<=== observer ===> "GHELOU",\ "Helou, G.",\ "Infrared Processing and Analysis Center",\ "California Institute of Technology",\ "1201 E. California Blvd.",\ "MailCode 100-22",\ "91125",\ "Pasadena, CA",\ "USA",\ "1 818 3979555",\ "1 818 3979600",\ "helou@ipac.caltech.edu" <=== proposal ===> "SF_GLX_5",2,4,\ {"irregular galaxies", "early-type galaxies", "normal galaxies",\ "starburst galaxies", "star formation"},\ {"Hollenbach, D.J.","Thronson, H.A., Jr.","Stacey, G.J.","Rubin, R.H.",\ "Dinerstein, H.L.", "Lord, S.D.", "Werner, M.","Hunter, D.A.", "Lo, K.Y.",\ "Beichman, C.A."} <=== title ===> The Interstellar Medium of Normal Galaxies: Properties and Evolution \ Part 5 of 7 <=== abstract ===> SCIENTIFIC ABSTRACT: We propose to observe an ensemble of atomic and ionic fine structure lines and the infrared continuum to characterize the interstellar medium and the global star formation process in a broad sample of normal galaxies. In this context, normal galaxies are those whose luminosity is dominated by stars and various amounts of ongoing star formation. Uniquely suited to the Infrared Space Observatory (ISO), these observations will probe the birth-sites of stars, yield the physical properties of the gas, dust and radiation field, and refine our picture of the global energetics in galaxies. We propose to study about 70 unresolved galaxies and selected regions of eight nearby, spatially resolved galaxies: NGC 6946, NGC 4449, IC 10, NGC 1313, NGC6744, NGC 2366 or NGC 6822, M101 or NGC 1365 and NGC 4258. We plan to use the LWS to probe the warm neutral phase with the [CII] line at 158 um, and [OI] at 63 um, and to probe HII regions with [NII] at 122 um, [NIII] at 57 um, and the [OIII] lines at 88 and 52 um. We propose to measure with PHOT the spectral energy distribution of our sources between 100 and 200 um to supplement IRAS data, and to obtain their images at 7 and 15 um using CAM. For the brighter sources, we will also obtain the 3-12 um spectrum using PHT-S. We plan then to study how these measured and derived physical parameters relate to the global properties of galaxies -- morphology and kinematics, environment, gas content, metallicity, and star formation efficiency. The ultimate goal of this program is to constrain the evolutionary processes in galaxies, discriminating for example between mechanisms for global star formation activation (cloud-cloud collisions or gravitational instability), and suppression (spatial dispersal or photodissociation and heating). Normal galaxies account for most of the luminous mass in the local Universe. The galaxies we would study sample wide ranges in total luminosity ($10^8-10^{10} L_{sun}$), infrared-to-blue luminosity ratio (0.3-50), morphology (S0 to Im; two or three Elliptical), and relative gas content. We exclude galaxies with active nuclei (Seyferts), but include a few objects with extreme infrared-to-blue ratio, or 60 um surface brightness. Spatial resolution in nearby galaxies allows us to study well-defined components such as HII complexes, spiral arms, bars and inter-arm disk regions, and variations in the properties of gas, dust and radiation within a disk. OBSERVATION SUMMARY: The proposed science objectives will be pursued by probing the ISM in star forming galaxies using various capabilities available on ISO. We use LWS for spectral lines, CAM for mapping the hot dust, and PHOT to detect long-wavelength emission from cold dust and for near-infrared spectroscopy. There are two groups of targets in this project: selected positions within ten nearby, resolved galaxies (proposal parts 6 and 7 of this project), and about 70 more distant, essentially unresolved galaxies (proposal parts 1 to 6). The planned observations are essentially the same for all targets except that some mapping is possible for the nearby sample. The data on the more distant objects will yield global fluxes, and rough sizes from CAM imaging. The basic set of observations consist of:\ LWS: A: [CII] 158 um, [NII] 122 um,\ B: [OI] 63 um, [OIII] 88 um,\ C: [NIII] 57 um, [OIII] 52 um;\ D: Full spectral scan for the few brightest sources;\ CAM: imaging at 6"/pixel in LW2 (7 um), LW3 (15 um) filters;\ PHT: photometry at 135 um and 200 um, using the C_200 module;\ resolved galaxies will be partially mapped at 60 um with C_100,\ and at 135 and 200 um with C_200;\ PHT-S: 3-12 um spectra will be obtained for the brighter targets.\ Wherever possible, especially for bright targets, all these data are collected for each object. However, various observations are eliminated for individual targets if they become too time-consuming. Thus PHT-S observations are only carried out for targets with an IRAS 12 um flux density greater than about 0.3 Jy. In the case of LWS spectroscopy, as the targets become fainter, the lines observed are reduced from sets A, B and C to A and B, and only to A for faint areas within nearby resolved galaxies. In the case of the very brightest sources, the LWS will be used to scan the whole spectrum. Some CAM and PHT observations for certain bright sources are not included because they already appear in the ISO Central Programme. Wherever CAM observations are planned, they include both LW2 and LW3 filters and use micro-scanning. Long-wavelength photometric observations are made with the PHOT-C instrument and complement the spectroscopy being carried out with the LWS. <=== scientific_justification ===> OBSERVING TIMES: LWS The LWS integration times are matched to the brightness of the targeted sources. For unresolved galaxies we take 60 and 100 um fluxes from the IRAS PSC and compute the total FIR flux (Helou et al 1988). We estimate an expected flux in the CII line F(CII)=0.004*FIR. We then use the LWS time estimator to derive the times needed to achieve a noise level equivalent to 1/50 F(CII) for the NII, OI, OIII (88 um) and NIII lines. The noise levels targeted for CII and OIII (52 um) are set at 3/50 F(CII). If the time required for an object became too long, the most time-consuming lines were dropped. The resulting times are shown in the AOT lists, whereas the specific lines for each target are given below in the section on OBSERVING DETAILS ON INDIVIDUAL OBJECTS. For each resolved galaxy we have estimated the 60 um flux expected in each LWS beam position using HiRes IRAS maps, and scaled that to an expected CII flux, using a conservative mean 60/100 um ratio of 0.5. We then estimated the integration times following the rules outlined above for unresolved objects. The resulting times are shown in the AOT lists, whereas the specific lines for each target are given below in the section on OBSERVING DETAILS ON INDIVIDUAL OBJECTS. For the following bright objects we plan to conduct full spectral scans with the LWS for the complete wavelength range: N278, N986, N1569, N3620, N4102, N4418, N4490, N4536, N6000, N6215, UGC2855, UGC2866. OBSERVING TIMES: PHOT The aim of the PHT-C observations of the unresolved galaxy sample is to obtain 135 and 200 um observations to determine the amount of cold dust present in these galaxies. These data will be used in conjunction with IRAS 12-100 um observations and CAM observations to infer the total dust luminosity, rough temperature distribution and dust mass. The observing sequence is simple and uses the sparse map AOTs (PHT 37 and PHT39) to measure an ON and an OFF position for each galaxy in each of the 2 wavelengths with a 32 second integration time. The second PHOT measurement for distant galaxies consists of spectra taken with the PHOT-S instrument in the chopped mode (PHT40). 128 second exposures are taken at ON and OFF positions for all objects brighter than about 0.3 Jy at 12 um. If we adopt flux density ratios of fv(7.7)/fv(12)=0.6 (Cohen and Volk 1993) and fv(3.3)/fv(12)=0.05 (Willner et al 1977) for galaxies, then the sensitivity achieved in these observations should be adequate to measure the PAH features with an SNR of at least 5 in all cases. The strength of the silicate feature will be determined and any strong atomic or ionized lines will be detected. The brighter sources will be detectable over a large fraction of the PHT-S spectral range. For spatially resolved galaxies, the fundamental observing PHOT mode is to make one or more strip scans across the galaxy at wavelengths of 60, 135 and 200um. The C100 and C200 arrays are used in conjunction with the sparse map AOTs. In all cases overlap of at least one pixel is used between array pointings to ensure adequate sampling and to mitigate against detector drifts. Integration time is 16 seconds at each point and is driven by the need for adequate detector stabilization. In the detailed AOTs that follow, the beginning (PHT37), middle (PHT38) and end points (PHT39) of the scans are given. It should be noted that each scan is between 7 and 11 points long. All the intermediate points have been summed together in a single PHT38 observation of the appropriate integration time. In a few cases the cost of doing two scans to match up with all LWS positions was prohibitive. In these cases, individual LWS points were covered with PHT38 observations. These PHOT observations can be summarized as follows: Galaxy |# Scans | # Extra Points | Time(sec)| Lambda NGC 6946 |2 | 0 | 2775 |60,135,200 IC 10 |1 | 1 | 1740 |60,135,200 NGC 4258 |1 | 2 | 1614 |60,135,200 NGC 1313 |1 | 0 | 1445 |60,135,200 NGC 6744 |1 | 0 | 1316 |60,135,200 OBSERVING TIMES: CAM All CAM observations of unresolved galaxies will use the same integration time of 200 seconds per filter per galaxy. They use micro-scanning in a 3x3 pattern, stepped by 1' in each direction. The expected 1-sigma surface brightness is about 5mJy/arcmin^2 (depending on the zodiacal background), which should be adequate since almost all these sources have more than 100 mJy in an area several times smaller than a square arcminute. For resolved galaxies the integration time has been set to reach the same surface brightness limit for the whole galaxy, and somewhat deeper at faint locations covered by the LWS beams. OBSERVING DETAILS ON INDIVIDUAL OBJECTS: UNRESOLVED GALAXIES Most unresolved galaxies are observed at six fine-structure lines (CII at 158 um, NII at 122, OI at 63, OIII at 88, NIII at 57 and OIII at 52). The following 25 objects however will only be measured with four lines, CII, NII, OI and OIII (88 um). MCG -03-06-010 NGC 3705 NGC 1317 NGC 5691 NGC 5534 NGC 1341 NGC 6796 NGC 5970 NGC 2742 NGC 1186 UGC 02519 NGC 4519 NGC 6821 NGC 1517 UGC 01449 NGC 3839 NGC 3353 NGC 3239 UGC 05720 NGC 2537 UGC 05613 NGC 1155 NGC 3265 Finally, two elliptical galaxies, NGC 6958 and NGC 1052. are observed only at CII and NII. Reference beam observations for LWS appear labeled by the source name suffixed with "_R", and are tagged with the position of the source itself. The actual positions to be used for reference will be determined during phase 2, after examination of the IRAS Sky Survey Atlas maps in the target area. OBSERVING DETAILS ON INDIVIDUAL OBJECTS: SPATIALLY RESOLVED GALAXIES We have selected ten galaxies for spatially resolved observations, of which six will be observed in either spring or autumn launch cases (N6946, N4449, IC10, N1313, N4258, N6744), plus N2366 and M101 for an autumn launch, or N6822 and N1365 for a spring launch. The proposed observing plans on each are outlined below: NGC 6946: This galaxy will be fully mapped, with a pattern of 3 by 5 LWS beams, plus an extension along the minor axis out to the edge of the HI envelope. We will also map out a 3' wide strip along each of the minor and major axes using PHOT at three wavelengths: 60 (C_100), 135 (C_200), and 200 um (C_200). CAM mapping of the whole disk, roughly 10'x10', plus the minor axis extension, will be done in a mosaic of 10 separate subfields, using 10 AOTs whose details will be worked out in phase 2; we show only one AOT in this listing. NGC 4449: Three LWS beam positions strung at a position angle of about 30 degrees, sampling the brightest region of the disk. CAM mapping of the bright inner disk, roughly 5'x5' in one AOT. IC 10: Three LWS beams centered on star forming complexes. Because of the large size and low Galactic latitude of IC10, two reference points are chosen 12' to either side of the center, in a N-W direction. The strip connecting these two points will be mapped by PHOT; the third LWS position will also be observed with PHOT. CAM mapping of the inner bright disk, roughly 5'x5' in one AOT. NGC 1313: Two LWS beams on the brightest parts of the disk. One strip-map will be made with PHOT along the line defined by these two beam positions. The whole disk will be mapped with CAM using two 4'x4' subfields. NGC 4258: Three LWS beams centered on infrared-bright spots at the nucleus and on the arms, then two more beams in less bright inter-arm regions. One PHT strip-map along the axis defined by the bright spots, plus single-point observations of the inter-arm regions. The whole disk will be mapped with CAM using two 4'x4' subfields. NGC 6744: Five LWS beam positions, aligned at a position angle of about 150 degrees, crossing the nuclear infrared-faint region, and two brighter arm positions. PHOT strip-map of the same axis. CAM mapping of the same strip, in 3 subfields 4'x4' each, only in the spring launch program. NGC 2366: Two LWS beams. CAM mapping of a 5'x5' area in one AOT. NGC 6822: Two LWS beams. CAM mapping of the disk in two subfields 4'x4' each. M 101: One LWS beam on the center, one on a bright HII complex to the West, and a line of six LWS beams connecting two relatively bright HII complexes and crossing through more quiescent disk regions. These observations were coordinated to complement data in the same regions collected by CAM and PHOT as part of the ISO Central Programme. NGC 1365: Three LWS beam positions along the bar, and an additional beam on a bright complex in the Northern arm. For these nearby galaxies, the infrared surface brightness of the disk varies greatly among the various beam positions, even on the same galaxy. Since we adjust the LWS observation strategy of each beam position to the expected flux, we list below the specific lines observed at each beam position in each galaxy. Three positions, one in each of IC10, N1365, and N6946, are sufficiently bright that we plan to obtain a full spectral scan for them over the whole wavelength range of the LWS. GALAXY-POSITION CII NII OI OIII NIII OIII 158 122 63 88 57 52 um ------------------------------------------------------ NGC_6946 Ref C NGC_6946 mn-1mj+2 C N O O NGC_6946 major+2 C N O O NGC_6946 mn+1mj+2 C N NGC_6946 mn-1mj+1 C N O O NGC_6946 major+1 C N O O N O NGC_6946 mn+1mj+1 C N O O NGC_6946 minor-1 C N O O NGC_6946 center C N O O N O + full spectral scan NGC_6946 minor+1 C N O O NGC_6946 mn-1mj-1 C N O O NGC_6946 major-1 C N O O NGC_6946 mn+1mj-1 C N O O NGC_6946 mn-1mj-2 C N NGC_6946 major-2 C N NGC_6946 mn+1mj-2 C N NGC_6946 minor-2 C N NGC_6946 minor-3 C N NGC_6946 minor-4 C N NGC_4449 Ref C NGC_4449 North1 C N O O N O NGC_4449 Center C N O O N O NGC_4449 South1 C N IC_10 Ref C N IC_10 Ref1 C N IC_10 North C N O O N O IC_10 East C N O O N O + full spectral scan IC_10 West C N O O NGC_2366 Ref C NGC_2366 Center C N O O NGC_2366 North C N M101 Ref C M101 Center C N O O M101 West1 C N O O M101 NE1 C N O O M101 NE2 C N M101 NE3 C N M101 NE4 C N M101 NE5 C N M101 NE6 C N NGC_6822 Ref C NGC_6822 North C N O O N O NGC_6822 South C N NGC_1365 Ref C NGC_1365 Center C N O O N O + full spectral scan NGC_1365 Bar_East C N O O N O NGC_1365 Bar_West C N NGC_1365 Arm_N C N NGC_1313 Ref C NGC_1313 North C N O O N O NGC_1313 South C N O O N O NGC_4258 Ref C NGC_4258 South2 C N O O NGC_4258 South1 C N NGC_4258 Center C N O O N O NGC_4258 North1 C N NGC_4258 North2 C N O O NGC_6744 Ref C NGC_6744 North2 C N NGC_6744 North1 C N NGC_6744 Center C N NGC_6744 South1 C N NGC_6744 South2 C N NO LINKED observations are requested. CONCATENATION is requested. When multiple observations with different instruments are called for on the same target, the various AOTs are concatenated. This follows from the high scientific priority that the project attaches to obtaining data from the various instruments on the same objects, rather than obtaining same-instrument data on a large number of objects. Concatenation is also used to connect the observations of contiguous pointings when mapping galaxies. TIME SUMMARIES: For the whole SF_GLX project, all 7 parts: Time distribution for autumn launch targets: Team Top 40% Next 30% Last 30% USA 119,700 93,600 90,300 total 119,700 93,600 90,300 Time distribution for spring launch targets: Team Top 40% Next 30% Last 30% USA 118,400 93,300 90,800 total 118,400 93,300 90,800 <=== autumn_launch_targets ===> 1, "LWS02", 1.,"N", "IC 4662 ", 17.78511, -64.64030, 2000, 0., 0., 2016, 2 2, "LWS02", 1.,"N", "IC 4662 _R", 17.78511, -64.64030, 2000, 0., 0., 348, 3 3, "CAM01", 1.,"N", "IC 4662 ", 17.78511, -64.64030, 2000, 0., 0., 420, 4 4, "PHT37", 1.,"N", "IC 4662 ", 17.78511, -64.64030, 2000, 0., 0., 66, 5 5, "PHT39", 1.,"N", "IC 4662 ", 17.78511, -64.64030, 2000, 0., 0., 96, 6 6, "PHT37", 1.,"N", "IC 4662 ", 17.78511, -64.64030, 2000, 0., 0., 84, 7 7, "PHT39", 1.,"N", "IC 4662 ", 17.78511, -64.64030, 2000, 0., 0., 94, 0 8, "LWS02", 3.,"N", "NGC 5433 ", 14.04334, 32.51040, 2000, 0., 0., 2406, 9 9, "LWS02", 3.,"N", "NGC 5433 _R", 14.04334, 32.51040, 2000, 0., 0., 348, 10 10, "CAM01", 3.,"N", "NGC 5433 ", 14.04334, 32.51040, 2000, 0., 0., 420, 11 11, "PHT37", 3.,"N", "NGC 5433 ", 14.04334, 32.51040, 2000, 0., 0., 66, 12 12, "PHT39", 3.,"N", "NGC 5433 ", 14.04334, 32.51040, 2000, 0., 0., 96, 13 13, "PHT37", 3.,"N", "NGC 5433 ", 14.04334, 32.51040, 2000, 0., 0., 84, 14 14, "PHT39", 3.,"N", "NGC 5433 ", 14.04334, 32.51040, 2000, 0., 0., 94, 15 15, "PHT40", 3.,"N", "NGC 5433 ", 14.04334, 32.51040, 2000, 0., 0., 362, 0 16, "LWS02", 3.,"N", "NGC 3839 ", 11.73179, 10.78300, 2000, 0., 0., 1942, 17 17, "LWS02", 3.,"N", "NGC 3839 _R", 11.73179, 10.78300, 2000, 0., 0., 348, 18 18, "CAM01", 3.,"N", "NGC 3839 ", 11.73179, 10.78300, 2000, 0., 0., 420, 19 19, "PHT37", 3.,"N", "NGC 3839 ", 11.73179, 10.78300, 2000, 0., 0., 66, 20 20, "PHT39", 3.,"N", "NGC 3839 ", 11.73179, 10.78300, 2000, 0., 0., 96, 21 21, "PHT37", 3.,"N", "NGC 3839 ", 11.73179, 10.78300, 2000, 0., 0., 84, 22 22, "PHT39", 3.,"N", "NGC 3839 ", 11.73179, 10.78300, 2000, 0., 0., 94, 0 23, "LWS02", 2.,"N", "NGC 3353 ", 10.75630, 55.96000, 2000, 0., 0., 1762, 24 24, "LWS02", 2.,"N", "NGC 3353 _R", 10.75630, 55.96000, 2000, 0., 0., 348, 25 25, "PHT37", 2.,"N", "NGC 3353 ", 10.75630, 55.96000, 2000, 0., 0., 66, 26 26, "PHT39", 2.,"N", "NGC 3353 ", 10.75630, 55.96000, 2000, 0., 0., 96, 27 27, "PHT37", 2.,"N", "NGC 3353 ", 10.75630, 55.96000, 2000, 0., 0., 84, 28 28, "PHT39", 2.,"N", "NGC 3353 ", 10.75630, 55.96000, 2000, 0., 0., 94, 0 29, "LWS02", 1.,"N", "UGC 02238 ", 2.77139, 13.09560, 2000, 0., 0., 1699, 30 30, "LWS02", 1.,"N", "UGC 02238 _R", 2.77139, 13.09560, 2000, 0., 0., 348, 31 31, "CAM01", 1.,"N", "UGC 02238 ", 2.77139, 13.09560, 2000, 0., 0., 420, 32 32, "PHT37", 1.,"N", "UGC 02238 ", 2.77139, 13.09560, 2000, 0., 0., 66, 33 33, "PHT39", 1.,"N", "UGC 02238 ", 2.77139, 13.09560, 2000, 0., 0., 96, 34 34, "PHT37", 1.,"N", "UGC 02238 ", 2.77139, 13.09560, 2000, 0., 0., 84, 35 35, "PHT39", 1.,"N", "UGC 02238 ", 2.77139, 13.09560, 2000, 0., 0., 94, 36 36, "PHT40", 1.,"N", "UGC 02238 ", 2.77139, 13.09560, 2000, 0., 0., 362, 0 37, "LWS02", 3.,"N", "MRK 0331 ", 23.85727, 20.58560, 2000, 0., 0., 1064, 38 38, "LWS02", 3.,"N", "MRK 0331 _R", 23.85727, 20.58560, 2000, 0., 0., 348, 39 39, "CAM01", 3.,"N", "MRK 0331 ", 23.85727, 20.58560, 2000, 0., 0., 420, 40 40, "PHT37", 3.,"N", "MRK 0331 ", 23.85727, 20.58560, 2000, 0., 0., 66, 41 41, "PHT39", 3.,"N", "MRK 0331 ", 23.85727, 20.58560, 2000, 0., 0., 96, 42 42, "PHT37", 3.,"N", "MRK 0331 ", 23.85727, 20.58560, 2000, 0., 0., 84, 43 43, "PHT39", 3.,"N", "MRK 0331 ", 23.85727, 20.58560, 2000, 0., 0., 94, 44 44, "PHT40", 3.,"N", "MRK 0331 ", 23.85727, 20.58560, 2000, 0., 0., 362, 0 45, "LWS02", 3.,"N", "UGC 08335 NED02 ", 13.25979, 62.12400, 2000, 0., 0., 1520, 46 46, "LWS02", 3.,"N", "UGC 08335 NED0_R", 13.25979, 62.12400, 2000, 0., 0., 348, 47 47, "CAM01", 3.,"N", "UGC 08335 NED02 ", 13.25979, 62.12400, 2000, 0., 0., 420, 48 48, "PHT37", 3.,"N", "UGC 08335 NED02 ", 13.25979, 62.12400, 2000, 0., 0., 66, 49 49, "PHT39", 3.,"N", "UGC 08335 NED02 ", 13.25979, 62.12400, 2000, 0., 0., 96, 50 50, "PHT37", 3.,"N", "UGC 08335 NED02 ", 13.25979, 62.12400, 2000, 0., 0., 84, 51 51, "PHT39", 3.,"N", "UGC 08335 NED02 ", 13.25979, 62.12400, 2000, 0., 0., 94, 52 52, "PHT40", 3.,"N", "UGC 08335 NED02 ", 13.25979, 62.12400, 2000, 0., 0., 362, 0 53, "LWS02", 2.,"N", "IRAS F23365+3604", 23.65037, 36.35290, 2000, 0., 0., 2525, 54 54, "LWS02", 2.,"N", "IRAS F23365+36_R", 23.65037, 36.35290, 2000, 0., 0., 348, 55 55, "CAM01", 2.,"N", "IRAS F23365+3604", 23.65037, 36.35290, 2000, 0., 0., 420, 0 56, "LWS02", 2.,"N", "IC 0860 ", 13.25063, 24.62090, 2000, 0., 0., 1070, 57 57, "LWS02", 2.,"N", "IC 0860 _R", 13.25063, 24.62090, 2000, 0., 0., 348, 58 58, "CAM01", 2.,"N", "IC 0860 ", 13.25063, 24.62090, 2000, 0., 0., 420, 59 59, "PHT37", 2.,"N", "IC 0860 ", 13.25063, 24.62090, 2000, 0., 0., 66, 60 60, "PHT39", 2.,"N", "IC 0860 ", 13.25063, 24.62090, 2000, 0., 0., 96, 61 61, "PHT37", 2.,"N", "IC 0860 ", 13.25063, 24.62090, 2000, 0., 0., 84, 62 62, "PHT39", 2.,"N", "IC 0860 ", 13.25063, 24.62090, 2000, 0., 0., 94, 0 63, "LWS02", 2.,"N", "CGCG 1510.8+0725", 15.22036, 7.22650, 2000, 0., 0., 925, 64 64, "LWS02", 2.,"N", "CGCG 1510.8+07_R", 15.22036, 7.22650, 2000, 0., 0., 348, 65 65, "CAM01", 2.,"N", "CGCG 1510.8+0725", 15.22036, 7.22650, 2000, 0., 0., 420, 66 66, "PHT37", 2.,"N", "CGCG 1510.8+0725", 15.22036, 7.22650, 2000, 0., 0., 66, 67 67, "PHT39", 2.,"N", "CGCG 1510.8+0725", 15.22036, 7.22650, 2000, 0., 0., 96, 68 68, "PHT37", 2.,"N", "CGCG 1510.8+0725", 15.22036, 7.22650, 2000, 0., 0., 84, 69 69, "PHT39", 2.,"N", "CGCG 1510.8+0725", 15.22036, 7.22650, 2000, 0., 0., 94, 0 70, "LWS02", 2.,"N", "IC 0883 ", 13.34313, 34.13930, 2000, 0., 0., 1077, 71 71, "LWS02", 2.,"N", "IC 0883 _R", 13.34313, 34.13930, 2000, 0., 0., 348, 72 72, "CAM01", 2.,"N", "IC 0883 ", 13.34313, 34.13930, 2000, 0., 0., 420, 73 73, "PHT37", 2.,"N", "IC 0883 ", 13.34313, 34.13930, 2000, 0., 0., 66, 74 74, "PHT39", 2.,"N", "IC 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2.55949, -39.04600, 2000, 0., 0., 884, 88 88, "LWS01", 2.,"N", "NGC 0986 _R", 2.55949, -39.04600, 2000, 0., 0., 348, 0 <=== spring_launch_targets ===> 1, "LWS02", 3.,"N", "UGC 05376 ", 10.00747, 3.37500, 2000, 0., 0., 3203, 2 2, "LWS02", 3.,"N", "UGC 05376 _R", 10.00747, 3.37500, 2000, 0., 0., 348, 3 3, "CAM01", 3.,"N", "UGC 05376 ", 10.00747, 3.37500, 2000, 0., 0., 420, 4 4, "PHT37", 3.,"N", "UGC 05376 ", 10.00747, 3.37500, 2000, 0., 0., 66, 5 5, "PHT39", 3.,"N", "UGC 05376 ", 10.00747, 3.37500, 2000, 0., 0., 96, 6 6, "PHT37", 3.,"N", "UGC 05376 ", 10.00747, 3.37500, 2000, 0., 0., 84, 7 7, "PHT39", 3.,"N", "UGC 05376 ", 10.00747, 3.37500, 2000, 0., 0., 94, 8 8, "PHT40", 3.,"N", "UGC 05376 ", 10.00747, 3.37500, 2000, 0., 0., 362, 0 9, "LWS02", 3.,"N", "NGC 2537 ", 8.22071, 45.99120, 2000, 0., 0., 2610, 10 10, "LWS02", 3.,"N", "NGC 2537 _R", 8.22071, 45.99120, 2000, 0., 0., 348, 11 11, "CAM01", 3.,"N", "NGC 2537 ", 8.22071, 45.99120, 2000, 0., 0., 420, 12 12, "PHT37", 3.,"N", "NGC 2537 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