262 research outputs found
Water in massive star-forming regions: HIFI observations of W3 IRS5
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.Comment: Accepted for publication in the A&A HIFI special issu
Water abundances in high-mass protostellar envelopes: Herschel observations with HIFI
We derive the dense core structure and the water abundance in four massive
star-forming regions which may help understand the earliest stages of massive
star formation. We present Herschel-HIFI observations of the para-H2O 1_11-0_00
and 2_02-1_11 and the para-H2-18O 1_11-0_00 transitions. The envelope
contribution to the line profiles is separated from contributions by outflows
and foreground clouds. The envelope contribution is modelled using Monte-Carlo
radiative transfer codes for dust and molecular lines (MC3D and RATRAN), with
the water abundance and the turbulent velocity width as free parameters. While
the outflows are mostly seen in emission in high-J lines, envelopes are seen in
absorption in ground-state lines, which are almost saturated. The derived water
abundances range from 5E-10 to 4E-8 in the outer envelopes. We detect cold
clouds surrounding the protostar envelope, thanks to the very high quality of
the Herschel-HIFI data and the unique ability of water to probe them. Several
foreground clouds are also detected along the line of sight. The low H2O
abundances in massive dense cores are in accordance with the expectation that
high densities and low temperatures lead to freeze-out of water on dust grains.
The spread in abundance values is not clearly linked to physical properties of
the sources.Comment: 8 pages, 5 figures, accepted for publication the 15/07/2010 by
Astronomy&Astrophysics as a letter in the Herschel-HIFI special issu
Sensitive limits on the abundance of cold water vapor in the DM Tau protoplanetary disk
We performed a sensitive search for the ground-state emission lines of ortho-
and para-water vapor in the DM Tau protoplanetary disk using the Herschel/HIFI
instrument. No strong lines are detected down to 3sigma levels in 0.5 km/s
channels of 4.2 mK for the 1_{10}--1_{01} line and 12.6 mK for the
1_{11}--0_{00} line. We report a very tentative detection, however, of the
1_{10}--1_{01} line in the Wide Band Spectrometer, with a strength of
T_{mb}=2.7 mK, a width of 5.6 km/s and an integrated intensity of 16.0 mK km/s.
The latter constitutes a 6sigma detection. Regardless of the reality of this
tentative detection, model calculations indicate that our sensitive limits on
the line strengths preclude efficient desorption of water in the UV illuminated
regions of the disk. We hypothesize that more than 95-99% of the water ice is
locked up in coagulated grains that have settled to the midplane.Comment: 5 pages, 3 figures. Accepted for publication in the Herschel HIFI
special issue of A&
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Fort Lewis electric energy baseline and efficiency resource assessment
The mission of the US Department of Energy (DOE) Federal Energy Management Program (FEMP) is to lead the improvement of energy efficiency and fuel flexibility within the federal sector. Through Pacific Northwest Laboratory, FEMP is developing a fuel-neutral approach for identifying, evaluating, and acquiring all cost-effective energy projects at federal installations. In this report, we describe PNL's assessment of the electric energy efficiency resource potential at Fort Lewis (near Tacoma, WA). Through this assessment, we developed an estimate of the electricity use baseline and efficiency improvement potential for major sectors and end uses at the Fort. Developing the baseline was essential to segment the end uses that are targets for broad-based efficiency improvement programs and to provide TPU with the basis for its proposal to Bonneville. An estimate of the efficiency resource is presented to reflect the available quantity of resource for three electricity price ranges. The baseline and efficiency resource estimates did not identify all possible areas of opportunity, but instead identified the majority of the resource; areas of additional opportunity are noted, to encourage further effort. 2 figs., 2 tabs
Recommended from our members
Fort Lewis electric energy baseline and efficiency resource assessment
In support of the US DOE Federal Energy Management Program, the Pacific Northwest Laboratory is developing a fuel-neutral approach for identifying, evaluating, and acquiring all cost-effective energy projects at federal installations. Fort Lewis, a US Army installation near Tacoma, Washington, was selected as the pilot site for developing this approach. This site was chosen in conjunction with the interests of the Bonneville Power Administration to develop programs for its federal sector customers and the Army Forces Command to develop an in-house program to upgrade the energy efficiency of its installations. This report documents the electricity assessment portion of the approach, providing an estimate of the electricity use baseline and efficiency improvement potential for major sectors and end uses at the Fort. Although the assessment did not identify all possible efficiency improvement opportunities, it is estimated that electricity use can be reduced by at least 20% cost-effectively at the $0.045/kWh marginal cost of electricity in the Pacific Northwest. 12 refs., 3 figs., 7 tabs
HERSCHEL-HIFI spectroscopy of the intermediate mass protostar NGC7129 FIRS 2
HERSCHEL-HIFI observations of water from the intermediate mass protostar
NGC7129 FIRS 2 provide a powerful diagnostic of the physical conditions in this
star formation environment. Six spectral settings, covering four H216O and two
H218O lines, were observed and all but one H218O line were detected. The four
H2 16 O lines discussed here share a similar morphology: a narrower, \approx 6
km/s, component centered slightly redward of the systemic velocity of NGC7129
FIRS 2 and a much broader, \approx 25 km/s component centered blueward and
likely associated with powerful outflows. The narrower components are
consistent with emission from water arising in the envelope around the
intermediate mass protostar, and the abundance of H2O is constrained to \approx
10-7 for the outer envelope. Additionally, the presence of a narrow
self-absorption component for the lowest energy lines is likely due to
self-absorption from colder water in the outer envelope. The broader component,
where the H2O/CO relative abundance is found to be \approx 0.2, appears to be
tracing the same energetic region that produces strong CO emission at high J.Comment: 6 pages, 4 figures, accepted by A&
Water in Star-Forming Regions with the Herschel Space Observatory (WISH): Overview of key program and first results
`Water In Star-forming regions with Herschel' (WISH) is a key program on the
Herschel Space Observatory designed to probe the physical and chemical
structure of young stellar objects using water and related molecules and to
follow the water abundance from collapsing clouds to planet-forming disks.
About 80 sources are targeted covering a wide range of luminosities and
evolutionary stages, from cold pre-stellar cores to warm protostellar envelopes
and outflows to disks around young stars. Both the HIFI and PACS instruments
are used to observe a variety of lines of H2O, H218O and chemically related
species. An overview of the scientific motivation and observational strategy of
the program is given together with the modeling approach and analysis tools
that have been developed. Initial science results are presented. These include
a lack of water in cold gas at abundances that are lower than most predictions,
strong water emission from shocks in protostellar environments, the importance
of UV radiation in heating the gas along outflow walls across the full range of
luminosities, and surprisingly widespread detection of the chemically related
hydrides OH+ and H2O+ in outflows and foreground gas. Quantitative estimates of
the energy budget indicate that H2O is generally not the dominant coolant in
the warm dense gas associated with protostars. Very deep limits on the cold
gaseous water reservoir in the outer regions of protoplanetary disks are
obtained which have profound implications for our understanding of grain growth
and mixing in disks.Comment: 71 pages, 10 figures, PASP, in pres
From international health to global health: how to foster a better dialogue between empirical and normative disciplines.
BACKGROUND: Public health recommendations are usually based on a mixture of empirical evidence and normative arguments: to argue that authorities ought to implement an intervention that has proven effective in improving people's health requires a normative position confirming that the authorities are responsible for improving people's health. While public health (at the national level) is based on a widely accepted normative starting point - namely, that it is the responsibility of the state to improve people's health - there is no widely accepted normative starting point for international health or global health. As global health recommendations may vary depending on the normative starting point one uses, global health research requires a better dialogue between researchers who are trained in empirical disciplines and researchers who are trained in normative disciplines. DISCUSSION: Global health researchers with a background in empirical disciplines seem reluctant to clarify the normative starting point they use, perhaps because normative statements cannot be derived directly from empirical evidence, or because there is a wide gap between present policies and the normative starting point they personally support. Global health researchers with a background in normative disciplines usually do not present their work in ways that help their colleagues with a background in empirical disciplines to distinguish between what is merely personal opinion and professional opinion based on rigorous normative research. If global health researchers with a background in empirical disciplines clarified their normative starting point, their recommendations would become more useful for their colleagues with a background in normative disciplines. If global health researchers who focus on normative issues used adapted qualitative research guidelines to present their results, their findings would be more useful for their colleagues with a background in empirical disciplines. Although a single common paradigm for all scientific disciplines that contribute to global health research may not be possible or desirable, global health researchers with a background in empirical disciplines and global health researchers with a background in normative disciplines could present their 'truths' in ways that would improve dialogue. This paper calls for an exchange of views between global health researchers and editors of medical journals
Herschel observations of the hydroxyl radical (OH) in young stellar objects
Water in Star-forming regions with Herschel (WISH) is a Herschel Key Program
investigating the water chemistry in young stellar objects (YSOs) during
protostellar evolution. Hydroxyl (OH) is one of the reactants in the chemical
network most closely linked to the formation and destruction of H2O.
High-temperature chemistry connects OH and H2O through the OH + H2 H2O + H
reactions. Formation of H2O from OH is efficient in the high-temperature regime
found in shocks and the innermost part of protostellar envelopes. Moreover, in
the presence of UV photons, OH can be produced from the photo-dissociation of
H2O. High-resolution spectroscopy of the OH 163.12 micron triplet towards HH 46
and NGC 1333 IRAS 2A was carried out with the Heterodyne Instrument for the Far
Infrared (HIFI) on board Herschel. The low- and intermediate-mass YSOs HH 46,
TMR 1, IRAS 15398-3359, DK Cha, NGC 7129 FIRS 2, and NGC 1333 IRAS 2A were
observed with the Photodetector Array Camera and Spectrometer (PACS) in four
transitions of OH and two [OI] lines. The OH transitions at 79, 84, 119, and
163 micron and [OI] emission at 63 and 145 micron were detected with PACS
towards the class I low-mass YSOs as well as the intermediate-mass and class I
Herbig Ae sources. No OH emission was detected from the class 0 YSO NGC 1333
IRAS 2A, though the 119 micron was detected in absorption. With HIFI, the
163.12 micron was not detected from HH 46 and only tentatively detected from
NGC 1333 IRAS 2A. The combination of the PACS and HIFI results for HH 46
constrains the line width (FWHM > 11 km/s) and indicates that the OH emission
likely originates from shocked gas. This scenario is supported by trends of the
OH flux increasing with the [OI] flux and the bolometric luminosity. Similar OH
line ratios for most sources suggest that OH has comparable excitation
temperatures despite the different physical properties of the sources.Comment: Accepted for publication in Astronomy and Astrophysics (Herschel
special issue
Herschel-HIFI detections of hydrides towards AFGL 2591 (Envelope emission versus tenuous cloud absorption)
The Heterodyne Instrument for the Far Infrared (HIFI) onboard the Herschel
Space Observatory allows the first observations of light diatomic molecules at
high spectral resolution and in multiple transitions. Here, we report deep
integrations using HIFI in different lines of hydrides towards the high-mass
star forming region AFGL 2591. Detected are CH, CH+, NH, OH+, H2O+, while NH+
and SH+ have not been detected. All molecules except for CH and CH+ are seen in
absorption with low excitation temperatures and at velocities different from
the systemic velocity of the protostellar envelope. Surprisingly, the CH(JF,P =
3/2_2,- - 1/2_1,+) and CH+(J = 1 - 0, J = 2 - 1) lines are detected in emission
at the systemic velocity. We can assign the absorption features to a foreground
cloud and an outflow lobe, while the CH and CH+ emission stems from the
envelope. The observed abundance and excitation of CH and CH+ can be explained
in the scenario of FUV irradiated outflow walls, where a cavity etched out by
the outflow allows protostellar FUV photons to irradiate and heat the envelope
at larger distances driving the chemical reactions that produce these
molecules.Comment: Accepted for publication in Astronomy and Astrophysics (HIFI first
results issue
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