/ftp/cats/A+A/648/A33



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J/A+A/648/A33       ALMA continuum images of TW Hya              (Macias+, 2021)
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	list.dat
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Beginning of ReadMe : J/A+A/648/A33 ALMA continuum images of TW Hya (Macias+, 2021) ================================================================================ Characterizing the dust content of disk substructures in TW Hya. Macias E., Guerra-Alvarado O., Carrasco-Gonzalez C., Ribas A., Espaillat C.C., Huang J., Andrews S.M. <Astron. Astrophys. 648, A33 (2021)> =2021A&A...648A..33M (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Stars, pre-main sequence ; Protostars ; Interferometry ; Millimetric/submm sources Keywords: accretion, accretion disks - protoplanetary disks - planets and satellites: formation - stars: pre-main sequence - radio continuum: general - techniques: interferometric Abstract: A key piece of information to understand the origin and role of protoplanetary disk substructures is their dust content. In particular, disk substructures associated with gas pressure bumps can work as dust traps, accumulating grains and reaching the necessary conditions to trigger the streaming instability. In order to shed some light on the origin and role that disk substructures play in planet formation, we aim to characterize the dust content of substructures in the disk of TW Hya. We present Atacama Large Millimeter Array (ALMA) observations of TW Hya at 3.1mm with  50 milliarcsecond resolution. These new data were combined with archival high angular resolution ALMA observations at 0.87mm, 1.3mm, and 2.1mm. We analyze these multiwavelength data to infer a disk radial profile of the dust surface density, maximum particle size, and slope of the particle size distribution. Most previously known annular substructures in the disk of TW Hya are resolved at the four wavelengths. Inside the inner 3au cavity, the 2.1mm and 3.1mm images show a compact source of free-free emission, likely associated with an ionized jet. Our multiwavelength analysis of the dust emission shows that the maximum particle size in the disk of TW Hya is >1mm. The inner 20au are completely optically thick at all four bands, which results in the data tracing different disk heights at different wavelengths. Coupled with the effects of dust settling, this prevents the derivation of accurate density and grain size estimates in these regions. At r>20au, we find evidence of the accumulation of large dust particles at the position of the bright rings, indicating that these are working as dust traps. The total dust mass in the disk is between 250 and 330M_sun_, which represents a gas-to-dust mass ratio between 50 and 70. Our mass measurement is a factor of 4.5-5.9 higher than the mass that one would estimate using the typical assumptions of large demographic surveys. Our results indicate that the ring substructures in TW Hya are ideal locations to trigger the streaming instability and form new generations of planetesimals. Description: We present images of the dust continuum emission at 0.87mm, 1.3mm, 2.1mm, and 3.1mm of the protoplanetary disk around TW Hya, obtained with the Atacama Large Millimeter/submillimeter Array. Three images at each wavelength are presented. One image is obtained using a Briggs robust weighting that provides a good balance between sensitivity and resolution (main panels in Figure 1 of the paper). Another image is obtained with a Briggs robust weighting that produces a higher angular resolution (insets in Figure 1 of the paper). The third image at each wavelength (with suffix _circularbeam) has a circular beam with FWHM=0.05" (images used in the analysis presented in the paper). All images are presented as FITS files. Objects: ----------------------------------------------- RA (2000) DE Designation(s) ----------------------------------------------- 11 01 51.91 -34 42 17.0 TW Hya = HIP 53911 -----------------------------------------------