2019A&A...631A...3M


C.D.S. - SIMBAD4 rel 1.7 - 2020.02.25CET11:27:14

2019A&A...631A...3M - Astronomy and Astrophysics, volume 631A, 3-3 (2019/11-1)

Multi-scale analysis of the Monoceros OB 1 star-forming region. II. Colliding filaments in the Monoceros OB1 molecular cloud.

MONTILLAUD J., JUVELA M., VASTEL C., HE J., LIU T., RISTORCELLI I., EDEN D.J., KANG S.-J., KIM K.-T., KOCH P.M., LEE C.W., RAWLINGS M.G., SAAJASTO M., SANHUEZA P., SOAM A., ZAHORECZ S., ALINA D., BOGNER R., CORNU D., DOI Y., MALINEN J., MARSHALL D.J., MICELOTTA E.R., PELKONEN V.-M., TOTH L.V., TRAFICANTE A. and WANG K.

Abstract (from CDS):


Context. We started a multi-scale analysis of star formation in G202.3+2.5, an intertwined filamentary sub-region of the Monoceros OB1 molecular complex, in order to provide observational constraints on current theories and models that attempt to explain star formation globally. In the first paper (Paper I, Montillaud et al. 2019A&A...631L...1M), we examined the distributions of dense cores and protostars and found enhanced star formation activity in the junction region of the filaments.
Aims. In this second paper, we aim to unveil the connections between the core and filament evolutions, and between the filament dynamics and the global evolution of the cloud.
Methods. We characterise the gas dynamics and energy balance in different parts of G202.3+2.5 using infrared observations from the Herschel and WISE telescopes and molecular tracers observed with the IRAM 30-m and TRAO 14-m telescopes. The velocity field of the cloud is examined and velocity-coherent structures are identified, characterised, and put in perspective with the cloud environment.
Results. Two main velocity components are revealed, well separated in radial velocities in the north and merged around the location of intense N2H+ emission in the centre of G202.3+2.5 where Paper I found the peak of star formation activity. We show that the relative position of the two components along the sightline, and the velocity gradient of the N2H+ emission imply that the components have been undergoing collision for ∼105yr, although it remains unclear whether the gas moves mainly along or across the filament axes. The dense gas where N2H+ is detected is interpreted as the compressed region between the two filaments, which corresponds to a high mass inflow rate of ∼1x10–3M/yr and possibly leads to a significant increase in its star formation efficiency. We identify a protostellar source in the junction region that possibly powers two crossed intermittent outflows. We show that the HII region around the nearby cluster NCG 2264 is still expanding and its role in the collision is examined. However, we cannot rule out the idea that the collision arises mostly from the global collapse of the cloud.
Conclusions. The (sub-)filament-scale observables examined in this paper reveal a collision between G202.3+2.5 sub-structures and its probable role in feeding the cores in the junction region. To shed more light on this link between core and filament evolutions, one must characterise the cloud morphology, its fragmentation, and magnetic field, all at high resolution. We consider the role of the environment in this paper, but a larger-scale study of this region is now necessary to investigate the scenario of a global cloud collapse.

Abstract Copyright: © J. Montillaud et al. 2019

Journal keyword(s): ISM: clouds - stars: formation

VizieR on-line data: <Available at CDS (J/A+A/631/A3): list.dat fits/*>

Status in Simbad:  being processed

Simbad objects: 20

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Number of rows : 20

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 1333 SFR 03 28 55 +31 22.2   10.9       ~ 1200 1
2 NAME Mon I MoC 06 35 +10.1           ~ 206 0
3 HH 576 HH 06 40 35.9 +10 39 48           ~ 6 0
4 HH 577 HH 06 40 36.6 +10 34 02           ~ 6 0
5 IRAS 06381+1039 HII 06 40 58.0 +10 36 49           ~ 22 1
6 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1564 1
7 * 15 Mon Be* 06 40 58.65963 +09 53 44.7229 3.360 4.400 4.640   4.88 O7V+B1.5/2V 743 0
8 JCMTSF J064059.1+103608 smm 06 40 59.1 +10 36 09           ~ 5 0
9 [WMF2003] 27 S3 smm 06 41 02.0 +10 35 30           ~ 4 0
10 IRAS 06382+1017 Y*O 06 41 02.660 +10 15 01.91           ~ 49 0
11 HH 124 HH 06 41 02.68 +10 15 03.6           ~ 26 0
12 IRAS 06382+0939 Y*O 06 41 02.81160 +09 36 16.1712         19.89 ~ 74 0
13 NAME Mon OB1 H PoC 06 41 03 +10 37.0           ~ 14 1
14 NAME Cone Nebula DNe 06 41.1 +09 53           ~ 74 1
15 RAFGL 989 Y*O 06 41 10.1592954288 +09 29 33.635497596   17.4 16.8 18.26 17.28 B2 237 0
16 NAME Musca Cld 12 23 -71.3           ~ 155 0
17 [PFA2014] SDC13 DNe 18 14 29.7 -17 32 35           ~ 10 0
18 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 897 2
19 PGCC G026.53+00.71 MoC 18 37 10.159 -05 22 20.84           ~ 3 0
20 NAME Aql Region reg ~ ~           ~ 295 0

    Equat.    Gal    SGal    Ecl

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2020.02.25-11:27:14

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