CaltechAUTHORS
  A Caltech Library Service

Monitoring Inner Regions in the RY Tau Jet

Uyama, Taichi and Takami, Michihiro and Cugno, Gabriele and Deo, Vincent and Guyon, Olivier and Hashimoto, Jun and Lozi, Julien and Norris, Barnaby and Tamura, Motohide and Vievard, Sebastien and Günther, Hans Moritz and Schneider, P. Christian and Akiyama, Eiji and Beck, Tracy L. and Currie, Thayne and Hodapp, Klaus and Kwon, Jungmi and Mayama, Satoshi and Ohyama, Youichi and Pyo, Tae-Soo and Wisniewski, John P. (2022) Monitoring Inner Regions in the RY Tau Jet. Astronomical Journal, 163 (6). Art. No. 268. ISSN 0004-6256. doi:10.3847/1538-3881/ac67a0. https://resolver.caltech.edu/CaltechAUTHORS:20220517-214234864

[img] PDF - Published Version
Creative Commons Attribution.

888kB
[img] PDF - Accepted Version
Creative Commons Attribution Non-commercial No Derivatives.

1MB

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20220517-214234864

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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/ac67a0DOIArticle
https://arxiv.org/abs/2201.11911arXivDiscussion Paper
ORCID:
AuthorORCID
Uyama, Taichi0000-0002-6879-3030
Takami, Michihiro0000-0001-9248-7546
Cugno, Gabriele0000-0001-7255-3251
Deo, Vincent0000-0003-4514-7906
Guyon, Olivier0000-0002-1097-9908
Hashimoto, Jun0000-0002-3053-3575
Lozi, Julien0000-0002-3047-1845
Norris, Barnaby0000-0002-8352-7515
Tamura, Motohide0000-0002-6510-0681
Vievard, Sebastien0000-0003-4018-2569
Günther, Hans Moritz0000-0003-4243-2840
Schneider, P. Christian0000-0002-5094-2245
Akiyama, Eiji0000-0002-5082-8880
Beck, Tracy L.0000-0002-6881-0574
Currie, Thayne0000-0002-7405-3119
Hodapp, Klaus0000-0003-0786-2140
Kwon, Jungmi0000-0003-2815-7774
Mayama, Satoshi0000-0002-3424-6266
Ohyama, Youichi0000-0001-9490-3582
Pyo, Tae-Soo0000-0002-3273-0804
Wisniewski, John P.0000-0001-9209-1808
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.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Japan Society for the Promotion of Science (JSPS)JP21J01220
Ministry of Science and Technology (Taipei)106-2119-M-001-026-MY3
Ministry of Science and Technology (Taipei)109-2112-M-001-019
Ministry of Science and Technology (Taipei)110-2112-M-001-044
Swiss National Science Foundation (SNSF)200021_169131
Japan Society for the Promotion of Science (JSPS)18H05442
Japan Society for the Promotion of Science (JSPS)15H02063
Japan Society for the Promotion of Science (JSPS)22000005
Japan Society for the Promotion of Science (JSPS)17K05399
NASAHST-GO-15210.002
NASANAS5-26555
Deutsches Zentrum für Luft- und Raumfahrt (DLR)DLR 50 OR 2012
W. M. Keck FoundationUNSPECIFIED
Gaia Multilateral AgreementUNSPECIFIED
Subject Keywords:Stellar jets; T Tauri stars
Issue or Number:6
Classification Code:Unified Astronomy Thesaurus concepts: Stellar jets (1607); T Tauri stars (1681)
DOI:10.3847/1538-3881/ac67a0
Record Number:CaltechAUTHORS:20220517-214234864
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220517-214234864
Official Citation:Taichi Uyama et al 2022 AJ 163 268
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:114780
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:18 May 2022 14:20
Last Modified:03 Jun 2022 18:00

Repository Staff Only: item control page