TY - JOUR
T1 - A CANDIDATE PLANETARY-MASS OBJECT with A PHOTOEVAPORATING DISK in ORION
AU - Fang, Min
AU - Kim, Jinyoung Serena
AU - Pascucci, Ilaria
AU - Apai, Dániel
AU - Manara, Carlo Felice
N1 - Funding Information:
This material is based upon work supported by the National Aeronautics and Space Administration under Agreement No. NNX15AD94G for the program Earths in Other Solar Systems. The results reported herein benefited from collaborations and/or information exchange within NASAs Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASAs Science Mission Directorate. CFM gratefully acknowledges an ESA Research Fellowship. This research is based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA).
Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.
PY - 2016/12/20
Y1 - 2016/12/20
N2 - In this work, we report the discovery of a candidate planetary-mass object with a photoevaporating protoplanetary disk, Proplyd 133-353, which is near the massive star θ 1 Ori C at the center of the Orion Nebula Cluster (ONC). The object was known to have extended emission pointing away from θ 1 OriC, indicating ongoing external photoevaporation. Our near-infrared spectroscopic data and the location on the H-R diagram suggest that the central source of Proplyd 133-353 is substellar (∼M9.5) and has a mass probably less than 13 Jupiter mass and an age younger than 0.5 Myr. Proplyd 133-353 shows a similar ratio of X-ray luminosity to stellar luminosity to other young stars in the ONC with a similar stellar luminosity and has a similar proper motion to the mean one of confirmed ONC members. We propose that Proplyd 133-353 formed in a very low-mass dusty cloud or an evaporating gas globule near θ 1 Ori C as a second generation of star formation, which can explain both its young age and the presence of its disk.
AB - In this work, we report the discovery of a candidate planetary-mass object with a photoevaporating protoplanetary disk, Proplyd 133-353, which is near the massive star θ 1 Ori C at the center of the Orion Nebula Cluster (ONC). The object was known to have extended emission pointing away from θ 1 OriC, indicating ongoing external photoevaporation. Our near-infrared spectroscopic data and the location on the H-R diagram suggest that the central source of Proplyd 133-353 is substellar (∼M9.5) and has a mass probably less than 13 Jupiter mass and an age younger than 0.5 Myr. Proplyd 133-353 shows a similar ratio of X-ray luminosity to stellar luminosity to other young stars in the ONC with a similar stellar luminosity and has a similar proper motion to the mean one of confirmed ONC members. We propose that Proplyd 133-353 formed in a very low-mass dusty cloud or an evaporating gas globule near θ 1 Ori C as a second generation of star formation, which can explain both its young age and the presence of its disk.
KW - brown dwarfs
KW - circumstellar matter
KW - stars: pre-main sequence
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U2 - 10.3847/2041-8213/833/2/L16
DO - 10.3847/2041-8213/833/2/L16
M3 - Article
AN - SCOPUS:85007008949
SN - 2041-8205
VL - 833
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 2
M1 - L16
ER -