2019A&A...623A.112D


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.05CET12:28:56

2019A&A...623A.112D - Astronomy and Astrophysics, volume 623A, 112-112 (2019/3-1)

Stellar population of Sco OB2 revealed by Gaia DR2 data.

DAMIANI F., PRISINZANO L., PILLITTERI I., MICELA G. and SCIORTINO S.

Abstract (from CDS):


Context. The Sco OB2 association is the nearest OB association, extending over approximately 2000 square degrees on the sky. Only its brightest and most massive members are already known (from HIPPARCOS) across its entire size, while studies of its lower mass population refer only to small portions of its extent.
Aims. In this work we exploit the capabilities of Gaia DR2 measurements to search for Sco OB2 members across its entire size and down to the lowest stellar masses.
Methods. We used both Gaia astrometric (proper motions and parallaxes) and photometric measurements (integrated photometry and colors) to select association members, using minimal assumptions derived mostly from the HIPPARCOS studies. Gaia resolves small details in both the kinematics of individual Sco OB2 subgroups and their distribution with distance from the Sun. We developed methods to explore the 3D kinematics of a stellar population covering large sky areas.
Results. We find nearly 11000 pre-main-sequence (PMS) members of Sco OB2 (with less than 3% field-star contamination), plus ∼3600 main-sequence (MS) candidate members with a larger (10-30%) field-star contamination. A higher confidence subsample of ∼9200 PMS (and ∼1340 MS) members is also selected (<1% contamination for the PMS), however this group is affected by larger (∼15%) incompleteness. We separately classify stars in compact and diffuse populations. Most members belong to one of several kinematically distinct diffuse populations, whose ensemble clearly outlines the shape of the entire association. Upper Sco is the densest region of Sco OB2. It is characterized by a complex spatial and kinematical structure and has no global pattern of motion. Other dense subclusters are found in Lower Centaurus-Crux and in Upper Centaurus-Lupus; the richest example of the latter, which has been recently identified, is coincident with the group near V1062 Sco. Most of the clustered stars appear to be younger than the diffuse PMS population, suggesting star formation in small groups that rapidly disperse and are diluted, reaching space densities lower than field stars while keeping memory of their original kinematics. We also find that the open cluster IC 2602 has a similar dynamics to Sco OB2, and its PMS members are currently evaporating and forming a diffuse (size ∼10°) halo around its double-peaked core.

Abstract Copyright: © ESO 2019

Journal keyword(s): open clusters and associations: individual: Sco OB2 - stars: pre-main sequence - parallaxes - proper motions

VizieR on-line data: <Available at CDS (J/A+A/623/A112): pms.dat ums.dat list.dat fits/*>

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

CDS comments: UCL-1, -2, -3 not in SIMBAD.

Simbad objects: 33

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Number of rows : 33

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 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 3064 0
2 HD 79208 * 09 09 50.2482625928 -62 17 09.819558113   9.64 9.31     A9V 9 0
3 TYC 8944-1821-1 * 09 10 51.4433124497 -62 20 48.688512408   12.40 11.23     ~ 3 0
4 * i Car * 09 11 16.7208929 -62 19 01.129500 3.13 3.774 3.943     B3V 106 0
5 HD 79796 * 09 13 12.5216888539 -62 25 19.917104337   9.62 9.17     F5IV 7 0
6 HD 309549 * 09 13 19.5154050243 -62 25 47.559296529   10.96 10.51     G0 6 0
7 V* V479 Car Ro* 09 23 34.9795566274 -61 11 35.880725963   10.77 10.134   9.181 K1V(e) 33 0
8 HD 81991 * 09 26 38.8767154588 -60 40 35.243339940   9.75 9.30     F3V 11 0
9 HD 87933 * 10 06 53.0358404910 -53 54 48.385970946   8.45 8.02     F5V 21 0
10 IC 593 GiG 10 08 18.0005782793 -02 31 36.432405376   14.2       ~ 28 0
11 HD 90692 * 10 27 08.0793546141 -49 47 15.488533373   8.48 8.30     A5/7V 9 0
12 HD 91922 * 10 35 50.5719105499 -47 05 55.817239982   8.42 8.02     F3V 7 0
13 IC 2602 OpC 10 42 58 -64 24.0           ~ 571 0
14 HD 93749 * 10 48 43.8961085115 -43 25 20.183707289   9.05 8.76     F0III/IV 8 0
15 UCAC2 13751697 * 10 51 21.3732154664 -42 06 44.629720398   13.32 12.40 12.19 11.42 ~ 1 0
16 TYC 7728-1105-1 * 10 54 47.7600659474 -41 10 41.977927772   11.18 10.49     ~ 2 0
17 TYC 7728-1101-1 * 10 55 00.5941299801 -41 01 04.334049031   12.91 11.90     ~ 1 0
18 HD 96054 ** 11 04 16.6549704279 -36 43 17.394857537   7.34 7.11     A8V 16 0
19 TYC 6662-147-1 * 11 19 20.7721026009 -29 45 06.611027450   11.646 11.085     ~ 2 0
20 NAME Lower Centaurus Crux As* 12 19 -57.1           ~ 372 1
21 NAME Upper Centaurus Lupus As* 15 24 -41.9           ~ 378 1
22 NAME Lupus I Cld 15 43 02.1 -34 09 06           ~ 236 0
23 NAME Lup II MoC 15 57 08 -37 47.1           ~ 97 1
24 NAME Lupus IV MoC 16 03 12.4 -42 07 43           ~ 133 0
25 NAME Lupus III SFR 16 09.6 -39 03           ~ 283 0
26 NAME Upper Sco Association As* 16 12 -23.4           ~ 1086 1
27 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1160 1
28 NAME rho Oph Cluster Cl* 16 26 22 -24 23.7           ~ 53 0
29 V* V1062 Sco a2* 16 38 30.9410761468 -39 09 08.390526654   6.92 6.95     ApSi 47 0
30 LDN 1746 DNe 17 11.3 -27 22           ~ 117 0
31 NAME Oph Cluster ClG 17 12 24.7 -23 21 01           ~ 246 0
32 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 351 1
33 GAL 000.0+00.0 gam 17 45 39.60213 -29 00 22.0000           ~ 12012 0

    Equat.    Gal    SGal    Ecl

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2021.03.05-12:28:56

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