2018A&A...615A...9P

Query : 2018A&A...615A...9P

2018A&A...615A...9P - Astronomy and Astrophysics, volume 615A9-9 (2018/7-1)

Distribution of Serpens South protostars revealed with ALMA.

PLUNKETT A.L., FERNANDEZ-LOPEZ M., ARCE H.G., BUSQUET G., MARDONES D. and DUNHAM M.M.

Abstract (from CDS):


Context. Clusters are common sites of star formation, whose members display varying degrees of mass segregation. The cause may be primordial or dynamical, or a combination both. If mass segregation were to be observed in a very young protostellar cluster, then the primordial case can be assumed more likely for that region.
Aims. We investigated the masses and spatial distributions of pre-stellar and protostellar candidates in the young, low-mass star forming region Serpens South, where active star formation is known to occur along a predominant filamentary structure. Previous observations used to study these distributions have been limited by two important observational factors: (1) sensitivity limits that leave the lowest-mass sources undetected or (2) resolution limits that cannot distinguish binaries and/or cluster members in close proximity.
Methods. Recent millimeter-wavelength interferometry observations can now uncover faint and/or compact sources in order to study a more complete population of protostars, especially in nearby (D<500pc) clusters. Here we present ALMA observations of 1mm (Band 6) continuum in a 3x2-arcmin region at the center of Serpens South. Our angular resolution of ∼1'' is equivalent to ∼400 au, corresponding to scales of envelopes and/or disks of protostellar sources.
Results. We detect 52 sources with 1mm continuum, and we measure masses of 0.002-0.9 solar masses corresponding to gas and dust in the disk and/or envelope of the protostellar system. For the deeply embedded (youngest) sources with no IR counterparts, we find evidence of mass segregation and clustering according to: the minimum spanning tree method, distribution of projected separations between unique sources, and concentration of higher-mass sources near to the dense gas at the cluster center.
Conclusions. The mass segregation of the mm sources is likely primordial rather than dynamical given the young age of this cluster, compared with segregation time. This is the first case to show this for mm sources in a low-mass protostellar cluster environment.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: formation - stars: protostars - submillimeter: stars - techniques: interferometric - methods: observational

VizieR on-line data: <Available at CDS (J/A+A/615/A9): tablea1.dat list.dat fits/*>

Nomenclature: Fig. and Table A.1: [PFA2018] serpsNN (Nos 1-67).

Simbad objects: 98

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Number of rows : 98
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NGC 1333 OpC 03 29 09.2 +31 20 59           ~ 1575 1
2 IC 348 OpC 03 44 31.1 +32 10 02           ~ 1476 1
3 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4971 0
4 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2514 0
5 Cl Trumpler 14 OpC 10 43 56.0 -59 33 07   5.70 5.5     ~ 547 0
6 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1266 1
7 NGC 3603 OpC 11 14 57.9 -61 14 32           ~ 1136 1
8 4C 05.64 Bla 15 50 35.26924234 +05 27 10.4483641   19.10 18.73 19.02   ~ 371 1
9 Lupus 3 SFR 16 09.6 -39 03           ~ 348 0
10 NAME rho Oph Cluster Cl* 16 26 22 -24 23.7           ~ 73 0
11 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3969 1
12 Cl Westerlund 1 OpC 16 47 02.4 -45 51 07           ~ 655 1
13 QSO B1730-130 Bla 17 33 02.70578907 -13 04 49.5482119   18 19.50 18.78 17.39 ~ 1198 1
14 4C 09.57 BLL 17 51 32.81857326 +09 39 00.7284066   17.46 16.78 15.57   ~ 1007 1
15 EGO G011.92-0.61 of? 18 13 58.1 -18 54 17           ~ 54 0
16 [CBH2011b] G11.92-0.61 MM1 mm 18 13 58.103 -18 54 20.19           ~ 41 0
17 MIRES G028.6768+03.8471 Y*O 18 29 58.29 -02 01 21.0           ~ 3 0
18 [PFA2018] serps2 mm 18 29 58.3360 -02 01 18.859           ~ 1 0
19 MIRES G028.6763+03.8459 Y*O 18 29 58.49 -02 01 24.6           ~ 4 0
20 [PFA2018] serps4 mm 18 29 58.7160 -02 02 20.477           ~ 1 0
21 CXOU J182958.9-020125 Y*O 18 29 58.91 -02 01 25.5           ~ 7 0
22 2MASS J18295902-0201575 Y*O 18 29 59.023 -02 01 57.52           ~ 6 0
23 JCMTPP J182959.6-020100 Y*O 18 29 59.45 -02 01 06.4           ~ 10 0
24 HGBS J182959.6-020058 Y*O 18 29 59.66 -02 01 03.2           ~ 4 0
25 NAME Serpens South molecular cloud MoC 18 30 -02.0           ~ 116 0
26 2MASS J18300005-0202333 Y*O 18 30 00.050 -02 02 33.31           ~ 4 0
27 2MASS J18300056-0202112 Y*O 18 30 00.565 -02 02 11.22           ~ 6 0
28 2MASS J18300065-0202047 Y*O 18 30 00.659 -02 02 04.78           ~ 4 0
29 MIRES G028.6805+03.8359 Y*O 18 30 01.10 -02 01 27.8           ~ 6 0
30 MIRES G028.6757+03.8327 Y*O 18 30 01.24 -02 01 48.5           ~ 7 0
31 [PFA2018] serps12 Y*O 18 30 01.2390 -02 03 41.801           ~ 1 0
32 MSX6C G028.6477+03.8174 Y*O 18 30 01.320 -02 03 43.10           ~ 15 0
33 2MASS J18300228-0201596 Y*O 18 30 02.282 -02 01 59.66           ~ 6 0
34 [PFA2018] serps16 mm 18 30 02.4070 -02 02 49.219           ~ 2 0
35 2MASS J18300245-0202578 Y*O 18 30 02.450 -02 02 57.83           ~ 8 0
36 [MAM2011] SerpS-MM15 Y*O 18 30 02.45 -02 01 10.0           ~ 5 0
37 [MAM2011] SerpS-MM16 Y*O 18 30 02.4980 -02 02 48.337           ~ 7 0
38 [PFA2018] serps19 mm 18 30 02.6660 -02 02 42.254           ~ 1 0
39 2MASS J18300270-0203001 Y*O 18 30 02.706 -02 03 00.11           ~ 4 0
40 [KKT2016] VLA 9 Rad 18 30 02.80 -02 02 25.3           ~ 2 0
41 SSTgbs J1830028-020240 Y*O 18 30 02.839248 -02 02 40.59936           ~ 4 0
42 MIRES G028.6704+03.8224 Y*O 18 30 02.84 -02 02 22.4           ~ 4 0
43 [KKT2016] VLA 10 Rad 18 30 02.95 -02 02 32.2           ~ 2 0
44 SSTgbs J1830029-020133 Y*O 18 30 02.995656 -02 01 33.19460           ~ 3 0
45 NAME Serpens South Cluster Cl* 18 30 03.00 -02 01 58.2           ~ 148 0
46 [PFA2018] serps24 mm 18 30 03.0250 -02 03 23.399           ~ 1 0
47 [PFA2018] serps25 mm 18 30 03.1280 -02 02 39.377           ~ 1 0
48 SSTgbs J1830031-020234 Y*O 18 30 03.171384 -02 02 34.83201           ~ 4 0
49 2MASS J18300321-0203252 Y*O 18 30 03.215 -02 03 25.22           ~ 6 0
50 [PFA2018] serps28 mm 18 30 03.2990 -02 02 40.327           ~ 1 0
51 MHO 3247 Y*O 18 30 03.41 -02 02 45.3           ~ 15 0
52 [PFA2018] serps30 mm 18 30 03.4110 -02 02 52.165           ~ 1 0
53 [PFA2018] serps31 mm 18 30 03.4550 -02 01 31.377           ~ 1 0
54 SSTYSV J183003.48-020308.5 Y*O 18 30 03.488712 -02 03 08.57862           ~ 8 0
55 [PFA2018] serps32 mm 18 30 03.5200 -02 03 09.678           ~ 1 0
56 [PFA2018] serps34 mm 18 30 03.5750 -02 02 54.913           ~ 1 0
57 [PFA2018] serps35 mm 18 30 03.7440 -02 03 14.879           ~ 1 0
58 [PFA2018] serps36 mm 18 30 03.7760 -02 03 00.614           ~ 1 0
59 [PFA2018] serps37 mm 18 30 03.8010 -02 03 13.244           ~ 1 0
60 [KKT2016] VLA 14 Y*? 18 30 03.84 -02 03 12.2           ~ 2 0
61 [PFA2018] serps39 mm 18 30 03.9030 -02 03 12.861           ~ 1 0
62 [PFA2018] serps40 mm 18 30 03.9400 -02 02 59.886           ~ 1 0
63 [PFA2018] serps41 mm 18 30 04.0370 -02 03 00.932           ~ 1 0
64 2MASS J18300404-0201234 Y*O 18 30 04.046 -02 01 23.49           ~ 5 0
65 [PFA2018] serps43 mm 18 30 04.0600 -02 02 48.639           ~ 1 0
66 [KKT2016] VLA 12 Y*? 18 30 04.10 -02 03 02.5           ~ 30 0
67 [PFA2018] serps44 mm 18 30 04.1150 -02 03 06.961           ~ 1 0
68 [MAM2011] SerpS-MM18 Y*O 18 30 04.13 -02 03 02.1           ~ 19 0
69 [PFA2018] serps46 mm 18 30 04.1550 -02 03 03.548           ~ 1 0
70 [PFA2018] serps47 mm 18 30 04.2160 -02 03 06.955           ~ 1 0
71 [PFA2018] serps48 mm 18 30 04.2630 -02 03 08.577           ~ 1 0
72 2MASS J18300439-0201383 Y*O 18 30 04.398 -02 01 38.31           ~ 7 0
73 [KKT2016] VLA 15 Rad 18 30 04.60 -02 03 14.1           ~ 2 0
74 GBS-VLA J183004.81-020227.8 Y*O 18 30 04.789776 -02 02 27.91146           ~ 4 0
75 2MASS J18300497-0201424 Y*O 18 30 04.976 -02 01 42.50           ~ 3 0
76 [PFA2018] serps52 mm 18 30 05.0360 -02 03 18.612           ~ 1 0
77 MIRES G028.6849+03.8191 Y*O 18 30 05.15 -02 01 41.7           ~ 5 0
78 [PFA2018] serps53 mm 18 30 05.1530 -02 03 20.367           ~ 1 0
79 2MASS J18300515-0201044 Y*O 18 30 05.158 -02 01 04.49           ~ 6 0
80 SSTgbs J1830052-020206 Y*O 18 30 05.230368 -02 02 06.50341           ~ 5 0
81 MIRES G028.6593+03.8054 Y*O 18 30 05.26 -02 03 25.9           ~ 6 0
82 2MASS J18300527-0202341 Y*O 18 30 05.277 -02 02 34.17           ~ 8 0
83 SSTgbs J1830055-020107 Y*O 18 30 05.527008 -02 01 08.03319           ~ 4 0
84 [PFA2018] serps60 mm 18 30 05.7680 -02 01 58.145           ~ 1 0
85 2MASS J18300580-0201444 Y*O 18 30 05.810 -02 01 44.43           ~ 7 0
86 [PFA2018] serps62 mm 18 30 05.8470 -02 03 02.224           ~ 1 0
87 2MASS J18300619-0202196 Y*O 18 30 06.197 -02 02 19.60           M 7 0
88 SSTgbs J1830062-020304 Y*O 18 30 06.251952 -02 03 04.11352           ~ 4 0
89 [PFA2018] serps65 mm 18 30 06.3860 -02 03 03.713           ~ 1 0
90 [PFA2018] serps66 mm 18 30 06.5340 -02 03 04.281           ~ 1 0
91 [KKT2016] VLA 6 Rad 18 30 06.62 -02 01 28.9           ~ 2 0
92 MIRES G028.6593+03.7983 Y*O 18 30 06.77 -02 03 37.7           ~ 6 0
93 [KKT2016] VLA 8 Y*? 18 30 06.89 -02 02 11.5           ~ 2 0
94 NAME Aql Region reg 18 31.1 -02 10           ~ 456 0
95 LBN 028.77+03.43 HII 18 31 26.5 -02 04 22           ~ 255 2
96 NAME Aql Rift DNe 18 32 -01.0           ~ 355 1
97 Cl Berkeley 94 OpC 22 22 49.3 +55 51 46   9.10 8.7     ~ 50 0
98 Cl Berkeley 96 OpC 22 29 54.0 +55 24 31           ~ 38 0

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