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A YOUNG STELLAR CLUSTER TOWARDS IRAS 06361-0142

A YOUNG STELLAR CLUSTER TOWARDS IRAS 06361-0142. My first Star Formation case. Ana López Sepulcre. 1. Introduction: How I started 2. IRAS 06361-0142 Observations and data reduction Results Summary 3. Other tasks at the University of Barcelona. Francesca Figueras.

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A YOUNG STELLAR CLUSTER TOWARDS IRAS 06361-0142

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  1. A YOUNG STELLAR CLUSTER TOWARDS IRAS 06361-0142 My first Star Formation case Ana López Sepulcre

  2. 1. Introduction: How I started 2. IRAS 06361-0142 Observations and data reduction Results Summary 3. Other tasks at the University of Barcelona

  3. Francesca Figueras José María Torrelles João Lin Yun 1. Introduction: How I started 1. Introduction: How I started Collaboration Grant for last year undergraduate students (Beca de col·laboració amb departaments) João’s project: Study of several star formation sites located far from the Galactic centre (3rd Galactic quadrant). Particular case: IRAS 06361-0142 Yun, J.L., López-Sepulcre, A, Torrelles, J.M. 2007 A&A A new young stellar cluster embedded in a molecular cloud in the far outer Galaxy

  4. Observations and data reduction • Near-IR: J,H and Ks observations with ESO Antu telescope + ISAAC camera, 2000 November 10. • For each band, 15 images with 4 s exposure time at each of 6 different jitter positions were taken. • (a) Image reduction performed with IRAF, resulting in a final mosaic image for each band: CLEANi = (RAWi – SKYi) / FLAT i = 1,...,6 Combination of all i: MOSAIC image 2. IRAS 06361-0142. Observations and data reduction 2. IRAS 06361-0142

  5. Calibration with 2MASS stars within field Aperture photometry List of sources 2. IRAS 06361-0142. Observations and data reduction (b) Photometry with IRAF for each band: - CO(1-0) line observations using the 15m Swedish-ESO Submillimetre Telescope (SEST) in Chile, 1999 September. • VLA 6 cm continuum maps obtained from VLA Archive data. Observed on 2005 May 8 in VLA’s B configuration. • Image reduction and calibration was carried out with AIPS.

  6. Line centred at a LSR velocity of ~53 km/s Kinematic distance to the cloud: 7 kpc Galactocentric distance: 15 kpc 2. IRAS 06361-0142. Results Results CO(1-0) spectrum:Molecular gas towards IRAS 06361-0142 Resolution: 0.22 km/s

  7. Near-IR images towards IRAS 06361-0142 J H K 2. IRAS 06361-0142. Results Yun, J.L. et al (2007)

  8. The “cluster region”: central region about 36” on each side (R.A. and dec)  1.2 x 1.2 pc2 at 7 kpc. The reddening effect at the cluster region separates foreground from embedded stars Membership: A star which is within the “cluster region” and has (H-Ks) > 0.65 is considered to be a cluster member. 2. IRAS 06361-0142. Results Observed (H-Ks) as a function of R.A. offset (Yun, J.L. et al, 2007)

  9. Inner-disk frequencies in young clusters vs age Haisch, K.E. et al, 2001 More than 50% of the cluster members have cleared their inner circumstellar disks responsible for (H-Ks) excess  Age > 3 Myr 2. IRAS 06361-0142. Results Colour-colour diagram Yun, J.L. et al, 2007

  10. 2. IRAS 06361-0142. Results Colour-magnitude diagram Isochrone fitting: Isochrones computed by Siess, Dufour & Forestini (2000) for stars between 0.1 and 7Msun Possible fit to age: 4 Myr, with variable extinction between AV = 6 and AV = 13 within the cloud Yun, J.L. et al, 2007

  11. rms = 140 μJy/beam Upper luminosity limit: L~5500Lsun for the individual members of the cluser (~12 Msun) 2. IRAS 06361-0142. Results Radio-continuum observations (6 cm) from VLA archive The source was not detected at this wavelength

  12. 2. IRAS 06361-0142. Summary Summary • New distant young stellar cluster embedded in a molecular cloud, seen towards IRAS 06361-0142. Distance: 7 kpc. Galactocentric distance: 15 kpc (in the far outer Galaxy). • Composed of several tens of low and intermediate-mass young reddened stars, surrounded by a spherical nebulosity. Approximate size of the region: 1.2 x 1.2 pc2. • Possible fit to the age of the cluster: 4 Myr, with variable extinction within the cloud between AV = 6 and AV = 13. • The outer Galactic disk is active in the formation of new stellar clusters; the star formation process is unaffected by the properties that distinguish the outer Galaxy from the inner Galaxy.

  13. 3. Other tasks at the University of Barcelona 3. Other tasks at the University of Barcelona Search for radio-continuum observations of the rest of Joao’s list of distant candidate forming regions (IRAS) in the VLA archive  reduction and calibration with AIPS. Part of the results of the reduction No centimetric emission found

  14. eVLA continuum observations toward IRAS 06468-0325 at 3.6 cm rms = 20 μJy/beam 3. Other tasks at the University of Barcelona A diamond ring! Yun et al. A “diamond-ring” star: the unusual morphology of a young (multiple?) object. 2007. The source was not detected at this wavelength. This sets an upper luminosity limit (at 3 kpc) of ~1000Lsun (~8Msun) for an individual source.

  15. THANK YOU VERY MUCH FOR YOUR ATTENTION! Me struggling with AIPS. Photograph: João

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