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Published June 2022 | Published + Accepted Version
Journal Article Open

Monitoring Inner Regions in the RY Tau Jet

Abstract

We present multiepoch observations of the RY Tau jet for Hα and [Fe ii] 1.644 μm emission lines obtained with the Subaru Coronagraphic Extreme-AO and Visible Aperture Masking Polarimetric Imager for Resolved Exoplanetary Structures (VAMPIRES), Gemini Near-infrared Integral Field Spectrograph, and Keck/OSIRIS in 2019–2021. These data show a series of four knots within 1″ consistent with the proper motion of ∼0.″3 yr⁻¹, analogous to the jets associated with another few active T Tauri stars. However, the spatial intervals between the knots suggest the time intervals of the ejections of about 1.2, 0.7, and 0.7 yr, significantly shorter than those estimated for the other stars. These Hα images contrast with the archival Very Large Telescope Spectro-Polarimetric High-contrast Exoplanet Research and Zurich IMaging POLarimeter (ZIMPOL) observations from 2015, which showed only a single knot-like feature at ∼0.″25. The difference between the 2015 and 2019–2021 epochs suggests an irregular ejection interval within the six-year range. Such variations of the jet ejection may be related to a short-term (α emissions with the ZIMPOL data taken in 2015, showing the brighter profile at the base (<0.″3) than the 2020–2021 VAMPIRES profiles due to time-variable mass ejection rates or the heating–cooling balance in the jet. The observed jet knot structures may be alternatively attributed to stationary shocks, but a higher angular resolution is required to confirm its detailed origin.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2022 January 25; revised 2022 April 13; accepted 2022 April 13; published 2022 May 16. The authors would like to thank the anonymous referee for their constructive comments and suggestions to improve the quality of the paper. T.U. is supported by Grant-in-Aid for Japan Society for the Promotion of Science (JSPS) Fellows and JSPS KAKENHI grant No. JP21J01220. M.Takami is supported by the Ministry of Science and Technology (MoST) of Taiwan (grant Nos. 106-2119-M-001-026-MY3, 109-2112-M-001-019, 110-2112-M-001-044). G.C. thanks the Swiss National Science Foundation for financial support under grant No. 200021_169131. M.Tamura is supported by JSPS KAKENHI grant Nos. 18H05442, 15H02063, and 22000005. E.A. is supported by MEXT/JSPS KAKENHI grant No. 17K05399. H.M.G. was supported by Program number HST-GO-15210.002 provided through a grant from the STScI under NASA contract NAS5-26555. P.C.S. gratefully acknowledges support by DLR 50 OR 2102. This research is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, and those via the time exchange program between Subaru and the international Gemini Observatory, a program of NSFs NOIRLab. The part of data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Part of the data are based on observations collected at the European Southern Observatory under ESO program 096.C-0454(A). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. This research has made use of NASA's Astrophysics Data System Bibliographic Services. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.

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Additional details

Created:
August 22, 2023
Modified:
October 24, 2023