2012A&A...546A..24R


Query : 2012A&A...546A..24R

2012A&A...546A..24R - Astronomy and Astrophysics, volume 546A24-24 (2012/10-1)

High-contrast imaging of the close environment of HD 142527. VLT/NaCo adaptive optics thermal and angular differential imaging.

RAMEAU J., CHAUVIN G., LAGRANGE A.-M., THEBAULT P., MILLI J., GIRARD J.H. and BONNEFOY M.

Abstract (from CDS):

It has long been suggested that circumstellar disks surrounding young stars may be the signposts of planets, and even more so since the recent discoveries of embedded substellar companions. According to models, the planet-disk interaction may create large structures, gaps, rings, or spirals in the disk. In that sense, the Herbig star HD142527 is particularly compelling, as its massive disk displays intriguing asymmetries that suggest the existence of a dynamical peturber of unknown nature. Our goal was to obtain deep thermal images of the close circumstellar environment of HD142527 to re-image the reported close-in structures (cavity, spiral arms) of the disk and to search for stellar and substellar companions that could be connected to their presence. We obtained high-contrast images with the NaCo adaptive optics system at the Very Large Telescope in L'-band. We applied different analysis strategies using both classical PSF-subtraction and angular differential imaging to probe for any extended structures or point-like sources. The circumstellar environment of HD142527 is revealed at an unprecedented spatial resolution down to the subarcsecond level for the first time at 3.8µm. Our images reveal important radial and azimuthal asymmetries that invalidate an elliptical shape for the disk. It instead suggests a bright inhomogeneous spiral arm plus various fainter spiral arms. We also confirm an inner cavity down to 30AU and two important dips at position angles of 0 and 135°. The detection performance in angular differential imaging enables exploration of the planetary mass regime for projected physical separations as close as 40AU. Use of our detection map together with Monte Carlo simulations sets stringent constraints on the presence of planetary mass, brown dwarf or stellar companions as a function of the semi-major axis. They severely limit any presence of massive giant planets with semi-major axis beyond 50AU, i.e. probably within the large disk's cavity which extends radially up to 145AU or even farther outside.

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Journal keyword(s): instrumentation: adaptive optics - stars: variables: T Tauri, Herbig Ae/Be - stars: individual: HD142527 - disks protoplanetary

VizieR on-line data: <Available at CDS (J/A+A/546/A24): list.dat fig/*>

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 1176 2
2 HD 44627B BD* 06 19 12.9988086984 -58 03 20.198341332           L1 155 1
3 HD 135344B Or* 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 548 0
4 NAME Upper Centaurus Lupus MGr 15 24 -41.9           ~ 567 1
5 Ass Sco OB 2-2 * 15 43.6 -27 19           ~ 20 0
6 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 741 1
7 RX J1609.5-2105B LM* 16 09 30.377 -21 04 56.97           ~ 123 0
8 NAME Upper Sco-Cen As* 16 15 -24.2           ~ 1497 1
9 * eta Tel PM* 19 22 51.2060774616 -54 25 26.145617376   5.035 5.020   4.99 A0V 228 0
10 * 51 Peg PM* 22 57 27.9804852576 +20 46 07.797040104 6.39 6.16 5.46 4.97 4.61 G2IV 1216 1
11 * alf PsA PM* 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1303 3
12 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1285 0

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