contributions if interferometry for orion m. robberto (esa/stsci)
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Contributions if Interferometry for Orion
M. Robberto
(ESA/STScI)
The
Gre
at O
rion
Neb
ula
The Orion Cluster
2mass near-IR image
The Orion Cluster
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 Understanding the IR emission of
photoevaporated disksphotoevaporated disks• Disks in HII regions are under the Disks in HII regions are under the influence of a complex radiation fieldinfluence of a complex radiation field• HST dataHST data constrain the model constrain the model parameters (tilt angle with respect to the parameters (tilt angle with respect to the ionizing star and to the Earth, distance ionizing star and to the Earth, distance from the ionizing star, disk size…)from the ionizing star, disk size…)
Robberto, Beckwith and Panagia, Ap.J, 2002 (in press)
S 2.2m 3.5m 10m
182-336
1.0
10.0
100.0
0.1 1.0 10.0 100.0l (m)
Fn(J
y) x
10
11
dereddened
M0V star
observed
face-on passive disk
170-337
0
0
1
10
100
0.1 1.0 10.0 100.0l (m)
Fn(J
y) x
10
11
observedM0.5 stardereddenedface-on passive disk
Robberto, Beckwith and Herbst, 2000
MID-IR imaging > photometry > SEDs vs. disk models
BN/KL
IRC2
MAX N-band
Dougados et al. 1993 ApJ 406,111
OMC1-South
Search for the OMC1-South exciting source
Ney-Allen nebula
MAX 10/20mHST/WFPC2 F547M
MAX 10m
1Ori-C and SC3
F336W – PC 1s
1Ori-C and SC3
F336W – PC 30s
1Ori-C and SC3
F439W – PC 1s
1Ori-C and SC3
F439W – PC 30s
1Ori-B is extended/binary
F457M – PC 30s
Modeling the arcs
1Ori-D anomaly
Is Ney Allen Nebula associatedto 1Ori-D?