Issue |
A&A
Volume 521, October 2010
Herschel/HIFI: first science highlights
|
|
---|---|---|
Article Number | L30 | |
Number of page(s) | 6 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361/201015100 | |
Published online | 01 October 2010 |
Herschel/HIFI: first science highlights
LETTER TO THE EDITOR
Water in low-mass star-forming regions
with Herschel![[*]](/icons/foot_motif.png)
HIFI spectroscopy of NGC 1333![[*]](/icons/foot_motif.png)
L. E. Kristensen1
- R. Visser1 -
E. F. van Dishoeck1,2
- U. A. Yildiz1 -
S. D. Doty3 -
G. J. Herczeg2 - F.-C. Liu4
- B. Parise4 - J. K. Jørgensen5
- T. A. van Kempen6 -
C. Brinch1 -
S. F. Wampfler7 -
S. Bruderer7 -
A. O. Benz7 -
M. R. Hogerheijde1 -
E. Deul1 - R. Bachiller8
- A. Baudry9 - M. Benedettini10
- E. A. Bergin11 -
P. Bjerkeli12 -
G. A. Blake13 -
S. Bontemps9 - J. Braine9
- P. Caselli14,15 -
J. Cernicharo16 - C. Codella15
- F. Daniel16 -
Th. de Graauw17 -
A. M. di Giorgio10 -
C. Dominik18,19 - P. Encrenaz20
- M. Fich21 - A. Fuente22
- T. Giannini23 -
J. R. Goicoechea16 -
F. Helmich17 - F. Herpin9
- T. Jacq9 - D. Johnstone24,25
- M. J. Kaufman26 -
B. Larsson27 - D. Lis28
- R. Liseau12 - M. Marseille17
- C. MCoey21,29
- G. Melnick6 - D. Neufeld30
- B. Nisini23 - M. Olberg12
- J. C. Pearson31 -
R. Plume32 - C. Risacher17
- J. Santiago-García33 -
P. Saraceno10 - R. Shipman17
- M. Tafalla8 -
A. G. G. M. Tielens1
- F. van der Tak17,34
- F. Wyrowski4 - D. Beintema17
- A. de Jonge17 -
P. Dieleman17 - V. Ossenkopf35
- P. Roelfsema17 - J. Stutzki35
- N. Whyborn36
1 - Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden,
The Netherlands
2 - Max Planck Institut für Extraterrestrische Physik,
Giessenbachstrasse 1, 85748 Garching, Germany
3 - Department of Physics and Astronomy, Denison University, Granville,
OH, 43023, USA
4 - Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121
Bonn, Germany
5 - Centre for Star and Planet Formation, Natural History Museum of
Denmark, University of Copenhagen,
Øster Voldgade 5-7, 1350 Copenhagen K., Denmark
6 - Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS
42, Cambridge, MA 02138, USA
7 - Institute of Astronomy, ETH Zurich, 8093 Zurich, Switzerland
8 - Observatorio Astronómico Nacional (IGN), Calle Alfonso XII 3, 28014
Madrid, Spain
9 - Université de Bordeaux, Laboratoire d'Astrophysique de Bordeaux,
France; CNRS/INSU, UMR 5804, Floirac, France
10 - INAF - Instituto di Fisica dello Spazio Interplanetario, Area di
Ricerca di Tor Vergata, via Fosso del Cavaliere 100, 00133 Roma, Italy
11 - Department of Astronomy, University of Michigan, 500 Church
Street, Ann Arbor, MI 48109-1042, USA
12 - Department of Radio and Space Science, Chalmers University of
Technology, Onsala Space Observatory, 439 92 Onsala, Sweden
13 - California Institute of Technology, Division of Geological and
Planetary Sciences, MS 150-21, Pasadena, CA 91125, USA
14 - School of Physics and Astronomy, University of Leeds, Leeds LS2
9JT, UK
15 - INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5,
50125 Firenze, Italy
16 - Centro de Astrobiología, Departamento de Astrofísica, CSIC-INTA,
Carretera de Ajalvir, Km 4, Torrejón de Ardoz, 28850 Madrid, Spain
17 - SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV
Groningen, The Netherlands
18 - Astronomical Institute Anton Pannekoek, University of Amsterdam,
Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
19 - Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO
Box 9010, 6500 GL Nijmegen, The Netherlands
20 - LERMA and UMR 8112 du CNRS, Observatoire de Paris, 61 Av. de
l'Observatoire, 75014 Paris, France
21 - University of Waterloo, Department of Physics and Astronomy,
Waterloo, Ontario, Canada
22 - Observatorio Astronómico Nacional, Apartado 112, 28803 Alcalá de
Henares, Spain
23 - INAF - Osservatorio Astronomico di Roma, 00040 Monte Porzio
catone, Italy
24 - National Research Council Canada, Herzberg Institute of
Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
25 - Department of Physics and Astronomy, University of Victoria,
Victoria, BC V8P 1A1, Canada
26 - Department of Physics and Astronomy, San Jose State University,
One Washington Square, San Jose, CA 95192, USA
27 - Department of Astronomy, Stockholm University, AlbaNova, 106 91
Stockholm, Sweden
28 - California Institute of Technology, Cahill Center for Astronomy
and Astrophysics, MS 301-17, Pasadena, CA 91125, USA
29 - University of Western Ontario, Department of Physics &
Astronomy, London, Ontario, N6A 3K7, Canada
30 - Department of Physics and Astronomy, Johns Hopkins University,
3400 North Charles Street, Baltimore, MD 21218, USA
31 - Jet Propulsion Laboratory, California Institute of Technology,
Pasadena, CA 91109, USA
32 - Department of Physics and Astronomy, University of Calgary,
Calgary, T2N 1N4, AB, Canada
33 - Instituto de RadioAstronomía Milimétrica, Avenida Divina Pastora,
7, Núcleo Central E 18012 Granada, Spain
34 - Kapteyn Astronomical Institute, University of Groningen, PO Box
800, 9700 AV, Groningen, The Netherlands
35 - KOSMA, I. Physik. Institut, Universität zu Köln, Zülpicher Str.
77, 50937 Köln, Germany
36 - Atacama Large Millimeter/Submillimeter Array, Joint ALMA Office,
Santiago, Chile
Received 31 May 2010 / Accepted 13 July 2010
Abstract
``Water In Star-forming regions with Herschel''
(WISH) is a key programme dedicated to studying the role of water and
related species during the star-formation process and constraining the
physical and chemical properties of young stellar objects. The
Heterodyne Instrument for the Far-Infrared (HIFI) on the Herschel
Space Observatory observed three deeply embedded protostars in the
low-mass star-forming region NGC 1333 in several H216O,
H218O, and
CO transitions. Line profiles are resolved for five H216O transitions
in each source, revealing them to be surprisingly complex. The line
profiles are decomposed into broad (>20 km s-1),
medium-broad (5-10 km s-1),
and narrow (<5 km s-1)
components. The H218O emission
is only detected in broad 110-101 lines
(>20 km s-1),
indicating that its physical origin is the same as for the broad H216O component.
In one of the sources, IRAS4A, an inverse
P Cygni profile is observed, a clear sign of infall
in the envelope. From the line profiles alone, it is clear
that the bulk of emission arises from shocks, both on small (
1000 AU)
and large scales along the outflow cavity walls (
10 000 AU).
The H2O line profiles are compared to
CO line profiles to constrain the H2O abundance
as a function of velocity within these shocked regions. The H2O/CO abundance
ratios are measured to be in the range of
0.1-1, corresponding to H2O abundances
of
10-5-10-4
with respect to H2. Approximately 5-10%
of the gas is hot enough for all oxygen to be driven into water in warm
post-shock gas, mostly at high velocities.
Key words: astrochemistry - stars: formation - ISM: molecules - ISM: jets and outflows - ISM: individual objects: NGC 1333
1 Introduction
In the deeply embedded phase of low-mass star formation, it is often only possible to trace the dynamics of gas in a young stellar object (YSO) by analysing resolved emission-line profiles. The various dynamical processes include infall from the surrounding envelope towards the central protostar, molecular outflows caused by jets ejected from the central object, and strong turbulence induced within the inner parts of the envelope by small-scale shocks (Jørgensen et al. 2007; Arce et al. 2007). One of the goals of the Water In Star-forming regions with Herschel (WISH) key programme is to use water as a probe of these processes and determine its abundance in the various components as a function of evolution (van Dishoeck et al., in prep.).
Spectrally resolved observations of the H2O
110-101 line at
557 GHz with ODIN and SWAS towards low-mass star-forming
regions have revealed it to be broad, 20 km s-1,
indicative of an origin in shocks (e.g., Bergin
et al. 2003). Within the large beams (2
and 4
), where both
the envelope and the entire outflow are present, outflow emission most
likely dominates. Observations and subsequent modelling of the more
highly excited H2O lines with ISO-LWS
were unable to distinguish between an origin in shocks or an infalling
envelope (e.g., Ceccarelli
et al. 1996; Nisini et al. 2002; Maret
et al. 2002). Herschel/HIFI has
a much higher sensitivity, higher spectral resolution, and smaller beam
than previous space-based missions, thus is perfectly suited to
addressing this question. Complementary CO data presented by Yildiz et al. (2010) are
used to constrain the role of the envelope and determine outflow
temperatures and densities.
NGC 1333 is a well-studied region of clustered, low-mass star
formation at a distance of 235 pc (Hirota
et al. 2008). In particular,
the three deeply embedded, low-mass class 0 objects
IRAS2A, IRAS4A, and IRAS4B have been observed extensively with
ground-based submillimetre telescopes (e.g., Maret et al. 2005; Jørgensen
et al. 2005) and interferometers (e.g., Jørgensen
et al. 2007; Di Francesco et al. 2001).
All sources have strong outflows extending over arcmin scales
(>15 000 AU). Both IRAS4A and 4B
consist of multiple protostars (e.g., Choi
2005). Because of the similarities between the three sources
in terms of luminosity (20, 5.8, and 3.8 ), envelope
mass (1.0, 4.5, and 2.9
;
Jørgensen et al. 2009)
and presumably also age, they provide ideal grounds for comparing YSOs
in the same region.
Table 1: H2O and H218O emissiona in the NGC 1333 sourcesb.
2 Observations and results
![]() |
Figure 1: H2O spectra of the three NGC 1333 sources. CO 10-9 is shown for comparison (Yildiz et al. 2010); the CO 10-9 emission in IRAS2A is affected by chopping into outflow material. The top panel shows the decomposition into broad (red), medium (blue), and narrow (black) components. The cartoon illustrates the physical origin of each component. The inset shows a zoom on the inverse P Cygni profile in the H2O 202-111 line of IRAS4A, where the other components have been subtracted; the vertical scale ranges from -0.3 to 0.3 K. |
Open with DEXTER |
![]() |
Figure 2:
H218O 110-101
spectra of the three NGC 1333 sources along with the
CH 536 GHz triplet from the lower sideband (dotted
lines). Spectra are shown for a channel size of
0.25 km s-1. The spectrum of
IRAS2A has been rebinned to 4 km s-1
to illustrate the detection of a broad feature. The red line shows the
source velocity at |
Open with DEXTER |
Three sources in NGC 1333, IRAS2A, IRAS4A, and IRAS4B, were
observed with HIFI (de Graauw
et al. 2010) on Herschel (Pilbratt et al. 2010)
on March 3-15, 2010 in dual beam switch mode in
bands 1, 3, 4, and 5 with a nod of 3.
Observations detected several transitions of H2O
and H218O in the range
50-250 K (Table 2).
Diffraction-limited beam sizes were in the range 19-40
(4500-9500 AU). In general, the calibration
is expected to be accurate to
20% and the pointing to
2
.
Data were reduced with HIPE 3.0. A main-beam
efficiency of 0.74 was used throughout. Subsequent analysis
was performed in CLASS. The rms was in the range 3-150 mK in
0.5 km s-1 bins. Linear
baselines were subtracted from all spectra, except around
750 GHz (corresponding to the H2O 211-202 transition)
where higher-order polynomials are required. A difference in
rms was always seen between the H- and V-polarizations, with the rms in
the H-polarization being lower. In cases where the difference
exceeded 30% and qualitative differences appear in the line profile,
the V-polarization was discarded, otherwise the spectra were averaged.
All targeted lines of H216O
were detected and are listed in Table 1 and
Fig. 1.
The 110-101 transition
at 557 GHz was not observed before the sources moved out of
visibility. The H218O 110-101 line
was detected in all sources (Fig. 2),
although the detection in IRAS2A was weak (5
=
0.13 K km s-1). This
line is superposed on the ground-state CH triplet at
536 GHz, observed in the lower sideband (Fig. 2).
Neither the H218O 111-000
nor the 202-111 line
in IRAS2A is detected down to
< 0.06 K km s-1.
The H2O lines exhibit multiple
components: a broad emission component (FWHM >
20 km s-1) sometimes offset
from the source velocity (
=
+7.2-7.7 km s-1);
a medium-broad emission component (FWHM
5-10 km s-1); and a deep,
narrow absorption component (FWHM
2 km s-1) seen at the source
velocity. The individual components are all reproduced well by Gaussian
functions. The absorption is only seen in the H2O 111-000 line
and is saturated in IRAS2A and IRAS4A. In IRAS4B, the absorption
extends below the continuum level, but is not saturated. Furthermore,
the IRAS4A spectrum of the 202-111 line
exhibits an inverse P Cygni profile. The shape of the lines is
the same within a source; only the relative contribution between the
broad and medium components changes. For example, in IRAS2A
the ratio of the peak intensities is
2, independent of the line,
whereas in IRAS4A it ranges from 1 to 2. The H218O line
profiles compare well to the broad component seen in H2O,
i.e., similar FWHM >
20 km s-1 and velocity offset.
The width is much larger than isotopologue emission of, e.g., C18O
(
1-2 km s-1)
and is centred on the source velocity (Yildiz
et al. 2010). The medium and narrow components are
not seen in the H218O 110-101
spectra down to an rms of 2-3 mK in 0.5 km s-1 bins.
The upper limits to the H218O
111-000 line are
invaluable for estimating upper limits to the optical depth, .
In the following, the limit on
is derived for the integrated intensity; in the line wings,
is
most likely lower (Yildiz
et al. 2010). In the broad component, the
limit ranges from 0.4 (IRAS4B) to 2 (IRAS2A), whereas
it ranges from 1.1 (IRAS4B) to 2.7 (IRAS2A) for the
medium component of the H216O
111-000 line.
Performing the same analysis to the upper limit on the H218O
202-111 line
observed in IRAS2A, infers an upper limit to the optical depth of H216O
202-111 of 1.5
for the medium component and 1.9 for the broad. Thus it is
likely that neither the broad nor the medium components are very
optically thick.
3 Discussion
Many physical components in a YSO are directly traced by the line profiles presented here, including the infalling envelope and shocks along the cavity walls. In the following, each component is discussed in detail, and the H2O abundance is estimated in the various physical components.
3.1 Line profiles
The most prominent feature of all the observed line profiles is their
width. All line wings span a range of velocities of 40-70 km s-1
at their base. The width alone indicates that the bulk of the H2O emission
originates in shocks along the cavity walls, also called shells, seen
traditionally as the standard high-velocity component in
CO outflow data, but with broader line-widths due to water
enhancement at higher velocities (Sect. 3.2 Santiago-García
et al. 2009; Bachiller et al. 1990).
The shocks release water from the grains by means of sputtering and in
high-temperature regions all free oxygen is driven into water. The
shocked regions may be illuminated by FUV radiation
originating in the star-disk boundary layer, thus further enhancing the
water abundance by means of photodesorption. The broad emission seen in
the H182O 110-101
line arises in the same shocks (see cartoon in Fig. 1).
The medium components (FWHM
5-10 km s-1) are most likely
also caused by shocks, although presumably on a smaller spatial scale
and in denser material than the shocks discussed above.
For example, the medium component in IRAS2A is seen
in other grain-product species such as CH3OH (Maret
et al. 2005; Jørgensen et al. 2005,
Fig. 3),
where emission arises from a compact region (<1
,
i.e., <250 AU) centred on the source (Jørgensen et al. 2007),
and the same is likely true for the medium H2O component
in that source. In interferometric observations of IRAS4A,
a small (
few arcsec)
blue-shifted outflow knot of similar width has been identified in,
e.g., SiO and SO (Choi
2005; Jørgensen
et al. 2007). Small-scale structures exist in the
other sources as well, which may produce the medium components.
![]() |
Figure 3: Left. Comparison between the medium component in IRAS2A and other species observed with ground-based telescopes. The broad component has been subtracted for easy comparison. The vertical red line indicates the source velocity at +7.7 km s-1. Right. Comparison between H2O 202-111 and CO 6-5 obtained with APEX-CHAMP+, and emission ratios for the blue- and red-shifted outflow lobes. |
Open with DEXTER |
The H2O 202-111
spectrum of IRAS4A shows an inverse P Cygni profile,
a clear sign of infall also detected in other molecular
tracers using interferometer observations (Jørgensen et al. 2007;
Di
Francesco et al. 2001). This infall signature is
also tentatively seen in the 111-000 line,
but here the absorption from the outer envelope dominates and little is
left of the blue emission peak. The signature is not seen in
higher-excitation lines. The separation of the emission and absorption
peaks is 0.8 km s-1,
whereas it is
1.5 km s-1
in the observations of Di
Francesco et al. (2001) and larger in the
observations by Jørgensen
et al. (2007), indicating that the infall observed
in H2O 202-111
takes place over larger spatial scales.
The passively heated envelope is seen in ground-based
observations of high-density tracers to produce narrow emission,
<3 km s-1, which may be
self-absorbed (Fig. 3).
For water, this type of emission is not seen in any of the sources; the
medium component is broader by a factor of 2-3 with respect to
what is expected from the envelope. The absorption seen in all three
sources is attributed to cold gas in the outer parts of the envelope.
Using interferometric observations, Jørgensen
& van Dishoeck (2010) detected compact, narrow (1 km s-1)
emission in the H182O 313-220 line
in IRAS4B possibly originating in the circumstellar disk. Scaling the
observed emission to the transitions observed here by assuming
=
170 K (Watson et al.
2007), the expected emission is typically less
than 10% of the rms for any given transition. Hence, when
extrapolated to the disks surrounding IRAS2A and 4A, the disk
contribution to the H2O emission probed
by HIFI is negligible. The H2O excitation
temperature of the broad component is 220
30 K, comparable to that found by Watson
et al. (2007), but the inferred column density is a
factor of 100 higher. Thus, the mid-infrared lines seen by Watson et al. may come
from the same broad outflowing gas found by HIFI, provided the
mid-infrared lines experience a factor of 100 more extinction.
3.2 Abundances
3.2.1 Shocks: H2O/CO
The observed broad components are compared directly with HIFI
observations of CO 10-9 (Yildiz
et al. 2010), because the width and position of the
lines are similar and they were obtained using approximately the same
beamsize (22
versus 19
). The exception is for
IRAS2A, where the blue line wing is not observed. The advantage is that
no detailed models are required to account for the H2O/CO abundance,
as long as the lines are optically thin,
in particular the emission from the wings. The abundance ratio
is estimated for various temperatures by using the RADEX escape
probability code (van der Tak
et al. 2007). The density is assumed to be 105 cm-3,
appropriate for the large-scale core. If the emission is
optically thin, the abundance ratio scales linearly with density
resulting in the same line ratio corresponding to a higher abundance
ratio. There is little variation in the predicted ratio for T >
150 K, the typical temperature inferred by Yildiz et al. (2010).
The line ratios and abundance ratios are listed as a function of
velocity in Table 3.
The abundance ratio increases with increasing velocity from H2O/CO
of 0.2 near the
line centre to H2O/CO
1
in the line wings of all sources for velocity offsets larger than
15 km s-1 with respect to that
of the source (Fig. 3).
Assuming that the CO abundance is 10-4,
the H2O abundances are in the range of
10-5-10-4.
Only at high velocities is the temperature high enough for oxygen to be
driven into water by means of the neutral-neutral reaction O +
H2
OH + H; OH + H2
H2O. The same result was found in the massive
outflow in Orion-KL (Franklin
et al. 2008), where less than 1% of the gas
in the outflow experiences this high-temperature phase. The fraction of
gas for which the H2O/CO abundance is
>1 is
5-10%
for the sources observed here.
For IRAS2A, a deep spectrum of CO 6-5 obtained with CHAMP+
on APEX simultaneously with observations of HDO 111-000
(Liu et al., in prep.) shows the same morphology in
terms of a broad and medium component (Fig. 3).
Furthermore, the velocity offset and FWHM are the
same as for H2O suggesting that the line
profiles are not unique to H2O,
although the broad component is far more prominent in H2O.
The ratio of peak intensities for the two components is 2-3 in H2O versus 10
in CO 6-5. Analysing the abundance ratio as a function of
temperature shows that H2O/CO
0.1-1 for T > 150 K
(Table 3),
consistent with what is found for CO 10-9.
3.2.2 Envelope
The simplest way to constrain the H2O abundance in the outer envelope is with calculations using RADEX on the narrow absorption in the 111-000 line. The absorption is optically thick - in particular for IRAS2A and 4A, where the feature is saturated - which requires a para-H2O column density of >1013 cm-2 if one assumes typical values for T and


For IRAS2A and 4A, the H2O abundance was further
constrained using radiative transfer models. The setup is a spherical
envelope with density and temperature profiles constrained from
continuum data (Jørgensen
et al. 2009), an infall velocity profile ,
and a Doppler parameter b=0.8 km s-1.
Line fluxes were computed with the new radiative transfer code LIME
(Brinch & Hogerheijde, submitted). The models constrained the
abundance of water in the outer envelope to be
10-8.
Lower values are insufficient to obtain saturated absorption in the 111-000 line,
and
10-8
is the highest abundance where the resulting narrow emission can be
hidden in the observed higher-excitation H2O lines.
The models predict that the H2O emission
from the warm inner envelope (r
100 AU)
is optically thick, hence no constraints can be obtained from the H2O spectra
on the inner abundance. However, the lack of narrow H218O emission
infers an upper limit on the H2O abundance
of
10-5
(Visser et al., in prep.).
4 Conclusions
These observations represent one of the first steps towards understanding the formation and excitation of water in low-mass star-forming regions by means of resolved line profiles. The three sources have remarkably similar line profiles. Both the H216O and H218O lines are very broad, indicating that the bulk of the emission originates in shocked gas. The broad emission also highlights that water is a far more reliable dynamical tracer than, e.g., CO. Comparing C18O to H182O emission and line profiles indicates that the H2O/CO abundance is high in outflows and low in the envelope. Additional modelling of the emission, should be able to constrain the total amount of water in the envelope and outflowing gas, thus test the high-temperature gas-phase chemistry models for the origin of water. This will be performed for a total sample of the 29 low-mass YSOs to be observed within the WISH key programme.
AcknowledgementsThis work is made possible thanks to the HIFI guaranteed time programme. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the US under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U.Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiología (CSIC-INTA); Sweden: Chalmers University of Technology - MC2, RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zürich, FHNW; USA: Caltech, JPL, NHSC. HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. We thank many funding agencies for financial support.
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Online Material
Table 2: Observed H2O, H218O and CH transitionsa.
Table 3: CO 6-5 and CO 10-9/H2O 202-111 line ratios in 5 km s-1 intervals and corresponding abundance ratio for T > 150 K and n = 105 cm-3.
Footnotes
- ...Herschel
- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
- ... 1333
- Tables 2 and 3 (page 6) are only available in electronic form at http://www.aanda.org
All Tables
Table 1: H2O and H218O emissiona in the NGC 1333 sourcesb.
Table 2: Observed H2O, H218O and CH transitionsa.
Table 3: CO 6-5 and CO 10-9/H2O 202-111 line ratios in 5 km s-1 intervals and corresponding abundance ratio for T > 150 K and n = 105 cm-3.
All Figures
![]() |
Figure 1: H2O spectra of the three NGC 1333 sources. CO 10-9 is shown for comparison (Yildiz et al. 2010); the CO 10-9 emission in IRAS2A is affected by chopping into outflow material. The top panel shows the decomposition into broad (red), medium (blue), and narrow (black) components. The cartoon illustrates the physical origin of each component. The inset shows a zoom on the inverse P Cygni profile in the H2O 202-111 line of IRAS4A, where the other components have been subtracted; the vertical scale ranges from -0.3 to 0.3 K. |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
H218O 110-101
spectra of the three NGC 1333 sources along with the
CH 536 GHz triplet from the lower sideband (dotted
lines). Spectra are shown for a channel size of
0.25 km s-1. The spectrum of
IRAS2A has been rebinned to 4 km s-1
to illustrate the detection of a broad feature. The red line shows the
source velocity at |
Open with DEXTER | |
In the text |
![]() |
Figure 3: Left. Comparison between the medium component in IRAS2A and other species observed with ground-based telescopes. The broad component has been subtracted for easy comparison. The vertical red line indicates the source velocity at +7.7 km s-1. Right. Comparison between H2O 202-111 and CO 6-5 obtained with APEX-CHAMP+, and emission ratios for the blue- and red-shifted outflow lobes. |
Open with DEXTER | |
In the text |
Copyright ESO 2010
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