J/A+A/642/A164 Edge-on protoplanetary disks ALMA images (Villenave+, 2020)
Observations of edge-on protoplanetary disks with ALMA.
I. Results from continuum data.
Villenave M., Menard F., Dent W.R.F., Duchene G., Stapelfeldt K.R.,
Benisty M., Boehler Y., van der Plas G., Pinte C., Telkamp Z., Wolff S.,
Flores C., Lesur G., Louvet F., Riols A., Dougados C., Williams H.,
Padgett D.
<Astron. Astrophys. 642, A164 (2020)>
=2020A&A...642A.164V 2020A&A...642A.164V (SIMBAD/NED BibCode)
ADC_Keywords: Stars, pre-main sequence ; Radio sources
Keywords: protoplanetary disks - stars: formation -
circumstellar matter - stars: variables: T Tauri, Herbig Ae/Be
Abstract:
We aim to study vertical settling and radial drift of dust in
protoplanetary disks from a different perspective: an edge-on view. An
estimation of the amplitude of settling and drift is highly relevant
to understanding planet formation.
We analyze a sample of 12 HST-selected edge-on protoplanetary disks
for which the vertical extent of the emission layers can be
constrained directly. We present ALMA high angular resolution
continuum images (0.1arcsec) of these disks at two wavelengths, 0.89mm
and 2.06mm (respectively ALMA bands 7 and 4), supplemented with
archival band 6 data (1.33mm) where available.
For most sources, the millimeter continuum emission is more compact
than the scattered light, both in the vertical and radial directions.
Six sources are resolved along their minor axis in at least one
millimeter band, providing direct information on the vertical
distribution of the millimeter grains. For the second largest disk of
the sample, the significant difference in vertical extent between band
7 and band 4 suggests efficient size-selective vertical settling of
large grains. Furthermore, the only Class I object in our sample shows
evidence of flaring in the millimeter. Along the major axis, all disks
are well resolved. Four of them are larger in band 7 than in band 4 in
the radial direction, and three have a similar radial extent in all
bands. For all disks, we derive the millimeter brightness temperature
and spectral index maps. We find that the disks are likely optically
thick and that the dust emission reveals low brightness temperatures
in most cases (<10K). The integrated spectral indices are similar to
those of disks at lower inclination.
The comparison of a generic radiative transfer disk model with our
data shows that at least 3 disks are consistent with a small
millimeter dust scale height, of a few au (measured at r=100au). This
is in contrast with the more classical value of hg∼10au derived
from scattered light images and from gas line measurements. These
results confirm, by direct observations, that large (millimeter)
grains are subject to significant vertical settling in protoplanetary
disks.
Description:
ALMA continuum observations of 12 very inclined protoplanetary disks
at several wavelengths: 0.89mm, 1.33mm and 2.06mm, which correspond to
ALMA bands 7, 6 and 4, respectively. The data were observed as part of
ALMA projects 2016.1.00460.S, 2016.1.01505.S, 2016.1.00771.S, and
2013.1.01175.S. The data were calibrated with the CASA pipeline except
for the band 7 observations of 2MASS J04202144+2813491, IRAS
04302+2247, HK Tau B, HV Tau C, and IRAS 04200+2759 which were
manually calibrated (see complete description in the paper).
The images were constructed from the calibrated visibilities with a
Briggs robust weighting parameter of 0.5, except for the band 6 image
of HH30 for which the reduction presented in Louvet et al. (2018,
robust of 0.56) is used. The images are used in all the paper, except
for Figure 4 and B.1, and table 4.
For the sources observed at two millimeter bands, we also provide maps
with a unique angular resolution in band 7 and band 4. These maps at
the restored beam resolution correspond to the fits files with '_rb'
in their title. They are used in the paper to produce Figure 4 and
B.1, and table 4.
Objects:
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RA (2000) DE Designation(s)
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04 20 21.4 +28 13 49.2 2MASS J04202144+2813491 = 2MASS J16313124-2426281
04 31 37.5 +18 12 24.5 HH30 = V* V1213 Tau
04 33 16.5 +22 53 20.4 IRAS 04302+2247 = 2MASS J04331650+2253204
04 31 50.6 +24 24 16.4 HK Tau B = WDS J04318+2424B
04 38 35.5 +26 10 41.3 HV Tau C = V* HV Tau C
04 23 07.8 +28 05 57.5 IRAS 04200+2759 = 2MASS J04230776+2805573
04 22 00.7 +26 57 32.5 Haro 6-5B = FS Tau B
04 18 58.1 +28 12 23.4 IRAS 04158+2805 = 2MASS J04185813+2812234
16 31 31.3 -24 26 28.5 2MASS J16313124-2426281 = 2MASS J16313124-2426281
11 11 10.8 -76 41 57.4 ESO-HA 569 = 2MASS J11111083-7641574
11 16 02.8 -76 24 53.2 ESO-HA 574 = 2MASS J16313124-2426281
11 04 22.8 -77 18 08.0 HH48 = HH 48
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 226 37 List of fits images
fits/* . 37 Individual fits images
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 23 I4 --- Nx Number of pixels along X-axis
25- 28 I4 --- Ny Number of pixels along Y-axis
30- 55 A26 "datime" Obs.date Observation date
57- 63 F7.3 GHz Freq ? Observed frequency
65- 69 I5 Kibyte size Size of FITS file
71- 90 A20 --- FileName Name of FITS file, in subdirectory fits
92-226 A135 --- Title Title of the FITS file
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Acknowledgements:
Marion Villenave, marion.villenave(at)univ-grenoble-alpes.fr
(End) Patricia Vannier [CDS] 27-Aug-2020