2001A&A...366..873F


Query : 2001A&A...366..873F

2001A&A...366..873F - Astronomy and Astrophysics, volume 366, 873-890 (2001/2-2)

Disks and outflows around intermediate-mass stars and protostars.

FUENTE A., NERI R., MARTIN-PINTADO J., BACHILLER R., RODRIGUEZ-FRANCO A. and PALLA F.

Abstract (from CDS):

In order to study the existence and evolution of circumstellar disks around intermediate-mass stars (M*>3M), we have obtained single-dish and interferometric continuum images at 2.6mm and 1.3mm of the intermediate-mass protostar NGC 7129 FIRS 2 and of the Herbig Be stars LkHα 234 and HD 200775. These objects are representative of the different stages of the pre-main sequence evolution with ages ranging from a few 103 to 8 106 years. Single-dish and interferometric observations of the outflows associated with these sources are also presented. In NGC 7129 FIRS 2, two millimeter sources are required to fit the interferometric 1.3mm continuum emission. Only the most intense of these millimeter objects, FIRS 2 - MM1, seems to be associated with the CO outflow. The second and weaker source, FIRS 2 - MM2, does not present any sign of stellar activity. The single-dish map of the CO outflow presents an unusual morphology with the blue and red lobes separated by an angle of 82°. The CO J=1->0 interferometric image shows that this unusual morphology is the result of the superposition of two outflows, one of them associated with FIRS 2 - MM1 (the blue lobe in the single-dish map) and the other (the red lobe) with a new infrared source (FIRS 2 - IR) which is not detected in the millimeter continuum images. The interferometric 1.3mm continuum image of NGC 7129 FIRS 1 reveals that LkHα 234 is a member of a cluster of embedded objects. Two millimeter clumps are detected in this far-infrared source. The strongest is spatially coincident with the mid-infrared companion of LkH α 234, IRS 6. A new millimeter clump, FIRS 1 - MM1, is detected at an offset (-3.23'', 3.0'') from LkHα 234. We have not detected any compact source towards LkHα 234 with a limit for the mass of a circumstellar disk, MD<0.1M. The comparison of the interferometric CO J=1->0 and continuum images reveals that IRS 6 very likely drives the energetic molecular outflow detected towards NGC 7129 FIRS 1 and the [SII] jet. The extremely young object FIRS 1 - MM1 (it has not been detected in the near-and mid-infrared) turns out to be the driving source of the H2 jet. There is no evidence for the existence of a bipolar outflow associated with LkHα 234. We have not detected 1.3mm continuum emission towards HD 200775. Our observations imply a 3-σ upper limit of < 0.002 M for the mass of a circumstellar disk. This is the lowest upper limit obtained so far in a Herbig Be star. Thus our observations provide new important information on three protostars (IRS 6, FIRS 1 - MM1 and FIRS 2 - MM1), one infrared star (FIRS 2 - IR) and two Herbig Be stars. The luminosities of the protostars are consistent with being intermediate-mass objects (M*∼3.5-4.5M). They are surrounded by thick envelopes with masses ranging between ∼2-3.5 M and drive energetic outflows. Circumstellar disks and bipolar outflows are not detected toward the Herbig Be stars. We have obtained an upper limit for the disk/stellar mass ratio, MD/M*, of<0.02 in LkHα 234 and of <0.0002 in HD 200775. Our limit in HD 200775 implies that in evolved Herbig Be stars the MD/M* ratio is more than two orders of magnitude lower than in T Tauri and Herbig Ae stars. We propose that in massive stars (M*≥5M) both the dispersal of the outer disk and the energetic mass-loss, occur early in the stellar evolution before the star becomes visible. Some mechanisms for the dispersal of the outer disk are discussed.

Abstract Copyright:

Journal keyword(s): stars: formation - fundamental parameters - pre-main sequence - ISM: abundances - clouds - molecules

Nomenclature: Table 1, Fig.1: [FNM2001] NGC 7129 MM N (Nos 1-5). Table 2, Figs 2, 6: [FNM2001] NGC 7129 FIRS 1 MM N (No. 1), [FNM2001] NGC 7129 FIRS 2 MM N (Nos 1-2), [FNM2001] NGC 7129 FIRS 2 IR N=1.

Simbad objects: 27

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Number of rows : 27
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 261 2
2 4C 73.18 BLL 19 27 48.4947009120 +73 58 01.572558816     15.5 15.11   ~ 515 2
3 QSO B2015+657 QSO 20 15 55.36865773 +65 54 52.6588750   19.7 19.7 19.03   ~ 51 1
4 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 772 0
5 NGC 7023 RNe 21 01 36.9 +68 09 48           ~ 682 0
6 HD 200775 Ae* 21 01 36.9205762896 +68 09 47.789578836 7.34 7.754 7.427 8.13   B2Ve 539 0
7 HH 103 * 21 42 24.7 +66 03 40           ~ 34 0
8 GGD 32 * 21 42 26.88 +66 04 27.9           ~ 26 0
9 [FNM2001] NGC 7129 MM 3 mm 21 42 38.1 +66 06 50           ~ 1 0
10 BD+65 1637 Ae* 21 42 50.1798725784 +66 06 35.186616864 10.21 10.56 10.53 10.29   B3IV-Vne 153 1
11 NGC 7129 OpC 21 42 58 +66 06.8     11.5     ~ 255 0
12 V* V392 Cep Or* 21 42 57.7396395240 +66 04 23.514247020       19.08 18.00 ~ 27 0
13 RNO 138 RNe 21 42 57.810 +66 04 23.07           ~ 27 0
14 [FNM2001] NGC 7129 MM 1 mm 21 42 57.9 +66 05 21           ~ 3 0
15 BD+65 1638 Y*O 21 42 58.5801989808 +66 06 10.505819988   10.63 10.42 10.09   B3V 30 0
16 [FNM2001] NGC 7129 MM 2 mm 21 42 58.7 +66 05 35           ~ 1 0
17 [FNM2001] NGC 7129 FIRS 2 MM 2 mm 21 43 01.6 +66 03 26           ~ 5 0
18 [FNM2001] NGC 7129 FIRS 2 MM 1 mm 21 43 01.7 +06 03 24           ~ 6 0
19 [FNM2001] NGC 7129 FIRS 2 IR mm 21 43 01.8 +66 03 27           ~ 5 0
20 [YIN2000] B214157.3+655309.6 mm 21 43 06.3 +66 06 57           ~ 13 0
21 [WKM94] IRS 6 IR 21 43 06.5 +66 06 55           ~ 14 0
22 EM* LkHA 234 Ae* 21 43 06.8218113480 +66 06 54.202272804 13.65 13.61 12.73 11.98 11.20 B5Ve 283 0
23 HH 105 HH 21 43 22.09 +66 07 47.3           ~ 19 0
24 JCMTSF J214327.2+660326 mm 21 43 26.3 +66 03 25           ~ 2 0
25 GGD 34 HH 21 43 30.4 +66 03 43           ~ 32 0
26 HH 235 HH 21 43.7 +66 09           ~ 32 0
27 NAME NGC 7129 FIR 2 IR 21 44 01.5 +66 03 40           ~ 94 0

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2023.02.04-10:56:08

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