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<\/a>Distribution of the JINGLE phase I & II targets and the parent galaxy sample (light grey dots) in the SFR-stellar mass (M\u2605<\/sub>) plane. Galaxies targeted by the JINGLE phase I generally lie on the galaxy main sequence. Galaxies targeted by JINGLE phase II lie either above the main sequence in the high-sSFR starburst regime (red dots) or are green valley galaxies (green dots) with generally low SFRs compared to normal star-forming galaxies. For the selection of starbursts two commonly advocated main-sequence shapes were considered: (1) a single power law SFR ~ M\u2605<\/sub>0.8<\/sup> and (2) a curved main sequence with flattening at high masses.<\/p><\/div>\n The position of the sample in the SFR-stellar mass plane is shown in the figure above. The observations will allow for the robust characterisation of the dust properties, as well as the measurement of total molecular gas masses for the RxA\/U\u2019u subsample. JINGLE targets are selected from fields with MaNGA optical integral-field spectroscopic coverage, have mid- to far-IR photometry from WISE and the Herschel-ATLAS survey and coverage from upcoming, new, blind interferometric HI surveys.<\/p>\n The combination of all these datasets will allow a detailed characterisation of the gas and dust properties and of the kinematics and metal contents of these galaxies, the derivation of scaling relations between dust, gas, and global properties, as well as provide critical benchmarks for high-redshift studies with JCMT and ALMA. Specific science questions that will be addressed in phase I include:<\/p>\n Left: H-ATLAS photometry of J120849.66+011130.5 (black points), with modified- blackbody models with different \u03b2 overlaid: \u03b2 = 1.5 (red dashed line) and \u03b2 = 2.0 (green dashed line). Clearly, the Herschel data alone cannot distinguish between the two scenarios, but the addition of a data point at 850\u03bcm does (e.g. the blue data point is a predicted 850\u03bcm SCUBA-2 flux for \u03b2 = 2). Right: Surface density plots showing the uncertainties in both \u03b2 and Tdust for Monte-Carlo simulations of Herschel data only (top) and Herschel+SCUBA-2 data (bottom). The uncertainties on \u03b2 and Tdust are drastically reduced with the addition of the SCUBA-2 850\u03bcm datum.<\/p><\/div>\n The main science drivers of the JINGLE phase II are:<\/p>\n Examples of starburst (1st\/2nd row) and green-valley galaxies (3rd row) targeted by JINGLE phase II. Upper row – morphologically disturbed, merging starburst galaxies; middle row – generally unperturbed starbursts with disk-like structure. Some of these show traces of minor interactions (e.g. central stamp in this row). Lower row – green valley galaxies.<\/p><\/div>\n By using the full JINGLE database, we will compare the interstellar medium properties of the outlier populations \u2013 i.e. starbursts and green valley galaxies \u2013 with those of \u2018normal\u2019 main sequence galaxies.<\/p>\n <\/p>\n Coordinators:<\/strong> H. S. Hwang (EAO\/Korea), L.-H. Lin (EAO\/Taiwan), A. Saintonge (UK), M. Sargent (UK), T. Tosaki (EAO\/Japan), Y. Koyama (EAO\/Japan), T. Xiao (EAO\/China), \u00a0C. Wilson (Canada)<\/p>\n \u2013 The JINGLE ADS Library can be accessed here<\/a><\/strong><\/p>\n \u2013 JCMT program code:<\/strong> M16AL005, M17BL010, M20AL013<\/strong><\/p>\n – \u00a0JINGLE homepage<\/a><\/strong><\/p>\n","protected":false},"excerpt":{"rendered":" – A new local galaxy evolution legacy survey JINGLE is a JCMT Large Program designed to systematically study the cold ISM of galaxies in the local Universe. With 780 hours of observing, phase I will provide integrated 850\u03bcm continuum measurements with SCUBA-2 for a representative sample of 193 Herschel-selected galaxies,\u2026 Continue reading<\/a><\/p>\n","protected":false},"author":5,"featured_media":0,"parent":3659,"menu_order":0,"comment_status":"closed","ping_status":"closed","template":"","meta":[],"_links":{"self":[{"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/pages\/3749"}],"collection":[{"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/users\/5"}],"replies":[{"embeddable":true,"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/comments?post=3749"}],"version-history":[{"count":18,"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/pages\/3749\/revisions"}],"predecessor-version":[{"id":12690,"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/pages\/3749\/revisions\/12690"}],"up":[{"embeddable":true,"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/pages\/3659"}],"wp:attachment":[{"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/media?parent=3749"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}\n
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