2019A&A...629A..10B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.15CEST08:35:17

2019A&A...629A..10B - Astronomy and Astrophysics, volume 629A, 10-10 (2019/9-1)

Fragmentation, rotation, and outflows in the high-mass star-forming region IRAS 23033+5951. A case study of the IRAM NOEMA large program CORE.

BOSCO F., BEUTHER H., AHMADI A., MOTTRAM J.C., KUIPER R., LINZ H., MAUD L., WINTERS J.M., HENNING T., FENG S., PETERS T., SEMENOV D., KLAASSEN P.D., SCHILKE P., URQUHART J.S., BELTRAN M.T., LUMSDEN S.L., LEURINI S., MOSCADELLI L., CESARONI R., SANCHEZ-MONGE A., PALAU A., PUDRITZ R., WYROWSKI F. and LONGMORE S.

Abstract (from CDS):


Context. The formation process of high-mass stars (>8M) is poorly constrained, particularly the effects of clump fragmentation creating multiple systems and the mechanism of mass accretion onto the cores.
Aims. We study the fragmentation of dense gas clumps, and trace the circumstellar rotation and outflows by analyzing observations of the high-mass (∼500M) star-forming region IRAS 23033+5951.
Methods. Using the Northern Extended Millimeter Array (NOEMA) in three configurations and the IRAM 30 m single-dish telescope at 220GHz, we probe the gas and dust emission at an angular resolution of ∼0.45'', corresponding to 1900 au.
Results. In the millimeter (mm) continuum emission, we identify a protostellar cluster with at least four mm-sources, where three of them show a significantly higher peak intensity well above a signal-to-noise ratio of 100. Hierarchical fragmentation from large to small spatial scales is discussed. Two fragments are embedded in rotating structures and drive molecular outflows, traced by 13CO (2-1) emission. The velocity profiles across two of the cores are similar to Keplerian but are missing the highest-velocity components close to the center of rotation, which is a common phenomena from observations like these, and other rotation scenarios are not excluded entirely. Position-velocity diagrams suggest protostellar masses of ∼6 and 19M. Rotational temperatures from fitting CH3CN (12K-11K) spectra are used for estimating the gas temperature and thereby also the disk stability against gravitational fragmentation, utilizing Toomre's Q parameter. Assuming that the candidate disk is in Keplerian rotation about the central stellar object and considering different disk inclination angles, we identify only one candidate disk as being unstable against gravitational instability caused by axisymmetric perturbations.
Conclusions. The dominant sources cover different evolutionary stages within the same maternal gas clump. The appearance of rotation and outflows of the cores are similar to those found in low-mass star-forming regions.

Abstract Copyright: © F. Bosco et al. 2019

Journal keyword(s): ISM: individual objects: IRAS 23033+5951 - ISM: kinematics and dynamics - ISM: jets and outflows - circumstellar matter - stars: formation - stars: massive

VizieR on-line data: <Available at CDS (J/A+A/629/A10): list.dat fits/*>

Status at CDS:   Examining the need for a new acronym.

Simbad objects: 22

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Number of rows : 22

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 6C 000852+702833 BLL 00 11 31.90287510 +70 45 31.6257033           ~ 10 1
2 ICRF J005952.2+581223 QSO 00 59 52.2083579204 +58 12 23.682108462           ~ 15 1
3 [KSP2003] J022531.18+620624.5 HII 02 25 31.18 +62 06 24.5           O8V-B0.5V 95 1
4 W 3(H2O) Mas 02 27 04.6 +61 52 25           ~ 123 0
5 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3545 3
6 EM* LkHA 101 Em* 04 30 14.438 +35 16 24.03   17.91 15.71 13.33   F 297 1
7 4C 09.57 BLL 17 51 32.81857318 +09 39 00.7284829   17.46 16.78 15.57   ~ 811 1
8 [DLW84] G35.2N HII 18 58 13.036 +01 40 36.00           ~ 91 0
9 ICRF J192748.4+735801 Sy1 19 27 48.4944745594 +73 58 01.571908984     15.5 15.11   ~ 491 2
10 RAFGL 2591 Y*O 20 29 25.03656 +40 11 20.3316           ~ 570 0
11 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 707 0
12 ICRF J220143.5+504856 QSO 22 01 43.5371323886 +50 48 56.391178986       18.8   ~ 49 3
13 ICRF J222318.0+624933 Bz? 22 23 18.09659524 +62 49 33.8054934           ~ 16 1
14 IRAS 23031+5948 * 23 05 15.8064542082 +60 05 08.626257807           ~ 3 0
15 [RM2008] IRAS 23033+5951-MMS2 mm 23 05 24.6 +60 08 08           ~ 3 0
16 [RTM2012b] VLA 1 Rad 23 05 24.967 +60 08 16.03           ~ 2 0
17 [RM2008] IRAS 23033+5951-MMS1 mm 23 05 25.0 +60 08 17           ~ 2 0
18 [RTM2012b] VLA 3 Rad 23 05 25.156 +60 08 15.74           ~ 2 0
19 IRAS 23033+5951 Y*O 23 05 25.16112 +60 08 15.4428           ~ 78 0
20 NGC 7538S Y*O 23 13 44.8 +61 26 51           ~ 73 1
21 [WBN74] NGC 7538 IRS 1 Y*O 23 13 45.318 +61 28 11.69           ~ 367 3
22 IRAS 23151+5912 HII 23 17 21.0 +59 28 49           ~ 93 0

    Equat.    Gal    SGal    Ecl

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2020.07.15-08:35:17

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