J/A+A/560/A76 Catalog of stellar clusters in the inner Galaxy (Morales+, 2013)
Stellar clusters in the inner Galaxy and their correlation with cold dust
emission.
Morales E.F.E., Wyrowski F., Schuller F., Menten K.M.
<Astron. Astrophys. 560, A76 (2013)>
=2013A&A...560A..76M 2013A&A...560A..76M
ADC_Keywords: Milky Way ; Clusters, open ; H II regions ; Molecular clouds;
Millimetric/submm sources ; Morphology ; Radial velocities
Keywords: open clusters and associations: general - Galaxy: disk -
Galaxy: stellar content - submillimeter: ISM - stars: formation -
catalogs
Abstract:
Stars are born within dense clumps of giant molecular clouds, and
constitute young stellar agglomerates known as embedded clusters,
which only evolve into bound open clusters under special conditions.
We statistically study all embedded clusters (ECs) and open clusters
(OCs) known so far in the inner Galaxy, in particular investigating
their interaction with the surrounding molecular environment and the
differences in their evolution.
Description:
We compiled a catalog of 695 embedded and open clusters within the
ATLASGAL Galactic range (|l|≤60° and |b|≤1.5°) from
different cluster catalogs in the literature, including 69 new (mostly
embedded) clusters discovered in this work using the Spitzer-GLIMPSE
survey (out of a total of 75 new clusters in the full GLIMPSE I and II
coverage). The catalog is focused on information related to the
correlation of the stellar clusters with the submm dust emission from
ATLASGAL (which traces dense molecular gas), including: the morphology
of the submm and mid-infrared emission, line velocities for the submm
clumps from the literature or follow-up observations, kinematic
distances, and membership in big molecular complexes. Additional
information from the literature is also provided, such as: correlation
with IR dark clouds, IR bubbles, and HII regions, stellar distance,
age, and the corresponding references.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
clusters.dat 774 695 The catalog of clusters for 300<l<60,, |b|≤1.5°
notes.dat 203 117 Notes
refs.dat 130 258 References
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See also:
B/ocl : Optically visible open clusters & Candidates (Dias+ 2002-2013)
J/A+A/397/177 : IR star clusters and stellar groups catalog (Bica+, 2003)
Byte-by-byte Description of file: clusters.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- ID [1/695] Identification number
5- 28 A24 --- Name Common designation
30- 65 A36 --- OName Other designations, comma-separated list
67- 79 A13 --- Cat Original catalogs, comma-separated list (1)
81- 87 F7.3 deg GLON Galactic longitude
89- 94 F6.3 deg GLAT Galactic latitude
96- 97 I2 h RAh Right ascension (J2000.0)
99-100 I2 min RAm Right ascension (J2000.0)
102-105 F4.1 s RAs Right ascension (J2000.0)
107 A1 --- DE- Declination sign (J2000.0)
108-109 I2 deg DEd Declination (J2000.0)
111-112 I2 arcmin DEm Declination (J2000.0)
114-115 I2 arcsec DEs Declination (J2000.0)
117-120 I4 arcsec Diam Angular diameter
122 A1 --- l_Dist Limit flag on Dist
123-127 F5.2 kpc Dist ? Distance (2)
129 A1 --- l_Dnear Limit flag on Dnear
130-133 F4.2 kpc Dnear ? Near Distance (2)
134 A1 --- --- [/]
135 A1 --- l_Dfar Limit flag on Dfar
136-140 F5.2 kpc Dfar ? Far Distance ?
145-148 F4.2 kpc e_Dist ? Error in Dist (3)
150-153 F4.2 kpc e_Dnear ? Error in Dnear (3)
154 A1 --- --- [/]
155-158 F4.2 kpc e_Dfar ? Error in Dfar (3)
160-173 A14 --- r_Dist Origin or reference for Dist,
in notes.dat file (7)
175-181 F7.2 Myr Age ? Age (4)
183-189 F7.2 Myr e_Age ? Error in Age (4)
191-198 A8 --- r_Age Reference(s) for Age, in refs.dat file
200-202 A3 --- Mtype Morphological type, as defined in Section 4.1
of the paper (18)
204-221 A18 --- Mflag Morphological flag, as defined in Section 3.1
of the paper (19)
223 A1 --- l_Sep Limit flag on Sep
224-229 F6.2 --- Sep [0/150] Normalized distance to the nearest
ATLASGAL emission pixel (8)
231-232 A2 --- Flg Flag about ATLASGAL and line velocities (9)
234-254 A21 --- NameVlsr Source name for line velocity
256-262 F7.2 km/s Vlsr ? (Molecular or ionized) gas line velocity
264-266 I3 --- r_Vlsr ? Reference(s) for Vlsr, in refs.dat file
268 A1 --- l_KDist Limit flag on KDist
269-273 F5.2 kpc KDist ? Kinematic distance from Vlsr (2)
275 A1 --- l_KDnear Limit flag on KDnear
276-279 F4.2 kpc KDnear ? Near Kinematic distance from Vlsr (2)
280 A1 --- --- [/]
281 A1 --- l_KDfar Limit flag on KDfar
282-286 F5.2 kpc KDfar ? Far Kinematic distance from Vlsr ?
288-291 F4.2 kpc e_KDist ? Error in KDist (3)
293-296 F4.2 kpc e_KDnear ? Error in KDnear (3)
297 A1 --- --- [/]
298-301 F4.2 kpc e_KDfar ? Error in KDfar (3)
303-304 A2 --- KDA Solution of the kinematic distance
ambiguity (10)
306-326 A21 --- r_KDA Reference(s) for KDA, in notes.dat file (11)
328-332 F5.2 kpc SDist ? Stellar distance
334-337 F4.2 kpc e_SDist ? Error in SDist
339-341 I3 --- r_SDist ? Reference for SDist, in refs.dat file
342-344 A3 ---- f_SDist [(K)] Recomputed SDist (12)
345 A1 --- --- [,]
346-348 I3 --- ref2 ? Second reference for SDist, in refs.dat file
350-352 I3 --- Dias ? Reference(s) for parameters adopted in
the Dias et al. (2002, B/ocl) catalog
354-364 A11 --- Conf Reference(s) for cluster confirmation or
further studies, in refs.dat file
366-397 A32 --- HII Associated HII region (13)
399-409 A11 --- Bub Associated IR bubble (14)
411-429 A19 --- IRDC Associated infrared dark cloud (15)
431 I1 --- noGL [0/1] 1 indicates no GLIMPSE data available
433-434 I2 --- SubCl [1/10]? Numeric flag that groups subclusters
436-454 A19 --- Complex Complex of physically associated clusters
harboring this cluster (16)
456-462 A7 --- r_Complex Reference(s) for Complex, in refs.dat file
464-654 A191 --- Comm1 Comments about the cluster (17)
656-774 A119 --- Comm2 Comments about associated objects (17)
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Note (1): The catalogs are identified as in Table 1 of the paper. Catalogs in
parentheses are not used in position/size averaging. The identification
codes are the following:
01 = Dias at al. (2002A&A...389..871D 2002A&A...389..871D, version 3.1)
02 = Kronberger et al. (2006A&A...447..921K 2006A&A...447..921K)
03 = Dutra & Bica (2000A&A...359L...9D 2000A&A...359L...9D)
04 = Bica et al. (2003A&A...397..177B 2003A&A...397..177B)
05 = Dutra et al. (2003A&A...400..533D 2003A&A...400..533D)
06 = Bica et al. (2003A&A...404..223B 2003A&A...404..223B)
07 = Lada & Lada (2003ARA&A..41...57L 2003ARA&A..41...57L)
08 = Porras et al. (2003AJ....126.1916P 2003AJ....126.1916P)
09 = Mercer at al. (2005ApJ...635..560M 2005ApJ...635..560M)
10 = Kumar at al. (2006A&A...449.1033K 2006A&A...449.1033K)
11 = Froebrich et al. (2007MNRAS.374..399F 2007MNRAS.374..399F)
12 = Faustini at al. (2009A&A...503..801F 2009A&A...503..801F)
13 = Glushkova et al. (2010AstL...36...75G 2010AstL...36...75G)
14 = Borissova et al. (2011A&A...532A.131B 2011A&A...532A.131B)
15 = Not cataloged (near-infrared; references given in r_Conf or Comm1)
16 = Not cataloged (mid-infrared; references given in r_Conf or Comm1)
17 = New GLIMPSE clusters (this work)
Note (2): When the kinematic distance ambiguity is not resolved, both near and
far distances are given, separated by "/". Upper and lower limits are
indicated by "<" and ">", respectively
Note (3): When the near and far distances are given, the corresponding errors
are separated by "/". When the distance is just an upper or lower limit,
the corresponding error does not exist and this is indicated by a "---"
Note (4): Format depends on the age range (all quoted as F7.2):
F4.2 for Age < 10 Myr,
F4.1 for 10 Myr ≤ Age < 100 Myr, and
I4 for Age ≥ 100 Myr
Note (7): The origin of adopted distance is indicated as:
K = Dist is KDist
S = Dist is SDist
KC = complex distance computed kinematically from an average position
and velocity, using the values compiled here for all the clusters
within the complex with available (and not repeated) Vlsr
SC = complex distance computed by averaging the stellar distances
(SDist) of the member clusters
Ref:N = From reference with identification number N in refs.dat
C(Ref:N) = distance for the whole complex adopted from reference with
identification number N in refs.dat.
CV(Ref:N) = complex distance computed kinematically from an average position
and velocity given by the reference with identification
number N in refs.dat
C(ID:M) = adopted for the whole complex the distance given for the cluster
with ID = M
Note (8): Normalized to the cluster angular radius.
Lower limits are indicated by ">"
Note (9): It is a two-digit flag. The first digit gives information about the
nearest ATLASGAL clump detected, and can take the values:
0 = when the nearest ATLASGAL clump does not seem to be associated with the
cluster
1 = when it does seem to be clearly associated
2 = physical connection less clear but still likely (in general, when the
clump appears to belong to the same star-forming region than the cluster)
The second digit of Flg provides information about the line velocities
Vlsr, and can take the values:
0 = when no velocity is available
1 = when Vlsr is from the nearest ATLASGAL clump or from a directly adjacent
clump
2 = when the clump with the velocity is not the nearest but within the field
of view covered by the cluster area
3 = when Vlsr is from a clump which is apparently associated with the cluster,
but is independent from the nearest one
4 = when Vlsr is the RRL velocity of the related HII region
Note (10): This flag can take the following values:
N = near solution
F = far solution
T = tangent point
NT = Vlsr within 7km/s of the terminal velocity, but with valid near solution
FT = Vlsr within 7km/s of the terminal velocity, but with valid far solution
B = KDist not computed, because the Galactocentric radius R<2.4kpc, i.e.,
in the region of the Galactic bar
Fb = Forbidden velocity, KDist not computed
A companion question mark (?) indicates a low-quality KDA solution.
Note on (11): An asterisk (*) following the reference means that the source
with resolved KDA is not the same as NameVlsr, but is close in phase-space.
A reference between parentheses means that it contradicts the adopted KDA
solution. The following non-numeric flags indicate complementary criteria
used in this work:
C = KDA solution for the whole associated complex, or from a particular
source in the complex
D = source associated with an IRDC, favoring the near distance
O = out of the solar circle, i.e., no ambiguity in the kinematic distance
S = adopted KDA solution consistent with the SDist
z = far distance discarded because otherwise z>200pc above the Galactic plane
Note (12): (K) indicates references giving a kinematic distance from average
stellar radial velocity. In theses cases, we recomputed the distance using
the same method as for KDist
Note (13): Flag "(UC)" at the end of the name indicates that the source is
classified as an UCHII region in the literature. Flag "(bub)" indicates that
the HII region appears to be associated with the listed IR bubble, but not
directly with the star cluster
Note (14): Bubble name is from the catalogs by Churchwell et al.
(2006ApJ...649..759C 2006ApJ...649..759C) or Churchwell et al. (2007ApJ...670..428C 2007ApJ...670..428C) when the
object is listed there, otherwise the identifier Bub(ID:M) is given, where M
is the ID of the associated stellar cluster
Note (15): IRDC name is from the catalogs by Simon et al. (2006ApJ...639..227S 2006ApJ...639..227S)
or Peretto & Fuller (2009A&A...505..405P 2009A&A...505..405P) when the object is listed there,
otherwise the identifier IRDC(ID:M) is given, where M is the ID of the
associated stellar cluster
Note (16): Complex name is from ref_Complex if the complex has been previously
identified in the literature. Small complexes of clusters whose IR
morphology suggests that they belong to the same star-forming region are
indicated by Complex = MC-i, where i is a record number. Bigger complexes of
clusters identified through the proximity of their members in the
phase-space are marked by Complex = KC-j, where j is another record number
Note (17): Quoted literature is indicated by the code Ref:N, where N is the
identification number in refs.dat
Note (18): The types are related to the cluster evolution stage:
EC1 = deeply embedded cluster
EC2 = partially embedded cluster
OC0 = emerging exposed cluster
OC1 = totally exposed cluster still physically associated with gas
OC2 = totally exposed cluster without correlation with ATLASGAL emission
Note (19): characterisation of the submm ATLASGAL emission around the
cluster position, made of 2 parts separated by a dot. The first part means:
emb = cluster fully embedded
p-emb = cluster partially embedded
surr = possibly associated submm emission surrounding the cluster
few = one or a few submm emission within the cluster area
few* = as few, but the submm emission is likely associed to the cluster
exp = exposed cluster, without submm emission
exp* = exposed cluster, with submm emission not associated with the cluster
The second part gives details about the mid-IR morphology:
bub-cen = presence of an IR bubble
bub-cen-trig = presence of an IR bubble and possible YSOs
bub-edge = the cluster appears at the edge of an IR bubble
pah = presence of emission related to PAH or warm dust
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Byte-by-byte Description of file: notes.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Note Code of the note
16-203 A188 --- Text Text of the note
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Ref [1/258] Reference number
5- 23 A19 --- BibCode BibCode
25- 58 A34 --- Author Author's name
60-130 A71 --- Comments Comments
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Acknowledgements:
Esteban Morales,
(End) Esteban Morales [MPIA, Germany], Patricia Vannier [CDS] 27-Sep-2013