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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, 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

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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