Spectral Sensitivity of SPICA

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Spectral Sensitivity of SPICA
Courtesy of Matt Bradford, JPL
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What will be the Best Spectral Resolution to aim
for?
With SPICA we will undoubtedly wish to look at
stars in different stages of evolution as well as
outflows, protostars and star forming regions
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VY CMa image
The Highly Evolved Star VY CMa
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VY CMa Properties
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Spectrophotometry of VY CMa
Harwit et al., ApJ 557, 844 (2002)
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VY CMa Mid-Infrared Grating Spectrum
VY CMa ISO Mid-Infrared Grating Spectrum, R 2000
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VY CMa P Cygni Profiles
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VY CMa 557 GHz
VY CMa o-H2O SWAS Spectrum
Spherical Outflow
Efstathiou / Rowan-Robinson Model
The 557 GHz (538 micron) ortho transition at R
3 x 105
Harwit Bergin, ApJ 565, L105, 2002
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At Spectral Resolution R 3 x 105
the cold primary mirror on SPICA no longer
provides advantages over Herschel. So, we should
probably restrict ourselves to lower spectral
resolving powers
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NML Cygnus Properties
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NML Cyg H2O SWS line collage
NML Cygnus H2O at Resolving Power 20,000
V. Zubko, D. Li, T. Lim M. Harwit, ApJ 610,
427, 2004
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NML Cyg H2O 100.983? line
NML Cyg H2O 100.983 ? line Observed at R 10,000
V. Zubko, D. Li, T. Lim M. Harwit, ApJ 610,
427, 2004
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Spectra of Star Forming Regions
Emission from a star forming region ( 70-100 K)
with spectral lines imposed on the dust continuum
Courtesy of Harold Yorke, JPL
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Spectra of Different Classes of Protostars
From papers by Spinoglio et al. 1999 Saraceno et
al. 1999 Nisini et al. 1999
These ISO Spectra Were Obtained with R 300
Courtesy of Harold Yorke, JPL