B. Parise

Cardiff University

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Co-Authors

E. F. van Dishoeck

Leiden University

C. Codella

Arcetri Astrophysical Observatory

D. C. Lis

California Institute of Technology

B. Nisini

Astronomical Observatory of Rome

J. Cernicharo

Consejo Superior de Investigaciones Científicas

A. Baudry

Université de Bordeaux

L. E. Kristensen

Frederiksberg Hospital

J. K. Jørgensen

Natural History Museum Aarhus

R. Plume

University of Calgary

J. R. Goicoechea

Consejo Superior de Investigaciones Científicas

Cooperative Institutions

Centre National de la Recherche Scientifique

Max Planck Society

Max Planck Institute for Radio Astronomy

SRON Netherlands Institute for Space Research

Institut de Planétologie et d'Astrophysique de Grenoble

California Institute of Technology

Leiden University

Université de Bordeaux

University of Cologne

Observatoire de Paris

Author Statistics

Papers

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Deuterated methanol in Orion BN/KL

Astronomy and Astrophysics (2012)

T.-C. Peng D. Despois N. Brouillet B. Parise A. Baudry

Deuterated molecules have been detected and studied toward Orion BN/KL in the past decades, mostly with single-dish telescopes. However, high angular resolution data are critical not only for interpreting the spatial distribution of the deuteration ratio but also for understanding this complex region in terms of cloud evolution involving star-forming activities and stellar feedbacks. We present here the first high angular resolution (1.8 arcsec \times 0.8 arcsec) images of deuterated methanol CH2DOH in Orion BN/KL observed with the IRAM Plateau de Bure Interferometer from 1999 to 2007 in the 1 to 3 mm range. Six CH2DOH lines were detected around 105.8, 223.5, and 225.9 GHz. In addition, three E-type methanol lines around 101-102 GHz were detected and were used to derive the corresponding CH3OH rotational temperatures and column densities toward different regions across Orion BN/KL. The strongest CH2DOH and CH3OH emissions come from the Hot Core southwest region with an LSR velocity of about 8 km/s. We derive [CH2DOH]/[CH3OH] abundance ratios of 0.8-1.3\times10^-3 toward three CH2DOH emission peaks. A new transition of CH3OD was detected at 226.2 GHz for the first time in the interstellar medium. Its distribution is similar to that of CH2DOH. Besides, we find that the [CH2DOH]/[CH3OD] abundance ratios are lower than unity in the central part of BN/KL. Furthermore, the HDO 3(1,2)-2(2,1) line at 225.9 GHz was detected and its emission distribution shows a shift of a few arcseconds with respect to the deuterated methanol emission that likely results from different excitation effects. The deuteration ratios derived along Orion BN/KL are not markedly different from one clump to another. However, various processes such as slow heating due to ongoing star formation, heating by luminous infrared sources, or heating by shocks could be competing to explain some local differences observed for these ratios.

Orion Nebula

Line (geometry)

10.1051/0004-6361/201118310

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Citations (48)

Chamaeleon I 870um sources (Belloche+, 2011)

HAL (Le Centre pour la Communication Scientifique Directe) (2011)

А. Беллоче F. Schüller B. Parise Paulo André J. Hatchell

Table 2 lists the sources extracted with GAUSSCLUMPS from the filtered 870 micron continuum emission map of Chamaeleon I obtained with the bolometer camera LABOCA at the APEX telescope. These sources are listed in the order in which they were found by GAUSSCLUMPS, i.e. roughly in order of decreasing peak flux density. The 870 micron dust continuum emission map of the Chamaeleon I molecular cloud is available in FITS format. The data were obtained with the bolometer camera LABOCA at the APEX telescope. They were calibrated, reduced, co-added, gridded, smoothed to an effective angular resolution of 21.2 (FWHM), and written in FITS format with the BoA software. The flux density unit is Jy/21.2-beam. The coordinates are equatorial (J2000) and the offsets are in RADIO projection. (2 data files).

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Citations (0)

Water in massive star-forming regions: HIFI observations of W3 IRS5

Astronomy and Astrophysics (2010)

L. Chavarría F. Herpin T. Jacq J. Braine S. Bontemps

We present Herschel observations of the water molecule in the massive star-forming region W3 IRS5. The o-H17O 110-101, p-H18O 111-000, p-H2O 22 202-111, p-H2O 111-000, o-H2O 221-212, and o-H2O 212-101 lines, covering a frequency range from 552 up to 1669 GHz, have been detected at high spectral resolution with HIFI. The water lines in W3 IRS5 show well-defined high-velocity wings that indicate a clear contribution by outflows. Moreover, the systematically blue-shifted absorption in the H2O lines suggests expansion, presumably driven by the outflow. No infall signatures are detected. The p-H2O 111-000 and o-H2O 212-101 lines show absorption from the cold material (T ~ 10 K) in which the high-mass protostellar envelope is embedded. One-dimensional radiative transfer models are used to estimate water abundances and to further study the kinematics of the region. We show that the emission in the rare isotopologues comes directly from the inner parts of the envelope (T > 100 K) where water ices in the dust mantles evaporate and the gas-phase abundance increases. The resulting jump in the water abundance (with a constant inner abundance of 10^{-4}) is needed to reproduce the o-H17O 110-101 and p-H18O 111-000 spectra in our models. We estimate water abundances of 10^{-8} to 10^{-9} in the outer parts of the envelope (T < 100 K). The possibility of two protostellar objects contributing to the emission is discussed.

Star (game theory)

10.1051/0004-6361/201015113

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Citations (55)

Deuterated formaldehyde inρOphiuchi A

Astronomy and Astrophysics (2010)

P. Bergman B. Parise R. Liseau Bengt Larsson

Context. Formaldehyde is an organic molecule that is abundant in the interstellar medium. High deuterium fractionation is a common feature in low-mass star-forming regions. Observing several isotopologues of molecules is an excellent tool for understanding the formation paths of the molecules.

Isotopologue

Organic molecules

10.1051/0004-6361/201015012

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Citations (49)

Imaging Polarimetric Observations of a New Circumstellar Disk System

The Astrophysical Journal (2001)

J. R. Kuhn D. Potter B. Parise

Few circumstellar disks have been observed directly. Here we use sensitive differential polarimetric techniques to overcome atmospheric speckle noise in order to image the circumstellar material around HD 169142. The detected envelope or disk is considerably smaller than expectations based on the measured strength of the far-IR excess from this system.

Circumstellar disk

Circumstellar envelope

Circumstellar dust

Envelope (radar)

10.1086/320686

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Citations (102)

Molecules in protostellar shocks: the CHESS view on L1157-B1

IAUS (2011)

B. Leflóch M. Benedettini S. Cabrit E. Caux C. Ceccarelli

Source

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The Hot Core around the Low-Mass Protostar IRAS 16293-2422: Scoundrels Rule!

The Astrophysical Journal (2003)

S. Cazaux A. G. G. M. Tielens C. Ceccarelli A. Castets Valentine Wakelam

While warm dense gas is prevalent around low-mass protostars, the presence of complex saturated molecules—the chemical inventory characteristic of hot cores—has remained elusive in such environments. Here we report the results of an IRAM 30 m study of the molecular composition associated with the low-mass protostar IRAS 16293-2422. Our observations highlight an extremely rich organic inventory in this source with abundant amounts of complex O- and N-bearing molecules such as formic acid, HCOOH, acetaldehyde, CH3CHO, methyl formate, CH3OCHO, dimethyl ether, CH3OCH3, acetic acid, CH3COOH, methyl cyanide, CH3CN, ethyl cyanide, C2H5CN, and propyne, CH3CCH. We compare the composition of the hot core around this low-mass young stellar object with those around massive protostars and address the chemical processes involved in molecular complexity in regions of star formation.

Protostar

Propyne

Methyl formate

Tetrahydrofuran

Low Mass

10.1086/378038

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Citations (480)

Theoretical HDO emission from low-mass protostellar envelopes

Astronomy and Astrophysics (2005)

B. Parise C. Ceccarelli S. Maret

We present theoretical predictions of the rotational line emission of deuterated water in low-mass protostar collapsing envelopes. The model accounts for the density and temperature structure of the envelope, according to the inside-out collapse framework. The deuterated water abundance profile is approximated by a step function, with a low value in the cold outer envelope and a higher value in the inner envelope where the grain mantles evaporate. The two abundances are the two main parameters of the modeling, along with the temperature at which the mantles evaporate. We report line flux predictions for a 30 and 5 source luminosity respectively. We show that ground-based observations are capable of constraining the three parameters of the model in the case of bright low-mass protostars ( ), and that no space-based observations, such as HSO observations, are required in this case. On the contrary, we show that the study of low-luminosity sources (), assuming the same HDO abundance profile, requires too much integration time to be carried out either with available ground-based telescopes or with the HIFI instrument on board HSO. For these sources, only the large interferometer ALMA will allow one to constrain the HDO abundance.

Protostar

Envelope (radar)

Line (geometry)

Low Mass

10.1051/0004-6361:20053081

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Citations (17)

Herschel/HIFI observations of high-JCO lines in the NGC 1333 low-mass star-forming region

Astronomy and Astrophysics (2010)

U. A. Yíldíz E. F. van Dishoeck L. E. Kristensen R. Visser J. K. Jørgensen

Herschel-HIFI observations of high-J lines (up to J_u=10) of 12CO, 13CO and C18O are presented toward three deeply embedded low-mass protostars, NGC 1333 IRAS 2A, IRAS 4A, and IRAS 4B, obtained as part of the Water In Star-forming regions with Herschel (WISH) key program. The spectrally-resolved HIFI data are complemented by ground-based observations of lower-J CO and isotopologue lines. The 12CO 10-9 profiles are dominated by broad (FWHM 25-30 km s^-1) emission. Radiative transfer models are used to constrain the temperature of this shocked gas to 100-200 K. Several CO and 13CO line profiles also reveal a medium-broad component (FWHM 5-10 km s^-1), seen prominently in H2O lines. Column densities for both components are presented, providing a reference for determining abundances of other molecules in the same gas. The narrow C18O 9-8 lines probe the warmer part of the quiescent envelope. Their intensities require a jump in the CO abundance at an evaporation temperature around 25 K, thus providing new direct evidence for a CO ice evaporation zone around low-mass protostars.

Isotopologue

Protostar

Line (geometry)

Envelope (radar)

10.1051/0004-6361/201015119

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Citations (45)

Hydrides in young stellar objects: Radiation tracers in a protostar-disk-outflow system

Astronomy and Astrophysics (2010)

A. O. Benz S. Bruderer E. F. van Dishoeck P. Stäuber S. F. Wampfler

Context: Hydrides of the most abundant heavier elements are fundamental molecules in cosmic chemistry. Some of them trace gas irradiated by UV or X-rays. Aims: We explore the abundances of major hydrides in W3 IRS5, a prototypical region of high-mass star formation. Methods: W3 IRS5 was observed by HIFI on the Herschel Space Observatory with deep integration (about 2500 s) in 8 spectral regions. Results: The target lines including CH, NH, H3O+, and the new molecules SH+, H2O+, and OH+ are detected. The H2O+ and OH+ J=1-0 lines are found mostly in absorption, but also appear to exhibit weak emission (P-Cyg-like). Emission requires high density, thus originates most likely near the protostar. This is corroborated by the absence of line shifts relative to the young stellar object (YSO). In addition, H2O+ and OH+ also contain strong absorption components at a velocity shifted relative to W3 IRS5, which are attributed to foreground clouds. Conclusions: The molecular column densities derived from observations correlate well with the predictions of a model that assumes the main emission region is in outflow walls, heated and irradiated by protostellar UV radiation.

Protostar

Young stellar object

Outflow

Line (geometry)

10.1051/0004-6361/201015111

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Citations (94)