2020A&A...640A..19T


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.26CET14:36:05

2020A&A...640A..19T - Astronomy and Astrophysics, volume 640A, 19-19 (2020/8-1)

Dust masses of young disks: constraining the initial solid reservoir for planet formation.

TYCHONIEC L., MANARA C.F., ROSOTTI G.P., VAN DISHOECK E.F., CRIDLAND A.J., HSIEH T.-H., MURILLO N.M., SEGURA-COX D., VAN TERWISGA S.E. and TOBIN J.J.

Abstract (from CDS):


Context. Recent years have seen building evidence that planet formation starts early, in the first ∼0.5Myr. Studying the dust masses available in young disks enables us to understand the origin of planetary systems given that mature disks are lacking the solid material necessary to reproduce the observed exoplanetary systems, especially the massive ones.
Aims. We aim to determine if disks in the embedded stage of star formation contain enough dust to explain the solid content of the most massive exoplanets.
Methods. We use Atacama Large Millimeter/submillimeter Array (ALMA) Band 6 (1.1-1.3mm) continuum observations of embedded disks in the Perseus star-forming region together with Very Large Array (VLA) Ka-band (9mm) data to provide a robust estimate of dust disk masses from the flux densities measured in the image plane.
Results. We find a strong linear correlation between the ALMA and VLA fluxes, demonstrating that emission at both wavelengths is dominated by dust emission. For a subsample of optically thin sources, we find a median spectral index of 2.5 from which we derive the dust opacity index β=0.5, suggesting significant dust growth. Comparison with ALMA surveys of Orion shows that the Class I dust disk mass distribution between the two regions is similar, but that the Class 0 disks are more massive in Perseus than those in Orion. Using the DIANA opacity model including large grains, with a dust opacity value of κ9mm=0.28cm2/g, the median dust masses of the embedded disks in Perseus are 158M for Class 0 and 52M for Class I from the VLA fluxes. The lower limits on the median masses from ALMA fluxes are 47M and 12M for Class 0 and Class I, respectively, obtained using the maximum dust opacity value κ1.3mm=2.3cm2/g. The dust masses of young Class 0 and I disks are larger by at least a factor of ten and three, respectively, compared with dust masses inferred for Class II disks in Lupus and other regions.
Conclusions. The dust masses of Class 0 and I disks in Perseus derived from the VLA data are high enough to produce the observed exoplanet systems with efficiencies acceptable by planet formation models: the solid content in observed giant exoplanets can be explained if planet formation starts in Class 0 phase with an efficiency of ∼15%. A higher efficiency of ∼30% is necessary if the planet formation is set to start in Class I disks.

Abstract Copyright: © ESO 2020

Journal keyword(s): protoplanetary disks - planets and satellites: formation - instrumentation: interferometers - stars: formation - submillimeter: ISM - planets and satellites: gaseous planets

CDS comments: Tables A.1 and A.2 not in SIMBAD.

Simbad objects: 19

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Number of rows : 19

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 4C 28.07 QSO 02 37 52.40567732 +28 48 08.9900231     18.5 16.99   ~ 510 1
2 NAME LDN 1448 IRS 1 Em* 03 25 09.430 +30 46 21.58     19.5     ~ 88 0
3 JCMTSE J032525.9+304502 Y*O 03 25 25.9 +30 45 03           ~ 47 0
4 LDN 1448NW Y*O 03 25 35.66 +30 45 34.2           ~ 61 0
5 LDN 1448NA smm 03 25 36.49 +30 45 22.2           ~ 173 1
6 LDN 1451 DNe 03 26.1 +30 10           ~ 45 0
7 NAME HH 7-11 MMS 3 smm 03 29 01.964 +31 15 38.04           ~ 52 0
8 NAME HH 7-11 MMS 2 smm 03 29 03.056 +31 15 51.67           ~ 68 0
9 [SVS76] NGC 1333 13A2 IR 03 29 03.374 +31 16 01.87           ~ 11 0
10 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 562 0
11 [HRF2005] 3 PoC 03 33 21.3 +31 07 27           ~ 62 0
12 [KJD2006] SMM J033335+31075 PoC 03 33 21.3 +31 07 28           ~ 79 0
13 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1086 0
14 4C 32.14 QSO 03 36 30.10760600 +32 18 29.3422210     17.50 16.6   ~ 584 1
15 IRAS 03363+3207 FIR 03 39 27.8 +32 17 11           ~ 5 0
16 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3545 0
17 QSO B0507+179 QSO 05 10 02.36912982 +18 00 41.5816534   20.0 19.0 19.09   ~ 322 1
18 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 866 1
19 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3066 0

    Equat.    Gal    SGal    Ecl

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2020.10.26-14:36:05

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