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High Precision Photometry Survey of the Orion Nebula Cluster at the 205th AAS Meeting

The HST Survey of the Orion Nebula Cluster team presented their findings at the 205th AAS Meeting in San Diego, focusing on high precision photometry to create an accurate HR diagram of PMS stars. The goals included analyzing the Initial Mass Function (IMF), studying accretion and disk dissipation in different environments, and identifying a population of PMS binaries and low-mass stars down to ~10 MJ. The strategy incorporated 104 HST orbits utilizing ACS, WFPC2, and NIC3 instruments, covering approximately 0.15 square degrees.

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High Precision Photometry Survey of the Orion Nebula Cluster at the 205th AAS Meeting

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  1. The HST Survey of the Orion Nebula ClusterScience team: M. Robberto (ESA-STScI), D. Soderblom (STScI), C. R. O’Dell (Vanderbilt), L. A. Hillenbrand (Caltech), M. Simon (Stony Brook), E. D. Feigelson (Penn State), J. Najita (NOAO), K. G. Stassun (Vanderbilt), J. Stauffer (IPAC-Caltech), M. Meyer (Steward), J. Krist (JPL), N. Panagia (STScI), M. Romaniello (ESO), F. Palla (Arcetri), I.N. Reid (STScI), P. McCullough (STScI), R. Makidon (STScI)Home team:E. Bergeron (STScI),M. McMaster (STScI), V. Kozhurina-Platais (STScI), H. McLaughlin (STScI),K. Smith (STScI), W. Sherry (NOAO) 205th AAS Meeting, San Diego

  2. Goals • Use deep, simultaneous, high precision photometry to assemble the richest, most accurate, unbiased HR diagram of PMS stars ever made • IMF and its variation with environment • Accretion and disk dissipation vs. environment • Stellar multiplicity vs. disk fraction • Discover substantial population of PMS binaries, low mass stars and brown dwarfs down to ~10MJ • Ha survey of disks, jets, proplyds 205th AAS Meeting, San Diego

  3. Strategy 104 HST orbits, parallel ACS+WFPC2+NIC3 • ACS: B (420s), V (385s), I (385s), z (385s), Ha (340s) • WFPC-2: U (2400s), B (80s), I (10s), Ha(400s) • NIC-3: J (5256s), H (4192s) 2 Orientations • 100° (36 orbits, Fall 2004) • 280° (68 orbits, Spring 2005) Precise tiling pattern allows for full coverage with ACS and WFPC2 205th AAS Meeting, San Diego

  4. Survey area Current on 2-Mass • ACS & WFP2: ~0.15sq. deg; NIC3~113-127 sq.arcmin • WFPC2: 205.4 Mpix • ACS: 904 Mpix • NIC-3: 7.4-8.3 Mpix final on ESO-WFI 205th AAS Meeting, San Diego

  5. An ACS strip B, Ha-V, I 205th AAS Meeting, San Diego

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  8. WFPC2 Ha 205th AAS Meeting, San Diego

  9. NICMOS FOM increases area surveyed by 1.6. Factor ~2 possible. Galaxies in NICMOS fields 205th AAS Meeting, San Diego

  10. ACS+NICMOS F850LP F775W F555W F658N F435W 205th AAS Meeting, San Diego

  11. NIC3 205th AAS Meeting, San Diego

  12. NIC-3 photometry • Two populations: • J~12-14 (M type stars) • J~18-22 (background objects) 205th AAS Meeting, San Diego

  13. CM diagrams: V vs. V-I 205th AAS Meeting, San Diego

  14. CM diagrams: I vs. I-z 205th AAS Meeting, San Diego

  15. Stellar density 205th AAS Meeting, San Diego

  16. Star counts – I band 205th AAS Meeting, San Diego

  17. Ground-based follow-up • Simultaneous UBVIJHK photometry of the ONC • ISPI @ CTIO Blanco 4m: JHK • WFI @ ESO 2.2m: UBVI+Ha Plus CTIO 0.9m, data taken on Jan 1-2, 2005 • Optical Multi-object spectroscopy (Hillenbrand) • Near-IR spectroscopy (Meyer) 205th AAS Meeting, San Diego

  18. A look at the core region 205th AAS Meeting, San Diego

  19. New objects in the outer regions V Ha 205th AAS Meeting, San Diego

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