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Applications of Precision Astrometry to Studies of Massive YSOs

Applications of Precision Astrometry to Studies of Massive YSOs. María José Rioja Luca Moscadelli Riccardo Cesaroni. +. 1- Epoch VLBA : Nov 21 1997. 3 - Epochs GLOBAL : Nov 9 , Nov 26 2000 and Mar 1 2001 8 EVN antennas : Eb , Mc , Nt , On , Jb , Mh , Sh , Ro VLBA : A ll.

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Applications of Precision Astrometry to Studies of Massive YSOs

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  1. Applications of PrecisionAstrometry to Studies of Massive YSOs MaríaJoséRioja LucaMoscadelli RiccardoCesaroni

  2. + 1-EpochVLBA : Nov211997 3-EpochsGLOBAL : Nov9, Nov 26 2000andMar1 20018EVNantennas : Eb, Mc, Nt, On, Jb, Mh, Sh, Ro VLBA : All Phase-referencingmodetoderiveabsolutemaserpositions 1-epochVLBAandmultiepochGLOBALobservations ofwatermaserstowardsIRAS20126+4104

  3. IRAS 20126+4104 Cesaroni et al.; Moscadelli,Cesaroni and Rioja M*=7 MO Mstar= 7 Msun ▵ (VLA) (VLA) (1-epoch VLBA)

  4. Conical Bipolar Model

  5. Best Fit Conical Outflow measured model Conevertexclosetocontinuum DRAv= 0.184arcsec DDECv= -0.132arcsec Wellcolllimated q(semi) = 17o Onthesky, parallleltopropermotions I-axis = 96o P-axis = 122o Highvelocityoutflow a (Hubble) = 250kms-1arcsec-1

  6. negative Z positive Z DEC offset (arcsec) RA offset (arcsec) Coneaxis

  7. GalacticMotion

  8. Encouraging results for IRAS20126+4104 Call for a larger number of observations of That kind of objects. 1st epoch EVN observations of a selection Of 5 high mass YSOs, in February 2004 9 antennas: Cm, Jb, Eb, Nt, On, Mh, Sh Aim: Asses the precise association of maser spots and molecular outflows Follow up with proper motion measurements.

  9. NGC281-W

  10. GGD12-15

  11. CONCLUSIONSANDFUTUREWORK •)The results obtained towards IRAS 20126+4104demonstrate that sensitive, multiepoch, phase-reference VLBI of water masers can unveil the gas kinematics near a high-mass YSO. •)Towards IRAS 20126+4104, water masers are clearly tracing a well collimated outflow, which remains similar, also in position angle, at a distance from the origin ranging from 0”.1 to 10”. •)We have extended the observations to a larger sample (5) of high-mass protostars in order to asses the association of the maser spots with the bipolar outflows and study the velocity field on scales of ca. 100 AU, in other sources. •)We plan to follow up the study of these new sources with proper motion measurements.

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