<=== observer ===> "JBALUTEA",\ "Baluteau, J.P.",\ "",\ "Observatoire de Marseille",\ "2, Place Le Verrier",\ "",\ "13004",\ "Marseille",\ "France",\ " 33 91959088",\ " 33 91621190",\ "baluteau@obmara.cnrs-mrs.fr" <=== proposal ===> "ISM_V",1,2,\ {"HII regions","diffuse interstellar medium","molecular clouds","star \ formation","dust properties"},\ {"LWS consortium","S. Miller","M.F. Kessler","T. Prusti"} <=== title ===> COMPLETE LWS SPECTRAL SURVEY AT HIGH RESOLUTION <=== abstract ===> SCIENTIFIC ABSTRACT It is now well accepted that systematic observations (of the survey type) are of great interest for the general astrophysics outcome. ISO offers a unique opportunity to completely explore the spectrum between 2.5 and 200 um at both unprecedented high sensitivity and spectral resolution, especially in the still unexplored gaps between the atmospheric windows. This opportunity has to be fully used given that many unexpected lines are likely to be discovered in the far infrared spectra of astronomical objects. We cannot rely on observing only lines (atomic and molecular) and solid state features that we already know about or expect to be seen. In this context we propose to observe selected bright astronomical source(s) over the spectral range covered by the ISO/LWS, from 45 to 196 um, in the high resolution Fabry-Perot mode. The main goal of this proposal is to detect new spectral features or lines with unexpected strength. In order to get the full capability of the ISO/LWS, Fabry-Perot spectra should be taken towards some of the brightest known infrared sources. Furthermore, since the proposed goal impose to obtain a very high signal to noise ratio (at least 100 seems mandatory) it might well be wisest to select only a limited number of objects probing in the best possible way the different phases associated with the interstellar medium. The detection of unexpected spectral features will prompt subsequent studies for the identification of the feature first, but also will need to elaborate a strategy, depending on the strenght ot the new feature, for follow-up observations. OBSERVATION SUMMARY In order to probe the different phases associated with the interstellar medium in only a very few lines of sight, the source(s) selection procedure is made to get both: i. an "emission" spectrum: the line of sight should probe characteristic regions of the interstellar medium exposed to a strong radiation field and sampling at least regions of ionised hydrogen, of photodissociation and with shocked gas. ii. an "absorption" spectrum: the line of sight should also probe interstellar material (molecules or solids) which remains protected from the radiation field (at least from its visible and ultraviolet parts) and hence traces highly processed material such as organic mantles on dust grains or volatile species such as ices. The source(s) should be chosen, naturally, among the brigthest objects in the infrared sky. Therefore "off-source" position are not required for the proposed programme. <=== scientific_justification ===> AOTs For all the sources the AOT LWS03 is used, with 4 samples per spectral element and the "fast" scanning mode. The signal to noise ratio expected, by spectral element, is 100. This can be achieved with the minimum integration time available (0.25 sec) per FP step except for some parts of the spectrum for Sgr B2, M 17 and W 51. Since the time required to cover the whole spectral range is too long, compared to the ISO orbit duration, the spectral domain is cut out in different bands. These are as follows: For Orion BN/KL , M17 and Sgr B2: # lambda start lambda end 1 45um 60um 2 60 75 3 75 90 4 90 120 5 120 150 6 150 196 For W51 A : # lambda start lambda end 1 47.7um 53um 2 53 60 3 60 67 4 67 75 5 75 82 6 82 90 7 90 105 8 105 120 9 120 135 10 135 155 11 155 175 12 175 196 The 1950. coordinates of the four selected targets are: ORION BN/KL 05h 32m 46.7s -05d 24' 27" Sgr B2 17h 44m 12.0s -28d 22' 12" M 17 18h 17m 29.9s -16d 13' 15" W51-IRS2 19h 21m 22.4s +14d 25' 15" For all the selected targets we plan to measure a full medium resolution spectrum, using AOT LWS01 with 4 samples per spectral element and the "fast" scanning mode. SPACECRAFT TIME DISTRIBUTION Time distribution for autumn launch targets: Team top 40% second 30% last 30% LWS: 50116 sec 50116 sec SOT: 18000 sec 18000 sec Total: 68116 sec 68116 sec Time distribution for spring launch targets: Team top 40% second 30% last 30% LWS: 50116 sec 50064 sec SOT: 18000 sec 18000 sec Total: 68116 sec 68064 sec <=== autumn_launch_targets ===> 1, "LWS03",1.0,"N","Sgr B2 ",17.73667,-28.37000,1950,0.,0.,12684,0 2, "LWS03",1.0,"N","Sgr B2 ",17.73667,-28.37000,1950,0.,0.,10794,0 3, "LWS03",1.0,"N","Sgr B2 ",17.73667,-28.37000,1950,0.,0., 9088,13 4, "LWS03",1.0,"N","Sgr B2 ",17.73667,-28.37000,1950,0.,0.,12402,0 5, "LWS03",1.0,"N","Sgr B2 ",17.73667,-28.37000,1950,0.,0., 9522,0 6, "LWS03",1.0,"N","Sgr B2 ",17.73667,-28.37000,1950,0.,0.,13130,0 7, "LWS03",2.0,"N","M17 ",18.29164,-16.22083,1950,0.,0.,12684,0 8, "LWS03",2.0,"N","M17 ",18.29164,-16.22083,1950,0.,0.,10794,0 9, "LWS03",2.0,"N","M17 ",18.29164,-16.22083,1950,0.,0., 9088,14 10,"LWS03",2.0,"N","M17 ",18.29164,-16.22083,1950,0.,0.,12402,0 11,"LWS03",2.0,"N","M17 ",18.29164,-16.22083,1950,0.,0., 9522,0 12,"LWS03",2.0,"N","M17 ",18.29164,-16.22083,1950,0.,0.,13130,0 13,"LWS01",1.0,"N","Sgr B2 ",17.73667,-28.37000,1950,0.,0., 496,0 14,"LWS01",2.0,"N","M17 ",18.29164,-16.22083,1950,0.,0., 496,0 <=== spring_launch_targets ===> 1, "LWS03",1.0,"N","Orion BN/KL ",05.54631,-05.40750,1950,0.,0.,12684,0 2, "LWS03",1.0,"N","Orion BN/KL ",05.54631,-05.40750,1950,0.,0.,10794,0 3, "LWS03",1.0,"N","Orion BN/KL ",05.54631,-05.40750,1950,0.,0., 9088,19 4, "LWS03",1.0,"N","Orion BN/KL ",05.54631,-05.40750,1950,0.,0.,12402,0 5, "LWS03",1.0,"N","Orion BN/KL ",05.54631,-05.40750,1950,0.,0., 9522,0 6, "LWS03",1.0,"N","Orion BN/KL ",05.54631,-05.40750,1950,0.,0.,13130,0 7, "LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 5064,0 8, "LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 5858,0 9, "LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 4714,0 10,"LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 6416,0 11,"LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 4838,0 12,"LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 4586,20 13,"LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 7180,0 14,"LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 5616,0 15,"LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 5048,0 16,"LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 6180,0 17,"LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 6298,0 18,"LWS03",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 5770,0 19,"LWS01",1.0,"N","Orion BN/KL ",05.54631,-05.40750,1950,0.,0., 496,0 20,"LWS01",2.0,"N","W51 A ",19.35622,+14.42083,1950,0.,0., 496,0