J/ApJ/771/129 Submillimetric Class II sources of Taurus (Andrews+, 2013)
The mass dependence between protoplanetary disks and their stellar hosts.
Andrews S.M., Rosenfeld K.A., Kraus A.L., Wilner D.J.
<Astrophys. J., 771, 129 (2013)>
=2013ApJ...771..129A 2013ApJ...771..129A
ADC_Keywords: Photometry, millimetric/submm ; Stars, ages ; Stars, masses ;
Stars, double and multiple ; Spectral types
Keywords: protoplanetary disks; submillimeter: planetary systems
Abstract:
We present a substantial extension of the millimeter (mm) wave
continuum photometry catalog for circumstellar dust disks in the
Taurus star-forming region, based on a new "snapshot" λ=1.3mm
survey with the Submillimeter Array. Combining these new data with
measurements in the literature, we construct a mm-wave luminosity
distribution, f(Lmm), for Class II disks that is statistically
complete for stellar hosts with spectral types earlier than M8.5 and
has a 3σ depth of roughly 3mJy. The resulting census eliminates
a longstanding selection bias against disks with late-type hosts, and
thereby demonstrates that there is a strong correlation between Lmm
and the host spectral type. By translating the locations of individual
stars in the Hertzsprung-Russell diagram into masses and ages, and
adopting a simple conversion between Lmm and the disk mass, Md, we
confirm that this correlation corresponds to a statistically robust
relationship between the masses of dust disks and the stars that host
them. A Bayesian regression technique is used to characterize these
relationships in the presence of measurement errors, data censoring,
and significant intrinsic scatter: the best-fit results indicate a
typical 1.3mm flux density of ∼25mJy for 1M☉ hosts and a
power-law scaling Lmm∝M*1.5-2.0. We suggest that a
reasonable treatment of dust temperature in the conversion from Lmm
to Md favors an inherently linear Md∝M* scaling, with a
typical disk-to-star mass ratio of ∼0.2%-0.6%. The measured rms
dispersion around this regression curve is ±0.7dex, suggesting that
the combined effects of diverse evolutionary states, dust opacities,
and temperatures in these disks imprint a full width at half-maximum
range of a factor of ∼40 on the inferred Md (or Lmm) at any given
host mass.
Description:
The infrared-selected Luhman et al. catalog (2010ApJS..186..111L 2010ApJS..186..111L) of
Tau-Aur Class II sources is used as the basis of our sample: it
includes 179 young stellar "systems" composed of 227 (known)
individual stars with spectral types from B8 to M9.
We observed 52 new targets with the Submillimeter Array (SMA) at
225.5GHz (1.33mm) in its compact configuration (8-70m baselines) over
six tracks from 2012 November to 2013 February.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 84 210 Millimeter-wave continuum photometry catalog
table3.dat 130 212 Stellar host masses and ages
table4.dat 62 224 Stellar spectrum fitting results
refs.dat 263 21 References
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See also:
II/297 : AKARI/IRC mid-IR all-sky Survey (ISAS/JAXA, 2010)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/ApJ/751/115 : Mm emission from Taurus binary systems (Harris+, 2012)
J/MNRAS/411/435 : Stellar parameters and extinction (Bailer-Jones, 2011)
J/ApJ/731/8 : Multiple star formation in Taurus-Auriga (Kraus+, 2011)
J/ApJ/724/835 : The Spitzer c2d survey of WTTSs. III. (Wahhaj+, 2010)
J/ApJ/720/480 : DISCS. I. Taurus protoplanetary disk data (Oberg+, 2010)
J/ApJS/186/259 : Taurus Spitzer survey: new candidate members (Rebull+, 2010)
J/ApJ/703/1511 : Wide binaries in Taurus and Upper Sco (Kraus+, 2009)
J/ApJ/693/L81 : Extinction in star-forming regions (McClure, 2009)
J/A+A/479/827 : UBVR light curves of weak-line T Tauri stars (Grankin+, 2008)
J/A+A/468/379 : XMM Optical Monitor Survey of TMC (Audard+, 2007)
J/A+A/461/183 : Variability of classical T Tauri (Grankin+, 2007)
J/ApJ/662/413 : 2MASS survey of wide multiplicity in 3 assoc. (Kraus+, 2007)
J/AJ/132/2665 : QUEST2 BRI photometry of Taurus-Auriga PMS (Slesnick+, 2006)
J/A+A/446/485 : New very low-mass members in Taurus (Guieu+, 2006)
J/ApJ/636/932 : Mid-infrared survey of T Tauri stars (McCabe+, 2006)
J/AJ/129/2294 : RVs of weak-lines T Tauri stars (Massarotti+, 2005)
J/AJ/129/1049 : Mm and sub-mm obs. of solar-type stars (Carpenter+, 2005)
J/AJ/126/2971 : UBVRI photometry of 131 Herbig Ae/Be (Vieira+, 2003)
J/A+A/380/609 : Southern emission-line star multiphotometry (de Winter+, 2001)
J/A+A/376/982 : Near-IR observations of young binaries (Woitas+, 2001)
J/A+A/337/403 : Low-mass stars evolutionary models (Baraffe+ 1998)
J/A+A/299/89 : COYOTES II (Bouvier+, 1995)
J/A+A/297/391 : T Tauri stars ROSAT survey (Neuhaeuser+, 1995)
J/ApJS/101/117 : UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995)
J/A+A/281/161 : Radio emission from stars at 250GHz (Altenhoff+, 1994)
J/A+AS/101/485 : Multisite UBVRI photometry in Tau-Aur cloud (Bouvier+ 1993)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Name Name
21 A1 --- f_Name [e] Note for V807 Tau B (1)
23- 38 A16 --- SpT MK spectral type(s) (2)
40- 45 A6 --- r_SpT Reference(s) or "est"imated flag (3)
47 A1 --- l_F0.89 3σ upper limit flag on F0.89
49- 54 F6.4 Jy F0.89 [0.001/1.4] 0.89mm flux (338GHz)
56- 61 F6.4 Jy e_F0.89 [0.001/0.2]? F0.89 uncertainty
63 A1 --- l_F1.3 3σ upper limit flag on F1.3
65- 70 F6.4 Jy F1.3 [0.001/0.5] 1.3mm flux (225GHz)
72- 77 F6.4 Jy e_F1.3 [0.0004/0.04]? F1.3 uncertainty
79- 84 A6 --- Notes Notes (4)
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Note (1):
e = The companions V807 Tau B (itself a binary) and V710 Tau B have no
observational disk signatures, and are therefore excluded from this
Class II sample. The V807 Tau system has no resolved mm-wave measurement,
but we associate all of the composite emission with the primary
component. Harris et al. (2012, J/ApJ/751/115) found no mm-wave emission
associated with V710 Tau B.
Note (2): Unless otherwise specified, the assumed spectral type uncertainty
is ±1 subclass.
Note (3): The spectral classifications were collated from the references listed
in refs.dat file. The classifications for FT Tau, ITG 1, and
IRAS 04370+2559 are unknown: we adopt the wide spectral type bins
advocated by Luhman et al. (2010ApJS..186..111L 2010ApJS..186..111L), listed here in
parenthesis.
Note (4): The "m" and "e" flags denote whether each source has a flux density
measurement available at (or near) 0.89 and 1.3mm: "m" implies direct
measurement and "e" implies an extrapolation as described in the text.
Notes in parenthesis indicate unresolved multiple systems where
composite measurements were applied to the primaries, and upper
limits to the secondaries (see Section 3.1).
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Name Name
22 A1 --- f_Name [ab] Flag on Name (1)
24- 28 F5.2 [Msun] logM* [-2.1/0.9] Log of stellar mass from DM97 (2)
30- 34 F5.2 [Msun] b_logM* [-2.2/0.8] Lower value of logM* (3)
36- 40 F5.2 [Msun] B_logM* [-1.7/1.1] Upper value of logM* (3)
42- 46 F5.2 [Myr] logt* [-1.6/1.7] Log of stellar age from DM97 (2)
48- 52 F5.2 [Myr] b_logt* [-2.5/1.1] Lower value of logt* (3)
54- 58 F5.2 [Myr] B_logt* [-1.3/1.9] Upper value of logt* (3)
60- 64 F5.2 [Msun] logM*2 [-2/1.5] Log of stellar mass from BCAH98 (2)
66- 70 F5.2 [Msun] b_logM*2 [-2.5/1.1] Lower value of logM*2 (3)
72- 76 F5.2 [Msun] B_logM*2 [-1.7/1.7] Upper value of logM*2 (3)
78- 82 F5.2 [Myr] logt*2 [-2.6/1.6] Log of stellar age from BCAH98 (2)
84- 88 F5.2 [Myr] b_logt*2 [-2.8/1.4] Lower value of logt*2 (3)
90- 94 F5.2 [Myr] B_logt*2 [-0.9/1.9] Lower value of logt*2 (3)
96-100 F5.2 [Msun] logM*3 [-2.1/0.9] Log of stellar mass from SDF00 (2)
102-106 F5.2 [Msun] b_logM*3 [-2.4/0.8] Lower value of logM*3 (3)
108-112 F5.2 [Msun] B_logM*3 [-1.6/1] Upper value of logM*3 (3)
114-118 F5.2 [Myr] logt*3 [-2.1/1.7] Log of stellar age from SDF00 (2)
120-124 F5.2 [Myr] b_logt*3 [-2.4/1.1] Lower value of logt*3 (3)
126-130 F5.2 [Myr] B_logt*3 [-0.6/1.9] Upper value of logt*3 (3)
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Note (1): Flag as follows:
a = The logM* values (and their confidence intervals) in these composite
multiple systems were determined by properly combining the marginal
probability density functions determined for their individual components,
as described in the text. The corresponding logt* values (and their
confidence intervals) correspond to the primary components.
b = These systems are either known or strongly suspected to be associated
with nearly edge-on disks. Since such a viewing geometry substantially
obscures the starlight, the derived estimates of L* for these cases are
not used to determine masses and ages. Instead, we compute the weighted
mean and standard deviation of the luminosities for the ensemble of
sources with the same spectral type (±1 subclass), and associate them
with L* and σL in the Bayesian inference method for
{M*, t*}: details are available in Appendix B.
Note (2): References as below:
DM97 = D'Antona & Mazzitelli 1997MmSAI..68..807D 1997MmSAI..68..807D
BCAH98 = Baraffe et al. 1998, J/A+A/337/403
SDF00 = Siess et al. 2000A&A...358..593S 2000A&A...358..593S
Note (3): Confidence intervals represent the extreme values of the variable that
span its 68.2% ("1σ") confidence interval, derived from its
associated marginal probability density function (see Section 3.2.1).
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Name Name
22- 24 A3 --- f_Name [abc, ] Flag on Name (1)
26- 31 F6.4 [K] logT* [3.3/4.1] log of stellar temperature
33- 38 F6.4 [K] e_logT* [0.01/0.2] logT* uncertainty
40- 45 F6.3 [Lsun] logL* [-3/2.2] log of stellar luminosity
47- 51 F5.3 [Lsun] e_logL* [0.03/0.9] logL* uncertainty
53- 57 F5.2 mag Av [0/28.2] Extinction
59- 62 F4.2 mag e_Av [0.2/3.3] Av uncertainty
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Note (1): Flag as follows:
a = The stellar parameters for these close pairs were determined by
simultaneous fits to both their composite SEDs and any available
contrast ratios, assuming that both components have the same extinction.
b = These stars are known or suspected to host edge-on disks. The
luminosities and extinctions reported here are the results of the formal
measurements described in Appendix B. However, their L* values are
modified before use in Section 3.2, as described in the text.
c = The components V807 Tau Bab and V710 Tau B are included here for
completeness, but are not considered part of the Class II sample. The
stellar photosphere parameters listed here were used to subtract off
their contribution to the composite SEDs shown in Appendix B.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- Ref Reference code
5- 23 A19 --- BibCode Bibcode
25- 43 A19 --- Aut Author's name(s)
45-263 A219 --- Comm Comment
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 26-Jan-2015