J/AJ/155/47 VRIJHK photometry of the T Tauri binary KH 15D (Aronow+, 2018)
Optical and radio observations of the T Tauri binary KH 15D (V582 Mon): stellar
properties, disk mass limit, and discovery of a CO outflow.
Aronow R.A., Herbst W., Hughes A.M., Wilner D.J., Winn J.N.
<Astron. J., 155, 47 (2018)>
=2018AJ....155...47A 2018AJ....155...47A (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Stars, pre-main sequence ;
Stars, variable ; Photometry, UBVRIJKLMNH
Keywords: binaries: close - ISM: jets and outflows -
open clusters and associations: individual (NGC 2264) -
stars: individual (KH 15D) - stars: pre-main sequence
Abstract:
We present VRIJHK photometry of the KH 15D T Tauri binary system for
the 2015/2016 and 2016/2017 observing seasons. For the first time in
the modern (CCD) era, we are seeing Star B fully emerge from behind
the trailing edge of the precessing circumbinary ring during each
apastron passage. We are, therefore, able to measure its luminosity
and color. Decades of photometry on the system now allow us to infer
the effective temperature, radius, mass, and age of each binary
component. We find our values to be in good agreement with previous
studies, including archival photographic photometry from the era when
both stars were fully visible, and they set the stage for a full model
of the system that can be constructed once radial velocity
measurements are available. We also present the first high-sensitivity
radio observations of the system, taken with the Atacama Large
Millimeter/submillimeter Array and the Submillimeter Array. The
respective 2.0 and 0.88 mm observations provide an upper limit on the
circumbinary (gas and dust) disk mass of 1.7 MJup and reveal an
extended CO outflow, which overlaps with the position, systemic
velocity, and orientation of the KH 15D system and is certainly
associated with it. The low velocity, tight collimation, and extended
nature of the emission suggest that the outflow is inclined nearly
orthogonal to the line of sight, implying it is also orthogonal to the
circumbinary ring. The position angle of the radio outflow also agrees
precisely with the direction of polarization of the optical emission
during the faint phase. A small offset between the optical image of
the binary and the central line of the CO outflow remains a puzzle and
possible clue to the jet launching mechanism.
Description:
For convenience, we have compiled in Table 1 all of the high-quality
(CCD) photometry of KH 15D that has been obtained since 1995
(Hamilton et al. 2005AJ....130.1896H 2005AJ....130.1896H; Kusakabe et al. 2005ApJ...632L.139K 2005ApJ...632L.139K;
Windemuth & Herbst 2014, J/AJ/147/9; Arulanantham et al.
2017ApJ...834..119A 2017ApJ...834..119A). The previously unpublished data, spanning the
interval 2015 September to 2017 March, were obtained with the ANDICAM
instrument on the 1.3 m telescope at Cerro-Tololo Inter-American
Observatory (CTIO), operated by the SMARTS consortium. KH 15D was
observed nightly during each observing season in three optical filters
(VRI) and three near-IR filters (JHK). These data are obtained within
an interval of about 30 minutes and combined to yield a single nightly
magnitude in each color. The observing and reduction process is
identical to what has been used for many years and is described in
more detail by Windemuth & Herbst (2014, J/AJ/147/9).
Objects:
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RA (ICRS) DE Designation(s)
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06 41 10.31 +09 28 33.2 KH 15D = V* V582 Mon
06 40 58 +09 53.7 NGC 2264 = NAME XMAS TREE CL
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 91 9211 VRIJHK Photometry of KH 15D
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See also:
J/AJ/114/2644 : UBVRIHa photometry of NGC2264 (Sung+, 1997)
J/AJ/138/963 : Rotation of NGC 2264 members (Baxter+, 2009)
J/AJ/140/2025 : KH 15D (V582 Mon) VI light curves (Herbst+, 2010)
J/AJ/147/9 : VRIJHK light curves of V582 Mon (Windemuth+, 2014)
J/AJ/147/82 : Monitoring of disk-bearing stars in NGC 2264 (Cody+, 2014)
J/AJ/151/90 : Spitzer and VRIJHK photometry of V582 Mon (Arulanantham+, 2016)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 F10.2 d JD Julian date of observation
12- 16 F5.2 mag Vmag [15.4/21.74]?=99.99 The V band magnitude
18- 22 F5.3 mag e_Vmag [0/1.624]?=9.999 The 1σ error in Vmag
24- 28 F5.2 mag Rmag [14.67/19.39]?=99.99 The R band magnitude
30- 34 F5.3 mag e_Rmag [0.003/0.289]?=9.999 The 1σ error in Rmag
36- 40 F5.2 mag Imag [14.01/19.79]?=99.99 The I band magnitude
42- 46 F5.3 mag e_Imag [0.001/1.09]?=9.999 The 1σ error in Imag
48- 52 F5.2 mag Jmag [13.17/18.33]?=99.99 The J band magnitude
54- 58 F5.3 mag e_Jmag [0/0.305]?=9.999 The 1σ error in Jmag
60- 64 F5.2 mag Hmag [12.43/19.99]?=99.99 The H band magnitude
66- 70 F5.3 mag e_Hmag [0/0.281]?=9.999 The 1σ error in Hmag
72- 76 F5.2 mag Kmag [12.22/19.53]?=99.99 The K band magnitude
78- 82 F5.3 mag e_Kmag [0.01/2.746]?=9.999 The 1σ error in Kmag
84- 87 A4 --- Obs Observatory code (1)
89- 91 A3 --- Ref Reference code (2)
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Note (1): Observatory code as follows:
IRSF = 1.4 m Infrared Survey Facility telescope, Sutherland, South Africa;
ESO = European Southern Observatory, La Silla, Chile;
CTIO = Cerro Tololo Inter-American Observatory SMARTS 1.3 m telescope ANDICAM;
KAIT = Katzman Automated Telescope, Mt. Hamilton, CA;
KONK = Konkoly Observatory, Hungary;
KPNO = Kitt Peak National Observatory telescopes;
MMO = Morgan-Monroe Observatory of Indiana University;
TEN = Tenagra Observatory, Nogales, AZ;
TENE = Teide Observatory, Tenerife, Spain;
USNO = US Naval Observatory's 1.3m and 1m telescopes;
UZBK = Mount Maidanak Observatory, Uzbekistan;
VVO = Van Vleck Observatory, Middletown, CT;
WISE = Wise Observatory, Israel.
Note (2): Reference code as follows:
H05 = Hamilton et al. (2005AJ....130.1896H 2005AJ....130.1896H);
H10 = Herbst et al. (2010, J/AJ/140/2025);
K05 = Kusakabe et al. (2005ApJ...632L.139K 2005ApJ...632L.139K);
W13 = Windemuth & Herbst (2014, J/AJ/147/9);
A16 = Arulanantham et al. (2017ApJ...834..119A 2017ApJ...834..119A);
A17 = This Paper.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 26-Sep-2018