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See detailCO Gas Inside the Protoplanetary Disk Cavity in HD 142527: Disk Structure from ALMA
Perez, S.; Casassus, S.; Ménard, F. et al

in Astrophysical Journal (2014), 798

Inner cavities and annular gaps in circumstellar disks are possible signposts of giant planet formation. The young star HD 142527 hosts a massive protoplanetary disk with a large cavity that extends up to ... [more ▼]

Inner cavities and annular gaps in circumstellar disks are possible signposts of giant planet formation. The young star HD 142527 hosts a massive protoplanetary disk with a large cavity that extends up to 140 AU from the central star, as seen in continuum images at infrared and millimeter wavelengths. Estimates of the survival of gas inside disk cavities are needed to discriminate between clearing scenarios. We present a spatially and spectrally resolved carbon monoxide isotopologue 2-1 line of $^12$CO, $^13$CO, and C[SUP]18[/SUP]$O obtained with the Atacama Large Millimeter/submillimeter Array (ALMA). We detect emission coming from inside the dust-depleted cavity in all three isotopologues. Based on our analysis of the gas in the dust cavity, the $^12$CO emission is optically thick, while $^13$CO and C[SUP]18[/SUP]$O emissions are both optically thin. The total mass of residual gas inside the cavity is \~1.5-2 M $_Jup$. We model the gas with an axisymmetric disk model. Our best-fit model shows that the cavity radius is much smaller in CO than it is in millimeter continuum and scattered light observations, with a gas cavity that does not extend beyond 105 AU (at 3$\sigma$). The gap wall at its outer edge is diffuse and smooth in the gas distribution, while in dust continuum it is manifestly sharper. The inclination angle, as estimated from the high velocity channel maps is 28 \plusmn 0.5 deg, higher than in previous estimates, assuming a fix central star mass of 2.2 M $_&sun;$. [less ▲]

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See detailSpatially Resolved HCN J = 4-3 and CS J = 7-6 Emission from the Disk around HD 142527
van der Plas, G.; Casassus, S.; Ménard, F. et al

in Astrophysical Journal Letters (2014), 792

The disk around HD 142527 attracts a great amount of attention compared to others because of its resolved (sub-)millimeter dust continuum that is concentrated into the shape of a horseshoe toward the ... [more ▼]

The disk around HD 142527 attracts a great amount of attention compared to others because of its resolved (sub-)millimeter dust continuum that is concentrated into the shape of a horseshoe toward the north of the star. In this Letter we present spatially resolved ALMA detections of 4-3 and CS J = 7-6 emission lines. These lines give us a deeper view into the disk compared to the (optically thicker) CO 7-6 coming from a protoplanetary disk. Both emission lines are azimuthally asymmetric and are suppressed under the horseshoe-shaped continuum emission peak. A possible mechanism for explaining the decrease under the horseshoe-shaped continuum is the increased opacity coming from the higher dust concentration at the continuum peak. Lower dust and/or gas temperatures and an optically thick radio-continuum reduce line emission by freezing out and shielding emission from the far side of the disk. [less ▲]

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See detailCharacterization of BoHV-5 field strains circulation and report of transient specific subtype of bovine herpesvirus 5 in Argentina
Maidana, S. S.; Ladelfa, M. F.; Perez, S. et al

in BMC Veterinary Research (2011), 7

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