Sökning: WFRF:(Lee Minju M.) > (2020) > ALMA uncovers the [...
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000 | 06236naa a2200541 4500 | |
001 | oai:DiVA.org:uu-411003 | |
003 | SwePub | |
008 | 200527s2020 | |||||||||||000 ||eng| | |
024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-4110032 URI |
024 | 7 | a https://doi.org/10.1093/mnras/staa5092 DOI |
040 | a (SwePub)uu | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a ref2 swepub-contenttype |
072 | 7 | a art2 swepub-publicationtype |
100 | 1 | a Bakx, Tom J. L. C.u Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan.;Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.4 aut |
245 | 1 0 | a ALMA uncovers the [C II] emission and warm dust continuum in a z=8.31 Lyman break galaxy |
264 | c 2020-03-05 | |
264 | 1 | b Oxford University Press (OUP),c 2020 |
338 | a print2 rdacarrier | |
520 | a We report on the detection of the [C II] 157.7 mu m emission from the Lyman break galaxy (LBG) MACS0416_Y1 at z = 8.3113, by using the Atacama Large Millimeter/submillimeter Array (ALMA). The luminosity ratio of [O III] 88 mu m (from previous campaigns) to [CII] is 9.3 +/- 2.6, indicative of hard interstellar radiation fields and/or a low covering fraction of photodissociation regions. The emission of [C II] is cospatial to the 850 mu m dust emission (90 mu m rest frame, from previous campaigns), however the peak [C II] emission does not agree with the peak [O III] emission, suggesting that the lines originate from different conditions in the interstellar medium. We fail to detect continuum emission at 1.5 mm (160 mu m rest frame) down to 18 mu Jy (3 sigma). This non-detection places a strong limits on the dust spectrum, considering the 137 +/- 26 mu Jy continuum emission at 850 mu m. This suggests an unusually warm dust component (T > 80 K, 90 per cent confidence limit), and/or a steep dust-emissivity index (beta(dust) > 2), compared to galaxy-wide dust emission found at lower redshifts (typically T similar to 30-50 K, beta(dust) similar to 1-2). If such temperatures are common, thiswould reduce the required dust mass and relax the dust production problem at the highest redshifts. We therefore warn against the use of only single-wavelength information to derive physical properties, recommend a more thorough examination of dust temperatures in the early Universe, and stress the need for instrumentation that probes the peak of warm dust in the Epoch of Reionization. | |
650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
653 | a galaxies: formation | |
653 | a galaxies: high-redshift | |
653 | a galaxies: ISM | |
700 | 1 | a Tamura, Yoichiu Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan.4 aut |
700 | 1 | a Hashimoto, Takuyau Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.;Univ Tsukubu, Fac Pure & Appl Sci, Tomonaga Ctr Hist Universe TCHoU, Tsukuba, Ibaraki 3058571, Japan.;Osaka Sangyo Univ, Fac Design Technol, Dept Environm Sci & Technol, 3-1-1 Nakagaito, Daito, Osaka 5748530, Japan.4 aut |
700 | 1 | a Inoue, Akio K.u Waseda Univ, Fac Sci & Engn, Sch Adv Sci & Engn, Dept Phys,Shinjuku Ku, 3-4-1 Okubo, Tokyo 1698555, Japan.;Waseda Univ, Fac Sci & Engn, Waseda Res Inst Sci & Engn, Shinjuku Ku, 3-4-1 Okubo, Tokyo 1698555, Japan.4 aut |
700 | 1 | a Lee, Minju M.u Max Planck Inst Extraterrestr Phys MPE, Giessenbachstr, D-85748 Garching, Germany.4 aut |
700 | 1 | a Mawatari, Kenu Osaka Sangyo Univ, Fac Design Technol, Dept Environm Sci & Technol, 3-1-1 Nakagaito, Daito, Osaka 5748530, Japan.;Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.4 aut |
700 | 1 | a Ota, Kazuakiu Kyoto Univ, Res Adm Off, Sakyo Ku, Kyoto 6068501, Japan.4 aut |
700 | 1 | a Umehata, Hidekiu Open Univ Japan, 2-11 Wakaba, Chiba 2618586, Japan.;RIKEN, Cluster Pioneering Res, 2-1 Hirosawa, Wako, Saitama 3510198, Japan.;Univ Tokyo, Grad Sch Sci, Inst Astron, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan.4 aut |
700 | 1 | a Zackrisson, Eriku Uppsala universitet,Observationell astrofysik4 aut0 (Swepub:uu)erzac792 |
700 | 1 | a Hatsukade, Bunyou Univ Tokyo, Grad Sch Sci, Inst Astron, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan.4 aut |
700 | 1 | a Kohno, Kotarou Univ Tokyo, Grad Sch Sci, Inst Astron, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan.;Univ Tokyo, Grad Sch Sci, Res Ctr Early Universe, Tokyo 1130033, Japan.4 aut |
700 | 1 | a Matsuda, Yuichiu Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.;Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.4 aut |
700 | 1 | a Matsuo, Hiroshiu Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.;Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.4 aut |
700 | 1 | a Okamoto, Takashiu Hokkaido Univ, Fac Sci, Kita Ku, N10 W8, Sapporo, Hokkaido 0600810, Japan.4 aut |
700 | 1 | a Shibuya, Takatoshiu Kitami Inst Technol, 165 Koen Cho, Kitami, Hokkaido 0908507, Japan.4 aut |
700 | 1 | a Shimizu, Ikkohu Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.4 aut |
700 | 1 | a Taniguchi, Yoshiakiu Kyoto Univ, Res Adm Off, Sakyo Ku, Kyoto 6068501, Japan.4 aut |
700 | 1 | a Yoshida, Naokiu Univ Tokyo, Grad Sch Sci, Dept Phys, Tokyo 1130033, Japan.;Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan.4 aut |
710 | 2 | a Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan.;Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.b Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan.4 org |
773 | 0 | t Monthly notices of the Royal Astronomical Societyd : Oxford University Press (OUP)g 493:3, s. 4294-4307q 493:3<4294-4307x 0035-8711x 1365-2966 |
856 | 4 | u https://academic.oup.com/mnras/article-pdf/493/3/4294/32920502/staa509.pdf |
856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-411003 |
856 | 4 8 | u https://doi.org/10.1093/mnras/staa509 |
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