J/ApJ/869/L42 DSHARP. II. Annular substructures data (Huang+, 2018)
The Disk Substructures at High Angular Resolution Project (DSHARP).
II. Characteristics of annular substructures
Huang J., Andrews S.M., Dullemond C.P., Isella A., Perez L.M., Guzman V.V.,
Oberg K.I., Zhu Z., Zhang S., Bai X.-N., Benisty M., Birnstiel T.,
Carpenter J.M., Hughes A.M., Ricci L., Weaver E., Wilner D.J.
<Astrophys. J., 869, L42 (2018)>
=2018ApJ...869L..42H 2018ApJ...869L..42H
ADC_Keywords: Millimetric/submm sources
Keywords: planets and satellites: formation - protoplanetary disks -
techniques: high angular resolution
Abstract:
The Disk Substructures at High Angular Resolution Project (DSHARP)
used the Atacama Large Millimeter/submillimeter Array (ALMA) to map
the 1.25mm continuum of protoplanetary disks at a spatial resolution
of ∼5au. We present a systematic analysis of annular substructures in
the 18 single-disk systems targeted in this survey. No dominant
architecture emerges from this sample; instead, remarkably diverse
morphologies are observed. Annular substructures can occur at
virtually any radius where millimeter continuum emission is detected
and range in widths from a few astronomical units to tens of
astronomical units. Intensity ratios between gaps and adjacent rings
range from near-unity to just a few percent. In a minority of cases,
annular substructures coexist with other types of substructures,
including spiral arms (3/18) and crescent-like azimuthal asymmetries
(2/18). No clear trend is observed between the positions of the
substructures and stellar host properties. In particular, the absence
of an obvious association with stellar host luminosity (and hence the
disk thermal structure) suggests that substructures do not occur
preferentially near major molecular snowlines. Annular substructures
like those observed in DSHARP have long been hypothesized to be due to
planet-disk interactions. A few disks exhibit characteristics
particularly suggestive of this scenario, including substructures in
possible mean-motion resonance and "double gap" features reminiscent
of hydrodynamical simulations of multiple gaps opened by a planet in a
low-viscosity disk.
Description:
The Disk Substructures at High Angular Resolution Project (DSHARP)
targeted 20 systems, 18 of which are single-disk systems (i.e., all
sources except AS 205 and HT Lup).
The analysis in this work is based on the "fiducial" images presented
in Andrews+ (Paper I; 2018, J/ApJ/869/L41), which also provides
details about the observational setup and the calibration and imaging
procedure.
For comparison, the annular substructure locations for the TW Hya and
HL Tau disks are appended to Table 1. The TW Hya analysis uses the
1.0mm image presented in Huang+ (2018ApJ...852..122H 2018ApJ...852..122H) and the HL Tau
analysis uses the 1.0mm image presented in ALMA Partnership+
(2015ApJ...808L...3A 2015ApJ...808L...3A). Although 1.3mm continuum observations are
available for both sources, the 1.0mm images are used instead because
of their better angular resolution and uv coverage.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 8 20 List of host stars; table added by CDS
table1.dat 145 107 Properties of annular substructures
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/A+A/378/116 : Classification & vsini of Vega-type & PMS stars (Mora+, 2001)
J/AJ/126/2971 : UBVRI photometry of 131 Herbig Ae/Be (Vieira+, 2003)
J/ApJ/749/79 : Transition disks. II. Southern MoC (Romero+, 2012)
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/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
J/A+A/561/A2 : 36 accreting YSOs emission lines (Alcala+, 2014)
J/ApJ/786/97 : Photospheric properties of T Tauri stars (Herczeg+, 2014)
J/ApJ/827/142 : ALMA observations of GKM stars in Upper Sco (Barenfeld+, 2016)
J/ApJ/828/46 : ALMA survey of Lupus protoplanetary disks. I. (Ansdell+, 2016)
J/MNRAS/461/794 : Scorpius-Centaurus K-Type Stars (Pecaut+, 2016)
J/A+A/600/A20 : Lupus YSOs X-shooter spectroscopy (Alcala+, 2017)
J/AJ/154/109 : California-Kepler Survey. III. Planet radii (Fulton+, 2017)
J/ApJ/845/44 : Nearby protoplanetary disk 340GHz SMA obs. (Tripathi+,2017)
J/A+A/610/A24 : AS 209 ALMA image (Fedele+, 2018)
J/A+A/619/A161 : ALMA images of HD 135344B (Cazzoletti+, 2018)
J/ApJ/859/33 : GOBELINS. IV. VLBA obs. of Taurus (Galli+, 2018)
J/ApJ/860/124 : ALMA continuum emission obs. of MWC 758 disk (Dong+, 2018)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Name of the host star
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Name of the host star
10 A1 --- f_Name [ab] Flag on name (1)
12- 15 A4 --- Label Substructure label (2)
17 A1 --- f_Label [c-e] Flag on label (1)
19- 24 F6.1 mas DeltaX [-244/111]? R.A. offset from phase center
(Δx)
26- 28 F3.1 mas e_DeltaX [0.2/5]? Minimum error on DeltaX
30- 32 F3.1 mas E_DeltaX [0.2/5]? Maximum error on DeltaX
34- 39 F6.1 mas DeltaY [-495/89]? Declination offset from phase center
(Δy)
41- 43 F3.1 mas e_DeltaY [0.6/4]? Minimum error on DeltaY
45- 47 F3.1 mas E_DeltaY [0.6/4]? Maximum error on DeltaY
49 A1 --- u_Angr0 [~] Approximate flag on Angr0
51- 56 F6.1 mas Angr0 [17/1550] Angular radial location of
substructure in mas
58- 61 F4.1 mas e_Angr0 [0.7/10]? Lower 1σ uncertainty in Angr0
63- 66 F4.1 mas E_Angr0 [0.7/10]? Upper 1σ uncertainty in Angr0
68 A1 --- u_Phyr0 [~] Approximate flag on Phyr0
70- 75 F6.2 au Phyr0 [1/155] Physical radial location of
substructure in astronomical units
77- 80 F4.2 au e_Phyr0 [0.07/1]? Lower 1σ uncertainty
in Phyr0 (3)
82- 85 F4.2 au E_Phyr0 [0.07/1]? Upper 1σ uncertainty
in Phyr0 (3)
87- 91 F5.2 deg Inc [17/68.2]? Inclination of substructure (0°
is face-on and 90° is edge-on)
93- 96 F4.2 deg e_Inc [0.1/2]? Lower 1σ uncertainty in Inc
98-101 F4.2 deg E_Inc [0.1/2]? Upper 1σ uncertainty in Inc
103-108 F6.2 deg PA [37/175]? Position angle of substructure
(east of north)
110-113 F4.2 deg e_PA [0.1/7]? Lower 1σ uncertainty in PA
115-118 F4.2 deg E_PA [0.1/7]? Upper 1σ uncertainty in PA
120 A1 --- Meth Method used to derive radial location of
substructure (4)
122 A1 --- l_Width Limit flag on Width
124-127 F4.1 au Width [1/23]? Width of substructure, only measured
for those identified via E and R methods
129-131 F3.1 au e_Width [0.1/1.4]? The 1σ uncertainty in Width
133 A1 --- f_Width [f] Flag on Width (1)
135-139 F5.3 --- Depth [0.01/1]? Depth of gap
141-145 F5.3 --- e_Depth [0.006/0.2]? The 1σ uncertainty in Depth
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Note (1): Flag as follows:
a = Fit to the 290GHz continuum image from Huang+ (2018ApJ...852..122H 2018ApJ...852..122H).
The PA and inclination are fixed at 155° and 7°, respectively,
based on values derived from 12CO observations in
Qi+ (2004ApJ...616L..11Q 2004ApJ...616L..11Q).
b = Measurements for substructure positions taken from ALMA
Partnership+ (2015ApJ...808L...3A 2015ApJ...808L...3A) and rescaled to a distance of 147pc
(Galli+, 2018, J/ApJ/859/33).
c = This feature shows tentative signs of being multiple gaps and rings.
d = This ring may be misaligned relative to the outer two rings and therefore
could have a larger radius than implied by the radial profile.
See Perez+ (2018ApJ...869L..50P 2018ApJ...869L..50P).
e = Substructures tentatively classified as annular.
f = Width of feature is narrower than the minor axis FWHM of the synthesized
beam (see Table 2 in the article for the synthesized beam size).
Note (2): If the annular substructure's coordinates were extracted by searching
for local minima in the radial profile cuts, it is labeled with the
prefix "D" (for "Dark"), followed by the semimajor axis of the
best-fit ellipse rounded to the nearest whole number of astronomical
units. Similarly, if the annular substructure's coordinates were
extracted by searching for local maxima, it is labeled with the prefix
"B" (for "Bright"), again followed by the semimajor axis of the
best-fit ellipse rounded to the nearest whole number of astronomical
units. This naming convention is adapted from that used for HL Tau in
ALMA Partnership+ (2015ApJ...808L...3A 2015ApJ...808L...3A).
Note (3): The uncertainties in the angular size are simply scaled from the
fitting procedure and do not account for the uncertainty in the
distance to the source.
Note (4): Method to derive radial location of substructure as follows:
E = ellipse-fitting
R = identification of local extrema in the radial profile
V = identification through visual inspection.
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History:
From electronic version of the journal
References:
Andrews et al. Paper I. 2018ApJ...869L..41A 2018ApJ...869L..41A Cat. J/ApJ/869/L41
Huang et al. Paper III. 2018ApJ...869L..43H 2018ApJ...869L..43H
Kurtovic et al. Paper IV. 2018ApJ...869L..44K 2018ApJ...869L..44K
Birnstiel et al. Paper V. 2018ApJ...869L..45B 2018ApJ...869L..45B
Dullemond et al. Paper VI. 2018ApJ...869L..46D 2018ApJ...869L..46D
Zhang et al. Paper VII. 2018ApJ...869L..47Z 2018ApJ...869L..47Z
Isella et al. Paper IX. 2018ApJ...869L..49I 2018ApJ...869L..49I
Perez et al. Paper X. 2018ApJ...869L..50P 2018ApJ...869L..50P
(End) Prepared by [AAS], Coralie Fix [CDS], 16-Jan-2020