318 research outputs found
[CII] 158m and [NII] 205m emission from IC 342 - Disentangling the emission from ionized and photo-dissociated regions
Aims: We investigate how much of the [CII] emission in the nucleus of the
nearby spiral galaxy IC 342 is contributed by PDRs and by the ionized gas. We
examine the spatial variations of starburst/PDR activity and study the
correlation of the [CII] line with the [NII] 205{\textmu}m emission line coming
exclusively from the HII regions. Methods: We present small maps of [CII] and
[NII] lines recently observed with the GREAT receiver on board SOFIA. In
particular we present a super-resolution method to derive how unresolved,
kinematically correlated structures in the beam contribute to the observed line
shapes. Results: We find that the emission coming from the ionized gas shows a
kinematic component in addition to the general Doppler signature of the
molecular gas. We interpret this as the signature of two bi-polar lobes of
ionized gas expanding out of the galactic plane. We then show how this requires
an adaptation of our understanding of the geometrical structure of the nucleus
of IC~342. Examining the starburst activity we find ratios
between 400 and 1800 in energy units.
Applying predictions from numerical models of HII and PDR regions to derive the
contribution from the ionized phase to the total [CII] emission we find that
35-90% of the observed [CII] intensity stems from the ionized gas if both
phases contribute. Averaged over the central few hundred parsec we find for the
[CII] contribution a HII-to-PDR ratio of 70:30. Conclusions: The ionized gas in
the center of IC 342 contributes more strongly to the overall [CII] emission
than is commonly observed on larger scales and than is predicted. Kinematic
analysis shows that the majority of the [CII] emission is related to the strong
but embedded star formation in the nuclear molecular ring and only marginally
emitted from the expanding bi-polar lobes of ionized gas.Comment: 20 pages spectra available online:
http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/ submitted to and accepted by
A&
The Photon Dominated Region in the IC 348 molecular cloud
In this paper we discuss the physical conditions of clumpy nature in the IC
348 molecular cloud.
We combine new observations of fully sampled maps in [C I] at 492 GHz and
12CO 4--3, taken with the KOSMA 3 m telescope at about 1' resolution, with
FCRAO data of 12CO 1--0, 13CO 1--0 and far-infrared continuum data observed by
HIRES/IRAS. To derive the physical parameters of the region we analyze the
three different line ratios. A first rough estimate of abundance is obtained
from an LTE analysis. To understand the [C I] and CO emission from the PDRs in
IC 348, we use a clumpy PDR model. With an ensemble of identical clumps, we
constrain the total mass from the observed absolute intensities. Then we apply
a more realistic clump distribution model with a power law index of 1.8 for
clump-mass spectrum and a power law index of 2.3 for mass-size relation.
We provide detailed fits to observations at seven representative positions in
the cloud, revealing clump densities between 4 10 cm and 4
10 cm and C/CO column density ratios between 0.02 and 0.26. The
derived FUV flux from the model fit is consistent with the field calculated
from FIR continuum data, varying between 2 and 100 Draine units across the
cloud. We find that both an ensemble of identical clumps and an ensemble with a
power law clump mass distribution produce line intensities which are in good
agreement (within a factor ~ 2) with the observed intensities. The models
confirm the anti-correlation between the C/CO abundance ratio and the hydrogen
column density found in many regions.Comment: 11 pages, 8 figures, accepted by A&
A clumpy-cloud PDR model of the global far-infrared line emission of the Milky Way
The fractal structure of the interstellar medium suggests that the
interaction of UV radiation with the ISM as described in the context of
photon-dominated regions (PDR) dominates most of the physical and chemical
conditions, and hence the far-infrared and submm emission from the ISM in the
Milky Way. We investigate to what extent the Galactic FIR line emission of the
important species CO, C, C+, and O, as observed by the Cosmic Background
Explorer (COBE) satellite can be modeled in the framework of a clumpy,
UV-penetrated cloud scenario. The far-infrared line emission of the Milky Way
is modeled as the emission from an ensemble of clumps with a power law clump
mass spectrum and mass-size relation with power-law indices consistent with the
observed ISM structure. The individual clump line intensities are calculated
using the KOSMA-tau PDR-model for spherical clumps. The model parameters for
the cylindrically symmetric Galactic distribution of the mass density and
volume filling factor are determined by the observed radial distributions. A
constant FUV intensity, in which the clumps are embedded, is assumed. We show
that this scenario can explain, without any further assumptions and within a
factor of about 2, the absolute FIR-line intensities and their distribution
with Galactic longitude as observed by COBE.Comment: 14 pages, 13 figures, accepted by A&A at the 7th of July, 200
Submillimeter Line Emission from LMC 30Dor: The Impact of a Starburst on a Low Metallicity Environment
(Abridged) The 30 Dor region in the Large Magellanic Cloud (LMC) is the most
vigorous star-forming region in the Local Group. Star formation in this region
is taking place in low-metallicity molecular gas that is exposed to an extreme
far--ultraviolet (FUV) radiation field powered by the massive compact star
cluster R136. We used the NANTEN2 telescope to obtain high-angular resolution
observations of the 12CO 4-3, 7-6, and 13CO 4-3 rotational lines and [CI]
3P1-3P0 and 3P2-3P1 fine-structure submillimeter transitions in 30Dor-10, the
brightest CO and FIR-emitting cloud at the center of the 30Dor region. We
derived the properties of the low-metallicity molecular gas using an
excitation/radiative transfer code and found a self-consistent solution of the
chemistry and thermal balance of the gas in the framework of a clumpy cloud PDR
model. We compared the derived properties with those in the N159W region, which
is exposed to a more moderate far-ultraviolet radiation field compared with
30Dor-10, but has similar metallicity. We also combined our CO detections with
previously observed low-J CO transitions to derive the CO spectral-line energy
distribution in 30Dor-10 and N159W. The separate excitation analysis of the
submm CO lines and the neutral carbon fine structure lines shows that the mid-J
CO and [CI]-emitting gas in the 30Dor-10 region has a temperature of about 160
K and a H2 density of about 10^4 cm^-3. We find that the molecular gas in
30Dor-10 is warmer and has a lower beam filling factor compared to that of
N159W, which might be a result of the effect of a strong FUV radiation field
heating and disrupting the low--metallicity molecular gas. We use a clumpy PDR
model (including the [CII] line intensity reported in the literature) to
constrain the FUV intensity to about chi_0 ~ 3100 and an average total H
density of the clump ensemble of about 10^5 cm^-3 in 30Dor-10.Comment: 11 pages, 8 figures. Accepted for publication in A&
The structure of hot gas in Cepheus B
By observing radiation-affected gas in the Cepheus B molecular cloud we probe
whether the sequential star formation in this source is triggered by the
radiation from newly formed stars. We used the dual band receiver GREAT onboard
SOFIA to map [C II] and CO 13--12 and 11--10 in Cep B and compared the spatial
distribution and the spectral profiles with complementary ground-based data of
low- transitions of CO isotopes, atomic carbon, and the radio continuum. The
interaction of the radiation from the neighboring OB association creates a
large photon-dominated region (PDR) at the surface of the molecular cloud
traced through the photoevaporation of C^+. Bright internal PDRs of hot gas are
created around the embedded young stars, where we detect evidence of the
compression of material and local velocity changes; however, on the global
scale we find no indications that the dense molecular material is dynamically
affected.Comment: Accepted for publication in A&A (SOFIA/GREAT special issue
The origin of the [C II] emission in the S140 PDRs - new insights from HIFI
Using Herschel's HIFI instrument we have observed [C II] along a cut through
S140 and high-J transitions of CO and HCO+ at two positions on the cut,
corresponding to the externally irradiated ionization front and the embedded
massive star forming core IRS1. The HIFI data were combined with available
ground-based observations and modeled using the KOSMA-tau model for photon
dominated regions. Here we derive the physical conditions in S140 and in
particular the origin of [C II] emission around IRS1. We identify three
distinct regions of [C II] emission from the cut, one close to the embedded
source IRS1, one associated with the ionization front and one further into the
cloud. The line emission can be understood in terms of a clumpy model of
photon-dominated regions. At the position of IRS1, we identify at least two
distinct components contributing to the [C II] emission, one of them a small,
hot component, which can possibly be identified with the irradiated outflow
walls. This is consistent with the fact that the [C II] peak at IRS1 coincides
with shocked H2 emission at the edges of the outflow cavity. We note that
previously available observations of IRS1 can be well reproduced by a
single-component KOSMA-tau model. Thus it is HIFI's unprecedented spatial and
spectral resolution, as well as its sensitivity which has allowed us to uncover
an additional hot gas component in the S140 region.Comment: accepted for publication in Astronomy and Astrophysics (HIFI special
issue
Photon Dominated Regions in NGC 3603
Aims: We aim at deriving the excitation conditions of the interstellar gas as
well as the local FUV intensities in the molecular cloud surrounding NGC 3603
to get a coherent picture of how the gas is energized by the central stars.
Methods: The NANTEN2-4m submillimeter antenna is used to map the [CI] 1-0, 2-1
and CO 4-3, 7-6 lines in a 2' x 2' region around the young OB cluster NGC 3603
YC. These data are combined with C18O 2-1 data, HIRES-processed IRAS 60 and 100
micron maps of the FIR continuum, and Spitzer/IRAC maps. Results: The NANTEN2
observations show the presence of two molecular clumps located south-east and
south-west of the cluster and confirm the overall structure already found by
previous CS and C18O observations. We find a slight position offset of the peak
intensity of CO and [CI], and the atomic carbon appears to be further extended
compared to the molecular material. We used the HIRES far-infrared dust data to
derive a map of the FUV field heating the dust. We constrain the FUV field to
values of \chi = 3 - 6 \times 10^3 in units of the Draine field across the
clouds. Approximately 0.2 to 0.3 % of the total FUV energy is re-emitted in the
[CII] 158 {\mu}m cooling line observed by ISO. Applying LTE and escape
probability calculations, we derive temperatures (TMM1 = 43 K, TMM2 = 47 K),
column densities (N(MM1) = 0.9 \times 10^22 cm^-2, N(MM2) = 2.5 \times 10^22
cm^-2) and densities (n(MM1) = 3 \times 10^3 cm^-3, n(MM2) = 10^3 -10^4 cm^-3)
for the two observed molecular clumps MM1 and MM2. Conclusions: The cluster is
strongly interacting with the ambient molecular cloud, governing its structure
and physical conditions. A stability analysis shows the existence of
gravitationally collapsing gas clumps which should lead to star formation.
Embedded IR sources have already been observed in the outskirts of the
molecular cloud and seem to support our conclusions.Comment: 13 pages, 10 figures, accepted for publication by A&
Velocity-resolved [CII] emission and [CII]/FIR Mapping along Orion with Herschel
We present the first 7.5'x11.5' velocity-resolved map of the [CII]158um line
toward the Orion molecular cloud-1 (OMC-1) taken with the Herschel/HIFI
instrument. In combination with far-infrared (FIR) photometric images and
velocity-resolved maps of the H41alpha hydrogen recombination and CO J=2-1
lines, this data set provides an unprecedented view of the intricate
small-scale kinematics of the ionized/PDR/molecular gas interfaces and of the
radiative feedback from massive stars. The main contribution to the [CII]
luminosity (~85%) is from the extended, FUV-illuminated face of the cloud
G_0>500, n_H>5x10^3 cm^-3) and from dense PDRs (G_0~10^4, n_H~10^5 cm^-3) at
the interface between OMC-1 and the HII region surrounding the Trapezium
cluster. Around 15% of the [CII] emission arises from a different gas component
without CO counterpart. The [CII] excitation, PDR gas turbulence, line opacity
(from [13CII]) and role of the geometry of the illuminating stars with respect
to the cloud are investigated. We construct maps of the [CII]/FIR and FIR/M_Gas
ratios and show that [CII]/FIR decreases from the extended cloud component
(10^-2-10^-3) to the more opaque star-forming cores (10^-3-10^-4). The lowest
values are reminiscent of the "[CII] deficit" seen in local ultra-luminous IR
galaxies hosting vigorous star formation. Spatial correlation analysis shows
that the decreasing [CII]/FIR ratio correlates better with the column density
of dust through the molecular cloud than with FIR/M_Gas. We conclude that the
[CII] emitting column relative to the total dust column along each line of
sight is responsible for the observed [CII]/FIR variations through the cloud.Comment: 21 pages, 17 figures. Accepted for publication in the Astrophysical
Journal (2015 August 12). Figures 2, 6 and 7 are bitmapped to lower
resolution. This is version 2 after minor editorial changes. Notes added
after proofs include
[12CII] and [13CII] 158 mum emission from NGC 2024: Large column densities of ionized carbon
Context: We analyze the NGC 2024 HII region and molecular cloud interface
using [12CII] and [13CII] observations. Aims: We attempt to gain insight into
the physical structure of the interface layer between the molecular cloud and
the HII region. Methods. Observations of [12CII] and [13CII] emission at 158
{\mu}m with high spatial and spectral resolution allow us to study the detailed
structure of the ionization front and estimate the column densities and
temperatures of the ionized carbon layer in the PDR. Results: The [12CII]
emission closely follows the distribution of the 8 mum continuum. Across most
of the source, the spectral lines have two velocity peaks similar to lines of
rare CO isotopes. The [13CII] emission is detected near the edge-on ionization
front. It has only a single velocity component, which implies that the [12CII]
line shape is caused by self-absorption. An anomalous hyperfine line-intensity
ratio observed in [13CII] cannot yet be explained. Conclusions: Our analysis of
the two isotopes results in a total column density of N(H)~1.6\times10^23 cm^-2
in the gas emitting the [CII] line. A large fraction of this gas has to be at a
temperature of several hundred K. The self-absorption is caused by a cooler
(T<=100 K) foreground component containing a column density of N(H)~10^22
cm^-2
A Sample of [CII] Clouds Tracing Dense Clouds in Weak FUV Fields observed by Herschel
The [CII] fine--structure line at 158um is an excellent tracer of the warm
diffuse gas in the ISM and the interfaces between molecular clouds and their
surrounding atomic and ionized envelopes. Here we present the initial results
from Galactic Observations of Terahertz C+ (GOTC+), a Herschel Key Project
devoted to study the [CII] fine structure emission in the galactic plane using
the HIFI instrument. We use the [CII] emission together with observations of CO
as a probe to understand the effects of newly--formed stars on their
interstellar environment and characterize the physical and chemical state of
the star-forming gas. We collected data along 16 lines--of--sight passing near
star forming regions in the inner Galaxy near longitudes 330 degrees and 20
degrees. We identify fifty-eight [CII] components that are associated with
high--column density molecular clouds as traced by 13CO emission. We combine
[CII], 12CO, and 13CO observations to derive the physical conditions of the
[CII]--emitting regions in our sample of high--column density clouds based on
comparison with results from a grid of Photon Dominated Region (PDR) models.
From this unbiased sample, our results suggest that most of [CII] emission
originates from clouds with H2 volume densities between 10e3.5 and 10e5.5 cm^-3
and weak FUV strength (CHI_0=1-10). We find two regions where our analysis
suggests high densities >10e5 cm^-3 and strong FUV fields (CHI=10e4-10e6),
likely associated with massive star formation. We suggest that [CII] emission
in conjunction with CO isotopes is a good tool to differentiate between regions
of massive star formation (high densities/strong FUV fields) and regions that
are distant from massive stars (lower densities/weaker FUV fields) along the
line--of--sightComment: To be published in A&A HIFI Special Editio
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