Paule Sonnentrucker

Space Telescope Science Institute

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D. E. Welty

Space Telescope Science Institute

David A. Neufeld

Johns Hopkins University

Donald G. York

University of Chicago

Cristina Oliveira

IPO Porto

Julia Román-Duval

Space Telescope Science Institute

S. D. Friedman

Corewell Health

Theodore P. Snow

University of Colorado Boulder

David J. Sahnow

Space Telescope Science Institute

Maryvonne Gérin

Laboratoire d’Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères

Charles Proffitt

Space Telescope Science Institute

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Space Telescope Science Institute

Centre National de la Recherche Scientifique

Max Planck Society

California Institute of Technology

Johns Hopkins University

Jet Propulsion Laboratory

University of Cologne

Goddard Space Flight Center

Sorbonne Université

Max Planck Institute for Radio Astronomy

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Interstellar CH absorption in the diffuse interstellar medium along the sight-lines to G10.6–0.4 (W31C), W49N, and W51

Astronomy and Astrophysics (2010)

Maryvonne Gérin M. De Luca J. R. Goicoechea Eric Herbst É. Falgarone

We report the detection of the ground state N,J = 1,3/2 1,1/2 doublet of the methylidyne radical CH at ~532 GHz and ~536 GHz with the Herschel/HIFI instrument along the sight-line to the massive star-forming regions G10.6–0.4 (W31C), W49N, and W51. While the molecular cores associated with these massive star-forming regions show emission lines, clouds in the diffuse interstellar medium are detected in absorption against the strong submillimeter background. The combination of hyperfine structure with emission and absorption results in complex profiles, with overlap of the different hyperfine components. The opacities of most of the CH absorption features are linearly correlated with those of CCH, CN, and HCO^{+^{in the same velocity intervals. In specific narrow velocity intervals, the opacities of CN and HCO^{+^{deviate from the mean trends, giving rise to more opaque absorption features. We propose that CCH can be used as another tracer of the molecular gas in the absence of better tracers, with [CCH]/[ H_{2_{] ~ 3.2±1.1×10^{-8^{. The observed [CN]/[CH], [CCH]/[CH] abundance ratios suggest that the bulk of the diffuse matter along the lines of sight has gas densities n_{H_{= n(H) + 2n(H_{2_{) ranging between 100 and 1000 cm^{-3^.}}}}}}}}}}}}}

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10.1051/0004-6361/201015115

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Citations (92)

Tiny-scale molecular structures in the Magellanic Clouds

Astronomy and Astrophysics (2004)

M. André Franck Le Petit Paule Sonnentrucker R. Ferlet E. Roueff

come from teaching and research institutions in France or abroad, or from public or private research centers.L'archive ouverte pluridisciplinaire

10.1051/0004-6361:20035903

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Citations (31)

UNCOVERING OBSCURED ACTIVE GALACTIC NUCLEI IN HOMOGENEOUSLY SELECTED SAMPLES OF SEYFERT 2 GALAXIES

The Astrophysical Journal (2011)

Stephanie LaMassa Timothy M. Heckman A. Ptak Lucimara P. Martins Vivienne Wild

We have analyzed archival Chandra and XMM-Newton data for two nearly complete homogeneously selected samples of type 2 Seyfert galaxies (Sy2s). These samples were selected based on intrinsic active galactic nuclei (AGNs) flux proxies: a mid-infrared (MIR) sample from the original IRAS 12 μm survey and an optical ([O iii]λ 5007 flux limited) sample from the Sloan Digital Sky Survey, providing a total of 45 Sy2s. As the MIR and [O iii] fluxes are largely unaffected by AGN obscuration, these samples can present an unbiased estimate of the Compton-thick (column density NH>1024 cm−2) subpopulation. We find that the majority of this combined sample are likely heavily obscured, as evidenced by the 2–10 keV X-ray attenuation (normalized by intrinsic flux diagnostics) and the large Fe Kα equivalent widths (several hundred eV to over 1 keV). A wide range of these obscuration diagnostics is present, showing a continuum of column densities, rather than a clear segregation into Compton-thick and Compton-thin sub-populations. We find that, in several instances, the fitted column densities severely underrepresent the attenuation implied by these obscuration diagnostics, indicating that simple X-ray models may not always recover the intrinsic absorption. We compared AGNs and host galaxy properties, such as intrinsic luminosity, central black hole mass, accretion rate, and star formation rate with obscuration diagnostics. No convincing evidence exists to link obscured sources with unique host galaxy populations from their less absorbed counterparts. Finally, we estimate that a majority of these Seyfert 2s will be detectable in the 10–40 keV range by the future NuSTAR mission, which would confirm whether these heavily absorbed sources are indeed Compton-thick.

10.1088/0004-637x/729/1/52

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A NEW ATLAS OF THE DIFFUSE INTERSTELLAR BANDS: HD 183143

65th International Symposium On Molecular Spectroscopy (2010)

Lewis M. Hobbs Donald G. York J. A. Thorburn Theodore P. Snow Michael Bishof

Author Institution: University of Chicago, Yerkes Observatory, Williams Bay, WI 53191; University of Chicago, Chicago, IL 60637; Carthage College, Kenosha, WI 53140; University of Colorado, Boulder, CO 80309; University of Chicago, Chicago, IL 60637; Space Telescope Science Institute, Baltimore, MD 21218; University of Illinois at Urbana-Champaign, Urbana, IL 61801; University of Chicago, Chicago, IL 60637; Embry-Riddle Aeronautical University, Prescott, AZ 86301; Johns Hopkins University, Baltimore, MD 21218; University of Illinois at Urbana-Champaign, Urbana, IL 61801

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STUDIES OF THE DIFFUSE INTERSTELLAR BANDS. IV. THE NEARLY PERFECT CORRELATION BETWEEN λλ6196.0 AND 6613.6

The Astrophysical Journal (2009)

Benjamin J. McCall Meredith M. Drosback J. A. Thorburn Donald G. York S. D. Friedman

In a sample of 114 diffuse cloud sightlines spanning a wide range of interstellar environments, we find the equivalent widths of the diffuse interstellar bands (DIBs) λ6196.0 and λ6613.6 to be extremely well correlated, with a correlation coefficient of 0.986.A maximum likelihood functional relationship analysis shows that the observations are consistent with a perfect correlation if the observational errors, which are dominated by continuum placement and other systematics such as interfering lines, have been underestimated by a factor of 2. The quality of this correlation far exceeds other previously studied correlations, such as that between the λ5780.5 DIB and either the color excess or the atomic hydrogen column density.The unusually tight correlation between these two DIBs would seem to suggest that they might represent the first pair of DIBs known to be due to the same molecular carrier.However, further theoretical work will be required to determine whether the different linewidths and band shapes of these two DIBs can be consistent with a common carrier.If the two DIBs do not in fact share the same molecular carrier, their two carriers must be chemically very closely related.

10.1088/0004-637x/708/2/1628

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Citations (86)

High resolution spectroscopy of HD 207538 from Far-UV (FUSE) to Visible (SARG-TNG)

Astronomy and Astrophysics (2003)

G. Catanzaro M. André F. Leone Paule Sonnentrucker

We present a detailed study of the suspected Chemically Peculiar star HD 207538 based on high resolution spectroscopy in the far Ultraviolet (1000–3350 Å) and visible (4600–7000 Å) ranges. The stellar abundance synthesis analysis was performed by using Kurucz's codes ATLAS9 and SYNTHE to compute the atmospheric model and the synthetic spectrum respectively. Observations were obtained with the Far Ultraviolet Spectroscopic Explorer, the International Ultraviolet Explorer satellites whereas the optical spectrum was collected with the ground-based Telescopio Nazionale Galileo telescope. With our analysis we refine the value of the rotational velocity to km s-1 and the microturbulence velocity to km s-1. The stellar abundances inferred in this study show that C, N, O, Al, Si, P, S and Mn are compatible with the standard solar abundances, within the experimental errors. On the other hand, Fe, Ni and Zn are definitively underabundant. We also show that the helium content is comparable to the typical abundance of B-type stars. Because this spectrum is rich in stellar and interstellar features, we computed simultaneously a synthetic spectrum of the stellar and interstellar lines in order to disentangle the different absorption contributions. We thus also determined the column densities of several interstellar elements (Feii, Ni, Pii, Hi, H2, HD, CO, Cli and Ari) present in the gas in front of the star. Although several components are present along this sightline, our results suggest the presence of some translucent interstellar gas among the diffuse components. With this work, we demonstrate that it is possible to perform a stellar spectroscopic analysis from the far-UV to visible spectral range, with consistent results in both ranges within errors, based on one single atmosphere model.

Microturbulence

Far ultraviolet

Ultraviolet

Line (geometry)

Radial velocity

10.1051/0004-6361:20030507

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Citations (3)

New estimates of ionization potentials of four DIB molecular carriers

Advances in Space Research (1999)

Paule Sonnentrucker B. H. Foing P. Ehrenfreund

Angstrom

10.1016/s0273-1177(99)00094-0

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Citations (2)

FUSE calibration pipeline version 3.0

Benoît Godard W. V. Dixon J. Dupuis R. D. Robinson David J. Sahnow

Fuse (electrical)

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Polarisation observations of VY Canis Majoris H₂O 5₃₂–4₄₁620.701 GHz maser emission with HIFI

Astronomy and Astrophysics (2010)

Martin Harwit Martin Houde Paule Sonnentrucker A. C. A. Boogert J. Cernicharo

CONTEXT: Water vapour maser emission from evolved oxygen-rich stars remains poorly understood. Additional observations, including polarisation studies and simultaneous observation of different maser transitions may ultimately lead to greater insight. AIMS: We have aimed to elucidate the nature and structure of the VY CMa water vapour masers in part by observationally testing a theoretical prediction of the relative strengths of the 620.701 GHz and the 22.235 GHz maser components of ortho water vapour. METHODS: In its high-resolution mode (HRS) the Herschel Heterodyne Instrument for the Infrared (HIFI) offers a frequency resolution of 0.125 MHz, corresponding to a line-of-sight velocity of 0.06 km/s, which we employed to obtain the strength and linear polarisation of maser spikes in the spectrum of VY CMa at 620.701 GHz. Simultaneous ground based observations of the 22.235 GHz maser with the Max-Planck-Institut f\"ur Radioastronomie 100-meter telescope at Effelsberg, provided a ratio of 620.701 GHz to 22.235 GHz emission. RESULTS:We report the first astronomical detection to date of water vapour maser emission at 620.701 GHz. In VY CMa both the 620.701 and the 22.235 GHz polarisation are weak. At 620.701 GHz the maser peaks are superposed on what appears to be a broad emission component, jointly ejected asymmetrically from the star. We observed the 620.701 GHz emission at two epochs 21 days apart, both to measure the potential direction of linearly polarised maser components and to obtain a measure of the longevity of these components. Although we do not detect significant polarisation levels in the core of the line, they rise up to approximately 6% in its wings.

10.1051/0004-6361/201015042

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Interstellar OH⁺, H₂O⁺and H₃O⁺along the sight-line to G10.6–0.4

Astronomy and Astrophysics (2010)

M. Gerin M. De Luca J. H. Black J. R. Goicoechea Eric Herbst

We report the detection of absorption lines by the reactive ions OH^{+^{, H_{2_{O^{+^{and H_{3_{O^{+^{along the line of sight to the submillimeter continuum source G10.6–0.4 (W31C). We used the Herschel HIFI instrument in dual beam switch mode to observe the ground state rotational transitions of OH^{+^{at 971 GHz, H_{2_{O^{+^{at 1115 and 607 GHz, and H_{3_{O^{+^{at 984 GHz. The resultant spectra show deep absorption over a broad velocity range that originates in the interstellar matter along the line of sight to G10.6–0.4 as well as in the molecular gas directly associated with that source. The OH^{+^{spectrum reaches saturation over most velocities corresponding to the foreground gas, while the opacity of the H_{2_{O^{+^{lines remains lower than 1 in the same velocity range, and the H_{3_{O^{+^{line shows only weak absorption. For LSR velocities between 7 and 50 km s^{-1^{we estimate total column densities of N(OH^{+^{) ≥ 2.5 × 10^{14^{cm^{-2^{, N(H_{2_{O^{+^{) ~6 × 10^{13^{cm^{-2^{and N(H_{3_{O^{+^{) ~4.0 × 10^{13^{cm^{-2^{. These detections confirm the role of O^{+^{and OH^{+^{in initiating the oxygen chemistry in diffuse molecular gas and strengthen our understanding of the gas phase production of water. The high ratio of the OH^{+^{by the H_{2_{O^{+^{column density implies that these species predominantly trace low-density gas with a small fraction of hydrogen in molecular form.}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}

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10.1051/0004-6361/201014576

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Citations (174)