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J/ApJ/847/31    Protoplanetary disk data in Cha I and Lupus    (Mulders+, 2017)

Constraints from dust mass and mass accretion rate measurements on angular momentum transport in protoplanetary disks. Mulders G.D., Pascucci I., Manara C.F., Testi L., Herczeg G.J., Henning T., Mohanty S., Lodato G. <Astrophys. J., 847, 31 (2017)> =2017ApJ...847...31M
ADC_Keywords: Accretion; Stars, masses; Spectral types; YSOs; Molecular clouds Keywords: accretion, accretion disks ; planets and satellites: formation ; protoplanetary disks ; stars: low-mass Abstract: In this paper, we investigate the relation between disk mass and mass accretion rate to constrain the mechanism of angular momentum transport in protoplanetary disks. We find a correlation between dust disk mass and mass accretion rate in Chamaeleon I with a slope that is close to linear, similar to the one recently identified in Lupus. We investigate the effect of stellar mass and find that the intrinsic scatter around the best-fit Mdust-M* and dMacc/dt-M* relations is uncorrelated. We simulate synthetic observations of an ensemble of evolving disks using a Monte Carlo approach and find that disks with a constant α viscosity can fit the observed relations between dust mass, mass accretion rate, and stellar mass but overpredict the strength of the correlation between disk mass and mass accretion rate when using standard initial conditions. We find two possible solutions. In the first one, the observed scatter in Mdust and dMacc/dt is not primordial, but arises from additional physical processes or uncertainties in estimating the disk gas mass. Most likely grain growth and radial drift affect the observable dust mass, while variability on large timescales affects the mass accretion rates. In the second scenario, the observed scatter is primordial, but disks have not evolved substantially at the age of Lupus and Chamaeleon I owing to a low viscosity or a large initial disk radius. More accurate estimates of the disk mass and gas disk sizes in a large sample of protoplanetary disks, through either direct observations of the gas or spatially resolved multiwavelength observations of the dust with ALMA, are needed to discriminate between both scenarios or to constrain alternative angular momentum transport mechanisms such as MHD disk winds. Description: We perform a homogeneous analysis of the dust disk mass, mass accretion rate, and stellar mass in the Chamaeleon I and Lupus star-forming regions. All observational data used in this analysis were previously published; the ALMA data surveys of disk masses were presented by Ansdell+ (2016, J/ApJ/828/46) and Pascucci+ (2016, J/ApJ/831/125); the X-Shooter surveys of mass accretion rates were presented by Alcala+ (2014, J/A+A/561/A2 ; 2017, J/A+A/600/A20) and Manara+ (2014A&A...568A..18M ; 2016A&A...585A.136M and 2017, arXiv:1704.02842). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 119 174 Stellar and disk properties for Chamaeleon I and Lupus
See also: J/A+A/452/245 : Near-IR photometry of PMS stars in rho Oph (Natta+, 2006) J/A+A/504/461 : YSOs in L1630N and L1641 (Fang+, 2009) J/ApJ/710/597 : Accretion in disks in Cep OB2 (Sicilia-Aguilar+, 2010) J/ApJ/771/129 : Submillimetric Class II sources of Taurus (Andrews+, 2013) J/ApJS/207/5 : YSOs in LDN 1641 with Hectochelle spectra (Fang+, 2013) J/A+A/561/A2 : 36 accreting YSOs emission lines (Alcala+, 2014) J/A+A/570/A82 : Mapping accretion variability in NGC 2264 (Venuti+, 2014) J/ApJ/814/130 : Planet occurrence rates calculated for KOIs (Mulders+, 2015) J/A+A/581/A66 : UV variability and accretion in NGC 2264 (Venuti+, 2015) J/ApJ/828/46 : ALMA survey of Lupus protoplanetary disks. I. (Ansdell+, 2016) J/ApJ/831/125 : ALMA 887um obs. of ChaI star-forming region (Pascucci+, 2016) J/A+A/592/A49 : TW Hya CO(2-1), CN(2-1) and CS(5-4) data cubes (Teague+, 2016) J/A+A/600/A20 : Lupus YSOs X-shooter spectroscopy (Alcala+, 2017) J/ApJ/841/116 : Herschel spectra of 11 very low mass stars (Hendler+, 2017) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 23 A23 --- ID Identifier, 2MASS J or other star name 25- 29 A5 --- SpT MK spectral type 31- 34 I4 K Teff [0/5110]? Stellar effective temperature 36- 40 F5.2 [Lsun] logL [-2.7/0.8]? log of stellar luminosity 42- 46 F5.2 [Rsun] logR [-0.9/0.6]? log of stellar radius 48- 52 F5.2 [Msun] logM [-1.6/0.3]? log of stellar mass 54- 57 F4.2 [Msun] e_logM [0.04/0.4]? Uncertainty in logM 59- 64 F6.2 [Lsun] logLacc [-5.3/0.7]? Log of accretion luminosity 66- 70 F5.2 [Mgeo] logMdust [-0.9/2.7]? Log of dust mass 72- 77 F6.4 [Mgeo] e_logMdust [0.0003/0.2]? Uncertainty in logMdust 79- 83 A5 --- Det [True /False] Source is detected in dust continuum emission (>3σ) 85- 91 F7.2 [Msun/yr] logMacc [-12.3/-6.6]? log of mass accretion rate 93- 96 F4.2 [Msun/yr] e_logMacc [0.2/0.5] Uncertainty in logMacc 98-102 A5 --- Det2 [True /False] Accretion luminosity > expected chromospheric emission 104-109 A6 --- Reg Region: Chamaeleon I (ChaI) or Lupus 111-119 A9 --- Exc Exclude? (1)
Note (1): Reason why sources are not included in analysis as follows: underlum = sub-luminous, lying below the ZAMS on HR diagram or known edge-on disk (9 occurrences); binary = apparent binary (1 occurrence); faint = source not detected with VLT/X-shooter (4 occurrences); noMdust = no dust mass measurement (14 occurrences); notinslit = source not in VLT/X-shooter slit (1 occurrence);
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 28-May-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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