Table 1
Summary of most relevant previous observations and disk constraints.
| Technique | Instrument | Observation | Interpretation or constraint | Ref. |
|
|
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| UV–mm photometry | several | SED: dip at 15 μm | 40 AU gap | 1, 2 |
| UV spectroscopy | HST-COS | shape of the continuum flux | spectral type F4V; E(B − V) < 0.129 | 3, 4, 5 |
| optical spectroscopy | VLT-UVES | photospheric absorption lines | Teff = 6750 ± 250 K; logg> 4.0 | this work |
| VLT-UVES | broad [O i] 6300 Å emission | hot gas down to 0.1 AU | 6,7 | |
| near-IR high-resolution spectroscopy | VLT-CRIRES | extended CO 4.7 μm emission; line profile and spectro-astrometry signal | gas in Keplerian rotation inside the cavity at least until 15 AU assuming d = 84 pc (25 AU @ 140 pc); i = 14° for M = 1.65 M⊙; PA ~ 56° | 8 |
| VLT-CRIRES | non-detection of H2 lines at 2 μm | fluxes < 10-17 W m-2 | 9 | |
| near-IR imaging | Subaru-HICIAO | dust scattered light emission | material down to 28 AU; no discontinuity at 45 AU; spiral patterns; flat outer disk | 10 |
| VLT-NACO | polarized dust scattered light emission | strong drop of polarized dust emission at 28 AU | 11 | |
| near-IR interferometry | VLTI/PIONIER | visibilities, closure phases | continuum emission inside the silicate sublimation radius (R< 0.2 AU) | this work |
| mid-IR spectroscopy | Spitzer/IRS | no 10 μm silicate feature | limit to the mass of small silicate grains | 12 |
| weak 11.2 μm PAH emission | limit to the PAH abundance | |||
| non detection H2 pure-rotational lines, and the [Ne ii] 12.8 μm line | fluxes < 10-17 W m-2 | 13 | ||
| far-IR spectroscopy | Herschel/PACS | [O i] 63μm detected, upper limits to the | F[ O i ] 63 μm = 3.6−4.8 × 10-17 W m-2 | 14, 20 |
| [O i] 145μm and [C ii] 157 μm lines | ||||
| sub-mm interferometry | SMA | weak 870 μm continuum at R< 40 AU; | cavity radius 46±5 AU; i ~ 12°; 3σ flux in a 0.24′′ × 0.5′′ (33 × 70 AU) beam centerred on the star 10.5 mJy | 15, 16 |
| ALMA | resolved 450 μm emission | asymmetries in the outer disk observed | 17 | |
| 12CO 6−5 detected at R< 40 AU | gas inside the dust cavity. | |||
| sub-mm line single dish | JCMT | 12CO 3−2 detected | double peak; FWHM = 2.2 km s-1; i ~ 11° | 18 |
| mm continuum and | SMA | extended 1.3 mm emission | Rout = 220 AU; i ~ 11° | 19 |
| line interferometry | extended 12CO 2−1 emission | |||
Reference. [1] see Table A.1, [2] Brown et al. (2007), [3] Grady et al. (2009), [4] France et al. (2012), [5] Schindhelm et al. (2012), [6] van der Plas et al. (2008), [7] Fedele et al. (2008), [8] Pontoppidan et al. (2008), [9] Carmona et al. (2011), [10] Muto et al. (2012), [11] Garufi et al. (2013), [12] Geers et al. (2006), [13] Lahuis et al. (2007), [14] Meeus et al. (2012), [15] Brown et al. (2009), [16] Andrews et al. (2011), [17] Pérez et al. (2014), [18] Dent et al. (2005), [19] Lyo et al. (2011), [20] Fedele et al. (2013).
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