2016AJ....152..128M


Query : 2016AJ....152..128M

2016AJ....152..128M - Astron. J., 152, 128-128 (2016/November-0)

Imaging an 80 au radius dust ring around the F5V star HD 157587.

MILLAR-BLANCHAER M.A., WANG J.J., KALAS P., GRAHAM J.R., DUCHENE G., NIELSEN E.L., PERRIN M., MOON D.-S., PADGETT D., METCHEV S., AMMONS S.M., BAILEY V.P., BARMAN T., BRUZZONE S., BULGER J., CHEN C.H., CHILCOTE J., COTTEN T., DE ROSA R.J., DOYON R., DRAPER Z.H., ESPOSITO T.M., FITZGERALD M.P., FOLLETTE K.B., GERARD B.L., GREENBAUM A.Z., HIBON P., HINKLEY S., HUNG L.-W., INGRAHAM P., JOHNSON-GROH M., KONOPACKY Q., LARKIN J.E., MACINTOSH B., MAIRE J., MARCHIS F., MARLEY M.S., MAROIS C., MATTHEWS B.C., OPPENHEIMER R., PALMER D., PATIENCE J., POYNEER L., PUEYO L., RAJAN A., RAMEAU J., RANTAKYRO F.T., SAVRANSKY D., SCHNEIDER A.C., SIVARAMAKRISHNAN A., SONG I., SOUMMER R., THOMAS S., VEGA D., WALLACE J.K., WARD-DUONG K., WIKTOROWICZ S. and WOLFF S.

Abstract (from CDS):

We present H-band near-infrared polarimetric imaging observations of the F5V star HD 157587 obtained with the Gemini Planet Imager (GPI) that reveal the debris disk as a bright ring structure at a separation of ∼80-100 au. The new GPI data complement recent Hubble Space Telescope/STIS observations that show the disk extending out to over 500 au. The GPI image displays a strong asymmetry along the projected minor axis as well as a fainter asymmetry along the projected major axis. We associate the minor and major axis asymmetries with polarized forward scattering and a possible stellocentric offset, respectively. To constrain the disk geometry, we fit two separate disk models to the polarized image, each using a different scattering phase function. Both models favor a disk inclination of ∼70deg and a 1.5 ± 0.6 au stellar offset in the plane of the sky along the projected major axis of the disk. We find that the stellar offset in the disk plane, perpendicular to the projected major axis is degenerate with the form of the scattering phase function and remains poorly constrained. The disk is not recovered in total intensity due in part to strong adaptive optics residuals, but we recover three point sources. Considering the system's proximity to the galactic plane and the point sources' positions relative to the disk, we consider it likely that they are background objects and unrelated to the disk's offset from the star.

Abstract Copyright: © 2016. The American Astronomical Society. All rights reserved.

Journal keyword(s): planet-disk interactions - stars: individual: HD 157587 - techniques: polarimetric - techniques: polarimetric

Simbad objects: 15

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Number of rows : 15
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 * q01 Eri PM* 01 42 29.3145176952 -53 44 26.991453264   6.05 5.52     F9V 320 1
2 HD 15745 PM* 02 32 55.8109019904 +37 20 01.040152092   7.84 7.49   7.05 F0 77 0
3 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1886 1
4 HD 53143 PM* 06 59 59.6550515452 -61 20 10.252631566 8.035 7.609 6.803 6.375 5.99 G9V 160 0
5 HD 61005 PM* 07 35 47.4623556456 -32 12 14.045086368   8.96 8.22     G8Vk 223 0
6 HD 106906 * 12 17 53.1915103944 -55 58 31.893027240   8.95 8.89 8.46   F5V 151 0
7 NAME Lower Centaurus Crux As* 12 19 -57.1           ~ 476 1
8 HD 109573 PM* 12 36 01.0317461592 -39 52 10.220465388   5.786 5.774 7.25 5.81 A0V 627 1
9 HD 131835 * 14 56 54.4677661992 -35 41 43.658813184   8.05 7.86     A2IV 119 0
10 HD 157587 * 17 24 52.2398598216 -18 51 33.189129828   8.96 8.50     F5V 33 0
11 HD 197481 BY* 20 45 09.5324974119 -31 20 27.237889841   10.05 8.627 9.078 6.593 M1VeBa1 1136 0
12 HD 202629 * 21 19 21.8112423552 -57 30 46.359017208   10.759 9.924     K1III 8 0
13 HD 207129 PM* 21 48 15.7511634187 -47 18 13.017893348   6.18 5.58     G2V 328 0
14 * alf PsA PM* 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1231 3
15 NAME Pleiades Moving Group MGr ~ ~           ~ 277 1

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