<=== observer ===> "HVOELK",\ "Voelk, H.J.",\ "",\ "Max-Planck-Institut fuer Kernphysik",\ "Saupfercheckweg 1",\ "103980",\ "D-69029",\ "Heidelberg",\ "Germany",\ " 496221516295",\ " 496221516324",\ "vlk@vampi.mpi-hd.mpg.de" <=== proposal ===> "VIRGO4",1,4,\ {"galaxy clusters","normal galaxies","irregular galaxies"},\ {"Hippelein, H.","Leech, K.","Metcalfe, L.",\ "Skaley, D.","Tuffs, R.J.","Xu, C."} <=== title ===> Statistical Sample of Late-Type Galaxies from the VIRGO Cluster Part 4 <=== abstract ===> SCIENTIFIC ABSTRACT We propose to study a complete volume-limited unbiased sample of 118 spiral, irregular and dwarf galaxies from the VIRGO cluster in the 40 - 220 micron spectral range with ISOPHOT. The completeness limit of Bt = 18 magnitude corresponds to the maximum (confusion limited) depth the instrument can achieve, allowing a complete dynamic range in star-formation activity to be measured. In parallel, wherever instrument sensitivity permits, we propose a degree of spectro-photometric resolution which by far exceeds that of IRAS, to provide a basis for distinguishing between dust components of different temperatures and grain size distributions in the galaxian interstellar media. These FIR observations will furthermore spatially resolve the central region from the disk for the giant spirals with diameters exceeding a few arcminutes. This should allow a distinction between FIR activity in the centres and the disks for about half the galaxies in the sample. Using LWS, we further propose to survey a subsample of 50 spiral galaxies with integrated blue magnitudes Bt < 14.5 for emission in the [CII] 158 micron fine structure line. OBSERVATION SUMMARY It is proposed to make the FIR continuum measurements at diffraction-limited angular resolutions with the PHT-C200 array in the C120, C160 and C200 filters, and with the C100 array in the C60, C70 and C100 filters. These filters provide the widest spectral range with an even spectral sampling. The use of the C60 and C100 micron filters will facilitate a cross calibration with the IRAS all sky survey. Irregular and dwarf galaxies will only be observed in the wide-band C60, C100 and C160 filters. Photometry for the fainter targets will be made using the PHT22 AOT with the focal plane chopper operating in it's "triangular" waveform mode. This should enable us to reach the confusion limit due to foreground cirrus of a few mJy rms at 100 micron, sufficient to detect a Bt = 18 magnitude VIRGO dwarf galaxy with a predicted FIR flux density of the order of 10 mJy. To provide optimum protection against confusion in the 120 - 200 micron spectral range, small spatially oversampled scans through each source will be performed using the PHT32 AOT. Use of the PHT32 AOT is also necessary to measure spatially integrated flux densities from the disks of brighter spiral galaxies whose spatial extent exceeds the unvignetted field of view of ISO. The close pair VCC1673 and VCC1676 will be covered by common rasters. Exposure times in each ISOPHOT filter were selected in the range 8 - 64s according to the integrated blue magnitude of the galaxy and whether it had been detected by IRAS. The limiting sensitivity of the survey, corresponding to the longest integrations in the broad band C60, C100 and C160 filters, is approximately 10mJy (3 sigma). Table A in the scientific justification section (below) tabulates exposure times in each filter, the spacecraft raster, and the coordinates for each AOT execution on a target galaxy (observations of background are not included) in this part of the proposal. The measured ratios of galaxian fluxes and brightnesses to the (generally much brighter) background from zodiacal- and broad-scale cirrus emission will be calibrated by concatenating observations of galaxies in a particular region to absolute photometric measurements of the background using the PHT25 AOT in the same 6 PHT-C filters. East of 12h 42m, where visibility is poor for a spring launch at the limit of the launch window, concatenations are <= 1.1 hours. The LWS survey will be in the grating mode to reach a (3 sigma) limiting line flux of approximately 3.10**(-17)Wm**(-2). Details of the observations with LWS of the subsample of 50 spiral galaxies are described in part 5 of this proposal. We also request to receive the data from the remaining LWS detectors not used to scan the [CII] line. These could give information about the spectrum of the background to validate the calibration of the PHT-C spectrophotometry. In the case of the very brightest galaxies this additional LWS data might furthermore provide detailed information about the spectrum of the galaxy itself - this would be used to validate the method adopted to distinguish dust components of different temperatures from the PHT-C spectrophotometry. <=== scientific_justification ===> The sample of 118 galaxies for ISOPHOT was selected from the Virgo Cluster Catalogue (VCC) of Bingelli et. al. (1985; AJ 1681), which is complete to Bt = 18 magnitude. Only galaxies classified as cluster members in the updated classification of Binggeli et al. (1993; preprint) were included. The sample for the ISO observations consists of two subsamples. The cluster- core subsample comprises of all 26 spiral VCC galaxies later than S0 having Bt < 14.5, and the 19 fainter late-type VCC galaxies having 14.5 <= Bt < 18 from the inner core of VIRGO (within 2 degrees projected angle from M87), essentially from within the "atmosphere" of M87. The cluster-periphery subsample comprises of all 73 spiral, irregular and dwarf VCC galaxies later than S0 having Bt < 18 from the cluster periphery (at least 4 degrees from the position of maximum galaxy surface density), essentially equivalent to galaxies from the field. The periphery subsample is roughly equally divided between dwarfs and irregulars on the one hand, and giant spirals on the other, and should provide unbiased statistical information on a variety of FIR properties, also at low luminosities. The two subsamples will allow unbiased comparisons and contrasts between the infrared activity and morphologies of cluster core galaxies and galaxies essentially selected from the field. This should provide physical insight into the various types of infrared phenomena discovered in the last decade, notably those related to the star-formation activity. Correlations with physical processes manifest at other wavelengths will enable the unfolding of the main evolutionary characteristics of these phenomena. Complementary observations in the CAM 5-8.5 and 12-17 micron bands of the 26 cluster core spirals and the entire cluster periphery sample of ISOPHOT are being proposed by the ISOCAM consortium in a separate proposal. The SWS consortium, also in a separate proposal, is proposing to spectrally scan the remaining four giant spirals with Bt < 14.5 using LWS. Obviously, the superior spatial resolution of CAM of about 6 arcseconds (corresponding to a few hundred parsecs at the distance of the cluster) is sufficient to separate the core region from the disk - at least as far as the warmer dust not covered by the ISOPHOT FIR observations is concerned. Among other structural informations this will place the best constraints on infrared emission powered, or triggered by a discrete non-stellar source at the dynamical centres of galaxies, such as an accreting super-massive object. The [CII] cooling line will probe not only photodissociation regions associated with massive star formation, but also the quiescent diffuse HI component of the interstellar medium. The combination of [CII] line fluxes and the FIR continuum with hydrogen recombination line fluxes, NIR continuum from old stellar populations, HI, CO, as well as radio (synchrotron), UV and X-ray measurements will provide detailed information on the structure and energy balance of the ISM in disks of galaxies, as well as their current and past star-formation activity. Table A: Summary of pointing directions, exposure times and rasters for each galaxy observation in part 4 (for both spring and autumn launches): ----------------------------------------------------------------------------- osn #vcc ra(1950) dec(1950) aot exposure times (s) at ny nz 60 70 100 120 160 200um ----------------------------------------------------------------------------- 1 802 12 22 57.0 13 46 24 PHT22 64 0 64 0 0 0 1 1 2 802 12 22 57.0 13 46 24 PHT32 0 0 0 0 16 0 3 1 3 1001 12 24 52.8 13 59 36 PHT22 32 0 32 0 0 0 1 1 4 1001 12 24 52.8 13 59 36 PHT32 0 0 0 0 16 0 3 1 5 809 12 23 0.6 12 32 12 PHT22 8 8 8 0 0 0 1 1 6 809 12 23 0.6 12 32 12 PHT32 0 0 0 8 8 16 3 1 7 945 12 24 18.0 13 27 12 PHT22 8 8 8 0 0 0 1 1 8 945 12 24 18.0 13 27 12 PHT32 0 0 0 8 8 16 3 1 9 793 12 22 49.8 13 21 0 PHT22 32 0 32 0 0 0 1 1 10 793 12 22 49.8 13 21 0 PHT32 0 0 0 0 16 0 3 1 17 1121 12 26 9.6 11 24 30 PHT22 32 0 32 0 0 0 1 1 18 1121 12 26 9.6 11 24 30 PHT32 0 0 0 0 16 0 3 1 19 950 12 24 21.6 11 50 18 PHT22 8 8 8 0 0 0 1 1 20 950 12 24 21.6 11 50 18 PHT32 0 0 0 8 8 16 3 1 21 995 12 24 49.2 11 8 36 PHT22 16 16 16 0 0 0 1 1 22 995 12 24 49.2 11 8 36 PHT32 0 0 0 16 16 16 3 1 23 1106 12 25 57.0 10 47 48 PHT22 32 0 32 0 0 0 1 1 24 1106 12 25 57.0 10 47 48 PHT32 0 0 0 0 16 0 3 1 25 1200 12 27 2.4 11 4 12 PHT22 8 0 8 0 0 0 1 1 26 1200 12 27 2.4 11 4 12 PHT32 0 0 0 0 16 0 3 1 27 1377 12 29 7.2 11 6 42 PHT22 16 0 16 0 0 0 1 1 28 1377 12 29 7.2 11 6 42 PHT32 0 0 0 0 16 0 3 1 29 1486 12 30 39.0 11 37 12 PHT22 16 16 16 0 0 0 1 1 30 1486 12 30 39.0 11 37 12 PHT32 0 0 0 16 16 16 3 1 31 1356 12 28 51.6 11 46 0 PHT22 8 8 8 0 0 0 1 1 32 1356 12 28 51.6 11 46 0 PHT32 0 0 0 8 8 16 3 1 39 1403 12 29 28.2 13 21 30 PHT22 64 0 64 0 0 0 1 1 40 1403 12 29 28.2 13 21 30 PHT32 0 0 0 0 16 0 3 1 41 1448 12 30 7.8 13 3 0 PHT22 8 0 8 0 0 0 1 1 42 1448 12 30 7.8 13 3 0 PHT32 0 0 0 0 16 0 3 1 43 1313 12 28 17.4 12 19 18 PHT22 32 0 32 0 0 0 1 1 44 1313 12 28 17.4 12 19 18 PHT32 0 0 0 0 16 0 3 1 45 1426 12 29 51.0 12 10 12 PHT22 16 0 16 0 0 0 1 1 46 1426 12 29 51.0 12 10 12 PHT32 0 0 0 0 16 0 3 1 47 1644 12 33 21.0 14 8 0 PHT22 16 16 16 0 0 0 1 1 48 1644 12 33 21.0 14 8 0 PHT32 0 0 0 16 16 16 3 1 49 1287 12 27 52.2 14 15 30 PHT22 32 0 32 0 0 0 1 1 50 1287 12 27 52.2 14 15 30 PHT32 0 0 0 0 16 0 3 1 ----------------------------------------------------------------------------- Table B: Time distribution for spring launch targets (full VIRGO proposal): Team top 40% second 30% last 30% PHT : 39302 17116 0 SOT : 24004 20276 0 total : 63306 37392 0 Table C: Time distribution for autumn launch targets (full VIRGO proposal): Team top 40% second 30% last 30% PHT : 39302 17116 0 SOT : 24004 20276 0 total : 63306 37392 0 <=== autumn_launch_targets ===> 1, "PHT22", 2.0, "N", "VCC0802", 12.38250, 13.77333, 1950, 0., 0., 584, 2 2, "PHT32", 2.0, "N", "VCC0802", 12.38250, 13.77333, 1950, 0., 0., 114, 3 3, "PHT22", 2.0, "N", "VCC1001", 12.41467, 13.99333, 1950, 0., 0., 296, 4 4, "PHT32", 2.0, "N", "VCC1001", 12.41467, 13.99333, 1950, 0., 0., 114, 5 5, "PHT22", 2.0, "N", "VCC0809", 12.38350, 12.53667, 1950, 0., 0., 223, 6 6, "PHT32", 2.0, "N", "VCC0809", 12.38350, 12.53667, 1950, 0., 0., 227, 7 7, "PHT22", 2.0, "N", "VCC0945", 12.40500, 13.45333, 1950, 0., 0., 223, 8 8, "PHT32", 2.0, "N", "VCC0945", 12.40500, 13.45333, 1950, 0., 0., 227, 9 9, "PHT22", 2.0, "N", "VCC0793", 12.38050, 13.35000, 1950, 0., 0., 296, 10 10, "PHT32", 2.0, "N", "VCC0793", 12.38050, 13.35000, 1950, 0., 0., 114, 11 11, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 160, 12 12, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 158, 13 13, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 156, 14 14, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 60, 15 15, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 48, 16 16, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 54, 0 17, "PHT22", 2.0, "N", "VCC1121", 12.43600, 11.40833, 1950, 0., 0., 456, 18 18, "PHT32", 2.0, "N", "VCC1121", 12.43600, 11.40833, 1950, 0., 0., 114, 19 19, "PHT22", 2.0, "N", "VCC0950", 12.40600, 11.83833, 1950, 0., 0., 223, 20 20, "PHT32", 2.0, "N", "VCC0950", 12.40600, 11.83833, 1950, 0., 0., 227, 21 21, "PHT22", 2.0, "N", "VCC0995", 12.41367, 11.14333, 1950, 0., 0., 271, 22 22, "PHT32", 2.0, "N", "VCC0995", 12.41367, 11.14333, 1950, 0., 0., 275, 23 23, "PHT22", 2.0, "N", "VCC1106", 12.43250, 10.79667, 1950, 0., 0., 296, 24 24, "PHT32", 2.0, "N", "VCC1106", 12.43250, 10.79667, 1950, 0., 0., 114, 25 25, "PHT22", 2.0, "N", "VCC1200", 12.45067, 11.07000, 1950, 0., 0., 200, 26 26, "PHT32", 2.0, "N", "VCC1200", 12.45067, 11.07000, 1950, 0., 0., 114, 27 27, "PHT22", 2.0, "N", "VCC1377", 12.48533, 11.11167, 1950, 0., 0., 232, 28 28, "PHT32", 2.0, "N", "VCC1377", 12.48533, 11.11167, 1950, 0., 0., 114, 29 29, "PHT22", 2.0, "N", "VCC1486", 12.51083, 11.62000, 1950, 0., 0., 271, 30 30, "PHT32", 2.0, "N", "VCC1486", 12.51083, 11.62000, 1950, 0., 0., 275, 31 31, "PHT22", 2.0, "N", "VCC1356", 12.48100, 11.76667, 1950, 0., 0., 223, 32 32, "PHT32", 2.0, "N", "VCC1356", 12.48100, 11.76667, 1950, 0., 0., 227, 33 33, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 160, 34 34, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 158, 35 35, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 156, 36 36, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 60, 37 37, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 48, 38 38, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 54, 0 39, "PHT22", 2.0, "N", "VCC1403", 12.49117, 13.35833, 1950, 0., 0., 584, 40 40, "PHT32", 2.0, "N", "VCC1403", 12.49117, 13.35833, 1950, 0., 0., 114, 41 41, "PHT22", 2.0, "N", "VCC1448", 12.50217, 13.05000, 1950, 0., 0., 200, 42 42, "PHT32", 2.0, "N", "VCC1448", 12.50217, 13.05000, 1950, 0., 0., 114, 43 43, "PHT22", 2.0, "N", "VCC1313", 12.47150, 12.32167, 1950, 0., 0., 296, 44 44, "PHT32", 2.0, "N", "VCC1313", 12.47150, 12.32167, 1950, 0., 0., 114, 45 45, "PHT22", 2.0, "N", "VCC1426", 12.49750, 12.17000, 1950, 0., 0., 232, 46 46, "PHT32", 2.0, "N", "VCC1426", 12.49750, 12.17000, 1950, 0., 0., 114, 47 47, "PHT22", 2.0, "N", "VCC1644", 12.55583, 14.13333, 1950, 0., 0., 271, 48 48, "PHT32", 2.0, "N", "VCC1644", 12.55583, 14.13333, 1950, 0., 0., 275, 49 49, "PHT22", 2.0, "N", "VCC1287", 12.46450, 14.25833, 1950, 0., 0., 296, 50 50, "PHT32", 2.0, "N", "VCC1287", 12.46450, 14.25833, 1950, 0., 0., 114, 51 51, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 160, 52 52, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 158, 53 53, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 156, 54 54, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 60, 55 55, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 48, 56 56, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 54, 0 <=== spring_launch_targets ===> 1, "PHT22", 2.0, "N", "VCC0802", 12.38250, 13.77333, 1950, 0., 0., 584, 2 2, "PHT32", 2.0, "N", "VCC0802", 12.38250, 13.77333, 1950, 0., 0., 114, 3 3, "PHT22", 2.0, "N", "VCC1001", 12.41467, 13.99333, 1950, 0., 0., 296, 4 4, "PHT32", 2.0, "N", "VCC1001", 12.41467, 13.99333, 1950, 0., 0., 114, 5 5, "PHT22", 2.0, "N", "VCC0809", 12.38350, 12.53667, 1950, 0., 0., 223, 6 6, "PHT32", 2.0, "N", "VCC0809", 12.38350, 12.53667, 1950, 0., 0., 227, 7 7, "PHT22", 2.0, "N", "VCC0945", 12.40500, 13.45333, 1950, 0., 0., 223, 8 8, "PHT32", 2.0, "N", "VCC0945", 12.40500, 13.45333, 1950, 0., 0., 227, 9 9, "PHT22", 2.0, "N", "VCC0793", 12.38050, 13.35000, 1950, 0., 0., 296, 10 10, "PHT32", 2.0, "N", "VCC0793", 12.38050, 13.35000, 1950, 0., 0., 114, 11 11, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 160, 12 12, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 158, 13 13, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 156, 14 14, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 60, 15 15, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 48, 16 16, "PHT25", 2.0, "N", "VBACK14", 12.39300, 13.39000, 1950, 0., 0., 54, 0 17, "PHT22", 2.0, "N", "VCC1121", 12.43600, 11.40833, 1950, 0., 0., 456, 18 18, "PHT32", 2.0, "N", "VCC1121", 12.43600, 11.40833, 1950, 0., 0., 114, 19 19, "PHT22", 2.0, "N", "VCC0950", 12.40600, 11.83833, 1950, 0., 0., 223, 20 20, "PHT32", 2.0, "N", "VCC0950", 12.40600, 11.83833, 1950, 0., 0., 227, 21 21, "PHT22", 2.0, "N", "VCC0995", 12.41367, 11.14333, 1950, 0., 0., 271, 22 22, "PHT32", 2.0, "N", "VCC0995", 12.41367, 11.14333, 1950, 0., 0., 275, 23 23, "PHT22", 2.0, "N", "VCC1106", 12.43250, 10.79667, 1950, 0., 0., 296, 24 24, "PHT32", 2.0, "N", "VCC1106", 12.43250, 10.79667, 1950, 0., 0., 114, 25 25, "PHT22", 2.0, "N", "VCC1200", 12.45067, 11.07000, 1950, 0., 0., 200, 26 26, "PHT32", 2.0, "N", "VCC1200", 12.45067, 11.07000, 1950, 0., 0., 114, 27 27, "PHT22", 2.0, "N", "VCC1377", 12.48533, 11.11167, 1950, 0., 0., 232, 28 28, "PHT32", 2.0, "N", "VCC1377", 12.48533, 11.11167, 1950, 0., 0., 114, 29 29, "PHT22", 2.0, "N", "VCC1486", 12.51083, 11.62000, 1950, 0., 0., 271, 30 30, "PHT32", 2.0, "N", "VCC1486", 12.51083, 11.62000, 1950, 0., 0., 275, 31 31, "PHT22", 2.0, "N", "VCC1356", 12.48100, 11.76667, 1950, 0., 0., 223, 32 32, "PHT32", 2.0, "N", "VCC1356", 12.48100, 11.76667, 1950, 0., 0., 227, 33 33, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 160, 34 34, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 158, 35 35, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 156, 36 36, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 60, 37 37, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 48, 38 38, "PHT25", 2.0, "N", "VBACK15", 12.47367, 11.76000, 1950, 0., 0., 54, 0 39, "PHT22", 2.0, "N", "VCC1403", 12.49117, 13.35833, 1950, 0., 0., 584, 40 40, "PHT32", 2.0, "N", "VCC1403", 12.49117, 13.35833, 1950, 0., 0., 114, 41 41, "PHT22", 2.0, "N", "VCC1448", 12.50217, 13.05000, 1950, 0., 0., 200, 42 42, "PHT32", 2.0, "N", "VCC1448", 12.50217, 13.05000, 1950, 0., 0., 114, 43 43, "PHT22", 2.0, "N", "VCC1313", 12.47150, 12.32167, 1950, 0., 0., 296, 44 44, "PHT32", 2.0, "N", "VCC1313", 12.47150, 12.32167, 1950, 0., 0., 114, 45 45, "PHT22", 2.0, "N", "VCC1426", 12.49750, 12.17000, 1950, 0., 0., 232, 46 46, "PHT32", 2.0, "N", "VCC1426", 12.49750, 12.17000, 1950, 0., 0., 114, 47 47, "PHT22", 2.0, "N", "VCC1644", 12.55583, 14.13333, 1950, 0., 0., 271, 48 48, "PHT32", 2.0, "N", "VCC1644", 12.55583, 14.13333, 1950, 0., 0., 275, 49 49, "PHT22", 2.0, "N", "VCC1287", 12.46450, 14.25833, 1950, 0., 0., 296, 50 50, "PHT32", 2.0, "N", "VCC1287", 12.46450, 14.25833, 1950, 0., 0., 114, 51 51, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 160, 52 52, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 158, 53 53, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 156, 54 54, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 60, 55 55, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 48, 56 56, "PHT25", 2.0, "N", "VBACK16", 12.50300, 14.32500, 1950, 0., 0., 54, 0