Research, Nagoya University , Furocho, Chikusa, Nagoya 464-8602, Japan; Department of Physics, Graduate School of Science, Nagoya University , Furocho, Chikusa, Nagoya 464-8602, Japan; Cahill Center for Astronomy and Astrophysics, California Institute of Technology , 1200 E California Blvd, MC 249-17, Pasadena, CA 91125, USACosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK2200 Copenhagen N, Denmark; European Southern Observatory , Karl-Schwarzschild-Str. 2, D-85748, Garching, GermanySchool of Astronomy and Space Science, Nanjing University , Nanjing 210093, People's Republic of China; Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University) , Ministry of Education, Nanjing 210093, People's Republic of ChinaInstitute of Astronomy and Astrophysics , Academia Sinica (ASIAA), AS/NTU Astronomy-Mathematics Building, No. 1, Sec. 4, Roosevelt Rd., Taipei 10617, TaiwanWe present a statistical study of 180 dust continuum sources identified in 33 massive cluster fields by the Atacama Large Millimeter/submillimeter Array Lensing Cluster Survey (ALCS) over a total of 133 arcmin ^2 area, homogeneously observed at 1.2 mm. ALCS enables us to detect extremely faint millimeter sources by lensing magnification, including near-infrared (NIR) dark objects showing no counterparts in existing Hubble Space Telescope and Spitzer images. The dust continuum sources belong to a blind sample ( N = 141) with signal-to-noise ratio (S/N) ≳ 5.0 (a purity of >0.99) or a secondary sample ( N = 39) with S/N = 4.0–5.0 screened by priors. With the blind sample, we securely derive 1.2 mm number counts down to ∼7 μ Jy, and find that the total integrated 1.2 mm flux is ${20.7}_{-6.5}^{+8.5}$ Jy deg ^−2 , resolving ≃80% of the cosmic infrared background light. The resolved fraction varies by a factor of 0.6–1.1 due to the completeness correction depending on the spatial size of the millimeter emission. We also derive infrared (IR) luminosity functions (LFs) at z = 0.6–7.5 with the $1/{V}_{\max }$ method, finding the redshift evolution of IR LFs characterized by positive luminosity and negative density evolution. The total (= UV + IR) cosmic star formation rate density (SFRD) at z > 4 is estimated to be ${161}_{-21}^{+25}$ % of the Madau and Dickinson measurements mostly based on rest-frame UV surveys. Although our general understanding of the cosmic SFRD is unlikely to change beyond a factor of 2, these results add to the weight of evidence for an additional (≈60%) SFRD component contributed by the faint millimeter population, including NIR-dark objects.https://doi.org/10.3847/1538-4365/ad5ae2Galaxy formationGalaxy evolutionStarburst galaxiesMillimeter astronomyCosmic background radiationLuminosity function |
| spellingShingle | Seiji Fujimoto Kotaro Kohno Masami Ouchi Masamune Oguri Vasily Kokorev Gabriel Brammer Fengwu Sun Jorge González-López Franz E. Bauer Gabriel B. Caminha Bunyo Hatsukade Johan Richard Ian Smail Akiyoshi Tsujita Yoshihiro Ueda Ryosuke Uematsu Adi Zitrin Dan Coe Jean-Paul Kneib Marc Postman Keiichi Umetsu Claudia del P. Lagos Gergö Popping Yiping Ao Larry Bradley Karina Caputi Miroslava Dessauges-Zavadsky Eiichi Egami Daniel Espada R. J. Ivison Mathilde Jauzac Kirsten K. Knudsen Anton M. Koekemoer Georgios E. Magdis Guillaume Mahler A. M. Muñoz Arancibia Timothy Rawle Kazuhiro Shimasaku Sune Toft Hideki Umehata Francesco Valentino Tao Wang Wei-Hao Wang ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8 The Astrophysical Journal Supplement Series Galaxy formation Galaxy evolution Starburst galaxies Millimeter astronomy Cosmic background radiation Luminosity function |
| title | ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8 |
| title_full | ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8 |
| title_fullStr | ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8 |
| title_full_unstemmed | ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8 |
| title_short | ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8 |
| title_sort | alma lensing cluster survey deep 1 2 mm number counts and infrared luminosity functions at z ≃ 1 8 |
| topic | Galaxy formation Galaxy evolution Starburst galaxies Millimeter astronomy Cosmic background radiation Luminosity function |
| url | https://doi.org/10.3847/1538-4365/ad5ae2 |
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