2022MNRAS.514.6038Z

Query : 2022MNRAS.514.6038Z

2022MNRAS.514.6038Z - Mon. Not. R. Astron. Soc., 514, 6038-6052 (2022/August-3)

ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - XI. From inflow to infall in hub-filament systems.

ZHOU J.-W., LIU T., EVANS II N.J., GARAY G., GOLDSMITH P.F., GOMEZ G.C., VAZQUEZ-SEMADENI E., LIU H.-L., STUTZ A.M., WANG K., JUVELA M., HE J., LI D., BRONFMAN L., LIU X., XU F.-W., TEJ A., DEWANGAN L.K., LI S., ZHANG S., ZHANG C., REN Z., TATEMATSU K., SHING LI P., WON LEE C., BAUG T., QIN S.-L., WU Y., PENG Y., ZHANG Y., LIU R., LUO Q.-Y., GE J., SAHA A., CHAKALI E., ZHANG Q., KIM K.-T., RISTORCELLI I., SHEN Z.-Q. and LI J.-Z.

Abstract (from CDS):

We investigate the presence of hub-filament systems in a large sample of 146 active proto-clusters, using H¹³CO⁺ J = 1-0 molecular line data obtained from the ATOMS survey. We find that filaments are ubiquitous in proto-clusters, and hub-filament systems are very common from dense core scales (∼0.1 pc) to clump/cloud scales (∼1-10 pc). The proportion of proto-clusters containing hub-filament systems decreases with increasing dust temperature (T_d) and luminosity-to-mass ratios (L/M) of clumps, indicating that stellar feedback from H II regions gradually destroys the hub-filament systems as proto-clusters evolve. Clear velocity gradients are seen along the longest filaments with a mean velocity gradient of 8.71 km s^–1 pc^–1 and a median velocity gradient of 5.54 km s^–1 pc^–1. We find that velocity gradients are small for filament lengths larger than ∼1 pc, probably hinting at the existence of inertial inflows, although we cannot determine whether the latter are driven by large-scale turbulence or large-scale gravitational contraction. In contrast, velocity gradients below ∼1 pc dramatically increase as filament lengths decrease, indicating that the gravity of the hubs or cores starts to dominate gas infall at small scales. We suggest that self-similar hub-filament systems and filamentary accretion at all scales may play a key role in high-mass star formation.

Journal keyword(s): ISM: clouds - ISM: H ii regions - ISM: kinematics and dynamics - stars: formation - stars: protostars

Simbad objects: 1

Full paper

View the references in ADS

Number of rows : 1

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Mag I	Sp type	#ref 1850 - 2026	#notes
1	[DBS2003] 127	cor	10 38 33	-58 19.3						~	39	0

Query : 2022MNRAS.514.6038Z

Basic data :

[DBS2003] 127 -- Dense Core
Other object types:	`Cl* ([DBS2003])`, `cor (2011ApJS)`, `MoC ([BYF2011])`
ICRS coord. (ep=J2000) :	`10 38 32.8 -58 19 19 (mm) [ ] D 2011ApJS..196...12B`
FK4 coord. (ep=B1950 eq=1950) :	`10 36 37.0 -58 03 41 [ ]`
Gal coord. (ep=J2000) :	`286.2100 +00.1680 [ ]`
VLSR :	`-19.80 -20.805 -18.795 [0.16] (mm)` `2016ApJ...831...67B`
Angular size (arcmin):	`2.60 1.72 140 (mm) D` `2011ApJS..196...12B`

Overlay

points in this preview

2MASS DSS

All

(CDSPortal)

Send to

Hierarchy : number of linked objects
whatever the membership probability is (see description here ) :

An access of full data is available using the icon Vizier near the identifier of the catalogue

GAL 286.21+00.17 [BYF2011] 73 [DBS2003] 127

References (39 between 1850 and 2026) (Total 39)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).

Follow new references on this object

Annotations :
Annotations allow a user to add a note or report an error concerning the astronomical object and its data. It requires registration to post a note. See description .
Please, have a look at Best practices. The list of all annotations to SIMBAD objects can be found here .

The annotation server is currently not available. Sorry for any inconvenience

To bookmark this query, right click on this link: simbad:objects in 2022MNRAS.514.6038Z and select 'bookmark this link' or equivalent in the popup menu