the cnm – how much, how cold, and where? john dickey university of tasmania 4 february 2013 c + as...
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The CNM – How Much, How Cold, and Where?
John DickeyUniversity of Tasmania
4 February 2013C+ as an Astronomical Tool
The Cycle of Galaxy EvolutionAtomic
hydrogen emission
Atomic hydrogen absorption +
diffuse OH emission
OH masers
OH masers
Synchrotron emission
Image credit: Bill Saxton (NRAO)
Murray, Stanimirovic, Goss,Heiles, JD, Begum, Hennebelle 2013 in prep.
The 21-SPONGE Project (EVLA)
Gaussian fitting gives:Tsp = 178 KTsp = 2280 K
Spin temperature distribution from Heiles and Troland (2003, Ap. J. 586, 1067) based on Gaussian fitting techniques.
Spin temperature distribution from Dickey et al. (2003, Ap. J. 585, 801) using data from Heiles and Troland (2003).
Stanimirovic and Heiles (2006 Ap. J. 631, 371), HI emission/absorption spectra from Arecibo.Using very bright background sources at high latitude (both at +81o latitude).
Moving from high latitude directions to low latitudes the CNM begins to cover a wider velocity range, due to differential Galactic rotation. But the CNM linewidths are still much narrower than the WNM emission, and there is lots of WNM emission at low levels that has no corresponding CNM.
Tsp temperature distribution of CNM clouds vs. RG
from Strasser (2006) based on SGPS, CGPS, VGPS data.
21-cm absorption can be visible againstthe bright background 21-cm emission in the Galactic plane. Recent surveys are by Gibson et al. (2005, Ap. J. 626, 195) and Kavars et al. (2005, Ap. J. 626, 887).
They find that half of all lines of sight at low latitudes contain some HISA, and roughly half of the detected HISA clouds have corresponding CO detections.
HISA – H I Self-Absorption
21-cm emission and absorption and self-absorptionfrom the Southern Galactic Plane Survey (HISA)
McClure-Griffiths et al. 2004
How much CNM is there?
Even counting the HISA gas, there is less CNM than WNM (maybe 1:3 ratio).
This ratio stays roughly constant with Galactic radius outside the solar circle.
Longitude Velocity diagrams in emission and absorption:
opacity, , binned in l and vdensity, n, measured at thesame locations and binnedin the same way as for
The structure of the CNM in the far outer Galaxy is interesting. It is located as cores or a network inside large (106 Msun) HI clouds.
The mixture of WNM, CNM, and molecular gas in these outer Galactic plane clouds resembles that in the Magellanic Clouds.
Strasser et al. 2007 A.J. 134, 2252.
This cloud is at a distance of 16 to 17 kpc from the Galactic center.
In the central 2 or 3 kpc of the Galaxy, there is CNM in most of the features that can be seen in CO and HI emission. But there is not as much CNM as we might expect, particularly in the structures inside the 3 kpc arms.
HI from McClure-Griffithset al. 2012
CO from Dame and Thaddeus 2008
Red dots: 21-cm absorption towardGalactic HII regions (Jones et al. 2013)
Galactic HII region recombination linevelocities (Jones et al. 2013)
CNM 21-cm absorption toward HII regions
Conclusions:• The CNM temperature is mostly in the range 15K to 250K. The median is about 50K.• The CNM is about 25% to 35% of the total HI mass. Thus only about 1/4 to 1/3 of the atomic medium is in the cool phase.• The CNM keeps a ~constant ratio with the WNM on a large scale in the outer MW. Some structures in the inner Galaxy have less CNM than we might expect given recent SF.
CGPS absorption and emission combined, from Strasser & Taylor 2004, Ap. J. 603, 560.
Cool phase clouds plus warm phase diffuse gas.
Data for emission/absorption spectral channels in the CGPS I+II survey (Strasser Ph.D. thesis 2006).
Monte Carlo model with random column density of HI (normal sigma 35K absolute value)...
Threshold column density of warm gas (50K + normal sig 10 K) for existence of cool gas...
All HI above the threshold is cool gas, with Tcool = 70 K...
Half of the warm gas emission is absorbed by the cool gas.