in the Central Molecular Zone of H

+ in the Central Molecular Zone of H 3 the Galactic Center: Revelation of a New Category of Gas Takeshi Oka Department of Astronomy and Astrophysics and Department of Chemistry, The Enrico Fermi Institute, University of Chicago Tom Geballe Gemini Observatory Smiles, Kos, Greece, October 5, 2010

The Central Molecular Zone (CMZ) The Treasure House of H 3+ R(1, 1)u R(1, 0) 3 × 1014 cm-2 10 -5 10% T. R. Geballe, Phil. Trans. Roy. Soc. Lond. A 358, 2503 (2000) CMZ 400 pc

Discovery of the (J, K) = (3, 3) Metastable H 3+ Goto, Mc. Call, Geballe, Usuda, Kobayashi, Terada, Oka, 2002, PASJ 54, 951 Spontaneous breakdown of symmetry (1, 1) ground Para I = 1/2 Ortho I = 3/2 J (3, 3) metastable 8 hrs 20. 4 days (1, 0) 16 hrs (3, 3) Metastable (2, 2) T ~ 250 K (2, 2) unstable n ≤ 100 cm-3 361 K 27. 2 days CO J = 1 (1, 1) K Pan and Oka, 1987, Ap. J, 305, 518 Oka, Geballe, Goto, Usuda, Mc. Call, 2005, Ap. J, 632, 882

Breaking Symmetry The 2 band of H 3+ μ 2 = 2521 cm 1 = 0. 158 D J R(1, 0) R(3, 3)l (3, 3) l R(2, 2)l R(1, 1) (2, 2) (1, 0) (1, 1) K Oka, Phys. Rev. Lett. 45, 531 (1980)

Telescopes and spectrometers Telescope UKIRT Subaru　 Gemini South VLT Gemini North D 3. 8 m 8. 2 m 8 m Spectrom. CGS 4 IRCS Phoenix CRIRES GENIRS Gemini North Subaru UKIRT λ/Δλ 40, 000 Mauna Kea 1982 20, 000 Mauna Kea 2000 60, 000 Cerro Pachon 2003 100, 000 Cerro Paranal 2006 18, 000 Mauna Kea 2011 Gemini South VLT

CMZ

Quintuplet Cluster Super-massive clusters GCS 3 -2 1° × 1° 140 pc × 140 pc

H 3+ near the GC Surprises 30 pc UKIRT Huge column density; rich profile Geballe et al. Ap. J 1999 Subaru (3, 3) metastable and (2, 2) unstable H 3+ Goto et al. PASJ 2002 Thermalization model analysis Oka & Epp Ap. J 2004 Gem. S Revelation of warm and diffuse gas Oka et al. Ap. J 2005 Review Oka PNAS 2006 Subaru From the center to 30 pc east Goto et al. Ap. J 2008 VLT Scrutiny of the Central core Goto et al. 2010 Gem. S Synthesis Oka et al. 2011

Simple chemistry of H 3+ ζ Production H 2 → H 2+ + e Destruction H 2+ +H 2 →H + H 3+ dn(H 3+)/dt = ζn(H 2) H 3+ + e → H + H = ken(H 3+)n(e) Mc. Call et al. Phys. Rev. A (2004) 7. 3 × 10 -8 cm 3/s 1. 6 × 10 -4 1 ζL = 2 ke N(H 3+) (n. C/n. H)SV RX / f (1. 8 -6. 1) × 1015 cm-2 3 (ζL)min = (1. 3 – 4. 3) × 105 cm/s ζ 10 -16 10 -15 L (0. 4 – 1. 4) kpc 40 - 140 pc Goto, Usuda, Nagata, Geballe, Indriolo, Mc. Call, Suto, Henning, Morong, and Oka, Ap. J, 668, 306 (2008)

Previous concept of gas in the CMZ need to be drastically changed f: 0. 8 107 -8 K 0. 1 104 -6 K 10 cm-3 0. 1 50 K 104 cm-3 > 0. 2 250 K 102 cm-3 Lazio & Cordes, Ap. J, 505, 715 (1998) Warm and diffuse gas

X-ray: Chandra comes to rescue Chandra 20 pc × 20 pc (0. 5 – 8) ke. V Muno et al. Ap. J 589, 225 (2003) Warwick, Sakano Decourchelle (2006) Revnivtsev et al. (2006)

Opening a New Vista CMZ

Search for bright and hot stars in the CMZ GLIMPSE Point Source Catalogue of the Spitzer Space Telescope, L to M Ramírez et al. 2008, Ap. JS, 175, 147 2 MASS photometry at J, H, and K bands Skrutskie et al. 2006, AJ, 131, 1163 ~ 2, 000 stars brightness L < 7. 5 8 Star GCS 3 -2 GCS 4 NHS 21 NHS 25 L 3. 03 3. 71 4. 62 6. 24 J – K K – L (J – K)/(K – L) 7. 33 3. 16 2. 32 7. 65 3. 45 2. 22 7. 03 2. 76 2. 55* 4. 81* 1. 27* 3. 79* ~ 3, 000 stars youth J - K > 5 K - L > 1. 5 (J – K)/(K – L) < 2. 5 ~ 300 stars 83 stars so far hotness Low res. CO first overtone, 2. 2 – 2. 4μm Candidate stars 10 new stars and 5 known stars location High res. H 3+ and CO spectroscopy Selected stars

New bright and hot dust embedded stars suitable for H 3+ spectroscopy Geballe and Oka, Ap. J, 709, L 70 -73 (2010)

Two sightlines with remarkable H 3+ spectrum Quintuplet, α, ι 0 – 30 pc East α ι Geballe and Oka, Ap. J, 709, L 70 -73 (2010)

Iota, the Monster “iota”, 85 pc East, Sgr B (2, 2) (3, 3) Geballe and Oka, Ap. J 709, L 70 -73 (2010) Subaru May 4, 2010 Low n High T

Remarkable similarity between velocity profiles of H 3+ toward Iota and H 2 O+, CH+ toward Sgr B 2 3 kpc Herschel observations of ortho- and paraoxidaniumyl (H 2 O+) in spiral arm clouds toward Sgr B 2(M) ⋆ Scutum Sgittarius H 2 O+ 110← 101 H 3+ R(1, 1)l H 2 O+ 111← 000 P. Schilke, 1, 2 C. Comito, 2 H. S. P. M¨uller, 1 E. A. Bergin, 3 E. Herbst, 14 D. C. Lis, 4 D. A. Neufeld, 20 T. G. Phillips, 4 T. A. Bell, 4 G. A. Blake 5 E. Caux, 6, 7 C. Ceccarelli, 8 J. Cernicharo, 9 N. R. Crockett, 3 F. Daniel, 9, 10 M. -L. Dubernet, 11, 12 M. Emprechtinger, 4 P. Encrenaz, 10 M. Gerin, 10 T. F. Giesen, 1 J. R. Goicoechea, 9 P. F. Goldsmith, 13 H. Gupta, 13 C. Joblin, 6, 7 D. Johnstone, 15 W. D. Langer 13 W. B. Latter 16 S. D. Lord, 16 S. Maret, 8 P. G. Martin, 17 G. J. Melnick, 18 K. M. Menten, 2 P. Morris, 16 J. A. Murphy, 19 V. Ossenkopf, 12, 21 J. C. Pearson, 13 M. P´erault, 10 R. Plume, 22 S. -L. Qin, 13 S. Schlemmer, 1 J. Stutzki, 1 N. Trappe, 19 F. F. S. van der Tak, 21 C. Vastel, 6, 7 S. Wang, 3 H. W. Yorke, 13 S. Yu, 13 N. Erickson, 25 F. W. Maiwald, 13 J. Kooi, 4 A. Karpov, 4 J. Zmuidzinas, 4 A. Boogert, 4 R. Schieder, 1 and P. Zaal 21 A&A June 22 2010 E. Falgarone et al. 2010 Geballe & Oka, 2010, Ap. J, 709, L 70 17 pc

β α

HCl+ H 2 Cl+ HCl Cl− ? ? ? 1 - 10 Dariusz Lis H 2+ H 3+ H 2 O + H 3 O + H 2 O OH− ~ 3. 3 Floris van der Tak H− 107

http: //www. dn. se/nyheter/vetenskap/the-frontrunners-of-the-nobel-prize-2010 -1. 1181788 Chemistry: Maybe the spectra of spectroscopy – a close up as well as all the way to outer space? William Moerner has developed a spectrometer that can discern individual molecules of elements. William Klemperer has developed methods to establish what molecules are present in the dust clouds between the stars. Maybe a combination of those two, and maybe Richard Zare and/or Allen Bard will be in on it.