Warm and Diffuse Gas and High Ionizzation Rate Near the Galactic Center from 140 pc West to 85 pc East of Sgr A* 66th OSU International Symposium, June 21, 2011 Takeshi Oka , Chris MORONG, University of Chicago, Chicago Tom Geballe, Gemini Observatory, Hilo Nick Indriolo, Ben McCall, University of Illinois at Urbana-Champaign, Urbana Miwa Goto, Max-Planck-Institute for Astronomy, Heidelberg Tomonori Usuda, Subaru Telescope, Hilo arvey Liszt, National Radio Astronomy Observatory
Warm and Diffuse Gas and High Ionizzation Rate Near the Galactic Center from 140 pc West to 85 pc East of Sgr A* 66th OSU International Symposium, June.
Dec 21, 2015
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Warm and Diffuse Gas and High Ionizzation Rate Near the Galactic Center
from 140 pc West to 85 pc East of Sgr A*
66th OSU International Symposium, June 21, 2011
Takeshi Oka, Chris MORONG, University of Chicago, Chicago Tom Geballe, Gemini Observatory, Hilo Nick Indriolo, Ben McCall, University of Illinois at Urbana-Champaign, Urbana Miwa Goto, Max-Planck-Institute for Astronomy, HeidelbergTomonori Usuda, Subaru Telescope, Hilo
Harvey Liszt, National Radio Astronomy Observatory
α+
λε+ ε-η+
θ-
θ+
δ+
30 pc
Oka, Geballe, Goto, Usuda, McCall, 2005, ApJ, 632, 882GCS 3-2
Goto, Usuda, Nagata, Geballe, McCall, Indriolo,Suto, Henning, Morong, Oka, 2008, ApJ, 688, 306
, Geballe, Oka, 2010, ApJ, 709, L70
T ~ 250 Kn < 100 cm-3
L > 2.2 105 cm/s = 2 10-15 s-1 L > 35 pc
Two sightlines with remarkable H3+ spectrum
α 140 pc West
ι 85 pc East
Geballe and Oka, 2010, ApJ, 709, L70-73
0 – 30 pc EastQuintuplet, α, ι
1.00
0.95
0.90
0.85
0.80
0.75
0.70
-200 -150 -100 -50 0 50 100
GCS 4
NHS 21
NHS 25
NHS 42
FMM 361
“alpha”, 140 pc West, 2.7 pc below
Alpha
Geballe and Oka, ApJ 709, L70-73 (2010)
H. Liszt, ApJL, 82, 495 (1992)
13CO
Sgr E, 144 pc West, 20 pc above
S
Sgr ESgr E 3 kpc SA
Alpha, EMR, warm and diffuse
Geballe and Oka, ApJ 709, L70-73 (2010)
N(1,1) = 1.86 (12) 1015 cm-2 N(3,3) = 1.33 (27) 1015 cm-2
15.0715.0)1,1(
)3,3(
N
N
T ~ 300 K
Goto et al., PASJ, 64, L13-17 (2010)
α
β
α 138.7 pc W 2.65 pc below
β 133.4 pc W 4.20 pc below
α+ 138.0 pc W 6.12 pc below
α+
Three stars within 7 pc of angular distance
Three stars within 7 pc of angular distance
+
+
α
βα+
Geballe and Oka, ApJ 709, L70-73 (2010)
Iota, the Monster
“iota”, 85 pc East, Sgr B
H3+ in Iota versus H2O+ and 13CH+ in Sgr B2
Peter SchilkeP. Schilke et al., A&A, 521, L11, 2010
Edith Falgarone
H3+
H2O+
Simple chemistry of H3+: N(H3
+) → ·L
L = 2 ke N(H3+) (nC/nH)SV RX / f(H2)
7.3 ×10-8 cm3/s 1.6 ×10-4 < 1
3.1 ×1015 cm-2 > 3
L > 2.2 ×105 cm/s
L
10-17 s-1 > 7 kpc 10-16 s-1 > 700 pc 10-15 s-1 > 70 pc
0.1!?
α+
λε+ ε-η+
θ-
θ+
δ+
30 pc
Oka, Geballe, Goto, Usuda, McCall, 2005, ApJ, 632, 882GCS 3-2
Goto, Usuda, Nagata, Geballe, McCall, Indriolo,Suto, Henning, Morong, Oka, 2008, ApJ, 688, 306
, Geballe, Oka, 2010, ApJ, 709, L70
T ~ 250 Kn < 100 cm-3
L > 2.2 105 cm/s = 2 10-15 s-1 L > 35 pc
Ubiquity of H3+
Sgr A* to 30 pc East
30 pc
1.00
0.95
0.90
0.85
0.80
0.75
0.70
-200 -150 -100 -50 0 50 100
GCS 4
NHS 21
NHS 25
NHS 42
FMM 361
Goto, et al. 2008, ApJ, 688, 306
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