Optical Observations of High- Latitude Clouds Adolf N. Witt University of Toledo.
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Optical Observations of High-Latitude Clouds
Adolf N. Witt
University of Toledo
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Collaborators:
Steve Mandel, Hidden Valley Obs., Soquel, CAThomas G. Dixon, Univ. of Hertfordshire, UKPaul H. Sell, Univ. of ToledoKarl D. Gordon, Univ. of ArizonaUma P. Vijh, STScI
With support from:
NSF Galactic Astronomy ProgramRC Optical SystemsSanta Barbara Instrument Group, Inc.Software BisqueAstrodon
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First optical studies of HLCs by Allan Sandage, 1976, AJ, 81, 954, with M81
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“Re-discovery” of HLCs by IRAS, F. J. Low et al. 1984, ApJ, 278, L19Led to new designation as “IR Cirrus”Followed by detailed studies at mm-wavelengths (CO) by Magnani et al.
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High-Latitude Clouds are ideal for studying the morphologyof the diffuse interstellar medium.
• Nearby, ~ 100 pc• Individual “clouds” seen in relative isolation• Little line-of-sight confusion• Free of star-formation effects• Wide range of optical depths• Atomic as well as molecular gas• Typical cloud “sizes” can be measured directly
We can see actual “clouds”
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Advantages of Optical Imaging Approach
• Combines high spatial resolution (arc sec) with large field of view• Sensitive to column density of dust ---> total gas column density• Insensitive to dust temperature• Independent of atomic or molecular state of the gas as long as dust-to-gas ratio is constant• Offers ideal conditions for study of dust luminescence• Direct evidence for small-scale structure on few 102 AU scale• Low cost Disadvantages (No such thing as a free lunch!!)
• Low surface brightness (few % of that of the dark night sky)
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Instrumentation
Remotely operated, self-guided small telescopes, equipped with CCD cameras.
Detection of diffuse, extended sources depends only on f-ratio, not aperture.
Location: New Mexico Skies Altitude ~7300 ft, near Cloudcroft, NM
Primary Goal: Determination of the optical SEDs of HLCs
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Optical Bandpasses
Special BGRIHa filter set during Phase1 of our program
15-band BATC filter set during Phase 2 of our program. These filters allow the determination of a detailed cloud SED while avoiding the strongest emission features of the permanent airglow from the Earth atmosphere.
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What makes a high-latitude cloud shine?
• Scattering of the Galactic interstellar radiation field by dust.• Photoluminescence by nanoparticles, primarily Extended Red
Emission excited by far-UV photons from the ISRF.• H-alpha in emission, mostly from Galactic HII regions, scattered by dust in the HLCs.
This is extended red emission ---->
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How important is ERE?
• about 30% of total surface brightness of HLCs near 600 nm at intermediate latitudes
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ERE is relatively important, because dust scattering is not very efficient at high galactic latitudes.
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Here’s why:
• Illumination of HLCs comes mainly from the Milky Way
• Most of the light is scattered with scattering angles ~90 0
• HG phase function for forward-scattering grains ---> highly inefficient at ~ 90 0
• ERE is emitted isotropically, no dependence on direction of incoming illuminating radiation; depends only on density of UV radiation.
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Focus: Large-Scale Cloud MorphologyMBM 12
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MBM 30
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MBM 32
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Focus: Small-Scale Structure in MBM 12
Linear structures ~ 500 AU wide
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MBM 12
Sharp edges
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MBM 12
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MBM 30
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Focus: Small-Scale Structure in AbsorptionM 81; Image Credit: Tony Hallas
http://www.astrophoto.com/ (with permission)
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M81 detail
Linear structures again; nT ~ 106 K cm-3
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Same M81 cirrus observed in CO by A. Heithausen2006, A&A, 450, 193
cirrus resolves into small molecular clumps
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Small-area molecular clumps (SAMS) near M81
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Combining optical structure data with IR and radio structure data can extend 2-D angular power spectrum (S. J. Gibson, 2006, SINS)
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We are collaborating with Steven Gibson on the analysis of our data.
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Conclusions
• Optical imaging data of high-latitude clouds reveal ISM morphology and small-scale structures over 3 orders of magnitude of linear scale
• Cloud morphology: Clumpy cores embedded in low-density envelope
• Small-scale structure: linear strands of high-density gas, ~500 AU
• Under special conditions (e.g. M81) structure in Galactic ISM can be observed in absorption.
• Illumination geometry of high-latitude clouds makes them ideal test beds for studies of extended red emission (ERE) in the diffuse ISM.