2022A&A...666A..16C


Query : 2022A&A...666A..16C

2022A&A...666A..16C - Astronomy and Astrophysics, volume 666A, 16 (2022/10-1)

Updated orbital monitoring and dynamical masses for nearby M-dwarf binaries.

CALISSENDORFF P., JANSON M., RODET L., KOHLER R., BONNEFOY M., BRANDNER W., BROWN-SEVILLA S., CHAUVIN G., DELORME P., DESIDERA S., DURKAN S., FONTANIVE C., GRATTON R., HAGELBERG J., HENNING T., HIPPLER S., LAGRANGE A.-M., LANGLOIS M., LAZZONI C., MAIRE A.-L., MESSINA S., MEYER M., MOLLER-NILSSON O., RABUS M., SCHLIEDER J., VIGAN A., WAHHAJ Z., WILDI F. and ZURLO A.

Abstract (from CDS):

Young M-type binaries are particularly useful for precise isochronal dating by taking advantage of their extended pre-main sequence evolution. Orbital monitoring of these low-mass objects becomes essential in constraining their fundamental properties, as dynamical masses can be extracted from their Keplerian motion. Here, we present the combined efforts of the AstraLux Large Multiplicity Survey, together with a filler sub-programme from the SpHere INfrared Exoplanet (SHINE) project and previously unpublished data from the FastCam lucky imaging camera at the Nordical Optical Telescope (NOT) and the NaCo instrument at the Very Large Telescope (VLT). Building on previous work, we use archival and new astrometric data to constrain orbital parameters for 20 M-type binaries. We identify that eight of the binaries have strong Bayesian probabilities and belong to known young moving groups (YMGs). We provide a first attempt at constraining orbital parameters for 14 of the binaries in our sample, with the remaining six having previously fitted orbits for which we provide additional astrometric data and updated Gaia parallaxes. The substantial orbital information built up here for four of the binaries allows for direct comparison between individual dynamical masses and theoretical masses from stellar evolutionary model isochrones, with an additional three binary systems with tentative individual dynamical mass estimates likely to be improved in the near future. We attained an overall agreement between the dynamical masses and the theoretical masses from the isochrones based on the assumed YMG age of the respective binary pair. The two systems with the best orbital constrains for which we obtained individual dynamical masses, J0728 and J2317, display higher dynamical masses than predicted by evolutionary models.

Abstract Copyright: © P. Calissendorff et al. 2022

Journal keyword(s): astrometry - binaries: visual - stars: fundamental parameters - stars: low-mass - stars: kinematics and dynamics

Simbad objects: 35

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Number of rows : 35
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 NAME THA As* 00 00 -62.0           ~ 468 0
2 G 131-26 Er* 00 08 53.9201067097 +20 50 25.593272581   15.17 13.52 12.19 10.50 M5V 49 0
3 LP 467-16 LM* 01 11 25.422648 +15 26 21.51204   16.19 14.43 14.07 11.03 M5.93 85 0
4 LP 410-22 PM* 02 25 54.515376 +17 46 46.59816   16.24 14.63 14.30   M4.0 12 0
5 LP 993-116 ** 02 45 14.3221 -43 44 10.076   14.34 12.65 12.42   M5 34 0
6 Cl Melotte 25 OpC 04 29 47.3 +16 56 53           ~ 3082 0
7 * 51 Eri PM* 04 37 36.1326090888 -02 28 24.775726260   5.486 5.209     F0IV 242 0
8 StKM 1-497 TT* 04 37 37.4553491592 -02 29 28.950973764   12.04 10.59   8.59 M1.1V 128 0
9 SCR J0459-0333 LM* 04 59 58.5699604896 -03 33 12.202006716   15.41 13.89 13.49   M4 22 0
10 V* V1311 Ori BY* 05 32 04.5017687952 -03 05 29.400403884   13.37 11.437 11.019 9.153 M1.5V 67 0
11 NAME Ori Trapezium OpC 05 35 16.5 -05 23 14           ~ 1621 1
12 NAME Columba Association As* 06 04 19.4 -22 20 40           ~ 282 0
13 AL 442 ** 06 11 29.9663575314 -72 13 38.760064259   15.45 13.91 13.54   M4.5 31 1
14 HD 43162B ** 06 13 45.4057411320 -23 52 07.573121148   12.46   12.31 10.15 M3.5 18 0
15 NAME AB Dor Moving Group MGr 06 38 53.4 -42 50 04           ~ 472 0
16 CD-29 4446 SB* 07 28 51.3552114700 -30 14 49.309736426 12.47 11.60 10.08 9.83 7.885 M1Ve 84 0
17 LSPM J0907+2154 PM* 09 07 58.2260157216 +21 54 11.009659104   13.8   12.783   M2.0 10 0
18 LP 845-40 cC* 09 16 43.9646800272 -24 47 43.209547692     11.821 11.415 9.56 M0.5 19 0
19 [K2001c] 27 TT* 10 14 08.07 -76 36 32.8   15.802 14.186     M4 18 0
20 PM J10367+1521 ** 10 36 44.8457 +15 21 39.354     13.308 12.974   M4.0V 27 0
21 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1898 1
22 NAME TW Hya Association As* 11 01.9 -34 42           ~ 942 0
23 NAME Ursa Major Moving Group MGr 12 32 +57.0           ~ 439 2
24 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 777 0
25 StKM 2-1439 LM* 20 16 33.8719341388 -07 11 46.145885047   12.62 11.525 11.187   M0V 20 0
26 M 15 GlC 21 29 58.33 +12 10 01.2           ~ 3143 0
27 PM J21374-0555 ** 21 37 28.9957 -05 55 07.845     12.969 12.626   M3.0 10 0
28 G 68-5 LM* 23 17 28.1434392636 +19 36 47.216769536   13.69   11.627   M2V 62 0
29 PM J23261+1700 ** 23 26 11.8550140704 +17 00 07.651417248   15.47 13.85 13.51   M4.0V 11 0
30 RX J2326.2+2752 BY* 23 26 17.0669713224 +27 52 03.493251084   13.75 12.20 11.85   M3 12 0
31 RX J2349.8+2427 PM* 23 49 53.6700932784 +24 27 49.324615596     13.980 13.498   M3.5 15 0
32 NAME Carina Moving Group MGr ~ ~           ~ 47 0
33 NAME Octans Association As* ~ ~           ~ 90 0
34 NAME Argus Association As* ~ ~           ~ 230 0
35 NAME Carina-near Moving Group MGr ~ ~           ~ 91 0

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