{"id":1959,"date":"2015-02-18T14:16:21","date_gmt":"2015-02-19T00:16:21","guid":{"rendered":"http:\/\/www.eaobservatory.org\/jcmt\/?page_id=1959"},"modified":"2019-12-27T17:07:19","modified_gmt":"2019-12-28T03:07:19","slug":"gbs","status":"publish","type":"page","link":"https:\/\/www.eaobservatory.org\/jcmt\/science\/legacy-survey\/gbs\/","title":{"rendered":"GBS"},"content":{"rendered":"<p><a href=\"http:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/JLSlogo1.jpg\"><img loading=\"lazy\" class=\"alignnone size-full wp-image-2595\" src=\"http:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/JLSlogo1.jpg\" alt=\"JLSlogo\" width=\"688\" height=\"237\" srcset=\"https:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/JLSlogo1.jpg 688w, https:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/JLSlogo1-300x103.jpg 300w, https:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/JLSlogo1-250x86.jpg 250w, https:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/JLSlogo1-150x52.jpg 150w\" sizes=\"(max-width: 688px) 100vw, 688px\" \/><\/a><\/p>\n<p><a href=\"http:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/gb_logo_small.gif\"><img loading=\"lazy\" class=\"alignnone size-full wp-image-1960\" src=\"http:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/gb_logo_small.gif\" alt=\"gb_logo_small\" width=\"200\" height=\"101\" \/><\/a><\/p>\n<h2>Gould Belt Survey<\/h2>\n<p>The Gould Belt Legacy Survey (GBS) is using three JCMT survey instruments (SCUBA-2, HARP and POL-2) to survey nearby star-forming regions (D &lt; 500 pc). The survey includes the best known Gould&#8217;s Belt clouds &#8211; Orion, Taurus, Perseus, Serpens and Ophiuchus &#8211; as well as less well-studied local star-forming regions, and complements similar Gould Belt surveys with the <i>Spitzer<\/i> and <i>Herschel<\/i> space telescopes. The SCUBA-2 targets are half-degree regions preselected on Herschel 500 micron emission to provide a deep, uniform 450\/850 micron survey. The HARP observations focus on subregions of the same clouds in <sup>12<\/sup>CO, <sup>13<\/sup>CO and C<sup>18<\/sup>O. The polarisation component of the survey is awaiting POL-2 commissioning. The science goals of the GBS are:<\/p>\n<ul>\n<li>Protostellar lifetimes and accretion rates;<\/li>\n<li>Origin of the IMF and brown dwarfs;<\/li>\n<li>Structure of cores to clouds;<\/li>\n<li>Evolutionary Classification<\/li>\n<li>Mass ejection and accretion rates;<\/li>\n<li>Core kinematics;<\/li>\n<li>Clouds and filaments;<\/li>\n<li>Tests of the standard model of star formation;<\/li>\n<li>Models of magnetic field geometry, strength and the Chandrasekhar-Fermi method;<\/li>\n<li>Large scale magnetic fields and turbulence.<\/li>\n<\/ul>\n<p>Target regions are: Orion A* \/ B* &#8211; Perseus* &#8211; Taurus*\/Auriga &#8211; Cepheus &#8211; Serpens*\/Aquila &#8211; Ophiuchus* &#8211; Pipe &#8211; IC5146 &#8211; CrA &#8211; Lupus V (* includes HARP data from GBS or GT)<\/p>\n<h3><a name=\"2-year\"><\/a>The 2-year programme<\/h3>\n<p>The 2012-14 allocated programme focusses on SCUBA-2: the HARP data were observed in 2007-2011.<\/p>\n<table border=\"1\">\n<tbody>\n<tr>\n<td align=\"center\"><b>Instrument<\/b><\/td>\n<td align=\"center\"><b>Tracer <\/b><\/td>\n<td align=\"center\"><b>Area <\/b><\/td>\n<td align=\"center\"><b>RMS<sup>(a)<\/sup> <\/b><\/td>\n<td align=\"center\"><b>\u0394v<br \/>\n(km\/s) <\/b><\/td>\n<td align=\"center\"><b>Weather<br \/>\nGrade <\/b><\/td>\n<td align=\"center\"><b>Time<br \/>\n(hrs)<\/b><\/td>\n<\/tr>\n<tr>\n<td>SCUBA-2<\/td>\n<td>450\/850 micron<\/td>\n<td>28 x 0.25 sq. deg.<\/td>\n<td>20\/5 mJy\/beam<\/td>\n<td><\/td>\n<td>1<\/td>\n<td>70<\/td>\n<\/tr>\n<tr>\n<td><\/td>\n<td>450\/850 micron<\/td>\n<td>67 x 0.25 sq. deg.<\/td>\n<td>50\/5 mJy\/beam<\/td>\n<td><\/td>\n<td>2<\/td>\n<td>342<\/td>\n<\/tr>\n<tr>\n<td>HARP-B<\/td>\n<td><sup>12<\/sup>CO<\/td>\n<td>5&#215;15&#8217;x15&#8242;<\/td>\n<td>0.3K<\/td>\n<td>1.0<\/td>\n<td>2<\/td>\n<td>250<\/td>\n<\/tr>\n<tr>\n<td><\/td>\n<td>C<sup>18<\/sup>O(<sup>13<\/sup>CO)<\/td>\n<td>5&#215;15&#8217;x15&#8242;<\/td>\n<td>0.3K (0.25K)<\/td>\n<td>0.1<\/td>\n<td>2<\/td>\n<td><\/td>\n<\/tr>\n<tr>\n<td>Total<\/td>\n<td><\/td>\n<td><\/td>\n<td><\/td>\n<td><\/td>\n<td><\/td>\n<td>662<\/td>\n<\/tr>\n<\/tbody>\n<\/table>\n<p><sup>(a)<\/sup>Approximate achieved sensitivities subject to variation between regions.<\/p>\n<h3><a name=\"Results\"><\/a>Results<\/h3>\n<p><a name=\"Results\"><\/a> <a name=\"Results\"><\/a><\/p>\n<ul>\n<li><a href=\"http:\/\/www.dunlap.utoronto.ca\/%7EjcmtGBLS\">Image gallery<\/a><\/li>\n<li><a href=\"http:\/\/adsabs.harvard.edu\/cgi-bin\/nph-abs_connect?db_key=AST&amp;db_key=PRE&amp;qform=AST&amp;arxiv_sel=astro-ph&amp;arxiv_sel=cond-mat&amp;arxiv_sel=cs&amp;arxiv_sel=gr-qc&amp;arxiv_sel=hep-ex&amp;arxiv_sel=hep-lat&amp;arxiv_sel=hep-ph&amp;arxiv_sel=hep-th&amp;arxiv_sel=math&amp;arxiv_sel=math-ph&amp;arxiv_sel=nlin&amp;arxiv_sel=nucl-ex&amp;arxiv_sel=nucl-th&amp;arxiv_sel=physics&amp;arxiv_sel=quant-ph&amp;arxiv_sel=q-bio&amp;sim_query=YES&amp;ned_query=YES&amp;adsobj_query=YES&amp;aut_req=YES&amp;aut_logic=OR&amp;obj_logic=OR&amp;author=Hatchell&amp;object=&amp;start_mon=&amp;start_year=2006&amp;end_mon=&amp;end_year=&amp;ttl_req=YES&amp;ttl_logic=BOOL&amp;title=%28JCMT+OR+James%29+AND+%28Gould+OR+Gould%27s%29+AND+Belt+&amp;txt_logic=AND&amp;text=&amp;nr_to_return=200&amp;start_nr=1&amp;jou_pick=ALL&amp;ref_stems=&amp;data_and=ALL&amp;group_and=ALL&amp;start_entry_day=&amp;start_entry_mon=&amp;start_entry_year=&amp;end_entry_day=&amp;end_entry_mon=&amp;end_entry_year=&amp;min_score=&amp;sort=SCORE&amp;data_type=SHORT&amp;aut_syn=YES&amp;ttl_syn=YES&amp;txt_syn=YES&amp;aut_wt=1.0&amp;obj_wt=1.0&amp;ttl_wt=0.3&amp;txt_wt=3.0&amp;aut_wgt=YES&amp;obj_wgt=YES&amp;ttl_wgt=YES&amp;txt_wgt=YES&amp;ttl_sco=YES&amp;txt_sco=YES&amp;version=1\">Publications list<\/a> from ADS<\/li>\n<li><a href=\"http:\/\/www.cadc-ccda.hia-iha.nrc-cnrc.gc.ca\/en\/search\/?collection=JCMT&amp;noexec=true\">The JCMT Science Archive at CADC<\/a><\/li>\n<li><a href=\"http:\/\/wiki.astro.ex.ac.uk\/bin\/view\/JCMTGouldBelt\/WebHome\">GBS Wiki<\/a>(team members only)<\/li>\n<\/ul>\n<p><b>For further information contact the coordinators:<\/b> Jenny Hatchell (University of Exeter), James Di Francesco (NRC Herzberg), Derek Ward-Thompson (UCLAN) and Michiel Hogerheijde (Leiden).<br \/>\n<a href=\"http:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/gb_hst_s2_orion.jpeg\"><img loading=\"lazy\" class=\" wp-image-1965 size-large aligncenter\" src=\"http:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/gb_hst_s2_orion-1021x1024.jpeg\" alt=\"gb_hst_s2_orion\" width=\"800\" height=\"802\" srcset=\"https:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/gb_hst_s2_orion-1021x1024.jpeg 1021w, https:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/gb_hst_s2_orion-150x150.jpeg 150w, https:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/gb_hst_s2_orion-300x300.jpeg 300w, https:\/\/www.eaobservatory.org\/jcmt\/wp-content\/uploads\/sites\/2\/2015\/02\/gb_hst_s2_orion.jpeg 1799w\" sizes=\"(max-width: 800px) 100vw, 800px\" \/><\/a>The dust lanes in Orion are detected in emission by SCUBA-2 at 850 microns (red) but appear as dark features blocking the optical starlight observed by the Hubble Space Telescope map (blue). Figure Credit: Carl Salji.<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Gould Belt Survey The Gould Belt Legacy Survey (GBS) is using three JCMT survey instruments (SCUBA-2, HARP and POL-2) to survey nearby star-forming regions (D &lt; 500 pc). The survey includes the best known Gould&#8217;s Belt clouds &#8211; Orion, Taurus, Perseus, Serpens and Ophiuchus &#8211; as well as less well-studied\u2026 <a class=\"continue-reading-link\" href=\"https:\/\/www.eaobservatory.org\/jcmt\/science\/legacy-survey\/gbs\/\">Continue reading<\/a><\/p>\n","protected":false},"author":7,"featured_media":0,"parent":1606,"menu_order":0,"comment_status":"closed","ping_status":"closed","template":"","meta":[],"_links":{"self":[{"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/pages\/1959"}],"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\/7"}],"replies":[{"embeddable":true,"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/comments?post=1959"}],"version-history":[{"count":10,"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/pages\/1959\/revisions"}],"predecessor-version":[{"id":5645,"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/pages\/1959\/revisions\/5645"}],"up":[{"embeddable":true,"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/pages\/1606"}],"wp:attachment":[{"href":"https:\/\/www.eaobservatory.org\/jcmt\/wp-json\/wp\/v2\/media?parent=1959"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}