Herschel spectral surveys of star-forming regions. Overview of the 555-636 GHz range

C. Ceccarelli; A. Bacmann; A. Boogert; E. Caux; C. Dominik; B. Lefloch; D. Lis; P. Schilke; F. F. S. van der Tak; P. Caselli; J. Cernicharo; C. Codella; C. Comito; A. Fuente; A. Baudry; T. A. Bell; M. Benedettini; E. A. Bergin; G. A. Blake; S. Bottinelli; S. Cabrit; A. Castets; A. Coutens; N. Crimier; K. Demyk; P. Encrenaz; E. Falgarone; M. Gerin; P. F. Goldsmith; F. Helmich; P. Hennebelle; T. Henning; E. Herbst; P. Hily-Blant; T. Jacq; C. Kahane; M. Kama; A. Klotz; W. D. Langer; S. Lord; A. Lorenzani; S. Maret; G. J. Melnick; D. A. Neufeld; B. Nisini; S. Pacheco; L. Pagani; B. Parise; J. C. Pearson; T. Phillips; M. Salez; P. Saraceno; K. Schuster; X. Tielens; M. H. D. van der Wiel; C. Vastel; S. Viti; V. Wakelam; A. Walters; F. Wyrowski; H. W. Yorke; René Liseau; Michael Olberg; R. Szczerba; A. O. Benz; M. Melchior

doi:10.1051/0004-6361/201015081

Herschel spectral surveys of star-forming regions. Overview of the 555-636 GHz range
Artikel i vetenskaplig tidskrift, 2010

High resolution line spectra of star-forming regions are mines of information: they provide unique clues to reconstruct the chemical, dynamical, and physical structure of the observed source. We present the first results from the Herschel key project \ldquoChemical HErschel Surveys of Star forming regions\rdquo, CHESS. We report and discuss observations towards five CHESS targets, one outflow shock spot and four protostars with luminosities bewteen 20 and 2 \times 10^5 L\_\.o: L1157-B1, IRAS 16293-2422, OMC2-FIR4, AFGL 2591, and NGC 6334I. The observations were obtained with the heterodyne spectrometer HIFI on board Herschel, with a spectral resolution of 1 MHz. They cover the frequency range 555-636 GHz, a range largely unexplored before the launch of the Herschel satellite. A comparison of the five spectra highlights spectacular differences in the five sources, for example in the density of methanol lines, or the presence/absence of lines from S-bearing molecules or deuterated species. We discuss how these differences can be attributed to the different star-forming mass or evolutionary status.

Författare

C. Ceccarelli

Laboratoire d'Astrophysique de Bordeaux

Université Grenoble Alpes

Institut National des Sciences de l'Univers

A. Bacmann

Université Grenoble Alpes

Laboratoire d'Astrophysique de Bordeaux

Institut National des Sciences de l'Univers

A. Boogert

California Institute of Technology (Caltech)

E. Caux

Universite Paul Sabatier Toulouse III

Institut National des Sciences de l'Univers

C. Dominik

Anton Pannekoek Institute for Astronomy

Radboud Universiteit

B. Lefloch

Université Grenoble Alpes

D. Lis

California Institute of Technology (Caltech)

P. Schilke

Universität zu Köln

Max-Planck-Gesellschaft

F. F. S. van der Tak

Rijksuniversiteit Groningen

Netherlands Institute for Space Research (SRON)

P. Caselli

Istituto di Fisica dello Spazio Interplanetario, Rome

University of Leeds

J. Cernicharo

Centro de Astrobiologia (CAB)

C. Codella

Osservatorio Astrofisico di Arcetri

C. Comito

Max-Planck-Gesellschaft

A. Fuente

Observatorio Astronómico Nacional (OAN)

A. Baudry

Laboratoire d'Astrophysique de Bordeaux

Institut National des Sciences de l'Univers

T. A. Bell

California Institute of Technology (Caltech)

M. Benedettini

Istituto di Fisica dello Spazio Interplanetario, Rome

E. A. Bergin

University of Michigan

G. A. Blake

California Institute of Technology (Caltech)

S. Bottinelli

Institut National des Sciences de l'Univers

Universite Paul Sabatier Toulouse III

S. Cabrit

Ecole Normale Superieure (ENS)

A. Castets

Institut National des Sciences de l'Univers

Université Grenoble Alpes

Laboratoire d'Astrophysique de Bordeaux

A. Coutens

Universite Paul Sabatier Toulouse III

Institut National des Sciences de l'Univers

N. Crimier

Centro de Astrobiologia (CAB)

Université Grenoble Alpes

K. Demyk

Institut National des Sciences de l'Univers

Universite Paul Sabatier Toulouse III

P. Encrenaz

Ecole Normale Superieure (ENS)

E. Falgarone

Ecole Normale Superieure (ENS)

M. Gerin

Ecole Normale Superieure (ENS)

P. F. Goldsmith

Jet Propulsion Laboratory, California Institute of Technology

F. Helmich

Netherlands Institute for Space Research (SRON)

P. Hennebelle

Ecole Normale Superieure (ENS)

T. Henning

Max-Planck-Gesellschaft

E. Herbst

Ohio State University

P. Hily-Blant

Université Grenoble Alpes

T. Jacq

Laboratoire d'Astrophysique de Bordeaux

Institut National des Sciences de l'Univers

C. Kahane

Université Grenoble Alpes

M. Kama

Anton Pannekoek Institute for Astronomy

A. Klotz

Universite Paul Sabatier Toulouse III

Institut National des Sciences de l'Univers

W. D. Langer

Jet Propulsion Laboratory, California Institute of Technology

S. Lord

California Institute of Technology (Caltech)

A. Lorenzani

Osservatorio Astrofisico di Arcetri

S. Maret

Université Grenoble Alpes

G. J. Melnick

Harvard-Smithsonian Center for Astrophysics

D. A. Neufeld

Johns Hopkins University

B. Nisini

Osservatorio Astronomico di Roma

S. Pacheco

Université Grenoble Alpes

L. Pagani

Ecole Normale Superieure (ENS)

B. Parise

Max-Planck-Gesellschaft

J. C. Pearson

Jet Propulsion Laboratory, California Institute of Technology

T. Phillips

California Institute of Technology (Caltech)

M. Salez

Ecole Normale Superieure (ENS)

P. Saraceno

Istituto di Fisica dello Spazio Interplanetario, Rome

K. Schuster

Institut de RadioAstronomie Millimetrique (IRAM)

X. Tielens

Universiteit Leiden

M. H. D. van der Wiel

Netherlands Institute for Space Research (SRON)

Rijksuniversiteit Groningen

C. Vastel

Institut National des Sciences de l'Univers

Universite Paul Sabatier Toulouse III

S. Viti

University College London (UCL)

V. Wakelam

Institut National des Sciences de l'Univers

Laboratoire d'Astrophysique de Bordeaux

A. Walters

Institut National des Sciences de l'Univers

Universite Paul Sabatier Toulouse III

F. Wyrowski

Max-Planck-Gesellschaft

H. W. Yorke

Jet Propulsion Laboratory, California Institute of Technology

René Liseau

Chalmers, Institutionen för radio- och rymdvetenskap, Radioastronomi och astrofysik

Forskning Andra publikationer

Michael Olberg

Chalmers, Institutionen för radio- och rymdvetenskap, Nationella anläggningen för radioastronomi

Forskning Andra publikationer

R. Szczerba

Polish Academy of Sciences

A. O. Benz

Eidgenössische Technische Hochschule Zürich (ETH)

M. Melchior

Institut für 4D-Technologien

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 521 1 L22+- L22

Ämneskategorier

Astronomi, astrofysik och kosmologi

Fundament

Grundläggande vetenskaper

DOI

10.1051/0004-6361/201015081

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Senast uppdaterat

2018-10-30

Herschel spectral surveys of star-forming regions. Overview of the 555-636 GHz range Artikel i vetenskaplig tidskrift, 2010

Författare

C. Ceccarelli

A. Bacmann

A. Boogert

E. Caux

C. Dominik

B. Lefloch

D. Lis

P. Schilke

F. F. S. van der Tak

P. Caselli

J. Cernicharo

C. Codella

C. Comito

A. Fuente

A. Baudry

T. A. Bell

M. Benedettini

E. A. Bergin

G. A. Blake

S. Bottinelli

S. Cabrit

A. Castets

A. Coutens

N. Crimier

K. Demyk

P. Encrenaz

E. Falgarone

M. Gerin

P. F. Goldsmith

F. Helmich

P. Hennebelle

T. Henning

E. Herbst

P. Hily-Blant

T. Jacq

C. Kahane

M. Kama

A. Klotz

W. D. Langer

S. Lord

A. Lorenzani

S. Maret

G. J. Melnick

D. A. Neufeld

B. Nisini

S. Pacheco

L. Pagani

B. Parise

J. C. Pearson

T. Phillips

M. Salez

P. Saraceno

K. Schuster

X. Tielens

M. H. D. van der Wiel

C. Vastel

S. Viti

V. Wakelam

A. Walters

F. Wyrowski

H. W. Yorke

René Liseau

Michael Olberg

R. Szczerba

A. O. Benz

M. Melchior

Astronomy and Astrophysics

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Fundament

DOI

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Herschel spectral surveys of star-forming regions. Overview of the 555-636 GHz range
Artikel i vetenskaplig tidskrift, 2010