Transparency of 2 μ m window of Titan's atmosphere
Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these interva...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Rannou, P. [verfasserIn] |
|---|
| Format: |
E-Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
2018transfer abstract |
|---|
| Umfang: |
16 |
|---|
| Übergeordnetes Werk: |
Enthalten in: ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS - Mekaroonkamol, Parit ELSEVIER, 2023, Kidlington [u.a.] |
|---|---|
| Übergeordnetes Werk: |
volume:151 ; year:2018 ; pages:109-124 ; extent:16 |
| Links: |
|---|
| DOI / URN: |
10.1016/j.pss.2017.11.015 |
|---|
| Katalog-ID: |
ELV041696344 |
|---|
| LEADER | 01000caa a22002652 4500 | ||
|---|---|---|---|
| 001 | ELV041696344 | ||
| 003 | DE-627 | ||
| 005 | 20230625235342.0 | ||
| 007 | cr uuu---uuuuu | ||
| 008 | 180726s2018 xx |||||o 00| ||eng c | ||
| 024 | 7 | |a 10.1016/j.pss.2017.11.015 |2 doi | |
| 028 | 5 | 2 | |a GBV00000000000106A.pica |
| 035 | |a (DE-627)ELV041696344 | ||
| 035 | |a (ELSEVIER)S0032-0633(17)30217-9 | ||
| 040 | |a DE-627 |b ger |c DE-627 |e rakwb | ||
| 041 | |a eng | ||
| 082 | 0 | |a 620 | |
| 082 | 0 | 4 | |a 620 |q DE-600 |
| 082 | 0 | 4 | |a 610 |q VZ |
| 084 | |a 44.87 |2 bkl | ||
| 100 | 1 | |a Rannou, P. |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Transparency of 2 μ m window of Titan's atmosphere |
| 264 | 1 | |c 2018transfer abstract | |
| 300 | |a 16 | ||
| 336 | |a nicht spezifiziert |b zzz |2 rdacontent | ||
| 337 | |a nicht spezifiziert |b z |2 rdamedia | ||
| 338 | |a nicht spezifiziert |b zu |2 rdacarrier | ||
| 520 | |a Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. | ||
| 520 | |a Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. | ||
| 700 | 1 | |a Seignovert, B. |4 oth | |
| 700 | 1 | |a Le Mouélic, S. |4 oth | |
| 700 | 1 | |a Maltagliati, L. |4 oth | |
| 700 | 1 | |a Rey, M. |4 oth | |
| 700 | 1 | |a Sotin, C. |4 oth | |
| 773 | 0 | 8 | |i Enthalten in |n Elsevier Science |a Mekaroonkamol, Parit ELSEVIER |t ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |d 2023 |g Kidlington [u.a.] |w (DE-627)ELV010254102 |
| 773 | 1 | 8 | |g volume:151 |g year:2018 |g pages:109-124 |g extent:16 |
| 856 | 4 | 0 | |u https://doi.org/10.1016/j.pss.2017.11.015 |3 Volltext |
| 912 | |a GBV_USEFLAG_U | ||
| 912 | |a GBV_ELV | ||
| 912 | |a SYSFLAG_U | ||
| 912 | |a SSG-OLC-PHA | ||
| 912 | |a GBV_ILN_66 | ||
| 912 | |a GBV_ILN_91 | ||
| 912 | |a GBV_ILN_165 | ||
| 912 | |a GBV_ILN_234 | ||
| 936 | b | k | |a 44.87 |j Gastroenterologie |q VZ |
| 951 | |a AR | ||
| 952 | |d 151 |j 2018 |h 109-124 |g 16 | ||
| 953 | |2 045F |a 620 | ||
| author_variant |
p r pr |
|---|---|
| matchkey_str |
rannoupseignovertblemoulicsmaltagliatilr:2018----:rnprnyfmidwfias |
| hierarchy_sort_str |
2018transfer abstract |
| bklnumber |
44.87 |
| publishDate |
2018 |
| allfields |
10.1016/j.pss.2017.11.015 doi GBV00000000000106A.pica (DE-627)ELV041696344 (ELSEVIER)S0032-0633(17)30217-9 DE-627 ger DE-627 rakwb eng 620 620 DE-600 610 VZ 44.87 bkl Rannou, P. verfasserin aut Transparency of 2 μ m window of Titan's atmosphere 2018transfer abstract 16 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. Seignovert, B. oth Le Mouélic, S. oth Maltagliati, L. oth Rey, M. oth Sotin, C. oth Enthalten in Elsevier Science Mekaroonkamol, Parit ELSEVIER ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS 2023 Kidlington [u.a.] (DE-627)ELV010254102 volume:151 year:2018 pages:109-124 extent:16 https://doi.org/10.1016/j.pss.2017.11.015 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 44.87 Gastroenterologie VZ AR 151 2018 109-124 16 045F 620 |
| spelling |
10.1016/j.pss.2017.11.015 doi GBV00000000000106A.pica (DE-627)ELV041696344 (ELSEVIER)S0032-0633(17)30217-9 DE-627 ger DE-627 rakwb eng 620 620 DE-600 610 VZ 44.87 bkl Rannou, P. verfasserin aut Transparency of 2 μ m window of Titan's atmosphere 2018transfer abstract 16 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. Seignovert, B. oth Le Mouélic, S. oth Maltagliati, L. oth Rey, M. oth Sotin, C. oth Enthalten in Elsevier Science Mekaroonkamol, Parit ELSEVIER ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS 2023 Kidlington [u.a.] (DE-627)ELV010254102 volume:151 year:2018 pages:109-124 extent:16 https://doi.org/10.1016/j.pss.2017.11.015 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 44.87 Gastroenterologie VZ AR 151 2018 109-124 16 045F 620 |
| allfields_unstemmed |
10.1016/j.pss.2017.11.015 doi GBV00000000000106A.pica (DE-627)ELV041696344 (ELSEVIER)S0032-0633(17)30217-9 DE-627 ger DE-627 rakwb eng 620 620 DE-600 610 VZ 44.87 bkl Rannou, P. verfasserin aut Transparency of 2 μ m window of Titan's atmosphere 2018transfer abstract 16 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. Seignovert, B. oth Le Mouélic, S. oth Maltagliati, L. oth Rey, M. oth Sotin, C. oth Enthalten in Elsevier Science Mekaroonkamol, Parit ELSEVIER ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS 2023 Kidlington [u.a.] (DE-627)ELV010254102 volume:151 year:2018 pages:109-124 extent:16 https://doi.org/10.1016/j.pss.2017.11.015 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 44.87 Gastroenterologie VZ AR 151 2018 109-124 16 045F 620 |
| allfieldsGer |
10.1016/j.pss.2017.11.015 doi GBV00000000000106A.pica (DE-627)ELV041696344 (ELSEVIER)S0032-0633(17)30217-9 DE-627 ger DE-627 rakwb eng 620 620 DE-600 610 VZ 44.87 bkl Rannou, P. verfasserin aut Transparency of 2 μ m window of Titan's atmosphere 2018transfer abstract 16 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. Seignovert, B. oth Le Mouélic, S. oth Maltagliati, L. oth Rey, M. oth Sotin, C. oth Enthalten in Elsevier Science Mekaroonkamol, Parit ELSEVIER ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS 2023 Kidlington [u.a.] (DE-627)ELV010254102 volume:151 year:2018 pages:109-124 extent:16 https://doi.org/10.1016/j.pss.2017.11.015 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 44.87 Gastroenterologie VZ AR 151 2018 109-124 16 045F 620 |
| allfieldsSound |
10.1016/j.pss.2017.11.015 doi GBV00000000000106A.pica (DE-627)ELV041696344 (ELSEVIER)S0032-0633(17)30217-9 DE-627 ger DE-627 rakwb eng 620 620 DE-600 610 VZ 44.87 bkl Rannou, P. verfasserin aut Transparency of 2 μ m window of Titan's atmosphere 2018transfer abstract 16 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. Seignovert, B. oth Le Mouélic, S. oth Maltagliati, L. oth Rey, M. oth Sotin, C. oth Enthalten in Elsevier Science Mekaroonkamol, Parit ELSEVIER ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS 2023 Kidlington [u.a.] (DE-627)ELV010254102 volume:151 year:2018 pages:109-124 extent:16 https://doi.org/10.1016/j.pss.2017.11.015 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 44.87 Gastroenterologie VZ AR 151 2018 109-124 16 045F 620 |
| language |
English |
| source |
Enthalten in ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS Kidlington [u.a.] volume:151 year:2018 pages:109-124 extent:16 |
| sourceStr |
Enthalten in ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS Kidlington [u.a.] volume:151 year:2018 pages:109-124 extent:16 |
| format_phy_str_mv |
Article |
| bklname |
Gastroenterologie |
| institution |
findex.gbv.de |
| dewey-raw |
620 |
| isfreeaccess_bool |
false |
| container_title |
ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |
| authorswithroles_txt_mv |
Rannou, P. @@aut@@ Seignovert, B. @@oth@@ Le Mouélic, S. @@oth@@ Maltagliati, L. @@oth@@ Rey, M. @@oth@@ Sotin, C. @@oth@@ |
| publishDateDaySort_date |
2018-01-01T00:00:00Z |
| hierarchy_top_id |
ELV010254102 |
| dewey-sort |
3620 |
| id |
ELV041696344 |
| language_de |
englisch |
| fullrecord |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">ELV041696344</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230625235342.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">180726s2018 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1016/j.pss.2017.11.015</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">GBV00000000000106A.pica</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)ELV041696344</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(ELSEVIER)S0032-0633(17)30217-9</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2=" "><subfield code="a">620</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">620</subfield><subfield code="q">DE-600</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">610</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">44.87</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Rannou, P.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Transparency of 2 μ m window of Titan's atmosphere</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2018transfer abstract</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">16</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zzz</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">z</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zu</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant.</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant.</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Seignovert, B.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Le Mouélic, S.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Maltagliati, L.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Rey, M.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sotin, C.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="n">Elsevier Science</subfield><subfield code="a">Mekaroonkamol, Parit ELSEVIER</subfield><subfield code="t">ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS</subfield><subfield code="d">2023</subfield><subfield code="g">Kidlington [u.a.]</subfield><subfield code="w">(DE-627)ELV010254102</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:151</subfield><subfield code="g">year:2018</subfield><subfield code="g">pages:109-124</subfield><subfield code="g">extent:16</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doi.org/10.1016/j.pss.2017.11.015</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_U</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ELV</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_U</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHA</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_66</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_91</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_165</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_234</subfield></datafield><datafield tag="936" ind1="b" ind2="k"><subfield code="a">44.87</subfield><subfield code="j">Gastroenterologie</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">151</subfield><subfield code="j">2018</subfield><subfield code="h">109-124</subfield><subfield code="g">16</subfield></datafield><datafield tag="953" ind1=" " ind2=" "><subfield code="2">045F</subfield><subfield code="a">620</subfield></datafield></record></collection>
|
| author |
Rannou, P. |
| spellingShingle |
Rannou, P. ddc 620 ddc 610 bkl 44.87 Transparency of 2 μ m window of Titan's atmosphere |
| authorStr |
Rannou, P. |
| ppnlink_with_tag_str_mv |
@@773@@(DE-627)ELV010254102 |
| format |
electronic Article |
| dewey-ones |
620 - Engineering & allied operations 610 - Medicine & health |
| delete_txt_mv |
keep |
| author_role |
aut |
| collection |
elsevier |
| remote_str |
true |
| illustrated |
Not Illustrated |
| topic_title |
620 620 DE-600 610 VZ 44.87 bkl Transparency of 2 μ m window of Titan's atmosphere |
| topic |
ddc 620 ddc 610 bkl 44.87 |
| topic_unstemmed |
ddc 620 ddc 610 bkl 44.87 |
| topic_browse |
ddc 620 ddc 610 bkl 44.87 |
| format_facet |
Elektronische Aufsätze Aufsätze Elektronische Ressource |
| format_main_str_mv |
Text Zeitschrift/Artikel |
| carriertype_str_mv |
zu |
| author2_variant |
b s bs m s l ms msl l m lm m r mr c s cs |
| hierarchy_parent_title |
ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |
| hierarchy_parent_id |
ELV010254102 |
| dewey-tens |
620 - Engineering 610 - Medicine & health |
| hierarchy_top_title |
ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |
| isfreeaccess_txt |
false |
| familylinks_str_mv |
(DE-627)ELV010254102 |
| title |
Transparency of 2 μ m window of Titan's atmosphere |
| ctrlnum |
(DE-627)ELV041696344 (ELSEVIER)S0032-0633(17)30217-9 |
| title_full |
Transparency of 2 μ m window of Titan's atmosphere |
| author_sort |
Rannou, P. |
| journal |
ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |
| journalStr |
ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |
| lang_code |
eng |
| isOA_bool |
false |
| dewey-hundreds |
600 - Technology |
| recordtype |
marc |
| publishDateSort |
2018 |
| contenttype_str_mv |
zzz |
| container_start_page |
109 |
| author_browse |
Rannou, P. |
| container_volume |
151 |
| physical |
16 |
| class |
620 620 DE-600 610 VZ 44.87 bkl |
| format_se |
Elektronische Aufsätze |
| author-letter |
Rannou, P. |
| doi_str_mv |
10.1016/j.pss.2017.11.015 |
| dewey-full |
620 610 |
| title_sort |
transparency of 2 μ m window of titan's atmosphere |
| title_auth |
Transparency of 2 μ m window of Titan's atmosphere |
| abstract |
Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. |
| abstractGer |
Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. |
| abstract_unstemmed |
Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant. |
| collection_details |
GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 |
| title_short |
Transparency of 2 μ m window of Titan's atmosphere |
| url |
https://doi.org/10.1016/j.pss.2017.11.015 |
| remote_bool |
true |
| author2 |
Seignovert, B. Le Mouélic, S. Maltagliati, L. Rey, M. Sotin, C. |
| author2Str |
Seignovert, B. Le Mouélic, S. Maltagliati, L. Rey, M. Sotin, C. |
| ppnlink |
ELV010254102 |
| mediatype_str_mv |
z |
| isOA_txt |
false |
| hochschulschrift_bool |
false |
| author2_role |
oth oth oth oth oth |
| doi_str |
10.1016/j.pss.2017.11.015 |
| up_date |
2024-07-06T20:49:26.031Z |
| _version_ |
1803864208607019008 |
| fullrecord_marcxml |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">ELV041696344</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230625235342.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">180726s2018 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1016/j.pss.2017.11.015</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">GBV00000000000106A.pica</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)ELV041696344</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(ELSEVIER)S0032-0633(17)30217-9</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2=" "><subfield code="a">620</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">620</subfield><subfield code="q">DE-600</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">610</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">44.87</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Rannou, P.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Transparency of 2 μ m window of Titan's atmosphere</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2018transfer abstract</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">16</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zzz</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">z</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zu</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant.</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Titan's atmosphere is optically thick and hides the surface and the lower layers from the view at almost all wavelengths. However, because gaseous absorptions are spectrally selective, some narrow spectral intervals are relatively transparent and allow to probe the surface. To use these intervals (called windows) a good knowledge of atmospheric absorption is necessary. Once gas spectroscopic linelists are well established, the absorption inside windows depends on the way the far wings of the methane absorption lines are cut-off. We know that the intensity in all the windows can be explained with the same cut-off parameters, except for the window at 2 μm. This discrepancy is generally treated with a workaround which consists in using a different cut-off description for this specific window. This window is relatively transparent and surface may have specific spectral signatures that could be detected. Thus, a good knowledge of atmosphere opacities is essential and our scope is to better understand what causes the difference between the 2 μm window and the other windows. In this work, we used scattered light at the limb and transmissions in occultation observed with VIMS (Visual Infrared Mapping Spectrometer) onboard Cassini, around the 2 μm window. Data shows an absorption feature that participates to the shape of this window. Our atmospheric model fits well the VIMS data at 2 μm with the same cut-off than for the other windows, provided an additional absorption is introduced in the middle of the window around ≃ 2.065 μm. It explains well the discrepency between the cut-off used at 2 μm, and we show that a gas with a fairly constant mixing ratio, possibly ethane, may be the cause of this absorption. Finally, we studied the impact of this absorption on the retrieval of the surface reflectivity and found that it is significant.</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Seignovert, B.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Le Mouélic, S.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Maltagliati, L.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Rey, M.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sotin, C.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="n">Elsevier Science</subfield><subfield code="a">Mekaroonkamol, Parit ELSEVIER</subfield><subfield code="t">ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS</subfield><subfield code="d">2023</subfield><subfield code="g">Kidlington [u.a.]</subfield><subfield code="w">(DE-627)ELV010254102</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:151</subfield><subfield code="g">year:2018</subfield><subfield code="g">pages:109-124</subfield><subfield code="g">extent:16</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doi.org/10.1016/j.pss.2017.11.015</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_U</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ELV</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_U</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHA</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_66</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_91</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_165</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_234</subfield></datafield><datafield tag="936" ind1="b" ind2="k"><subfield code="a">44.87</subfield><subfield code="j">Gastroenterologie</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">151</subfield><subfield code="j">2018</subfield><subfield code="h">109-124</subfield><subfield code="g">16</subfield></datafield><datafield tag="953" ind1=" " ind2=" "><subfield code="2">045F</subfield><subfield code="a">620</subfield></datafield></record></collection>
|
| score |
7.400012 |