Differences
This shows you the differences between two versions of the page.
Both sides previous revision Previous revision Next revision | Previous revision | ||
start [2021/06/15 15:36] fuente |
start [2021/06/23 15:24] fuente [Presentation] |
||
---|---|---|---|
Line 1: | Line 1: | ||
+ | {{: | ||
+ | |||
====== GEMS project ====== | ====== GEMS project ====== | ||
- | "Gas phase Elemental abundances in Molecular Clouds" | + | ===== Presentation ===== |
- | The goal is to determine the S, C, N, O depletions and X(e-) as a function of visual extinction, in a selected set of prototypical star forming filaments (TMC1, B213/L1495, Barnard 1, NGC 1333, IC348, L1448, B5, Orion A). | + | ### |
+ | "Gas phase Elemental abundances in Molecular Clouds" | ||
+ | ### | ||
+ | ### | ||
+ | The goal is to determine the S, C, N, O depletions and X(e-) as a function of visual extinction, in a selected set of prototypical star forming filaments (TMC 1, B 213/L 1495, Barnard 1, NGC 1333, IC 348, L 1448, B 5, Orion A). | ||
These parameters are the essential ingredients for chemical models and for cloud collapse simulations because they govern the gas cooling and the coupling of the gas with the magnetic field. Hence, they are of paramount importance for star formation galactic studies. From the chemical point of view, the variation of the elemental abundances in gas phase is a valuable information to determine the evolution of dust grains and the composition of the icy grain mantles across the cloud. | These parameters are the essential ingredients for chemical models and for cloud collapse simulations because they govern the gas cooling and the coupling of the gas with the magnetic field. Hence, they are of paramount importance for star formation galactic studies. From the chemical point of view, the variation of the elemental abundances in gas phase is a valuable information to determine the evolution of dust grains and the composition of the icy grain mantles across the cloud. | ||
As an intermediate product, we will provide a complete set of molecular data in dark clouds. | As an intermediate product, we will provide a complete set of molecular data in dark clouds. | ||
- | In particular, our dataset will include high-sensitivity spectroscopic observations of CS, SO, H2S, HCS+, SO2, OCS and H2CS. | + | In particular, our dataset will include high-sensitivity spectroscopic observations of CS, SO, H< |
Up to our knowledge, it constitutes the best S-bearing molecules dataset in dark clouds so far, and a key stone to progress in our understanding of the sulfur chemistry. | Up to our knowledge, it constitutes the best S-bearing molecules dataset in dark clouds so far, and a key stone to progress in our understanding of the sulfur chemistry. | ||
+ | ### | ||
- | ** Frequency and sensitivity coverage | + | ===== Frequency and sensitivity coverage |
- | 3 mm (FSW, rms ~ 10-20 mK) 2mm (FSW, rms ~ 10-20 mK for frequencies | + | 3 mm (FSW, rms ~ 10-20 mK) 2mm (FSW, rms ~ 10-20 mK for frequencies |
+ | | ||
| | ||
- | 85 GHz - 86.8 GHz 133.7 GHz - 135.5 GHz | + | 85.0 |
- | 88.3 GHz- 91.5 GHz | + | 88.3 GHz - 91.5 GHz 137.0 GHz - 138.8 GHz |
- | 92 GHz- 94.8 GHz | + | 92.0 |
- | 95.3 GHz- 97.0 GHz | + | 95.3 GHz - 97.0 GHz 146.4 GHz - 148.3 GHz |
- | 97.6 GHz - 99.4 GHz 158.8 GHz - 160.7 GHz | + | 97.6 GHz - 99.4 GHz 158.8 GHz - 160.7 GHz |
- | 101 GHz - 103 GHz 162.1 GHz - 163.9 GHz | + | 101.0 GHz - 103.0 GHz 162.1 GHz - 163.9 GHz |
- | 105.4 GHz -107.2 GHz | + | 105.4 GHz - 107.2 GHz 167.2 GHz - 169.0 GHz |
- | 108.7 GHz - 110.48 GHz | + | 108.7 GHz - 110.5 GHz 170.5 GHz - 172.3 GHz |
+ | ===== Source list ===== | ||
- | ** Source list ** | + | {{:: |
^ Source ^ J2000 position ^ | ^ Source ^ J2000 position ^ | ||
Line 137: | Line 147: | ||
| l1448-7 | 03:26:23.90 30:42:24.6 | | | l1448-7 | 03:26:23.90 30:42:24.6 | | ||
| l1448-8 | 03:26:39.41 30:42:24.6 | | | l1448-8 | 03:26:39.41 30:42:24.6 | | ||
+ | |||
+ | {{ :: | ||
+ | |||
+ | ^ Source ^ J2000 position ^ | ||
| 1333-c3-1 | 03:29:11.00 31:18:27.4 | | | 1333-c3-1 | 03:29:11.00 31:18:27.4 | | ||
| 1333-c3-2 | 03:29:13.35 31:18:27.4 | | | 1333-c3-2 | 03:29:13.35 31:18:27.4 | | ||
Line 212: | Line 226: | ||
| 79-c1-12 | 03:46:59.42 32:52:17.90 | | | 79-c1-12 | 03:46:59.42 32:52:17.90 | | ||
| 79-c1-13 | 03:46:27.67 32:52:17.90 | | | 79-c1-13 | 03:46:27.67 32:52:17.90 | | ||
+ | |||
+ | {{ :: | ||
+ | |||
+ | ^ Source ^ J2000 position ^ | ||
| Ori-c3-1 | 05: | | Ori-c3-1 | 05: | ||
| Ori-c3-2 | 05: | | Ori-c3-2 | 05: | ||
Line 266: | Line 284: | ||
| Ori-c1-20 | 05:33:17.54 -05:00:41.5 | | | Ori-c1-20 | 05:33:17.54 -05:00:41.5 | | ||
- | {{ ::map_perseo.png? | + | {{ ::figura-tmc1.png? |
- | {{ :: | + | |
- | {{ :: | + | |
- | {{ :: | + | |
+ | ^ Source ^ J2000 position ^ | ||
+ | |TMC1-CAL-1 | ||
+ | |TMC1-CAL-2 | ||
+ | |TMC1-CAL-3 | ||
+ | |TMC1-CAL-4 | 04:41:50.78 +25:41:27.1 | | ||
+ | |TMC1-CAL-5 | 04:41:55.22 +25:41:27.1 | | ||
+ | |TMC1-CAL-6 | 04:41:59.66 +25:41:27.1 | | ||
+ | |TMC1-NH3-1 | ||
+ | |TMC1-NH3-2 | ||
+ | |TMC1-NH3-3 | ||
+ | |TMC1-NH3-4 | 04:41:30.18 +25:48:07.0 | | ||
+ | |TMC1-NH3-5 | 04:41:34.62 +25:48:07.0 | | ||
+ | |TMC1-NH3-6 | 04:41:39.06 +25:48:07.0 | | ||
+ | |TMC1-C2-1 | ||
+ | |TMC1-C2-2 | ||
+ | |TMC1-C2-3 | ||
+ | |TMC1-C2-4 | ||
+ | |TMC1-C2-5 | ||
+ | |TMC1-C2-6 |
Last modified: le 2021/06/23 15:24