J/AJ/157/144 Protoplanetary disk masses in Taurus (Ballering+, 2019)
Protoplanetary disk masses from radiative transfer modeling: a case study
in Taurus.
Ballering N.P., Eisner J.A.
<Astron. J., 157, 144 (2019)>
=2019AJ....157..144B 2019AJ....157..144B (SIMBAD/NED BibCode)
ADC_Keywords: Star Forming Region ; Stars, double and multiple ;
Spectra, infrared ; Spectra, millimetric/submm ; Morphology
Keywords: circumstellar matter - planetary systems
Abstract:
Measuring the masses of protoplanetary disks is crucial for understanding
their planet-forming potential. Typically, dust masses are derived from
(sub-)millimeter flux density measurements plus assumptions for the
opacity, temperature, and optical depth of the dust. Here we use radiative
transfer models to quantify the validity of these assumptions with the aim
of improving the accuracy of disk dust mass measurements. We first carry
out a controlled exploration of disk parameter space. We find that the disk
temperature is a strong function of disk size, while the optical depth
depends on both disk size and dust mass. The millimeter-wavelength spectral
index can be significantly shallower than the naive expectation due to
a combination of optical depth and deviations from the Rayleigh-Jeans
regime. We fit radiative transfer models to the spectral energy
distributions (SEDs) of 132 disks in the Taurus-Auriga region using a
Markov chain Monte Carlo approach. We used all available data to produce
the most complete SEDs used in any extant modeling study. We perform the
fitting twice: first with unconstrained disk sizes and again imposing the
disk size-brightness relation inferred for sources in Taurus. This
constraint generally forces the disks to be smaller, warmer, and more
optically thick. From both sets of fits, we find disks to be ∼1-5 times
more massive than when derived using (sub-)millimeter measurements and
common assumptions. With the uncertainties derived from our model fitting,
the previously measured dust mass-stellar mass correlation is present
in our study but only significant at the 2σ level.
Description:
We used the photometry for each target provided by Andrews et al. (2013,
J/ApJ/771/129). To this, we added additional measurements from the
literature, primarily at far-IR and (sub-)millimeter wavelengths. These
new data are listed in Table 2. We adopted the sample of class II sources
in Taurus from Andrews et al. (2013, J/ApJ/771/129), which they argued
was fairly complete. This totaled 178 systems. For the stellar properties
(T*, L*), we used the best-fit values from Table 4 of Andrews et al.
(2013, J/ApJ/771/129). We fit models to 132 disks from the original sample
of 178. To explore the effects of the model parameters, we constructed
a fiducial model and varied each parameter individually from its fiducial
value. The fiducial model has Mdust=10-4 M☉, rin=0.1 au,
rc=100 au, H100=10 au, β=1.15, amax=104 µm, q=3.5, and
i=40°. We fixed the stellar parameters to T*=3500 K and
L*=0.5 L☉.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 279 132 Fit results (without size constraint)
table4.dat 279 132 Fit results (with size constraint)
table2.dat 113 613 Additional SED data
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See also:
J/ApJ/636/932 : Mid-infrared survey of T Tauri stars (McCabe+, 2006)
J/ApJ/703/1964 : Spectra of three nearby star-forming regions (Furlan+, 2009)
J/ApJ/720/480 : DISCS. I. Taurus protoplanetary disk data (Oberg+, 2010)
J/ApJS/186/111 : Spitzer observations of Taurus members (Luhman+, 2010)
J/ApJS/186/259 : Taurus Spitzer survey: new candidate members (Rebull+, 2010)
J/ApJ/751/115 : Millimeter emission from Taurus binary systems (Harris+, 2012)
J/ApJ/771/129 : Submillimetric Class II sources of Taurus (Andrews+, 2013)
J/ApJ/784/62 : Circumstellar disks around binary stars in Taurus
(Akeson+, 2014)
J/ApJ/849/63 : FIR-mm data of YSOs in star-forming regions (Ribas+, 2017)
Byte-by-byte Description of file: table3.dat table4.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- ID Target identifier
21- 21 A1 --- f_ID [*] Flag on ID (1)
23- 27 F5.2 [Msun] logMd [-6.67/-2.69] Log dust mass
29- 34 F6.4 [Msun] E_logMd [0.0261/3.46] Upper uncertainty in logMd
36- 41 F6.4 [Msun] e_logMd [0.0387/4.54] Lower uncertainty in logMd
43- 49 F7.4 [AU] logRin [-2.52/0.958] Log inner edge radius
51- 56 F6.4 [AU] E_logRin [0.0387/2.25] Upper uncertainty in logRin
58- 63 F6.4 [AU] e_logRin [0.0489/2.07] Lower uncertainty in logRin
65- 69 F5.3 [AU] logRc [0.708/3.76] Log characteristic size
71- 76 F6.4 [AU] E_logRc [0.0232/3] Upper uncertainty in logRc
78- 84 F7.5 [AU] e_logRc [0.00923/2.95] Lower uncertainty in logRc
86- 90 F5.2 AU H100 [2.32/31.4] Scale height at 100 AU
92- 97 F6.3 AU E_H100 [0.406/14.2] Upper uncertainty in H100
99-104 F6.3 AU e_H100 [0.404/14.2] Lower uncertainty in H100
106-109 F4.2 --- beta [1.01/1.37] The flaring parameter β
111-117 F7.5 --- E_beta [0.00583/0.257] Upper uncertainty in beta
119-125 F7.5 --- e_beta [0.0056/0.193] Lower uncertainty in beta
127-130 F4.2 [um] logamax [1.07/6.06] Log maximum grain radius
132-136 F5.3 [um] E_logamax [0.267/5.56] Upper uncertainty logamax
138-142 F5.3 [um] e_logamax [0.133/4.25] Lower uncertainty logamax
144-147 F4.2 --- q [1.32/6.89] Power law distribution exponent
149-154 F6.4 --- E_q [0.0588/3.68] Upper uncertainty in q
156-161 F6.4 --- e_q [0.0575/4.13] Lower uncertainty in q
163-167 F5.2 deg i [8.24/73.3] Inclination
169-173 F5.2 deg E_i [1.35/35.2] Upper uncertainty in i
175-179 F5.2 deg e_i [2.19/35.2] Lower uncertainty in i
181-186 F6.4 cm2/g kappa [0.0151/5.88] Dust opacity κ
188-196 F9.7 cm2/g E_kappa [2.02e-05/5.29] Upper uncertainty in kappa
198-208 F11.9 cm2/g e_kappa [3e-07/3.49] Lower uncertainty in kappa
210-215 F6.2 K Tdust [4.49/117] Dust temperature
217-222 F6.3 K E_Tdust [0.596/93.5] Upper uncertainty in Tdust
224-229 F6.3 K e_Tdust [0.565/97.1] Lower uncertainty in Tdust
231-236 F6.4 --- Fnu/th [0.0507/1] Ratio of model flux density to
perfectly optically thin Fν/Fν,thin
238-244 F7.5 --- E_Fnu/th [0.00276/0.831] Upper uncertainty in Fnu/th
246-251 F6.4 --- e_Fnu/th [0.0129/0.808] Lower uncertainty in Fnu/th
253-258 F6.3 --- Md/ana [0.257/49.7] Ratio of true dust mass to model
Mdust/Mdust,ana (2)
260-270 F11.4 --- E_Md/ana [0.0314/138000] Upper uncertainty in Md/ana
272-279 F8.5 --- e_Md/ana [0.0208/48.4] Lower uncertainty in Md/ana
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Note (1): Flag as follows:
* = Target did not have a good fit and was excluded from our demographic
analysis.
Note (2): The mass derived from the flux density of the model disk at 1300 µm
using equations 1 (Mdust,ana=(Fνd2)/(κBν(Tdust,ana)))
and 2 (Tdust,ana=25(L*/L☉)1/4K) and κ=2.3 cm2/g.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 20 A20 --- ID Target identifier
22- 25 I4 um lambda [10/3330] Wavelength λ
27 A1 --- l_Flux [<] Limit flag on Flux
28- 36 F9.2 mJy Flux [0.18/137740] Flux density at λ
38- 44 F7.2 mJy e_Flux [0/2400]? Statistical 1σ uncertainty in
Flux
46- 47 I2 % Cal [0/20]? Calibration 1σ uncertainty in Flux
(1)
49- 62 A14 --- Inst Instrument used
64- 93 A30 --- Ref Reference
95-113 A19 --- Bibcode Bibcode of the reference (2)
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Note (1): This column gives the systematic or calibration uncertainty on the
flux density, and is an independent source of uncertainty from the statistical
uncertainty.
Note (2): See Marton et al. (2017arXiv170505693M 2017arXiv170505693M) for details regarding the PACS
Point Source Catalog and Schulz et al. (2017arXiv170600448S 2017arXiv170600448S) for details
regarding the SPIRE Point Source Catalog.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 08-Jul-2019