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1mm observations of Orion-KL
Plambeck, PACS team, Friedel, Eisner, Carpenter, ...
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fact 1: 2 massive stars in Orion-KL
Becklin-Neugebauer Object – brightest source at 5 μm
source I – heavily obscured even at 20 um
20 μm image(Downes et al. 1981)
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fact 2: source I and BN are recoiling from each other at 40 km/sec
+12 km/sec
27 km/sec NWmolecular cloud
(VLSR ~ 9 km/sec)
-4 km/sec
12 km/sec SE
source I
BN
ejected from a multiple stellar system ~500 years ago?
(proper motions proportional to line of sight velocities)
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fact 3: fingers of shock-excited H2
• proper motions suggest age of 1000 yrs
• related to the BN-I explosion?
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fact 4: SiO v=1 masers surround source I
• discovered by Snyder & Buhl
• unusual around a young star
43 GHz VLBA map
source I
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outflow from source I(Plambeck, Wright, Friedel et al 2009)
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Orion-KL 225 GHz map with 0.9’’ resolutionneed higher resolution to measure fluxes of BN and source I
BN?
source I
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we want to filter out large scale structure...the perfect job for an interferometer
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well-suited for PACS observations30 GHz calibrator is ~1 Jy, 1.6 degrees away
CARMA B-array data, Dec 2008
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check fluxes against Dec 2007 B-array map obtained in superb weather
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BN
source I
229 GHz continuum map0.15’’ resolution
circles are centered on 1995 positions
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source I continuum elongated perpendicular to SiO outflow
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radio continuum spectra
Beuther et al SMA
CARMA 86 GHz (Friedel & Widicus Weaver 2009)
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limiting cases of radio spectra
uniform density HII regionS ~υ2 at low freqS ~ υ-0.1 at high freq
freely expanding fully ionized windS ~ ν0.6
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fits - uniform density HII regions
R = 7.6 AU, ne = 7.1e7
R = 10.5 AUne = 2.8e7
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BN – can fit low freqs with power law ‘halo’
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H recombination lines toward BNRodriguez et al 2009 CARMA CARMA
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line/continuum opacity ~ υ1.1
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BN
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no detection of H30α toward source I
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H30α line profiles predicted by HII region model
free-free continuum optically thin, but no recombination line?
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implication: H is not ionized – opacity from H- free-free, as in stellar atmospheres
• T ~ 1500 K• ionized Na, K contribute the
electrons• opacity (per H) ~ 10-3 of p+-e-
opacity• responsible for the radio
photospheres of Miras (Reid and Menten 1997)
p+
e-
p+ - e-
H
e-
H – e-
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implications for source I(Reid et al. 2007)
• need high densities (~ 1014 cm-3 at 4 AU) to get enough opacity – total disk mass ~ 3 Mo
• central star unlikely to maintain T = 1500 K at r = 25 AU – heated by accretion?