2006AJ....131.2967M


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.21CET06:41:53

2006AJ....131.2967M - Astron. J., 131, 2967-2979 (2006/June-0)

Precision kinematics and related parameters of the α Persei open cluster.

MAKAROV V.V.

Abstract (from CDS):

A kinematical study of the nearby open cluster α Persei is presented based on the astrometric proper motions and positions in the Tycho-2 catalog and Second USNO CCD Astrographic Catalog (UCAC2). Using the astrometric data and photometry from the Tycho-2 and ground-based catalogs, 139 probable members of the cluster are selected, 18 of them new. By the classical convergent point method, systematic motions of stars inside the cluster and velocity dispersions are estimated. As directly observed, the upper limit on the internal velocity dispersion per coordinate is 1.1 km/s. The actual velocity dispersion is much smaller than that value, since all of it appears to come from the expected errors of the astrometric proper motions. The relative position of the convergent point with respect to the cluster stars yields the ``astrometric'' radial velocity, which turns out larger by a few km/s than the mean observed spectroscopic radial velocity. This implies an overall contraction of the cluster. Kinematic parallaxes are computed for each member, and an improved H-R diagram is constructed. An age of 52 Myr is determined by isochrone fitting. The star α Per itself fits an isochrone of this age computed with overshooting from the boundary of the convective zone. The theoretical mass of the star α Per is 6.65 M. With respect to the common center of mass, half of the higher mass members (earlier than G) are located within a radius of 10.3 pc. The cluster appears to be roughly twice as large, or as sparse, as the Pleiades, retaining nonetheless a similar dynamical coherence. The low rate of binaries is another feature of this cluster, where we find only about 20% of members to be known or suspected spectroscopic, astrometric, or visual binaries or multiple systems. X-ray emitters in the cluster appear to have the same dispersion of internal velocities as the rest of the membership. The cluster is surrounded by an extended, sparse halo of comoving dwarfs, which are found by combining the proper-motion data from UCAC2 with Two Micron All-Sky Survey infrared photometry. Since many of these external stars are outside the tidal radius, the cluster being in an active stage of disintegration or evaporation could be considered. This hypothesis is not supported by the weak compression and the nonmeasurable velocity dispersion found in the kinematic analysis. A search for stars ejected from the α Persei cluster is carried out by tracking a large number of nearby stars 70 Myr back in time and matching their positions with the past location of the cluster. Only one plausible ejection is found prior to 10 Myr ago. The nearby star GJ 82, an active M dwarf with a strong Hα emission, is likely a former member ejected 47 Myr ago at 5 km/s.

Abstract Copyright:

Journal keyword(s): Stars: Binaries: General - Galaxy: Open Clusters and Associations: General - Stars: Kinematics

VizieR on-line data: <Available at CDS (J/AJ/131/2967): table1.dat>

Nomenclature: Table: Cl* Melotte 20 M NNN (Nos 1-139).

Status at CDS : All or part of tables of objects could be ingested in SIMBAD with priority 2.

CDS comments: Designation HE = Cl Melotte 20 in SIMBAD (ex. Cl Melotte 20 605 is the star alf Per).

Simbad objects: 42

goto Full paper

goto View the reference in ADS

Number of rows : 42

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 Ross 15 Er* 01 59 23.5138062650 +58 31 16.105242872   12.90 12.155 11.871   M4Ve 81 0
2 V* V572 Per Al* 03 15 48.67668 +50 57 21.2108   6.79 6.71     A0 25 1
3 Cl Melotte 20 350 ** 03 17 36.9405473883 +48 50 08.504554446   11.87 11.20 10.99   ~ 35 1
4 HD 20282 * 03 17 43.2783083645 +50 21 39.699166131 9.628 7.63 7.51     A0 9 0
5 HD 20537 * 03 20 23.6671996224 +51 37 06.091638143   7.30 7.29     B9 25 0
6 Cl* Melotte 20 AP 97 * 03 20 41.8725806259 +48 24 37.540568528   12.95 12.08   11.33 G6.5 19 0
7 Cl* Melotte 20 AP 102 * 03 21 20.2133396863 +48 45 27.025701687   12.76 11.96   11.27 ~ 14 0
8 BD+48 892 * 03 21 40.2205897866 +49 07 12.824596897   9.92 9.60     F3IV-V 49 0
9 HD 20675 PM* 03 21 52.5332653198 +49 04 15.256137087       5.7   F6V 71 0
10 HD 20701 * 03 22 03.5601184275 +47 56 04.754936438   8.46 8.35     A1V 29 0
11 * alf Per V* 03 24 19.3700924 +49 51 40.245455 2.64 2.27 1.79     F5Ib 805 1
12 Cl* Melotte 20 AP 14 * 03 24 19.9236694393 +48 47 19.834522647   12.77 11.94     G4 17 0
13 Cl* Melotte 20 AP 25 * 03 25 16.2285473206 +48 22 23.915438390   13.13 12.25   11.50 K0 20 0
14 Cl Melotte 20 696 * 03 26 19.3612946597 +49 13 32.494576942   12.37 11.61     G3 27 0
15 HD 21117 * 03 26 39.4502640523 +50 50 47.406697453 7.700 7.720 7.630     B8 25 0
16 Cl Melotte 20 OpC 03 26 42 +48 48.0           ~ 765 0
17 HD 232793 * 03 27 14.1291525608 +50 52 43.995000853   10.68 10.12     F5V 26 0
18 V* V534 Per BY* 03 27 51.0404936330 +49 12 10.037450384   13.21 12.29     K2 17 0
19 Cl Melotte 20 828 * 03 28 59.6428788283 +48 14 08.236806088   12.30 11.59     ~ 19 0
20 * 34 Per * 03 29 22.05019 +49 30 32.2114 4.01 4.610 4.735     B3V 156 0
21 BD+48 931 * 03 29 46.8612655833 +49 00 34.219274948   9.72 9.21     F6V 19 0
22 HD 21481 Em* 03 29 49.9910035558 +47 58 36.546620098   7.77 7.66     A0Vn 55 0
23 HD 21479 * 03 29 51.8809257252 +49 12 48.500782866   7.38 7.31     A1IVn 52 0
24 1RXS J033042.8+490314 X 03 30 42.3 +49 03 03           ~ 2 0
25 HD 21641 Be* 03 31 33.1358824052 +47 51 44.698818825 6.47 6.733 6.763     B8.5V 90 0
26 HD 21672 * 03 31 53.9459006555 +48 44 06.529697794   6.61 6.63     B8V 62 0
27 BD+49 958 * 03 31 58.7243287204 +49 52 12.598794012   9.58 9.25     F1V 44 0
28 Cl* Melotte 20 AP 199 * 03 32 44.4414116386 +47 41 35.135108746   13.08 12.10     ~ 7 0
29 HD 21931 * 03 34 12.9645235601 +48 37 02.909706330   7.39 7.37     B9V 62 1
30 Cl Melotte 20 1102 * 03 34 43.3626066997 +47 53 12.559910014   11.52 10.67     G1V 10 0
31 * psi Per Be* 03 36 29.3798227 +48 11 33.478941 3.60 4.17 4.23     B5Ve 397 0
32 TYC 3313-1551-1 * 03 38 50.5169321607 +46 36 12.580457941   10.81 10.25     G1 4 0
33 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 3047 0
34 HD 24980 * 04 00 20.4738899245 +47 34 18.100633788   8.56 8.36     A2 18 0
35 NAME Cas-Tau As* 04 16 +27.6           ~ 68 1
36 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2731 0
37 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2031 1
38 M 41 OpC 06 46 01 -20 45.4   4.89 4.5     ~ 250 0
39 NGC 2547 OpC 08 09 52.360 -49 10 35.01           ~ 323 0
40 NGC 2632 OpC 08 40 24 +19 40.0           ~ 1279 0
41 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11927 0
42 NGC 6547 G 18 05 10.020 +25 13 57.52   14.3       ~ 38 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2006AJ....131.2967M and select 'bookmark this link' or equivalent in the popup menu


2021.01.21-06:41:53

© Université de Strasbourg/CNRS

    • Contact