2011A&A...531A..33C


Query : 2011A&A...531A..33C

2011A&A...531A..33C - Astronomy and Astrophysics, volume 531A, 33-33 (2011/7-1)

No substellar objects at the center of the Lupus 3 star-forming cloud.

COMERON F.

Abstract (from CDS):

Current surveys of nearby star-forming regions and young aggregates that produce samples of objects spanning the entire mass range down to masses of a few Jupiter masses can address questions about differences in the substellar mass function among different regions and the lowest masses of objects that can form in isolation. Deep imaging of a selected area in the Lupus 3 star-forming region, characterized by a large number of known young stellar objects, has been carried out with the goal of producing a complete sampling of the mass function down to sub-Jupiter masses. ICJHKS imaging complemented with intermediate-band imaging sensitive to methane absorption has been obtained with the VLT. The observed area measures 7'3x7'4 (0.42x0.43pc2 at 200pc) and the background is obscured by AV<5mag in approximately 70% of it. Detection limits (3σ) are IC=25.6, J=23.1, H=22.3, and KS=21.3. Cool objects with temperatures below 3000K are identified by means of reddening-free indices. Objects cooler than ∼1300K should also be detectable by comparing the flux in the H and methane-continuum bands. The luminosities of the 17 identified cool objects are too low in all cases to be consistent with membership in the star-forming region. Their number agrees with the statistical expectation for the background population of very low-mass stars. A reexamination of known candidate young stellar objects leads to excluding eight of them, reducing the number of bona fide members in the area to 15, of which ten lie in low extinction regions. The expectation based on the stars-to-brown dwarf ratios derived in other young aggregates is to find two or three new brown dwarfs, whereas none have been found. The low-mass young stellar object Par-Lup3-3 is found to consist of two close components of similar brightness separated by 0.3". A very faint object is also detected 1.2" from the jet-driving very low-mass star Par-Lup3-4 that, if confirmed as a physical companion, would have an estimated mass of 1-2MJup. The absence of brown dwarfs in one of the most crowded areas of the Lupus 3 clouds, although limited by small-number statistics, argues against a mass function rich in very low-mass objects, as might have been expected if the apparent overabundance of mid-M spectral types in Lupus extended toward later types. The results also stress the importance of critically examining the actual nature of previously identified candidate young stellar objects at the time of drawing statistical conclusions about the substellar population.

Abstract Copyright:

Journal keyword(s): brown dwarfs - stars: formation - stars: luminosity function, mass function

Nomenclature: Table 3: [C2011] JHHMMSS.ss+DDMMSS.s N=17.

CDS comments: Table 4 2MASS J16085427-3906575 is a misprint for 2MASS J16085427-3906057.

Simbad objects: 55

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Number of rows : 55
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1337 1
2 IC 348 OpC 03 44 32 +32 09.5           ~ 1314 1
3 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3972 0
4 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2160 1
5 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1549 1
6 NAME sigma Orionis Cluster MGr 05 38 42 -02 36.0           ~ 525 0
7 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1070 1
8 V* V856 Sco Ae* 16 08 34.2870044544 -39 06 18.325711332 7.66 7.41 7.05 6.92   A7IIIne_sh 370 0
9 V* V1027 Sco a2* 16 08 34.5616203192 -39 05 34.278268848   6.552 6.629 6.66   A0/3III 184 0
10 [C2011] J160845.47-390129.4 NIR 16 08 45.47 -39 01 29.4         24.89 ~ 1 0
11 [MJS2008] 61 Y*O 16 08 46.79 -39 02 07.4       22.28 21.04 ~ 7 0
12 [C2011] J160846.81-390303.0 NIR 16 08 46.81 -39 03 03.0         25.48 ~ 1 0
13 2MASS J16084747-3905087 Y*O 16 08 47.4985740432 -39 05 08.731928508       20.93 19.32 ~ 8 1
14 V* V1191 Sco Or* 16 08 48.1612456128 -39 04 19.195145724   18.23 16.43 15.71 13.57 M6.5 22 0
15 IRAS 16054-3857 Y*O 16 08 49.3987083072 -39 05 39.447341844   16.76 17.71 15.89 14.24 M4.5 45 0
16 [G2006] 82 * 16 08 49.6916979408 -39 01 22.509120036           ~ 2 0
17 V* V1192 Sco Or* 16 08 51.4348063536 -39 05 30.460358652     21.9 18.97 18.18 M5 65 0
18 V* V1193 Sco Or* 16 08 51.5693655096 -39 03 17.707587264   15.27 14.58 13.72 12.28 M4.5 59 0
19 [C2011] J160852.41-390347.0 NIR 16 08 52.41 -39 03 47.0         24.68 ~ 1 0
20 [C2011] J160852.58-390342.7 NIR 16 08 52.58 -39 03 42.7         24.30 ~ 1 0
21 2MASS J16085361-3904093 Y*O 16 08 53.615 -39 04 09.35       19.19 18.39 ~ 5 0
22 RX J1608.9-3905 TT* 16 08 54.2744987760 -39 06 05.799061764 12.57 11.91 10.88 10.28 9.74 ~ 22 0
23 Sz 112 Y*O 16 08 55.5289090032 -39 02 33.941081832   16.62 15.39 14.78 12.93 M6 57 0
24 [C2011] J160855.95-390351.4 NIR 16 08 55.95 -39 03 51.4         25.09 ~ 1 0
25 [C2011] J160856.33-390211.3 NIR 16 08 56.33 -39 02 11.3         24.75 ~ 1 0
26 [C2011] J160857.33-390121.3 NIR 16 08 57.33 -39 01 21.3         24.38 ~ 1 0
27 THA 15-34 Y*O 16 08 57.8026653048 -39 02 22.853868252   17.46 16.50 16.64 14.65 M6 50 0
28 [C2011] J160858.21-390253.5 NIR 16 08 58.21 -39 02 53.5         24.84 ~ 1 0
29 2MASS J16085828-3907355 Y*O 16 08 58.287 -39 07 35.55           ~ 11 0
30 2MASS J16085834-3907491 Y*O 16 08 58.347 -39 07 49.17           ~ 9 0
31 2MASS J16085890-3904460 Y*O 16 08 58.910 -39 04 46.02       21.76 19.79 ~ 5 0
32 [C2011] J160900.46-390118.0 NIR 16 09 00.46 -39 01 18.0         24.41 ~ 1 0
33 [C2011] J160901.36-390547.8 NIR 16 09 01.36 -39 05 47.8         25.36 ~ 1 0
34 [C2011] J160901.49-390139.9 NIR 16 09 01.49 -39 01 39.9         24.48 ~ 1 0
35 2MASS J16090155-3905055 BD? 16 09 01.559 -39 05 05.59           ~ 3 0
36 THA 15-35 Or* 16 09 01.8486544824 -39 05 12.414717240   15.33 14.12 14.35 12.54 M5.5 89 0
37 2MASS J16090245-3905494 Y*O 16 09 02.4534990840 -39 05 49.521871176       19.53 18.60 ~ 5 0
38 [C2011] J160902.60-390219.1 NIR 16 09 02.60 -39 02 19.1         24.06 ~ 1 0
39 [C2011] J160902.76-390144.1 NIR 16 09 02.76 -39 01 44.1         25.23 ~ 1 0
40 [C2011] J160903.52-390122.7 NIR 16 09 03.52 -39 01 22.7         23.44 ~ 1 0
41 2MASS J16090797-3907264 Y*O 16 09 07.975 -39 07 26.47         21.65 ~ 5 0
42 2MASS J16090849-3902133 PM* 16 09 08.4946942128 -39 02 13.411432464       13.75 11.97 ~ 3 0
43 2MASS J16090850-3903430 Y*O 16 09 08.5062297456 -39 03 43.080273612   18.00 16.60 16.43 14.16 ~ 11 0
44 [G2006] 96 X 16 09 10.6 -39 06 59           ~ 2 0
45 [G2006] 98 X 16 09 11.0 -39 04 03           ~ 2 0
46 [C2011] J160911.18-390314.8 NIR 16 09 11.18 -39 03 14.8         24.92 ~ 1 0
47 [C2011] J160912.32-390209.7 NIR 16 09 12.32 -39 02 09.7         24.66 ~ 1 0
48 HH 78 HH 16 09 12.8 -39 05 02           ~ 16 0
49 [C2011] J160913.03-390152.6 NIR 16 09 13.03 -39 01 52.6         24.55 ~ 1 0
50 2MASS J16091644-3904438 Y*O 16 09 16.447 -39 04 43.81           ~ 9 0
51 IRAS 16059-3857 Y*O 16 09 18.07 -39 04 53.4           ~ 40 0
52 2MASS J16092032-3904015 Y*O 16 09 20.328 -39 04 01.53           ~ 9 0
53 Lupus 3 SFR 16 09.6 -39 03           ~ 305 0
54 NAME Upper Sco Association As* 16 12 -23.4           ~ 1205 1
55 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3373 1

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2022.08.08-16:06:28

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