Eiji Akiyama NAOJ Chile Observatory Dec. 26 2017 ALMA/45m/ASTE Users Meeting 2017 Atacama Large Millimeter/submillimeter Ar
Asimmaa Atacama Large Millimeter/submillimeter Array
Kraus et al. 2017, van der Marel et al. 2013, 2016 ALMA 870μm ALMA + H-band ALMA + L’-band •Crescent structure implies dust trapping. •High pressure may be generated by an orbiting planet. •The presence of a planet is supported by NIR result (spiral feature). Atacama Large Millimeter/submillimeter Arra
Polarization due to self-scattering • Polarization fraction strongly depends on wavelength • Another method for confining dust size Derived dust size ~100 μm
Loomis et al. 2017 Casassus et al. 2013 Dutrey et al. 2014 AA Tau simulation •3 rings at 49, 95, and 143 au are found. • Streamer structure was found at inner region. eg. HD142527, GG Tau • Warped disk structure ? Atacama Large Millimeter/submillimeter Arra
Tsukagoshi et al. 2016 Andrews et al. 2016 Dust Observations • Little large dust grain exist at the ring gap. • The ring gap at 22 au can be explained by a Neptunian planet. ref. Kanagawa et al. 2015, 2016 Large Millimeter/submillimeter Array
Nomura et al. 2016
Gas Observations
•CO is drastically depleted inside of the CO snowline. •H, gas / dust = 1 ~ 0.1 ref. ~100 in ISM • The amount of CO directly affects the planet atmosphere. • Amino acid might be formed from a little CO gas (Aoki & Kobayashi’s experiments).
Walsh et al. 2014b Walsh et al. 2016 Theoretical prediction of CH3OH in protoplanetary disk 10-8 10-9 10-11 10-13 10-14 10-15 10-16
: etc. Atacama Large Millimeter/submillimeter Array
ive Declination (arcse 4 m 0 2 −2    −3 1 −1 Relative Right Ascension (arcsec) ー4
Glycolaldehyde (HCOCH,OH) a it Jorgensen et al. 2012. Large organic molecules were found in IRAS16293 – 2422 star forming region. 220.20 Freq (GHz) Credit: ESO/L. Calçada & NASA/JPL-Caltech/WISE Team
Martin-Domenech et al. 2017. Ligterink et al. 2017. Methyl isocyanate (CHLNCO) Methyl chloride (CH1,CL) Discovery ot Fayolle et al. 2017 CF1,Cl can not be treated as prebiotic molecule but comblex organic moleculês can be formed in star forming region.
Gerdes et al 2017 Trumbo et al. 2017 Palmer et al. 2017 Lellouch et al. 2017 •2014UZ 224 TNO object at 92 au observation • As results of ALMA & Blanco telescopes, it could be dwarf planet. •D = 635 ± 70 km • albedo = 13 ± 4 % ALMA image Model image • Europa, plume source investigation •nighttime (ALMA) & daytime (Galileo) image comparison •Heat excess in nighttime image is not due to endogenic heat flow but local thermal inertia. • Titan, Vinyl Cyanide has been confirmed at the Titan’s atmosphere. •Pluto, CO and HCN was detected in Pluto’s atmosphere.
Atacama Large Millimeter/submillimeter Array
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The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership among Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization for Astronomical Research in the Southern Hemisphere (ESO), in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in Japan by the National Institutes of Natural Sciences (NINS) in cooperation with the Academia Sinica (AS) in Taiwan. ALMA construction and operations are led on behalf of Europe by ESO, on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (AUI) and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.