Background Spectral Line Energy Distribution (SLED): Flux per emission line Sensitive to physical conditions (i.e., density, temperature, radiation field) Can we differentiate between excitation mechanisms (e.g., shocks, PDR, XDR)? What if only a limited number of lines have been observed/detected? June 24, th ISMS: WI083
CO Spectral Line Energy Distributions in Orion Sources:
Templates for Extragalactic Observations Nick Indriolo & Ted
Bergin University of Michigan June 24, th ISMS: WI081
Acknowledgments Javier Goicoechea & Jose Cernicharo Orion maps
in PACS & SPIRE Christine Joblin Orion Bar HIFI & PACS data
Peter Schilke & Darek Lis Sgr B2 HIFI data June 24, th ISMS:
WI082 Background Spectral Line Energy Distribution (SLED): Flux per
emission line Sensitive to physical conditions (i.e., density,
temperature, radiation field) Can we differentiate between
excitation mechanisms (e.g., shocks, PDR, XDR)? What if only a
limited number of lines have been observed/detected? June 24, th
ISMS: WI083 CO Rotational Ladder CO rotational transitions evenly
spaced in frequency Above J8 requires space- based observatory
Herschel Space Observatory HIFI: 5J16; v0.5 km/s PACS: 14J48; v200
km/s SPIRE: 4J13; v300 km/s June 24, th ISMS: WI084 NGC 253
Herschel SPIRE Spectrum June 24, th ISMS: WI085 Rosenberg et al
A&A, 564, A126 1 Jy = W m -2 Hz -1 NGC 253 CO SLED Emission
line flux from each transition Curves are for models with variety
of conditions Requires multiple components with different physical
conditions June 24, th ISMS: WI086 Rosenberg et al A&A, 564,
A126 Extragalactic CO SLEDs June 24, th ISMS: WI087 Mashian et al.
2015, ApJ, 802, 81 Spatial Resolution SPIRE-FTS beam sizes at long
(red) and short (blue) wavelengths Emission from many regions is
blended, and observed region is changing with wavelength/transition
June 24, th ISMS: WI088 Spinoglio et al ApJ, 758, 108 NGC 1068
nucleus; CO kpc Orion Nebula June 24, th ISMS: WI089 Peng et al
2012 A&A, 538, A12; 13 CO 8-7 ODell et al. 2008, Handbook of
Star Forming Regions, Vol. I ODell 2001 ARA&A, 39, 99
Star-forming region about 410 pc away Orion Nebula: Line Profiles
June 24, th ISMS: WI0810 Peng et al A&A, 538, A12 Orion Nebula:
Line Profiles June 24, th ISMS: WI0811 Orion Bar (PDR)Orion South
(protostars, outflows, PDR) Line Profile Comparison Broad, more
complex profiles including self-absorption in Ori KL and H 2 Peak 1
Decomposition not straightforward in all cases June 24, th ISMS:
WI0812 CO SLED: Orion Bar June 24, th ISMS: WI0813 CO SLED: Orion
South June 24, th ISMS: WI0814 CO SLED: Orion KL and H 2 Peak 1
June 24, th ISMS: WI0815 Orion H 2 Peak 1 Interpretation Fit with
three different components cool plateau warm shock hot shock June
24, th ISMS: WI0816 Goicoechea et al. 2015, ApJ, 799, 102 CO SLED:
M 82 and NGC 1068 June 24, th ISMS: WI0817 NGC 1068: scaled to 410
pc June 24, th ISMS: WI0818 NGC 1068 Interpretation Models use XDR,
PDR, and shock to fit CO emission line fluxes XDR and shock are
favored, but cannot be distinguished Note importance of J=30 point
June 24, th ISMS: WI0819 Hailey-Dunsheath et al ApJ, 755, 57
Summary & Future Work CO SLEDs measured in a sizeable sample of
galaxies (primarily active) Overall shapes are combinations of
different excitation mechanisms and conditions The nearby Orion
star-forming region, where conditions are "well-known", can be used
to make templates for shocks, PDRs, etc. What combination of these
objects/regions can reproduce extragalactic CO SLEDs? June 24, th
ISMS: WI0820
