How do stars gain their mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star Forming Regions

Autor: Herczeg, Gregory J., Johnstone, Doug, Mairs, Steve, Hatchell, Jennifer, Lee, Jeong-Eun, Bower, Geoffrey C., Chen, Huei-Ru Vivien, Aikawa, Yuri, Yoo, Hyunju, Kang, Sung-Ju, Kang, Miju, Chen, Wen-Ping, Williams, Jonathan P., Bae, Jaehan, Dunham, Michael M., Vorobiov, Eduard I., Zhu, Zhaohuan, Rao, Ramprasad, Kirk, Helen, Takahashi, Satoko, Morata, Oscar, Lacaille, Kevin, Lane, James, Pon, Andy, Scholz, Aleks, Samal, Manash R., Bell, Graham S., Graves, Sarah, Lee, E'lisa M., Parsons, Harriet, He, Yuxin, Zhou, Jianjun, Kim, Mi-Ryang, Chapman, Scott, Drabek-Maunder, Emily, Chung, Eun Jung, Eyres, Stewart P. S., Forbrich, Jan, Hillenbrand, Lynne A., Inutsuka, Shu-ichiro, Kim, Gwanjeong, Kim, Kyoung Hee, Kuan, Yi-Jehng, Kwon, Woojin, Lai, Shih-Ping, Lalchand, Bhavana, Lee, Chang Won, Lee, Chin-Fei, Long, Feng, Lyo, A-Ran, Qian, Lei, Scicluna, Peter, Soam, Archana, Stamatellos, Dimitris, Takakuwa, Shigehisa, Tang, Ya-Wen, Wang, Hongchi, Wang, Yiren
Rok vydání: 2017
Předmět:
Druh dokumentu: Working Paper
DOI: 10.3847/1538-4357/aa8b62
Popis: Most protostars have luminosities that are fainter than expected from steady accretion over the protostellar lifetime. The solution to this problem may lie in episodic mass accretion -- prolonged periods of very low accretion punctuated by short bursts of rapid accretion. However, the timescale and amplitude for variability at the protostellar phase is almost entirely unconstrained. In "A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star Forming Regions", we are monitoring monthly with SCUBA-2 the sub-mm emission in eight fields within nearby (<500 pc) star forming regions to measure the accretion variability of protostars. The total survey area of ~1.6 sq.deg. includes ~105 peaks with peaks brighter than 0.5 Jy/beam (43 associated with embedded protostars or disks) and 237 peaks of 0.125-0.5 Jy/beam (50 with embedded protostars or disks). Each field has enough bright peaks for flux calibration relative to other peaks in the same field, which improves upon the nominal flux calibration uncertainties of sub-mm observations to reach a precision of ~2-3% rms, and also provides quantified confidence in any measured variability. The timescales and amplitudes of any sub-mm variation will then be converted into variations in accretion rate and subsequently used to infer the physical causes of the variability. This survey is the first dedicated survey for sub-mm variability and complements other transient surveys at optical and near-IR wavelengths, which are not sensitive to accretion variability of deeply embedded protostars.
Comment: ApJ, accepted
Databáze: arXiv
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