2014A&A...562A.111B


C.D.S. - SIMBAD4 rel 1.7 - 2019.08.18CEST11:52:50

2014A&A...562A.111B - Astronomy and Astrophysics, volume 562A, 111-111 (2014/2-1)

Characterization of the gaseous companion κ Andromedae b. New Keck and LBTI high-contrast observations.

BONNEFOY M., CURRIE T., MARLEAU G.-D., SCHLIEDER J.E., WISNIEWSKI J., CARSON J., COVEY K.R., HENNING T., BILLER B., HINZ P., KLAHR H., MARSH BOYER A.N., ZIMMERMAN N., JANSON M., McELWAIN M., MORDASINI C., SKEMER A., BAILEY V., DEFRERE D., THALMANN C., SKRUTSKIE M., ALLARD F., HOMEIER D., TAMURA M., FELDT M., CUMMING A., GRADY C., BRANDNER W., HELLING C., WITTE S., HAUSCHILDT P., KANDORI R., KUZUHARA M., FUKAGAWA M., KWON J., KUDO T., HASHIMOTO J., KUSAKABE N., ABE L., BRANDT T., EGNER S., GUYON O., HAYANO Y., HAYASHI M., HAYASHI S., HODAPP K., ISHII M., IYE M., KNAPP G., MATSUO T., MEDE K., MIYAMA M., MORINO J.-I., MORO-MARTIN A., NISHIMURA T., PYO T., SERABYN E., SUENAGA T., SUTO H., SUZUKI R., TAKAHASHI, TAKAMI M., TAKATO N., TERADA H., TOMONO D., TURNER E., WATANABE M., YAMADA T., TAKAMI H. and USUDA T.

Abstract (from CDS):

We previously reported the direct detection of a low-mass companion at a projected separation of 55±2 AU around the B9-type star κ Andromedae. The properties of the system (mass ratio, separation) make it a benchmark for understanding the formation and evolution of gas giant planets and brown dwarfs on wide orbits. We present new angular differential imaging (ADI) images of the system at 2.146 (Ks), 3.776 (L'), 4.052 (NB_4.05), and 4.78µm (M') obtained with Keck/NIRC2 and LBTI/LMIRCam, as well as more accurate near-infrared photometry of the star with the MIMIR instrument. We aim to determine the near-infrared spectral energy distribution of the companion and use it to characterize the object. We used analysis methods adapted to ADI to extract the companion flux. We compared the photometry of the object to reference young, and old objects and to a set of seven PHOENIX-based atmospheric models of cool objects accounting for the formation of dust. We used evolutionary models to derive mass estimates considering a wide range of plausible initial conditions. Finally, we used dedicated formation models to discuss the possible origin of the companion. We derive a more accurate J=15.86±0.21, H=14.95±0.13, Ks=14.32±0.09mag for κ And b. We detect the companion in all our high-contrast observations. We confirm previous contrasts obtained at Ks and L' band. We derive NB_4.05=13.0 ±0.2, and b mostly falls in the brown-dwarf regime, owing to remaining uncertainties in age and in mass-luminosity models. According to the formation models, disk instability in a primordial disk may account for the position and a wide range of plausible masses of κ And b.

Abstract Copyright:

Journal keyword(s): instrumentation: adaptive optics - techniques: photometric - planetary systems - stars: individual: kappa Andromedae

Simbad objects: 41

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Number of rows : 41

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME Tuc Moving Group MGr 00 00 -64.0           ~ 63 0
2 NAME THA As* 00 00 -62.0           ~ 311 0
3 HD 1160C LM* 00 15 57.2389782387 +04 15 09.090222186           M3.5 8 0
4 HD 1160B LM* 00 15 57.26 +04 15 03.7           ~ 21 0
5 HD 1160 * 00 15 57.3020078544 +04 15 04.004951787   7.159 7.119     A0V 71 1
6 NAME 2MASS J01033563-5515561(AB)b Pl 01 03 35.654 -55 15 56.23           ~ 29 1
7 2MASS J01415823-4633574 BD* 01 41 58.2345784233 -46 33 57.347491326           L2 62 0
8 2MASS J02411151-0326587 BD* 02 41 11.52 -03 26 58.8           L0 25 0
9 HD 23514B BD* 03 46 38.26 +22 55 09.4           M8 8 0
10 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2890 0
11 [BLH2002] KPNO-Tau 4 BD* 04 27 27.9997171623 +26 12 05.097974406     24.722 20.54 18.75 L0 63 0
12 CD-35 2722b Pl 06 09 19.2082646634 -35 49 31.062882043           ~ 48 1
13 NAME Columba Association As* 06 14.0 -40 03           ~ 182 0
14 HD 44627B BD* 06 19 12.94 -58 03 20.9           L1 104 1
15 CoRoT-20b Pl 06 30 52.9022405280 +00 13 36.858471822           ~ 26 1
16 HAT-P-20b Pl 07 27 39.9487418539 +24 20 11.518276475           ~ 50 1
17 IC 2391 OpC 08 40 32 -53 02.0     2.5     ~ 700 0
18 * alf Leo PM* 10 08 22.31099 +11 58 01.9516 0.88 1.24 1.40 1.37 1.47 B8IVn 796 1
19 HD 95086b Pl 10 57 03.0216129217 -68 40 02.446874288           ~ 63 1
20 NAME TW Hya Association As* 11 01.9 -34 42           ~ 789 0
21 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 604 1
22 HD 109573 PM* 12 36 01.0317721349 -39 52 10.222698506   5.786 5.774 7.25 5.81 A0V 530 1
23 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 517 0
24 HD 143567 * 16 01 55.4546289923 -21 58 49.397570493   7.27 7.19 7.87   B9V 93 1
25 NAME UScoCTIO 108B BD* 16 05 54.095 -18 18 48.86           ~ 37 2
26 NAME 1RXS1609 b Pl 16 09 30.3076191853 -21 04 58.945280778           ~ 87 1
27 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1071 1
28 HD 145689 PM* 16 17 05.4100392664 -67 56 28.624694971   6.090 5.944     A3V 50 0
29 NAME GSC 06214-00210 b Pl 16 21 54.6675132629 -20 43 09.138884434           ~ 52 2
30 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2467 0
31 * eta Tel ** 19 22 51.20620 -54 25 26.1473   5.035 5.020   4.99 A0V+M7/8V 178 0
32 * eta Tel B BD* 19 22 51.26 -54 25 30.7           M7.5V 64 1
33 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 846 1
34 HD 222109 * 23 37 32.04280 +44 25 44.3723   5.784 5.846     B8V 70 1
35 2MASS J23373296+4423122 * 23 37 32.9814775466 +44 23 12.261874876           ~ 1 0
36 * kap And b Pl 23 40 24.5064536189 +44 20 02.175809921           ~ 47 1
37 * kap And PM* 23 40 24.5076320 +44 20 02.156595 3.80 4.06 4.14 4.15 4.22 A0V 170 1
38 NAME AB Dor Moving Group MGr ~ ~           ~ 327 0
39 NAME Argus Association As* ~ ~           ~ 154 0
40 NAME Carina Moving Group MGr ~ ~           ~ 33 0
41 NAME Sirius-UMa Moving Group MGr ~ ~           ~ 13 0

    Equat.    Gal    SGal    Ecl

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2019.08.18-11:52:50

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