Transcript Contributions of interferometry for Orion

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?