HIGH-RESOLUTION MID-INFRARED IMAGING OF THE CIRCUMSTELLAR DISKS OF HERBIG Ae/Be STARS

Mariñas, Naibí; Telesco, C. M.; Fisher, Richard F.; Packham, C.

doi:10.1088/0004-637x/737/2/57

Cited by 36 publications

(57 citation statements)

References 64 publications

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“…As seen above, in our images the position angle is close to the eastwest direction. We note, however, that we are probing different spatial scales and that, overall, the brightness asymmetry in east-west direction is mostly confined to radial distances >0.5 in the PAH filters and not to the MIR continuum (Doucet et al 2007;van Boekel et al 2004;Mariñas et al 2011). Habart et al (2004) showed that emission features at 3.43 and 3.53 μm, which were attributed to hydrogenated diamonds (Van Kerckhoven et al 2002;Habart et al 2004;Guillois et al 1999, and references therein), as well as the nearby continuum emission was slightly extended and most likely arising from the innermost 15 AU of a circumstellar disk seen face-on.…”

Section: Hd 97048 Resolved In Pah Continuum and Gas Emissionmentioning

confidence: 75%

Resolving the inner regions of the HD 97048 circumstellar disk with VLT/NACO polarimetric differential imaging

Quanz

Birkmann

Apai

et al. 2012

A&A

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Context. Circumstellar disks are the cradles of planetary systems and their physical and chemical properties directly influence the planet formation process. Because most planets supposedly form in the inner disk regions, i.e., within a few tens of AU, it is crucial to study circumstellar disks on these scales to constrain the conditions for planet formation. Aims. Our aims are to characterize the inner regions of the circumstellar disk around the young Herbig Ae/Be star HD 97048 in polarized light. Methods. We used VLT/NACO to observe HD 97048 in polarimetric differential imaging (PDI) mode in the H and K s band. This technique offers high-contrast capabilities at very small inner working angles and probes the dust grains on the surface layer of the disk that act as the scattering surface. Results. We spatially resolve the disk around HD 97048 in polarized flux in both filters on scales between ∼0.1 -1.0 corresponding to the inner ∼16-160 AU. Fitting isophots to the flux calibrated H-band image between 13-14 mag/arcsec 2 and 14-15 mag/arcsec 2 , we derive an apparent disk inclination angle of 34 • ± 5 • and 47 • ± 2 • , respectively. The disk position angle in both brightness regimes is almost identical and roughly 80 • . Along the disk major axis the surface brightness of the polarized flux drops from ∼11 mag/arcsec 2 at ∼0.1 (∼16 AU) to ∼15.3 mag/arcsec 2 at ∼1.0 (∼160 AU). The brightness profiles along the major axis are fitted with power-laws falling off as ∝r −1.78±0.02 in H and ∝r −2.34±0.04 in K s . Because the surface brightness decreases more rapidly in K s compared to H, the disks becomes relatively bluer at larger separations, possibly indicating changing dust grain properties as a function of radius. Conclusions. We imaged for the first time the inner ∼0.1 -1.0 (∼16-160 AU) of the surface layer of the HD 97048 circumstellar disk in scattered light, which demonstrates the power of ground-based imaging polarimetry. Our data fill an important gap in a large collection of existing data that include resolved thermal dust and polycyclic aromatic hydrocarbon (PAH) emission and also resolved gas emission lines. HD 97048 therefore is an ideal test case for sophisticated models of circumstellar disks and a prime target for future high-contrast imaging observations.

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Section: Hd 97048 Resolved In Pah Continuum and Gas Emissionmentioning

confidence: 75%

Resolving the inner regions of the HD 97048 circumstellar disk with VLT/NACO polarimetric differential imaging

Quanz

Birkmann

Apai

et al. 2012

A&A

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“…Observations of spatially resolved Q-band imaging (Mariñas et al 2011), the SED, and the absence of the silicate feature are indications of a dust gap Maaskant et al (2013). HD 100453 has a close M-type companion (projected distance of 120 AU), and the connection of the companion with the disk structure is not well understood (Collins et al 2009).…”

Section: Hd 100453mentioning

confidence: 96%

“…HD 100453 and HD 34282 were observed as part of a larger high-resolution imaging survey of protoplantary disks around Herbig Ae/Be stars (Mariñas et al 2011). Q-band images (18.1 µm, ∆λ = 1.1) were obtained using MICHELLE on the Gemini North telescope on February 2, 2006 for HD 100453 and December 4, 2003 for HD 34282.…”

Section: Datamentioning

confidence: 99%

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Large dust gaps in the transitional disks of HD 100453 and HD 34282

Khalafinejad

Maaskant

Mariñas

et al. 2016

A&A

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Context. The formation of dust gaps in protoplanetary disks is one of the most important signs of disk evolution and might indicate the formation of planets. Aims. We aim to characterize the flaring disk structure around the Herbig Ae/Be stars HD 100453 and HD 34282. Their spectral energy distributions (SEDs) show an emission excess between 15−40 µm, but very weak (HD 100453) and no (HD 34282) signs of the 10 and 20 µm amorphous silicate features. We investigate whether this implies the presence of large dust gaps. Methods. We investigated spatially resolved mid-infrared Q-band images taken with Gemini North/MICHELLE. We performed radiative transfer modeling and examined the radial distribution of dust. We simultaneously fit the Q-band images and SEDs of HD 100453 and HD 34282. Results. Our solutions require that the inner halos and outer disks be separated by large dust gaps that are depleted with respect to the outer disk by a factor of 1000 or more. The inner edges of the outer disks of HD 100453 and HD 34282 have temperatures of ∼160 ± 10 K and ∼60 ± 5 K, respectively. Because of the high surface brightness of these walls, they dominate the emission in the Q band. Their radii are constrained at 20 +2 −2 AU and 92 +31 −17 AU, respectively. Conclusions. HD 100453 and HD 34282 most likely have disk dust gaps. The upper limit of the dust mass in each gap is estimated to be about 10 −7 M . We find that the locations and sizes of disk dust gaps are connected to the SED, as traced by the mid-infrared flux ratio F 30 /F 13.5 . We propose a new classification scheme for the Meeus groups based on the F 30 /F 13.5 ratio. The absence of amorphous silicate features in the observed SEDs is caused by the depletion of small ( 1 µm) silicate dust at temperatures above 160 K, which could be related to the presence of a dust gap in that region of the disk.

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“…Several data sets give different inclinations for HD 135344B: (Mariñas et al 2011). For our analysis of the SED and line profiles, we used i = 14 • .…”

Section: Disk Inclination and Position Anglementioning

confidence: 99%

Constraining the structure of the transition disk HD 135344B (SAO 206462) by simultaneous modeling of multiwavelength gas and dust observations

Carmona

Pinte

Thi

et al. 2014

A&A

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Context. Constraining the gas and dust disk structure of transition disks, particularly in the inner dust cavity, is a crucial step toward understanding the link between them and planet formation. HD 135344B is an accreting (pre-)transition disk that displays the CO 4.7 µm emission extending tens of AU inside its 30 AU dust cavity. Aims. We constrain HD 135344B's disk structure from multi-instrument gas and dust observations. Methods. We used the dust radiative transfer code MCFOST and the thermochemical code ProDiMo to derive the disk structure from the simultaneous modeling of the spectral energy distribution (SED), VLT/CRIRES CO P(10) 4.75 µm, Herschel/PACS [O ] 63 µm, Spitzer/IRS, and JCMT 12 CO J = 3−2 spectra, VLTI/PIONIER H-band visibilities, and constraints from (sub-)mm continuum interferometry and near-IR imaging. Results. We found a disk model able to describe the current gas and dust observations simultaneously. This disk has the following structure. (1) To simultaneously reproduce the SED, the near-IR interferometry data, and the CO ro-vibrational emission, refractory grains (we suggest carbon) are present inside the silicate sublimation radius (0.08 < R < 0.2 AU). (2) The dust cavity (R < 30 AU) is filled with gas, the surface density of the gas inside the cavity must increase with radius to fit the CO ro-vibrational line profile, a small gap of a few AU in the gas distribution is compatible with current data, and a large gap of tens of AU in the gas does not appear likely. (4) The gas-to-dust ratio inside the cavity is >100 to account for the 870 µm continuum upper limit and the CO P(10) line flux.(5) The gas-to-dust ratio in the outer disk (30 < R < 200 AU) is <10 to simultaneously describe the [O ] 63 µm line flux and the CO P(10) line profile. (6) In the outer disk, most of the gas and dust mass should be located in the midplane, and a significant fraction of the dust should be in large grains. Conclusions. Simultaneous modeling of the gas and dust is required to break the model degeneracies and constrain the disk structure. An increasing gas surface density with radius in the inner cavity echoes the effect of a migrating jovian planet in the disk structure. The low gas mass (a few Jupiter masses) throughout the HD 135344B disk supports the idea that it is an evolved disk that has already lost a large portion of its mass.

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HIGH-RESOLUTION MID-INFRARED IMAGING OF THE CIRCUMSTELLAR DISKS OF HERBIG Ae/Be STARS

Cited by 36 publications

References 64 publications

Resolving the inner regions of the HD 97048 circumstellar disk with VLT/NACO polarimetric differential imaging

Resolving the inner regions of the HD 97048 circumstellar disk with VLT/NACO polarimetric differential imaging

Large dust gaps in the transitional disks of HD 100453 and HD 34282

Constraining the structure of the transition disk HD 135344B (SAO 206462) by simultaneous modeling of multiwavelength gas and dust observations

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