MG
M Goto
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2 records found
1
Journal article
(2018)
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M Goto, J.D. Bailey, S. Hocuk, P. Caselli, G. B. Esplugues, Stephanie Cazaux, M. Spaans
Context. Spectroscopic studies of ices in nearby star-forming regions indicate that ice mantles form on dust grains in two distinct steps, starting with polar ice formation (H2O rich) and switching to apolar ice (CO rich). Aims. We test how well the picture applies to more diffuse and quiescent clouds where the formation of the first layers of ice mantles can be witnessed.
Methods. Medium-resolution near-infrared spectra are obtained toward background field stars behind the Pipe Nebula. Results. The water ice absorption is positively detected at 3.0 µm in seven lines of sight out of 21 sources for which observed spectra are successfully reduced. The peak optical depth of the water ice is significantly lower than those in Taurus with the same AV . The
source with the highest water-ice optical depth shows CO ice absorption at 4.7 µm as well. The fractional abundance of CO ice with respect to water ice is 16+7
−6 %, and about half as much as the values typically seen in low-mass star-forming regions.
Conclusions. A small fractional abundance of CO ice is consistent with some of the existing simulations. Observations of CO2 ice in the early diffuse phase of a cloud play a decisive role in understanding the switching mechanism between polar and apolar ice formation. ...
Methods. Medium-resolution near-infrared spectra are obtained toward background field stars behind the Pipe Nebula. Results. The water ice absorption is positively detected at 3.0 µm in seven lines of sight out of 21 sources for which observed spectra are successfully reduced. The peak optical depth of the water ice is significantly lower than those in Taurus with the same AV . The
source with the highest water-ice optical depth shows CO ice absorption at 4.7 µm as well. The fractional abundance of CO ice with respect to water ice is 16+7
−6 %, and about half as much as the values typically seen in low-mass star-forming regions.
Conclusions. A small fractional abundance of CO ice is consistent with some of the existing simulations. Observations of CO2 ice in the early diffuse phase of a cloud play a decisive role in understanding the switching mechanism between polar and apolar ice formation. ...
Context. Spectroscopic studies of ices in nearby star-forming regions indicate that ice mantles form on dust grains in two distinct steps, starting with polar ice formation (H2O rich) and switching to apolar ice (CO rich). Aims. We test how well the picture applies to more diffuse and quiescent clouds where the formation of the first layers of ice mantles can be witnessed.
Methods. Medium-resolution near-infrared spectra are obtained toward background field stars behind the Pipe Nebula. Results. The water ice absorption is positively detected at 3.0 µm in seven lines of sight out of 21 sources for which observed spectra are successfully reduced. The peak optical depth of the water ice is significantly lower than those in Taurus with the same AV . The
source with the highest water-ice optical depth shows CO ice absorption at 4.7 µm as well. The fractional abundance of CO ice with respect to water ice is 16+7
−6 %, and about half as much as the values typically seen in low-mass star-forming regions.
Conclusions. A small fractional abundance of CO ice is consistent with some of the existing simulations. Observations of CO2 ice in the early diffuse phase of a cloud play a decisive role in understanding the switching mechanism between polar and apolar ice formation.
Methods. Medium-resolution near-infrared spectra are obtained toward background field stars behind the Pipe Nebula. Results. The water ice absorption is positively detected at 3.0 µm in seven lines of sight out of 21 sources for which observed spectra are successfully reduced. The peak optical depth of the water ice is significantly lower than those in Taurus with the same AV . The
source with the highest water-ice optical depth shows CO ice absorption at 4.7 µm as well. The fractional abundance of CO ice with respect to water ice is 16+7
−6 %, and about half as much as the values typically seen in low-mass star-forming regions.
Conclusions. A small fractional abundance of CO ice is consistent with some of the existing simulations. Observations of CO2 ice in the early diffuse phase of a cloud play a decisive role in understanding the switching mechanism between polar and apolar ice formation.
Journal article
(1993)
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Y Han, Isabelle Vergroesen, M Goto, Jenny Dankelman, CPB van der Ploeg, Jos A.E. Spaan
In six open-thorax-anaesthetized dogs with paced hearts and a retrogradely cannulated epicardial lymph vessel, the sensitivity of myocardial lymph pres- sure to left ventricular pressure during systole and during diastole was determined. The lymph vessels were can- nulated using PE-90 tubing, and lymph pressure was measured by connecting the cannula to a microtip press- ure transducer. To obtain the systolic sensitivity, left ven- tricular pressure was changed by clamping the de- scending aorta, which caused left ventricular pressure to increase. The diastolic sensitivity was obtained from natural variation to left ventricular pressure caused by atrial contractions during induced long diastoles. The mean ratio of the pulse in lymph pressure to the pulse in left ventricular pressure was determined: systole: 0.069 + 0.013, n = 213, diastole: 0.76 -+ 0.16, n = 249 and, if possible, linear regression analysis between lymph and left ventricular pressure was performed. The systolic regression coefficients could be determined in six dogs and the diastolic coefficients in three dogs. Dur- ing long diastoles lymph pressure variations are on aver- age 76 per cent of those in the left ventricle. However, during systole, the sensitivity of lymph pressure to left ventricular pressure is more than ten times lower. It is not unlikely that the structural embedment of lymph ves- sels within the myocardium is such that volume vari- ations by cardiac contraction are limited.
...
In six open-thorax-anaesthetized dogs with paced hearts and a retrogradely cannulated epicardial lymph vessel, the sensitivity of myocardial lymph pres- sure to left ventricular pressure during systole and during diastole was determined. The lymph vessels were can- nulated using PE-90 tubing, and lymph pressure was measured by connecting the cannula to a microtip press- ure transducer. To obtain the systolic sensitivity, left ven- tricular pressure was changed by clamping the de- scending aorta, which caused left ventricular pressure to increase. The diastolic sensitivity was obtained from natural variation to left ventricular pressure caused by atrial contractions during induced long diastoles. The mean ratio of the pulse in lymph pressure to the pulse in left ventricular pressure was determined: systole: 0.069 + 0.013, n = 213, diastole: 0.76 -+ 0.16, n = 249 and, if possible, linear regression analysis between lymph and left ventricular pressure was performed. The systolic regression coefficients could be determined in six dogs and the diastolic coefficients in three dogs. Dur- ing long diastoles lymph pressure variations are on aver- age 76 per cent of those in the left ventricle. However, during systole, the sensitivity of lymph pressure to left ventricular pressure is more than ten times lower. It is not unlikely that the structural embedment of lymph ves- sels within the myocardium is such that volume vari- ations by cardiac contraction are limited.