J/ApJ/636/932 Mid-infrared survey of T Tauri stars (McCabe+, 2006)
Investigating disk evolution: a high spatial resolution mid-infrared survey of
T Tauri stars.
McCabe C., Ghez A.M., Prato L., Duchene G., Fisher R.S., Telesco C.
<Astrophys. J., 636, 932-951 (2006)>
=2006ApJ...636..932M 2006ApJ...636..932M
ADC_Keywords: Stars, double and multiple ; Stars, pre-main sequence ;
Photometry, infrared
Keywords: binaries: close - circumstellar matter -
planetary systems: protoplanetary disks - stars: pre-main-sequence
Abstract:
We present a high spatial resolution, 10-20µm survey of 65 T Tauri
binary stars in Taurus, Ophiuchus, and Corona Australis using the Keck
10m telescopes. Designed to probe the inner ∼1AU region of the
circumstellar disks around the individual stellar components in these
binary systems, this study increases the number of binaries with
spatially resolved measurements at 10µm by a factor of ∼5.
Description:
High angular resolution mid-infrared observations were made at the
Keck 10m telescopes using two instruments: OSCIR, a visiting
mid-infrared (8-25µm) camera, and the Long Wavelength Spectrometer
(LWS), the facility mid-infrared imaging spectrograph.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 78 65 T Tauri binary sample
table3.dat 133 195 Observational results
table4.dat 108 71 Stellar component colors
refs.dat 159 15 References
--------------------------------------------------------------------------------
See also:
J/A+A/376/982 : Near-IR observations of young binaries (Woitas+, 2001)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Const Constellation
18- 33 A16 --- Name Object name
35 A1 --- m_Name Multiplicity index on Name
37- 40 F4.2 arcsec Sep Separation between components
41 A1 --- --- [/]
42- 46 F5.2 arcsec Sep2 ? Second value of separation
48- 49 I2 h RAh Hour of Right Ascension (J2000.0)
51- 52 I2 min RAm Minute of Right Ascension (J2000.0)
54- 57 F4.1 s RAs Second of Right Ascension (J2000.0)
59 A1 --- DE- Sign of the Declination (J2000.0)
60- 61 I2 deg DEd Degree of Declination (J2000.0)
63- 64 I2 arcmin DEm Arcminute of Declination (J2000.0)
66- 67 I2 arcsec DEs Arcsecond of Declination (J2000.0)
69- 78 A10 --- Ref References (1)
--------------------------------------------------------------------------------
Note (1): References, defined as follows:
1 = Ghez et al. 1993AJ....106.2005G 1993AJ....106.2005G
2 = Leinert et al. 1993A&A...278..129L 1993A&A...278..129L
3 = Simon et al. 1995ApJ...443..625S 1995ApJ...443..625S
4 = Ghez et al. 1997ApJ...490..353G 1997ApJ...490..353G
5 = Reipurth & Zinnecker 1993A&A...278...81R 1993A&A...278...81R
6 = Simon et al. 1996ApJ...469..890S 1996ApJ...469..890S
7 = Walter et al. 1988AJ.....96..297W 1988AJ.....96..297W
8 = Ghez et al. 1994, in ASP Conf. Ser. 56, Interacting Binary Stars,
ed. A.W. Shafter (San Francisco: ASP), 221
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Const Constellation
18- 33 A16 --- Name Object name
35- 39 A5 --- m_Name Multiplicity index on Name
41 A1 --- n_Name [ef] Individual notes (1)
43- 52 A10 "YYYY/MM/DD" ObsDate UT year of the observation
54- 58 A5 --- Filt Filter used (2)
60- 65 F6.3 arcsec Sep ? Separation
67- 71 F5.3 arcsec e_Sep ? Uncertainty in Sep
73- 77 F5.1 deg PA ? Position angle
79- 81 F3.1 deg e_PA ? Uncertainty in PA
83- 88 F6.3 --- Ratio ? Flux ratio F(A)/F(B)
90- 94 F5.3 --- e_Ratio ? Uncertainty in Ratio
96-101 F6.3 mag magA ? The Filt magnitude of the Primary
103-107 F5.3 mag e_magA ? Uncertainty in magA
109-114 F6.3 mag magB ? The Filt magnitude of the Secondary
116-120 F5.3 mag e_magB ? Uncertainty in magB
122-126 F5.2 mag magT ? The Filt magnitude of the Total (3)
128-131 F4.2 mag e_magT ? Uncertainty in mag
133 A1 --- f_magT [*cd] Flag on Totmag (4)
--------------------------------------------------------------------------------
Note (1): Note on Name, defined as follows:
e = A third object, situated 11.1" from NTTS155203-2338A at a position
angle of 164.4°, was observed at K band (12.2±0.2mag) and
L band (11.57±0.01mag). Given the preponderance of objects
within 1' of NTTS 155203-2338, this is likely to be a background
object but has not been confirmed.
f = A third object, located 16.5" away from DoAr 26 A at a position angle
of 49.3°, was also detected, with K=11.6±0.2mag and
L=11.6±0.8mag. It is not known whether this object is physically
associated with DoAr 26 or not.
Note (2): The filters used here are defined as follows:
12.5 = OCLI-S band (12.5µm ; F(Vega)=24.96Jy)
8.8 = OCLI-O band (8.8µm ; F(Vega)=49.26Jy)
IHW18 = IHW band (18.1µm ; F(Vega)=11.96Jy)
N = N band (10.8µm ; F(Vega)=33.99Jy)
K = K band (2.2µm)
L = L band (3.5µm)
SiC = SiC band (11.8µm ; Vega flux = 24.96Jy)
See Appendix B for details on the absolute photometric calibration.
Note (3): Represents the magnitude of both primary and secondary combined,
unless the value is starred. In this case, the observations reveal one
point source and it is not clear which component the flux belongs to.
Note (4): Flag on magT, defined as follows:
c = Chopping errors provide unresolved flux only.
d = Secondary marginally resolved in IRTF L-band observations causing
large uncertainties in fluxes from PSF fitting. Used L-band results
from White & Ghez (2001ApJ...556..265W 2001ApJ...556..265W) for final sample.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Name Object name
18 A1 --- m_Name Multiplicity index on Name
20 A1 --- f_Name [d] Flag on Name (1)
22- 26 A5 --- Comp Component
29- 32 F4.2 mag AV The V band extinction (2)
33 A1 --- f_AV Flag on AV (3)
35- 38 A4 --- SpType Spectral type
40- 44 F5.2 mag K-L The dereddened (K-L) color index
46- 49 F4.2 mag e_K-L Uncertainty in K-L
51- 55 F5.2 mag K-N The dereddened (K-[N]) color index
57- 60 F4.2 mag e_K-N Uncertainty in K-N
62- 63 I2 --- r_Nmag The MIR (N bands) reference (4)
65 A1 --- r_Kmag The NIR (K band) reference(s) (4)
67 A1 --- r_Lmag The NIR (L band) reference(s) (4)
69- 78 A10 --- Line Emission line present
80- 84 F5.1 0.1nm EWHa ? The Hα equivalent width in Angstroms
86- 88 A3 --- TTcl The T Tau class (I, II or III)
90 A1 --- TTt [CW] The T Tauri type: Classical or Weak
92 A1 --- f_TTt [c] Borderline case on TTt (5)
94-100 A7 --- r_Line Line emission and spectral type reference(s) (4)
102-108 A7 --- Notes Additional notes
--------------------------------------------------------------------------------
Note (1): A "d" indicates that ROX 15 flickers in accretion; Prato et al.
(2003ApJ...584..853P 2003ApJ...584..853P) see no Brγ in either component, whereas
Greene & Meyer (1995ApJ...450..233G 1995ApJ...450..233G) and Luhman & Rieke
(1999ApJ...525..440L 1999ApJ...525..440L) do see Brγ in resolved system. Went with
C/C because system seen to be accreting at least on some occasions.
Note (2): Measured from photometry for combined system.
Note (3): A "]" indicates an assumed extinction of 0.0mag in cases where
J-H and H-K colors fall below the CTTS (Classical T Tau star) locus.
Note (4): Note that the reference numbers differ from the printed version.
Note (5): A "c" indicates that Hartigan & Kenyon (2003ApJ...583..334H 2003ApJ...583..334H) find
an EWHa=23±4Å, on the border between CTTS/WTTS (classical/weak).
Based on this, the lack of veiling and [OI] emission, and NIR excess,
they define it to be a WTTS. We use their classification here.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Ref Reference number
4- 22 A19 --- Bibcode Bibcode
24- 48 A25 --- Aut Author's name
50-159 A110 --- Com Comment
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 29-Dec-2006