TY - JOUR
T1 - Near-infrared photometric monitoring of the pre-main-sequence object KH 15D
AU - Kusakabe, Nobuhiko
AU - Tamura, Motohide
AU - Nakajima, Yasushi
AU - Kandori, Ryo
AU - Ishihara, Akika
AU - Nagata, Tetsuya
AU - Nagayama, Takahiro
AU - Nishiyama, Shogo
AU - Baba, Daisuke
AU - Sato, Shuji
AU - Sugitani, Koji
AU - Turner, Edwin L.
AU - Abe, Lyu
AU - Kimura, Hiroshi
AU - Yamamoto, Tetsuo
PY - 2005/10/20
Y1 - 2005/10/20
N2 - Extensive photometric monitoring of KH 15D, an enigmatic variable in the young star cluster NGC 2264, has been conducted. Simultaneous and accurate near-infrared photometry (JHK, bands) between 2003 December and 2005 March is presented, covering most of the variable phase. The infrared variability is characterized by a large-amplitude and long-lasting eclipse, as observed in the optical. The period of variability is 48.3 ± 0.2 days, the maximum photometric amplitude of variability is ∼4.2 mag, and the eclipse duration is ∼0,5 in phase units. These are consistent with the most recent period, amplitude, and duration in the optical. The blueing of the J-H color (∼0.16 mag) during eclipse, which has been suggested before, is unambiguously confirmed; a similar blueing at H-K, is less clear but is probably present at a similar level. The overall shape of the JHK, light curves is very similar to the optical one, including a fair time symmetry and less stable flux during eclipse, with a slight hump near zero phase. Most of these variability features of KH 15D observed at near-infrared wavelengths can be explained with the recent model that employs an eclipse by an inclined, precessing disk and an outer scattering region around a pre-main-sequence binary.
AB - Extensive photometric monitoring of KH 15D, an enigmatic variable in the young star cluster NGC 2264, has been conducted. Simultaneous and accurate near-infrared photometry (JHK, bands) between 2003 December and 2005 March is presented, covering most of the variable phase. The infrared variability is characterized by a large-amplitude and long-lasting eclipse, as observed in the optical. The period of variability is 48.3 ± 0.2 days, the maximum photometric amplitude of variability is ∼4.2 mag, and the eclipse duration is ∼0,5 in phase units. These are consistent with the most recent period, amplitude, and duration in the optical. The blueing of the J-H color (∼0.16 mag) during eclipse, which has been suggested before, is unambiguously confirmed; a similar blueing at H-K, is less clear but is probably present at a similar level. The overall shape of the JHK, light curves is very similar to the optical one, including a fair time symmetry and less stable flux during eclipse, with a slight hump near zero phase. Most of these variability features of KH 15D observed at near-infrared wavelengths can be explained with the recent model that employs an eclipse by an inclined, precessing disk and an outer scattering region around a pre-main-sequence binary.
KW - Circumstellar matter
KW - Planetary systems: protoplanetary disks
KW - Stars: individual (KH 15D)
KW - Stars: pre-main-sequence
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U2 - 10.1086/497912
DO - 10.1086/497912
M3 - Article
AN - SCOPUS:30444440013
SN - 0004-637X
VL - 632
SP - L139-L142
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2 II
ER -