CH +, CH, and CN Emission from the Red Rectangle Lewis M. Hobbs, Julie A. Thorburn, D. G. York, Takeshi Oka, Department of Astronomy and Astrophysics,

Slides:

Advertisements

Similar presentations

June 26, th International Symposium on Molecular Spectroscopy The Pure Rotational Spectrum of ZnS (X 1  + ) Lindsay N. Zack Lucy M. Ziurys Department.

Advertisements

R. S. RAM and P. F. BERNATH Department of Chemistry, University of York, Heslington, York YO10 5DD, UK. and Department of Chemistry, University of Arizona,

Dissociative Recombination of Cold H 3 + and its Interstellar Implications  T. Oka (University of Chicago), T. R. Geballe (Gemini Observatory)  A. J.

Estimated SOFT X-ray Spectrum and Ionization of Molecular Hydrogen in the Central Molecular Zone of the Galactic Center Masahiro Notani and Takeshi Oka.

Ionization of H 2 by X-rays in the Central Molecular Zone of the Galactic Center Masahiro Notani and Takeshi Oka Department of Astronomy and Astrophysics,

21 November 2002Millimetre Workshop 2002, ATNF First ATCA results at millimetre wavelengths Vincent Minier School of Physics University of New South Wales.

Benjamin McCall and Takeshi Oka University of Chicago Kenneth H. Hinkle National Optical Astronomy Observatories Thomas R. Geballe Joint Astronomy Centre.

Linear Analysis of Infrared CO Spectra Takeshi Oka Department of Astronomy and Astrophysics and Department of Chemistry, The Enrico Fermi Institute, University.

The Non-Thermal Rotational Distribution of Interstellar H 3 + (ApJ, in press ) Takeshi Oka and Erik Epp, Department of Astronomy and Astrophysics, and.

The (3, 3) metastable rotational level of H 3 + Takeshi Oka Department of Chemistry and Department of Astronomy and Astrophysics The Enrico Fermi Institute,

Galactic Center Region Concentrated stars and interstellar matter High Energy Density (gravity, MHD, kinetic) Strong magnetic field :B ~ mG High external.

H 3 +, in planetary Ionospheres: Emission Spectrum 岡武史 Department of Astronomy and Astrophysics, Departmen of Chemistry and The Enrico Fermi Institute,

Hot and Diffuse Gas near the Galactic Center Probed by Metastable H 3 + Thomas R. Geballe Gemini Observatory Miwa Goto Max Planck Institute for Astronomy.

H3+H3+. Search for hot and bright stars for H 3 + spectroscopy Near the Galactic center Takeshi Oka Department of Astronomy and Astrophysics and Department.

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.

H 3 + : A new probe of the Galactic center Takeshi Oka Department of Astronomy and Astrophysics and Department of Chemistry, The Enrico Fermi Institute,

The Galactic center region Concentrated stars and interstellar matter High energy density (gravity, MHD, kinetic) Strong magnetic field :B ~ mG High external.

Two Sightlines toward the Galactic Center with Remarkable H 3 + and CO Spectra Takeshi Oka Department of Astronomy and Astrophysics and Department of Chemistry,

Thermalization of interstellar CO Takeshi Oka Department of Astronomy and Astrophysics and Department of Chemistry The Enrico Fermi Institute, University.

Interstellar H 3 + in Metastable Rotational Levels Takeshi Oka and Erik Epp Department of Chemistry and Department of Astronomy and Astrophysics, The Enrico.

H 3 +, the new probe for ionization rate  Takeshi Oka Department of Astronomy and Astrophysics and Department of Chemistry The Enrico Fermi Institute,

HD , the C 2, C 3 rich sightline. The C 2 Diffuse Interstellar Bands Takeshi Oka Department of Astronomy and Astrophysics And Department of Chemistry.

OBSERVATIONS OF INTERSTELLAR HYDROGEN FLUORIDE AND HYDROGEN CHLORIDE IN THE GALAXY Raquel R. Monje Darek C. Lis, Thomas Phillips, Paul F. Goldsmith Martin.

ISM Lecture 13 H 2 Regions II: Diffuse molecular clouds; C + => CO transition.

Progress in measurements of dissociative recombination CRP on Atomic and Molecular Data for Plasma Modelling Mats Larsson Department of Physics Stockholm.

Hydroxyl Emission from Shock Waves in Interstellar Clouds Catherine Braiding.

TiH IN SUBDWARFS P. F. Bernath Department of Chemistry, University of Waterloo, Waterloo, Ont., Canada N2L 3G1 C.W. Bauschlicher, Jr NASA Ames Research.

Molecular Survival in Planetary Nebulae: Seeding the Chemistry of Diffuse Clouds? Jessica L. Dodd Lindsay Zack Nick Woolf Emily Tenenbaum Lucy M. Ziurys.

A Study of HCO + and CS in Planetary Nebulae Jessica L. Edwards Lucy M. Ziurys Nick J. Woolf The University of Arizona Departments of Chemistry and Astronomy.

Modeling Linear Molecules as Carriers of the 5797 and 6614 Å Diffuse Interstellar Bands Jane Huang, Takeshi Oka 69 th International Symposium on Molecular.

June 21, th International Symposium on Molecular Spectroscopy Nicholas R. Zeigler Lindsay N. Zack Neville J. Woolf Lucy M. Ziurys Department of.

Spectroscopy of H 3 + and CO toward the Galactic center Takeshi Oka, Christopher P. Morong, Department of Astronomy And Astrophysics and Department of.

Observations of OH + and H 2 O + Across the Galaxy with Herschel Nick Indriolo 1, David Neufeld 1, Maryvonne Gerin 2, & PRISMAS consortium 1 – Johns Hopkins.

The Nearly Perfect Correlation between the Diffuse Interstellar Bands λλ and Ben McCall Department of Chemistry and Department of Astronomy.

June 16-20, rd International Symposium on Molecular Spectroscopy Direct Measurements of the Fundamental Rotational Transitions of CD and 13 CH.

H 3 + Toward and Within the Galactic Center Tom Geballe, Gemini Observatory With thanks to Takeshi Oka, Ben McCall, Miwa Goto, Tomonori Usuda.

Molecular Interstellar Absorption toward the Pleiades Star Cluster Adam Ritchey Department of Physics & Astronomy University of Toledo June 21, 2006.

FC10; June 25, 2010Image credit: Gerhard Bachmayer Constraining the Flux of Low- Energy Cosmic Rays Accelerated by the Supernova Remnant IC 443 N. Indriolo.

A Survey of Large Molecules toward the Protoplanetary Nebula CRL 618 Anthony J. Remijan NASA/GSFC Friedrich Wyrowski Max-Planck-Institut fur Radioastronomie.

1 The Red Rectangle Nebula excited by excited species Nadine Wehres, Claire Romanzin, Hans Van Winckel, Harold Linnartz, Xander Tielens.

Further studies of λ Diffuse Interstellar Band Takeshi Oka, Lew M. Hobbs, Daniel E. Welty, Donald G. York Department of Astronomy and Astrophysics,

The anomalous DIBs in the spectrum of Herschel 36 II. Analysis of radiatively excited CH +, CH, and diffuse interstellar bands Takeshi Oka, Daniel E. Welty,

The anomalous DIBs in the spectrum of Herschel 36 II. Analysis of radiatively excited CH +, CH, and diffuse interstellar bands Takeshi Oka, Daniel E. Welty,

Fourier Transform Emission Spectroscopy of the B 2 Σ + -X 2 Σ + (Violet) System of CN R.S. Ram Department of Chemistry, University of Arizona, Tucson,

Warm, Dense Gas Near the Massive Protostar AFGL 2136 IRS 1 as Revealed by Absorption from the ν 1, ν 2, and ν 3 Bands of Water Nick Indriolo 1, David Neufeld.

Analysis of Anomalous DIBs in the Spectrum of Herschel 36 Takeshi Oka, Daniel E. Welty, Sean Johnson, Donald G. York, Julie Dahlstrom, and Lew Hobbs Department.

Analysis of OH +, H 2 O +, and H 3 + in a Diffuse Molecular Cloud Toward W51 Nick Indriolo 1, David Neufeld 1, Maryvonne Gerin 2, & Tom Geballe 3 1 – Johns.

R. S. RAM, J. S. A. BROOKE Department of Chemistry, University of York, Heslington, York YO10 5DD, UK. G. LI Harvard-Smithsonian Center for Astrophysics,

Diffuse Interstellar Bands, Atoms, and Small Molecules

The Distribution, Excitation, and Abundance of C +, CH +, and CH in Orion KL Harshal Gupta, 1 Patrick W. Morris, 1 Zsofia Nagy, 2 John C. Pearson, 3 Volker.

A Search for Interstellar H2DO+

AND HIGH H2 IONIZATION RATE

MODIFICATIONS OF THE RELATION BETWEEN

CH+ spectrum and diffuse interstellar bands

HCO+ in the Helix Nebula

arXiv: OBSERVATIONS AND ANALYSIS

Nick Indriolo1, Thomas R. Geballe2, Takeshi Oka3, and Benjamin J

Molecules: Probes of the Interstellar Medium

Can We Use Metastable Helium to Trace the Cosmic-Ray Ionization Rate?

CH+ and DIBs toward Herschel 36

Observation of H3+ in the Diffuse Interstellar Medium

LARGE PICTURE OF THE GALACTIC CENTER STUDIED BY H3+:

Can We Use Metastable Helium to Trace the Cosmic-Ray Ionization Rate?

Ubiquitous Argonium, ArH+, in the Interstellar Medium

Investigating the Cosmic-Ray Ionization Rate in the Galactic Interstellar Medium through Observations of H3+ Nick Indriolo,1 Ben McCall,1 Tom Geballe,2.

Diffuse Interstellar Bands: HD

Morphology of the Galactic center from the H3+ spectrum:

A New Catalog of Diffuse Interstellar Bands

International Symposium on Molecular Spectroscopy

Thermalization of interstellar CO

Presentation transcript:

CH +, CH, and CN Emission from the Red Rectangle Lewis M. Hobbs, Julie A. Thorburn, D. G. York, Takeshi Oka, Department of Astronomy and Astrophysics, the University of Chicago, Theodore P. Snow, Center for Astrophysics and Space Astronomy, University of Colorado, and John Barentine, New Mexico State University and Apache Point Observatory 59 th Ohio State University International Symposium on Molecular Spectroscopy WI02, 2:05 pm, June 23, 2004

1937 Birth of Molecular Astrophysics Theodore Dunham, Jr Walter Sydney Adams, T. Adams, Jr. PASP 49, 29 (1937) PAAS 9, 5 (1937) P. Swings & L. Rosenfeld, ApJ 86, 483 (1937) A.McKellar, PASP 52, 187, 312 (1940) 53, 233 (1941) CH CN Pub. Dom. Astroph. Obs. 7, 251 (1941) A. E. Douglas and G. Herzberg, ApJ 94, 381 (1941) CH +

Men’shchikov et al. A & A 393, 867 (2002)

Apache Point Observatory 3.5-meter 3,800–10,000 Å ; /  ~ 38,000 (8 km/s) S/N ~ nights, from Feb to Feb emission lines detected. 57 atomic, 76 molecular

CH + CH CN (0 - 0) 4236 Å Waelkens, van Winckel, Trams, Waters, A & A 256, L15 (1992) Balm and Jura, A & A 261, L25 (1992) Hall, Miles, Sarre, Fossey, Nature 358, 629 (1992) Bakkers, van Dishoeck, Waters, Schoenmaker, A & A 323, 469 (1997) (1  0) 3969 Å, (2-1) 4177 Å, (1-1) 4443 Å, (0- 1) 4793 Å, (1-2) 5029 Å, 52 lines up to J = Å 3 lines 3875 Å 24 lines up to N = 14

f = 5.45 × f = 1.08 × 10 -3

CH + (0 - 0) CH (0 - 0) CH + and CH are in different regions

CN up to N = 14

CH + Spontaneous emission time τ A → X τ ~ 1 μs Larsson, Siegbahn, CP 76, 175 (1983) v = 1→0 τ ~ 1 s Ornellas, Machado, JCP 84, 1296 (1985) J = 6→5 τ ~ 2.15 s Sun, Freed, JCP 88, 2659 (1988) μ A→X = 0.47 Debye μ 1→0 = Debye μ 0 = Debye B 0 = cm -1 Critical density n c ~ 10 8 cm -3 ! NGC 7072 up to J = 6 Cernicharo, Liu, Gonzalez-Alfonso, Cox, Barlow, Lim, Swinyard, ApJ 483, L65 (1997)

Collisional thermalization ?? What is the collision partner ?? H, H 2, (He), (e - )

The Enigma of CH + Chemistry Production C + + H → CH + + hν cm 3 s -1 C + + H 2 → CH + + H Endothermic by 0.4 eV C + H 3 + → CH + + H 2 Destruction CH + + H → C + + H 2 Exothermic by 0.4 eV CH + + H 2 → CH H Exothermic by 1.7 eV CH + + e - → C + H No way to thermalize CH + by collisions!!

Lambert, Danks, ApJ, 303, 401(1986) C + + H 2 * ↔ CH + + H v = eV CH + + H 2 → CH H k 1 n(C + )n(H 2 * ) = k -1 n(CH + )n(H) + k 2 n(CH + )n(H 2 ) The critical density should still be high > 10 8 cm -3

CN Spontaneous emission time τ A → X τ ~ 0.2 μs Bauschlicher, Langhoff, Taylor (1988) J = 14 → 13 τ ~ 12 s Langhoff, Bauschlicher(1989) μ 0 = Debye B 0 = cm -1 Critical density n c ~ 10 8 cm -3 !

Hertzprung-Russell Diagram R ~ 300R 