2020A&A...633A.128F


Query : 2020A&A...633A.128F

2020A&A...633A.128F - Astronomy and Astrophysics, volume 633A, 128-128 (2020/1-1)

Mirror, mirror on the outflow cavity wall. Near-infrared CO overtone disc emission of the high-mass YSO IRAS 11101-5829.

FEDRIANI R., CARATTI O GARATTI A., KOUTOULAKI M., GARCIA-LOPEZ R., NATTA A., CESARONI R., OUDMAIJER R., COFFEY D., RAY T. and STECKLUM B.

Abstract (from CDS):


Aims. The inner regions of high-mass protostars are often invisible in the near-infrared, obscured by thick envelopes and discs. We aim to investigate the inner gaseous disc of IRAS 11101-5829 through scattered light from the outflow cavity walls.
Methods. We observed the immediate environment of the high-mass young stellar object IRAS 11101-5829 and the closest knots of its jet, HH135-136, with the integral field unit VLT/SINFONI. We also retrieved archival data from the high-resolution long-slit spectrograph VLT/X-shooter. We analysed imaging and spectroscopic observations to discern the nature of the near-infrared CO emission.
Results. We detect the first three bandheads of the υ=2-0 CO vibrational emission for the first time in this object. It is coincident with continuum and Brγ emission and extends up to ∼10000au to the north-east and ∼10000au to the south-west. The line profiles have been modelled as a Keplerian rotating disc assuming a single ring in local thermodynamic equilibrium. The model output gives a temperature of ∼3000K, a CO column density of ∼1x1022cm–2, and a projected Keplerian velocity vKsini–disc∼25km/s, which is consistent with previous modelling in other high-mass protostars. In particular, the low value of vK sin idisc suggests that the disc is observed almost face-on, whereas the well-constrained geometry of the jet imposes that the disc must be close to edge-on. This apparent discrepancy is interpreted as the CO seen reflected in the mirror of the outflow cavity wall.
Conclusions. From both jet geometry and disc modelling, we conclude that all the CO emission is seen through reflection by the cavity walls and not directly. This result implies that in the case of highly embedded objects, as for many high-mass protostars, line profile modelling alone might be deceptive and the observed emission could affect the derived physical and geometrical properties; in particular the inclination of the system can be incorrectly interpreted.

Abstract Copyright: © ESO 2020

Journal keyword(s): accretion, accretion disks - ISM: jets and outflows - stars: protostars - stars: massive - stars: individual: IRAS 11101-5829 - ISM: individual objects: HH 135-HH 136

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 V* V1213 Tau Or* 04 31 37.5055489536 +18 12 24.383952396           K7 546 0
2 HH 111 HH 05 51 44.2 +02 48 34           ~ 399 0
3 HD 94108 * 10 50 49.7544144216 -52 28 17.020792020   7.65 7.77     B4V 15 0
4 HH 135 HH 11 12 16.462 -58 46 34.33           ~ 16 0
5 2MASS J11121780-5846425 * 11 12 17.8125412920 -58 46 42.591282024           ~ 1 0
6 NAME HH 135-136 HH 11 12 18 -56 46.3           ~ 9 0
7 IRAS 11101-5829 Y*O 11 12 18.19248 -58 46 20.8452           ~ 30 0
8 Gaia DR3 5339406246100053888 * 11 12 18.2431814736 -58 46 22.525444704           ~ 1 0
9 HH 136 HH 11 12 19.6 -58 46 04           ~ 16 0
10 Cl Stock 13 OpC 11 13 05 -58 53.0           ~ 46 0
11 HD 104839 * 12 04 16.7047787736 -51 28 21.055598472   6.43 6.47     B9.5V 29 0
12 W 33a Y*O 18 14 39.0 -17 52 03           ~ 618 0

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2022.11.28-12:13:56

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