2018A&A...617A..27P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST02:42:12

2018A&A...617A..27P - Astronomy and Astrophysics, volume 617A, 27-27 (2018/9-1)

Kinematics of dense gas in the L1495 filament.

PUNANOVA A., CASELLI P., PINEDA J.E., PON A., TAFALLA M., HACAR A. and BIZZOCCHI L.

Abstract (from CDS):


Context. Nitrogen bearing species, such as NH3, N2H+, and their deuterated isotopologues show enhanced abundances in CO-depleted gas, and thus are perfect tracers of dense and cold gas in star-forming regions. The Taurus molecular cloud contains the long L1495 filament providing an excellent opportunity to study the process of star formation in filamentary environments.
Aims. We study the kinematics of the dense gas of starless and protostellar cores traced by the N2D+(2-1), N2H+(1-0), DCO+(2-1), and H13CO+(1-0) transitions along the L1495 filament and the kinematic links between the cores and surrounding molecular cloud.
Methods. We measured velocity dispersions, local and total velocity gradients, and estimate the specific angular momenta of 13 dense cores in the four transitions using on-the-fly observations with the IRAM 30-m antenna. To study a possible connection to the filament gas, we used the C18O(1-0) observations.
Results. The velocity dispersions of all studied cores are mostly subsonic in all four transitions and are similar and almost constant dispersion across the cores in N2D+(2-1) and N2H+(1-0). A small fraction of the DCO+(2-1) and H13CO+(1-0) lines show transonic dispersion and exhibit a general increase in velocity dispersion with line intensity. All cores have velocity gradients (0.6-6.1km/s/pc), typical of dense cores in low-mass star-forming regions. All cores show similar velocity patterns in the different transitions, simple in isolated starless cores, and complex in protostellar cores and starless cores close to young stellar objects where gas motions can be affected by outflows. The large-scale velocity field traced by C18O(1-0) does not show any perturbation due to protostellar feedback and does not mimic the local variations seen in the other four tracers. Specific angular momentum J/M varies in a range (0.6-21.0)x1020cm2/s, which is similar to the results previously obtained for dense cores. The J/M measured in N2D+(2-1) is systematically lower than J/M measured in DCO+(2-1) and H13CO+(1-0).
Conclusions. All cores show similar properties along the 10pc-long filament. N2D+(2-1) shows the most centrally concentrated structure, followed by N2H+(1-0) and DCO+(2-1), which show similar spatial extent, and H13CO+(1-0). The non-thermal contribution to the velocity dispersion increases from higher to lower density tracers. The change of magnitude and direction of the total velocity gradients depending on the tracer used indicates that internal motions change at different depths within the cloud. N2D+ and N2H+ show smaller gradients than the lower density tracers DCO+ and H13CO+, implying a loss of specific angular momentum at small scales. At the level of cloud-core transition, the core's external envelope traced by DCO+ and H13CO+ is spinning up, which is consistent with conservation of angular momentum during core contraction. C18O traces the more extended cloud material whose kinematics is not affected by the presence of dense cores. The decrease in specific angular momentum towards the centres of the cores shows the importance of local magnetic fields to the small-scale dynamics of the cores. The random distributions of angles between the total velocity gradient and large-scale magnetic field suggests that magnetic fields may become important only in high density gas within dense cores.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: formation - ISM: kinematics and dynamics - ISM: clouds - ISM: molecules - ISM: individual objects: L1495 - radio lines: ISM

VizieR on-line data: <Available at CDS (J/A+A/617/A27): list.dat fits/*>

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 - 2020
#notes
1 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3544 3
2 [DB2002b] G168.46-15.58 DNe 04 17.4 +28 33           ~ 9 0
3 Barnard 211 DNe 04 17 35 +27 43.1           ~ 91 0
4 HGBS J041750.3+275604 cor 04 17 50.6 +27 56 01           ~ 5 0
5 [HTK2013] 3 cor 04 17 56.0 +28 12 23           ~ 2 0
6 [HTK2013] 4 cor 04 18 04.0 +28 08 14           ~ 2 0
7 LDN 1495 DNe 04 18.1 +27 37           ~ 289 1
8 HGBS J041807.8+280506 cor 04 18 08.4 +28 05 12           ~ 6 0
9 [HTK2013] 7 cor 04 18 11.5 +27 35 15           ~ 4 0
10 3C 111 Sy1 04 18 21.2773655604 +38 01 35.801523843   19.75 18.05     ~ 856 1
11 [OMK2002] 11 MoC 04 18 34.4 +28 26 12           ~ 3 0
12 [DB2002b] G168.87-15.58 DNe 04 18.7 +28 16           ~ 17 0
13 HGBS J041937.7+271526 cor 04 19 37.6 +27 15 31           ~ 10 0
14 [OMK2002] 13b MoC 04 19 42.4 +27 13 24           ~ 3 0
15 IRAS 04166+2706 Y*O 04 19 42.62736 +27 13 38.4312           ~ 111 0
16 HGBS J041951.2+271138 cor 04 19 51.7 +27 11 33           ~ 4 0
17 [OMK2002] 14 MoC 04 19 57.8 +27 10 10           ~ 3 0
18 Barnard 213 DNe 04 20 51 +27 16.3           ~ 153 0
19 [HTK2013] 16 cor 04 21 21.0 +27 00 09           ~ 2 0
20 Barnard 216 DNe 04 24.0 +26 37           ~ 43 0
21 Barnard 217 DNe 04 27 46.5 +26 17 52           ~ 86 0
22 [HTK2013] 17 cor 04 27 54.0 +26 17 50           ~ 2 0
23 Barnard 218 DNe 04 28.1 +26 16           ~ 30 0
24 [HTK2013] 19 cor 04 28 14.0 +26 20 34           ~ 2 0
25 LDN 1521F DNe 04 28 39.3 +26 51 43           ~ 183 1
26 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
27 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 680 0

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2020.07.04-02:42:12

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