Free Access
Issue
A&A
Volume 543, July 2012
Article Number A156
Number of page(s) 13
Section Galactic structure, stellar clusters and populations
DOI https://doi.org/10.1051/0004-6361/201118708
Published online 16 July 2012

Online material

Appendix A: MWSCS.Q2: The Catalogue of Milky Way Cluster Stars in the 2nd Galactic Quadrant

The Catalogue of the Milky Way Cluster Stars in the 2nd Galactic Quadrant (MWSCS.Q2) exists in machine-readable form only and can be retrieved from the CDS online archive9. The catalogue consists of 650 files with data on stars in areas with confirmed clusters. The information given for each star is shown in Table A.1.

Table A.1

Contents of the MWSCS table of stellar data.

Appendix B: MWSCD.Q2: the Catalogue of Milky Way Cluster Data in the 2nd Galactic Quadrant

Table B.1

Contents of the MWSCD main table.

The Catalogue of the Milky Way Cluster Data in the 2nd Galactic Quadrant (MWSCD.Q2) exists in machine-readable form only and can be retrieved from the CDS online archive. The catalogue consists of the main table with the derived parameters of the confirmed clusters, the list of all clusters, and a notes file. The latter two files contain all surveyed clusters including those that were NOT confirmed. To inform the reader on the data scope included in the catalogue, we describe here the main table (Table B.1). Object types are indicated by A1 strings: empty – open cluster, a – association, g – globular cluster, m – moving group, n – nebulosity/presence of nebulosity, r – remnant cluster,  ∗  – asterism. Source object types are given with A3 strings describing a larger variety of previous classifications, e.g. dubious clusters, clusters with variable extinction, embedded clusters, etc. The cluster metallicities have been adopted from the compilation of Dias et al. (2002a), their uncertainties are of about 0.1 dex.

Appendix C: MWSCA.Q2: the Atlas of Milky Way Cluster Diagrams in the 2nd Galactic Quadrant

thumbnail Fig. C.1

Open cluster King 19 in the MWSC atlas (page 1). See text for the description.

Open with DEXTER

For each cluster we prepared two pages of diagrams that are combined in the atlas. For a better understanding, we describe the diagrams of the atlas taking the cluster King 19 as an example.

We consider the cluster map as the basic diagram of the first page, and the CMDs Ks,(J − H) and Ks,(J − Ks) as the basic diagrams of the second page. Stars are shown as coloured circles or dots. Symbols and their colours have the same meaning in all plots. Cyan symbols mark stars outside the cluster radius r2, green symbols stars within r2. The most probable kinematic and photometric members (1σ-members) are indicated in black for members located within r1, red for members between r1 and r2, and blue for stars outside r2. Cyan bars show the uncertainty for 1σ-members (page 2).

Page 1 of the atlas (Fig. C.1) contains five diagrams with spatial information and a legend on the derived cluster parameters. The right panel is a map of the cluster surrounding, the left panels show magnitudes Ks, proper motions PMx, PMy, and surface density N versus distances r of stars from the cluster centre.

The sky map: stars are shown by circles. The size corresponds to star brightness arranged in six Ks magnitude bins. The blue cross indicates the cluster centre determined in this study, while the blue plus sign is the cluster position taken from the literature. If by chance other clusters appear in this cluster area, their centres are marked by magenta plus signs. Large blue circles (shown by dotted, solid, or dashed curves) indicate the cluster radii r0, r1, or r2, respectively. The left panels: blue vertical lines (dotted, solid, or dashed) mark r0, r1, or r2. Magenta horizontal lines in the PM vs. r diagrams correspond to the derived average proper motion of the cluster. The RDPs in the bottom panel are shown with green for all stars, blue for 3σ-members, magenta for 2σ-members and black for 1σ-members.

thumbnail Fig. C.2

Open cluster King 19 in the MWSC atlas (page 2). See text for the description.

Open with DEXTER

The legend gives cluster name, MWSC number, and COCD number in parentheses; equatorial RAJ2000, DecJ2000, and galactic l,   b coordinates of the cluster centre; apparent cluster sizes r0, r1, r2 and number of 1σ-members within the corresponding radius; weighted average components PMX,Y of proper motion with their rms errors and number of stars used to compute the average; the average radial velocity, RV, rms error, and the number of stars used to compute the average; distance to the cluster, d, distance modulus, (Ks − MKs); NIR interstellar reddening, E(J − H),   E(J − Ks), and interstellar extinction, A(Ks); cluster age, its rms error, the number in brackets gives the number of stars used to compute the average age, or it is  − 1 if an isochrone fitting was applied. ΔH shown below the photometric diagrams indicates the empirical correction to the H-magnitude introduced in Sects. 3.2 and 3.4.3.

Page 2 (Fig. C.2) contains three diagrams with kinematic information (left panels), and six diagrams with photometric information (right panels).

The three left panels with kinematic data: the two upper diagrams show PMX,Y vs. Ks relations, i.e.“PM-magnitude equation”. Magenta vertical lines correspond to the average proper motion of the cluster. The magenta dashed line shows the apparent magnitude , which corresponds to the bluest colour (J − Ks) of the adopted isochrone. The bottom panel is the vector point diagram of proper motions.

The six right panels with photometric data: the two upper diagrams are CMDs (Ks,(J − H) and Ks,(J − Ks)). The magenta curve is the apparent isochrone closest to the determined cluster age. Solid blue lines outline a domain of 100% photometric members. Solid red lines are the ZAMS and TAMS (shown only in Ks,(J − Ks)). The magenta dashed line shows the apparent magnitude . The thick yellow circles mark the stars used for the age determination (see Kharchenko et al. 2005a, for details). The black arrows show the vectors of increasing extinction. The four bottom panels show the two-colour (H − Ks)/(J − H) diagram (left column) and QJHK-colour diagram (right column).

The upper row is for stars brighter than , the lower row is for stars fainter than . Magenta curves indicate the apparent isochrone (i.e., observed colours), while cyan curves show the intrinsic isochrone.

The legend is the same as in page 1.


© ESO, 2012

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