! File: 2301C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:04:56:08 coverpage: title_1: IMAGING OF RADIO HOT SPOTS sci_cat: QUASARS & AGN sci_subcat: JETS proposal_for: GO pi_title: DR. pi_fname: KLAUS pi_lname: MEISENHEIMER pi_inst: MPI FOR ASTRONOMY pi_country: FRG pi_phone: 06221-528-206 keywords_1: RADIO GALAXIES, RADIO JETS, CONTINUUM EMISSION hours_pri: 4.00 num_pri: 1 wf_pc: Y pi_position: RESEARCH FELLOW off_fname: HANS off_lname: ELSAESSER off_title: PROF. DR. off_inst: MPI FUER ASTRONOMIE off_addr_1: D-6900 HEIDELBERG 1, KOENIGSTUHL 17 off_city: HEIDELBERG off_zip: D6900 off_country: FRG ! end of coverpage abstract: line_1: We proposed to obtain optical images of radio hot spots with the HST Planetary line_2: Camera. Based on results of our groundbased observations we selected 3 hot spots line_3: which emit optical synchrotron light (3C 20 west B, 3C 33 south, 3C 111 east). line_4: 3C20 and 3C 33 are in the GTO list and had thus to be omitted. 3C 111 has z ~ line_5: 0.05 where HST will reach a linear resolution of 0.1 kpc, i.e., ~ 1/10 of the line_6: hot spot diameter. We already marginally resolved the optical hot spot from the line_7: ground and will thus be able to study the structure of the places of particle line_8: acceleration in detail. These observations will help to decide between various line_9: models of radio jets feeding the hot spots. ! ! end of abstract general_form_proposers: lname: MEISENHEIMER fname: KLAUS title: P.I. inst: MPI FOR ASTRONOMY country: FRG esa: Y ! lname: ROESER fname: HERMANN-JOSEF title: DR. inst: MPI FUER ASTRONOMIE country: FRG esa: Y ! lname: LAING fname: ROBERT title: DR. inst: ROYAL GREENWICH OBSERVATORY country: UK esa: Y ! lname: PERLEY fname: RICHARD title: DR. mi: A. inst: NRAO country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: This is a very straightforward imaging project. In order to get clean images line_2: of the optical morphology a signal-to-noise ratio of ~ 15 per resolution line_3: element is required. The overall spectra determine the selection of two line_4: appropriate wavebands: 606W and 814W. They essentially use the PC at the lower line_5: and upper limit of its efficiency curve. With F814W we split line_6: the required integration time into 3 exposures in order to detect cosmic ray line_7: events and place the object onto different parts of the detector to improve line_8: flatfielding. Due to the steep spectrum of the hot spot line_9: (flux = 1 microJy/arcsec**2 at 600 nm) three ONE-ORBIT integrations have to line_10: be stacked to reach the attempted S/N ratio in the red filter F606W. ! question: 4 section: 1 line_1: The optimum resolution for optical imaging of radio hot spots would be <= 0.03 line_2: arcsec. Obviously, this is well beyond the capability of any groundbased line_3: observing technique because the targets are faint or very faint (R <= line_4: 22.mag/arcsec**2). Thus interferometric observations won't be possible even with line_5: the next generation of very large ground-based telescopes. Sensitivity and line_6: resolution of the HST should be just sufficient to reach the goals outlined in line_7: the scientific justification. We feel that we actually have pushed the line_8: ground-based observations to their limits: we obtained VLA maps with 0.1 arcsec line_9: resolution, our optical search for radio hot spot counterparts reached a line_10: limiting magnitude of R >= 24.5mag and we have demonstrated that it is possible line_11: to verify the emission of synchrotron radiation by optical polarimetry of line_12: sources as faint as 3C 20 west (R = 23.3mag line_13: our radio & optical observations by flux measurements at 1.3 mm and 2.2 - 1.2 line_14: micron . ! question: 5 section: 1 line_1: Exposure times have been calculated on the basis of the WF/PC Instr. Handbook line_2: (vers. May 89). A S/N of 14 per resolution element (= 22 PC pixel, i.e. the line_3: resolution in F814W) is required in order to study the morpholgy and compare it line_4: with the radio data. Summing up the data in one resolution element allows to line_5: determine the spectral index with an accuracy of +/- 0.35 which is sufficient to line_6: detect the expected variations across the source. ! question: 7 section: 1 line_1: Two of us (KM & HJR) have quite a substantial experience in reducing CCD-data line_2: from ground-based telescopes. Thus the basic data reduction is no problem. We line_3: already have compared data from the VLA with optical images. All necassary line_4: software is at hand. We have done Monte Carlo simulations of synchrotron sources line_5: to get the spectra from various field geometries. The latter will be compared line_6: with the results of the HST observations. ! question: 10 section: 1 line_1: The MPI fuer Astronomie is the largest optical observatory in Germany operating line_2: the German Spanish Observatory on Calar Alto (Spain). We do have all image line_3: processing facilities, man power and experience needed to accomplish the line_4: complete data reduction and analysis at the institute (MIDAS, AIPS etc.). Our line_5: group at the MPIA currently consists of 3 research scientists and 3 PhD line_6: students. More students may get involved in this project in the near future. line_7: Travel funds (for us and for guests) are available for regular meetings with our line_8: collaboratours. ! !end of general form text general_form_address: lname: MEISENHEIMER fname: KLAUS title: DR. category: PI inst: MAX-PLANCK INSTITUT FUER ASTRONOMIE addr_1: KOENIGSTUHL 17 city: D6900 HEIDELBERG 1 country: FR GERMANY ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: 3C111EAST descr_1: HOT SPOT OF FR-II RADIO GALAXY pos_1: RA = 4H 15M 09.74S +/- 0.07S, pos_2: DEC = +37D 55' 15.1" +/- 1.0" equinox: 1950.0 rv_or_z: Z = 0.0485 fluxnum_1: 1 fluxval_1: SURF(8100) = 1.4 +/- 0.2 E-18 fluxnum_2: 2 fluxval_2: SURF(6000) = 0.8 +/- 0.1 E-18 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: 3C111EAST config: PC opmode: IMAGE aperture: P6 sp_element: F814W num_exp: 1 time_per_exp: 1300S s_to_n: 7 s_to_n_time: 1300S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO param_2: PRE-FLASH=YES req_1: POS TARG -16.5, +16.5 comment_1: S/N IS CALCULATED FOR A RESOLUTION comment_2: ELEMENT OF 22 PIXELS ! linenum: 2.000 targname: 3C111EAST config: PC opmode: IMAGE aperture: P6 sp_element: F814W num_exp: 1 time_per_exp: 1300S s_to_n: 7 s_to_n_time: 1300S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO param_2: PRE-FLASH=YES req_1: POS TARG -13.5, +16.5 comment_1: S/N IS CALCULATED FOR A RESOLUTION comment_2: ELEMENT OF 22 PIXELS ! linenum: 3.000 targname: 3C111EAST config: PC opmode: IMAGE aperture: P6 sp_element: F814W num_exp: 1 time_per_exp: 1300S s_to_n: 7 s_to_n_time: 1300S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO param_2: PRE-FLASH=YES req_1: POS TARG -16.5, +13.5 comment_1: S/N IS CALCULATED FOR A RESOLUTION comment_2: ELEMENT OF 22 PIXELS ! linenum: 4.000 targname: 3C111EAST config: PC opmode: IMAGE aperture: P6 sp_element: F606W num_exp: 1 time_per_exp: 2500S s_to_n: 8 s_to_n_time: 2500S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -16.5, +16.5 comment_1: S/N IS CALCULATED FOR A RESOLUTION comment_2: ELEMENT OF 22 PIXELS ! linenum: 5.000 targname: 3C111EAST config: PC opmode: IMAGE aperture: P6 sp_element: F606W num_exp: 1 time_per_exp: 2500S s_to_n: 8 s_to_n_time: 2500S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -13.5, +16.5 comment_1: S/N IS CALCULATED FOR A RESOLUTION comment_2: ELEMENT OF 22 PIXELS ! linenum: 6.000 targname: 3C111EAST config: PC opmode: IMAGE aperture: P6 sp_element: F606W num_exp: 1 time_per_exp: 2500S s_to_n: 8 s_to_n_time: 2500S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -16.5, +13.5 comment_1: S/N IS CALCULATED FOR A RESOLUTION comment_2: ELEMENT OF 22 PIXELS ! ! end of exposure logsheet ! No scan data records found