2019A&A...621A.140J


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.20CEST20:47:50

2019A&A...621A.140J - Astronomy and Astrophysics, volume 621A, 140-140 (2019/1-1)

Extreme fragmentation and complex kinematics at the center of the L1287 cloud.

JUAREZ C., LIU H.B., GIRART J.M., PALAU A., BUSQUET G., GALVAN-MADRID R., HIRANO N. and LIN Y.

Abstract (from CDS):


Aims. The filamentary ∼10-pc-scale infrared dark cloud L1287 located at a parallax distance of ∼929pc is actively forming a dense cluster of low-mass young stellar objects (YSOs) at its inner ∼0.1pc region. To help understand the origin of this low-mass YSO cluster, the present work aims at resolving the gas structures and kinematics with high angular resolution.
Methods. We performed ∼1" angular resolution (∼930 AU) observations at ∼1.3mm wavelengths using the Submillimeter Array (SMA), which simultaneously cover the dust continuum emission and various molecular line tracers for dense gas, warm gas, shocks, and outflows.
Results. From a 1.3-mm continuum image with a resolution of ∼2" we identified six dense cores, namely SMA1-6. Their gas masses are in the range of ∼0.4-4M. From a 1.3-mm continuum image with a resolution of ∼1", we find a high fragmentation level, with 14 compact millimeter sources within 0.1pc: SMA3 contains at least nine internal condensations; SMA5 and SMA6 are also resolved with two internal condensations. Intriguingly, one condensation in SMA3 and another in SMA5 appear associated with the known accretion outburst YSOs RNO 1C and RNO 1B. The dense gas tracer DCN (3-2) well traces the dust continuum emission and shows a clear velocity gradient along the NW-SE direction centered at SMA3. There is another velocity gradient with opposite direction around the most luminous YSO, IRAS 00338 + 6312.
Conclusions. The fragmentation within 0.1pc in L1287 is very high compared to other regions at the same spatial scales. The incoherent motions of dense gas flows are sometimes interpreted by being influenced by (proto)stellar feedback (e.g., outflows), which is not yet ruled out in this particular target source. On the other hand, the velocities (with respect to the systemic velocity) traced by DCN are small, and the directions of the velocity gradients traced by DCN are approximately perpendicular to those of the dominant CO outflow(s). Therefore, we alternatively hypothesize that the velocity gradients revealed by DCN trace the convergence from the ≥0.1pc scales infalling motion towards the rotational motions around the more compact (∼0.02pc) sources. This global molecular gas converging flow may feed the formation of the dense low-mass YSO cluster. Finally, we also found that IRAS 00338 + 6312 is the most likely powering source of the dominant CO outflow. A compact blue-shifted outflow from RNO 1C is also identified.

Abstract Copyright: © ESO 2019

Journal keyword(s): stars: formation - ISM: individual objects: L1287 - ISM: molecules

Nomenclature: Fig. 2, Table 2: [JLG2019] SMANa (Nos SMA1-SMA6, SMA3a-SMA3i, SMA5a-SMA5b, SMA6a-SMA6b).

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 - 2019
#notes
1 [JLG2019] SMA3e mm 00 36 46.1980 +63 28 56.829           ~ 1 0
2 [JLG2019] SMA5b mm 00 36 46.2550 +63 28 52.307           ~ 1 0
3 V* V710 Cas FU* 00 36 46.30 +63 28 54.1           F8II 81 0
4 [JLG2019] SMA3h mm 00 36 46.3300 +63 28 54.583           ~ 1 0
5 [JLG2019] SMA3f mm 00 36 46.3480 +63 28 55.930           ~ 1 0
6 [JLG2019] SMA3d mm 00 36 46.3870 +63 28 57.326           ~ 1 0
7 [JLG2019] SMA3g mm 00 36 46.4500 +63 28 54.966           ~ 1 0
8 [JLG2019] SMA6a mm 00 36 46.5840 +63 28 49.613           ~ 1 0
9 2MASS J00364659+6328574 FU* 00 36 46.6020931957 +63 28 57.617542780           ~ 48 0
10 [JLG2019] SMA3i mm 00 36 46.6060 +63 28 54.248           ~ 1 0
11 [ARG94] VLA 1 Rad 00 36 46.7610 +63 28 57.583           ~ 3 0
12 [JLG2019] SMA3a mm 00 36 46.8600 +63 28 59.414           ~ 1 0
13 [JLG2019] SMA6b mm 00 36 46.9360 +63 28 47.078           ~ 1 0
14 [ARG94] VLA 2 Rad 00 36 47.09 +63 28 50.5           ~ 3 0
15 JCMTSE J003646.4+632902 Rad 00 36 47.3660 +63 29 02.237           ~ 12 0
16 [ARG94] VLA 4 Rad 00 36 47.39 +63 28 53.7           ~ 5 0
17 LDN 1287 DNe 00 36 47.5 +63 29 02           ~ 82 0
18 GM 1-33 HH 00 36 47.5 +63 29 02           ~ 110 0
19 7C 0059+5808 QSO 01 02 45.76238248 +58 24 11.1366009   20.09 19.22 18.57 17.90 ~ 179 1
20 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3460 3
21 HH 2 HH 05 36.4 -06 47           ~ 335 1
22 V* FU Ori FU* 05 45 22.3650208559 +09 04 12.296285806   10.72 9.60     F0Iab 685 1
23 NAME NGC 6334 FIR V Cl* 17 19 57 -35 57.5           ~ 81 0
24 W 31c HII 18 10 29.1 -19 56 05           ~ 298 0
25 [WWB83] G033.91+0.11 HII 18 52 50.4 +00 55 29           ~ 85 1
26 W 49a SFR 19 10 15.7 +09 06 05           ~ 255 2
27 3C 454.3 QSO 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2439 2

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2019.10.20-20:47:50

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