<=== observer ===> "LMETCALF",\ "Metcalfe, L.",\ "",\ "SAI",\ "ESTEC",\ "Keplerlaan 1",\ "2200 AG",\ "Noordwijk",\ "The Netherlands",\ "31 1719 83616",\ "31 1719 85434",\ "lmetcalf@isosa6.estec.esa.nl" <=== proposal ===> "HARO",1,4,\ {"compact galaxies","star formation","galaxy formation","irregular galaxies"},\ {"P. Barr","J. Clavel","P. Gallais","K. Leech", "R. Laureijs","B. McBreen",\ "N. Smith"} <=== title ===> ISO Observations of Blue Compact Galaxies: <=== abstract ===> SCIENTIFIC ABSTRACT Blue Compact Galaxies (BCGs) appear to be relatively unevolved and it is still not clear whether at least some of these are recently formed low-mass galaxies undergoing their first burst of star formation or whether they have experienced a series of bursts. Under close examination at visible wavelengths they exhibit several distinctive morphologies. The evolutionary relationship between BCGs, other dwarf galaxies (such as Low Surface Brightness dwarves) and other galaxy types is still open to speculation. In this proposal, LWS grating, PHT-S spectroscopy and ISOCAM imaging are proposed for a sample of 16 BCGs selected from the catalogues of Haro, Markarian and Zwickey. SWS observations are proposed for two systems, to complement related work by the LWS consortium. For those galaxies bright enough to yield measurements of the strengths of several spectral lines, emission line strengths and line ratios derived from LWS and SWS spectroscopy, along with the continuum spectra, will permit detailed study of the nature of, and the physical conditions in and around, the star- bursts, including elemental abundances, densities and temperatures and the gas-to-dust ratio and dust properties in the systems. For fainter galaxies, measurements of the 158 micron CII fine structure line will probe photodissoc- iation regions associated with massive star formation and also the quiescent diffuse HI component of the interstellar medium. CAM imaging will allow the distribution of dust and related PAH emission to be compared with the structures seen in the visible. PHT-S spectra will support the identification of the "Unidentified feature" (PAH?) emission in the NIR, tracing formation of Carbon rich material around old stars. A correlation will be sought between distinc- tive visible and NIR properties of the sample galaxies and their FIR spectral properties that could help provide the key to identifying truly young galaxies experiencing their first starburst. OBSERVATION SUMMARY The target sources for this proposal can be divided into two categories. Those which have detections recorded in the IRAS PSC and those which have not. Estimates have been made of the fluxes which can be expected from the systems not seen by IRAS, based upon available data at other wavelengths and assuming a visible to FIR spectrum similar to that of their brighter (though not necess- arily more luminous) counterparts. CAM Observations (AOT CAM01): The target galaxies are typically 1 to 2 arcminutes in diameter in the visible. Therefore the CAM 6 arcsecond per pixel f.o.v. has been chosen because it matches well the diffraction spot size for the LW3 and 6 filters used and because it gives an overall f.o.v. (3 arcminutes diameter) well matched to the outer halo size of the target galaxies. Each target observed with CAM is observed in both the LW3 (high sensitivity dust - 12 to 18 micron) filter and the LW6 (Unidentified IR feature - 7 to 8.5 micron ) filter. The IRAS upper limit for the 12 micron flux of those included galaxies not detected by IRAS is as low as 0.1 Jansky. If this flux were spread uniformly over the typical area of one of these targets (about 1 arcminute sq.) that would imply a surface brightness of about 30 micro Jy per square arcsecond. Of course, any IR emmission which does occur is likely to be more concentrated towards the centres of the galaxies, implying higher surface brightness there. Consequently, an observation tuned to detect with S/N of 3 at the 3 microJy per square arcsecond contour should comfortably record any IR emission from the full extent of the galaxies, unless their IR flux is dramatically below the IRAS detection limit. This is highly unlikely since about half of the sample were detected by IRAS. The required observation then is a 3x3 step micro-scan (AOT CAM01) in both the LW3 and LW6 filters in the 6 arcsecond per pixel f.o.v. with a fundamental on-chip integration time (tint) of 5 seconds and a total observation time, including all instrumental and spacecraft overheads, of about 650 seconds per filter on source. The micro-scanning step size is 1.33 pixels. Note that the chosen on-chip integration time is a compromise between longer on-chip integration times, giving lower total read noise, and shorter integration times, giving better immunity to responsive transients in the detector which may follow a movement of the source over the array during the micro-scan. Since the Zodiacal light is bright relative to the target sources in the filters used, such scan-induced transients should not be too severe (the array illumination is quite uniform). It has therefore been assumed that the worst case stabilisation time for the conditions of these observations will not apply, so that dwell times at each position of the microscan can be minimised allowing relatively short overall exposure times. Since we are not forced to use long exposure times to avoid transients, the observation time has been fixed at a duration close to that at which flat-fielding noise causes the S/N to saturate in any case. SWS observations (AOT SWS06): Based upon the IRAS measurements of the two targets to be observed with SWS (25 micron fluxes of about 1 JY) we have determined that the continuum of these galaxies can be detected with S/N of around 10 or better in the 21 to 40 micron range of SWS for a total exposure time of 2609 seconds per target on source. Since these galaxies are typically characterised in the visible as emission line galaxies and since they should be associated with linewidths slightly greated than the SWS spectral resolution at these wavelengths, we may expect to detect and to partly resolve any emission lines standing above the continuum. Consequently, we propose to observe the central regions of these galaxies at the full resolution of the SWS grating in the above wavelength range. Since the short wavelength part of the SWS instrument also records signal while the long wavelength part is scanning, we request also to receive the telemetry from the SWS short wavelength detectors which is recorded during our LW measurements. PHT-S Observations (AOT PHT40): Based upon the IRAS detection of these targets or, for those sources never detected by IRAS, assuming continuum fluxes of around 0.3 to 0.5 of the weakest IRAS upper limit, we conclude that the continuum flux from these galaxies can be detected with S/N in the range 3 to 10 over most of the PHT-S wavelength range if we make single pointing PHT-S observations of the central 25 arcseconds square of the galaxies, as listed in the observation list attached. These observations are performed in triangular chopping mode with chopper throw 150 arcseconds. LWS Observations: For those of the target galaxies which have been detected by IRAS, we propose to obtain full LWS grating spectra using the LWS Grating Wavelength Range AOT (AOT LWS01). For those galaxies too weak to be detected by IRAS, we concentrate on measuring the 158 micron CII line and in the process, taking advantage of the 10 detector spectral multiplex of the LWS instrument to get 9 other samples of the galaxy continua across the full LWS wavelength range, in narrow wavelength bands. The dedicated line measurements employ the LWS Grating Line spectrum AOT (AOT LWS02). For the line scanning measurements for pointed observations in the grating mode. The line scanning AOT LWS02 will be used to achieve a spectral scan about the appropriately redshifted wavelength of the 158 micron CII line. The wavelength range of the scan will cover 4 grating resolution elements on either side of the line with four spectral samples per resolution element. The scans will be performed in the fast scanning mode to ensure optimal detection of weak emission superimposed on a strong continuum. The survey will be complete for all targets observed in this way, down to a line flux of 3.10**(-17)Wm**(-2) with a signal-to-noise ratio of three in the line detection. Due to the design of the LWS instrument in which the 10 detectors spectrally multiplex during a wavelength scan, our CII line scans will also generate 10 fragments of spectra right across the LWS wavelength range giving information about the broader continuum spectrum of the targets. We request this data coming from all LWS detectors. Typical observing times are about 1400 seconds on-source and the same off-source, except for the case of IZW18, which is observed for about 2000 seconds on-source and 2000 seconds off-source. For those galaxies for which full range grating spectra are obtained, the measurement parameters are tailored to the properties of the galaxies as measured by IRAS and are listed in the table below. The table shows the wavel- ength at which the scan starts (start range), the end wavelength (end range), the number of spectral samples per spectral resolution element, whether the scan is performed in fast scanning mode and the total integration time per spectral step. TABLE: Observational settings with LWS for Full Grating Scan observations (LWS01) Galaxy Start range End range Samples per res. Fast (y/n) time/step (sec.) Haro 1 45 180 8 y 1 Haro 5 45 180 4 y 2.5 Haro 9 45 180 4 y 2.5 Haro32 45 180 4 y 3 Haro42 45 180 4 y 4 Mkn297 45 180 8 y 1 Using these observational parameters, the brighter sources are detected with signal to noise ratios on the continuum ranging from 10 to several times 10 over the full LWS range. The fainter targets have S/N in the range 5 to 20 or so. With these S/N values the CII line will be detected comfortably, even if it is several times weaker than expected for these sources. Even for a line strength no greater than 3.10**(-17)Wm**(-2), the value taken as the detection limit for the galaxies not seen by IRAS, such a line, buried in the continuum and unresolved by a factor of about five, would constitute a 2 sigma detection. However, for the galaxies in the table above, the CII line should be much stronger than this. Generic observational requirements for all instruments: For each target observation, reference measurements for background subtraction are recorded on nearby regions of the sky. These background measurements must be contiguous with the source measurements and so they are concatenated to the source observations. We request a peak-up for each PHT-S and SWS pointing. <=== scientific_justification ===> Time distribution for spring launch targets: Team top 40.6% second 36% last 23.4% SOT : 40124 35514 23132 Time distribution for autumn launch targets: Team top 39.8% second 36.8% last 23.4% SOT : 39984 36876 23482 <=== autumn_launch_targets ===> 1, "CAM01", 1.0, "N", "haro03", 10.70458, 56.22306, 1950, 0., 0.,1470, 2 2, "CAM01", 1.0, "N", "bcnd03", 10.70458, 56.30639, 1950, 0., 0.,1310, 0 3, "LWS01", 1.0, "N", "haro05", 11.91556, 32.61333, 1950, 0., 0., 1340, 4 4, "LWS01", 1.0, "N", "bcnd05", 11.91556, 32.69667, 1950, 0., 0., 1180, 0 5, "LWS01", 1.0, "N", "haro09", 12.71389, 27.39861, 1950, 0., 0., 1340, 6 6, "LWS01", 1.0, "N", "bcnd09", 12.71389, 27.48194, 1950, 0., 0., 1180, 0 7, "LWS02", 1.0, "N", "haro22", 09.78831, 28.24667, 1950, 0., 0., 1422, 8 8, "LWS02", 1.0, "N", "bcnd22", 09.78831, 28.33000, 1950, 0., 0., 1262, 0 9, "LWS02", 1.0, "N", "haro23", 10.05717, 29.19556, 1950, 0., 0., 1422, 10 10, "LWS02", 1.0, "N", "bcnd23", 10.05717, 29.27889, 1950, 0., 0., 1262, 0 11, "LWS02", 1.0, "N", "haro30", 12.58697, 27.40139, 1950, 0., 0., 1422, 12 12, "LWS02", 1.0, "N", "bcnd30", 12.58697, 27.48472, 1950, 0., 0., 1262, 0 13, "LWS01", 1.0, "N", "haro32", 12.69264, 55.17972, 1950, 0., 0., 1728, 14 14, "LWS01", 1.0, "N", "bcnd32", 12.69264, 55.26306, 1950, 0., 0., 1568, 0 15, "LWS02", 1.0, "N", "haro33", 12.70167, 28.75000, 1950, 0., 0., 1422, 16 16, "LWS02", 1.0, "N", "bcnd33", 12.70167, 28.83333, 1950, 0., 0., 1262, 0 17, "LWS02", 1.0, "N", "haro36", 12.74425, 51.88639, 1950, 0., 0., 1422, 18 18, "LWS02", 1.0, "N", "bcnd36", 12.74425, 51.96972, 1950, 0., 0., 1262, 0 19, "LWS02", 1.0, "N", "haro38", 13.55453, 29.47111, 1950, 0., 0., 1422, 20 20, "LWS02", 1.0, "N", "bcnd38", 13.55453, 29.55444, 1950, 0., 0., 1262, 0 21, "LWS01", 1.0, "N", "haro42", 14.48222, 27.45194, 1950, 0., 0., 2050, 22 22, "LWS01", 1.0, "N", "bcnd42", 14.48222, 27.53528, 1950, 0., 0., 1890, 0 23, "LWS02", 1.0, "N", "haro43", 14.56586, 28.66778, 1950, 0., 0., 1422, 24 24, "LWS02", 1.0, "N", "bcnd43", 13.55453, 28.75111, 1950, 0., 0., 1262, 0 25, "LWS02", 1.0, "N", "IZW18", 09.50842, 55.46278, 1950, 0., 0., 2180, 26 26, "LWS02", 1.0, "N", "bcndzw18", 09.50842, 55.54611, 1950, 0., 0., 2020, 0 27, "CAM01", 2.0, "N", "haro05", 11.91556, 32.61333, 1950, 0., 0., 1470, 28 28, "CAM01", 2.0, "N", "bcnd05", 11.91556, 32.69667, 1950, 0., 0., 1310, 0 29, "CAM01", 2.0, "N", "haro09", 12.71389, 27.39861, 1950, 0., 0., 1470, 30 30, "CAM01", 2.0, "N", "bcnd09", 12.71389, 27.48194, 1950, 0., 0., 1310, 0 31, "CAM01", 2.0, "N", "haro10", 13.61806, -31.39029, 1950, 0., 0., 1470, 32 32, "CAM01", 2.0, "N", "bcnd10", 13.61806, -31.47362, 1950, 0., 0., 1310, 0 33, "CAM01", 2.0, "N", "haro22", 09.78831, 28.24667, 1950, 0., 0., 1470, 34 34, "CAM01", 2.0, "N", "bcnd22", 09.78831, 28.33000, 1950, 0., 0., 1310, 0 35, "CAM01", 2.0, "N", "haro23", 10.05717, 29.19556, 1950, 0., 0., 1470, 36 36, "CAM01", 2.0, "N", "bcnd23", 10.05717, 29.27889, 1950, 0., 0., 1310, 0 37, "CAM01", 2.0, "N", "haro30", 12.58697, 27.40139, 1950, 0., 0., 1470, 38 38, "CAM01", 2.0, "N", "bcnd30", 12.58697, 27.48472, 1950, 0., 0., 1310, 0 39, "CAM01", 2.0, "N", "haro32", 12.69264, 55.17972, 1950, 0., 0., 1470, 40 40, "CAM01", 2.0, "N", "bcnd32", 12.69264, 55.26306, 1950, 0., 0., 1310, 0 41, "CAM01", 2.0, "N", "haro33", 12.70167, 28.75000, 1950, 0., 0., 1470, 42 42, "CAM01", 2.0, "N", "bcnd33", 12.70167, 28.83333, 1950, 0., 0., 1310, 0 43, "CAM01", 2.0, "N", "haro36", 12.74425, 51.88639, 1950, 0., 0., 1470, 44 44, "CAM01", 2.0, "N", "bcnd36", 12.74425, 51.96972, 1950, 0., 0., 1310, 0 45, "CAM01", 2.0, "N", "haro38", 13.55453, 29.47111, 1950, 0., 0., 1470, 46 46, "CAM01", 2.0, "N", "bcnd38", 13.55453, 29.55444, 1950, 0., 0., 1310, 0 47, "CAM01", 2.0, "N", "haro42", 14.48222, 27.45194, 1950, 0., 0., 1470, 48 48, "CAM01", 2.0, "N", "bcnd42", 14.48222, 27.53528, 1950, 0., 0., 1310, 0 49, "CAM01", 2.0, "N", "haro43", 14.56586, 28.66778, 1950, 0., 0., 1470, 50 50, "CAM01", 2.0, "N", "bcnd43", 13.55453, 28.75111, 1950, 0., 0., 1310, 0 51, "SWS06", 2.0, "N", "haro03", 10.70458, 56.22306, 1950, 0., 0., 2609, 52 52, "SWS06", 2.0, "N", "bcnd03", 10.70458, 56.30639, 1950, 0., 0., 2629, 0 53, "SWS06", 2.0, "N", "Tololo3", 10.07172, -29.69139, 1950, 0., 0., 2609, 54 54, "SWS06", 2.0, "N", "bcndtol3", 10.07172, -29.60806, 1950, 0., 0., 2629, 0 55, "PHT40", 3.0, "N", "haro03", 10.70458, 56.22306, 1950, 0., 0., 776, 0 56, "PHT40", 3.0, "N", "haro05", 11.91556, 32.61333, 1950, 0., 0., 776, 0 57, "PHT40", 3.0, "N", "haro09", 12.71389, 27.39861, 1950, 0., 0., 776, 0 58, "PHT40", 3.0, "N", "haro22", 09.78831, 28.24667, 1950, 0., 0., 1290, 0 59, "PHT40", 3.0, "N", "haro23", 10.05717, 29.19556, 1950, 0., 0., 1290, 0 60, "PHT40", 3.0, "N", "haro30", 12.58697, 27.40139, 1950, 0., 0., 1290, 0 61, "PHT40", 3.0, "N", "haro32", 12.69264, 55.17972, 1950, 0., 0., 776, 0 62, "PHT40", 3.0, "N", "haro33", 12.70167, 28.75000, 1950, 0., 0., 1290, 0 63, "PHT40", 3.0, "N", "haro36", 12.74425, 51.88639, 1950, 0., 0., 1290, 0 64, "PHT40", 3.0, "N", "haro38", 13.55453, 29.47111, 1950, 0., 0., 1290, 0 65, "PHT40", 3.0, "N", "haro42", 14.48222, 27.45194, 1950, 0., 0., 1290, 0 66, "PHT40", 3.0, "N", "haro43", 14.56586, 28.66778, 1950, 0., 0., 1290, 0 67, "PHT40", 3.0, "N", "MKN297", 16.05028, 20.67889, 1950, 0., 0., 776, 68 68, "CAM01", 3.0, "N", "MKN297", 16.05028, 20.67889, 1950, 0., 0., 1310, 69 69, "CAM01", 3.0, "N", "bcnd297", 16.05028, 20.76222, 1950, 0., 0., 1310, 70 70, "LWS01", 3.0, "N", "MKN297", 16.05028, 20.67889, 1950, 0., 0., 1180, 71 71, "LWS01", 3.0, "N", "bcnd297", 16.05028, 20.76222, 1950, 0., 0., 1180, 0 72, "PHT40", 3.0, "N", "IZW18", 09.50842, 55.46278, 1950, 0., 0., 1290, 0 73, "PHT40", 3.0, "N", "Tololo3", 10.07172, -29.69139, 1950, 0., 0., 776, 74 74, "CAM01", 3.0, "N", "Tololo3", 10.07172, -29.69139, 1950, 0., 0., 1310, 75 75, "CAM01", 3.0, "N", "bcndtol3", 10.07172, -29.60806, 1950, 0., 0., 1310, 0 <=== spring_launch_targets ===> 1, "LWS01", 1.0, "N", "haro01", 07.56097, 35.35417, 1950, 0., 0., 1340, 2 2, "LWS01", 1.0, "N", "bcnd01", 07.56097, 35.43750, 1950, 0., 0., 1180, 0 3, "LWS01", 1.0, "N", "haro05", 11.91556, 32.61333, 1950, 0., 0., 1340, 4 4, "LWS01", 1.0, "N", "bcnd05", 11.91556, 32.69667, 1950, 0., 0., 1180, 0 5, "LWS01", 1.0, "N", "haro09", 12.71389, 27.39861, 1950, 0., 0., 1340, 6 6, "LWS01", 1.0, "N", "bcnd09", 12.71389, 27.48194, 1950, 0., 0., 1180, 0 7, "LWS02", 1.0, "N", "haro21", 03.45386, -17.95028, 1950, 0., 0., 1422, 8 8, "LWS02", 1.0, "N", "bcnd21", 03.45386, -18.03361, 1950, 0., 0., 1262, 0 9, "LWS02", 1.0, "N", "haro22", 09.78831, 28.24667, 1950, 0., 0., 1422, 10 10, "LWS02", 1.0, "N", "bcnd22", 09.78831, 28.33000, 1950, 0., 0., 1262, 0 11, "LWS02", 1.0, "N", "haro23", 10.05717, 29.19556, 1950, 0., 0., 1422, 12 12, "LWS02", 1.0, "N", "bcnd23", 10.05717, 29.27889, 1950, 0., 0., 1262, 13 13, "CAM01", 1.0, "N", "haro23", 10.05717, 29.19556, 1950, 0., 0., 1325, 14 14, "CAM01", 1.0, "N", "bcnd23", 10.05717, 29.27889, 1950, 0., 0., 1325, 0 15, "LWS02", 1.0, "N", "haro27", 11.62983, 28.64611, 1950, 0., 0., 1422, 16 16, "LWS02", 1.0, "N", "bcnd27", 11.62983, 28.72944, 1950, 0., 0., 1262, 0 17, "LWS01", 1.0, "N", "haro32", 12.69264, 55.17972, 1950, 0., 0., 1728, 18 18, "LWS01", 1.0, "N", "bcnd32", 12.69264, 55.26306, 1950, 0., 0., 1568, 0 19, "LWS02", 1.0, "N", "haro33", 12.70167, 28.75000, 1950, 0., 0., 1422, 20 20, "LWS02", 1.0, "N", "bcnd33", 12.70167, 28.83333, 1950, 0., 0., 1262, 0 21, "LWS02", 1.0, "N", "haro36", 12.74425, 51.88639, 1950, 0., 0., 1422, 22 22, "LWS02", 1.0, "N", "bcnd36", 12.74425, 51.96972, 1950, 0., 0., 1262, 23 23, "CAM01", 1.0, "N", "haro36", 12.74425, 51.88639, 1950, 0., 0., 1325, 24 24, "CAM01", 1.0, "N", "bcnd36", 12.74425, 51.96972, 1950, 0., 0., 1325, 0 25, "LWS02", 1.0, "N", "haro38", 13.55453, 29.47111, 1950, 0., 0., 1422, 26 26, "LWS02", 1.0, "N", "bcnd38", 13.55453, 29.55444, 1950, 0., 0., 1262, 0 27, "LWS02", 1.0, "N", "IZW18", 09.50842, 55.46278, 1950, 0., 0., 2180, 28 28, "LWS02", 1.0, "N", "bcndzw18", 09.50842, 55.54611, 1950, 0., 0., 2020, 0 29, "CAM01", 1.0, "N", "haro03", 10.70458, 56.22306, 1950, 0., 0.,1485, 30 30, "CAM01", 1.0, "N", "bcnd03", 10.70458, 56.30639, 1950, 0., 0.,1325, 0 31, "CAM01", 2.0, "N", "haro01", 07.56097, 35.35417, 1950, 0., 0., 1485, 32 32, "CAM01", 2.0, "N", "bcnd01", 07.56097, 35.43750, 1950, 0., 0., 1325, 0 33, "CAM01", 2.0, "N", "haro05", 11.91556, 32.61333, 1950, 0., 0., 1485, 34 34, "CAM01", 2.0, "N", "bcnd05", 11.91556, 32.69667, 1950, 0., 0., 1325, 0 35, "CAM01", 2.0, "N", "haro09", 12.71389, 27.39861, 1950, 0., 0., 1485, 36 36, "CAM01", 2.0, "N", "bcnd09", 12.71389, 27.48194, 1950, 0., 0., 1325, 0 37, "CAM01", 2.0, "N", "haro21", 03.45386, -17.95028, 1950, 0., 0., 1485, 38 38, "CAM01", 2.0, "N", "bcnd21", 03.45386, -18.03361, 1950, 0., 0., 1325, 0 39, "CAM01", 2.0, "N", "haro22", 09.78831, 28.24667, 1950, 0., 0., 1485, 40 40, "CAM01", 2.0, "N", "bcnd22", 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