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Title: AN ALMA DISK MASS FOR THE CANDIDATE PROTOPLANETARY COMPANION TO FW TAU

Abstract

We present ALMA observations of the FW Tau system, a close binary pair of M5 stars with a wide-orbit (300 AU projected separation) substellar companion. The companion is extremely faint and red in the optical and near-infrared, but boasts a weak far-infrared excess and optical/near-infrared emission lines indicative of a primordial accretion disk of gas and dust. The component-resolved 1.3 mm continuum emission is found to be associated only with the companion, with a flux (1.78 ± 0.03 mJy) that indicates a dust mass of 1-2 M {sub ⊕}. While this mass reservoir is insufficient to form a giant planet, it is more than sufficient to produce an analog of the Kepler-42 exoplanetary system or the Galilean satellites. The mass and geometry of the disk-bearing FW Tau companion remains unclear. Near-infrared spectroscopy shows deep water bands that indicate a spectral type later than M5, but substantial veiling prevents a more accurate determination of the effective temperature (and hence mass). Both a disk-bearing ''planetary-mass'' companion seen in direct light or a brown dwarf tertiary viewed in light scattered by an edge-on disk or envelope remain possibilities.

Authors:
 [1];  [2];  [3];  [4];  [5];  [6];  [7];  [8]
  1. Department of Astronomy, The University of Texas at Austin, Austin, TX 78712 (United States)
  2. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
  3. California Institute of Technology, Division of Geological and Planetary Sciences, 1200 East California Boulevard, Pasadena, CA 91101 (United States)
  4. Kavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Lu 5, Haidian Qu, Beijing 100871 (China)
  5. Research School of Astronomy and Astrophysics, Australian National University, Canberra ACT 2611 (Australia)
  6. Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States)
  7. Department of Physics and Astronomy, The University of Western Ontario, London, ON N6A 3K7 (Canada)
  8. Department of Physics and Astronomy, Hunter College, City University of New York, New York, NY 10065 (United States)
Publication Date:
OSTI Identifier:
22364713
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 798; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION SPECTROSCOPY; ACCRETION DISKS; COSMIC DUST; INFRARED SPECTRA; MASS; ORBITS; PLANETS; PROTOPLANETS; SATELLITES; STARS; VISIBLE RADIATION; WATER

Citation Formats

Kraus, Adam L., Andrews, Sean M., Bowler, Brendan P., Herczeg, Gregory, Ireland, Michael J., Liu, Michael C., Metchev, Stanimir, and Cruz, Kelle L. AN ALMA DISK MASS FOR THE CANDIDATE PROTOPLANETARY COMPANION TO FW TAU. United States: N. p., 2015. Web. doi:10.1088/2041-8205/798/1/L23.
Kraus, Adam L., Andrews, Sean M., Bowler, Brendan P., Herczeg, Gregory, Ireland, Michael J., Liu, Michael C., Metchev, Stanimir, & Cruz, Kelle L. AN ALMA DISK MASS FOR THE CANDIDATE PROTOPLANETARY COMPANION TO FW TAU. United States. doi:10.1088/2041-8205/798/1/L23.
Kraus, Adam L., Andrews, Sean M., Bowler, Brendan P., Herczeg, Gregory, Ireland, Michael J., Liu, Michael C., Metchev, Stanimir, and Cruz, Kelle L. Thu . "AN ALMA DISK MASS FOR THE CANDIDATE PROTOPLANETARY COMPANION TO FW TAU". United States. doi:10.1088/2041-8205/798/1/L23.
@article{osti_22364713,
title = {AN ALMA DISK MASS FOR THE CANDIDATE PROTOPLANETARY COMPANION TO FW TAU},
author = {Kraus, Adam L. and Andrews, Sean M. and Bowler, Brendan P. and Herczeg, Gregory and Ireland, Michael J. and Liu, Michael C. and Metchev, Stanimir and Cruz, Kelle L.},
abstractNote = {We present ALMA observations of the FW Tau system, a close binary pair of M5 stars with a wide-orbit (300 AU projected separation) substellar companion. The companion is extremely faint and red in the optical and near-infrared, but boasts a weak far-infrared excess and optical/near-infrared emission lines indicative of a primordial accretion disk of gas and dust. The component-resolved 1.3 mm continuum emission is found to be associated only with the companion, with a flux (1.78 ± 0.03 mJy) that indicates a dust mass of 1-2 M {sub ⊕}. While this mass reservoir is insufficient to form a giant planet, it is more than sufficient to produce an analog of the Kepler-42 exoplanetary system or the Galilean satellites. The mass and geometry of the disk-bearing FW Tau companion remains unclear. Near-infrared spectroscopy shows deep water bands that indicate a spectral type later than M5, but substantial veiling prevents a more accurate determination of the effective temperature (and hence mass). Both a disk-bearing ''planetary-mass'' companion seen in direct light or a brown dwarf tertiary viewed in light scattered by an edge-on disk or envelope remain possibilities.},
doi = {10.1088/2041-8205/798/1/L23},
journal = {Astrophysical Journal Letters},
number = 1,
volume = 798,
place = {United States},
year = {Thu Jan 01 00:00:00 EST 2015},
month = {Thu Jan 01 00:00:00 EST 2015}
}