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2. Herschel/HIFI discovery of interstellar chloronium (H2Cl+)

Author

D. C. Lis, J. C. Pearson, D. A. Neufeld, P. Schilke, H. S. P. Müller, H. Gupta, T. A. Bell, C. Comito, T. G. Phillips, E. A. Bergin, C. Ceccarelli, P. F. Goldsmith, G. A. Blake, A. Bacmann, A. Baudry, M. Benedettini, A. Benz, J. Black, A. Boogert, S. Bottinelli, S. Cabrit, P. Caselli, A. Castets, E. Caux, J. Cernicharo, C. Codella, A. Coutens, N. Crimier, N. R. Crockett, F. Daniel, K. Demyk, C. Dominic, M.-L. Dubernet, M. Emprechtinger, P. Encrenaz, E. Falgarone, A. Fuente, M. Gerin, T. F. Giesen, J. R. Goicoechea, F. Helmich, P. Hennebelle, Th. Henning, E. Herbst, P. Hily-Blant, Å. Hjalmarson, D. Hollenbach, T. Jack, C. Joblin, D. Johnstone, C. Kahane, M. Kama, M. Kaufman, A. Klotz, W. D. Langer, B. Larsson, J. Le Bourlot, B. Lefloch, F. Le Petit, D. Li, R. Liseau, S. D. Lord, A. Lorenzani, S. Maret, P. G. Martin, G. J. Melnick, K. M. Menten, P. Morris, J. A. Murphy, Z. Nagy, B. Nisini, V. Ossenkopf, S. Pacheco, L. Pagani, B. Parise, M. Pérault, R. Plume, S.-L. Qin, E. Roueff, M. Salez, A. Sandqvist, P. Saraceno, S. Schlemmer, K. Schuster, R. Snell, J. Stutzki, A. Tielens, N. Trappe, F. F. S. van der Tak, M. H. D. van der Wiel, E. van Dishoeck, C. Vastel, S. Viti, V. Wakelam, A. Walters, S. Wang, F. Wyrowski, H. W. Yorke, S. Yu, J. Zmuidzinas, Y. Delorme, J.-P. Desbat, R. Güsten, J.-M. Krieg, B. Delforge, California Institute of Technology (CALTECH), foreign laboratories (FL), CERN [Genève], I. Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, Max Planck Institute for Radio Astronomy, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Astronomy [Ann Arbor], University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Optimisation de la Conception et Ingénierie de l'Environnement (LOCIE), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), FORMATION STELLAIRE 2010, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Indiana University Cyclotron Facility (IUCF), Indiana University [Bloomington], Indiana University System-Indiana University System, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), INAF - 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Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Consiglio Nazionale delle Ricerche (CNR), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Université Paris Diderot - Paris 7 (UPD7)-Université d'Artois (UA), Universiteit Leiden [Leiden], Astronomy, Kapteyn Astronomical Institute, Universität zu Köln, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Institut National Polytechnique de Grenoble (INPG), Smithsonian Institution-Harvard University [Cambridge], Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Faure, Alexandre, Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Experimental Physics, STAR-FORMING REGION, CHLORINE-BEARING MOLECULES, FOS: Physical sciences, Astrophysics, 01 natural sciences, COLOGNE DATABASE, ISM: abundances, 0103 physical sciences, Absorption (logic), HYDROGEN-CHLORIDE, 010306 general physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, NGC 6334 I, Physics, SPECTROSCOPY, astrochemistry, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Space observatory, ISM: molecules, SPIRAL ARM CLOUDS, Interstellar medium, submillimetre: ISM, molecular processes, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), GROUND-STATE, ISOTOPIC RATIO, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], SUBMILLIMETER, line: identification
Abstract

We report the first detection of chloronium, H$_2$Cl$^+$, in the interstellar medium, using the HIFI instrument aboard the \emph{Herschel} Space Observatory. The $2_{12}-1_{01}$ lines of ortho-H$_2^{35}$Cl$^+$ and ortho-H$_2^{37}$Cl$^+$ are detected in absorption towards NGC~6334I, and the $1_{11}-0_{00}$ transition of para-H$_2^{35}$Cl$^+$ is detected in absorption towards NGC~6334I and Sgr~B2(S). The H$_2$Cl$^+$ column densities are compared to those of the chemically-related species HCl. The derived HCl/H$_2$Cl$^+$ column density ratios, $\sim$1--10, are within the range predicted by models of diffuse and dense Photon Dominated Regions (PDRs). However, the observed H$_2$Cl$^+$ column densities, in excess of $10^{13}$~cm$^{-2}$, are significantly higher than the model predictions. Our observations demonstrate the outstanding spectroscopic capabilities of HIFI for detecting new interstellar molecules and providing key constraints for astrochemical models., Comment: Accepted for publication in A&A, HIFI Special Issue; 4 pages, 2 figures, 1 table

Published
2010
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3. Excitation and Abundance of C3 in star forming cores:Herschel/HIFI observations of the sight-lines to W31C and W49N

Author

B. Mookerjea, T. Giesen, J. Stutzki, J. Cernicharo, J. R. Goicoechea, M. De Luca, T. A. Bell, H. Gupta, M. Gerin, C. M. Persson, P. Sonnentrucker, Z. Makai, J. Black, F. Boulanger, A. Coutens, E. Dartois, P. Encrenaz, E. Falgarone, T. Geballe, B. Godard, P. F. Goldsmith, C. Gry, P. Hennebelle, E. Herbst, P. Hily-Blant, C. Joblin, M. Kaźmierczak, R. Kołos, J. Krełowski, D. C. Lis, J. Martin-Pintado, K. M. Menten, R. Monje, J. C. Pearson, M. Perault, T. G. Phillips, R. Plume, M. Salez, S. Schlemmer, M. Schmidt, D. Teyssier, C. Vastel, S. Yu, P. Dieleman, R. Güsten, C. E. Honingh, P. Morris, P. Roelfsema, R. Schieder, A. G. G. M. Tielens, and J. Zmuidzinas

Subjects
Mean kinetic temperature, FOS: Physical sciences, DUST, Astrophysics, HII-REGIONS, SPIRAL-ARM CLOUDS, Atmospheric radiative transfer codes, ABSORPTION, Radiative transfer, Continuum (set theory), IRC+10216, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, SPECTROSCOPY, Line-of-sight, INTERSTELLAR C-3, Triatomic molecule, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, ISM: molecules, H-II-REGIONS, G10.6-0.4, ISM: lines and bands, radiative transfer, Space and Planetary Science, TRANSLUCENT, Astrophysics of Galaxies (astro-ph.GA), ISM: individual objects: W49N, Atomic physics, ISM: individual objects: W31C, Ground state
Abstract

We present spectrally resolved observations of triatomic carbon (C3) in several ro-vibrational transitions between the vibrational ground state and the low-energy nu2 bending mode at frequencies between 1654-1897 GHz along the sight-lines to the submillimeter continuum sources W31C and W49N, using Herschel's HIFI instrument. We detect C3 in absorption arising from the warm envelope surrounding the hot core, as indicated by the velocity peak position and shape of the line profile. The sensitivity does not allow to detect C3 absorption due to diffuse foreground clouds. From the column densities of the rotational levels in the vibrational ground state probed by the absorption we derive a rotation temperature (T_rot) of ~50--70 K, which is a good measure of the kinetic temperature of the absorbing gas, as radiative transitions within the vibrational ground state are forbidden. It is also in good agreement with the dust temperatures for W31C and W49N. Applying the partition function correction based on the derived T_rot, we get column densities N(C3) ~7-9x10^{14} cm^{-2} and abundance x(C3)~10^{-8} with respect to H2. For W31C, using a radiative transfer model including far-infrared pumping by the dust continuum and a temperature gradient within the source along the line of sight we find that a model with x(C3)=10^{-8}, T_kin=30-50 K, N(C3)=1.5 10^{15} cm^{-2} fits the observations reasonably well and provides parameters in very good agreement with the simple excitation analysis., Accepted for publication in Astronomy and Astrophysics (HIFI first results issue)

Published
2010

5. Deuterium enhancement in H3+ in pre-stellar cores

Author

Charlotte, Vastel, T G, Phillips, P, Caselli, C, Ceccarelli, and L, Pagani

Abstract

Deuterium enhancement of monodeuterated species has been recognized for more than 30 years as a result of chemical fractionation that results from the difference in zero-point energies of deuterated and hydrogenated molecules. The key reaction is the deuteron exchange in the reaction between HD, the reservoir of deuterium in dark interstellar clouds, and the H3+ molecular ion, leading to the production of H2D+ molecule, and the low temperature in dark interstellar clouds favours this production. Furthermore, the presence of multiply deuterated species have incited our group to proceed further and consider the subsequent reaction of H2D+ with HD, leading to D2H+, which can further react with HD to produce D3+. In pre-stellar cores, where CO was found to be depleted, this production should be increased as CO would normally destroy H3+. The first model including D2H+ and D3+ predicted that these molecules should be as abundant as H2D+. The first detection of the D2H+ was made possible by the recent laboratory measurement for the frequency of the fundamental line of para-D2H+. Here, we present observations of H2D+ and D2H+ towards a sample of dark clouds and pre-stellar cores and show how the distribution of ortho-H2D+ (1(1,0)-1(1,1)) can trace the deuterium factory in pre-stellar cores. We also present how future instrumentation will improve our knowledge concerning the deuterium enhancement of H3+.

Published
2006

7. Topical therapies for glaucoma: what family physicians need to know

Author

P R, Lewis, T G, Phillips, and J W, Sassani

Subjects
Patient Education as Topic, Teaching Materials, Adrenergic beta-Antagonists, Prostaglandins, Synthetic, Humans, Glaucoma, Sympathomimetics, Carbonic Anhydrase Inhibitors, Family Practice, Miotics
Abstract

Medication classes historically used in the management of glaucoma include beta blockers, miotics, sympathomimetics and carbonic anhydrase inhibitors. Because topically applied medications are more site specific, they are preferred in the treatment of glaucoma. Compared with oral medications, topical agents are associated with a decreased incidence of systemic side effects. With topical administration, conjunctival and localized skin allergic reactions are relatively common, whereas severe reactions, including death, are rare. Recently introduced topical agents for glaucoma therapy include dorzolamide and brinzolamide, the first topical carbonic anhydrase inhibitors; brimonidine and apraclonidine, more ocular-specific alpha agonists; and latanoprost, a prostaglandin analog, which is a new class of glaucoma medication. Latanoprost has the unique side effect of increasing iris pigmentation. Like their predecessors, the newer agents lower intraocular pressure by a statistically significant degree. Preservation of visual field, the more substantial patient-oriented end point, continues to be studied.

Published
1999

8. The Self-Similar Structure of Molecular Clouds

Author

T. G. Phillips and E. Falgarone

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Molecular cloud, Gaussian, Interstellar cloud, Structure (category theory), Function (mathematics), Astrophysics, Molecular physics, symbols.namesake, symbols, Scale size, Emission spectrum, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

Information on the structure of the interstellar clouds is contained in both spatial maps and spectral profiles of molecular gas emission lines. In this paper, we show that non gaussian aspects of line profiles are found at all scales. This excess wing emission is shown to be generated in dense gas. From a study of the moments of the lines as a function of scale size, we deduce a break-down in the exactness of self-similarity in the hierarchical structure of the interstellar clouds.

Published
1990
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9. Detection of Submillimeter Lines of CO (0.65 mm) and H2O (0.79 mm)

Author

John Kwan, P. J. Huggins, and T. G. Phillips

Subjects
Telescope, Interstellar medium, Physics, Infrared astronomy, law, Molecular cloud, Brightness temperature, Orion Nebula, Kuiper Airborne Observatory, Astrophysics, Water vapor, law.invention
Abstract

The 91.5 cm telescope of NASA's Kuiper Airborne Observatory has been used, in conjunction with an InSb heterodyne receiver, to detect the J = 4-3 submillimeter transition of CO (461 GHz) and the 414−321 transition of H2O (380 GHz). The water emission was detected from the Orion “plateau” region.

Published
1980
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16. A Low Temperature Bolometer Heterodyne Receiver for Millimeter Wave Astronomy

Author

K. B. Jefferts and T. G. Phillips

Subjects
Physics, Noise temperature, Sideband, business.industry, Superheterodyne receiver, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, law.invention, Optics, law, Extremely high frequency, Antenna (radio), business, Instrumentation, Astrophysics::Galaxy Astrophysics, Microwave
Abstract

Liquid helium cooled InSb hot electron bolometers are used in a balanced mixer configuration as detectors for an imageless microwave receiver. The system is designed for mounting at the prime focus of the National Radio Astronomy Observatory (NRAO) 11 m antenna at Kitt Peak, Arizona, and is suitable for the study of rotational line spectra of interstellar gas molecules. Currently the operating frequency is in the 90–140 GHz band where the double sideband system noise temperature is 250 K.

Published
1973
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19. Determination of Exchange Interactions between CoupledCo2+Ions in MgF2by Far-Infrared Spectroscopy

Author

T. G. Phillips, E. Belorizky, and S. C. Ng

Subjects
Physics, symbols.namesake, Zeeman effect, Absorption spectroscopy, Exchange interaction, symbols, General Physics and Astronomy, Atomic physics, Hamiltonian (quantum mechanics), Spectroscopy, Magnetic dipole, Spectral line, Ion
Abstract

We report here a far-infrared spectroscopy experiment in which we observe absorption lines due to pairs and triads of magnetic ions. A crystal of Mg${\mathrm{F}}_{2}$ containing ${\mathrm{Co}}^{2+}$ ions substituted for ${\mathrm{Mg}}^{2+}$ is investigated and is found to show spectra due to next-nearest-neighbor ${\mathrm{Co}}^{2+}$ pairs, and also spectra due to groups of three ${\mathrm{Co}}^{2+}$ ions containing two next-nearest-neighbor bonds. The isotropic component of the pair exchange interaction is determined to be 9.8 ${\mathrm{cm}}^{\ensuremath{-}1}$, and the anisotropic components are also evaluated. Identification and evaluation are carried out with the information obtained from the Zeeman effect. The exchange and Zeeman Hamiltonian matrices for pairs and triads are developed using symmetry considerations, and it is shown that magnetic dipole transitions are allowed and are of the correct strength to account for the observed spectra. It is also shown that the next-nearest-neighbor exchange constant found from the spinwave dispersion curve for Co${\mathrm{F}}_{2}$ is in close agreement with the spectroscopic value found here.

Published
1969
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21. Microscopic origin of piezomagnetism of αFe2O3

Author

T. G. Phillips, Robert L. White, and R. L. Townsend

Subjects
Chemistry, Stress dependence, Materials Chemistry, Analytical chemistry, Thermodynamics, General Chemistry, Condensed Matter Physics, Piezomagnetism
Abstract

The piezomagnetism constants of αFe 2 O 3 are predicted from the stress dependence of the g-factor of Fe 3+ in Al 2 O 3 as measured in an EPR experiment at 26 Gc. The predicted constants [P 11 = 2.6 × 10 −5 , P 14 = 2.4 × 10 −4 (emu/g) / (kg/cm 2 )] are in acceptable agreement with the observed constants [P 11 = 3.6 × 10 −5 , P 14 = 6.4 × 10 −5 (emu/g) / (kg/cm 2 )].

Published
1968
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24. Radio telescope surface measurement with a sharing Fourier transform spectrometer

Author

E. Serabyn, C. R. Masson, and T. G. Phillips

Abstract

A broadband technique for measuring the surface accuracy of near millimeter wavelength radio telescopes has been developed. The near millimeter wavelength radiation from a distant astronomical point source is first focused by the telescope’s primary and secondary mirrors and then recollimated by an off-axis tertiary paraboloid for passage through a Twyman-Green interferometer. The end mirrors of the interferometer are situated so that the combination of tertiary paraboloid and beam splitter creates two identical images of the primary on their surfaces. By rotating one of the end mirrors out of its plane, the wavefronts are sheared with respect to each other, with the result that the focal plane pattern is scanned across the detector, where it interferes with the reference arm pattern. A 2-D Fourier transform of the focal plane data then yields the telescope’s aperture plane electric field. To separate the effects of different frequencies, the second end mirror is scanned. The resultant sheared interferograms, after being inverted, give the frequency dependence of the electric fields. Thus a 3-D Fourier transform of a grid of sheared interferograms simultaneously provides a measurement of the telescope surface at a number of frequencies.

Published
1988
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25. THE DETERMINATION OF POLYSACCHARIDES

Author

W. E. Tottingham, W. E. Loomis, J. J. Willaman, T. G. Phillips, and C. O. Appleman

Subjects
chemistry.chemical_classification, chemistry, Physiology, Genetics, Plant Science, Computational biology, Articles, Polysaccharide
Published
1927

26. THE DETERMINATION OF SOLUBLE CARBOHYDRATES*

Author

C. O. Appleman, J. J. Willaman, T. G. Phillips, W. E. Loomis, and W. E. Tottingham

Subjects
Text mining, Biochemistry, Physiology, business.industry, Chemistry, Genetics, Plant Science, Articles, business
Published
1927

27. Molecular Gas in the Nucleus of M82

Author

K. Y. Lo, K. W. Cheung, C. R. Masson, T. G. Phillips, N. Z. Scoville, and D. P. Woody

Abstract

7″-resolution CO (1-0) observations of M82 with the Owens Valley millimeter-wave interferometer have resolved 2 components of molecular gas in the central 1.5 arcmin of the galaxy: (1) a high plane of M82, and (2) shell-like or filamentary structures of molecular gas, with size-scale as large as 400 pc, extending most likely out of the plane of the galaxy.

Published
1987
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28. High Resolution Studies of Star-Forming Molecular Clouds

Author

A. I. Sargent, N. Z. Scoville, C. R. Masson, K. Y. Lo, and T. G. Phillips

Abstract

Observations of star formation sites in a number of molecular clouds, including NGC 7538, NGC 2071, Cepheus A and K3-50A, have been made using the Owens Valley millimeter wave interferometer. The measurements of 12CO, 13CO, CS and continuum emission are at resolutions of order 7″. Continuum emission at 2.7 mm is detected from all the cloud cores and, in general, the 12CO interferometer maps reveal the presence of high velocity, bipolar outflows within 10″ of these continuum sources. Thus, the origins of the outflows are readily identifiable; the flows themselves appear to remain collimated on scales of less than 1017 cm. The orientations of the flows are similar to those seen at lower resolution, except in Cepheus A, where the interferometer is capable of distinguishing between two outflows which are confused in single telescope maps.

Published
1987
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31. EPR Pressure Experiments on Rare Earths in Diamagnetic Garnets and the Single‐Ion Magnetostriction of Rare‐Earth Iron Garnets

Author

R. L. White and T. G. Phillips

Subjects
Crystal, Nuclear magnetic resonance, Condensed matter physics, Single ion, law, Chemistry, Rare earth, General Physics and Astronomy, Diamagnetism, Magnetostriction, Electron paramagnetic resonance, Spectral line, law.invention
Abstract

The EPR spectra of Gd3+, Yb3+, and Er3+ in diamagnetic garnet hosts have been measured as uniaxial pressures were applied to the crystal, and the parameters ∂gkl/∂eij and ∂Dkl/∂eij evaluated. A theory connecting these parameters with the magnetoelastic energy of the rare‐earth iron garnets has been developed, and the single‐ion contribution to the magnetostriction constants λ100 and λ111 of GdIG, YbIG, and ErIG calculated. In most cases the predicted single‐ion magnetostriction constants are of the same sign and within a factor of 2 of the observed magnetostriction constants at low temperatures. We conclude that single‐ion effects play a dominant role in the magnetoelastic behavior of the rare‐earth iron garnets.

Published
1967
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35. Detection of 13CO J=3-2 Emission from the Molecular Clouds OMG-1 and NGC2264

Author

P. M. Solomon, G. N. Blair, P. J. Huggins, and T. G. Phillips

Subjects
Physics, chemistry.chemical_classification, Isotope, Molecular cloud, Carbon-13, Astronomy and Astrophysics, Astrophysics, Spectral line, chemistry.chemical_compound, chemistry, Space and Planetary Science, Isotopes of carbon, Molecule, Compounds of carbon, Carbon monoxide
Abstract

We have made the first measurements of the 330 GHz J = 3--2 lines of /sup 13/CO in the molecular clouds OMC-1 and NGC 2264. Simple velocity gradient calculations can give a consistent description of the intensities of these lines, together with the available CO (J = 2--1) isotopic lines and the equivalent J = 1--0 transitions. They indicate fractional /sup 13/CO abundances similar to those found in dark clouds, but low values of the molecular hydrogen density, n(H/sub 2/)roughly-equal5 x 10/sup 3/ cm/sup -3/. The higher densities (approx.10/sup 5/ cm/sup -3/) indicated by other molecular observations of these clouds suggest either the presence of high density fragments within the clouds or that the simple analysis is not appropriate for the CO lines, and more complex models are required to explain all the observations.

Published
1981
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36. ANALYSIS OF THE HERSCHEL/HEXOS SPECTRAL SURVEY TOWARD ORION SOUTH: A MASSIVE PROTOSTELLAR ENVELOPE WITH STRONG EXTERNAL IRRADIATION.

Author

K. Tahani, R. Plume, D. Johnstone, K. M. Menten, H. S. P. Müller, V. Ossenkopf-Okada, F. F. S. van der Tak, E. A. Bergin, V. Tolls, T. G. Phillips, D. C. Lis, E. Caux, S. Cabrit, L. Pagani, J. R. Goicoechea, P. F. Goldsmith, and J. C. Pearson

Subjects
IRRADIATION, HETERODYNE detection, LOCAL thermodynamic equilibrium, KINEMATICS, MAGNETIC fields
Abstract

We present results from a comprehensive submillimeter spectral survey toward the source Orion South, based on data obtained with the Heterodyne Instrument for the Far-Infrared instrument on board the Herschel Space Observatory, covering the frequency range of 480 to 1900 GHz. We detect 685 spectral lines with signal-to-noise ratios (S/Ns) > 3σ, originating from 52 different molecular and atomic species. We model each of the detected species assuming conditions of Local Thermodynamic Equilibrium. This analysis provides an estimate of the physical conditions of Orion South (column density, temperature, source size, and VLSR). We find evidence for three different cloud components: a cool (Tex ∼ 20–40 K), spatially extended (>60″), and quiescent (ΔVFWHM ∼ 4 km s−1) component; a warmer (Tex ∼ 80–100 K), less spatially extended (∼30″), and dynamic (ΔVFWHM ∼ 8 km s−1) component, which is likely affected by embedded outflows; and a kinematically distinct region (Tex > 100 K; VLSR ∼ 8 km s−1), dominated by emission from species that trace ultraviolet irradiation, likely at the surface of the cloud. We find little evidence for the existence of a chemically distinct “hot-core” component, likely due to the small filling factor of the hot core or hot cores within the Herschel beam. We find that the chemical composition of the gas in the cooler, quiescent component of Orion South more closely resembles that of the quiescent ridge in Orion-KL. The gas in the warmer, dynamic component, however, more closely resembles that of the Compact Ridge and Plateau regions of Orion-KL, suggesting that higher temperatures and shocks also have an influence on the overall chemistry of Orion South. [ABSTRACT FROM AUTHOR]

Published
2016
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