A deep photometric survey of the η Chamaeleontis cluster down to the brown dwarf - Planet boundary

A. Ran Lyo; Inseok Song; Warrick A. Lawson; M. S. Bessell; B. Zuckerman

doi:10.1111/j.1365-2966.2006.10232.x

A deep photometric survey of the η Chamaeleontis cluster down to the brown dwarf - Planet boundary

A. Ran Lyo^*, Inseok Song, Warrick A. Lawson, M. S. Bessell, B. Zuckerman

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

17 Citations (Scopus)

Abstract

We report the outcome of the deep optical/infrared photometric survey of the central region (33 × 33 arcmin² or 0.9 pc²) of the η Chamaeleontis (η Cha) pre-main sequence star cluster. The completeness limits of the photometry are I = 19.1, J = 18.2 and H = 17.6, faint enough to reveal low-mass members down to the brown dwarf and planet boundary of ≈13 M_jup. We found no such low-mass members in this region. Our result combined with a previous shallower (I = 17) but larger area survey indicates that low-mass objects (0.013 < M/M_⊙ < 0.075) were either not created in the η Cha cluster or lost due to the early dynamical history of the cluster and ejected to outside the surveyed areas.

Original language	English
Pages (from-to)	1451-1455
Number of pages	5
Journal	Monthly Notices of the Royal Astronomical Society
Volume	368
Issue number	3
DOIs	https://doi.org/10.1111/j.1365-2966.2006.10232.x
Publication status	Published - May 2006

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title = "A deep photometric survey of the η Chamaeleontis cluster down to the brown dwarf - Planet boundary",

abstract = "We report the outcome of the deep optical/infrared photometric survey of the central region (33 × 33 arcmin2 or 0.9 pc2) of the η Chamaeleontis (η Cha) pre-main sequence star cluster. The completeness limits of the photometry are I = 19.1, J = 18.2 and H = 17.6, faint enough to reveal low-mass members down to the brown dwarf and planet boundary of ≈13 Mjup. We found no such low-mass members in this region. Our result combined with a previous shallower (I = 17) but larger area survey indicates that low-mass objects (0.013 < M/M⊙ < 0.075) were either not created in the η Cha cluster or lost due to the early dynamical history of the cluster and ejected to outside the surveyed areas.",

keywords = "Open clusters and associations: individual: η Chamaeleontis, Stars: fundamental parameters, Stars: pre-main-sequence",

author = "Lyo, {A. Ran} and Inseok Song and Lawson, {Warrick A.} and Bessell, {M. S.} and B. Zuckerman",

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doi = "10.1111/j.1365-2966.2006.10232.x",

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T1 - A deep photometric survey of the η Chamaeleontis cluster down to the brown dwarf - Planet boundary

AU - Lyo, A. Ran

AU - Song, Inseok

AU - Lawson, Warrick A.

AU - Bessell, M. S.

AU - Zuckerman, B.

PY - 2006/5

Y1 - 2006/5

N2 - We report the outcome of the deep optical/infrared photometric survey of the central region (33 × 33 arcmin2 or 0.9 pc2) of the η Chamaeleontis (η Cha) pre-main sequence star cluster. The completeness limits of the photometry are I = 19.1, J = 18.2 and H = 17.6, faint enough to reveal low-mass members down to the brown dwarf and planet boundary of ≈13 Mjup. We found no such low-mass members in this region. Our result combined with a previous shallower (I = 17) but larger area survey indicates that low-mass objects (0.013 < M/M⊙ < 0.075) were either not created in the η Cha cluster or lost due to the early dynamical history of the cluster and ejected to outside the surveyed areas.

AB - We report the outcome of the deep optical/infrared photometric survey of the central region (33 × 33 arcmin2 or 0.9 pc2) of the η Chamaeleontis (η Cha) pre-main sequence star cluster. The completeness limits of the photometry are I = 19.1, J = 18.2 and H = 17.6, faint enough to reveal low-mass members down to the brown dwarf and planet boundary of ≈13 Mjup. We found no such low-mass members in this region. Our result combined with a previous shallower (I = 17) but larger area survey indicates that low-mass objects (0.013 < M/M⊙ < 0.075) were either not created in the η Cha cluster or lost due to the early dynamical history of the cluster and ejected to outside the surveyed areas.

KW - Open clusters and associations: individual: η Chamaeleontis

KW - Stars: fundamental parameters

KW - Stars: pre-main-sequence

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U2 - 10.1111/j.1365-2966.2006.10232.x

DO - 10.1111/j.1365-2966.2006.10232.x

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JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

A deep photometric survey of the η Chamaeleontis cluster down to the brown dwarf - Planet boundary

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