Lupus ALMA
ALMA revolution
Disk Survey

on planet formation
A&A proofs: manuscript no. hd97048-gap

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Megan
Ansdell8
IfA (University of Hawaii)
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MEM model

Jonathan Williams(IfA)
The AstrophysicalJournal Letters, 783:L13
1.0
1.0
1.0
Nienke van der Marel (IfA)
Carlo
The highly asymmetric crescent-shaped
dustManara (ESA)
the standard
0.5 core-accretion picture, dust grains0.5
0.5
Anna
con-Miotello (Leiden)must grow from submicrometer sizes to rocky structure revealed by the 0.44-mm ALMA
Marco Tazzari (ESO)
0.0
0.0
millimetercores ~10 times
the mass of Earth (MEarth) within0.0 tinuum (Fig. 1) traces emission from45 and Hogerheijde (Leiden)the ~10-million-year lifetime of the circumstellar sized dust grains and is located betweenMichiel
−0.5
−0.5
−0.5
Sierk
vanLetters,
Terwisga(Leiden)80 AU (T9 AU) from the star.The
The
azimuthaldisk. However,this growth process is stymied
AstrophysicalJournal783:L13 (6pp),
2014 March 1(MCTI)
withOliveiranoby what is usually called the radial drift and extent is less than one-third of the ring, Isa
−1.0
−1.0
−1.0
A INAF)
Leonardo
Testi (ESO,infragmentation barrier: Particles of intermediate detected flux at a 3s level (2.4 mJy per beam)
size [~1 m at 1 astronomical unit (AU) (1 AU = the northern part (fig. S1). The peak emission
Ewine
van
Dishoeck(Leiden, MPE)
1.0
0.5
0.0
−0.5
−1.0
1.0
0.5
0.0
−0.5
−1.0
1.0
0.5
0.0
−0.5
−1.0
8
[arcseconds]∆α high[arcseconds]∆αAlcala[arcseconds] (INAF)
signal-to-noise ratio of ~390,
1.5 × 10 km = distance∆αfrom
Earth to the Sun), has a very
JuanandPublications
oftheAstronomical
SocietyofJapan(2015),
Vol.
67,
No.
6
1
oppositeor ~1 mm at 50 AU from the star] acquire high the contrast with the upper limit on the John
Carpenter (ALMA)1
sideof7 theis at least
factorof 130.
drift velocities
toward thestar ofwith
theALMA
Fig. 2. Reconstructed
imagesHD respect
97048 fortothe
band
data.ring
The intensity
scalea for
all images
is inThe
units
of Jy beam
. To highlight
Greta
Guidi
(INAF)
the4).
small-scale
structure
we majorshow (fromleft to right)
imagesreconstructedwithprogressively
smallerbeams.
The
left panel shows the image
completeabsenceofdustemission
in
the
north
of
gascarried
(3,
This
leads
to
two
problemsforGeoff image
Mathews(IfA)
out intheextendedarray configuration
withasuperuniformly
maxreconstructedusingsuperuniform
weighting.
The centralIRS
panel48shows
reconstructedresulting from clipping
andtheresulting
highweighted
contrast
makethefurthergrowth (5):First,
high-velocity
collisions
Antonella
Natta(INAF,
all baselines
below 160
. Finally, therightm.
panel
showsobservations
the MEM model image.
range between
the panels
is dueDIAS)
toimumbaselineof k about
480
The
con-The di↵erence in dynamic∆δ [arcseconds]

REPORTSextremethan earlier
betweenparticles
different
drift velocities
flux loss
incurredwith
by clipping
the shortest
baselines for thecrescent-shaped
central panel, and feature
due to themore
smallerreconstructedbeam for the right panel.
(10, 13). The spectral slope
cause
fragmentation.
Second, evenif particles
sistedof six scheduling
blocksduringdust
theasymmetries
period fromof themillimetertofluxes
F [0.44 mm comavoid
this Junefragmentation,
they willrapidlydrift abeam
1
2012
to of
August.
The
correlator
configured
dynamical
range⇡ 1200 and
a RMS
of 0.20 mJywas. We 2.3. ALMA
Cyclen1 band 3 data
inwardandbe using
lost into
the star
beforethey foundbinedinwith
shift
allthusimagesthe propermotioncorrection
van fluxes at lower frequencies n (14)]
B
a
store
dual
polarizations
infour
separate
spectralwindows
have Leeuwen
time to (2007)
grow tosize.
This 1 andis only
andplanetesimalthese are shownin Figs.
2 for 2.67
the T 0.25 (Fn º n ), suggesting that
ALMA
Early Science
Cycle 1 observations
were conducted oncontinuum
emission.
Weappliedself-calibration
solutionseach,
with
469
MHz
and
3840 channels
andradialdrift
barrieris ofonebandwidthof themostthepersistentmillimeter-sizedgrains(15) dominate
the+1 December
2013 withHowever,
72.6 seconds
obtainedfromthe continuum
emissionto the HCO0.44-mm
J=4-3 andcontinuum
issuesplanetformation
theories.
A 330.588,
possibleemission.
theof total time on HD 97048
12 in central
theirfrequencies
were329.331,342.883
CO J=3-2 data and subtracted the continuum emission using (Program
12 ID 2012.1.00031.S, see also Dunham et al. 2016). The
solutionisdusttrapping
inso-calledpressuregas
tracedbythe
CO 6-5 lineprovided
from thesame ranging between 15.8 andarray configuration
baselines
the 342.400
CASA taskGHz,
uvcontsub,
resulting in a toper-channel
RMS
ofmolecularandrespectively,
targetthe
1bumps:
pressuremaximawhere theThe
dust
ALMA
data set
indicates
Kepleriandisk pro- the perceptible water va462.9
meters.aDuring
the observations
19.5localand 23.7
mJy beam
respectively.
resulting
momentLupus ALMA
Disks Survey
Akimasa Kataoka (Heidelberg University)
13

18

ALMA revolution
A&A proofs: manuscript no. hd97048-gap•

High resolution studies - HL Tau, TW Hya, HD 97048
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The Astrophysical Journal Letters, 820:L40 (5pp), 2016 April 1

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Andrews et al.

superuniform

uvclip/superuniform

MEM model

November 23 and 0.7 mm on the latter two executions. The
total on-target integration time was ∼2 hr.
These raw data were calibrated by NRAO staff. After
1.0
1.0
applying phase corrections from water 1.0vapor radiometermeasurements, the data were time-averaged into 2 s integrations and ﬂagged for problematic antennas
and times. The
0.5
0.5
0.5
bandpass response of each spectral window was calibratedusing the observations of J1058+0133. The amplitude scale
was determined from J1037–2934 and 0.0
J1107–4449. The
0.0
0.0
complex gain response of the system was calibrated using thefrequent observations of J1103–3251. Although images
generated from these data are relatively −0.5
free of artifacts and
−0.5
−0.5
recover the integrated ﬂux density of the target (1.5 Jy), folding
in additional ALMA observations with a higher density of short
−1.0
−1.0
−1.0
antenna spacings improves the image reconstruction.
To that end, we calibrated three archival ALMA data
observations of TW Hya, from 2012 May 20, 2012 November
20, and 2014 December 31, using 16, 25, and 341.0antennas
0.5
0.0
−0.5
−1.0
1.0
0.5
0.0
−0.5
−1.0
1.0
0.5
0.0
−0.5
−1.0
∆α [arcseconds]∆α [arcseconds]
spanning baselines from 15 to 375 m. The ﬁrst two observa-∆α [arcseconds]
tions had four 59 MHz wide spectral windows centered at
Figure 1. Synthesized image of the 870 μm continuum emission from the TW
333.8, 335.4, 345.8, and 347.4 GHz. The latter had two
Hya disk with a 30 mas FWHM (1.6 au) circular beam. The rms noise level is
235 MHz windows (at 338.2 and 349.4 GHz), one 469 MHz∼35 μJy beam−1. The inset shows a 0 2 wide (10.8 au) zoom using an image
Fig. 2. Reconstructed imageswithofﬁnerHDresolution
97048(24×18
for themas,
ALMA
band 7 data. The intensity scale for all images is in units of Jy beam 1 . To highlightor 1.3×1.0 au, FWHM beam).
window (at 352.0 GHz), and one 1875 MHz window (atthe small-scale
structure we show (from left to right) images reconstructed with progressively smaller beams. The left panel shows the image
338.4 GHz). J1037–2934 was employed
as a gain calibrator,
reconstructedsuperuniform weighting. The central panel shows the superuniformly weighted reconstructed image resulting from clipping
and Titan and 3C 279 (May 20),
Ceres and using
J0522-364(November 20), or Ganymede and J0158+0133
31) k . Finally, the right panel shows the MEM model image. The di↵erence in dynamic range between the panels is due toall baselines(December
below 160
served as ﬂux or bandpass calibrators.
Theweatherfor
theseflux loss incurred by clipping the shortest baselines for the central panel, and due to the smaller reconstructed beam for the right panel.
observations was excellent, with PWV levels of 0.5–1 mm. The
10
combined on-target integration time was 95 minutes. The basic0.88 mm continuum images, 0.34’’ resolution
calibration was as described above. As a check, we comparedM⇤ fundamentallycorrelation
betweenCycle 1 band 3 data
dynamicalof ⇡ 1200 and aandRMS
of 0.20 mJy explains
beam 1the. We
2.3. ALMA
the amplitudes from each individual
data set onrange
overlapping
giant planet frequency and host star mass identified inspatial frequencies and found exceptional
consistency.
shift allimages using the properthe
motioncorrection
found
van2006; Johnson et al.
exoplanet
population(Endl inet al.
The calibrated visibilities from eachobservation
were shifted
2007;
Bonfils
et al.12013;
Bowleret al. 2010). This is
I. Introduction
Leeuwen(2007)
and
these
are
shown
in
Figs.
and
2
for
the
to account for the proper motion of the target and thenbecause core growth is more efficient both in higher-masscontinuum
emission.
the self-calibration solutions ALMA Early Science Cycle 1 observations were conducted on
combined after excising channels withpotential
emission
II. Our
Survey from We applied
disks (e.g., Thommes et+al. 2008; Mordasini et al. 2012)
spectral lines. Some modest improvements
weremadethewitha
1 December
obtainedfromcontinuum
emission
to higher-mass
the HCO stars
J=4-3
and
and around(e.g.,
Kennedy& Kenyon 2013 with 72.6 seconds of total time on HD 97048
III. Disk Fluxes
12 Continuumround of phase-only self-calibration.
imagesat a subtracted2008).
Thus the sourcesin the using
upper rightof FigureID
6 2012.1.00031.S, see also Dunham et al. 2016). The(Program
CO J=3-2
data
and
the
continuum
emissionand Masses
mean frequency of 345.9 GHz (867 μm) weregenerated byare more likely to form giant planet cores before the gas
arrayconfiguration provided baselines ranging between 15.8 and
the CASA withtaska uvcontsub,
resultingin a per-channel
Fourier inverting the visibilities, deconvolving
multidisk dissipates,
allowing the RMS
cores toofaccrete
substantial
IV. Disk Evolution
462.9
and
beam 1 respectively.
The
resulting
momentscale, multi-frequency synthesis 19.5
versionof23.7the mJy
CLEAN
gaseous envelopes and become gas giant planets. meters. During the observations the perceptible water vaLupus disks
also exhibit
dispersion
in theMdust,
algorithm, and then restoring with0,a1synthesized
beam.
All
V.
Summary
por inatmosphere
were stable within 5% of the median value
and 8 maps and spectra are shownin Figs.
3 and 4a large
for thespanning ⇠2 orders of magnitude for a given M⇤ . Ancalibration and imaging were performed
with the CASA +
12
of
0.535
mm.
Three
of
the four spectral windows of the ALMA
CO
J=3-2
and
HCO
J=4-3.
drews et al. (2013) noted that the similarly large dispackage (v4.5.0).
persion in Taurus is likely a consequence of
the inherent
correlator
were configured in TDM to maximise the sensitivity
After some experimentation, we settled on an analysis of two
diversity in disk temperatures, dust opacities,
andevoimages made from the same composite data set. The ﬁrst used afor continuum observations (128 channels over 1.875 GHz uslutionary states across the region. The large dispersion
Briggs weighting (with a robust parameter of 0) to provide aable bandwidth).
These spectral windows were centred at 101.9
5
in Lupus may result from di↵erent environments
and/or
2.2.1.
Imagingthethislong baselines
24×18 mas synthesized beam (atP.A.=78°).
Whilestates(24×18
across mas
thebeam)
Lupus
I–IV
clouds.
To GHz and 113.1 GHz. The fourth spectral window
GHz,
103.9
provides enhanced resolution, it comes at the cost of a dirty
Figure 2.evolutionary(top) High-resolution
synthesized
image
this,2,were-derived
M⇤ wascorrelation
usFigure 8. Dust mass cumulative
distributions
described testin Section
deprojected
into athe
mapMindustpolarvs.
coordinates
to morebeam with ∼20% sidelobes (due to the sparse coverage at long
configuredin
FDM to target the 12 CO J=1-0
line forandLupus,
cenTaurus, and Upper Sco disks around host stars with 1M⇤ >
ing
only
Lupus
III
sources;
we
chose
Lupus
III
becauseiteasily
view
the
disk
substructure.
(bottom)Theazimuthally
averagedradialWe alsoreconstructedbaselines) that degrades the image quality.
A second
image was the images using only baselines above 160 tered at 105.2 GHz,a spectral
resolution
ofmasses
159 mforseachand
0.1 Mwith(Section
6.2). The
average dust
resurface brightness
For reference,
red curveshows
the discontainsproﬁle.
the most
sourcesthein dashedour sample
andis moremade with a robust parameter of 0.5
elliptical thetapercontrast
to
k and
to an
enhanceof faint,
small-scalein themidplanetemperature
proﬁle toderivedfroma representative
model
disk.
The
gion
are
given GHz.
for reference.
The distributions
were calculatedtantcompared
thestructureotherclouds,thus
possiblyinbandwidtha difa
total
of
0.117
The
data
were
calibrated
using
create a circular 30 mas beam with negligible sidelobes. Bothgray curveferent
in the bottom
left reﬂects We
the proﬁlethe synthesized
beam.(1.4±0.5)
using the Kaplan-Meier estimator to include upper limits andenvironment.
foundof consistent
slope
These
data were
CASA version
images are consistent (within the disk.
resolutiondifferences)and cleaned using superuniform weighting, re- the provided datathereduction
line widths script
indicateand
1 confidence
intervals. 4.3. Uponanddispersion
(1.1
±
0.3)
valuestowithinerrors,indi0000
sulting
at PAthat
= 18
.
The
reconstructed. a beam of 0.48 ⇥ 0.26cating
have rms noise levels around 35 μJybeam−1inthe visibilities,
amplitudes
thesurveyed
spectralin window
the large dispersion in Lupusinspecting
is an intrinsic
Taurus andtheUpper
Sco, have ofbeen
the suband panel
azimuthally
averageda radial surface
image is shown in the centralof Fig.
2. diskintopopulation
propertyoftheresultingbrightness
from a rangemmwithsimilar anomalous
sensitivity andcompleteness.
Tauruscentered
at
113.1
GHz
showedbehaviour
andwedeAkimasa 3.Kataoka(Heidelberg University),
Disk workshop,
Island,26-30,
2016
proﬁle. Japan-Germanyof initial disk conditionsPlanet(e.g., core&angularmomentum) Ishigaki
has a similar
age to Sep.
Lupus (⇠1–2
Myr)
and its Class II
RESULTSTW HyaHD 97048∆δ [arcseconds]

HL TauALMA Partnership 2015•

Andrews et al. 2016van der Plas et al. 2016

Surveys on Upper Sco, Lupus, and Chameleon
4

Figure 2. 890 µm continuum images of the 61 Lupus disks detected in our ALMA Cycle 2 program (i.e., excluding Sz 82, which

was observed by Cleeves et al., in prep), ordered by decreasing continuum flux density (as reported in Table 2). Images are
200 ⇥200 and the typical beam size is shown in the first panel.

•

Barenfeld, et al. 2016, Andsell et al. 2016, Pascucci et al. 2016

ALMA Polarization

2 /25

High resolution studies
A&A proofs: manuscript no. hd97048-gap

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0.15

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0.00

The Astrophysical Journal Letters, 820:L40 (5pp), 2016 April 1

0.02

0.04

0.06

0.08

0.00

0.01

0.02

0.03

0.04

Andrews et al.

superuniform

uvclip/superuniform

MEM model

November 23 and 0.7 mm on the latter two executions. The
total on-target integration time was ∼2 hr.
These raw data were calibrated by NRAO staff. After
1.0
1.0
applying phase corrections from water 1.0vapor radiometermeasurements, the data were time-averaged into 2 s integrations and ﬂagged for problematic antennas
and times. The
0.5
0.5
0.5
bandpass response of each spectral window was calibratedusing the observations of J1058+0133. The amplitude scale
was determined from J1037–2934 and 0.0
J1107–4449. The
0.0
0.0
complex gain response of the system was calibrated using thefrequent observations of J1103–3251. Although images
generated from these data are relatively −0.5
free of artifacts and
−0.5
−0.5
recover the integrated ﬂux density of the target (1.5 Jy), folding
in additional ALMA observations with a higher density of short
−1.0
−1.0
−1.0
antenna spacings improves the image reconstruction.
To that end, we calibrated three archival ALMA data
observations of TW Hya, from 2012 May 20, 2012 November
20, and 2014 December 31, using 16, 25, and 341.0antennas
0.5
0.0
−0.5
−1.0
1.0
0.5
0.0
−0.5
−1.0
1.0
0.5
0.0
−0.5
−1.0
∆α [arcseconds]∆α [arcseconds]
spanning baselines from 15 to 375 m. The ﬁrst two observa-∆α [arcseconds]
tions had four 59 MHz wide spectral windows centered at
Figure 1. Synthesized image of the 870 μm continuum emission from the TW
333.8, 335.4, 345.8, and 347.4 GHz. The latter had two
Hya disk with a 30 mas FWHM (1.6 au) circular beam. The rms noise level is
235 MHz windows (at 338.2 and 349.4 GHz), one 469 MHz∼35 μJy beam−1. The inset shows a 0 2 wide (10.8 au) zoom using an image
Fig. 2. Reconstructed imageswithofﬁnerHDresolution
97048(24×18
for themas,
ALMA
band 7 data. The intensity scale for all images is in units of Jy beam 1 . To highlightor 1.3×1.0 au, FWHM beam).
window (at 352.0 GHz), and one 1875 MHz window (atthe small-scale
structure we show (from left to right) images reconstructed with progressively smaller beams. The left panel shows the image
338.4 GHz). J1037–2934 was employed
as a gain calibrator,
reconstructedsuperuniform weighting. The central panel shows the superuniformly weighted reconstructed image resulting from clipping
and Titan and 3C 279 (May 20),
Ceres and using
J0522-364(November 20), or Ganymede and J0158+0133
31) k . Finally, the right panel shows the MEM model image. The di↵erence in dynamic range between the panels is due toall baselines(December
below 160
served as ﬂux or bandpass calibrators.
Theweatherfor
theseflux loss incurred by clipping the shortest baselines for the central panel, and due to the smaller reconstructed beam for the right panel.
observations was excellent, with PWV levels of 0.5–1 mm. The
combined on-target integration time was 95 minutes. The basic
calibration was as described above. As a check, we compareddynamicalof ⇡ 1200 and a RMS of 0.20 mJy beam 1 . We 2.3. ALMA Cycle 1 band 3 data
the amplitudes from each individual
data set onrange
overlapping
spatial frequencies and found exceptional
consistency.
shift allimages using the proper motion correction found in van
The calibrated visibilities from eachobservation
were shifted
Leeuwen(2007)and these are shown in Figs. 1 and 2 for theto account for the proper motion of the target and thencontinuum
emission.
combined after excising channels withpotential emission
from We applied the self-calibration solutions ALMA Early Science Cycle 1 observations were conducted on
spectral lines. Some modest improvements
weremadethewithaobtainedfromcontinuum
emission to the HCO+ J=4-3 and 1 December 2013 with 72.6 seconds of total time on HD 97048
12 Continuum images at around of phase-only self-calibration.
CO J=3-2 data and subtracted the continuum emission using (Program ID 2012.1.00031.S, see also Dunham et al. 2016). The
mean frequency of 345.9 GHz (867 μm) were generated by
the CASA withtaska uvcontsub,
resulting in a per-channel RMS of array configuration provided baselines ranging between 15.8 andFourier inverting the visibilities, deconvolving
multiandof23.7
beam 1 respectively. The resulting moment 462.9 meters. During the observations the perceptible water vascale, multi-frequency synthesis 19.5
versionthe mJy
CLEAN
algorithm, and then restoring with0,a1synthesized
beam.andAll spectra are shown in Figs. 3 and 4 for the por in the atmosphere were stable within 5% of the median value
and 8 maps
calibration and imaging were performed
with the CASA +12
of 0.535 mm. Three of the four spectral windows of the ALMA
CO J=3-2 and HCO J=4-3.
package (v4.5.0).
correlator were configured in TDM to maximise the sensitivity
After some experimentation, we settled on an analysis of two
images made from the same composite data set. The ﬁrst used afor continuum observations (128 channels over 1.875 GHz usBriggs weighting (with a robust parameter of 0) to provide aable bandwidth). These spectral windows were centred at 101.9
2.2.1.
Imagingthethislong baselines
24×18 mas synthesized beam (atP.A.=78°).
While
GHz,
103.9 GHz and 113.1 GHz. The fourth spectral window
provides enhanced resolution, it comes at the cost of a dirty
Figure 2. (top) High-resolution (24×18 mas beam) synthesizedimage
described in Section 2, deprojected into a map in polar coordinates
to morebeam with ∼20% sidelobes (due to the sparse coverage at longwasconfigured in FDM to target the 12 CO J=1-0 line and ceneasily view using
the disk only
substructure.
(bottom) The
azimuthallyradialWe alsoreconstructedbaselines
above
160 averaged
baselines) that degrades the image quality.
A second
image was the images
at 105.2 GHz, with a spectral resolution of 159 m s 1 andsurface brightness proﬁle. For reference, the dashed red curveteredshows themade with a robust parameter of 0.5
elliptical thetapercontrast
to
k and
to an
enhanceof faint,
small-scalein themodela disk.
midplanetemperature
proﬁle derivedstructurefrom a representativeThe
total bandwidth of 0.117 GHz. The data were calibrated using
create a circular 30 mas beam with negligible sidelobes. Bothgray curve in the bottom left reﬂects the proﬁle of the synthesized beam.
disk.
These
data
were
cleanedusing
superuniform
weighting,rethe provided data reduction script and CASA version 4.3. Upon
images are consistent (within the resolution differences) and00
00
sulting. a beam of 0.48 ⇥ 0.26 at PA = 18 . The reconstructed inspecting the visibilities, the amplitudes of the spectral window
have rms noise levels around 35 μJybeam−1inand panelazimuthally
averaged
image is shown in the centralof Fig.
2. into a radial surface brightness
centeredat 113.1
GHz showedanomalous
behaviour
Akimasa 3.Kataoka(Heidelberg
University),
workshop,Ishigaki
Island,Sep. 26-30,
2016and we deproﬁle. Japan-Germany Planet & Disk
RESULTSTW HyaHD 97048∆δ [arcseconds]

HL TauALMA Partnership 2015•

Andrews et al. 2016van der Plas et al. 2016

Rings are common in dust:•

Dust rings appear for any stages (HL Tau: <1-2 Myr, HD 97048: 3 Myr,TW Hya: 10 Myr)•

Are there gaps also in gas?

•

Grain growth at rings/gaps?

•

Comparison with IR images?

3 /25

Ring formation mechanisms
HL TauALMA Partnership 2015•

Planet-inducing gaps (e.g.,
Kanagawa et al. 2015, see his talk)•Enhanced growth at snowlines(Zhang et al. 2015)•

Sintering-induced fragmentation ofdust grains at snowlines (Okuzumi
et al. 2016, see his talk)•

MHD instabilities (e.g., Flock et al.
2015, see talk by H. Klahr)•

Secular gravitational instability(Takahashi and Inutsuka 2014,2016, see his talk)

Akimasa Kataoka (Heidelberg University), Japan-Germany Planet & Disk workshop, Ishigaki Island, Sep. 26-30, 20164 /25

– 12 –
(b)
(a)

(c)
(b)

HL TauD1 B1

Gas gaps?
ALMA Partnership 2015

The Astrophysical Journal Letters, 808:L3 (10pp), 2015 July 20

D2 B2

D5B5 D6 B6

D2

D5B5 D6 B6HCO+

Gas model•

Correlation between the dust andgas gaps•

Is HCO+ really trace the gas?

Figure 3. Panel (a) shows the deprojected 1.0 mm B6+B7 image of
HL Tau (see Section 3.1.3); the angular resolution is 38.6 × 19.3 mas (P.A .
−20 ◦.7). Rings for which a full range of ellipse parameters could be ﬁt arelabeled horizontally (solid and dashed lines), while the less distinct rings arelabeled vertically (dotted lines). Panels (b) and (c) show cross-cuts at P.A.
=138° through the continuum peak of the 1.0 mm continuum and spectral
index images shown in Figures 2(e) and (f) (positive values of distancecorrespond to the SE portion of Figure 2(e)). In panel (c) the gray region
delineates the statistical 1σ spectral index uncertainty; it does not account for
the absolute ﬂux uncertainty. For the fully ﬁtted rings, panels (b) and (c) showdashed lines for the locations of dark rings and solid lines for bright rings. The
ﬁtted offsets from the continuum peak (Table 2) have been taken into account.
D5B5 D6 B6
D2
Panel (d) shows the same cross-cut as panel (b) but on a Planck brightness
temperature (TB) scale. Panels (b) and (d) are shown on a log scale on the yaxis. The dashed curve on panel (d) shows a representative power law for TB as
a function of radius with an exponent of −0.65 extending from the B1 peak; it
Akimasa Kataoka (Heidelberg University), Japan-Germany Planet & Disk workshop,
is not a ﬁt. Ishigaki Island, Sep. 26-30, 2016•(c)

most of the outﬂoto spatially resolv
gas disk for thechannel maps shoblueshifted versus
tion near the syst
Keplerian velocity
range of 2.0 tocontinuum disk s
To further explor
from the 1″. 1 resoof the lines show
HCN(1-0) are on
absorption is nonincrease in absor
steeper rise on theblueshifted outﬂoon the continuumi ≈ 47°. Self-abs
responsible for b
deﬁcit of observa
absorption for thevelocity of 7.0 ±velocity of the sy
Under the ass
noting that the ve
at ΔV ± 5 km s−1(7.0 km s−1) at athe enclosed massof the range prev
However, it is cle
side, the velocity
have a contributi
D’Alessio 2000)
coupled with a phcomplex HCO+(HL Tau disk instellar mass.

Is there too much continuum At 2.9 mm we3.
into two compone
subtraction?
see Forgan et al.

file of the HCO+ integrated intensity in the disk around HL Tau observed

separated by 273
separation is 8% s
for a circular, fac
This is likely an i
require future ob
Forgan et al. (201
5 /25
(a putative
third

Hsi-Wei Yen et al., 2016

Grain size variation in gaps
9

TW Hya observed with ALMA
8

40

Band4
Band6
Band4+6
Td(R)Tbr [K]20
T10=28K

10

T10=22K

Ricci et al. 2010

5

Fig. 3. Millimeter dust opacity for the adopted dust model. Left top panel: dust opa•
n(a) ∝ a−q between
amin = 0.1 µm and amax . Diﬀerent curves are for diﬀerent val
composite spheres made of astronomical silicates (≈10% in volume), carbonace
references to the optical constants). Left bottom panel: β between 1 and 3 mm as a
3. Millimeter
dustfor
opacityfor theadoptedust opacity at 1 mm as function of βFig.
between1 and 3 mm
the same
grain
dist
−q
2
n(a)
∝
a
between
a
=
0.1
µm
and
a
mincm per gram of dust
max
shown. In the plots the unit of measure for the dust opacity iscomposite spheres made of astronomical sil•
references to the optical constants). Left botto
dust opacity at 1 mm as function of β betwee
shown. In the plots the unit of measure for th

Two-band, high resolution
observation

3.2
3.0
2.8
2.6

Spectral index is low at dust
gaps : grain size is smaller atin the midplanethein a protoplanetarygaps. disk is much higher than in Natta eαthe surface. At millimeter wavelengths, where the disk is mostly by the s
optically thin to its own radiation, the midplane total emission tral inde
2.2
dominates over that of the surface(althoughtheinsurface
dust the disk
Mdu
in themidplanea protoplanetary
plays a crucial role for the heatingofthe disk).
As a consesible tow
2.0
thesurface.
Atmillimeter
wavelengths,
Figure 1. (a) and (b) show ALMA continuum images at 145 GHz (band 4) and 233 GHz (band quence,6), rewe can extract informationfrom ouronlyradiation,
on since
optically
thinanalysis
to its own
the itm
spectively. The ellipse
1.8at the bottom-left corner in each panel shows the synthesized beam. (c) showsthethedust opacity of the midplane, dominatesand so when
wethatconsiderthesurface
very(alth
fla
over
of
the
′′ 3) forcombined image of bands 4 and 6 with the MFS method. The inset indicates a close-up view (0.′′ 3 × 0.
dust
opacity
we will refer only
toplays
the midplanecomponent
files.ofH
Tsukagoshi,
Nomura,Muto
2016
a crucialroleetforal.,
theforheating
1.6
rest of the paper.
tionsfrompeemphasis of the central structure.
The10
contour indicatesand 150σ. (d)index
020 130, 140,30
40shows the spectral
50 thewe Andrews
can extractetinformation
See also Nomura etquence,al. 2016,
al. 2016
W
For the dust grains in the disk thesurfaceassumedthemidplane,same 1996;
map derived from the MFS method.
Radius [au]dust we
opacityof theand soAndrewchemical composition and shapedust
as forthe midplanegrains,opacity
we
will
refer
only
to
the m
Akimasa Kataoka (Heidelberg University), Japan-Germany& Disk workshop,
IshigakiSep. 26-30,
6/252009).
whilePlanet
we assumed
for their
size Island,
distribution
for a2016
and
a
min
max

2.4

Comparison with IR obs.

The Astrophysical Journal Letters, 820:L40 (5pp), 2016 April 1

Andrews et al.

e Astrophysical Journal Letters, 820:L40 (5pp), 2016 April 1 Akiyama et al.

Andrews et al.

November 23 and 0.7 mm on the latter two executions. The

ovember 23 total
and on-target
0.7 mm integrationon the lattertwo ∼2
executions.
The
time washr.
al on-target integration
hr.
These rawtime
data waswere∼2calibrated
by NRAO staff. Afterphasecorrectionsby fromwaterstaff.
vaporAfterradiometer
These raw applying
data were
calibrated
NRAO
measurements,
the
data
were
time-averaged
into2
s integraplying phase corrections from water vapor radiometerand ﬂagged for problematic antennas and times. The
easurements, tions
the data
were time-averaged into 2 s integrabandpass response of each spectral window was calibrated•
ns and ﬂagged
and Thetimes.
The scaleusingforthe problematic
observations ofantennas
J1058+0133.
amplitudendpass responseof each spectral
window wascalibrated The
was determinedfrom J1037–2934
and J1107–4449.
complex gainof the system
was calibratedusing theing the observationsof response
J1058+0133.
The amplitudescale
frequent
observations
ofJ1103–3251.
Althoughas determined from J1037–2934 and J1107–4449. Theimages
generated offromdata wasare relatively
freeusingof artifacts
mplex gain response
thethesesystemcalibrated
the andrecover the integrated ﬂux density of the target (1.5 Jy), folding
quent observations
J1103–3251.
Althoughimagesof shortin additionalof
ALMA
observations witha higher density•
nerated fromantennathese spacings
data areimproves
relatively
free ofartifacts andthe imagereconstruction.
To that
we calibrated
three(1.5archival
ALMA data
cover the integrated
ﬂuxend,densityof the target
Jy), folding
observationsof TW Hya,2012 May20, 2012
Novemberadditional ALMA
observations
withfroma higherdensityof short
20,
and
2014
December
31,
using
16,
25,
and
34
antennastenna spacings improves the image reconstruction.
spanning baselines from 15 to 375 m. The ﬁrst two observaTo that end,
wehadcalibrated
three
ALMA centered
data
tions
four 59 MHz
widearchival
spectral windowsatFigure 1. Synthesized image of the 870 μm continuum emission from the TW
servations of333.8,
TW Hya,2012
20,
2012TheNovember
335.4,from345.8,
andMay347.4
GHz.
latter had two
Hya disk with a 30 mas FWHM (1.6 au) circular beam. The rms noise level is•, and 2014 235
December
31, using16, and25, 349.4
and GHz),34 antennas
MHz windows(at 338.2
one 469 MHz∼35 μJy beam−1. The inset shows a 0 2 wide (10.8 au) zoom using an image
with
ﬁner
resolution(24×18mas,
or
1.3×1.0
au,
FWHMbeam).
window
(at
352.0
GHz),
and
one
1875
MHz
window(atanning baselines from 15 to 375 m. The ﬁrst two observaGHz). wide
J1037–2934
was windows
employed asa gain calibrator,
ns had four338.4
59 MHzspectralcenteredatarcsecSynthesized image 0.03
of the 870
μm continuum emission from the TW
and Titan and 0.15
3C 279arcsec(May 20), Ceres and J0522-364 Figure 1.Resolution:
Resolution:
3.8, 335.4, (November
345.8, and
347.4
GHz.
The
latterhad
two
a 30 mas FWHM (1.6 au) circular beam. The rms noise level is20), or Ganymede and J0158+0133 (December 31) Hya disk with −1
5 MHz windows
338.2
and 349.4
GHz), one469 MHzserved(atas ﬂuxor bandpass
calibrators.
The weather
for these ∼35 μJy beam . The inset shows a 0 2 wide (10.8 au) zoom using an image
ndow
(at
352.0
GHz),
and
one
1875
MHz
window(atobservations
wasof
excellent,
PWV
levelsof 0.5–1
Theiswith
Figure 1. H-band
PI image
TW Hyawith
in ADI
mode.
North
is up mm.
and east
to ﬁner resolution (24×18 mas, or 1.3×1.0 au, FWHM beam).
Akiyamaetal.
2015
Andrews et al. 2016combined
integration
95 minutes.
The basicmask
8.4 GHz).
wascircle
employed
as awasgain
calibrator,
the left.J1037–2934
The
dark on-target
ﬁlled
at the time
centerindicatesa software
calibration
was(Mayasdescribed
above.
we compared
Letters,
802:L17(5pp), 2015
AprilAs1 a check,
Akiyama et al.
with r and= 0″.Journal
2.3C 279
dhe Astrophysical
Titan
20),
Ceres
and
J0522-364
theamplitudes
from
each
individual
data
set
on
overlapping
ovember 20), or Ganymede and J0158+0133 (December 31)
spatial frequencies and found exceptional consistency.
rved as ﬂux orThebandpass
Theeachweather
for thesecalibratedcalibrators.
visibilities
fromobservation
were
with
a
total
integration
time
for
the
PI
image
of
390
s. shifted
The data
servations was
excellent,
with
PWV
levels
of
0.5–1
mm.
The
to account for the proper motion of the target and thensets on-target
werecombined
takeninAngularDifferential
Imaging(ADI)frommodembinedintegration
time channels
was 95 withminutes.
Theemission
basic
after excisingpotentialwith wasa net
rotation
ofmodest
12°.
spectrallines.
Somemade with alibration
asﬁelddescribed
above.
As improvementsa check, we werecomparedAll
unﬂaggeddata
were
corrected
forﬁeld
rotationroundofphase-only
self-calibration.
Continuum
imagesat aande amplitudes from each individual data set on overlappingmeanfrequencyof imaging
345.9 GHzmethod(867 μm)
were generated
byThe
standard(Hinkleyet al. 2009)
atialintegrated.
frequencies
andinverting
found exceptional
consistency.
Fourierthevisibilities,
deconvolving
withamultiapplied
to the polarimetricdata, including
corrections for
Thewascalibrated
visibilities
from eachobservation
were
scale,
multi-frequency
synthesis
versionof shifted
the CLEAN
distortionand proper
ﬂat-ﬁelding,
using
the
Image
Reductionaccount
foralgorithm,
themotionofthetargetandand then32restoring with a synthesized thenbeam. Alland
)with
as in
previous
SEEDS
publications
Analysis
Facility (IRAF
and imaging
wereperformed
with fromthe CASA
mbinedafter calibration
excisingchannelspotential
emission
package(v4.5.0).
(e.g.,
Hashimoto
et
al.
2011;
Muto
et
al.
2012).
Correctionsforectral lines. Some modest improvements were made with a
After
some
experimentation,
wesettledonananalysisoftwopolarizationof theContinuum
Nasmyth HiCIAO
und instrumentalof phase-only
self-calibration.
images atinstrumentaimages made from the same composite data set. The ﬁrst used aappliedwith GHzthe(with
Mueller-matrices
technique,ean werefrequencyof 345.9(867μm) were
generatedby which
Briggsweightinga robust
parameterof0) to provideapolarization
characteristics
al.While2008).
urierquantizes
invertingthe visibilities,
deconvolving
with eta multi24×18
mas synthesized
beam (at (Joos
P.A.=78°).
this PI2
providesfrom
enhanced
it comesatthe
theUCLEAN
cost
a dirty
Figure 2. (top) High-resolution (24×18 mas beam) synthesized imageale, wasmulti-frequency
synthesisofQ and, whereare oforthogonal
calculated
Q 2resolution,+ Uversion
described in Section 2, deprojected into a map in polar coordinates to more
beam
with
∼20%
sidelobes
(due
to
the
sparsecoverageatlonggorithm,
andthen restoringwitha synthesized
beam.
All
linearpolarizations,
and
the
ﬁnal
PI
proﬁlewasobtained
after
substructure.
(bottom)The0″.azimuthally
averaged radialbaselines)that
degradesquality.
Athesecondimage
was proﬁleeasily
igure 2. Polarized intensity
proﬁlesof theTW Hya the
diskimagein the H-band(left),
andazimuthalbrightness
imagesview
at r =the0″. 2disk(∼11AU), 0″. 5 (∼27AU), and8librationandimaging
were
performed
withCASA
surfacebrightness
proﬁle.
Forreference,thedashedred
curveshows the∼43 AU),
respectively(right).
Thebars show
1σ. The numbers
1–3
the ellipticalleft panel
denotezones for which a separate polarized intensity slope
applying
10×with
10aerrorpixel
smoothing
disk.
made
robustparameterof to0.5theandinentireantaperthetothree radial
midplanetemperature proﬁle Planet
derived froma representativemodel disk.
The
Akimasa
Kataoka(Heidelberg
University),
Japan-Germany&
Diskworkshop,Ishigaki
Island, Sep. 26-30, 2016
ﬁt.
ckage
(v4.5.0).
create a circular 30 mas beam with negligible sidelobes. Both

HiCIAOALMA

IR traces the surface
layer
Is there any
correlation?
(see talk about
SPHERE results by
Roy van Boekel)

gray curve in the bottom left reﬂects the proﬁle of the synthesized beam.

7 /25

Lopsided or rings?

The highly asymmetric crescent-shaped dust
grainsrocky structure revealed by the 0.44-mm ALMA conThe Astrophysical Journal Letters, 783:L13 (6pp), 2014 March 1
within tinuum (Fig. 1) traces emission from millimeterL14-2 sized dust grains and is located between 45 and M. Fukagawa et al.
[Vol. 65,
mstellartymied 80 AU (T9 AU) from the star. The azimuthal
ift and extent is less than one-third of the ring, with noA
mediate detected flux at a 3s level (2.4 mJy per beam) in
1 AU = the northern part (fig. S1). The peak emissione Sun), has a very high signal-to-noise ratio of ~390, andre high the contrast with the upper limit on the opposite
t to the side of the ring is at least a factor of 130. The
ems for complete absence of dust emission in the north ofllisions IRS 48 and resulting high contrast make thelocities crescent-shaped feature more extreme than earlier
articles dust asymmetries (10, 13). The spectral slope
A&A proofs: manuscript no. hd97048-gap
ly drift a of the millimeter fluxes Fn [0.44 mm comre they bined with fluxes at lower frequencies n (14)]B
Fukagawaal.(5pp),2013
van der Marel etAndrews
al. et2013
Perez et al. 2014
e. This is only 2.67
T 0.25(FJournaln a), etsuggesting
The Astrophysical
820:L40
2016that
April 1al.
n º Letters,
sistentFig. 1.millimeter-sizedgrains(15)
thethe The
uvclip/superuniform
MEM model
Dust continuum
mapGHz(890 two!m)executions.
fordisksuperuniformofNovember 23
and at0.7 336mmonthedominate
latter
HD
97048
total
on-target
integration
time
was
∼2
hr.
ossibleHD 142527.
0.44-mm
However,temperaturetheThecontinuumcolor scale emission.
shows the brightness
on
These
raw
data were calibrated by NRAO staff. After
HL
Tau
TW Hya 1.0
125,radiometer
10, 15, andscale.
black
contours
denoteressurea logarithmicgas traced
by ThethephaseCO
6-5 line
from
the
same
b
1.0=
1.0
applying
corrections
fromwaterTvapor
measurements,
the datathe
weretime-averaged
into 2ofs integra20
K,
while
the
white
one
denotes5"level.
Thesize
thesynthehe dust ALMA data
set indicates a Keplerian disk protions and ﬂagged for problematic antennas and times. The
sized beam is shownat the left cornerofspectral
the imagewitha calibrated
white ellipse
Fig. 2. Moment
0 (left) and 1 (right) maps in 13 CO 0.5(upper) and C18 O
0.5 was0.5
bandpass response
eachdisk
windowe bump 00 file characteristicof a ofgas
with
an
inner
00
ı
(= 55
! 48 au) witha major-axis
PA of 57 .
of 0: 39 ! 0: 34 using
J = 3–2 (lower). The contours in the left panels show the 5 " levels.
theauobservationsof J1058+0133.
The
12 amplitude
ap dust cavity aroundthecentralstar(Fig. 1B).
CO 6-5 scale
was determinedfrom
J1037–2934
and J1107–4449.
TheIn
the right0.0panels, the first moment maps are presented
for the emis0.0
0.0
gain responseof theusing the).
emission complex
is detecteddown
to systema 20 was
AUcalibrated
radius,sion detected above 5 ". The contours for the integrated intensity are
frequent observationsof J1103–3251.
Although wereimages 380 m
Cycle 0. The maximum
and minimum
baselines
meter/ which is consistent
with
the
hot
CO
ring
at
30
AU
generated from these data are relatively freeof artifacts andoverplotted,
steps. The cross−0.5−0.5starting from 5 " and increasing by 5 "−0.5
and 20(14).
m, respectively,
andthere
thedensity
latterthe integrated
ﬂux
of the corresponded
target(1.5Jy), folding to thea highThisrecover
indicatesthatisindeedstill
somein each panel denotes the position of the central star. The synthesized00
in additional
ALMA
observations witha higher density ofof short.
Thelargestangular
scale
of
the
detectablecomponent
10
beam size −1.0
is displayed with a white ellipse in each −1.0
panel, and is 0:00 43
spacings
improves
reconstruction.
r-sized CO insideantenna
the dust
hole,
withtheaimage
significant−1.0 drop
C ! 0:00 37 with a PA of 50ı for both 13 CO and C18 O.
To thatinend,
calibrated
three archival
ALMAschedulingdatareported
thisweletter
consistedfour
he observations
star of the gas
surfacedensityinside
of
~25
Tof
52012
AU.
observationsof TW Hya,
from 2012
May 20,Novemberblocks The
over simultaneous
the 20,periodfrom2012
August.
The0.5 correand 2014
December
31,
using
25,
and 34 1.0
antennasz) conALMA
lineJuneand16,tocontinuum
0.0
−0.5
−1.0
1.0
0.5
0.0
−0.5
−1.0
1.0
0.5
0.0
−0.5
−1.0
spanningtobaselines
from
15polarizations
to 375 m. The ﬁrst two
observa∆α [arcseconds]∆α [arcseconds]∆α [arcseconds]
lator
was
configured
store
dual
in
four
separate
his can observations
doubt
relativetions leave
had fourno
59 MHzwideabout
spectralthewindows
centered at
Figure 1. Synthesized image of the 870 μm continuum emission from the TW
333.8,
335.4,
345.8,
and
347.4
GHz.
The
latter
had two
spectralwindows
withabandwidth
of
469
MHz
and withetbeam.al.
2016
ALMA
Partnership2015
van der Plas et al. 2016
Hya disk with a 30 masAndrews
FWHM (1.6 au) circular
The rmsnoise level isapping position of
gas
and
dust.
235 MHz windows (at 338.2 and 349.4 GHz), one 469 MHz∼35 μJy beam . The inset shows a 0 2 wide (10.8 au) zoom using an image
Figure1.
ALMA
observations
and1gas
2.MHz
ReconstructedHD
97048
for theband
7 data.
The intensity scale for all images is in units ofofJydust
beam. Toemission
highlightfor the disks surroundprovidingchannelspacingof 0.122
MHz
withofﬁner
resolution(24×18
mas,ALMA
or 1.3×1.0
au, FWHMbeam).
. 3840 channels,
The observations
indicatethatlargewindow(at 352.0athus
GHz),and one Fig.
1875
window(at images
Table
1.
Left
panels:dust
continuum
emission(colorscale) and dust brightne
thespectral
small-scale
structure we show
(from left to right) images reconstructed with progressively smaller beams. The left panel shows the image
GHz).
J1037–2934
was employed
as a gain calibrator,
Note
that
the
effective
resolutionis(0.11 kms"1 ). 338.4
8 [dismillimeter-sizedgrainsare
distributedinanasymmoment
0
map,
contours
start
and
are
spacedby
3σ,where σ is the rms nois
and Titan and 3C 279 (May 20),reconstructed
Ceres and J0522-364
using superuniform weighting. The central panel shows the superuniformly weighted
reconstructed image resulting from clipping−1"1
1 km s . in dynamic range between the panels is due to(November
20),
GanymedeandsJ0158+0133(December)micrometerbecauseof 31)
Hanninglower
a factorof #2 orthat
(#0.2
= 3.1
× by
metricstructure,
but
thekm
small
all
baselines
below
160
k . Finally, the right panel shows the MEM model image. The di↵erence
served as ﬂux or bandpass calibrators.
Theweather
for
these
flux
lossfourincurredby clipping
the shortest baselines for the central panel, and due to the smaller
reconstructedbeam
for istheavailable
right panel.
(A color
version of thisfigurein the online journal.)
sizedThe
grainsare spreadthroughout
the
Tomm.
a largesmoothing.
centralfrequencies
windows
areobservations
was excellent,
withfor
PWVtheselevelsring.
of 0.5–1
The
on-targettime
was 95 GHz,
minutes.
Thebasicknowledge,
theonlyintegration
known
mechanismthater 330.588,
disk our329.331,
342.883,
and 342.400
respectively,• combined
calibration was as described above. As a check, we compared
13 range of ⇡ 1200 and a RMS of 0.20 mJy beam 1 . We 2.3. ALMA Cycle 1 band 3 data
could
this separationin lines
thedynamical
distribution
nfraredamplitudes
from each individualdata
set on overlapping
CO J = 3–2,
allowing
us generate
to theobserve
molecularofImage Properties for Dust Co
spatial frequencies and found exceptional
consistency.
18
shift
all
imagesusing
thepropermotioncorrection
found
in
van
large
and
grainsisaeach
long-lived
gas
inCtheO Jof=the
3–2,
andCSsmall
J =7–6. fromThe
results
ofweretheshifted
CS obserThe calibrated
visibilities
observation
Target
R.A.a
Deca
Leeuwen(2007)and these are shown in Figs. 1 and 2 for thetoaccountforthepropermotionofthetarget
and
then
bump
in
the
radialandazimuthal
din atvations
an pressure
will be combined
reportedelsewhere. The
quasars
3C
279 andcontinuum
emission.
after excising channels withpotential emission
from We applied the self-calibration solutions ALMA Early Science Cycle 1 observations were conducted on
Sν b
rm
+
rection.
The
reasonthat
dust
particles
gettrappeddiusor
1. IRSemission
48 dusttoandgas observations.
spectrallines.
Some modest
improvements
werefrom
made thewithFig.
awhereas
QSO J1924"2914
weretargetedas bandpass
calibrators,
December 2013 with 72.6 seconds of total time on HD 97048
obtained
continuum
the HCO
J=4-3 and 1The
(J2000)(J2000)
(Jy)
(Jy
bea
12Continuum
roundof Akimasa
phase-only
atand
a subtracted
in pressure
bumps
isweretheirself-calibration.
driftwith respect
to images
thedataesolved
Kataoka(Heidelberg
University),
Japan-Germany
Planet&DiskALMA
workshop,Ishigaki Island,seeSep.
26-30, 2016
(Program
ID 2012.1.00031.S,
also Dunham
et al. 2016). The
CO
J=3-2
the continuum
using
inclineddiskaroundIRS 48 asemission
observed
with
8 /25
the amplitude
andmonitored
throughobservations
meanphasefrequencyof 345.9
GHz (867 μm)
were generated
by
0.15

−1

0.20

0.00

0.02

0.04

0.06

0.08

ownloaded from www.sciencemag.org on June 6, 20130.10

∆δ [arcseconds]

0.05

0.00

0.01

0.02

0.03

What physical mechanism does make this difference?

0.04

How to measure dust and gas mass?
Gas mass
Bulk Dust & Gas Masses
infraredmm continuum

7

DUST FROM SUB-MM CONTINUUM
Sub-mm flux density(ALMA observations)GAS FROM CO ISOTOPOLOGUES

Source distance(150-200 pc)

Williams & Best (2014)

Dust massF⌫ dMdust =
⌫ B⌫ (Tdust )•Flux (observed value)

Isothermal disk
dust emission(T =20 K)

grids, color-coded by gas mass. The two panels show di↵erent values for the [C18 O]/[CO] isotopologue ratio, the ISM valueof 550 (left) and 3⇥ reduced abundance (right), to account for isotope-selective photodissociation. The 11 Lupus disks withboth lines detected are plotted as white circles and the 25 Lupus disks with only 13 CO detections are plotted as black circles
with arrows indicating 3 upper limits on C18 O. Error bars include both the statistical uncertainties (Table 3) and a 10% flux
calibration error. Stars show locations of the stacked non-detections (Section 5.3); error bars are roughly the size of the symbol.

•

If we can measure H2, of coursethat’s the best…

•

CO is used as a tracer of the gas•

conversion: a factor of 3 lower
than ISM.

Opacity (taken single value)

Temperature (assumed to be
isothermal or related to L*)Howmaterial available for planet
formation evolves with time → inputs•

Williams and Best 2014, Ansdell et al. 2016

Figure 4. 13 CO and C18 O 3–2 line luminosities and associated gas masses (Section 5.2). Colored points show the WB14 model

pected given the undetected continuum, but the absence
Mgas . 0.2 MJup (Figure 4), for an average gas-to-dustof continuum emission is surprising given the sensitivratio of .13 for disks detected in the continuum but unity of the stacked image. We measured a mean signal
detected in both 13 CO and C18 O (Figure 3).
of 0.08 ± 0.06 mJy, which gives a 3 upper limit on the
average dust mass of individually undetected continuum
5.4. Transition Disks
sources of ⇠6 Lunar masses (0.03 M ), comparable toTransition disks (TDs) are protoplanetary disks withdebris disk levels (Wyatt 2008). The stark contrast beinner cavities and/or annular gaps in their dust and gas
tween the detected and undetected continuum sources
distributions. TDs were initially identified by the mid(see Figure 3, top panel) suggests that protoplanetary
IR deficits in their Spectral Energy Distributions (SEDs),
disks evolve quickly to debris disk levels once disk cleardust
indicating a lack of warm micron-sized dust grains close
ing begins (Alexander et al. 2014).
to the central star (see review in Espaillat et al. 2014).
We then stacked the 24 sources detected in the continInner disk clearings and dust rings were later confirmed
13
18
uum and CO, but not C O. We measured a continuumwith resolved mm continuum images (e.g., Andrews et al.
13mean signal of 45.25 ± 0.20 mJy and a CO mean signal2011). TDs are now considered to be sites of ongoing disk
1of 586 ± 27 mJy km s (Figure 5, upper left panel). Inevolution, and their dust and gas distributions may be interestingly, the stacking also revealed a significant meansome cases signposts of embedded planets clearing gaps
signal for C18 O of 132 ± 20 mJy km s 1 (Figure 5, lower
in the disk (e.g., Pinilla et al. 2012; Pérez et al. 2014; vanleft panel). The stacked continuum flux corresponds toder Marel et al. 2015, 2016a; Canovas et al. 2015)
Mdust ⇠ 19 M and the stacked line fluxes correspond
Our ALMA continuum images show several Lupus
to Mgas ⇠ 0.4 MJup (Figure 4), giving an average gas-todisks with signatures of inner dust cavities. Three disks
dust ratio of only ⇠7 for sources detected in the contin(2MASS J16083070-3828268, RY Lup, Sz 111) show
uum and 13 CO, but not C18 O (Figure 3).
clearly resolved dust rings with cavity diameters of ⇠0.800
Finally, we stacked the 27 sources that were detected in(⇠80 AU radius at 200 pc). 2MASS J16083070-3828268
13
18
the continuum, but undetected in both CO and C O.
and Sz 111 were previously recognized as TDs from theWe measured a continuum mean signal of 9.53 ± 0.13
mid-IR deficits in their SEDs (Merı́n et al. 2008). AlmJy. The stacking revealed a significant mean signal
though RY Lup was not previously identified as a TD
for 13 CO (Figure 5, upper right panel), but not C18 O
by its SED (Manset et al. 2009), this is likely because
5, lowerright panel);the stacked
gas fluxes were
itsSep.
strong 10µm silicate
emission feature, seen in its IRS
Akimasa Kataoka (Heidelberg University), Japan-Germany (Figure
Planet&Disk
workshop,Ishigaki
Island,26-30,
2016
1
1
54 ± 7 mJy km s and 3 ± 8 mJy km s , respectively.
spectrum (Kessler-Silacci et al. 2006), washes out theSingle grain opacity• cm
2 g−1 at 1000
distance(fixed)
(10
GHz)
•

C18O

2

13CO

• Parametric disk models

9 /25• Simple CO chemistry (freeze out + photodiss.)

1206

Disk surveys
HERNÁNDEZ ET AL.

This could indicate that the low disk presence
Velorum cluster is abnormal for its evolutionar
disk fraction from IR excess• Today’s talk is based on theronmental effects, such as strong stellar winds
results
of from the ! Velorum system, cdiation fields
physical mechanism for the low disk frequency.
the disk-bearingstars SMA
in the !survey)
Velorum clu•of Taurus(1-3Myr,
SED slopes smaller than the median values ofby Andrews
2013
stellargroups plottedetinal.
Figure10 suggesting th! Velorum cluster have a higher degree of dus
the median
IRAC by
SEDAnsdell
slopes for the d•ticular,Lupus(1-2 Myr)NGC 2362, the k Orionis cluster, the OB1b su
al. 2016
theet! Velorum
cluster are "1.72, "1.60, "1.7spectively (with a typical error of 0.06).
Studying the young
Myr)• Chameleon(2 (2–3
Myr)
byopen cluster N
et al. (2007) showed that high-mass stars (O-typ
Pascucci et al. 2016
the primordial disks of lower mass members
within !0.5 pc of the high-mass star. We fin
the ! Velorum
cluster. Myr)
Using the•forUpper
Sco (5-11
byphotometV"J > 3:5 (!M2orlater),
we find a disk fre
Barenfeld
et
al.
2016
3% at a projected distance of 0.25–1.0 pc; incentral objects of the cluster contaminate the oused to select photometric candidates (x 3). Th
Hernandez et al. 2007
dial disk is located at projected distance of !
projected distance (>1.0 pc), the disk frequenc
Fig. 11.—Fraction of stars with near-infrared disk emission as a function of
the age of the stellar group. Open circles represent the disk frequency for stars in2%). This suggests that the relative fast dispers
the T Tauri ( TTS) mass
rangeKataoka(!K5 orlater), derived
usingJapan-Germany
JHKL observations:
Akimasa(Heidelberg
University),
Planet & Disk workshop,
Ishigakicluster
Island, Sep.
26-30, 2016 by the strong
10/25! Velorumis producedraauri stars, 50 K for Herbig Ae stars and for each main-sequence
we use a temperature corresponding to the blackbody fit todisc emission, i.e. the same method as applied in Section 3.1.
ically thin to the stellar emission, the debris discs are heatedserved massive (≈0.5 M⊕ ) debris discs across ages from 10 to abov1000 Myr, and investigate possible evolutionary trends in mass dis
tribution. Nonetheless, it is possible that disc mass remains nearlconstant on the main sequence. The maximum mass of ≈0.5 M⊕

Time evolution of dust mass
protoplanetary disks

debris disks

Panic et al., 2013

Kataoka(Heidelberg
University),
Japan-Germany
Planet & Disk
workshop,Island, Sep. 26-30,
2016
ure 3. Dust masses of Akimasa
circumstellar
discs
derived basedon observed(sub)millimetre
fluxestowardsIshigaki
pre-main-sequenceand main-sequencestars.
11Obser/25

Lupus survey•

89 disks observed (96%complete)•

62 continuum detections•

35 13CO detections•

11 C18O detections•

0.3" beam (50 AU)•

0.3 Mearth of dust

Ansdell et al., 2016

Akimasa
University),
Japan-Germany& Disk workshop, Ishigaki Island, Sep. 26-30, 2016
Figure 2. 890 µm continuum imagesof the 61Kataoka
Lupus disks(Heidelberg
detected in our ALMA
Cycle 2 program(i.e., excludingPlanetSz 82, which

12/25

Survey of Upper Sco– 26 –•

106 disks observed•

continuum detections•

Barenfeld et al., 2016
Fig. 3.— Images of the 0.88 mm continuum for the 58 primordial and debris/evolved transitional
disks detected (> 3 ) in the Upper Sco sample. Each image is centered on the fitted position of
the source and is 300 ⇥ 300 in size.

•

53 of 75 primordial disks•

5 of 31 debris/evolved disks

12CO detections•

26 of 76 primordial disks•

0 of 31 debris/evolved disks•

0.34" beam (50 AU)•

0.1 Mearth of dust

Akimasa Kataoka (Heidelberg University), Japan-Germany Planet & Disk workshop, Ishigaki Island, Sep. 26-30, 201613/25

Stellar mass - dust mass relationlog Mdust (Mearth)Taurus
Lupus
ChaI
UpperSco

2•

Mdust ∝ M∗1.3−1.9

1•Taurus, Lupus, andChamaeleon I (1-3 Myr)share the same relation•

Upper Sco (5-11 Myr) has
steeper relation

0-1
Tdust fixed to 20K

-2
-1.0

-0.5
log M* (Msun)

0.0

0.5

Pascucci et al., 2016

— The Mdust − M∗ relation in four diﬀerent regions: Taurus (green solid line), Lupus (red dot-dashedhamaeleon I (black dashed line), and Upper Sco (light blue dotted line). These relations are obtainedg a fixed dust temperature of 20 K (see also Table 4). For Chamaeleon I we also plot the individualk masses. Note that the ∼10 Myr-old Upper Sco has a steeper Mdust − M∗ relation than the otherming regions.
Akimasa Kataoka (Heidelberg University), Japan-Germany Planet & Disk workshop, Ishigaki Island, Sep. 26-30, 201614/25

Dust mass of disks

Dust mass cumulative distributions for Lupus,
Taurus, and Upper Sco disks around host stars with M⇤ >0.1 M (Section 6.2). The average dust masses for each region are given for reference. The distributions were calculated•

Lupus and Taurus (1-3Myr) share the same dust
mass range•

Lupus and Taurus (15Mearth) has 3× higher mass
than Upper Sco (5 Mearth,5-11 Myr)

Figure 8.

Akimasa Kataoka (Heidelberg University), Japan-Germany Planet & Disk workshop, Ishigaki Island, Sep. 26-30, 2016

15/25

6

Lupus survey

Gas-to-dust ratio

Figure 3. Dust masses (top), gas masses (middle), and gas-to-dust ratios (bottom) for the continuum-detected sources in our•

Gas-to-dust ratio
varies from 1 to 100•

Typical g/d ratio is~10 (cf. ISM ~ 100)•

Quick gasdissipation or CO
depletion?

Ansdell et al., 2016

Lupus sample. Dust masses and associated uncertainties are from Table 2; error bars are smaller than the symbol size unlessshown. Gas masses and upper
limitsare taken(Heidelberg
from Table 3;error bars represent
the range ofpossiblegas masses,
as described
Akimasa
Kataoka
University),
Japan-Germany
Planet& Diskworkshop,Ishigaki Island, Sep. 26-30, 2016
in Section 5.2. Gas-to-dust ratios and error bars are directly derived from the dust masses and range of possible gas masses. Blue

16/25

6

Lupus survey

Gas-to-dust ratio•

89 disks observed (96% complete)•

62 continuum detections•

Stacking analysis of undetected sources →< 6 Lunar masses (0.03 Mearth)•

Rapid disk dissipation once thedissipation begins?

Figure 3. Dust masses (top), gas masses (middle), and gas-to-dust ratios (bottom) for the continuum-detected sources in our•

Gas-to-dust ratio
varies from 1 to 100•

Typical g/d ratio is~10 (cf. ISM ~ 100)•

Quick gasdissipation or CO
depletion?

*g/d is affected bygrain growth(Tsukamoto et al.
2016) See his talkAnsdell et al., 2016

Lupus sample. Dust masses and associated uncertainties are from Table 2; error bars are smaller than the symbol size unlessshown. Gas masses and upper
limitsare taken(Heidelberg
from Table 3;error bars represent
the range ofpossiblegas masses,
as described
Akimasa
Kataoka
University),
Japan-Germany
Planet& Diskworkshop,Ishigaki Island, Sep. 26-30, 2016
in Section 5.2. Gas-to-dust ratios and error bars are directly derived from the dust masses and range of possible gas masses. Blue

17/25

Gas mass measurement
doi:10.1038/nature11805

rming a planetary systemffrey A. Blake5, Joel D. Green6, Sean M. Andrews7,
9, Chunhua Qi7, Colette Salyk10 & Ewine F. van Dishoeck11,12

HD line @ 112 µm
data with existing molecularobservations
to set new
Mass measurements
in protoplanetarydisksconstraints
withhe disk massobserved
within 100 AU, whichis theHershel
most fundamental quan-

HD measured

CO measured

TW Hya> 5.0×10−2 Msun

4.7×10−4-6×10−2 Msun*

DM Tau1.0-4.7×10−2 Msun

1.4×10−3 Msun*

GM Aur

2.5-20.4×10−2 Msun

< 0.35×10−3 Msun*

3

that determines whether planets can form. The disk mass alsoa
3.8

HD J = 1 → 0

TW HyaCO J = 23 → 22

Flux (Jy)

3.7

3.6

3.5
112

113

114

*Thi et al. 2010, Gorti et al. 2011, Dutrey et al. 1996

b 4.2

PACS spectra of our sample in the region around the HD line. The continuum (blue, dashed line) was determined by fitting apolynomial to regions on either
the feature
OH 2sideΠ1/2of 9/2→ 7/2(grey fill). The red arrow indicates the location of the HD line.

Flux (Jy)

4.0•

HD line : good tracer of gas mass•

HD-measured gas mass > COmeasured gas mass•

CO freeze-out, photodissociation, or
chemical depletion

HD J = 2 → 1

3.8

3.6

3.4
56.0

56.5
Wavelength (μm)

57.0

ure 1 | Herschel detection of HD in the TW Hya protoplanetary disk.
he fundamental J 5 1 R 0 line of HD lies at ,112 mm. On 20 November
1, it was detected from the direction of the TW Hya disk at the 9s level. Thel integrated flux is (6.3 6 0.7) 3 10218 W m22. We also report a detection ofwarm disk atmosphere in CO J 5 23 R 22 with a total integrated flux of
218(red) to 22
Gaussian
spectra(black).
FWHM andcentral wavelength were fixed at theW m the. continuum
The J 5 1subtracted
R 0 lineof HD
wasThepreviously
detected
60.7) 3line
10fitsal and theoretical values, respectively. The thicker red line indicates the region over which the RMS deviation of the residuals
d.
1 uncertainty
is described
Sectiongas
2. cloud exposed to radiation
heThe
InfraredSpacecalculation
Observatory
in ainwarm
m nearby stars27. Other transitions have also been detected in shocked
ons associated with supernovae and outflows from massive stars28,29.
multaneous observations of HD J 5 2 R 1 are shown. For HD J 5 2 R 1,
ind a detection limit of ,8.0 3 10218 W m22 (3s). We also report action of the OH 2P1/2 9/2 R 7/2 doublet near 55.94 mm with an integrated
Akimasa
Kataoka(Heidelberg University), Japan-Germany Planet & Disk workshop, Ishigaki Island, Sep. 26-30, 2016
include theobserved thermalof (4.93 6 0.27) 3 10217 W m22. The spectra

Bergin et al. 2013, McClure et al. 201618/25

Macc(X-shooter) vs. Mdust (ALMA)

correlation between Ṁacc and Mdisk•

Accretion rate from UV
excess in VLT/X-Shooter•

g/d is assumed to be 100•

Consistent with theviscous accretion theory•

Transition disks havelower Macc.

Fig. 4. Logarithm of Ṁacc vs. logarithm of Mdisk = 100 · Mdisk,dust . SymManara et al. 2016bols are as in Fig. 1. Also here, the best fit with the procedure by Kelly(2007) overlaps with the least-squares best fit. The dashed lines represent di↵erent ratiosof Kataoka
Mdisk / (Heidelberg
Ṁacc , as labeled.
Akimasa
University), Japan-Germany Planet & Disk workshop, Ishigaki Island, Sep. 26-30, 201619/25

mm-wave polarization of disksNo. 2, 2007

POLARIZED EMISSION FROM T TAURI DISKSThe Astrophysical Journal, 809:78 (15pp), 2015 August
The Astrophysical10
Journal, 809:78 (15pp), 2015 August 10

1093

Kataoka et al.

Magnetic Field

1.Thermal emission from
elongated dust grains alignedwith magnetic field

Thermal emission

Linearpolarization→ a probe of the magnetic
field structure
Figure 7. Same as Figure 5, but for the case of the ring-shaped
Same as Figure
disk.
5, but for the case of the ring-shaped pro
Cho and Lazarian 2007Figure 7.protoplanetaryFig. 11.—Simulated observations. Degree of polarization is calculated for the radiation from the disk interior only.

disk symmetry axis and the line of sight. We plot the direction ofpolarization for three different wavelengths and two different
viewing angles. The lines represent the direction of polarization.
Since we assume that magnetic field is azimuthal, the directionof polarization is predominantly radial (see Fig. 10, bottom). In
Figure 11 we show similar plots for radiation from the disk interior only. For k > 100 !m, the polarization patterns in Figure 11
are very similar to those in Figure 10. But near the disk edges,
Figure 10 shows a larger degree of polarization than Figure 11,
because the emission from the disk interior is very weak there
compared with that from the disk surface layer. For k < 100 !m,the polarization patterns in Figure 11 are very different from thosein Figure 10, because polarized emission from the disk surface layer
dominates that from the disk interior. Note that since the degreeof polarization of emission from the disk surface layer is very sensitive to the maximum grain size in the surface layer, the results fork < 100 !m should be very sensitive to the maximum grain sizein the surface layer.
While the polarimetry of the spatially resolved accretion disks
is promising with a new generation of instruments (see x 6.2), atpresent one can study disk magnetic fields with unresolved accretion disks. Below we provide predictions for this case. Figure 12
shows a SED for such a disk for four different viewing angles.
When " ¼ 90 (i.e., for edge-on disk), the inner part of the disk
(i.e., region close to the star) is invisible due to high opacity.
Therefore, the SED truncates for k < 10 !m. When " ¼ 0 (i.e., for
4
Figure 8. Same as Figure 5, but for model
Adisk),
in thecaseFigure
ofemission
the 8.lopsided
asprotoplanetary
Figure5, but disk.
for model
The object
A in theis opticallycase of thethinlopsided
everywhere.
protoplanetary disk
face-onthe polarized
isSamezero as expected.
Finally, Figure 13 shows the change of the degree of polarization
for selected wavelengths. The left panel shows the degree of polarization for total emission, while the right panel shows that for
Fig. 12.— SED for four different viewing angles. When " ¼ 90 (i.e., for edge-ondisk), inner part of the disk (i.e., region close to the star) is invisible because it isradiation from the interior only. The degree of polarization is large

2.Self-scattering of thermal dust
emission→ measuring the grain size at
midplane

Kataoka et al., 2015

grain density distribution is assumed to be grain density distribution
is assumed
be corresponds to point B polarizedpolarized
ring.toThis
in Figurering.
6. By
Thocculted by the outer part of the disk. Therefore, the SED truncates for k < 10 !m.
contrast, Ishigaki
the vectors
areSep.
in thedirection
contrast,in thetheinnervect
When " ¼ 0 (i.e.,
for face-ondisk), theradialpolarized emission
is zeroas expected,
Akimasa Kataoka (Heidelberg
University),
Japan-Germany
Planet&Disk
workshop,Island,2016
2see
2 configuration
That is, we do not
thick dottedorthick dashedlines in Fig. 212d.
becausethe assumed
magnetic26-30,
field
is perfectly azimuthal.
20
/25
⎤
⎤
⎡
⎡
2
⎤
⎤
⎡
⎡
⎞
⎞
⎛
⎛
⎛
⎞
⎛ polarization⎞
ring. This is due to the net ﬂux frompolarization
the azimuthalring.
4Synthetic Observations

Figure 1. The ring state: Self-consistent radiative
Fig. 4. Radial profiles of space and time averaged surface density (solid line), magnetic pressure (dashed line) and deviation of Keplerian rotation(dotted line) for model D2G_e-2 (left) and model D2G_e-4 (right). The background contour color shows the space and time averaged value of 1.3
the mm (top row), and simulated ALMA observatio
Elsasser number. The red solid line and annotation show the region of super Keplerian rotating gas. At this location, large particles are getting
minimal displayed polarization degree is 1%, i.e., ttrapped.

1.Thermal emission from elongated dust grains aligned with magnetic field
L4

G. H.-M. Bertrang et al.

right edge-on). The color map shows the total (unpowith the spatial resolution indicated by the beamcharacteristic polarization structure in all of the th

SmoothVortex

A 574, A68 (2015)
Fig. 5. 3D plot of the toroidal magnetic field of models D2G_e-2 (left) and D2G_e-4 (right).

Fig. 6 (bottom right), shows that these large-scale structures correlate with a minimum in vorticity. These structures could potentially concentrate particles, similar to concentrations of particles
in fully ionized MRI turbulence (Dittrich et al. 2013).

vortices is around −0.3 [Ω−1 ], which matches those generated by
the RWI (Meheut et al. 2012b, 2013).
We summarize that both models developed surface density
enhancements. In the fully turbulent model D2G_e-4 the enhancements are stronger, but with a smaller spatial extent thanfor model D2G_e-2. In the fiducial model D2G_e-2 we observea gap followed by a bump in surface density. Inside the bump,vortices are formed by the RWI with a lifetime of around 40 local orbits.

Surface density and vorticity maps of model D2G_e-2 arepresented in Fig. 7 after 800 and 1045 inner orbits. Both outputs
show the clear gap and following jump in surface density, visible
between 50 and 80 AU. The structures are mostly axisymmetric,
with small azimuthal fluctuations of about 4%. In this model weobserve the formation of a large vortex inside the ring structure 4. Radiative transfer and simulated ALMA maps
at 60 AU (see Fig. 7 bottom), with a surface density enhancement and a corresponding low-vorticity region. The radial extent The fiducial model showed the generation of a gap and bumpof the vortex is around 2 scale heights, which corresponds to a in surface density, visible as ring structures located at the outerradial extent of 10 AU at this location. The azimuthal extent is edge ofthe dead1.
zone.
Theringdecreaseand Self-consistentfollowing enhancement
Figure transfer
2. The vortex
state: of
Asthein Fig.
1. Theemiss
toro
FigureThe
state:
radiative
simulations
polarized
around 10 H, corresponding to an extent of 50 AU. We tracked of the surface density emerges thanks to a zonal-flow-analog
both orientations
the CASA
simulated
ALMA
1.3 mm (top row), and simulated ALMA observations(bottominrow;v5.4.2,
bandobserva
6, contwo vortices in model D2G_e-2 with similar strength over the structure, which is located at the transition between the MRI
disk.
polarization
degreeis amount
1%,face-on
i.e., the3 level of ALMA) at three di↵erent dis
full simulation. The first has a lifetime of around 40 local orbits dead minimal
and active displayedzone. The modelwith a reduced
dust
right
The colorshowswethetotal (unpolarized) intensity which is overplotted by poat 60 AU, starting after 350 inner orbits and lasting for 200 inner showed
fullyedge-on).
evolved turbulence.
In mapthis section
investigate
orbits. The second cycle starts at around 850 and is still present and compare
these
two
model
configurations
whenobservedwith the spatial resolution indicated by the beam size given as white ellipses. The toroidald a distance of
pc. Themaps
for model
D2G_e-4
at 100the final
output;see areFig.calculated
7. The vorticity
amplitude
inside(left)
the andwith ALMA.
characteristic polarization structure in all of the three orientations in the simulated ALMA obs

Bertrang, Flock, and Wolf 2016

lent structure in D2G_e-4 and the gap in D2G_e-2 are conserved.

A68, page
5 of 13Island, Sep. 26-30, 2016
Akimasa Kataoka (Heidelberg University), Japan-Germany Planet & Disk workshop,
Ishigaki

21/25

Synthetic Observations

SYNTHETIC IMAGES OF A FACE-ON TRANSITION DISK
2.Self-scattering of thermal dust emissiont = 1 Myr●

Reference model:
1 Myr of dust evolution
Polarization
is emitted
onlyfrom ice)
locations– Dust mixture(silicate,carbon,where amax = 150µm (λ=870 µm)– λ = 870 μm (band 7), face-on disk (i = 0°)–•~ 150 μm•

In a disk with a planet, three polarization
rings are expected.
2
2P=

Stokes I (continuum)

Polarized intensity PI

PI √ Q + U=
IIPolarization degree P

λ = 870 μm

Pohl et al. 2016, submittedPohl, Kataoka, et al., 2016

Adriana Pohl (MPIA Heidelberg) – Planet Formation 2016 – May 17, 2016

Akimasa Kataoka (Heidelberg University), Japan-Germany Planet & Disk workshop, Ishigaki Island, Sep. 26-30, 2016

7

22/25

Summary

A&A proofs: manuscript no. hd97048-gap•

There are rings and lopsided disks.
0.05

0.10

0.15

0.20

0.00

The Astrophysical Journal Letters, 820:L40 (5pp), 2016 April 1

superuniform

0.02

0.04

0.06

0.08

0.00

0.01

0.02

0.03

0.04

Andrews et al.

uvclip/superuniform

MEM model

November 23 and 0.7 mm on the latter two executions. The
total on-target integration time was ∼2 hr.
These raw data were calibrated by NRAO staff. After
1.0
1.0
applying phase corrections from water 1.0vapor radiometermeasurements, the data were time-averaged into 2 s integrations and ﬂagged for problematic antennas
and times. The
0.5
0.5
0.5
bandpass response of each spectral window was calibratedusing the observations of J1058+0133. The amplitude scale
was determined from J1037–2934 and 0.0
J1107–4449. The
0.0
0.0
complex gain response of the system was calibrated using thefrequent observations of J1103–3251. Although images
generated from these data are relatively −0.5
free of artifacts and
−0.5
−0.5
recover the integrated ﬂux density of the target (1.5 Jy), folding
in additional ALMA observations with a higher density of short
−1.0
−1.0
−1.0
antenna spacings improves the image reconstruction.
To that end, we calibrated three archival ALMA data
observations of TW Hya, from 2012 May 20, 2012 November
20, and 2014 December 31, using 16, 25, and 341.0antennas
0.5
0.0
−0.5
−1.0
1.0
0.5
0.0
−0.5
−1.0
1.0
0.5
0.0
−0.5
−1.0
∆α [arcseconds]∆α [arcseconds]
spanning baselines from 15 to 375 m. The ﬁrst two observa-∆α [arcseconds]
tions had four 59 MHz wide spectral windows centered at
Figure 1. Synthesized image of the 870 μm continuum emission from the TW
333.8, 335.4, 345.8, and 347.4 GHz. The latter had two
Hya disk with a 30 mas FWHM (1.6 au) circular beam. The rms noise level is
235 MHz windows (at 338.2 and 349.4 GHz), one 469 MHz∼35 μJy beam−1. The inset shows a 0 2 wide (10.8 au) zoom using an image
Fig. 2. Reconstructed imageswithofﬁnerHDresolution
97048(24×18
for themas,
ALMA
band 7 data. The intensity scale for all images is in units of Jy beam 1 . To highlightor 1.3×1.0 au, FWHM beam).
window (at 352.0 GHz), and one 1875 MHz window (atthe small-scale
structure we show (from left to right) images reconstructed with progressively smaller beams. The left panel shows the image
338.4 GHz). J1037–2934 was employed
as a gain calibrator,
reconstructedsuperuniform weighting. The central panel shows the superuniformly weighted reconstructed image resulting from clipping
and Titan and 3C 279 (May 20),
Ceres and using
J0522-364(November 20), or Ganymede and J0158+0133
31) k . Finally, the right panel shows the MEM model image. The di↵erence in dynamic range between the panels is due toall baselines(December
below 160
served as ﬂux or bandpass calibrators.
Theweatherfor
theseflux loss incurred by clipping the shortest baselines for the central panel, and due to the smaller reconstructed beam for the right panel.
observations was excellent, with PWV levels of 0.5–1 mm. The
10
combined on-target integration time was 95 minutes. The basic0.88 mm continuum images, 0.34’’ resolution
calibration was as described above. As a check, we comparedM⇤ fundamentallycorrelation
betweenCycle 1 band 3 data
dynamicalof ⇡ 1200 and aandRMS
of 0.20 mJy explains
beam 1the. We
2.3. ALMA
the amplitudes from each individual
data set onrange
overlapping
giant planet frequency and host star mass identified inspatial frequencies and found exceptional
consistency.
shift allimages using the properthe
motioncorrection
found
van2006; Johnson et al.
exoplanet
population(Endl inet al.
The calibrated visibilities from eachobservation
were shifted
2007;
Bonfils
et al.12013;
Bowleret al. 2010). This is
I. Introduction
Leeuwen(2007)
and
these
are
shown
in
Figs.
and
2
for
the
to account for the proper motion of the target and thenbecause core growth is more efficient both in higher-masscontinuum
emission.
the self-calibration solutions ALMA Early Science Cycle 1 observations were conducted on
combined after excising channels withpotential
emission
II. Our
Survey from We applied
disks (e.g., Thommes et+al. 2008; Mordasini et al. 2012)
spectral lines. Some modest improvements
weremadethewitha
1 December
obtainedfromcontinuum
emission
to higher-mass
the HCO stars
J=4-3
and
and around(e.g.,
Kennedy& Kenyon 2013 with 72.6 seconds of total time on HD 97048
III. Disk Fluxes
12 Continuumround of phase-only self-calibration.
imagesat a subtracted2008).
Thus the sourcesin the using
upper rightof FigureID
6 2012.1.00031.S, see also Dunham et al. 2016). The(Program
CO J=3-2
data
and
the
continuum
emissionand Masses
mean frequency of 345.9 GHz (867 μm) weregenerated byare more likely to form giant planet cores before the gas
arrayconfiguration provided baselines ranging between 15.8 and
the CASA withtaska uvcontsub,
resultingin a per-channel
Fourier inverting the visibilities, deconvolving
multidisk dissipates,
allowing the RMS
cores toofaccrete
substantial
IV. Disk Evolution
462.9
and
beam 1 respectively.
The
resulting
momentscale, multi-frequency synthesis 19.5
versionof23.7the mJy
CLEAN
gaseous envelopes and become gas giant planets. meters. During the observations the perceptible water vaLupus disks
also exhibit
dispersion
in theMdust,
algorithm, and then restoring with0,a1synthesized
beam.
All
V.
Summary
por inatmosphere
were stable within 5% of the median value
and 8 maps and spectra are shownin Figs.
3 and 4a large
for thespanning ⇠2 orders of magnitude for a given M⇤ . Ancalibration and imaging were performed
with the CASA +
12
of
0.535
mm.
Three
of
the four spectral windows of the ALMA
CO
J=3-2
and
HCO
J=4-3.
drews et al. (2013) noted that the similarly large dispackage (v4.5.0).
persion in Taurus is likely a consequence of
the inherent
correlator
were configured in TDM to maximise the sensitivity
After some experimentation, we settled on an analysis of two
diversity in disk temperatures, dust opacities,
andevoimages made from the same composite data set. The ﬁrst used afor continuum observations (128 channels over 1.875 GHz uslutionary states across the region. The large dispersion
Briggs weighting (with a robust parameter of 0) to provide aable bandwidth).
These spectral windows were centred at 101.9
5
in Lupus may result from di↵erent environments
and/or
2.2.1.
Imagingthethislong baselines
24×18 mas synthesized beam (atP.A.=78°).
Whilestates(24×18
across mas
thebeam)
Lupus
I–IV
clouds.
To GHz and 113.1 GHz. The fourth spectral window
GHz,
103.9
provides enhanced resolution, it comes at the cost of a dirty
Figure 2.evolutionary(top) High-resolution
synthesized
image
this,2,were-derived
M⇤ wascorrelation
usFigure 8. Dust mass cumulative
distributions
described testin Section
deprojected
into athe
mapMindustpolarvs.
coordinates
to morebeam with ∼20% sidelobes (due to the sparse coverage at long
configuredin
FDM to target the 12 CO J=1-0
line forandLupus,
cenTaurus, and Upper Sco disks around host stars with 1M⇤ >
ing
only
Lupus
III
sources;
we
chose
Lupus
III
becauseiteasily
view
the
disk
substructure.
(bottom)Theazimuthally
averagedradialWe alsoreconstructedbaselines) that degrades the image quality.
A second
image was the images using only baselines above 160 tered at 105.2 GHz,a spectral
resolution
ofmasses
159 mforseachand
0.1 Mwith(Section
6.2). The
average dust
resurface brightness
For reference,
red curveshows
the discontainsproﬁle.
the most
sourcesthein dashedour sample
andis moremade with a robust parameter of 0.5
elliptical thetapercontrast
to
k and
to an
enhanceof faint,
small-scalein themidplanetemperature
proﬁle toderivedfroma representative
model
disk.
The
gion
are
given GHz.
for reference.
The distributions
were calculatedtantcompared
thestructureotherclouds,thus
possiblyinbandwidtha difa
total
of
0.117
The
data
were
calibrated
using
create a circular 30 mas beam with negligible sidelobes. Bothgray curveferent
in the bottom
left reﬂects We
the proﬁlethe synthesized
beam.(1.4±0.5)
using the Kaplan-Meier estimator to include upper limits andenvironment.
foundof consistent
slope
These
data were
CASA version
images are consistent (within the disk.
resolutiondifferences)and cleaned using superuniform weighting, re- the provided datathereduction
line widths script
indicateand
1 confidence
intervals. 4.3. Uponanddispersion
(1.1
±
0.3)
valuestowithinerrors,indi0000
sulting
at PAthat
= 18
.
The
reconstructed. a beam of 0.48 ⇥ 0.26cating
have rms noise levels around 35 μJybeam−1inthe visibilities,
amplitudes
thesurveyed
spectralin window
the large dispersion in Lupusinspecting
is an intrinsic
Taurus andtheUpper
Sco, have ofbeen
the suband panel
azimuthally
averageda radial surface
image is shown in the centralof Fig.
2. diskintopopulation
propertyoftheresultingbrightness
from a rangemmwithsimilar anomalous
sensitivity andcompleteness.
Tauruscentered
at
113.1
GHz
showedbehaviour
andwedeAkimasa 3.Kataoka(Heidelberg University),
Disk workshop,
Island,26-30,
2016
proﬁle. Japan-Germanyof initial disk conditionsPlanet(e.g., core&angularmomentum) Ishigaki
has a similar
age to Sep.
Lupus (⇠1–2
Myr)
and its Class II
RESULTSTW HyaHD 97048∆δ [arcseconds]

HL TauALMA Partnership 2015•

Andrews et al. 2016van der Plas et al. 2016

Surveys show the disk evolution in Myr time scale
4

Figure 2. 890 µm continuum images of the 61 Lupus disks detected in our ALMA Cycle 2 program (i.e., excluding Sz 82, which

was observed by Cleeves et al., in prep), ordered by decreasing continuum flux density (as reported in Table 2). Images are
200 ⇥200 and the typical beam size is shown in the first panel.

•

Barenfeld, et al. 2016, Andsell et al. 2016, Pascucci et al. 2016

ALMA polarization as a new tool of measuring grain growth

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