J/ApJ/828/46 ALMA survey of Lupus protoplanetary disks. I. (Ansdell+, 2016)
ALMA survey of Lupus protoplanetary disks.
I. Dust and gas masses.
Ansdell M., Williams J.P., van der Marel N., Carpenter J.M., Guidi G.,
Hogerheijde M., Mathews G.S., Manara C.F., Miotello A., Natta A.,
Oliveira I., Tazzari M., Testi L., van Dishoeck E.F., van Terwisga S.E.
<Astrophys. J., 828, 46-46 (2016)>
=2016ApJ...828...46A 2016ApJ...828...46A (SIMBAD/NED BibCode)
ADC_Keywords: YSOs ; Millimetric/submm sources ; Stars, masses ; Radio lines ;
Surveys
Keywords: circumstellar matter; planets and satellites: formation;
protoplanetary disks; stars: formation; stars: late-type;
stars: protostars
Abstract:
We present the first high-resolution sub-millimeter survey of both
dust and gas for a large population of protoplanetary disks.
Characterizing fundamental properties of protoplanetary disks on a
statistical level is critical to understanding how disks evolve into
the diverse exoplanet population. We use the Atacama Large
Millimeter/Submillimeter Array (ALMA) to survey 89 protoplanetary
disks around stars with M*>0.1M☉ in the young (1-3Myr), nearby
(150-200pc) Lupus complex. Our observations cover the 890µm
continuum and the 13CO and C18O 3-2 lines. We use the
sub-millimeter continuum to constrain Mdust to a few Martian masses
(0.2-0.4M⊕) and the CO isotopologue lines to constrain Mgas
to roughly a Jupiter mass (assuming an interstellar medium (ISM)-like
[CO]/[H2] abundance). Of 89 sources, we detect 62 in continuum, 36
in 13CO, and 11 in C18O at >3σ significance. Stacking
individually undetected sources limits their average dust mass to
≲6 Lunar masses (0.03M⊕), indicating rapid evolution once
disk clearing begins. We find a positive correlation between Mdust
and M*, and present the first evidence for a positive correlation
between Mgas and M*, which may explain the dependence of giant
planet frequency on host star mass. The mean dust mass in Lupus is 3x
higher than in Upper Sco, while the dust mass distributions in Lupus
and Taurus are statistically indistinguishable. Most detected disks
have Mgas≲1MJup and gas-to-dust ratios <100, assuming an ISM-like
[CO]/[H2] abundance; unless CO is very depleted, the inferred gas
depletion indicates that planet formation is well underway by a few
Myr and may explain the unexpected prevalence of super-Earths in the
exoplanet population.
Description:
Our ALMA Cycle 2 observations (Project ID: 2013.1.00220.S) were
obtained on 2015 June 14 (AGK-type sources and unknown spectral types)
and 2015 June 15 (M-type sources). The continuum spectral windows were
centered on 328.3, 340.0, and 341.8GHz with bandwidths of 1.875,
0.938, and 1.875 GHz and channel widths of 15.625, 0.244, and
0.977MHz, respectively. The bandwidth-weighted mean continuum
frequency was 335.8GHz (890um). The spectral setup included two
windows covering the 13CO and C18O 3-2 transitions; these spectral
windows were centered on 330.6 and 329.3GHz, respectively, with
bandwidths of 58.594MHz, channel widths of 0.122MHz, and velocity
resolutions of 0.11km/s.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 38 93 *Stellar properties
table2.dat 111 89 The ALMA 890 micron continuum properties
table3.dat 51 89 Gas properties
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Note on table1.dat: Table 1 gives the 93 Lupus disks that fit our selection
criteria. Our adopted nomenclature uses primarily Sz or 2MASS names,
supplemented with c2d names.
Our ALMA Cycle 2 program did not observe Sz 76, Sz 77, Sz 82, Sz 91, or
V1094 Sco. However, for Sz 82 (IM Lup) we utilize existing ALMA data
(Cleeves et al., in preparation) in this work.
Note that although RXJ1556.1-3655 and RXJ1615.3-3255 are listed as Class II
Lupus disks in the literature, we excluded them from our sample as their
coordinates are off the Lupus I-IV clouds (e.g., Cambresy 1999A&A...345..965C 1999A&A...345..965C).
Thus we obtained ALMA data for 89 (out of 93) sources in our sample for a
96% completeness rate.
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See also:
J/A+A/588/A108 : Spectra of CO and [CI] in protoplanetary disks (Kama+, 2016)
J/A+A/561/A2 : 36 accreting YSOs emission lines (Alcala+, 2014)
J/ApJ/749/79 : Transition disks. II. Southern MoC (Romero+, 2012)
J/ApJ/724/835 : The Spitzer c2d survey of WTTSs. III. (Wahhaj+, 2010)
J/ApJS/181/321 : Properties of Spitzer c2d dark clouds (Evans+, 2009)
J/ApJS/177/551 : Spitzer c2d survey of Lupus dark clouds (Merin+, 2008)
J/A+A/291/943 : Protostellar cores (Ossenkopf+, 1994)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Source identifier
19- 21 I3 pc Dist [150/200] Distance
23- 26 A4 --- SpT MK spectral type
28- 31 F4.2 Msun Mass [0.1/3]? Stellar mass
33- 36 F4.2 Msun e_Mass [0.01/0.4]? Uncertainty Mass
38 I1 --- Ref ? Reference (1)
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Note (1): Reference as follows:
1 = Alcala et al. (2014, J/A+A/561/A2);
2 = Alcala et al. (in prep);
3 = Alecian et al. (2013MNRAS.429.1001A 2013MNRAS.429.1001A);
4 = Mortier et al. (2011MNRAS.418.1194M 2011MNRAS.418.1194M);
5 = Merin et al. (2008, J/ApJS/177/551);
6 = Cleeves et al. (in prep);
7 = Bustamante et al. (2015A&A...578A..23B 2015A&A...578A..23B);
8 = Comeron (2008hsf2.book..295C 2008hsf2.book..295C).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Source identifier
19- 20 I2 h RAh [15/16] Hour of Right Ascension (J2000)
22- 23 I2 min RAm Minute of Right Ascension (J2000)
25- 29 F5.2 s RAs Second of Right Ascension (J2000)
31- 31 A1 --- DE- [-] Sign of the Declination (J2000)
32- 33 I2 deg DEd [34/42] Degree of Declination (J2000)
35- 36 I2 arcmin DEm Arcminute of Declination (J2000)
38- 42 F5.2 arcsec DEs Arcsecond of Declination (J2000)
44- 49 F6.2 mJy F890 [-0.6/600] ALMA 890um continuum flux density
51- 55 F5.2 mJy e_F890 [0.1/90] Uncertainty in F890
57- 62 F6.2 mJy/beam rms [0.2/0.7]? Root mean square; mJy/beam
64- 70 F7.3 arcsec a [0.08/0.98]? Semi-major axis
72- 78 F7.3 arcsec e_a [0.001/0.03]? Uncertainty in a
80- 82 I3 deg PA [-86/59]? Position angle
84- 86 I3 deg e_PA [0/57]? Uncertainty in PA
88- 90 I3 deg i [0/82]? Inclination
92- 94 I3 deg e_i [0/28]? Uncertainty in i
96-103 F8.4 Mgeo MDust [-0.24/141.1] Dust mass
105-111 F7.4 Mgeo e_MDust [0.04/21.2] Uncertainty in MDust
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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- 17 A17 --- Name Source identifier
19- 19 A1 --- l_F13CO Limit flag on F13CO
20- 23 I4 mJy.km/s F13CO [66/8880] Flux density of 13CO line
25- 27 I3 mJy.km/s e_F13CO [42/317]? Uncertainty in F13CO
29- 29 A1 --- l_F18CO Limit flag on F18CO
30- 33 I4 mJy.km/s F18CO [90/2410] Flux density of 18CO line
35- 37 I3 mJy.km/s e_F18CO [45/238]? Uncertainty in F18CO
39- 39 A1 --- l_Mgas Limit flag on Mgas
40- 42 F3.1 Mjup Mgas [0.1/8.2] Gas mass
44- 46 F3.1 Mjup b_Mgas [0.3/3.1]? Lower boundary of Mgas
48- 51 F4.1 Mjup B_Mgas [1/31.4]? Upper boundary of Mgas
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History:
From electronic version of the journal
References:
Ansdell et al. Paper II. 2018ApJ...859...21A 2018ApJ...859...21A Cat. J/ApJ/859/21
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 02-Dec-2016