J/ApJ/859/21 ALMA survey of Lupus protoplanetary disks. II. (Ansdell+, 2018)
ALMA survey of Lupus protoplanetary disks.
II. Gas disk radii.
Ansdell M., Williams J.P., Trapman L., van Terwisga S.E., Facchini S.,
Manara C.F., van der Marel N., Miotello A., Tazzari M., Hogerheijde M.,
Guidi G., Testi L., van Dishoeck E.F.
<Astrophys. J., 859, 21 (2018)>
=2018ApJ...859...21A 2018ApJ...859...21A
ADC_Keywords: Millimetric/submm sources ; Stars, masses ; Radio lines;
Star Forming Region; Carbon monoxide
Keywords: accretion, accretion disks; circumstellar matter; planetary systems;
protoplanetary disks; stars: pre-main sequence;
stars: variables: T Tauri, Herbig Ae/Be
Abstract:
We present Atacama Large Millimeter/Sub-Millimeter Array (ALMA) Band 6
observations of a complete sample of protoplanetary disks in the young
(∼1-3Myr) Lupus star-forming region, covering the 1.33mm continuum and
the 12CO, 13CO, and C18O J=2-1 lines. The spatial resolution is
∼0.25" with a medium 3σ continuum sensitivity of 0.30mJy,
corresponding to Mdust ∼0.2M⊕. We apply Keplerian masking to
enhance the signal-to-noise ratios of our 12CO zero-moment maps,
enabling measurements of gas disk radii for 22 Lupus disks; we find
that gas disks are universally larger than millimeter dust disks by a
factor of two on average, likely due to a combination of the optically
thick gas emission and the growth and inward drift of the dust. Using
the gas disk radii, we calculate the dimensionless viscosity
parameter, αvisc, finding a broad distribution and no
correlations with other disk or stellar parameters, suggesting that
viscous processes have not yet established quasi-steady states in
Lupus disks. By combining our 1.33mm continuum fluxes with our
previous 890µm continuum observations, we also calculate the
millimeter spectral index, αmm, for 70 Lupus disks; we find an
anticorrelation between αmm and millimeter flux for low-mass
disks (Mdust≲5), followed by a flattening as disks approach
αmm∼2, which could indicate faster grain growth in higher-mass
disks, but may also reflect their larger optically thick components.
In sum, this work demonstrates the continuous stream of new insights
into disk evolution and planet formation that can be gleaned from
unbiased ALMA disk surveys.
Description:
Our ALMA Cycle 3 program (ID: 2015.1.00222.S; PI: Williams) observed
86 sources in our sample in Band 6 on 2016 July 24 and September 8
using 58 12m antennas on baselines of 15-1110m and 15-2483m,
respectively (bandwidth-weighted mean continuum frequency of 225.66GHz
(1.33mm)).
Our ALMA Cycle 4 program (ID: 2016.1.01239.S; PI: van Terwisga)
observed an additional seven sources in our sample (Sz75, Sz76, Sz77,
Sz102, EX Lup, V1094 Sco, and J15560210-3655282) in Band 6 on 2017
July 7 (see also S. E. van Terwisga 2018, in preparation for
descriptions of the ALMA Band 7 observations of these seven sources).
The two remaining sources in our sample (Sz82 and Sz91) have Band 6
continuum observations as well as 12CO, 13CO, and C18O J=2-1
line observations in the ALMA archive (ID: 2013.1.00226.S and
2013.1.01020.S).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 94 95 1330um continuum properties
table2.dat 58 95 Gas properties
table3.dat 45 22 Disk radii
table4.dat 77 7 Secondary source properties
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See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
J/A+A/369/249 : T Tauri binary systems orbital motion (Woitas+, 2001)
J/ApJ/662/1067 : Sptizer observations of sigma Orionis (Hernandez+, 2007)
J/ApJS/177/551 : Spitzer c2d survey of Lupus dark clouds (Merin+, 2008)
J/ApJS/181/321 : Properties of Spitzer c2d dark clouds (Evans+, 2009)
J/other/Nat/481.167 : 2002-2007 PLANET microlensing events (Assan+, 2012)
J/ApJ/771/129 : Submillimetric Class II sources of Taurus (Andrews+, 2013)
J/A+A/561/A2 : 36 accreting YSOs emission lines (Alcala+, 2014)
J/A+A/564/A51 : 3mm maps of 4 transition disks (Pinilla+, 2014)
J/ApJ/788/59 : Parametric model for circumstellar disks gas mass
(Williams+, 2014)
J/ApJS/216/7 : Planets Around Low-Mass Stars (PALMS). IV. (Bowler+, 2015)
J/ApJS/220/11 : SEDs of Spitzer YSOs in the Gould Belt (Dunham+, 2015)
J/ApJ/828/46 : ALMA survey of Lupus protopl. disks. I. (Ansdell+, 2016)
J/ApJ/827/142 : ALMA obs. of GKM stars in Upper Sco (Barenfeld+, 2016)
J/MNRAS/457/2877 : Kepler M dwarf stars revised properties (Gaidos+, 2016)
J/A+A/594/A85 : 2D disk models from CO isotopologues line (Miotello+, 2016)
J/ApJ/831/125 : ALMA 887µm obs. of ChaI region (Pascucci+, 2016)
J/A+A/592/A49 : TW Hya CO(2-1), CN(2-1) & CS(5-4) data cubes (Teague+, 2016)
J/A+A/600/A20 : Lupus YSOs X-shooter spectroscopy (Alcala+, 2017)
J/AJ/153/240 : ALMA survey of protopl. disks in sigma Ori (Ansdell+, 2017)
J/A+A/602/A33 : X-Shooter spectroscopy of YSOs in Lupus (Frasca+, 2017)
J/ApJ/847/31 : Protoplanetary disk data in Cha I and Lupus (Mulders+, 2017)
J/ApJ/849/63 : FIR-mm data of YSOs in star-forming regions (Ribas+, 2017)
J/A+A/606/A125 : HD163296 DCO+, DCN and N2D+ data cubes (Salinas+, 2017)
J/ApJ/845/44 : 340GHz obs. of 50 nearby protopl. disks (Tripathi+, 2017)
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 name
19- 20 I2 h RAh [15/16] Hour of Right Ascension (J2000) (1)
22- 23 I2 min RAm Minute of Right Ascension (J2000) (1)
25- 30 F6.3 s RAs Second of Right Ascension (J2000) (1)
32- 32 A1 --- DE- [-] Sign of the Declination (J2000)(1)
33- 34 I2 deg DEd [34/42] Degree of Declination (J2000) (1)
36- 37 I2 arcmin DEm Arcminute of Declination (J2000) (1)
39- 44 F6.3 arcsec DEs Arcsecond of Declination (J2000) (1)
46- 48 I3 pc Dist [150/200] Distance: Lupus III=200pc;
Other=150pc
50- 53 A4 --- SpT Spectral Type
55- 58 F4.2 Msun Mstar [0.1/3]? Mass, in solar units
60- 63 F4.2 Msun e_Mstar [0.01/0.4]? Uncertainty in Mstar
65- 65 I1 --- r_Mstar [1/5]? Reference for Mstar (2)
67- 72 F6.2 mJy Fcont [-0.3/205] 1.33mm Continuum Flux density
74- 77 F4.2 mJy e_Fcont [0.09/7] Uncertainty in Fcont (3)
79- 82 F4.2 mJy/beam rms [0.08/0.2] Image rms for each source (4)
84- 89 F6.2 Mgeo Mdust [-0.3/217] Mass of the emitting dust,
Earth masses
91- 94 F4.2 Mgeo e_Mdust [0.06/8.5] Uncertainty in Mdust
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Note (1): Fitted source centers output by uvmodelfit for the detections, and
the phase centers of our ALMA observations (based on 2MASS source positions)
for the non-detections.
Note (2): Reference for Mstar as follows:
1 = Alcala et al. (2014, J/A+A/561/A2),
2 = Alcala et al. (2017, J/A+A/600/A20),
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. (2016ApJ...832..110C 2016ApJ...832..110C),
7 = Bustamante et al. (2015A&A...578A..23B 2015A&A...578A..23B),
8 = Comeron (2008hsf2.book..295C 2008hsf2.book..295C).
Note (3): The uncertainties are statistical errors and do not include the
10% absolute flux calibration error; see Section 3.
Note (4): Image rms for each source, derived from a 4-9 arcsecond radius
annulus centered on the fitted or expected source position for detections
or non-detections, respectively.
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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 name
19- 19 A1 --- l_F13CO Limit flag on F13CO
21- 25 I5 mJy.km/s F13CO [48/13800] Integrated flux density, 13CO
27- 30 I4 mJy.km/s e_F13CO [26/4300]? Uncertainty for F13CO
32- 32 A1 --- l_FC18O Limit flag on FC18O
34- 37 I4 mJy.km/s FC18O [45/1633] Integrated flux density, C18O
39- 41 I3 mJy.km/s e_FC18O [15/357]? Uncertainty for FC18O
43- 43 A1 --- l_Mgas Limit flag on Mgas
45- 48 F4.1 Mjup Mgas [0/21.8]? Derived gas mass, mean (5)
50- 53 F4.1 Mjup b_Mgas [0.3/10.5]? Gas mass, min (5)
55- 58 F4.1 Mjup B_Mgas [0/31.4]? Gas mass, max (5)
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Note (5): For the 8 sources detected in both 13CO and C18O, we calculate the
mean (in log space) of the WB14 (Williams+, 2014, J/ApJ/788/59) model
grid points within ±3σ of our measured 13CO and C18O line
luminosities (Mgas), and also gas set upper (Mgas,max) and lower
(Mgas,min) limits based on the maximum and minimum WB14 model grid
points consistent with the data. For the 12 disks with 13CO detections
and C18O upper limits, we similarly calculate Mgas and Mgas,max but
set Mgas,min to zero as isotope-selective photodissociation may be
stronger for low-mass disks (Miotello et al. 2016A&A...594A..85M 2016A&A...594A..85M).
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Name Source name
19- 23 F5.1 deg PA [17.4/175.8] Disk position angle, east of north
25- 29 F5.1 deg i [-74/78.5] Disk inclination
31- 33 I3 au Rdust [38/334] Radius, dust
35- 36 I2 au e_Rdust [2/20] Uncertainty in Rdust
38- 40 I3 au Rgas [68/462] Radius, gas
42- 45 I4 au e_Rgas [3/112] Uncertainty in Rgas
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Name Source name, primary
19- 20 I2 h RAh [15/16] Hour of Right Ascension (J2000) (1)
22- 23 I2 min RAm [7/55] Minute of Right Ascension (J2000) (1)
25- 30 F6.3 s RAs Second of Right Ascension (J2000) (1)
32- 32 A1 --- DE- [-] Sign of the Declination (J2000) (1)
33- 34 I2 deg DEd [34/39] Degree of Declination (J2000) (1)
36- 37 I2 arcmin DEm [1/21] Arcminute of Declination (J2000) (1)
39- 44 F6.3 arcsec DEs Arcsecond of Declination (J2000) (1)
46- 49 F4.2 mJy Fcont2 [0.3/8.3]? 1.33mm Continuum Flux density,
secondary (2)
51- 54 F4.2 mJy e_Fcont2 [0.1]? Uncertainty in Fcont2 (2)
56- 60 F5.2 mJy Fcont1 [0.5/66.4] 1.33mm Continuum Flux density,
primary
62- 65 F4.2 mJy e_Fcont1 [0.09/0.4] Uncertainty in Fcont1
67- 72 F6.2 deg PA Position angle, secondary relative to
primary, east of north
74- 77 F4.2 arcsec Sep [0.3/3] Projected angular separation
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Note (1): Position of secondary from fitting point source models to the
visibility data with the uvmodelfit routine in CASA.
Note (2): Sz 74 and Sz 88A are too close to their primary source to allow
reliable individual Fcont2 measurements.
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History:
From electronic version of the journal
References:
Ansdell et al. Paper I. 2016ApJ...828...46A 2016ApJ...828...46A Cat. J/ApJ/828/46
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 03-Apr-2019