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The Blue Gray Needle: LBT AO Imaging of the HD 15115 Debris Disk

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The Blue Gray Needle: LBT AO Imaging of the HD 15115 Debris Disk The Blue Gray Needle: LBT AO Imaging of the HD 15115 Debris Disk Timothy J. Rodigas + Phil Hinz, Andy Skemer, Kate Su, Glenn Schneider, Laird Close, Vanessa Bailey, Thayne Currie & 48 Co-authors… University of Arizona/LBTO/INAF Rodigas et al. 2012 (ApJ) L86 KALAS, FITZGERALD, & GRAHAM Vol. 661 TABLE 1 to the edge of the field, no nebulosity is detected 9.0Љ–14.9Љ Stellar Properties radius. The appearance of the disk is more symmetric in the Parameter HD 15115 HIP 12545 Reference 2006 October Keck data, which show the disk between 0.7Љ (31 AU) and 2.5Љ (112 AU). Spectral type ...... F2 M0 Hipparcos Optical surface brightness contours (Fig. 2) reveal a sharp mV (mag) .......... 6.79 10.28 Hipparcos Mass (M, ) ........ 1.6 0.5 Cox (2006) midplane morphology for the west extension that indicates an ϩ2.22 ϩ4.38 Distance (pc) ...... 44.78Ϫ2.01 40.54Ϫ3.61 Hipparcos edge-on orientation to the line of sight. The west midplane is R.A. (ICRS) ....... 02 26 16.2447 02 41 25.89 Hipparcos qualitatively similar to that of b Pic’s northeast midplane, in- Decl. (ICRS) ...... ϩ06 17 33.188 ϩ05 59 18.41 Hipparcos Ϫ1 cluding a characteristic width asymmetry (Kalas & Jewitt 1995; Hipparcos 4.46 ע 82.32 1.09 ע ma(mas yr )....... 86.09 Ϫ1 Hipparcos Golimowski et al. 2006). The northern side of the west midplane 2.45 ע Ϫ55.13 0.71 ע md (mas yr )...... Ϫ50.13 Ϫ1 ,Tycho-2 is more vertically extended than the southern side. For example 4.3 ע 82.3 1.2 ע ma(mas yr )....... 87.1 Ϫ1 Tycho-2 the full width at half-maximum across the disk midplane at 2Љ 2.7 ע Ϫ55.1 1.2 ע md (mas yr )...... Ϫ50.9 Ϫ1 a -0.10Љ in both the optical and NIR data. How ע radius is 0.19Љ … 0.5 ע Ϫ14.0 1.9 ע U (km s )........ Ϫ13.2 a… 0.9 ע Ϫ16.7 1.2 ע V (km sϪ1)......... Ϫ17.8 a ever, the vertical cuts are not symmetric about the midplane when… 0.5 ע Ϫ10.0 2.3 ע W (km sϪ1)........ Ϫ6.0 measuring the half-width at quarter-maximum (HWQM). The a Galactic kinematics for HD 15115 and HIP 12545 from Moo´r et al. times greater 0.1 ע and Song et al. (2003), respectively. HWQM north of the west midplane is1.6 (2006) than that of the HWQM south of the west midplane. This width resulting in disk self-subtraction at small radii. Our analysis of asymmetry is confirmed in the Keck data. If the width asymmetry the 2007 January data therefore yields a detection of the west is found to be in the opposite direction in the opposite midplane, ansa in the region 1.3Љ–3.3Љ radius. The photometry in this then Kalas & Jewitt (1995) refer to such a feature as the butterfly second epoch agrees well with that of the first epoch (on av- asymmetry. The butterfly asymmetry is evident in the mor- erage, the 2007 January disk photometry is 0.13 mag phology of b Pic that Golimowski et al. (2006) recently related arcsecϪ2 fainter than 2006 October), suggesting that our frame to the presence of a second disk midplane tilted relative to the selection technique for the first epoch of cloudy conditions main disk midplane. However, our detection of HD 15115’s east effectively filtered out nonphotometric data. midplane has insufficient signal-to-noise to confirm the presence of a width asymmetry here. We note that none of the surface brightness profiles show evi- 3. RESULTS dence for significant flattening inward toward the star (Fig. 3). All Figure 1 shows the PSF-subtracted images of HD 15115 four surface brightness profiles are well represented by a single with HST and with Keck. The west side of the disk in the power-law decrease with radius. If there is an inner dust depletion, and is detected from then it resides within a 40 AU radius. This constraint is consistent 0.5 ע optical HST data hasP.A. p 278Њ.5 the edge of the occulting spot at 1.5Љ (67 AU) radius to the with model fits of the spectral energy distribution that place the edge of the field at 12.38Љ (554 AU) radius. The east midplane dominant emitting dust component at 35 AU radius (Zuckerman is detected as far as 7Љ (315 AU) radius. At this radius the &Song2004;Williams&Andrews2006).∼ ∼ east midplane begins to intersect the outer portion of the co- The color of the disk may be estimated in the 2.0"" –3.3 "" ronagraph’s 3.0Љ occulting spot. FurtherHD east, 15115’s past the spot and debrisregion where the diskH-band and V-band data overlap (Fig. 3). At V band (HST) H band (Keck) 5” 5” Kalas et al. 2007 p p Fig. 1.—False-color,• High log scale fractional images of the HDluminosity 15115 disk as originally disk discovered (5x10^-4; using the Moor ACS/HRC F606Wet al. (l c2006)591 nm,Dl 234 nm; left)and confirmed in H band with Keck II adaptive optics (right;2006October26data).Northisup,eastisleft,andthescalebarsspan5Љ. In the HST image we use gray fields over the occulting bar and a 3.0Љ occulting spot located to the left of HD 15115, as well as a gray disk covering PSF-subtraction artifacts surrounding HD 15115 itself.• IfVery the HD 15115asymmetric disk were a symmetric structure, then the east side of the disk would have been detected within the rectangular box, shown below the ACS/HRC occulting finger. The NIR data (right) show a more symmetric disk within a 2Љ radius, with asymmetry becoming more apparent beyond the 2Љ radius. Due to poor observing conditions, the field is contaminated by residual noise due to the diffraction pattern of the telescope (e.g., at 2 o’clockand 7 o’clock relative• toDynamical HD 15115). However, interactions whereas the residual with diffraction ISM pattern noiseto south-east? of the telescope rotates (Debes relative to the et sky al. orientation 2008) over a series of exposures, the image of the disk remains fixed and it is confirmed as real. • BLUE colors (V-H) → small dust grains (< ~ 1 µm?) (Kalas et al. 2007, Debes et al. 2008) Rodigas/NCAD/July 20, 2012 L42 DEBES, WEINBERGER, & SONG Vol. 684 Is the disk really that blue/asymmetric? No. 1, 2008 HD 15115 AT 1.1 mm L43 1.1 µm 1” Red 2” Blue Debes et al. 2008 Fig. 1.—Top: False-color images of the observations of HD 15115 in the F110W filter at two spacecraft orientations. The images are logarithmically scaled. Bottom: False-color, final combined image of the HD 15115 disk, showing the contaminatingRed feature inside A. The dashed line 1”? represents the nominal position angle of the disk at 278.9Њ, while the asterisk represents the position of the star. We have masked out separations in the disk within 0.68Љ, where 3” Blue PSF subtraction residuals dominate. Noticeable are a warp on the western lobe, Fig. 2.—Measurements of the HD 15115 disk midplane PA (top) and FWHM and the asymmetries between the western and eastern lobes. (bottom) as a function of distance for the two lobes of the disk. Squares represent the western lobe, while triangles represent the eastern lobe. The disk emission to measure the location of the midplane (and sharp rise in PA for the western lobe interior 1.7Љ is due to the warp, and the thus the local PA) as well as the FWHM of the disk. We took eastern lobe’s PA beyond 1.8Љ is marginally different than the western lobe. [See the electronic edition of the Journal for a color version of this figure.] an average of the values for both orientations and estimated the uncertaintyFavorable as being half for the differenceNIR betweenimaging the two Fig. 4.—Comparison of the scattering efficiency (or color) vs. wavelength Fig. 3.—Surface brightness profiles of the eastern and western lobes of the 0.23Љ apertures centered on the midplane of the disk. Be- measurements.disk in F110W magnitudes Figure 2 per shows square arcsecond the PA for and a 0.23 FWHMЉ # 0.23Љ ofaperture. the west- of HD 15115’s# disk at 1Љ (45 AU), 2Љ (90 AU), and 3Љ (135 AU). The symbols ernNo lobe corrections of the were disk applied. as a The function symbols are of the radius. same as in Beyond Fig. 2. [See 1.7 theЉ, we are the sametween as in 0.7 Fig.Љ 2.and The disk 1.8 dramaticallyЉ, the disk changes SB color of the over wavelength western lobe falls as 0.06עfrom0.1 the central star. [See theRodigas/NCAD/July electronic edition of the 20, Journal 2012Ϫ3.56 עelectronic edition of the Journal for a color version of this figure.] and distanceϪ1.4 for a colorrr version, of while this figure. at radii] 11.8Љ, the SB drops as . The 0.06ע0.2Њ,whichisconsistent Ϫ2.14עfind a PA for the disk of 278.9Њ .0.5Њ.However,interiorto eastern lobe drops steadily asr from 0.7Љ to 3Љעwith KFG07’s value of 278.5Њ for the H band ,0.02 ע 1.7Љits, we and note Strehl that ratios, the but disk no PA standard increases technique with is decreasing applied to dis- PSF, we found a correction of 1.23 Efficiency0.06, and for vs. F110W Wavelength we ע the study of circumstellar disks. Intuitively, one would expect we found a correction3.3.
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