High-Resolution Near-Infrared Polarimetry of a Circumstellar Disk around UX Tau A

Tanii, Ryoko; Itoh, Yoichi; Kudo, Tomoyuki; Hioki, Tomonori; Oasa, Yumiko; Gupta, Ranjan; Sen, A. K.; Wisniewski, John P.; Muto, Takayuki; Grady, C. A.; Hashimoto, Jun; Fukagawa, Misato; Mayama, Satoshi; Hornbeck, Jeremy; Sitko, Michael L.; Russell, R. W.; Werren, Chelsea; Curé, M.; Currie, Thayne; Ohashi, Nagayoshi; Okamoto, Y.; Momose, Munetake; Honda, Mitsuhiko; Inutsuka, Shu Ichi; Takeuchi, Taku; Dong, Ruobing; Abe, Lyu; Brandner, W.; Brandt, Timothy D.; Carson, J.; Egner, Sebastian; Feldt, M.; Fukue, T.; Goto, Miwa; Guyon, Olivier; Hayano, Yutaka; Hayashi, Masahiko; Hayashi, Saeko S.; Henning, Thomas; Hodapp, Klaus W.; Ishii, Miki; Iye, Masanori; Janson, Markus; Kandori, Ryo; Knapp, G. R.; Kusakabe, Nobuhiko; Kuzuhara, Masayuki; Matsuo, Taro; McElwain, Michael W.; Miyama, Shoken M.; Morino, Jun Ichi; Moro‐Martín, Amaya; Nishimura, Tetsuro; Pyo, Tae‐Soo; Serabyn, Eugene; Shimada, Hiroshi; Suzuki, Ryuji; Miki, Takami; Takato, Naruhisa; Terada, Hiroshi; Thalmann, Christian; Tomono, Daigo; Turner, Edwin L.; Watanabe, Makoto; Yamada, Tōru; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide

doi:10.1093/pasj/64.6.124

Cited by 40 publications

(13 citation statements)

References 42 publications

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“…The radial index of −3 is expected for a vertically flat disk or a disk with a constant opening angle (Whitney & Hartmann 1992;Momose et al 2015). This slope has commonly been observed for protoplanetary disks in Stokes I, and has been found in P I as well (e.g., Tanii et al 2012). Therefore, we propose that the region behind the arc is vertically settled and shadowed by the arc structure.…”

Section: Radial Surface Brightness Distributionsupporting

confidence: 83%

Extreme asymmetry in the polarized disk of V1247 Orionis

Ohta

Fukagawa

Sitko

et al. 2016

Publications of the Astronomical Society of Japan

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We present the first near-infrared scattered-light detection of the transitional disk around V1247 Ori, which was obtained using high-resolution polarimetric differential imaging observations with Subaru/HiCIAO. Our imaging in the H band reveals the disk morphology at separations of ∼ 0. ′′ 14-0. ′′ 86 (54-330 au) from the central star. The polarized intensity (P I) image shows a remarkable arc-like structure toward the southeast of the star, whereas the fainter northwest region does not exhibit any notable features. The shape of the arm is consistent with an arc of 0. ′′ 28 ± 0. ′′ 09 in radius (108 au from the star), although the possibility of a spiral arm with a small pitch angle cannot be excluded. V1247 Ori features an exceptionally large azimuthal contrast in scattered, polarized light; the radial peak of the southeastern arc is about three times brighter than the northwestern disk measured at the same distance from the star. Combined with the previous indication of an inhomogeneous density distribution in the gap at < ∼ 46 au, the notable asymmetry in the outer disk suggests the presence of unseen companions and/or planet-forming processes ongoing in the arc.3

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Section: Radial Surface Brightness Distributionsupporting

confidence: 83%

Extreme asymmetry in the polarized disk of V1247 Orionis

Ohta

Fukagawa

Sitko

et al. 2016

Publications of the Astronomical Society of Japan

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“…For HD 142527, Canovas et al (2013) derived polarisation fraction of 10%-25% at H-band; however, Avenhaus et al (2014) reported significantly higher polarisation fraction for this object (20%-45%) at H-band. Tanii et al (2012) show that polarisation fraction of UX Tau is up to 66% at H-band. Furthermore, Poteet et al (2018) have shown that polarisation fraction of TW Hya is as high as 63% ± 9%.…”

Section: Comparison With Disc Observationsmentioning

confidence: 86%

Effect of dust size and structure on scattered-light images of protoplanetary discs

Tazaki

Tanaka

Muto

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study scattered light properties of protoplanetary discs at near-infrared wavelengths for various dust size and structure by performing radiative transfer simulations. We show that different dust structures might be probed by measuring disk polarisation fraction as long as the dust radius is larger than the wavelength. When the radius is larger than observing wavelength, disc scattered light will be highly polarised for highly porous dust aggregates, whereas more compact dust structure tends to show low polarisation fraction. Next, roles of monomer radius and fractal dimension for scattered light colours are studied. We find that, outside the Rayleigh regime, as fractal dimension or monomer radius increases, colours of the effective albedo at nearinfrared wavelengths vary from blue to red. Our results imply that discs showing grey or slightly blue colours and high polarisation fraction in near-infrared wavelengths might be explained by the presence of large porous aggregates containing sub-microns sized monomers.

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“…Instead of bare stellar photospheres, the calibrators used for LkCa 15 in Sallum et al (2015b) and especially Kraus & Ireland (2012) include multiple stars with bright resolved disk emission on the same spatial scale as LkCa 15's disk: some are also highly variable (e.g. GM Aur, UX Tau; Tanii et al 2012;Oh et al 2016b).…”

Section: Discussionmentioning

confidence: 99%

No Clear, Direct Evidence for Multiple Protoplanets Orbiting LkCa 15: LkCa 15 bcd are Likely Inner Disk Signals

Currie

Marois

Cieza

et al. 2019

ApJL

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103

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Two studies utilizing sparse aperture-masking (SAM) interferometry and H α differential imaging have reported multiple jovian companions around the young solar-mass star, LkCa 15 (LkCa 15 bcd): the first claimed direct detection of infant, newly formed planets ("protoplanets"). We present new near-infrared direct imaging/spectroscopy from the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with the Coronagraphic High 2 Angular Resolution Imaging Spectrograph (CHARIS) integral field spectrograph and multi-epoch thermal infrared imaging from Keck/NIRC2 of LkCa 15 at high Strehl ratios. These data provide the first direct imaging look at the same wavelengths and in the same locations where previous studies identified the LkCa 15 protoplanets, and thus offer the first decisive test of their existence.The data do not reveal these planets. Instead, we resolve extended emission tracing a dust disk with a brightness and location comparable to that claimed for LkCa 15 bcd. Forward-models attributing this signal to orbiting planets are inconsistent with the combined SCExAO/CHARIS and Keck/NIRC2 data. An inner disk provides a more compelling explanation for the SAM detections and perhaps also the claimed H α detection of LkCa 15 b.We conclude that there is currently no clear, direct evidence for multiple protoplanets orbiting LkCa 15, although the system likely contains at least one unseen jovian companion. To identify jovian companions around LkCa 15 from future observations, the inner disk should be detected and its effect modeled, removed, and shown to be distinguishable from planets. Protoplanet candidates identified from similar systems should likewise be clearly distinguished from disk emission through modeling.

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High-Resolution Near-Infrared Polarimetry of a Circumstellar Disk around UX Tau A

Cited by 40 publications

References 42 publications

Extreme asymmetry in the polarized disk of V1247 Orionis

Extreme asymmetry in the polarized disk of V1247 Orionis

Effect of dust size and structure on scattered-light images of protoplanetary discs

No Clear, Direct Evidence for Multiple Protoplanets Orbiting LkCa 15: LkCa 15 bcd are Likely Inner Disk Signals

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