2011A&A...526A..40C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST08:05:11

2011A&A...526A..40C - Astronomy and Astrophysics, volume 526A, 40-40 (2011/2-1)

Searching for jet rotation in class 0/I sources observed with GEMINI/GNIRS.

COFFEY D., BACCIOTTI F., CHRYSOSTOMOU A., NISINI B. and DAVIS C.

Abstract (from CDS):

In recent years, there has been a number of detections of gradients in the radial velocity profile across jets from young stars. The significance of these results is considerable. They may be interpreted as a signature of jet rotation about its symmetry axis, thereby representing the only existing observational indications supporting the theory that jets extract angular momentum from star-disk systems. However, the possibility that we are indeed observing jet rotation in pre-main sequence systems is undergoing active debate. To test the validity of a rotation argument, we must extend the survey to a larger sample, including younger sources. We present the latest results of a radial velocity analysis on jets from Class 0 and I sources, using high resolution data from the infrared spectrograph GNIRS on GEMINI South. We obtained infrared spectra of protostellar jets HH34, HH111-H, HH212 NK1 and SK1. The [Fe II] emission was unresolved in all cases and so Doppler shifts across the jet width could not be accessed. The H2 emission was resolved in all cases except HH34. Doppler profiles across the molecular emission were obtained, and gradients in radial velocity of typically 3km/s identified. Agreement with previous studies implies they may be interpreted as jet rotation, leading to toroidal velocity and angular momentum flux estimates of 1.5km/s and 1x10–5M/yr.AU.km/s respectively. However, caution is needed. For example, emission is asymmetric across the jets from HH212 suggesting a more complex interpretation is warranted. Furthermore, observations for HH212 and HH111-H are conducted far from the source implying external influences are more likely to confuse the intrinsic flow kinematics. These observations demonstrate the difficulty of conducting this study from the ground, and highlight the necessity for high angular resolution via adaptive optics or space-based facilities.

Abstract Copyright:

Journal keyword(s): ISM: jets and outflows - Herbig-Haro objects - ISM: individual objects: HH 111 - ISM: individual objects: HH 212 - ISM: individual objects: HH 34

Simbad objects: 19

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Number of rows : 19

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 2MASS J03290842+3115284 IR 03 29 08.420 +31 15 28.48           ~ 225 1
2 HH 211 cor 03 43 56.52 +32 00 52.8           ~ 293 0
3 V* CW Tau Or* 04 14 17.0041128798 +28 10 57.765657757 13.92 13.64 12.36 12.86   K0Ve 315 0
4 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 923 1
5 V* V1213 Tau Or* 04 31 37.47192 +18 12 24.4800           K7 516 0
6 LDN 1439 DNe 05 00 09 +52 04.9           ~ 77 0
7 V* RW Aur TT* 05 07 49.5662483 +30 24 05.177426   10.86 9.60 9.95   K1/5e+K5e 708 0
8 HH 34 HH 05 35 31.30 -06 28 43.0     16     ~ 469 2
9 [ZMR98] SK4 ? 05 43 51.07 -01 03 05.4           ~ 8 0
10 [ZMR98] SK2 ? 05 43 51.18 -01 03 01.8           ~ 9 0
11 [ZMR98] SK1 ? 05 43 51.28 -01 02 58.3           ~ 13 0
12 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 280 1
13 [ZMR98] NK1 ? 05 43 51.56 -01 02 48.2           ~ 9 0
14 HH 26 HH 05 46 05.1 -00 14 17           ~ 93 1
15 HH 111 HH 05 51 44.2 +02 48 34           ~ 385 0
16 HH 111H HH 05 51 44.2 +02 48 34           ~ 17 0
17 HH 121 HH 05 51 46.2 +02 48 32           ~ 36 0
18 Ced 96 Y*O 07 20 10.3 -24 02 24           ~ 29 1
19 WRAY 16-203 Or* 16 08 29.7086692265 -39 03 10.994386198   16.26 15.91 15.38 15.69 K0: 152 1

    Equat.    Gal    SGal    Ecl

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2020.07.13-08:05:11

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