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hat we look for when e look for the dark gas * John Dickey Wentworth Falls 26 Nov 2013 *Wordplay on a title by Raymond Carver, "What we talk about, when we talk about love"

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What we look for when we look for the dark gas *. John Dickey Wentworth Falls 26 Nov 2013. *Wordplay on a title by Raymond Carver, "What we talk about, when we talk about love". Summary: - PowerPoint PPT Presentation

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Page 1: What we look for when we look for the dark gas *

What we look for whenwe look for the dark gas*

John DickeyWentworth Falls26 Nov 2013

*Wordplay on a title by Raymond Carver, "What we talk about, when we talk about love"

Page 2: What we look for when we look for the dark gas *

Summary:• The Dark Gas is a mixture of atomic and molecular hydrogen that is not traced by either 21-cm emission or CO emission.• The Dark Gas shows the continuity between the CNM and the diffuse molecular medium.• The large amount of dark gas indicated by the dust emission shows that the effects of 21-cm absorption are significant and must be included to interpret low latitude surveys.• The C+ line probes this medium; it will be excellent for comparison with 21-cm in both emission and absorption!

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Boulanger & Perrault 1988 (see also Heiles, Reach, & Koo 1988)

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For 20 years we thought we understood this! Why was the dark gas a surprise in 2008/10 ?

The physics is similar to what we see in photo-dissociation regions.

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Lee et al. 2012 GALFA + IRAS + COMPLETE study of the Perseus molecular cloud and its surroundings

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Lee et al. 2012 Arecibo map of Perseus, cf. Planck consortium XXIV GBT maps of 14 high latitude fields. Note that Rmol drops suddenly at a threshold radius.

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Lee et al. 2012 compare with theoretical models by Wolfire, Hollenbach & McKee 2010 and Krumholz, McKee &Tumlinson 2008, 2009. They find a clear threshold for the molecular/atomic transition, but they don't see the dark molecular gas – there is still a factor of 3 disagreement between the observations and the models.

The equilibrium between H2 formation and destruction is very complicated!

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A quick review of PDR physics, following Draine & Bertoldi 1996a,b and Draine 2011 book.

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from

The transitions are compressed in a PDR :

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A view of the far uv, from 10.4 eV to 13.6 eV photon energy:

l (Angstroms)912

1101 C – C+

1216 Ly a 1110

Lyman-Werner Bands

1026 Ly b

The photon energy for ionization of Carbon is at the lower edge of the Lyman-Werner band where photons can photodissociate H2, and H2 self-shields.

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fmol

time

From Draine and Bertoldi 1996

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interstellar radiation field in the neutral medium near an HII region

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Interstellar radiation field in the neutral medium in a typical region (near the sun)

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10%

50%

90%

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So there must be a range of at least an order of magnitude in shielding column density over which the molecular fraction of H changes smoothly from 0.1 to 0.9.

So is there much molecular H in classical CNM regions?

Yes, it was seen in far-uv absorption by FUSE and Copernicus.

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1977

molecularfraction f

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Rachford et al. 2009 Summary of FUSE and Copernicus results for the excitation temperature of the H2 molecules and their fractional abundance.

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Correcting 21-cm Measurements ofHI Column Density for self-absorption

How can there be so much more CNM than we thought there was?

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Conclusion:No wonder there's "dark gas".

The dust emission shows that we have underestimated the correction factor due to the optical depth of the CNM acting on the background continuum as well as the background line emission.

Page 36: What we look for when we look for the dark gas *

What about the optical depths of the fine structure lines?

Could an absorption-emission experiment be done to measure the optical depth?

Page 37: What we look for when we look for the dark gas *

WNM

CNM

The atomic ISM cools through the 158m C II and the 63m O I lines.

Tracing these lines traces the energy flow through the ISM.

Page 38: What we look for when we look for the dark gas *

The fine structure lines have sub-thermal excitation in diffuse ISM conditions:

n T = 2000 K cm-3

n T = 4000 K cm-3

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In diffuse atomic clouds every collisional excitation is followed by a radiativede-excitation.

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What does Herschel see?

Langer et al. 2010

Page 41: What we look for when we look for the dark gas *

Nearby SGPS HI emission and absorption spectra (Strasser 2006)note the HISA features

Page 42: What we look for when we look for the dark gas *

Comparing the integrated line fluxes of the C II and H I lines...(Langer et al. 2010)

Page 43: What we look for when we look for the dark gas *

Gerin et al. 2013 A&A submitted

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Page 45: What we look for when we look for the dark gas *

Slide from Gerin et al. 2013

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Slide from Gerin et al. 2013

Page 47: What we look for when we look for the dark gas *

Conclusions:• The dark gas must be partly CNM• We can trace the missing gas by combining continuum and 21-cm emission surveys with a densely sampled absorption survey.• The 158m C+ line will be a great tracer of the CNM

Page 48: What we look for when we look for the dark gas *

Questions:• Theory: could we please have a dynamical model of the molecule formation vs. photodissociation that includes time dependent changes in the radiation field?

• Observations: Let's make a well sampled map of the 21-cm optical depth along a large number of lines of sight at low latitudes, plus a continuum map to use with them to correct the HI column density maps.


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