The Circumestellar Disk of the B0 Protostar Powering the HH 80-81 Radio Jet

Girart, J. M.; Estalella, R.; Fernández-López, Manuel; Curiel, S.; Frau, P.; Galván-Madrid, Roberto; Rao, Ramprasad; Busquet, G.; Juárez, Carmen

doi:10.3847/1538-4357/aa81c9

Cited by 26 publications

(37 citation statements)

References 78 publications

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“…The brightest blueshifted emission appears in the south-east side of the disk, while the redshifted emission arises from the north-west side of the disk. This is in agreement with previous lower angular resolution and less sensitive observations (Fernández-López et al 2011b;Carrasco-González et al 2012;Girart et al 2017). We note that there is also significant red/blueshifted emission in the SW/NE side of the disk.…”

Section: The Ggd 27-mm1 Disk-jet Systemsupporting

confidence: 93%

“…In addition, observed velocity gradients in the molecular gas perpendicular to the HH80-81 radio jet have been interpreted as rotating motions (Fernández-López et al 2011b;Carrasco-González et al 2012;Girart et al 2017). Definitive evidence of a compact disk around IRAS 18162-2048 comes from ALMA observations at 1.14 mm with an angular resolution of ∼ 40 mas (∼ 56 au), which reveal a compact dust disk clearly perpendicular to the radio-jet (Girart et al 2018, see Fig.…”

Section: Introductionmentioning

confidence: 99%

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Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1

Añez-López

Osorio

Busquet

et al. 2020

ApJ

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Recent high-angular resolution ( 40 mas) ALMA observations at 1.14 mm resolve a compact (R 200 au) flattened dust structure perpendicular to the HH 80-81 jet emanating from the GGD 27-MM1 high-mass protostar, making it a robust candidate for a true accretion disk. The jet/disk system (HH 80-81/GGD 27-MM1) resembles those found in association with low-and intermediate-mass protostars. We present radiative transfer models that fit the 1.14 mm ALMA dust image of this disk which allow us to obtain its physical parameters and predict its density and temperature structure.Our results indicate that this accretion disk is compact ( R disk 170 au) and massive ( 5 M ), about 20% of the stellar mass of 20 M . We estimate the total dynamical mass of the star-disk system from the molecular line emission finding a range between 21 and 30 M , which is consistent with our model. We fit the density and temperature structures found by our model with power law functions. These results suggest that accretion disks around massive stars are more massive and hotter than their low-mass siblings, but they still are quite stable. We also compare the temperature distribution in the GGD 27-MM1 disk with that found in low-and intermediate-mass stars and discuss possible implications on the water snow line. We have also carried out a study of the distance based on Gaia DR2 data and the population of young stellar objects (YSOs) in this region, and from the extinction maps. We conclude that the source distance is within 1.2 and 1.4 kpc, closer than what was derived in previous studies (1.7 kpc).

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Section: The Ggd 27-mm1 Disk-jet Systemsupporting

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1

Añez-López

Osorio

Busquet

et al. 2020

ApJ

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“…Figure 1 shows the position of the 1.14 mm continuum sources detected with ALMA. We detected a cluster of 25 contin- uum sources, including the three previously know sites of massive star formation: MM1/ALMA 5, MM2(W)/ALMA 13 and MM2(W)/ALMA 17 (Fernández-López et al 2011a;Girart et al 2017, here on MM1, MM2(W) and MM2(E), respectively). The remaining 22 sources are new detections (Table A.1) and are distributed mainly north and southeast of MM1.…”

Section: Observationsmentioning

confidence: 74%

“…MM1 powers the HH80-81 radio jet with a dynamical time of ∼ 10 4 years (Masqué et al 2012). MM2(E) is even in an earlier stage (Qiu & Zhang 2009;Fernández-López et al 2011a;Girart et al 2017). This suggests certain coevality of the lowmass cluster members with the two massive YSOs and therefore a smaller age dependece of the protostellar disk masses (see Appendix D.3).…”

Section: Clustering and Mass Segregationmentioning

confidence: 99%

Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1

Busquet

Girart

Estalella

et al. 2019

A&A

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Context. Most stars form in clusters, and thus it is important to characterize the protostellar disk population in dense environments to assess whether the environment plays a role in the subsequent evolution; specifically, whether planet formation is altered with respect to more isolated stars formed in dark clouds. Aims. Investigate the properties of the protostellar disks in the GGD 27 cluster and compare them with those obtained from disks formed in nearby regions. Methods. We used ALMA to observe the star-forming region GGD 27 at 1.14 mm with an unprecedented angular resolution, 40 mas (∼ 56 au) and sensitivity (∼ 0.002 M ⊙ ). Results.We detected a cluster of 25 continuum sources, most of which are likely tracing disks around Class 0/I protostars. Excluding the two most massive objects, disks masses are in the range 0.003-0.05 M ⊙ . The analysis of the cluster properties indicates that GGD 27 displays moderate subclustering. This result combined with the dynamical timescale of the radio jet (∼ 10 4 years) suggests the youthfulness of the cluster. The lack of disk mass segregation signatures may support this too. We found a clear paucity of disks with R disk > 100 au. The median value of the radius is 34 au, smaller than the median of 92 au for Taurus but comparable to the value found in Ophiuchus and in the Orion Nebula Cluster. In GGD 27 there is no evidence of a distance-dependent disk mass distribution (i. e., disk mass depletion due to external photoevaporation), most likely due to the cluster youth. There is a clear deficit of disks for distances < 0.02 pc. Only for distances > 0.04 pc stars can form larger and more massive disks, suggesting that dynamical interactions far from the cluster center are weaker, although the small disks found could be the result of disk truncation. This work demonstrates the potential to characterize disks from low-mass YSOs in distant and massive (still deeply embedded) clustered environments.

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“…Previous pre-ALMA sub-arcsecond angular resolution observations reveal the presence of a ∼1000 au rotating molecular flattened structure perpendicular to the radio jet (Gómez et al 2003;Fernández-López et al 2011b;Carrasco-González et al 2012;Girart et al 2017) and of a compact, barely resolved dust emission from the putative disk (Fernández-López et al 2011a;Carrasco-González et al 2012;Girart et al 2017). The dynamical mass (star and disk) derived from these observations is roughly 10-20 M (e.g., Girart et al 2017). These observations put an upper limit for the dust linear polarization of 0.8% at circumstellar scales.…”

Section: Introductionmentioning

confidence: 92%

Resolving the Polarized Dust Emission of the Disk around the Massive Star Powering the HH 80–81 Radio Jet

Girart

Fernández-López

et al. 2018

ApJL

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Here we present deep (16 µJy beam −1 ), very high (40 mas) angular resolution 1.14 mm, polarimetric, Atacama Large Millimeter/submillimeter Array (ALMA) observations towards the massive protostar driving the HH 80-81 radio jet. The observations clearly resolve the disk oriented perpendicular to the radio jet, with a radius of 0. 171 (∼291 au at 1.7 kpc distance). The continuum brightness temperature, the intensity profile, and the polarization properties clearly indicate that the disk is optically thick for a radius of R 170 au. The linear polarization of the dust emission is detected almost all along the disk and its properties suggest that dust polarization is produced mainly by self-scattering. However, the polarization pattern presents a clear differentiation between the inner (optically thick) part of the disk and the outer (optically thin) region of the disk, with a sharp transition that occurs at a radius of ∼ 0. 1 (∼170 au). The polarization characteristics of the inner disk suggest that dust settling has not occurred yet with a maximum dust grain size between 50 and 500 µm. The outer part of the disk has a clear azimuthal pattern but with a significantly higher polarization fraction compared to the inner disk. This pattern is broadly consistent with self-scattering of a radiation field that is beamed radially outward, as expected in the optically thin outer region, although contribution from non-spherical grains aligned with respect to the radiative flux cannot be excluded.

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The Circumestellar Disk of the B0 Protostar Powering the HH 80-81 Radio Jet

Cited by 26 publications

References 78 publications

Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1

Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1

Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1

Resolving the Polarized Dust Emission of the Disk around the Massive Star Powering the HH 80–81 Radio Jet

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