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J/A+A/568/A51 Milky Way global survey of star clusters. III. (Schmeja+, 2014)
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Global survey of star clusters in the Milky Way.
III. 139 new open clusters at high Galactic latitudes.
Schmeja S., Kharchenko N.V., Piskunov A.E., Roeser S., Schilbach E.,
Froebrich D., Scholz R.-D.
<Astron. Astrophys. 568, A51 (2014)>
=2014A&A...568A..51S
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ADC_Keywords: Clusters, open ; Proper motions ; Milky Way
Keywords: techniques: photometric - catalogs - astrometry - stars: kinematics -
open clusters and associations: general - Galaxy: stellar content
Abstract:
We present a list of 139 new open clusters at high Galactic latitudes
(|b|>18.5deg) that are found in the frame of the project Milky Way
Star Clusters (MWSC). The target list was compiled as density
enhancements using the 2MASS catalogue. For confirmed clusters we
determined a homogeneous set of astrophysical parameters such as
membership, angular radii of the main morphological parts, proper
motion, distance, reddening, age, tidal parameters.
Description:
We were looking for stellar density enhancements using a star count
algorithm in the 2MASS point source catalogue (II/246). In total we
discovered 714 density enhancements (regarded as cluster candidates).
The candidates were cross-identified with known objects. Unidentified
objects were passed through the standard MWSC pipeline for
verification, cluster membership construction and structure, kinematic
and astrophysical parameter determination. The basic stellar data were
taken from the all-sky catalogue 2MAst (2MASS with Astrometry), that
was extracted from the all-sky catalogues PPMXL (Roeser et al. 2010,
Cat. I/317) and 2MASS (Cutri et al. 2003, Cat. II/246). We found
that 359 candidates coincide with known objects, other 355 candidates
are non identified, and 139 of them we classified as real star
clusters and determined their basic cluster parameters.
Around each confirmed object from our target list we defined a
circular area with a radius of ra=r2+radd where r2 is initial
estimate of cluster radius, and radd=0.3deg. In these areas we
selected in 2MAst only those stars with flags Rflg (the 2nd triple of
the flags in 2MASS) set to 1, 2, or 3 in each band, i.e. the stars
with the best quality detections in photometric and astrometric data.
The 139 sky areas with confirmed clusters contain about 0.52 mln 2MAst
stars with best quality detections in photometric and astrometric
data. We selected most probable members and determined - with a
homogeneous method/pipeline - angular sizes of the main morphological
parts, heliocentric distances, colour-excesses, mean proper motions,
ages, tidal parameters.
This work extends MWSC project having input list of 3784 targets by
714 new candidates. We have adopted for them that MWSC numbering
starts with 5001. Since the search was performed for Northern and
Southern hemispheres separately the candidate numbering is
discontinuous: the numbers 5001<=MWSC<5499 are assigned at b>18.5,
and 5500<=MWSC<5999 designate candidates at b<-18.5.
We present:
The Catalogue of new MWSC open clusters found at high galactic
latitudes (|b|>18.5deg) which includes several files:
Catalogue of cluster parameters (confirmed clusters only);
Index of all MWSC(|b|>18.5 deg) candidates;
Notes for every item of index list.
Within each list the entries are ordered along with MWSC number.
The Catalogues of the MWSC Stars in 139 circular sky areas with
confirmed clusters. Files are ordered by MWSC number; inside each sky
area the entries are ordered by Ks magnitudes.
The Atlas of new MWSC clusters diagrams.
In the Atlas the Cluster pages are ordered by MWSC number.
All the data are given in the same format as in the main MWSC catalogue
(Cat. J/A+A/558/A53).
Description of file: atlas/*
For each cluster we prepared two EPS-pages of diagrams:
* Page 1 contains the cluster map as the basic panel
(file MWSC_Name_map.eps.gz),
* Page 2 contains the Ks,(J-Ks) and Ks,(J-H) CMDs as basic panels
(file MWSC_Name_cmd.eps.gz).
The legend on each page gives the cluster name, MWSC number, (COCD
number); equatorial RAJ2000, DecJ2000, and galactic l, b coordinates
of the cluster centre; apparent cluster sizes r0, r1, r2, [number of
1sigma-members within the corresponding radius]; weighted average
components PM_(X,Y) of proper motion with their rms errors, [number of
stars used to compute the average]; the average radial velocity, RV
with their rms error, [the number of stars used to compute the
average]; distance to the cluster, d, distance modulus, (Ks-M_Ks);
NIR colour-excesses, E(J-H), E(J-Ks), interstellar extinction, A(Ks);
cluster age, its rms error, [the number of stars used to compute the
average age, or it is -1 if a manual isochrone fit was applied].
Additionally we show in the 2nd pages: an empirical correction
Delta_H for a better isochrone fit in the K_s,(J-H) diagram.
Symbols and their colours have the same meaning in all plots. Stars
are shown as coloured circles or dots. Cyan symbols mark stars outside
the cluster radius r2, green symbols are stars within r2. The most
probable kinematic and photometric members (1sigma-members) are
indicated in black, red, or blue. Black is for members located within
r1 (a visible radius of the central part), red for members between r1
and r2, and blue for stars outside r2 (the probabilities are formal).
Cyan bars show the uncertainty for 1sigma-members.
Description of files MWSC_Name_map.eps.gz (Page 1):
Page 1 contains five diagrams with spatial information.
The right panel is a map of the cluster neighborhood (MAP),
the left panels show (upside-down) relations depending on the distance from
the cluster centre, r, for:
-magnitude Ks (Ks vs. r),
-proper motions (PM vs. r),
-density profile diagram (DPD).
MAP:
Stars are displayed as small circles.
The circle size corresponds to the stellar magnitude ranged in six
Ks mag intervals:
< 6.0, 6.0 - 8.0, 8.0 - 10.0, 10.0 - 12.0, 12.0 - 14.0, > 14.0.
Blue cross : cluster centre selected in this study;
Blue plus : cluster centre from the literature;
Magenta plusses : centres of other clusters (from target list) visible
(if any) in the map;
Dotted blue large circle : cluster core border (r0);
Solid blue large circle : inner cluster border (r1);
Dashed blue large circle : cluster corona border (r2).
The left panels:
Blue vertical dotted, solid, dashed lines mark r0, r1, r2, respectively.
PM vs. r: Magenta horizontal lines correspond to the average proper
motion of the cluster determined in this paper;
DPD: Density profiles (Log of Number of stars per 1 sq.deg) are shown for
all stars (green line), 3sigma-members (blue line), 2sigma-members (magenta
line) and 1sigma-members (black line).
Description of files MWSC_Name_cmd.eps.gz (Page 2):
Page 2 contains diagrams with kinematic and photometric information.
The three left panels are:
-two PM_(X,Y) vs. Ks relations, i.e. PM-magnitude equation diagrams (MEDs);
-the vector point diagram of proper motions (VPD).
The two upper right panels are:
-relations (Ks,(J-H) and Ks,(J-Ks), i.e. the colour-magnitude diagrams
(CMDs).
The bottom right panels:
-colour-colour diagrams (CCDs);
-reddening-independent parameter Q-colour diagrams (QCDs).
The CCDs and QCDs are separated into two subpanels (as well as CMDs and MEDs
are separated into two parts via a broken line). The division is made with
respect to the Ks_mc magnitude: in the bottom subpanels we place data for Ks
> Ks_mc, in the upper ones - for Ks < Ks_mc, where Ks_mc is Ks-magnitude at
the bluest colour (J-Ks) of the isochrone closest to the determined cluster
age.
CMDs:
Magenta curve: the apparent isochrone closest to the determined cluster age;
Solid blue lines: left and right borders of a domain of 100% photometric
cluster members;
Solid red lines: ZAMS and TAMS (shown only in the Ks,(J-Ks) diagram), the
borders of the evolved Main Sequence stars;
Magenta dashed line: corresponds to the Ks_mc;
Thick yellow circles: stars selected for age determination;
Black arrows: increasing interstellar extinction vectors.
MED:
Magenta solid lines correspond to the average proper motion of the
cluster; the magenta dashed line corresponds to the Ks_mc.
CCD and QCD:
The Magenta curve corresponds to the apparent isochrone (observed magnitudes
and colours); the cyan curve corresponds to the intrinsic isochrone.