! File: 2698C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:10:27:53 coverpage: title_1: LYMAN-ALPHA IMAGING OF YOUNG AND FORMING GALAXIES AT LARGE REDSHIFTS sci_cat: GALAXIES & CLUSTERS proposal_for: GO pi_title: P.I. pi_fname: S. pi_lname: DJORGOVSKI pi_inst: CALTECH pi_country: USA pi_phone: (818)-356-4415 keywords_1: GALAXIES: FORMATION-GALAXIES: RADIO-GALAXIES:EMISSION keywords_2: LINE-COSMOLOGY. hours_pri: 16.10 num_pri: 2 wf_pc: X funds_amount: 141633 funds_length: 27 funds_date: JUN-91 pi_position: ASSOCIATE PROFESSOR off_fname: DR. EARL off_lname: FREISE off_title: DIRECTOR, SPONS.RES. off_inst: CALIFORNIA INSTITUTE OF TECHNOLOGY off_addr_1: MS 213-06,CALTECH off_city: PASADENA off_state: CA. off_zip: 91125 off_country: USA off_phone: (818)-356-6357 off_telex: 188192 OR 675425 ! end of coverpage abstract: line_1: A number of the recently discovered optical counterparts of powerful radio line_2: sources such as 3C 326.1 at z ~= 1.8 have properties which can be interpreted line_3: as those of giant galaxies or cluster cores in the process of formation. line_4: Among these are the galaxies' large size, clumpy appearance, strong Ly alpha line_5: emission, low continuum surface brightness, large velocity fields, and line_6: estimated star formation rates of several hundred Mo/yr. While the presence line_7: of strong radio lobes marks these objects as atypical, they are the best line_8: candidates for primeval galaxies now known. UV imaging with the HST can check line_9: this hypothesis, and provide further insights into their nature. We propose line_10: to do imaging in intermediate width bands containing the Ly alpha line of line_11: 3C 326.1, our primary primeval galaxy candidate, and 3C 256, a radio galaxy line_12: with comparable redshift which shows a strong Ly alpha, bright and compact line_13: stellar continuum, and is an excellent example of the radio-optical alignment line_14: effects. The initial burst of star formation in 3C 256 may be over, but it is line_15: still very young and actively evolving. Ly alpha imaging will reveal the line_16: distribution of star formation in these galaxies, and constrain estimates of line_17: star formation rate, jet-galaxy interaction, and and gas ionization mechanisms. ! ! end of abstract general_form_proposers: lname: SPINRAD fname: H. inst: CALIFORNIA, UNIVERSITY OF, BERKELEY country: USA ! lname: DICKINSON fname: M. inst: CALIFORNIA, UNIVERSITY OF, BERKELEY country: USA ! lname: STRAUSS fname: M. inst: CALTECH country: USA ! lname: WEIR fname: N. inst: CALTECH country: USA ! lname: THOMPSON fname: D. inst: CALTECH country: USA ! lname: SMITH fname: J. inst: CALTECH country: USA ! lname: VAN BREUGEL fname: W. inst: CALIFORNIA, UNIVERSITY OF, BERKELEY country: USA ! lname: DJORGOVSKI fname: S. title: P.I. inst: CALTECH country: USA ! lname: MCCARTHY fname: P. inst: OCIW country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: This revised proposal reflects our reassessment and suggested modifications of line_2: the original proposal, and resulting recommendations by the TAC. The changes line_3: in the scope of the proposal are as follows: line_4: The original (phase 1) version of this proposal had eight targets; per the TAC line_5: request, this list was pared down to four objects in phase 2. Since one must line_6: now increase the integration times by a factor of a few in order to compensate line_7: for the OTA problems, we believe that the best course at this point is to line_9: reduce the number of targets and the diversity of exposure types, and to invest line_10: more integration time in fewer objects and filters. Thus, we decided to devote line_11: an approximately equal net observing time to the two most interesting objects, line_12: 3C 326.1 and 3C 256, and to do them well. We also decided to eliminate any line_13: FOC/96 exposures, and replace them with the closest PC equivalents (in terms line_14: of the bandpasses). This is motivated by the desire to include some PSF stars line_15: in the fields, and thus help any image restoration attempts, and to simplify line_16: the operational requirements. Since the PC exposures provide more signal per line_17: unit time than the FOC/96 exposures, and there is no instrument setup change line_18: (all of our new proposed exposures are with PC), there is some time saving. line_19: (The FOC was originally proposed in part because of its better sampling, an line_20: issue which is now practically irrelevant.) The details of filters, etc., line_21: are given in the answer to Question 5 below. According to the RPSS resource line_22: estimator, our total exposure time is 14.14 hours, the spacecraft time is line_23: 16.09 hours, and the efficiency is thus 87.9 %. ! question: 4 section: 1 line_1: We have pursued the optical imaging from the ground of the four 3CR galaxies line_2: mentioned above as far as is practical with 3 to 5-m class telescopes. We also line_3: have high-quality VLA maps, and will be obtaining more spectra and near-IR line_4: images in the future. However, high-resolution imaging with HST is essential line_5: to determine the kpc-scale structure of these systems, especially in the light line_6: of Ly alpha; recall that it is the morphology of these systems, and their line_7: strong Ly alpha emission which make them interesting and good primeval galaxy line_8: candidates in the first place. ! question: 5 section: 1 line_1: For both targets, we wish to obtain images using PC8 (it has the highest UV line_2: sensitivity), and filters F336W (which includes the redshifted Ly alpha line line_3: near the peak of its transmission, for both objects), and F413M (which samples line_4: the line-free continuum). The former replaces the originally proposed FOC line_5: exposures; the latter is the same as originally proposed. For 3C326.1, we wish line_6: to obtain 2 exposures of 600 sec, and 6 exposures of 1800 sec with F413M (which line_7: samples the line-free continuum), and 2 exposures of 600 sec, one of 1100 sec, line_8: and 9 of 1800 sec with F336W (which samples the Lyman alpha line and some line_9: continuum). For 3C256, we wish to obtain 2 exposures of 600 sec, and 4 exposures line_10: of 1800 sec with F413M, and 2 exposures of 600 sec, and 6 of 1800 sec with line_11: F336W. For this integration time, our estimates of the S/N, using the Handbook, line_12: the Preliminary Report on HST Performance for Cycle 1 GO's, and the materials line_13: provided at the recent STScI workshop, with the increase factor of 5, give the line_14: range S/N =~ 10 - 30 for individual bright regions in these galaxies, or S/N =~ line_15: 20 - 40 for the entire objects (or slightly higher in F336W, due to the large line_16: equivalent widths of the Ly alpha lines). ! question: 7 section: 1 line_1: We have working image processing and data analysis packages at our home line_2: institutions, including a superb Maximum Entropy image restoration package, line_3: which was exported to the STScI, and assorted other software (Lucy, Wiener, line_4: and other methods). We have done extensive image restoration experiments, line_5: using both real and simulated HST data. We are confident that we can restore line_6: the effective angular resolution of the HST images comparable to those line_7: proposed here down to the angular resolution of about 0.1 arcsec, with the line_8: photometric distortions well understood. ! question: 10 section: 1 line_1: Our institutions have extensive computing and other research facilities line_2: (libraries, etc.), and there is no shortage of additional graduate students line_3: which can participate in this project. Along with the support requested line_4: with the present proposal, we should have quite adequate resources to line_5: analyse the data and publish the results very rapidly. ! !end of general form text general_form_address: lname: DJORGOVSKI fname: S. title: PROF. category: PI inst: CALTECH addr_1: ASTRONOMY, MS 105-24 addr_2: CALTECH city: PASADENA state: CA zip: 91125 country: USA phone: 818-356-4415 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: 3C326.1 descr_1: GALAXY; RADIO GALAXY pos_1: RA = 15H 53M 57.3S +/- 1", pos_2: DEC = +20D 13' 00" +/- 1" equinox: 1950 pm_or_par: N rv_or_z: Z = 1.825 comment_1: WE WISH TO USE PC8, AS IT HAS THE comment_2: HIGHEST UV SENSITIVITY, BUT ALSO comment_3: TO AVOID THE BAUM SPOT (SEE OUR comment_4: POS TARG REQUIREMENTS). IF THIS comment_5: IS TOO DIFFICULT TO SCHEDULE, comment_6: PC6 CCD WITH THE DEFAULT (MIDDLE) comment_7: POINTING MAY BE ACCEPTABLE. fluxnum_1: 1 fluxval_1: V = 23 +/- 0.5 ! targnum: 2 name_1: 3C256 descr_1: GALAXY; RADIO GALAXY pos_1: RA = 11H 18M 04.15S +/- 0.5", pos_2: DEC = +23D 44' 21.2" +/- 0.5" equinox: 1950 pm_or_par: N rv_or_z: Z = 1.819 comment_1: WE WISH TO USE PC8, AS IT HAS THE comment_2: HIGHEST UV SENSITIVITY, BUT ALSO comment_3: TO AVOID THE BAUM SPOT (SEE OUR comment_4: POS TARG REQUIREMENTS). IF THIS comment_5: IS TOO DIFFICULT TO SCHEDULE, comment_6: PC6 CCD WITH THE DEFAULT (MIDDLE) comment_7: POINTING MAY BE ACCEPTABLE. fluxnum_1: 1 fluxval_1: V = 22.5 +/- 0.3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: 3C326.1 config: PC opmode: IMAGE aperture: P8 sp_element: F413M num_exp: 2 time_per_exp: 600S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ; req_2: POS TARG 8.4, -8.4 ; comment_1: WE WISH TO USE PC8, SINCE HIGHEST comment_2: UV SENSITIVITY, BUT ALSO WISH TO comment_3: AVOID THE BAUM SPOT (SEE POS TARG comment_4: REQUIREMENTS). IF TOO DIFFICULT comment_5: TO SCHEDULE, PC6 WITH THE DEFAULT comment_6: (MIDDLE) POINTING MAY BE ACCEPTABLE. ! linenum: 2.000 targname: 3C326.1 config: PC opmode: IMAGE aperture: P8 sp_element: F413M num_exp: 6 time_per_exp: 1800S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ; req_2: POS TARG 8.4, -8.4 ; ! linenum: 3.000 targname: 3C326.1 config: PC opmode: IMAGE aperture: P8 sp_element: F336W num_exp: 2 time_per_exp: 600S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ; req_2: POS TARG 8.4, -8.4 ; ! linenum: 4.000 targname: 3C326.1 config: PC opmode: IMAGE aperture: P8 sp_element: F336W num_exp: 1 time_per_exp: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ; req_2: POS TARG 8.4, -8.4 ; ! linenum: 5.000 targname: 3C326.1 config: PC opmode: IMAGE aperture: P8 sp_element: F336W num_exp: 9 time_per_exp: 1800S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ; req_2: POS TARG 8.4, -8.4 ; ! linenum: 6.000 targname: 3C256 config: PC opmode: IMAGE aperture: P8 sp_element: F413M num_exp: 2 time_per_exp: 600S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ; req_2: POS TARG 8.4, -8.4 ; comment_1: WE WISH TO USE PC8, SINCE HIGHEST comment_2: UV SENSITIVITY, BUT ALSO WISH TO comment_3: AVOID THE BAUM SPOT (SEE POS TARG comment_4: REQUIREMENTS). IF TOO DIFFICULT comment_5: TO SCHEDULE, PC6 WITH THE DEFAULT comment_6: (MIDDLE) POINTING MAY BE ACCEPTABLE. ! linenum: 7.000 targname: 3C256 config: PC opmode: IMAGE aperture: P8 sp_element: F413M num_exp: 4 time_per_exp: 1800S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ; req_2: POS TARG 8.4, -8.4 ; ! linenum: 8.000 targname: 3C256 config: PC opmode: IMAGE aperture: P8 sp_element: F336W num_exp: 2 time_per_exp: 600S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ; req_2: POS TARG 8.4, -8.4 ; ! linenum: 9.000 targname: 3C256 config: PC opmode: IMAGE aperture: P8 sp_element: F336W num_exp: 6 time_per_exp: 1800S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ; req_2: POS TARG 8.4, -8.4 ; ! ! end of exposure logsheet ! No scan data records found