<=== observer ===> "CBONOLI",\ "Bonoli, C.",\ "",\ "Osservatorio Astronomico di Padova",\ "vicolo Osservatorio 5",\ "",\ "35122",\ "Padova",\ "Italy",\ " 39 49 8293481",\ " 39 49 8759840",\ "39003::BONOLI" <=== proposal ===> "CAMBARRE",\ 1,\ 5,\ {"normal galaxies","starburst galaxies","star formation", \ "HII regions"},\ {"Bosma, A.","Gallais, P.","Hawarden, T.",\ "Mazzei, P.","Vigroux, L."} <=== title ===> Star formation in Barred Spiral Galaxies <=== abstract ===> SCIENTIFIC ABSTRACT: It is well known that morphological peculiarities in galaxies like bars and rings correlate with star formation activity and that the most favorable wavelength region to observe them is the infrared. ISOCAM is the instrument operating at the highest spatial resolution available on ISO. It will be possible to resolve nuclear and circumnuclear regions, where starbursts principally occur in barred spiral galaxies, or diffuse components. We propose a broad band mapping with ISOCAM to study the phenomenology of infrared activity in barred spiral galaxies in order to investigate the distribution of star formation within the galaxies. The goal of this program is to study the distribution of warm dust inside the HII regions and the distribution of PAHs, stressing the mechanisms of destruction of small grains. Correlations with optical (H alpha) and radio (HI, CO) maps will permit an assessment of the relationship between star formation and global dynamics of the systems. A comparison sample of unbarred spiral galaxies, with both high and low FIR luminosity, will be provided by the study of the Virgo cluster spirals considered in the complementary proposal: "A coordinated study of galaxies in the Virgo cluster". OBSERVATION SUMMARY: A sample of 12 barred spiral galaxies was selected with the following criteria: almost face-on; within a distance of nearly 25 Mpc; with absolute B magnitudes around -20.5; with a FIR luminosity >= 5 E9 L(sun). Each galaxy will be observed with 2 filters: LW2 (5.0-8.5 micron, resolution = 2) and LW3 (12.0-18.0 micron, resolution = 3) and in two optical configurations: 6 arcsec and 3 arcsec PFOV. LW3 will allow to determine the "normal" warm dust emission, while the LW2 will trace the strongest very small grains or PAH emissions at 6.2 and 7.7micron. This filter strategy is identical to the one used in the proposal for mapping nearby normal galaxies. >From known examples (e.g. NGC 1097 (Osmer and Smith, Ap.J. 192, 279, 1974) or NGC 1068 (Telesco and Decher, Ap.J. 334, 573, 1988)) the diameter of the circumnuclear rings is between 1.5 to 2 kpc. At a distance of 20 Mpc, this corresponds to nearly 20 arcsec and, in the configuration of PFOV=6 arcsec, corresponds to 3-4 pixels, and to 6-8 pixels with PFOV=3 arcsec. Observations with the 3 arcsec will be used to separate the nuclear emission from the ring emission, if any; and the 6 arcsec will be used to measure the relative contribution of star forming regions and the diffuse disk component. We estimated an exposure time of 1.0 hours for each galaxy (total for the two filters), where 0.47 hours will be spent on the inner region. This time is comprehensive of stabilisation, repointing and slew times. It is given for a signal to noise ratio of 3 at 2mJy/arcsec2 (the sensitivity limit of the IRAS map at 12 micron) and estimating the background level with the IRSKY facility (IPAC) for each galaxy position and wavelength range. <=== scientific_justification ===> Time distribution for autumn launch targets: Team top 40% second 30% last 30% CAM : 21600 25200 total : 21600 25200 Time distribution for spring launch targets: Team top 40% second 30% last 30% CAM : 21600 25200 total : 21600 25200 <=== autumn_launch_targets ===> 1, "CAM01", 2.0, "N", "NGC289", 00.83811, -31.47833, 1950, 0, 0, 3600, 0 2, "CAM01", 2.0, "N", "NGC1097", 02.73647, -30.48388, 1950, 0, 0, 3600, 0 3, "CAM01", 2.0, "N", "NGC4535", 12.53008, +08.47111, 1950, 0, 0, 3600, 0 4, "CAM01", 2.0, "N", "NGC1530", 04.28419, +75.17777, 1950, 0, 0, 3600, 0 5, "CAM01", 2.0, "N", "NGC1672", 04.74906, -59.33500, 1950, 0, 0, 3600, 0 6, "CAM01", 2.0, "N", "NGC4027", 11.94911, -18.98722, 1950, 0, 0, 3600, 0 7, "CAM01", 3.0, "N", "NGC5383", 13.91778, +42.08889, 1950, 0, 0, 3600, 0 8, "CAM01", 3.0, "N", "NGC337", 00.95555, -07.84778, 1950, 0, 0, 3600, 0 9, "CAM01", 3.0, "N", "NGC613", 01.53308, -29.67555, 1950, 0, 0, 3600, 0 10, "CAM01", 3.0, "N", "NGC1022", 02.61572, +27.63444, 1950, 0, 0, 3600, 0 11, "CAM01", 3.0, "N", "NGC4691", 12.76075, -03.06000, 1950, 0, 0, 3600, 0 12, "CAM01", 3.0, "N", "NGC7552", 23.22358, -42.85750, 1950, 0, 0, 3600, 0 13, "CAM01", 3.0, "N", "NGC1433", 3.67722, -47.3800, 1950, 0, 0, 3600, 0 <=== spring_launch_targets ===> 1, "CAM01", 2.0, "N", "NGC289", 00.83811, -31.47833, 1950, 0, 0, 3600, 0 2, "CAM01", 2.0, "N", "NGC1097", 02.73647, -30.48388, 1950, 0, 0, 3600, 0 3, "CAM01", 2.0, "N", "NGC1398", 03.61238, -26.49833, 1950, 0, 0, 3600, 0 4, "CAM01", 2.0, "N", "NGC3351", 10.68858, -11.96722, 1950, 0, 0, 3600, 0 5, "CAM01", 2.0, "N", "NGC3359", 10.72253, +63.48444, 1950, 0, 0, 3600, 0 6, "CAM01", 2.0, "N", "NGC1530", 04.28419, +75.17777, 1950, 0, 0, 3600, 0 7, "CAM01", 3.0, "N", "NGC1672", 04.74906, -59.33500, 1950, 0, 0, 3600, 0 8, "CAM01", 3.0, "N", "NGC337", 00.95555, -07.84778, 1950, 0, 0, 3600, 0 9, "CAM01", 3.0, "N", "NGC613", 01.53308, -29.67555, 1950, 0, 0, 3600, 0 10, "CAM01", 3.0, "N", "NGC1022", 02.61572, +27.63444, 1950, 0, 0, 3600, 0 11, "CAM01", 3.0, "N", "NGC3504", 11.00792, +28.24083, 1950, 0, 0, 3600, 0 12, "CAM01", 3.0, "N", "NGC7552", 23.22358, -42.85750, 1950, 0, 0, 3600, 0 13, "CAM01", 3.0, "N", "NGC1433", 3.67722, -47.3800, 1950, 0, 0, 3600, 0