Issue |
A&A
Volume 521, October 2010
Herschel/HIFI: first science highlights
|
|
---|---|---|
Article Number | L40 | |
Number of page(s) | 7 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361/201015119 | |
Published online | 01 October 2010 |
Herschel/HIFI: first science highlights
LETTER TO THE EDITOR
Herschel/HIFI observations of high-J CO lines in the NGC 1333 low-mass star-forming region
,![[*]](/icons/foot_motif.png)
U. A. Yildiz1 - E. F. van Dishoeck1,2 - L. E. Kristensen1 - R. Visser1 - J. K. Jørgensen3 - G. J. Herczeg2 - T. A. van Kempen1,4 - M. R. Hogerheijde1 - S. D. Doty5 - A. O. Benz6 - S. Bruderer6 - S. F. Wampfler6 - E. Deul1 - R. Bachiller7 - A. Baudry8 - M. Benedettini9 - E. Bergin10 - P. Bjerkeli11 - G. A. Blake12 - S. Bontemps8 - J. Braine8 - P. Caselli13,14 - J. Cernicharo15 - C. Codella14 - F. Daniel15 - A. M. di Giorgio9 - C. Dominik16,17 - P. Encrenaz18 - M. Fich19 - A. Fuente20 - T. Giannini21 - J. R. Goicoechea15 - Th. de Graauw22 - F. Helmich22 - F. Herpin8 - T. Jacq8 - D. Johnstone23,24 - B. Larsson25 - D. Lis26 - R. Liseau11 - F.-C. Liu27 - M. Marseille22 - C. MCoey19,28 - G. Melnick4 - D. Neufeld29 - B. Nisini21 - M. Olberg11 - B. Parise27 - J. C. Pearson30 - R. Plume31 - C. Risacher22 - J. Santiago-García32 - P. Saraceno9 - R. Shipman22 - M. Tafalla7 - A. G. G. M. Tielens1 - F. van der Tak22,33 - F. Wyrowski27 - P. Dieleman22 - W. Jellema22 - V. Ossenkopf34 - R. Schieder34 - J. Stutzki34
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
- Centre for Star and Planet Formation, Natural History Museum of
Denmark, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen
K., Denmark
4 - Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 42, Cambridge, MA 02138, USA
5 - Department of Physics and Astronomy, Denison University, Granville, OH, 43023, USA
6 - Institute of Astronomy, ETH Zurich, 8093 Zurich, Switzerland
7 - Observatorio Astronómico Nacional (IGN), Calle Alfonso XII 3, 28014 Madrid, Spain
8 - Université de Bordeaux, Laboratoire d'Astrophysique de Bordeaux, France; CNRS/INSU, UMR 5804, Floirac, France
9
- INAF - Istituto di Fisica dello Spazio Interplanetario, Area di
Ricerca di Tor Vergata, via Fosso del Cavaliere 100, 00133 Roma, Italy
10 - Department of Astronomy, The University of Michigan, 500 Church Street, Ann Arbor, MI 48109-1042, USA
11
- Department of Radio and Space Science, Chalmers University of
Technology, Onsala Space Observatory, 439 92 Onsala, Sweden
12 - California Institute of Technology, Division of Geological and Planetary Sciences, MS 150-21, Pasadena, CA 91125, USA
13 - School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK
14 - INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
15 - Centro de Astrobiología. Departamento de Astrofísica.
CSIC-INTA. Carretera de Ajalvir, Km 4, Torrejón de Ardoz., 28850
Madrid, Spain
16 - Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
17 - Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
18 - LERMA and UMR 8112 du CNRS, Observatoire de Paris, 61 Av. de l'Observatoire, 75014 Paris, France
19 - University of Waterloo, Department of Physics and Astronomy, Waterloo, Ontario, Canada
20 - Observatorio Astronómico Nacional, Apartado 112, 28803 Alcalá de Henares, Spain
21 - INAF - Osservatorio Astronomico di Roma, 00040 Monte Porzio catone, Italy
22 - SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV, Groningen, The Netherlands
23 - National Research Council Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
24 - Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 1A1, Canada
25 -
Department of Astronomy, Stockholm University, AlbaNova, 106 91 Stockholm, Sweden
26
- California Institute of Technology, Cahill Center for Astronomy and
Astrophysics, MS 301-17, Pasadena, CA 91125, USA
27 - Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
28 - the University of Western Ontario, Department of Physics and Astronomy, London, Ontario, N6A 3K7, Canada
29 - Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA
30 - Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
31 -
Department of Physics and Astronomy, University of Calgary, Calgary, T2N 1N4, AB, Canada
32 - Instituto de Radioastronomía Milimétrica (IRAM), Avenida Divina Pastora 7, Núcleo Central, 18012 Granada, Spain
33 - Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV, Groningen, The Netherlands
34 - KOSMA, I. Physik. Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
Received 31 May 2010 / Accepted 2 August 2010
Abstract
Herschel/HIFI observations of high-J lines (up to
)
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.
Key words: astrochemistry - stars: formation - ISM: jets and outflows - ISM: molecules
1 Introduction
The earliest protostellar phase just after cloud collapse - the so-called Class 0 phase - is best studied at mid-infrared and longer wavelengths (André et al. 2000). To understand the physical and chemical evolution of low-mass protostars, in particular the relative importance of radiative heating and shocks in their energy budget, observations are required that can separate these components. The advent of the Heterodyne Instrument for the Far Infrared (HIFI) on Herschel opens up the possibility to obtain spectrally resolved data from higher-frequency lines that are sensitive to gas temperatures up to several hundred Kelvin.
Because of its high abundance and strong lines, CO is the primary
molecule to probe the various components of protostellar systems
(envelope, outflow, disk). The main advantage of CO compared with
other molecules (including water) is that its chemistry is simple,
with most carbon locked up in CO in dense clouds. Also, its
evaporation temperature is low, around 20 K for pure CO ice
(Öberg et al. 2005; Collings et al. 2003), so that its freeze-out zone is much
smaller than that of water. Most ground-based observations of CO and
its isotopologues have been limited to the lowest rotational
lines originating from levels up to 35 K. The ISO has detected strong far-infrared CO lines up to
from Class 0 sources (Giannini et al. 2001) but the emission is spatially unresolved in the large 80
beam.
ISO also lacked the spectral resolution needed to separate the shocked
and quiescent gas or to detect intrinsically-weaker 13CO and C18O lines on top of the strong continuum.
The NGC 1333 region in Perseus
(d=235 pc; Hirota et al. 2008) contains several deeply embedded Class 0 sources within a 1 pc region driving powerful outflows
(e.g., Liseau et al. 1988; Hatchell & Fuller 2008). The protostars IRAS 4A
and 4B, separated by
31
,
and IRAS 2A are prominent
submillimeter continuum sources (luminosities of 5.8, 3.8 and 20
)
with envelope masses of 4.5, 2.9 and 1.0
,
respectively (Jørgensen et al. 2009; Sandell et al. 1991). All three are among the
brightest and best studied low-mass sources in terms of molecular
lines, with several complex molecules detected
(e.g., Bottinelli et al. 2007; Blake et al. 1995).
Here
HIFI data of CO and its isotopologues are presented for these three
sources and used to quantify the different physical components. In an
accompanying letter, Kristensen et al. (2010) present complementary HIFI observations of
H2O and analyze CO/H2O abundance ratios.
2 Observations and results
The NGC 1333 data were obtained with HIFI (de Graauw et al. 2010) onboard the Herschel Space Observatory (Pilbratt et al. 2010),
in the context of the WISH key program
(van Dishoeck et al. in prep.). Single pointings at the three
source positions were carried out between 2010 March 3 and
15 during the
Herschel/HIFI priority science program (PSP). Spectral lines were observed in dual-beam switch
(DBS) mode in HIFI bands 1a, 4a, 4b, and 5a with a chop reference
position located 3
from the source positions. The observed positions (J2000) are:
IRAS 2A:
,
;
IRAS 4A:
,
;
and
IRAS 4B:
,
(Jørgensen et al. 2009).
Table 1 summarizes the lines observed with HIFI
together with complementary lower-J lines obtained with
ground-based telescopes. The Herschel data were taken using the wide band spectrometer (WBS) and high resolution spectrometer (HRS)
backends. Owing to the higher noise (
more) in HRS
than WBS, mainly WBS data are presented here. Only the narrow C 18O 5-4 lines use the HRS data.
Integration times (on+off) are 10, 20, 30, 40, and 60 min for the
12CO 10-9, C 18O 9-8, 10-9, 13CO 10-9, and
C 18O 5-4 lines respectively. The HIFI beam sizes correspond to
20
(
4700 AU) at 1152 GHz and
42
(
10 000 AU) at 549 GHz. Except for the
12CO 10-9 line, all
isotopologue lines were observed together with H2O lines.
The calibration uncertainty for the HIFI data is of the order of 20% and
the pointing accuracy is around 2
.
The measured line
intensities were converted to the main-beam brightness temperatures
by using a
beam efficiency
for all HIFI lines.
Data processing started from the standard HIFI pipeline in the
Herschel interactive processing environment
(HIPE
) ver. 3.0.1
(Ott et al. 2010), where the
precision is
of the order of a few m s-1.
Further reduction and analysis were done using the
GILDAS-
CLASS
software. The spectra from the H- and V-polarizations were averaged in
order to obtain a better S/N. In some cases a discrepancy of 30%
was found between the two polarizations, in which case only the H band
spectra were used for analysis since their rms is lower.
Table 1: Overview of the observations of IRAS 2A, 4A, and 4B.
Complementary ground-based spectral line observations of
12CO 6-5 were obtained at the 12-m Atacama
Pathfinder EXperiment telescope (APEX), using the CHAMP+
pixel array receiver (Güsten et al. 2008). The
lower-J spectral lines were obtained from the James Clerk Maxwell
Telescope (JCMT) archive and from Jørgensen et al. (2002). Details will
be presented elsewhere (Yildiz et al., in prep.).
Table 2: Observed line intensities.
The observed line profiles are presented in Fig. 1 and the corresponding line intensities in Table 2. For the 12CO 10-9 toward IRAS 2A, the emission from the blue line wing was chopped out due to emission at the reference position located in the blue part of the SVS 13 outflow. A Gaussian fitted to the red component of the line was used to obtain the integrated intensity.
![]() |
Figure 1:
Spectra at the central positions of IRAS 2A, 4A and 4B. Top to bottom: H2O 202-111 line from Kristensen et al. (2010) illustrating the medium and broad components, and spectra of 12CO, 13CO, and C 18O. The red lines correspond to the source velocities as obtained from the low-J C 18O lines. The insert in the C18O 5-4 line for IRAS 4A illustrates the weak medium component with peak
|
Open with DEXTER |
Kristensen et al. (2010) identify three components in the H2O
line profiles centered close to the source velocities: a broad
underlying emission profile (Gaussian with
-30 km s-1), a medium-broad emission profile (
-10 km s-1), and narrow self-absorption lines
(
-3 km s-1); see the H2O 202-111 lines in Fig. 1. The same components are
also seen in the CO line profiles, albeit less prominently than for
H2O. The broad component dominates the
12CO 10-9 lines of IRAS 4A and 4B and is also apparent
in the deep 12CO 6-5 spectrum of IRAS 2A
(Fig. 2). The medium component is best seen in the
13CO 10-9 profiles of IRAS 4A and 4B and as the red
wing of the 12CO 10-9 profile for IRAS 2A. A blow-up of the
very high S/N spectrum of C18O 5-4 for IRAS 4A
(insert in Fig. 1) also reveals a weak
C18O medium-broad profile.
The narrow component is clearly observed in
C18O emission and 12CO low-J self-absorption.
Kristensen et al. (2010) interpret the broad component as
shocked gas along the outflow cavity walls, the medium component
as smaller-scale shocks created by the outflow in the inner (<1000
AU) dense envelope, and the narrow component as the quiescent envelope,
respectively.
3 Analysis and discussion
3.1 Broad and medium components: shocked gas
To quantify the physical properties of the broad outflow component,
line ratios are determined for the wings of the line profiles. Figure 2 shows the CO
6-5/ CO 10-9 ratio as a function of velocity.
The APEX-CHAMP+ CO 6-5 maps of IRAS 4A and 4B
from Yildiz et al. (in prep.) and IRAS 2A from
van Kempen et al. (2009) are resampled
to a 20
beam so that both lines refer to the same beam. The
ratios are compared with model non-LTE excitation line intensities
calculated using the
RADEX
code (van der Tak et al. 2007)
(Fig. A.1, Appendix A). The density within a
20
diameter is taken to be
105 cm-3 based on the
modeling results of Jørgensen et al. (2002, see also Sect. 3.3 and Appendix A).
The detection of medium-broad CS 10-9 emission by
Jørgensen et al. (2005b) toward IRAS 4A and 4B indicates densities of the order of a few 106 cm-3. For the range of densities indicated in
Fig. A.1, the line ratios imply high temperatures: IRAS 2A,
-130 K;
IRAS 4A,
-120 K; and IRAS 4B,
-180 K.
The optical depth of the 12CO emission is constrained by
the 12CO 10-9/ 13CO 10-9
ratios. For IRAS 4B, the optical depth of the 12CO line
wings is found to drop with velocity, ranging from
near the center to
0.4 at the
highest velocities where 13CO is detected. This
justifies the assumption that the broad
12CO 10-9 lines are optically thin.
Total CO column densities in the broad component for these conditions
are 4 and
cm-2 for IRAS 4A and 4B,
respectively. For IRAS 2A, the broad column density is
calculated from the CO 6-5 spectrum as
cm-2. Using CO/H
2 = 10-4
gives the H2 column densities listed in Table 3.
![]() |
Figure 2: Ratios of CO 6-5/ CO 10-9. Top: CO line profiles. The CO 6-5 and 10-9 profiles have been multiplied by a factor of 2 for IRAS 2A and 4B. Middle and bottom: ratio of line wing intensity in the specified velocity range indicated in the top panel for the red and blue wings. |
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The medium component attributed to small-scale shocks in the
inner envelope can be probed directly by the
13CO 10-9 data for IRAS 4A and 4B. For
IRAS 2A, the Gaussian fit to the red wing of the 12CO 10-9 is used.
By assuming a similar range of temperatures and densities as for the broad component, beam averaged 12CO column densities of 2, 6,
and
cm-2 are found for IRAS 2A, 4A,
and 4B respectively, if the lines are optically thin and using
12C/13C = 65. The very weak medium component found in
the C18O 5-4 profile for IRAS 4A agrees with this value if the
emission arises from a compact (few
)
source. Assuming
CO/H
2 = 10-4 leads to the numbers in Table 3. The overall uncertainty in all column densities is a factor of 2 due to
the range of physical conditions used to derive them and
uncertainties in the adopted CO/H2 ratio and calibration. The total amount of shocked gas is <1% of the total gas column density in the beam for each source (Jørgensen et al. 2002).
3.2 Narrow component: bulk warm envelope
Table 3: Summary of column densities, N(H2) in cm-2 in the broad and medium components in 20'' beam.
![]() |
Figure 3: Dependence of line intensities on temperature T0 of C18O ( left) and 13CO ( right) for an ``anti-jump'' model of the CO abundance in the IRAS 2A envelope. The line intensities are measured relative to a model where the CO abundance is undepleted at all radii. Each curve therefore represents the fraction of the line intensity for the given transition, which has its origin in gas at temperatures below T0. The dashed lines indicate the levels corresponding to 50 and 90% respectively. |
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The narrow width of the C18O emission clearly indicates an origin
in the quiescent envelope. Naively, one would associate emission
coming from a level with
K (9-8)
with the warm gas in the innermost part of the envelope. To test this
hypothesis, a series of envelope models was run with varying CO
abundance profiles. The models were constructed assuming a power-law
density structure and then calculating the temperature structure by
fitting both the far-infrared spectral energy distribution and the
submillimeter spatial extent (Jørgensen et al. 2002). Figure 3 compares the fractional line intensities for
the C18O and 13CO transitions in a spherical envelope model
for IRAS 2A as a function of temperature. In these models, the
abundance in the outer envelope was kept high,
with respect to H2 (all
available gas-phase carbon in CO), decreasing by a factor of 1000 at
temperatures higher than a specific temperature, T0 (a so-called
``anti-jump'' model (see Schöier et al. 2004, for nomenclature). These
models thereby give an estimate of the fraction of the line emission
for a given transition (in the respective telescope beams) which has
its origin at temperatures lower than T0.
For C18O, 90% of the emission in the transitions up to and including the 5-4 HIFI transition has its origin at temperatures lower than 25-30 K, meaning that these transitions are predominantly sensitive to the outer parts of the protostellar envelope. The 9-8 transition is more sensitive to the warm parts of the envelope, but still 50% of the line flux appears to come from the outer envelope with temperatures less than 50 K. The 13CO transitions become rapidly optically thick in the outer envelopes: even for the 9-8 transition, 90% of the line flux can be associated with the envelope material with temperatures lower than 40 K.
The C18O 9-8 line
is clearly a much more sensitive probe of a CO ice
evaporation zone than any other observed CO line. Jørgensen et al. (2005c)
showed that the low-J C18O lines require a drop in the
abundance at densities higher than
cm-3 due to
freeze-out. However, they did not have strong proof for CO evaporation
in the inner part from that dataset. Using the temperature and density
structure for IRAS 2A as described above, we computed the
C18O line intensities in the respective telescope beams following the
method by Jørgensen et al. (2005c). In this ``anti-jump'' model,
the outer C18O abundance is kept fixed at
,
whereas the inner abundance
and
the freeze-out density
are free parameters.
A
fit to only the C18O 1-0, 2-1 and 3-2 lines
gives best-fit values of
and
cm-3, consistent with those
of Jørgensen et al. (2005c). However, this model underproduces the higher-J lines by a factor of 3-4 (Fig. B.2 in Appendix B).
To solve this underproduction, the inner
abundance has to be increased in a so-called ``drop-abundance'' profile.
The fit parameters are now the inner abundance
and the
evaporation temperature
,
keeping
and
fixed at the above values. Figure B.5 in Appendix B shows the
plots to the
C18O 6-5 and 9-8 lines. The evaporation temperature is not
well constrained, but low temperatures of
25 K are
favored because theyproduce more C18O 5-4 emission.
The best-fit
indicates a jump of a factor of 5
compared with
.
Alternatively,
can be kept
fixed at 25 K and both
and
can be varied by
fitting all five lines simultaneously. In this case, the same best-fit
value for
is found but only an upper limit on
of
.
Thus, for this physical model,
,
implying that a jump in the abundance is needed for IRAS 2A.
4 Conclusions
Spectrally resolved Herschel/HIFI observations of high-J CO
lines up to 12CO 10-9 and
C 18O 9-8 have been performed toward three
low-mass young stellar objects for the first time. These data provide
strong constraints on the density and temperature in the various
physical components, such as the quiescent envelope, extended
outflowing gas, and small-scale shocks in the inner envelope. The
derived column densities and temperatures are important for
comparison with water and other molecules such as O2, for which
HIFI observations are planned. Furthermore, it is shown conclusively
that in order to reproduce higher-J C18O lines within
the context of the adopted physical model, a jump in the CO
abundance due to evaporation is required in the inner envelope,
something that was inferred, but not measured, from ground-based
observations. Combination with even higher-J CO lines
to be obtained with Herschel/PACS in the frame of the WISH
key program will allow further quantification of the different
physical processes invoked to explain the origin of the high-Jemission.
Acknowledgements
The authors are grateful to many funding agencies and the HIFI-ICC staff who has been contributing for the construction of Herschel and HIFI for many years. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and 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, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronómico 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 Zurich, FHNW; USA: Caltech, JPL, NHSC.
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Online Material
Appendix A: Radex model
Figure A.1 shows the CO 6-5/10-9 line ratios for a slab model with a range of temperatures and densities.![]() |
Figure A.1: Model line ratios of CO 6-5/10-9 for a slab model with a range of temperatures and densities. The adopted CO column density is 1017 cm-2 with a line width of 10 km s-1, comparable to the inferred values. For these parameters the lines involved are optically thin. The colored lines give the range of densities within the 20'' beam for the three sources based on the models of Jørgensen et al. (2002). |
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Appendix B: Abundance profiles for IRAS 2A
Among the three sources, IRAS 2A has been selected for detailed CO abundance profile modeling because more data are available on this source, and because its physical and chemical structure has been well characterized through the high angular resolution submillimeter single dish and interferometric observations of Jørgensen et al. (2005a,2002). The physical parameters are taken from the continuum modeling results of Jørgensen et al. (2002). In that paper, the 1D dust radiative transfer code
DUSTY
(Ivezic & Elitzur 1997) was used assuming a power law to describe the
density gradient. The dust temperature as function of radius was
calculated self-consistently through radiative transfer given a
central source luminosity. Best-fit model parameters were obtained by
comparison with the spectral energy distribution and the submillimeter
continuum spatial extent. The resulting envelope structure parameters
are used as input to the Ratran
radiative transfer modeling
code (Hogerheijde & van der Tak 2000) to model the CO line intensities for a
given CO abundance structure through the envelope. The model
extends to 11000 AU from the protostar, where the density has dropped
to

The C18O lines are used to determine the CO abundance structure because the lines of this isotopologue are largely optically thin and because they have well-defined Gaussian line shapes originating from the quiescent envelope without strong contaminations from outflows. Three types of abundance profiles are examined, namely ``constant'', ``anti-jump'' and ``drop'' abundance profiles. Illustrative models are shown in Fig. B.1 and the results from these models are summarized in Table B.1.
![]() |
Figure B.1:
Examples of constant, anti-jump, and drop abundance profiles for IRAS 2A for
|
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Table B.1: Summary of CO abundance profiles for IRAS 2A.
B.1 Constant abundance model
The simplest approach is to adopt a constant abundance across the entire envelope. However, with this approach, and within the framework of the adopted source model, it is not possible to simultaneously reproduce all line intensities. This was already shown by Jørgensen et al. (2005c). For lower abundances it is possible to reproduce the lower-J lines, while higher abundances are required for higher-J lines. In Fig. B.2 the C18O spectra of a constant-abundance profile are shown for an abundance of
B.2 Anti-jump abundance models
The anti-jump model is commonly adopted in models of pre-stellar cores without a central heating source (e.g., Tafalla et al. 2004; Bergin & Snell 2002). Following Jørgensen et al. (2005c), an anti-jump abundance profile was employed by varying the desorption density,



The best fit to the three lowest C18O lines (1-0, 2-1 and 3-2)
is consistent with that found by Jørgensen et al. (2005c),
corresponding to
cm-3 and
(CO abundance of
). In the
fits, the calibration uncertainty
of each line (ranging from 20 to 30%) is taken into account.
These modeled spectra are overplotted on the observed spectra in
Fig. B.2 as the blue lines, and show that the anti-jump
profile fits well the lower-J lines but very much underproduces the
higher-J lines.
The value of X0 was verified a posteriori by keeping
at two different values of
and
cm-3. This is illustrated in Fig. B.3 where the
contours show that for both values of
,
the best-fit value of X0 is
,
the value also found in Jørgensen et al. (2005c). The
contours have been calculated from the lower-J lines only, as these are paramount in constraining the value of X0. Different
plots were made, where it was clear that higher-J lines only constrain
,
as expected. The effect of
is illustrated in Fig. B.4 for the two values given above.
![]() |
Figure B.2:
Best fit constant (green), anti-jump (blue) and drop abundance (red) Ratran models overplotted on the observed spectra. All
spectra refer to single pointing observations. The
calibration uncertainty for each spectrum is around 20-30 |
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![]() |
Figure B.3:
The |
Open with DEXTER |
![]() |
Figure B.4:
The IRAS 2A spectra for the X0 and |
Open with DEXTER |
![]() |
Figure B.5:
Reduced |
Open with DEXTER |
B.3 Drop-abundance profile
In order to fit the higher-J lines, it is necessary to employ a
drop-abundance structure in which the inner abundance
increases above the ice evaporation temperature
(Jørgensen et al. 2005c). The abundances
and X0 for
are kept the same as in the anti-jump model, but
is not necessarily the same as X0. In order to
find the best-fit parameters for the higher-J lines, the inner
abundance
and the evaporation temperature
were varied. The
plots (Fig. B.5, left
panel) show best-fit values for an inner abundance of
and an evaporation temperature of
25 K (consistent with the laboratory values), although the latter
value is not strongly constrained. These parameters fit well the
higher-J C18O 6-5 and 9-8 lines (Fig. B.2). The
C18O 5-4 line is underproduced in all models, likely
because the larger HIFI beam picks up extended emission from
additional dense material to the northeast of the source seen in
BIMA C18O 1-0 map (Volgenau et al. 2006).
Because the results do not depend strongly on
,
an
alternative approach is to keep the evaporation temperature fixed at
25 K and vary both
and
by fitting both low-
and high-J lines simultaneously. In this case, only an upper limit
on
of
is found
(Fig. B.5, right panel), whereas the inferred value of
is the same. This figure conclusively illustrates that
,
i.e., that a jump in the abundance due to
evaporation is needed.
The above conclusion is robust within the context of the
adopted physical model. Alternatively, one could investigate
different physical models such as those used by Chiang et al. (2008),
which have a density enhancement in the inner envelope due to a
magnetic shock wall. This density increase could partly mitigate the
need for the abundance enhancement although it is unlikely that the
density jump is large enough to fully compensate. Such models are
outside the scope of this paper. An observational test of our model
would be to image the N2H+ 1-0 line at high angular
resolution: its emission should drop in the inner 900 AU
(
4
)
where N2H+ would be destroyed by the enhanced
gas-phase CO.
Footnotes
- ... region
- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
- ...
- Appendices and acknowledgements (pages 5 to 7) are only available in electronic form at http://www.aanda.org
- ...
(HIPE
- 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.
- ...
- http://www.iram.fr/IRAMFR/GILDAS/
All Tables
Table 1: Overview of the observations of IRAS 2A, 4A, and 4B.
Table 2: Observed line intensities.
Table 3: Summary of column densities, N(H2) in cm-2 in the broad and medium components in 20'' beam.
Table B.1: Summary of CO abundance profiles for IRAS 2A.
All Figures
![]() |
Figure 1:
Spectra at the central positions of IRAS 2A, 4A and 4B. Top to bottom: H2O 202-111 line from Kristensen et al. (2010) illustrating the medium and broad components, and spectra of 12CO, 13CO, and C 18O. The red lines correspond to the source velocities as obtained from the low-J C 18O lines. The insert in the C18O 5-4 line for IRAS 4A illustrates the weak medium component with peak
|
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In the text |
![]() |
Figure 2: Ratios of CO 6-5/ CO 10-9. Top: CO line profiles. The CO 6-5 and 10-9 profiles have been multiplied by a factor of 2 for IRAS 2A and 4B. Middle and bottom: ratio of line wing intensity in the specified velocity range indicated in the top panel for the red and blue wings. |
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In the text |
![]() |
Figure 3: Dependence of line intensities on temperature T0 of C18O ( left) and 13CO ( right) for an ``anti-jump'' model of the CO abundance in the IRAS 2A envelope. The line intensities are measured relative to a model where the CO abundance is undepleted at all radii. Each curve therefore represents the fraction of the line intensity for the given transition, which has its origin in gas at temperatures below T0. The dashed lines indicate the levels corresponding to 50 and 90% respectively. |
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In the text |
![]() |
Figure A.1: Model line ratios of CO 6-5/10-9 for a slab model with a range of temperatures and densities. The adopted CO column density is 1017 cm-2 with a line width of 10 km s-1, comparable to the inferred values. For these parameters the lines involved are optically thin. The colored lines give the range of densities within the 20'' beam for the three sources based on the models of Jørgensen et al. (2002). |
Open with DEXTER | |
In the text |
![]() |
Figure B.1:
Examples of constant, anti-jump, and drop abundance profiles for IRAS 2A for
|
Open with DEXTER | |
In the text |
![]() |
Figure B.2:
Best fit constant (green), anti-jump (blue) and drop abundance (red) Ratran models overplotted on the observed spectra. All
spectra refer to single pointing observations. The
calibration uncertainty for each spectrum is around 20-30 |
Open with DEXTER | |
In the text |
![]() |
Figure B.3:
The |
Open with DEXTER | |
In the text |
![]() |
Figure B.4:
The IRAS 2A spectra for the X0 and |
Open with DEXTER | |
In the text |
![]() |
Figure B.5:
Reduced |
Open with DEXTER | |
In the text |
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