2009A&A...506.1183B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST21:28:10

2009A&A...506.1183B - Astronomy and Astrophysics, volume 506, 1183-1198 (2009/11-2)

Low-mass protostars and dense cores in different evolutionary stages in IRAS 00213+6530.

BUSQUET G., PALAU A., ESTALELLA R., GIRART J.M., ANGLADA G. and SEPULVEDA I.

Abstract (from CDS):

The aim of this paper is to study with high angular resolution a dense core associated with a low-luminosity IRAS source, IRAS00213+6530, in order to investigate whether low mass star formation is taking place in isolation.We carried out observations at 1.2mm with the IRAM30m telescope, and VLA observations in the continuum mode at 6cm, 3.6cm, 1.3cm and 7mm, together with H2O maser and NH3 lines toward IRAS00213+6530. Additionally, we observed the CCS JN=21-10 transition, and H2O maser emission using the NASA 70m antenna at Robledo de Chavela, Spain. We studied the nature of the centimeter and millimeter emission of the young stellar objects (YSOs) found in the region, and the physical properties of the dense gas and dust emission.The centimeter and millimeter continuum emission, together with the near infrared data from 2MASS allowed us to identify three YSOs, IRS 1, VLA 8A, and VLA 8B, with different radio and infrared properties, and which seem to be in different evolutionary stages. IRS 1, detected only in the infrared, is in the more advanced stage. On the other hand, VLA 8A, bright at centimeter and millimeter wavelengths, coincides with a near infrared 2MASS source, whereas VLA 8B has no infrared emission associated with it and is in the earliest evolutionary stage. The overall structure of the NH3 emission consists of three clouds. Two of these, MM1 and MM2, are associated with dust emission at millimeter wavelengths, while the southern cloud is only detected in NH3. The YSOs are embedded in MM1, where we found evidence of line broadening and temperature enhancements. On the other hand, the southern cloud and MM2 appear to be quiescent and starless. Concerning the 1.2mm dust emission, we modeled the radial intensity profile of MM1. The model fits the data reasonably well, but it underestimates the intensity at small projected distances from the 1.2mm peak, probably due to the presence of multiple YSOs embedded in the dusty envelope. There is a strong differentiation in the relative NH3 abundance with low values of ∼2x10–8 toward MM1, which harbors the YSOs, and high values, up to 10–6, toward the southern cloud and MM2, suggesting that these clouds could be in a young evolutionary stage.IRAS00213+6530 harbors a multiple system of low-mass protostars, indicating that star formation in this cloud is taking place in groups or clusters, rather than in isolation. The low-mass YSOs found in IRAS00213+6530 are in different evolutionary stages, suggesting that star formation takes place in different episodes.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: individual objects: IRAS 00213+6530 - ISM: clouds

Nomenclature: Table 2: [BPE2009] MMN (Nos MM1-MM2). Table 3: [BPE2009] VLA NN (Nos VLA 1-VLA 12). Table 5: [BPE2009] VLA NA (Nos VLA 8A-VLA 8B). Table 6: [BPE2009] IRS 1, [BPE2009] SC.

Simbad objects: 39

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Number of rows : 39

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 NGC 7822 HII 00 01 08.58 +67 25 17.0           ~ 112 3
2 Ass Cep OB 4 As* 00 02 +67.7           ~ 67 1
3 4C 60.01 Rad 00 14 48.79215207 +61 17 43.5420962           ~ 24 1
4 QSO B0016+73 QSO 00 19 45.7863740 +73 27 30.017554     19.0 18.26   ~ 273 1
5 [BPE2009] VLA 1 ? 00 23 21.01 +65 43 46.5           ~ 1 0
6 [BPE2009] VLA 2 ? 00 23 45.65 +65 48 36.1           ~ 1 0
7 [BPE2009] VLA 3 ? 00 23 46.41 +65 49 12.7           ~ 1 0
8 [BPE2009] VLA 4 ? 00 23 49.01 +65 46 14.7           ~ 1 0
9 [BPE2009] VLA 5 ? 00 23 52.06 +65 39 58.9           ~ 1 0
10 [BPE2009] VLA 6 ? 00 23 53.70 +65 49 41.6           ~ 1 0
11 [BPE2009] MM2 ? 00 24 04.4 +65 48 12           ~ 1 0
12 [BPE2009] SC ? 00 24 05.30 +65 47 47.0           ~ 1 0
13 [BPE2009] VLA 7 ? 00 24 09.11 +65 46 58.0           ~ 1 0
14 MSX6C G120.1368+03.0617 IR 00 24 09.9 +65 47 07           ~ 1 0
15 2MASS J00241010+6547091 Y*O 00 24 10.102 +65 47 09.12           ~ 1 0
16 IRAS 00213+6530 IR 00 24 10.4 +65 47 01           ~ 16 0
17 [BPE2009] MM1 ? 00 24 10.7 +65 47 09           ~ 1 0
18 [BPE2009] VLA 8A Y*O 00 24 11.01 +65 47 09.9           ~ 1 0
19 2MASS J00241110+6547095 IR 00 24 11.108 +65 47 09.53           ~ 1 0
20 [BPE2009] VLA 8B Y*O 00 24 11.76 +65 47 09.8           ~ 1 0
21 UCAC3 312-2163 * 00 24 12.5020889972 +65 46 41.778814396           ~ 1 0
22 [BPE2009] VLA 9 ? 00 24 24.46 +65 49 05.9           ~ 1 0
23 IRAS 00217+6533 mul 00 24 34.3 +65 49 38           ~ 4 0
24 [BPE2009] VLA 10 ? 00 24 36.71 +65 48 27.5           ~ 1 0
25 [BPE2009] VLA 11 ? 00 24 56.70 +65 49 10.3           ~ 1 0
26 [BPE2009] VLA 12 ? 00 25 24.75 +65 45 48.3           ~ 1 0
27 3C 48 QSO 01 37 41.2995845985 +33 09 35.079126038   16.62 16.20     ~ 2495 2
28 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3544 3
29 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1061 0
30 NAME [BM89] L1498 PoC 04 10 51.4 +25 09 58           ~ 187 0
31 LDN 1498 DNe 04 11.0 +24 58           ~ 247 0
32 LDN 1551 DNe 04 31 30.0 +18 12 30           ~ 768 1
33 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
34 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1359 0
35 LDN 1512 MoC 05 04 09.7 +32 43 09           ~ 160 0
36 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3715 1
37 LDN 183 MoC 15 54 12.2 -02 49 42           ~ 682 1
38 GAL 120.1+03.0 MoC 22 52 +55.0           ~ 3 0
39 NGC 7538 OpC 23 13 37 +61 30.0           ~ 827 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-21:28:10

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