2007A&A...476..229D


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.08CET04:19:41

2007A&A...476..229D - Astronomy and Astrophysics, volume 476, 229-242 (2007/12-2)

Multiple protostellar systems. II. A high resolution near-infrared imaging survey in nearby star-forming regions.

DUCHENE G., BONTEMPS S., BOUVIER J., ANDRE P., DJUPVIK A.A. and GHEZ A.M.

Abstract (from CDS):

Multiple systems are the product of protostellar core fragmentation. Studying their statistical properties in young stellar populations therefore probes the physical processes at play during star formation. Our project endeavors to obtain a robust view of multiplicity among embedded ClassI and Flat Spectrum protostars in a wide array of nearby molecular clouds to disentangle ``universal'' from cloud-dependent processes. We have used near-infrared adaptive optics observations at the VLT through the H, Ks and L' filters to search for tight companions to 45 ClassI and Flat Spectrum protostars located in 4 different molecular clouds (Taurus-Auriga, Ophiuchus, Serpens and L1641 in Orion). We complemented these observations with published high-resolution surveys of 13 additional objects in Taurus and Ophiuchus. We found multiplicity rates of 32±6% and 47±8% over the 45-1400AU and 14-1400AU separation ranges, respectively. These rates are in excellent agreement with those previously found among T Tauri stars in Taurus and Ophiuchus, and represent an excess of a factor ∼1.7 over the multiplicity rate of solar-type field stars. We found no non-hierarchical triple systems, nor any quadruple or higher-order systems. No significant cloud-to-cloud difference has been found, except for the fact that all companions to low-mass Orion protostars are found within 100AU of their primaries whereas companions found in other clouds span the whole range probed here. Based on this survey, we conclude that core fragmentation always yields a high initial multiplicity rate, even in giant molecular clouds such as the Orion cloud or in clustered stellar populations as in Serpens, in contrast with predictions of numerical simulations. The lower multiplicity rate observed in clustered Class II and Class III populations can be accounted for by a universal set of properties for young systems and subsequent ejections through close encounters with unrelated cluster members.

Abstract Copyright:

Journal keyword(s): stars: binaries: close - stars: formation - stars: pre-main sequence

Simbad objects: 78

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Number of rows : 78

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* AA Per Mi* 03 15 14.4493699914 +46 34 51.674234058   11.04 9.42     M6 24 0
2 IRAS 04016+2610 Y*O 04 04 43.071 +26 18 56.39     20.45     ~ 229 0
3 IRAS 04113+2758 ** 04 14 26.31 +28 06 04.5           ~ 57 0
4 NAME CoKu Tau 1 Y*O 04 18 51.4865838204 +28 20 26.105713878     19.3     K7+M 74 0
5 IRAS 04169+2702 Y*O 04 19 58.449 +27 09 57.07           K0-M4 99 1
6 IRAS 04239+2436 Y*O 04 26 56.297 +24 43 35.33           ~ 144 2
7 NAME DG Tau B Y*O 04 27 02.666 +26 05 30.38           ~ 126 1
8 IRAS 04248+2612 Y*O 04 27 57.307 +26 19 18.30           M 141 0
9 V* GV Tau TT* 04 29 23.734 +24 33 00.28 19.20         K7 266 2
10 NAME Tau-Aur Region SFR 04 30 +25.0           ~ 1183 1
11 HBC 393 FU* 04 31 34.077 +18 08 04.90           K3V/M3III 775 2
12 IRAS 04295+2251 Y*O 04 32 32.055 +22 57 26.67           K0-M4 84 0
13 IRAS 04302+2247 Y*O 04 33 16.501 +22 53 20.40           ~ 131 0
14 LDN 1536 DNe 04 33 24.6 +22 43 29           ~ 93 0
15 IRAS 04361+2547 Y*O 04 39 13.898 +25 53 20.63           ~ 183 1
16 IRAS 04365+2535 Y*O 04 39 35.194 +25 41 44.73           ~ 227 0
17 IRAS 04381+2540 Y*O 04 41 12.679 +25 46 35.42           K0-M2 119 2
18 Haro 6-33 TT* 04 41 38.8300758211 +25 56 26.681998749     18.40     M0.5 97 2
19 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1330 0
20 IRAS 04489+3042 Y*O 04 52 06.6859847880 +30 47 17.016855701           M2 61 0
21 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1912 1
22 V* V801 Ori Fl* 05 35 26.8300595489 -06 26 47.616088933     14.901   13.225 M0 76 1
23 NAME HH 34 IR Em* 05 35 29.8494479625 -06 26 58.295802627         18.18 ~ 89 0
24 [CTF93] 29 IR 05 36 05 -06 31.8           ~ 3 0
25 2MASS J05362513-0644418 Y*O 05 36 25.1312112025 -06 44 41.842095753     18.160   14.634 K4.5 50 0
26 2MASS J05372447-0658329 Y*O 05 37 24.4768626806 -06 58 32.904404770           K5 16 0
27 NAME Ori A MoC 05 38 -07.1           ~ 2619 0
28 V* V883 Ori FU* 05 38 18.0974260202 -07 02 25.963144400   14.80       F:I: 96 1
29 IC 430 ISM 05 38 18.24 -07 02 26.2     14.4     ~ 58 1
30 LDN 1641 MoC 05 39.0 -07 00           ~ 420 0
31 [MB91] 31 pr* 05 39 05.3710430611 -07 11 05.150904914     19.862   15.708 M0.2 17 0
32 [VSS88] 73 pr* 05 39 59.2631842044 -07 37 33.046046733   11.59 10.82 10.37   F9.5 15 0
33 V* V1791 Ori Or* 05 40 37.3591178327 -08 04 03.017021735     11.55   11.822 F 25 0
34 IRAS 05385-0907 pr* 05 40 53.8909723681 -09 06 04.330821610           ~ 6 0
35 V* DL Ori Em* 05 41 25.3543568979 -08 05 54.724911984     12.00     K1 48 0
36 IRAS 05391-0836 * 05 41 34.9 -08 35 25           M0 10 0
37 IRAS 05393-0822 pr* 05 41 44.8717156399 -08 21 30.626125932     20.798   16.052 ~ 13 0
38 Haro 4-491 pr* 05 42 26.4965678498 -07 58 50.849874724     17.445   14.524 K6 21 0
39 WLY 2-5 * 16 25 40.8043914721 -24 26 17.214627263           ~ 6 0
40 GSS 30 Y*O 16 26 21.38160 -24 23 04.0524           ~ 194 1
41 [JJK2008] SMM J162622-24225 smm 16 26 21.60 -24 22 54.8           ~ 40 0
42 [CHG85] GSS 30 IRS 3 Y*O 16 26 21.77376 -24 22 51.3948           ~ 53 0
43 [RR90] Oph 2320.8-1721 Y*O 16 26 22.26912 -24 24 07.0632           M8 62 0
44 [GY92] 21 Y*O 16 26 23.57976 -24 24 39.4956           K7 60 2
45 VSSG 27 Y*O 16 26 30.46896 -24 22 57.1440           M 56 1
46 BKLT J162636-241554 Y*O 16 26 36.8346898479 -24 15 51.848175020       17.37 15.67 K7-M1 30 1
47 CRBR 2356.6-3058 Y*O 16 26 58.27872 -24 37 40.9584           ~ 21 0
48 WL 17 Y*O 16 27 06.77616 -24 38 14.9964           ~ 80 0
49 [JJK2008] SMM J162707-24381 smm 16 27 07.10 -24 38 13.4           ~ 46 0
50 Elia 2-29 Y*O 16 27 09.43032 -24 37 18.7716           ~ 261 1
51 WL 20 Y*O 16 27 15.69840 -24 38 43.4364           ~ 78 0
52 NAME WL 20E Y*O 16 27 15.87648 -24 38 43.3896           ~ 71 0
53 YLW 13B Y*O 16 27 21.46872 -24 41 43.0692           ~ 83 0
54 WL 6 Y*O 16 27 21.80448 -24 29 53.3616           ~ 111 0
55 CRBR 2422.8-3423 Y*O 16 27 24.61320 -24 41 03.4080           ~ 78 1
56 YLW 15 Y*O 16 27 26.93640 -24 40 50.8224           ~ 233 1
57 YLW 16A Y*O 16 27 28.02744 -24 39 33.5052           K8 181 0
58 YLW 16B Y*O 16 27 29.43528 -24 39 16.1892           ~ 98 0
59 Elia 2-33 Y*O 16 27 30.18024 -24 27 43.3656           M2 104 1
60 IRAS 16245-2423 TT* 16 27 37.1911764648 -24 30 35.031583716       16.66 14.67 B5-F2 224 0
61 YLW 45 Y*O 16 27 39.82824 -24 43 15.0672           ~ 103 0
62 [JJK2008] SMM J162740-24431 smm 16 27 39.90 -24 43 13.2           ~ 74 0
63 YLW 52 Y*O 16 27 51.80472 -24 31 45.5304           ~ 60 0
64 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2943 0
65 ISO-Oph 200 Y*O 16 31 43.7601980245 -24 55 24.587358028           ~ 12 0
66 ISO-Oph 204 TT* 16 31 52.1212410606 -24 56 15.712413458           ~ 34 0
67 LDN 1689 DNe 16 32 22.5 -24 28 29           ~ 104 0
68 ESO-HA 279a cor 18 29 31.976 +01 18 42.59           K6.5 29 1
69 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 886 2
70 HBC 672 Em* 18 29 56.8828626544 +01 14 46.339137067   17.6       K8.0 98 0
71 2MASS J18295760+0113004 Y*O 18 29 57.602 +01 13 00.42           ~ 34 3
72 IRAS 18274+0112 Y*O 18 29 57.73680 +01 14 05.6940           M4: 132 2
73 2MASS J18295784+0112379 Y*O 18 29 57.849 +01 12 37.90           ~ 22 0
74 2MASS J18295785+0112514 Y*O 18 29 57.858 +01 12 51.40           ~ 58 3
75 [EC92] 95 Y*O 18 29 57.893 +01 12 46.25           K1.0 71 3
76 2MASS J18295876+0114257 Y*O 18 29 58.765 +01 14 25.78           ~ 24 1
77 2MASS J18300274+0112280 Y*O 18 30 02.747 +01 12 28.06           ~ 27 2
78 V* WY Cas S* 23 58 01.3075303591 +56 29 13.468672815   12.48 10.76     S6-6.5/6-e 68 0

    Equat.    Gal    SGal    Ecl

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2019.12.08-04:19:41

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