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Contributions if Interferometry for Orion M. Robberto (ESA/STScI) The Orion Cluster The Orion Cluster 2mass near-IR image Why Orion is important? • Is the nearest GMC and the most recent episode of massive star formation • Distance is fairly well known (~450pc) • Background contamination is low • Is the paradigm for typical star formation • Is the paradigm for typical planet formation? The HST mosaic HST; Ha+[OIII]+[SII] (courtesy Bob O’Dell) HST; F547M (courtesy Bob O’Dell) VLT JHK composite 3.5 micron image Lada et al., 2000 10 micron image 10 micron image BN-KL Ney-Allen OMC1-S 174 point N-micron point sources Understanding the IR emission of photoevaporated disks • Disks in HII regions are under the influence of a complex radiation field • HST data constrain the model parameters (tilt angle with respect to the ionizing star and to the Earth, distance from the ionizing star, disk size…) Robberto, Beckwith and Panagia, Ap.J, 2002 (in press) MID-IR imaging > photometry > SEDs vs. disk models Ha,[OIII],[SII] 2.2mm 3.5mm Robberto, Beckwith and Herbst, 2000 10mm BN/KL IRC2 Dougados et al. 1993 ApJ 406,111 MAX N-band OMC1-South Search for the OMC1-South exciting source Ney-Allen nebula MAX 10mm MAX 10/20mm HST/WFPC2 F547M q1Ori-C and SC3 F336W – PC 1s q1Ori-C and SC3 F336W – PC 30s q1Ori-C and SC3 F439W – PC 1s q1Ori-C and SC3 F439W – PC 30s q1Ori-B is extended/binary F457M – PC 30s Modeling the arcs q1Ori-D anomaly Is Ney Allen Nebula associated to q1Ori-D?