Probing the Inner Disk Emission of the Herbig Ae Stars HD 163296 and HD 190073

Setterholm, Benjamin R.; Monnier, John D.; Davies, Claire L.; Kreplin, Alexander; Kraus, Stefan; Baron, Fabien; Aarnio, Alicia; Berger, J.‐P.; Calvet, Nuria; Curé, M.; Kanaan, S.; Kloppenborg, Brian; Bouquin, J.-B. Le; Millan-Gabet, R.; E., Rubinstein, Adam; Sitko, Michael L.; Sturmann, J.; Brummelaar, Theo A. ten; Touhami, Y.

doi:10.3847/1538-4357/aaef2c

Cited by 28 publications

(42 citation statements)

References 50 publications

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“…reveal clear evidence of this same inclined ring structure whose flux is both azimuthally asymmetric and not the strongest along the major axis. In particular, the NW side of the major axis is brighter than the SE side of the disk in J-band GPI observations (see To illustrate these differences, we scaled the peak flux along the major axis of the 2016 VLT/SPHERE data and present these data as dashed horizontal lines in our which is consistent with previous near-IR interferometric observations (Tannirkulam et al 2008;Lazareff et al 2017;Setterholm et al 2018). However, our 2011 epoch data reveal the presence of no azimuthal asymmetry along the major axis in the same filter bandpass as the 2016 SPHERE observations.…”

Section: Modeling Of the Hd 163296 Disksupporting

confidence: 78%

Multi-epoch Direct Imaging and Time-variable Scattered Light Morphology of the HD 163296 Protoplanetary Disk

Rich

Wisniewski

Currie

et al. 2019

ApJ

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We present H-band polarized scattered light imagery and JHK high-contrast spectroscopy of the protoplanetary disk around HD 163296 observed with the HiCIAO and SCExAO/CHARIS instruments at Subaru Observatory. The polarimetric imagery resolve a broken ring structure surrounding HD 163296 that peaks at a distance along the major axis of 0. 65 (66 au) and extends out to 0. 98 (100 AU) along the major axis. Our 2011 H-band data exhibit clear axisymmetry, with the NW-and SE-side of the disk exhibiting similar intensities. Our data are clearly different than 2016 epoch H-band observations from VLT/SPHERE that found a strong 2.7x asymmetry between the NW-and SE-side of the disk.Collectively, these results indicate the presence of time variable, non-azimuthally symmetric illumination of the outer disk. While our SCExAO/CHARIS data are sensitive enough to recover the planet candidate identified from NIRC2 in the thermal IR, we fail to detect an object with JHK brightness nominally consistent with this object. This suggests that the candidate is either fainter in JHK bands than model predictions, possibly due to extinction from the disk or atmospheric dust/clouds, or that it is an artifact of the dataset/data processing, such as a residual speckle or partially subtracted disk feature. Assuming standard hot-start evolutionary models and a system age of 5 M yr, we set new, direct mass limits for the inner (outer) ALMA-predicted protoplanet candidate along the major (minor) disk axis of of 1.5 (2) M J . 42 While a real-time estimate of the Strehl ratio (S.R.) was not recorded for these data sets, the raw contrast for the May data was just slightly poorer than that obtained for κ And observations achieving S.R. ∼ 0.90-0.92 in H band (Currie et al. 2018b). Raw contrasts for the July data considered in our study are roughly a factor of 2.5-3 worse at 0. 4, more characteristic of performance at S.R. ∼ 0.65-0.70.

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Section: Modeling Of the Hd 163296 Disksupporting

confidence: 78%

Multi-epoch Direct Imaging and Time-variable Scattered Light Morphology of the HD 163296 Protoplanetary Disk

Rich

Wisniewski

Currie

et al. 2019

ApJ

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“…The halo contribution determination requires very short baselines, as reported in Setterholm et al (2018). These are generally not covered in our (uv) planes but the halo contribution in the H-band as constrained by the PIONIER observations is null or below 6% for all of our targets except HD 100546 (11%) and HD 169142 (8%) (see L17).…”

Section: Halo Contributionmentioning

confidence: 93%

The GRAVITY Young Stellar Object survey

Perraut

Labadie²,

Lazareff³

et al. 2019

A&A

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Context. The formation and the evolution of protoplanetary disks are important stages in the lifetime of stars. Terrestrial planets form or migrate within the innermost regions of these protoplanetary disks and so, the processes of disk evolution and planet formation are intrinsically linked. Studies of the dust distribution, composition, and evolution of these regions are crucial to understanding planet formation. Aims. We built a homogeneous observational dataset of Herbig Ae/Be disks with the aim of spatially resolving the sub au-scale region to gain a statistical understanding of their morphological and compositional properties, in addition to looking for correlations with stellar parameters, such as luminosity, mass, and age. Methods. We observed 27 Herbig Ae/Be stars with the GRAVITY instrument installed at the combined focus of the Very Large Telescope Interferometer (VLTI) and operating in the near-infrared K-band, focused on the K-band thermal continuum, which corresponds to stellar flux reprocessed by the dust grains. Our sample covers a large range of effective temperatures, luminosities, masses, and ages for the intermediate-mass star population. The circumstellar disks in our sample also cover a range of various properties in terms of reprocessed flux, flared or flat morphology, and gaps. We developed semi-physical geometrical models to fit our interferometric data. Results. Our best-fit models correspond to smooth and wide rings that support previous findings in the H-band, implying that wedge-shaped rims at the dust sublimation edge are favored. The measured closure phases are generally non-null with a median value of ~10°, indicating spatial asymmetries of the intensity distributions. Multi-size grain populations could explain the closure phase ranges below 20–25° but other scenarios should be invoked to explain the largest ones. Our measurements extend the Radius-Luminosity relation to ~104 L⊙ luminosity values and confirm the significant spread around the mean relation observed by PIONIER in the H-band. Gapped sources exhibit a large N-to-K band size ratio and large values of this ratio are only observed for the members of our sample that would be older than 1 Ma, less massive, and with lower luminosity. In the mass range of 2 M⊙, we do observe a correlation in the increase of the relative age with the transition from group II to group I, and an increase of the N-to-K size ratio. However, the size of the current sample does not yet permit us to invoke a clear, universal evolution mechanism across the Herbig Ae/Be mass range. The measured locations of the K-band emission in our sample suggest that these disks might be structured by forming young planets, rather than by depletion due to EUV, FUV, and X-ray photo-evaporation.

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“…Note that the exponent on f is 1 not 3/2 as was previously reported (Punsly et al 2018). The quantity f was estimated to be in the range of 10<f<20 for most FR II radio sources (Blundell & Rawlings 2000).…”

Section: ( )mentioning

confidence: 67%

“…The uncertainty in Equations (1) and (2) arises from the uncertainty in the HST composite continuum level and the uncertainty in L(C IV) and L λe (λ e =1350 Å), respectively, added in quadrature (Telfer et al 2002;Punsly et al 2018).…”

Section: The Bolometric Luminosity Of the Accretion Flowmentioning

confidence: 99%

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The Energetics of Launching the Most Powerful Jets in Quasars: A Study of 3C 82

Punsly

Hill

Marziani

et al. 2020

ApJ

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3C 82 at a redshift of 2.87 is the most distant 3C (Third Cambridge Catalogue) quasar. Thus, it is a strong candidate to have the most-luminous radio lobes in the universe. 3C 82 belongs to the class of compact steepspectrum radio sources. We use single-dish and interferometric radio observations in order to model the plasma state of these powerful radio lobes. It is estimated that the long-term time-averaged jet power required to fill these lobes with leptonic plasma is » ´-Q 2.66 1.33 10 erg s 47 1 , among the largest time-averaged jet powers from a quasar. Positing protonic lobes is not tenable as they would require two orders of magnitude more mass transport to the lobes than was accreted to the central black hole during their formation. The first high signal-to-noise optical spectroscopic observation obtained of this object indicates that there is a powerful high-ionization broad-line wind with a kinetic power of ∼10 45 erg s −1 and a velocity of ∼0.01c. We also estimate from the broad lines in 2018 and the UV continuum in three epochs spread out over three decades that the accretion flow bolometric luminosity is L bol ≈3.2-5.8×10 46 erg s −1. The ratio of »  Q L 5.91 3.41 bol / is perhaps the largest of any known quasar. Extremely powerful jets tend to strongly suppress powerful winds of ionized baryonic matter. Consequently, 3C 82 provides a unique laboratory for studying the dynamical limits of the central engine of outflow initiation in quasars. Unified Astronomy Thesaurus concepts: Black hole physics (159); Radio jets (1347); Relativistic jets (1390); Radio loud quasars (1349)

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Probing the Inner Disk Emission of the Herbig Ae Stars HD 163296 and HD 190073

Cited by 28 publications

References 50 publications

Multi-epoch Direct Imaging and Time-variable Scattered Light Morphology of the HD 163296 Protoplanetary Disk

Multi-epoch Direct Imaging and Time-variable Scattered Light Morphology of the HD 163296 Protoplanetary Disk

The GRAVITY Young Stellar Object survey

The Energetics of Launching the Most Powerful Jets in Quasars: A Study of 3C 82

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