# A narrow, edge-on disk resolved around HD 106906 with SPHERE

A. -M. Lagrange, M. Langlois, R. Gratton, A. -L. Maire, J. Milli, J. Olofsson, Arthur Vigan, V. Bailey, D. Mesa, G. Chauvin, et al.

► To cite this version:

A. -M. Lagrange, M. Langlois, R. Gratton, A. -L. Maire, J. Milli, et al. A narrow, edge-on disk resolved around HD 106906 with SPHERE. Astronomy and Astrophysics - A&A, 2016, 586, 10.1051/0004-6361/201527264. hal-01440700

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LETTER TO THE EDITOR

# A narrow, edge-on disk resolved around HD 106906 with SPHERE*,**

A.-M. Lagrange¹,², M. Langlois³,⁴, R. Gratton⁵, A.-L. Maire⁵,⁷, J. Milli⁶, J. Olofsson⁷,⁸,⁹, A. Vigan⁴,⁶ V. Bailey¹⁰,
D. Mesa⁵, G. Chauvin¹,², A. Boccaletti¹¹, R. Galicher¹¹, J. H. Girard⁶, M. Bonnefoy¹,², M. Samland⁷, F. Menard¹²,
T. Henning⁷, M. Kenworthy¹³, C. Thalmann¹⁴, H. Beust¹,², J.-L. Beuzit¹,², W. Brandner⁷, E. Buenzli⁷,¹⁴,
A. Cheetham¹⁵, M. Janson¹⁶, H. le Coroller⁴,¹⁷, J. Lannier¹,², D. Mouillet¹,², S. Peretti¹⁵, C. Perrot¹¹, G. Salter⁴,
E. Sissa⁵, Z. Wahhaj⁶, L. Abe¹⁸, S. Desidera⁵, M. Feldt⁷, F. Madec⁴, D. Perret¹¹, C. Petit¹⁹, P. Rabou¹,²,
C. Soenke⁷, and L. Weber¹⁵

*(Affiliations can be found after the references)*

Received 28 August 2015 / Accepted 28 September 2015

ABSTRACT

*Context.* HD 106906AB is the only young binary system so far around which a planet has been imaged and a debris disk has been shown to exist, thanks to a strong IR excess. As such, it represents a unique opportunity for studying the dynamics of young planetary systems.

*Aims.* We aim at further investigating the close (tens of au scales) environment of the HD 106906AB system.

*Methods.* We used the extreme adaptive-optics-fed, high-contrast imager SPHERE that has recently been installed on the VLT to observe HD 106906. Both the IRDIS imager and the Integral Field Spectrometer were used.

*Results.* We discovered a highly inclined, ring-like disk at a distance of 65 au from the star. The disk shows a strong brightness asymmetry with respect to its semi-major axis. It shows a smooth outer edge, compatible with ejection of small grains by the stellar radiation pressure. We show furthermore that the planet's projected position is significantly above the PA of the disk. Given the determined disk inclination, it is not excluded, however, that the planet could still orbit within the disk plane if at a large separation (2000–3000 au). We identified several additional point sources in the SPHERE/IRDIS field of view that appear to be background objects. We compare this system with other debris disks sharing similarities, and we briefly discuss the present results in the framework of dynamical evolution.

**Key words.** techniques: high angular resolution – stars: individual: HD 106906 – planetary systems

1. Introduction

Circumbinary planets offer valuable constraints on planet forma-
tion theories (Thalmann et al. 2014). Very few long-period cir-
cumbinary planets are known today. One of them is HD 106906,
a Lower Centaurus Crux (LCC) member that hosts a mas-
sive (M = 11 ± 2 M<sub>Jup</sub>) giant planet (GP) detected in pro-
jected separation at 650 au by Bailey et al. (2014). We recently
demonstrated that HD 106906 is a close binary, therefore named
HD 106906AB, with a total stellar mass probably greater than
2.5 M<sub>☉</sub> (Lagrange et al. 2016). In addition, a high-luminosity
(L<sub>d</sub>/L<sub>*</sub> = 1.4 × 10<sup>-3</sup>) circumbinary disk, indicated by the near-
infrared and far-infrared SPITZER data, is also present (Chen
et al. 2005), and the dynamical relation between the planet and
the disk is therefore unknown. Given its youth (13 ± 2 Myr;
Pecaut et al. 2012), this system offers unique opportunities to
study early dynamics of planetary systems. A very interesting
related question is where and how the planet formed. If formed
close to the star by core accretion or disk gravitational instability,
some mechanisms had to eject it onto its current orbit, without
destroying the disk material that is assumed to be located at ≈
20 au. If formed bound to the star at its present location, an alter-

native formation mechanism needs to be invoked, such as cloud
collapse. Alternatively, the planet may have been captured from
another star. This is a plausible scenario as the large-scale (clus-
ter) environment of HD 106906AB is and was certainly even
denser at earlier ages (for a discussion, see Lagrange et al. 2016).
Two related key questions are the position of the planet with re-
spect to the disk, and the disk morphological properties.

As part of a large survey to search for planets around mem-
bers of young and nearby associations, we recently recorded
high-contrast images of HD 106906AB with the SPHERE in-
strument that has recently been mounted on ESO's VLT Unit
Telescope 3 (Beuzit et al. 2008). The data resolve the disk for
the first time and constrain the planet position relative to the disk.
They also allow precisely constraining the GP population around
the binary. This Letter aims at presenting the observational re-
sults and developing qualitative arguments on the system. We
first describe the data and the observations (Sect. 2), then the re-
sults obtained on the disk (Sect. 3), the planet position relative
to the disk (Sect. 4), and the search for additional planets in the
system (Sect. 5).

2. Data

2.1. *Data log*

Various images of HD 106906AB were recorded in March, May,
and July, 2015 with different instrumental setups (see Table 1).

<footnote>* Based on data obtained with the VLT/Sphere at Paranal.
Programme: 095.C-0298(A).</footnote>

<footnote>** This work is based (in part) on data products produced at the SPHERE Data Center hosted at OSUG/IPAG, Grenoble.</footnote>
<table><caption>**Table 1.** Observing log.</caption><thead><tr><th>Date</th><th>Setup</th><th>DIT × NDIT × N (s)</th><th>Par. Ang. (deg)</th><th>Airmass</th><th>Seeing</th><th>Coh. time (ms)</th><th>Wind (m/s)</th><th>True North (deg)</th><th>Plate scale (mas/pixel)</th></tr></thead><tbody><tr><td>2015/03/30</td><td>IRDIS_H2H3<br>IFS_YJ</td><td>64 × 4 × 9<br>64 × 4 × 9</td><td>-3.2/14.0</td><td>1.17/1.18</td><td>≥1.7</td><td>1.2/1.4</td><td>14.5/18.3</td><td>-1.8 ± 0.1</td><td>12.255 ± 0.008</td></tr><tr><td>2015/05/06</td><td>IRDIS_H<br>IFS_YJ</td><td>16 × 14 × 16<br>64 × 4 × (7 + 9)</td><td>-20.6/0.98</td><td>1.17/1.18</td><td>0.78/1.11</td><td>1.7/2.2</td><td>4.1/9.6</td><td>-2.0 ± 0.1</td><td>12.220 ± 0.003</td></tr><tr><td>2015/05/12</td><td>IRDIS_H2H3<br>IFS_YJ</td><td>64 × 4 × 20<br>64 × 4 × 16</td><td>-12.7/17.8</td><td>1.17/1.18</td><td>0.76/1.06</td><td>3.1/4.3</td><td>2.2/5.7</td><td>-2.0 ± 0.1</td><td>12.220 ± 0.03</td></tr><tr><td>2015/07/03</td><td>IRDIS_K1K2<br>IFS_YJH</td><td>64 × 5 × 16<br>64 × 5 × 16</td><td>14.6/49.5</td><td>1.18/1.29</td><td>0.64/1.36</td><td>1.4/2.5</td><td>5.4/6.9</td><td>-1.8 ± 0.15</td><td>12.242 ± 0.033</td></tr></tbody></table>

**Notes.** DIT: detector integration time. Parallactic angle as measured at the start and end of each coronagraphic IRDIS sequence. Minimum and maximum values of the coherence time, airmass, wind speed, and seeing. Plate scales and TN were measured on non-coronagraphic data.

Exposures were taken in May at H band and in H2H3 dual-band imaging (centered at 1.59 and 1.67 µm, respectively; Vigan et al. 2010) with the IRDIS camera (Dohlen et al. 2008), and at YJ (0.95–1.35 µm, spectral resolution $R \approx 54$) with the Integral Field Spectrometer (IFS; Claudi et al. 2008). We note that these observations are unpolarized. In July, additional data were recorded in dual-band imaging at K1K2 (centered at 2.11 and 2.25 µm) with IRDIS and at YH (0.95–1.65 µm, $R \approx 33$) with IFS. In all these observations, we used an apodized Lyot coronagraph including a 185 mas focal mask (SPHERE mask N_ALC_YJH_S) as well as a pupil mask. IRDIS provides a $\approx 12'' \times 12''$ field of view (FoV; 1100 × 1100 au, given the star’s distance 92.1$^{+6.5}_{-5.7}$ pc; van Leeuwen 2007), with a $\approx 12.2$ mas/pixel scale. An IFS dataset consists of 21 000 spectra spread over 5.1 × 41 pixels on the detector. After extraction, the FoV is $1.7'' \times 1.7''$ and the spaxel size is $7.4 \times 7.4$ mas, that is, $0.68 \times 0.68$ au.

The coronagraphic observations were performed keeping the pupil stabilized so as to perform angular differential imaging (ADI) post-processing (Marois et al. 2006). This allows suppressing a large portion of the residual starlight after the coronagraph. The FoV rotations for the different sets of data are provided in Table 1. Our observing sequence was as follows: 1) Point spread function (PSF) imaging, with HD 106906AB offset from the mask, so as to record a PSF and a relative photometric calibration; 2) image of the star behind the mask, with four satellite footprints of the PSF that can be used for fine monitoring of the centering; 3) coronagraphic sequence; 4) image of the star behind the mask, with four satellite footprints again; 5) PSF imaging; and 6) sky observations, with DITs corresponding to the DITs of the coronagraphic sequence. Finally, the true North (TN) and plate scales were measured using astrometric calibrators observed during each run, as part of the SPHERE GTO survey (Maire et al. 2016). They are reported in Table 1. We note that the plate scales and TN values were measured on non-coronagraphic data. A shift of about 0.02 mas/pixel in plate scale has been found empirically between the non-coronagraphic and coronagraphic data. For this reason, we used conservative error bars below to measure the separation.

## 2.2. Data reduction

When observing with IRDIS in dual imaging at H2H3 (resp. K1K2), IRDIS produces two simultaneous images, the left one at H2 (resp. K1) and the right one at H3 (resp. K2). In classical imaging broadband H, two identical images are taken on the left and on the right detector quadrants. The IRDIS data were

corrected for cosmetics and sky background using the SPHERE data reduction and handling (DRH) pipeline (Pavlov et al. 2008). The outputs include cubes of left and right images recentered onto a common origin using the satellite spots that were also corrected for distortion. After these first steps, the data were sorted out according to their quality, and the following algorithms were applied: classical angular differential imaging (cADI, Marois et al. 2006), template locally optimized combination of images (TLOCI, Marois et al. 2014), and principal component analysis (PCA, Soummer et al. 2012). To do so, we used an analysis pipeline that we had developed to reduce and analyze our guaranteed time observations. The IFS data were also preprocessed using the DRH pipeline; then they were processed with PCA as described in Mesa et al. (2015). For the May sequences, the data were median-binned in 16 (May 12) and 14 (May 6) data cubes before reduction.

## 3. A disk around HD 106906AB

All IRDIS datasets (even the poor-quality set of March 30) and reductions reveal a disk seen close to edge-on. A set of resulting median images obtained using different algorithms is shown in Fig. 1. The IFS image resulting from the data of May 12 is shown in Fig. 2. The later image is a median over wavelength of the image obtained with PCA (with 50 components). A low-pass median filter (size of 31 pixels) and a software mask leaving the ring between 12 (0.09'') and 108 pixels (0.81'') from field center were used.

### 3.1. Disk properties

In our images, the disk appears mostly as a ring structure with a brightness distribution peaking at about 65 au, which is much farther away than inferred from modeling the spectral energy distribution under the assumption of pure blackbody grains (20 au, Bailey et al. 2014). It is detected out to 110 au in our images and is elongated in the SE-NW direction. Its northern side is much brighter than the southern side, which is not detected with all the reduction algorithms. Given the age of the system as well as the absence of significant amounts of circumstellar gas and because of its similarity with other debris disks (see below), we can safely conclude that the disk is a debris disk.

A full modeling of the disk is beyond the scope of this Letter. We nonetheless performed a simple forward modeling of the disk images as was done in Milli et al. (2012) using the GRATER code (Augereau et al. 1999) to constrain the disk morphology
<figure><img src="image_2.png" /><figcaption>**Fig. 1.** *From left to right:* CADI, LOCI, and PCA of the HD 106906AB disk at (from top to bottom) H2+H3, H and K1K2 bands (IRDIS data). North is up and east is to the left. The FoV of each image is 2.4" × 1.8". The intensity scale of the top right image has been adapted to highlight the southern part of the disk.</figcaption></figure>

<figure><img src="image_3.png" /><figcaption>**Fig. 2.** IFS YJH snr map of the HD 106906AB disk. N is up and E to the left.</figcaption></figure>

and separate ADI artifacts from real features. We modeled the disk as an inclined optically thin ring, centered on the star, with a dust density distribution that peaks at a radius $r_0$ and follows a power law of slope $\alpha_{in}$ within $r_0$ and $\alpha_{out}$ beyond $r_0$. The model geometry is defined by six free parameters: the inclination $i$, the position angle (PA), the radius of peak dust density $r_0$, the Henyey-Greenstein coefficient $g$ parametrizing the anisotropy of scattering, the outer slope $\alpha_{out}$, and a scaling factor to match

<table><caption>**Table 2.** Best model parameters for the HD 106906 disk after forward modeling.</caption><thead><tr><th>Filter</th><th>r<sub>0</sub> (au)</th><th>Incl. i (°)</th><th>PA (°)</th><th>g</th><th>α<sub>out</sub></th></tr></thead><tbody><tr><td>H2</td><td>66.0 ± 1.8</td><td>85.4 ± 0.1</td><td>104.4 ± 0.3</td><td>0.6 ± 0.1</td><td>-4.5 ± 0.3</td></tr><tr><td>H3</td><td>63.0 ± 1.0</td><td>85.2 ± 0.1</td><td>104.3 ± 0.3</td><td>0.6 ± 0.1</td><td>-3.8 ± 0.4</td></tr></tbody></table>

the disk total flux. We fixed the inner slope $\alpha_{in}$ to 10 because our images are unable to constrain this parameter. Likewise, the vertical dust density distribution was set to a Gaussian profile of scale height 0.5 au at $r_0$ with a linear flaring. For each set of data, the disk model was rotated to the appropriate parallactic angles, convolved with the instrumental PSF and subtracted from each frame. The resulting data cube was reduced using the same PCA algorithm as described previously, retaining eight components for the PSF subtraction. These steps were repeated by varying the free parameters until a reduced chi-squared is minimized. The reduced chi-squared was computed in an elliptical annulus where the disk was detected. The result of this minimization is given in Table 2. We derive an inclination of 85.3 ± 0.1 deg, a disk position angle (PA) of 104.4 ± 0.3 deg, a Henyey-Greenstein parameter of anisotropy $g$ of 0.6 ± 0.1. We also performed a simple elliptical fit on the IRDIS data, which gave similar values for the inclination and PA. The disk is strongly forward scattering. Finally, the inversion leads to a slope of -4 for the outer edge of the ring.

A remarkable feature of the disk is its E-W brightness asymmetry, as clearly seen in Figs. 1–3, where we show the brightness distribution along the southeast and northwest ansae as measured on the H2+H3+K1+K2 image. The SE side appears to be about 10% brighter than the NW side. Our simple symmetric model is not able to fully account for this brightness asymmetry. This asymmetry could be explained by an elliptic disk, with a pericenter located on the NW side (but see also below).
<table><caption>**Table 3.** Morphological properties of the disks of HD 106906, HR4796, HD15115, HD61005, and β Pictoris.</caption><thead><tr><th>System</th><th>Disk luminosity<br>L<sub>d</sub>/L<sub>s</sub></th><th>System age<br>Myr</th><th>Star ST</th><th>Star mass<br>(M<sub>☉</sub>)</th><th>Peak sep.<br>(au)</th><th>FWHM<br>(au)</th><th>α<sub>in</sub></th><th>α<sub>out</sub></th><th>offset</th></tr></thead><tbody><tr><td>HD 106906AB</td><td>1.4 × 10<sup>-3</sup></td><td>13 ± 2</td><td>F5V</td><td>2.6</td><td>65</td><td>30</td><td>10 (fixed)</td><td>-4</td><td>?</td></tr><tr><td>HR4796</td><td>5 × 10<sup>-3</sup></td><td>8 ± 2</td><td>A0V</td><td>2.4</td><td>80</td><td>10</td><td>≤-3</td><td>≤-13</td><td>≈YES</td></tr><tr><td>β Pictoris</td><td>3 × 10<sup>-3</sup></td><td>21 ± 3</td><td>A5V</td><td>1.75</td><td>100</td><td>≥40</td><td>≈-2</td><td>-3.5</td><td>NO</td></tr><tr><td>HD 15115</td><td>5 × 10<sup>-4</sup></td><td>12–100</td><td>F2V</td><td>1.6</td><td>90</td><td></td><td>10</td><td>-4</td><td>YES</td></tr><tr><td>HD 61005</td><td>2 × 10<sup>-3</sup></td><td>90 ± 40</td><td>G8V</td><td></td><td>60</td><td></td><td>≈5</td><td>-4.5</td><td>YES</td></tr></tbody></table>

**References.** HD 106906: Pecaut et al. (2012), this work. HR4796: Lagrange et al. (2012c), Milli et al. (2015), Schneider et al. (2009), Stauffer et al. (1995). β Pictoris: Lagrange et al. (2012b). HD15115: Kalas et al. (2007), Mazoyer et al. (2014). HD65001: Hines et al. (2007), Buenzli et al. (2010), Desidera et al. (2011).

<figure><img src="image_4.png" /><figcaption>**Fig. 3.** Disk brightness along the semi-major axis, extracted from H2+H3+K1+K2 data (see text). To improve the S/N, we averaged the flux over three pixels perpendicular to this axis. The black curve corresponds to the east, the red curve to the west side.</figcaption></figure>

## 3.2. Comparison with other debris disks

The disk of HD 106906AB shows similarities with the disk of HR4796 (Schneider et al. (2009), Lagrange et al. (2012c), see also Milli et al. 2015, and in prep.): they both present rings with an inner void, with similar distances and widths (Table 3). Their outer edges are quite different, however: while the HR4796 disk brightness slope is about -10, the HD 106906AB disk is -4, that is, more similar to that of the β Pictoris disk (Lagrange et al. 2012a). A full disk modeling of the β Pictoris system, including radiation pressure acting on the small grains produced by collisions, reproduced most of the disk asymmetries (Augereau et al. 2001). For HR4796, the steep edge is not fully understood; it may either imply the presence of a companion close to the outer disk, or be due to a higher opacity in the HR4796 disk that partly blocks the stellar flux (for a detailed discussion, see Lagrange et al. 2012c).

Neither the β Pictoris disk nor the HR4796 disk show strong side asymmetries, as does the disk of HD 106906AB. The disk around the F2V star HD 15115 (see also Table 3) is more similar from this point of view (Mazoyer et al. 2014), with asymmetries along both the minor and major axes. Possible explanations of the asymmetry along the semi-major axis include interactions with the interstellar medium, perturbation by a possible neighbor star (HIP 12545), or intrinsic disk properties. The disk of HD 15115 is bowed (see Rodigas et al. 2012); such a bow might be present in HD 106906 data, but the data are not good enough to allow a firm conclusion at this point.

A comparison with the disk of the solar-type star HD 61005 (Hines et al. 2007) is interesting because the disk also has a narrow ring-like shape, with a sharp inner edge. Brightness asymmetries are also detected along the semi-major and semi-minor axes. An extending, tenuous feature is seen to emerge from the ring, possibly due to interactions with a warm low-density cloud (Maness et al. 2009). Such extended features are not detected in our data.

<figure><img src="image_5.png" /><figcaption>**Fig. 4.** Disk and the planet around HD 106906AB. North is up and east is to the left. HD 106906AB b is the bright source in the top right corner.</figcaption></figure>

The HD 106906 system is the second known system with a resolved disk and an imaged planet; the other is the β Pictoris system<fnref n="1" />. In both cases, the planet is a massive giant and the disk bulk of material lies at a few tens of au. In both cases, the inner part of the disk shows a relative void of material. The host stars are both early-type, massive, young stars. But while HD 106906AB b is orbiting at more than 600 au, β Pictoris b orbits at less than 10 au. The dynamical histories of these planets and their formation histories might be different.

## 4. Position of the planet relative to the disk

HD 106906AB b is located more than 7" away from the central stars in projected separation (Bailey et al. 2014). With this separation, the planet is at the edge of our IRDIS FoV. We therefore carefully scheduled a series of observations to image both the disk and the planet on the same frames, to measure the planet PA relative to the disk PA as precisely as possible using a single dataset. Indeed, when comparing PA coming from different instruments or telescopes, the systematics due to TN can be very high, as demonstrated in Lagrange et al. (2012a). These observations yielded a timing constraint to ensure that the planet would be crossing the detector FoV in pupil-tracking mode and to also ensure a large enough FoV rotation. The image resulting from this set of observations is shown in Fig. 4². Based on the NICI

<footnote n="1">¹ Fomalhaut hosts a disk and a possible planet surrounded by dust, but the planet photons have not been detected yet (Kalas et al. 2008).</footnote>

<footnote n="2">² In practice, the planet was within the FoV in only 35 cubes of the whole dataset (consisting of 64 cubes). We selected these 35 cubes and reduced them again. We checked that the position of the planet using the extracted dataset was the same as using the whole dataset.</footnote>
<figure><img src="image_6.png" /></figure>

**Fig. 5.** *From left to right:* in blue, HD 106906AB b, relative positions of stars 1 and 3 with respect to their positions at the first epoch (2004/01/12). The 2015 positions are given in this paper, and the other positions are taken from Bailey et al. (2014). The curve shows the expected motion if the targets are background objects. In red, the expected positions, assuming the targets are background targets, at each epoch. We adopted very conservative error bars (30 mas) for all datasets in this diagram because of the uncontrolled variations during the exposures.

and HST ACS data, we confirm that HD 106906AB b shares a common proper motion with the central stars (see Fig. 5 and Table 4).

The first question addressed is whether the planet could still be orbiting within the disk, even though it is seen 23 degrees above the disk in projected position. Assuming a disk inclination of $i_d$ and a difference between the disk and the planet PA of $i_p$, then the planet could still be within the disk if it is located $650 \times \sqrt{(1 + (\frac{\sin(i_p)}{\tan(i_d)})^2)}$ au from the central stars. With $i_d = 5°$ (resp. $7°$), its physical separation to the central star would be ≈3000 (resp. 2000) au. Then, the planet could still be within the disk plane if located at a much larger distance than the projected separation. We note that even if, in contrast, the real inclination of HD 106906AB b is 23 degrees with respect to the disk, the planet would not induce Kozai resonance effects on the disk, regardless of its orbital properties. For most three-body systems, the Kozai mechanism starts only above a mutual inclination of around $40°$ (see Ford et al. 2000, and references therein). Whether the planet may be causing the observed disk asymmetry through regular perturbations is unclear. To answer this question, we would need to know the planet orbital properties, which are obviously be difficult to obtain. We conclude that even if complex, the stability of the binary + disk + planet system is probably not a problem. The binary is very tight, which means that it acts as a single massive central star at the distance of the inner ring. Moreover, as we showed above, if the orbit of HD 106906AB b is not coplanar with the disk, it probably will not destroy the disk provided its orbit is not too eccentric. To account for the inner edge of the disk, additional companions or other dynamic processes need to be invoked.

## 5. Search for other planets

Our IRDIS images reveal three additional point sources in the H2H3, H, or K1K2 FoV (see Table 4). Two of them (stars 1 and 2) were already present in ancillary HST ACS data (taken in 2004) and in the NICI planet b discovery images (taken in 2011). Given the long time span between the HST data (taken in 2004) and the present SPHERE data and given the HD 106906AB ppm, we could easily check that these sources do not share a common proper motion with HD 106906AB (see Fig. 5). Star 3³, located closer to the star, was not detected in NICI or ACS data. Finally, another very faint target is detected in the H images south of star 3; this was not present in the HST or NICI data. No point source was identified in the IFS FoV.

Using the SPHERE IRDIS and IFS data, we computed the contrasts achieved in these observations. We then translated

<table><caption>**Table 4.** Stars and planets around HD 106906AB.</caption><thead><tr><th></th><th>Sep<br>mas</th><th>PA<br>deg</th><th>ΔMag</th></tr></thead><tbody><tr><td rowspan="4">Star 1</td><td>6965. ± 28. (07/03)</td><td>299.70 ± 0.23 (07/03)</td><td>K1 = 12.7 ± 0.1<br>K2 = 12.6 ± 0.2</td></tr><tr><td>6957. ± 10. (05/12)</td><td>299.78 ± 0.1 (05/12)</td><td>H2 = 12.6 ± 0.1<br>H3 = 12.5 ± 0.1</td></tr><tr><td>6438. ± 20. (07/03)</td><td>11.89 ± 0.18 (07/03)</td><td>K1 = 12.0 ± 0.1<br>K2 = 11.8 ± 0.2</td></tr><tr><td>6440. ± 5. (05/12)</td><td>11.80 ± 0.05 (05/12)</td><td>H2 = 12.2 ± 0.1<br>H3 = 12.0 ± 0.1</td></tr><tr><td rowspan="3">Star 2</td><td>2362. ± 16. (07/03)</td><td>68.99 ± 0.40 (07/03)</td><td>K1 = 12.6 ± 0.1<br>K2 = 12.4 ± 0.1</td></tr><tr><td>2356. ± 4. (05/12)</td><td>68.62 ± 0.11 (05/12)</td><td>H2 = 12.6 ± 0.1<br>H3 = 12.6 ± 0.1</td></tr><tr><td>7111. ± 13. (07/03)</td><td>307.15 ± 0.1 (07/03)</td><td>K1 = 9.4 ± 0.1<br>K2 = 9.1 ± 0.1</td></tr></tbody></table>

**Notes.** PA and separations (in parenthesis, the month/day of observations, all taken in 2015) were measured using all images. The error bars provided here for the separation, PA, and the contrasts are those provided by the extraction procedure alone. Additional photometric error bars due to uncontrolled flux variations during the exposures are estimated to be 0.4 mag. Conservative astrometric error bars (dominated by uncontrolled variations plus distortion effects) of 30 mas are estimated for the targets farther away than 6".

these contrasts into masses, using the BT-Settl + COND interior models adapted to the SPHERE filters and assuming an age of 10 Myr. The results are summarized in Fig. 6. The extinction toward HD 106906AB is negligible ($A_V = 0.04 \pm 0.02$, Pecaut et al. 2012). We exclude companions with masses $1 M_{Jup}$ or more at projected separations 200 au or more, planets with masses in the range 1–2 $M_{Jup}$ between 100 and 200 au, planets more massive than 3 $M_{Jup}$ within 30–100 au, and planets more massive than 10 $M_{Jup}$ in the range 10–30 au. These limits are significantly improved with respect to those (5–7 $M_{Jup}$ farther away than about 40 au) obtained with the Clio L' data (Bailey et al. 2014). Additional massive inner planets are still not excluded; they may be responsible for the inner void of material within the disk. They also leave room for additional planets that could be responsible for the inner edge if they orbit closer than about 10 au from the inner edge, assuming that their separation (a), eccentricity (e), mass $M_p$, and distance to the edge $\delta a$ follow the Mustill & Wyatt (2012) criterium $\delta a/a = 1.8e^{1/5} (M_p/M_*)^{1/5}$.

**Acknowledgements.** The project is supported by CNRS, by the Agence Nationale de la Recherche (ANR-14-CE33-0018), and the Programme National de Planétologie (PNP, INSU) and Programme National de Physique Stellaire (PNPS, INSU). A.L.M., D.M., and R.G. acknowledge support by Italian MIUR through “Premiale WOW 2013”. J.O. acknowledges support from the

<footnote n="3">³ We label this target “star” for convenience, but we do not yet have information on its nature.</footnote>
<figure><img src="image_7.png" /><figcaption>**Fig. 6.** Top: azimuthally averaged contrasts obtained with IRDIS and IFS. Bottom: best detection limits expressed in Jupiter masses. For IRDIS, the detection limits were combined to produce the best limits after they were expressed in terms of masses.</figcaption></figure>

Millennium Nucleus RC130007 (Chilean Ministry of Economy). We thank P. Delorme and E. Lagadec (SPHERE Data Center) for their efficient help during the data reduction process. SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF – Osservatorio di Padova (Italy), Observatoire de Genève (Switzerland), ETH Zurich (Switzerland), NOVA (Netherlands), ONERA (France) and ASTRON (Netherlands) in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland) and NOVA (Netherlands). SPHERE also received funding from the European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004–2008), grant number 226604 for FP7 (2009–2012) and grant number 312430 for FP7 (2013–2016).

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1. Univ. Grenoble Alpes, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG, UMR 5274), 38000 Grenoble, France e-mail: lagrange@obs.ujf-grenoble.fr

2. CNRS, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG, UMR 5274), 38000 Grenoble, France

3. CRAL, UMR 5574, CNRS, Université Lyon 1, 9 avenue Charles André, 69561 Saint Genis Laval Cedex, France

4. Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388 Marseille, France

5. INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy

6. European Southern Observatory, Alonso de Cordova 3107, Casilla 19001 Vitacura, Santiago 19, Chile

7. Max Planck Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany

8. Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, Playa Ancha, Valparaíso, Chile

9. ICM nucleus on protoplanetary disks, Universidad de Valparaíso, Av. Gran Bretaña 1111, Valparaíso, Chile

10. Steward Observatory, Department of Astronomy, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA

11. LESIA, Observatoire de Paris, CNRS, Université Paris Diderot, Université Pierre et Marie Curie, 5 place Jules Janssen, 92190 Meudon, France

12. UMI-FCA, CNRS/INSU (UMI3386), France

13. Sterrewacht Leiden, PO Box 9513, Niels Bohrweg 2, 2300 RA Leiden, The Netherlands

14. Institute for Astronomy, ETH Zurich, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland

15. Geneva Observatory, University of Geneva, Ch. des Maillettes 51, 1290 Versoix, Switzerland

16. Department of Astronomy, Stockholm University, AlbaNova University Center, 106 91 Stockholm, Sweden

17. Observatoire de Haute-Provence, OH/CNRS, 04870 St. Michel l'Observatoire, France

18. Laboratoire Lagrange, Université de Nice-Sophia Antipolis, Observatoire de la Côte d'Azur, CNRS UMR 7293, Nice Cedex 4, France

19. Onera-The French Aerospace Lab, 92322 Châtillon, France