Detection of interstellar oxidaniumyl: Abundant H2O+ towards the star-forming regions DR21, Sgr B2, and NGC6334

V. Ossenkopf; H. S. P. Mueller; D. C. Lis; P. Schilke; T. A. Bell; S. Bruderer; E. Bergin; C. Ceccarelli; C. Comito; J. Stutzki; A. Bacman; A. Baudry; A. O. Benz; M. Benedettini; O. Berne; G. Blake; A. Boogert; S. Bottinelli; F. Boulanger; S. Cabrit; P. Caselli; E. Caux; J. Cernicharo; C. Codella; A. Coutens; N. Crimier; N. R. Crockett; F. Daniel; K. Demyk; P. Dieleman; C. Dominik; M. L. Dubernet; M. Emprechtinger; P. Encrenaz; E. Falgarone; K. France; A. Fuente; M. Gerin; T. F. Giesen; A. M. di Giorgio; J. R. Goicoechea; P. F. Goldsmith; R. Guesten; A. Harris; F. Helmich; E. Herbst; P. Hily-Blant; K. Jacobs; T. Jacq; Ch. Joblin; D. Johnstone; C. Kahane; M. Kama; T. Klein; A. Klotz; C. Kramer; W. Langer; B. Lefloch; C. Leinz; A. Lorenzani; S. D. Lord; S. Maret; P. G. Martin; J. Martin-Pintado; C. McCoey; M. Melchior; G. J. Melnick; K. M. Menten; B. Mookerjea; P. Morris; J. A. Murphy; D. A. Neufeld; B. Nisini; S. Pacheco; L. Pagani; B. Parise; J. C. Pearson; M. Perault; T. G. Phillips; R. Plume; S. -L. Quin; R. Rizzo; M. Roellig; M. Salez; P. Saraceno; S. Schlemmer; R. Simon; K. Schuster; F. F. S. van der Tak; A. G. G. M. Tielens; D. Teyssier; N. Trappe; C. Vastel; S. Viti; V. Wakelam; A. Walters; S. Wang; N. Whyborn; M. van der Wiel; H. W. Yorke; S. Yu; J. Zmuidzinas

doi:10.1051/0004-6361/201014577

Detection of interstellar oxidaniumyl: Abundant H2O+ towards the star-forming regions DR21, Sgr B2, and NGC6334

V. Ossenkopf^*, H. S. P. Mueller, D. C. Lis, P. Schilke, T. A. Bell, S. Bruderer, E. Bergin, C. Ceccarelli, C. Comito, J. Stutzki, A. Bacman, A. Baudry, A. O. Benz, M. Benedettini, O. Berne, G. Blake, A. Boogert, S. Bottinelli, F. Boulanger, S. CabritP. Caselli, E. Caux, J. Cernicharo, C. Codella, A. Coutens, N. Crimier, N. R. Crockett, F. Daniel, K. Demyk, P. Dieleman, C. Dominik, M. L. Dubernet, M. Emprechtinger, P. Encrenaz, E. Falgarone, K. France, A. Fuente, M. Gerin, T. F. Giesen, A. M. di Giorgio, J. R. Goicoechea, P. F. Goldsmith, R. Guesten, A. Harris, F. Helmich, E. Herbst, P. Hily-Blant, K. Jacobs, T. Jacq, Ch. Joblin, D. Johnstone, C. Kahane, M. Kama, T. Klein, A. Klotz, C. Kramer, W. Langer, B. Lefloch, C. Leinz, A. Lorenzani, S. D. Lord, S. Maret, P. G. Martin, J. Martin-Pintado, C. McCoey, M. Melchior, G. J. Melnick, K. M. Menten, B. Mookerjea, P. Morris, J. A. Murphy, D. A. Neufeld, B. Nisini, S. Pacheco, L. Pagani, B. Parise, J. C. Pearson, M. Perault, T. G. Phillips, R. Plume, S. -L. Quin, R. Rizzo, M. Roellig, M. Salez, P. Saraceno, S. Schlemmer, R. Simon, K. Schuster, F. F. S. van der Tak, A. G. G. M. Tielens, D. Teyssier, N. Trappe, C. Vastel, S. Viti, V. Wakelam, A. Walters, S. Wang, N. Whyborn, M. van der Wiel, H. W. Yorke, S. Yu, J. Zmuidzinas

^*Corresponding author for this work

Astronomy

Research output: Contribution to journal › Article › Academic › peer-review

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Abstract

Aims. We identify a prominent absorption feature at 1115 GHz, detected in first HIFI spectra towards high-mass star-forming regions, and interpret its astrophysical origin.

Methods. The characteristic hyperfine pattern of the H2O+ ground-state rotational transition, and the lack of other known low-energy transitions in this frequency range, identifies the feature as H2O+ absorption against the dust continuum background and allows us to derive the velocity profile of the absorbing gas. By comparing this velocity profile with velocity profiles of other tracers in the DR21 star-forming region, we constrain the frequency of the transition and the conditions for its formation.

Results. In DR21, the velocity distribution of H2O+ matches that of the [C II] line at 158 mu m and of OH cm-wave absorption, both stemming from the hot and dense clump surfaces facing the H II-region and dynamically affected by the blister outflow. Diffuse foreground gas dominates the absorption towards Sgr B2. The integrated intensity of the absorption line allows us to derive lower limits to the H2O+ column density of 7.2 x 10(12) cm(-2) in NGC 6334, 2.3 x 10(13) cm(-2) in DR21, and 1.1 x 10(15) cm(-2) in Sgr B2.

Original language	English
Article number	L111
Number of pages	5
Journal	Astronomy & astrophysics
Volume	518
DOIs	https://doi.org/10.1051/0004-6361/201014577
Publication status	Published - 2010

Keywords

astrochemistry
line: identification
molecular data
ISM: abundances
ISM: molecules
ISM: clouds
LASER MAGNETIC-RESONANCE
ROTATIONAL SPECTRUM
COMET-KOHOUTEK
GROUND-STATE
SPECTROSCOPY
ABSORPTION
OH
IDENTIFICATION
EMISSION
NGC-6334

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Ossenkopf, V., Mueller, H. S. P., Lis, D. C., Schilke, P., Bell, T. A., Bruderer, S., Bergin, E., Ceccarelli, C., Comito, C., Stutzki, J., Bacman, A., Baudry, A., Benz, A. O., Benedettini, M., Berne, O., Blake, G., Boogert, A., Bottinelli, S., Boulanger, F., ... Zmuidzinas, J. (2010). Detection of interstellar oxidaniumyl: Abundant H2O+ towards the star-forming regions DR21, Sgr B2, and NGC6334. Astronomy & astrophysics, 518, Article L111. https://doi.org/10.1051/0004-6361/201014577

@article{4087cbf630064e67aebb582f969c84db,

title = "Detection of interstellar oxidaniumyl: Abundant H2O+ towards the star-forming regions DR21, Sgr B2, and NGC6334",

abstract = "Aims. We identify a prominent absorption feature at 1115 GHz, detected in first HIFI spectra towards high-mass star-forming regions, and interpret its astrophysical origin.Methods. The characteristic hyperfine pattern of the H2O+ ground-state rotational transition, and the lack of other known low-energy transitions in this frequency range, identifies the feature as H2O+ absorption against the dust continuum background and allows us to derive the velocity profile of the absorbing gas. By comparing this velocity profile with velocity profiles of other tracers in the DR21 star-forming region, we constrain the frequency of the transition and the conditions for its formation.Results. In DR21, the velocity distribution of H2O+ matches that of the [C II] line at 158 mu m and of OH cm-wave absorption, both stemming from the hot and dense clump surfaces facing the H II-region and dynamically affected by the blister outflow. Diffuse foreground gas dominates the absorption towards Sgr B2. The integrated intensity of the absorption line allows us to derive lower limits to the H2O+ column density of 7.2 x 10(12) cm(-2) in NGC 6334, 2.3 x 10(13) cm(-2) in DR21, and 1.1 x 10(15) cm(-2) in Sgr B2.",

keywords = "astrochemistry, line: identification, molecular data, ISM: abundances, ISM: molecules, ISM: clouds, LASER MAGNETIC-RESONANCE, ROTATIONAL SPECTRUM, COMET-KOHOUTEK, GROUND-STATE, SPECTROSCOPY, ABSORPTION, OH, IDENTIFICATION, EMISSION, NGC-6334",

author = "V. Ossenkopf and Mueller, {H. S. P.} and Lis, {D. C.} and P. Schilke and Bell, {T. A.} and S. Bruderer and E. Bergin and C. Ceccarelli and C. Comito and J. Stutzki and A. Bacman and A. Baudry and Benz, {A. O.} and M. Benedettini and O. Berne and G. Blake and A. Boogert and S. Bottinelli and F. Boulanger and S. Cabrit and P. Caselli and E. Caux and J. Cernicharo and C. Codella and A. Coutens and N. Crimier and Crockett, {N. R.} and F. Daniel and K. Demyk and P. Dieleman and C. Dominik and Dubernet, {M. L.} and M. Emprechtinger and P. Encrenaz and E. Falgarone and K. France and A. Fuente and M. Gerin and Giesen, {T. F.} and {di Giorgio}, {A. M.} and Goicoechea, {J. R.} and Goldsmith, {P. F.} and R. Guesten and A. Harris and F. Helmich and E. Herbst and P. Hily-Blant and K. Jacobs and T. Jacq and Ch. Joblin and D. Johnstone and C. Kahane and M. Kama and T. Klein and A. Klotz and C. Kramer and W. Langer and B. Lefloch and C. Leinz and A. Lorenzani and Lord, {S. D.} and S. Maret and Martin, {P. G.} and J. Martin-Pintado and C. McCoey and M. Melchior and Melnick, {G. J.} and Menten, {K. M.} and B. Mookerjea and P. Morris and Murphy, {J. A.} and Neufeld, {D. A.} and B. Nisini and S. Pacheco and L. Pagani and B. Parise and Pearson, {J. C.} and M. Perault and Phillips, {T. G.} and R. Plume and Quin, {S. -L.} and R. Rizzo and M. Roellig and M. Salez and P. Saraceno and S. Schlemmer and R. Simon and K. Schuster and {van der Tak}, {F. F. S.} and Tielens, {A. G. G. M.} and D. Teyssier and N. Trappe and C. Vastel and S. Viti and V. Wakelam and A. Walters and S. Wang and N. Whyborn and {van der Wiel}, M. and Yorke, {H. W.} and S. Yu and J. Zmuidzinas",

year = "2010",

doi = "10.1051/0004-6361/201014577",

language = "English",

volume = "518",

journal = "Astronomy & astrophysics",

issn = "0004-6361",

publisher = " EDP Sciences",

}

Ossenkopf, V, Mueller, HSP, Lis, DC, Schilke, P, Bell, TA, Bruderer, S, Bergin, E, Ceccarelli, C, Comito, C, Stutzki, J, Bacman, A, Baudry, A, Benz, AO, Benedettini, M, Berne, O, Blake, G, Boogert, A, Bottinelli, S, Boulanger, F, Cabrit, S, Caselli, P, Caux, E, Cernicharo, J, Codella, C, Coutens, A, Crimier, N, Crockett, NR, Daniel, F, Demyk, K, Dieleman, P, Dominik, C, Dubernet, ML, Emprechtinger, M, Encrenaz, P, Falgarone, E, France, K, Fuente, A, Gerin, M, Giesen, TF, di Giorgio, AM, Goicoechea, JR, Goldsmith, PF, Guesten, R, Harris, A, Helmich, F, Herbst, E, Hily-Blant, P, Jacobs, K, Jacq, T, Joblin, C, Johnstone, D, Kahane, C, Kama, M, Klein, T, Klotz, A, Kramer, C, Langer, W, Lefloch, B, Leinz, C, Lorenzani, A, Lord, SD, Maret, S, Martin, PG, Martin-Pintado, J, McCoey, C, Melchior, M, Melnick, GJ, Menten, KM, Mookerjea, B, Morris, P, Murphy, JA, Neufeld, DA, Nisini, B, Pacheco, S, Pagani, L, Parise, B, Pearson, JC, Perault, M, Phillips, TG, Plume, R, Quin, S-L, Rizzo, R, Roellig, M, Salez, M, Saraceno, P, Schlemmer, S, Simon, R, Schuster, K, van der Tak, FFS, Tielens, AGGM, Teyssier, D, Trappe, N, Vastel, C, Viti, S, Wakelam, V, Walters, A, Wang, S, Whyborn, N, van der Wiel, M, Yorke, HW, Yu, S & Zmuidzinas, J 2010, 'Detection of interstellar oxidaniumyl: Abundant H2O+ towards the star-forming regions DR21, Sgr B2, and NGC6334', Astronomy & astrophysics, vol. 518, L111. https://doi.org/10.1051/0004-6361/201014577

TY - JOUR

T1 - Detection of interstellar oxidaniumyl

T2 - Abundant H2O+ towards the star-forming regions DR21, Sgr B2, and NGC6334

AU - Ossenkopf, V.

AU - Mueller, H. S. P.

AU - Lis, D. C.

AU - Schilke, P.

AU - Bell, T. A.

AU - Bruderer, S.

AU - Bergin, E.

AU - Ceccarelli, C.

AU - Comito, C.

AU - Stutzki, J.

AU - Bacman, A.

AU - Baudry, A.

AU - Benz, A. O.

AU - Benedettini, M.

AU - Berne, O.

AU - Blake, G.

AU - Boogert, A.

AU - Bottinelli, S.

AU - Boulanger, F.

AU - Cabrit, S.

AU - Caselli, P.

AU - Caux, E.

AU - Cernicharo, J.

AU - Codella, C.

AU - Coutens, A.

AU - Crimier, N.

AU - Crockett, N. R.

AU - Daniel, F.

AU - Demyk, K.

AU - Dieleman, P.

AU - Dominik, C.

AU - Dubernet, M. L.

AU - Emprechtinger, M.

AU - Encrenaz, P.

AU - Falgarone, E.

AU - France, K.

AU - Fuente, A.

AU - Gerin, M.

AU - Giesen, T. F.

AU - di Giorgio, A. M.

AU - Goicoechea, J. R.

AU - Goldsmith, P. F.

AU - Guesten, R.

AU - Harris, A.

AU - Helmich, F.

AU - Herbst, E.

AU - Hily-Blant, P.

AU - Jacobs, K.

AU - Jacq, T.

AU - Joblin, Ch.

AU - Johnstone, D.

AU - Kahane, C.

AU - Kama, M.

AU - Klein, T.

AU - Klotz, A.

AU - Kramer, C.

AU - Langer, W.

AU - Lefloch, B.

AU - Leinz, C.

AU - Lorenzani, A.

AU - Lord, S. D.

AU - Maret, S.

AU - Martin, P. G.

AU - Martin-Pintado, J.

AU - McCoey, C.

AU - Melchior, M.

AU - Melnick, G. J.

AU - Menten, K. M.

AU - Mookerjea, B.

AU - Morris, P.

AU - Murphy, J. A.

AU - Neufeld, D. A.

AU - Nisini, B.

AU - Pacheco, S.

AU - Pagani, L.

AU - Parise, B.

AU - Pearson, J. C.

AU - Perault, M.

AU - Phillips, T. G.

AU - Plume, R.

AU - Quin, S. -L.

AU - Rizzo, R.

AU - Roellig, M.

AU - Salez, M.

AU - Saraceno, P.

AU - Schlemmer, S.

AU - Simon, R.

AU - Schuster, K.

AU - van der Tak, F. F. S.

AU - Tielens, A. G. G. M.

AU - Teyssier, D.

AU - Trappe, N.

AU - Vastel, C.

AU - Viti, S.

AU - Wakelam, V.

AU - Walters, A.

AU - Wang, S.

AU - Whyborn, N.

AU - van der Wiel, M.

AU - Yorke, H. W.

AU - Yu, S.

AU - Zmuidzinas, J.

PY - 2010

Y1 - 2010

N2 - Aims. We identify a prominent absorption feature at 1115 GHz, detected in first HIFI spectra towards high-mass star-forming regions, and interpret its astrophysical origin.Methods. The characteristic hyperfine pattern of the H2O+ ground-state rotational transition, and the lack of other known low-energy transitions in this frequency range, identifies the feature as H2O+ absorption against the dust continuum background and allows us to derive the velocity profile of the absorbing gas. By comparing this velocity profile with velocity profiles of other tracers in the DR21 star-forming region, we constrain the frequency of the transition and the conditions for its formation.Results. In DR21, the velocity distribution of H2O+ matches that of the [C II] line at 158 mu m and of OH cm-wave absorption, both stemming from the hot and dense clump surfaces facing the H II-region and dynamically affected by the blister outflow. Diffuse foreground gas dominates the absorption towards Sgr B2. The integrated intensity of the absorption line allows us to derive lower limits to the H2O+ column density of 7.2 x 10(12) cm(-2) in NGC 6334, 2.3 x 10(13) cm(-2) in DR21, and 1.1 x 10(15) cm(-2) in Sgr B2.

AB - Aims. We identify a prominent absorption feature at 1115 GHz, detected in first HIFI spectra towards high-mass star-forming regions, and interpret its astrophysical origin.Methods. The characteristic hyperfine pattern of the H2O+ ground-state rotational transition, and the lack of other known low-energy transitions in this frequency range, identifies the feature as H2O+ absorption against the dust continuum background and allows us to derive the velocity profile of the absorbing gas. By comparing this velocity profile with velocity profiles of other tracers in the DR21 star-forming region, we constrain the frequency of the transition and the conditions for its formation.Results. In DR21, the velocity distribution of H2O+ matches that of the [C II] line at 158 mu m and of OH cm-wave absorption, both stemming from the hot and dense clump surfaces facing the H II-region and dynamically affected by the blister outflow. Diffuse foreground gas dominates the absorption towards Sgr B2. The integrated intensity of the absorption line allows us to derive lower limits to the H2O+ column density of 7.2 x 10(12) cm(-2) in NGC 6334, 2.3 x 10(13) cm(-2) in DR21, and 1.1 x 10(15) cm(-2) in Sgr B2.

KW - astrochemistry

KW - line: identification

KW - molecular data

KW - ISM: abundances

KW - ISM: molecules

KW - ISM: clouds

KW - LASER MAGNETIC-RESONANCE

KW - ROTATIONAL SPECTRUM

KW - COMET-KOHOUTEK

KW - GROUND-STATE

KW - SPECTROSCOPY

KW - ABSORPTION

KW - OH

KW - IDENTIFICATION

KW - EMISSION

KW - NGC-6334

U2 - 10.1051/0004-6361/201014577

DO - 10.1051/0004-6361/201014577

M3 - Article

SN - 0004-6361

VL - 518

JO - Astronomy & astrophysics

JF - Astronomy & astrophysics

M1 - L111

ER -