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Journal Paper

전체
The JCMT Transient Survey: Data Reduction and Calibration Methods SCI
  • Steve Mairs;James Lane;Doug Johnstone;Helen Kirk;Kevin Lacaille;Geoffrey C. Bower;Graham S. Bell;Sarah Graves;Scott Chapman;Yuri Aikawa;Joanna Bulger;Vivien Chen;WenPing Chen;정은정;JenniferHatchell;Yuxin He;Gregory Herczeg;Po-Chieh Huang;강미주;강성주;김종수;김경희;김미량;김신영;Yi-Jehng Kuan;권우진;Shih-Ping Lai;Bhavana Lalchand;이정은;Feng Long;여아란;Oscar Morata;Harriet Parsons;AndyPon;Ramprasad Rao;Jonathan Rawlings;Manash Samal;Aleks Scholz;Peter Scicluna;Archana soam;Dimitris Stamatellos;Wang Yiren;Hyunju Yoo;Miaomiao Zhang;Jianjun Zhou;Geoffrey Bower
  • 2017-07-01
  • THE ASTROPHYSICAL JOURNAL 843 1 : 55-1~55-16
Though there has been a significant amount of work investigating the early stages of low-mass star formation inrecent years, the evolution of the mass assembly rate onto the central protostar remains largely unconstrained.Examining in depth the variation in this rate is critical to understanding the physics of star formation. Instabilitiesin the outer and inner circumstellar disk can lead to episodic outbursts. Observing these brightness variations atinfrared or submillimeter wavelengths constrains the current accretion models. The JCMT Transient Survey is athree-year project dedicated to studying the continuum variability of deeply embedded protostars in eight nearbystar-forming regions at a one-month cadence. We use the SCUBA-2 instrument to simultaneously observe theseregions at wavelengths of 450 and 850 μm. In this paper, we present the data reduction techniques, imagealignment procedures, and relative flux calibration methods for 850 μm data. We compare the properties andlocations of bright, compact emission sources fitted with Gaussians over time. Doing so, we achieve a spatialalignment of better than 1″ between the repeated observations and an uncertainty of 2%?3% in the relative peakbrightness of significant, localized emission. This combination of imaging performance is unprecedented inground-based, single-dish submillimeter observations. Finally, we identify a few sources that show possible andconfirmed brightness variations. These sources will be closely monitored and presented in further detail inadditional studies throughout the duration of the survey.