! $Id: 5470,v 16.1 1994/08/25 15:42:42 pepsa Exp $ coverpage: title_1: WFPC2 IMAGING OF THE PROTOGALAXY CANDIDATE B2 0902+34 sci_cat: GALAXIES & CLUSTERS sci_subcat: DISTANT GALAXIES proposal_for: GO pi_fname: PETER pi_mi: R pi_lname: EISENHARDT pi_inst: JPL pi_country: USA pi_phone: 818-354-4395 hours_pri: 14.01 num_pri: 1 wf_pc: Y off_fname: CHARLES off_lname: ELACHI off_title: ASST. LAB. DIRECTOR off_inst: 2370 off_addr_1: JET PROPULSION LABORATORY off_addr_2: M/S 180-704 off_addr_3: 4800 OAK GROVE DRIVE off_city: PASADENA off_state: CA off_zip: 91109 off_country: USA off_phone: (818) 354 5673 ! end of coverpage abstract: line_1: We propose to obtain high spatial resolution imaging with WFPC2 of the line_2: continuum and Ly-alpha line emission from the distant radio galaxy B2 line_3: 0902+34. This object appears to have the largest UV to optical (rest line_4: frame) flux ratio measured for a radio galaxy, and at z=3.395 is also line_5: among the most distant galaxies known. It is therefore an excellent line_6: candidate for a protogalaxy. Our objective is to obtain a clearer picture line_7: of the formation process in this galaxy. The proposed observations will line_8: reveal the distribution of star-forming regions and emission line gas, line_9: and the relationship between them, on a 1 kpc scale, as well as their line_10: relationship to the radio source structure. ! ! end of abstract general_form_proposers: lname: EISENHARDT fname: PETER mi: R inst: 2370 country: USA ! lname: LILLY fname: SIMON inst: 4664 country: CANADA ! lname: LU fname: NANYAO mi: Y inst: 2370 country: USA ! lname: DICKINSON fname: MARK inst: 3470 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose to use WFPC2 to 5.5 hours of integration with the Planetary line_2: Camera and F622W to measure the rest frame UV continuum in B2 0902+34. line_3: We also propose to obtain a total of 6.1 hours of integration with the line_4: linear ramp filter, centering B2 0902+34 at the 5341 Angstrom line_5: position on the WF4 array, to measure the redshifted Ly alpha morphology. line_6: The total integration times of 19800 seconds through F622W and line_7: 22000 seconds through the LRG will each be broken into three line_8: groups of 3 to 4 2200 second exposures each. line_9: We use 2200 seconds as our estimate for the maximum line_10: available unocculted time per orbit, but because all of line_11: our observations will be read-noise limited, we hope that line_12: the actual per orbit exposure time can be adjusted to its line_13: maximum allowable length (within the constraint of the line_14: total spacecraft time allocation) in order to maximize our line_15: resulting S/N. The multiple exposures (3 to 4) taken within line_16: each FGS lock position will suffice to allow cosmic ray removal, line_17: thus we set CRSPLIT=NO. Between each FGS lock position, line_18: we plan to reposition the object by approx. 0.5 arcsec using line_19: POS TARG specifications in order to avoid bad pixels. The line_20: exposures taken through each filter should be obtained on line_21: consecutive orbits. ! question: 4 section: 1 line_1: Figure 2 of section 2 of our Phase I proposal illustrates deep line_2: (hours of KPNO 4m time) subarcsec line_3: imaging in narrow and broadband filters of B2 0902+34. line_4: We have also line_5: obtained deep optical and near IR spectra, which confirm line_6: the corrections for line emssion to the continuum flux, line_7: and result in a flat, line-free line_8: continuum characteristic of a protogalaxy. line_9: Both the flat (young) SED and line_10: figure 2 suggest there is complex structure within the line_11: central 2 " of the source, corresponding to roughly 14 kpc. line_12: Detecting whether there are two subcomponents or many line_13: (many subcomponents are plausible for a dynamically young object) line_14: requires significantly better spatial resolution than Figure line_15: 2 provides, or is currently feasible from the ground, line_16: while HST's ability line_17: to resolve 1kpc scales is well matched to the expected substructure. line_18: We will propose to obtain space IR measurements of this object line_19: from ISO and SIRTF, when they become available. ! ! question: 9 section: 1 line_1: 4575 "WF/PC Observations of the Most Luminous Galaxy in the line_2: Universe; the IRAS Source FSC 10214+4724", Peter Eisenhardt coI line_3: 1229 - "OPTICAL AND ULTRAVIOLET IMAGING OF LARGE REDSHIFT line_4: RADIO GALAXIES " S.Lilly coI line_5: 2365 - "HST IMAGING OF GROUND-BASED ULTRA-DEEP SURVEY FIELDS line_6: Simon J. Lilly PI line_7: 2684-KP - "HST MEDIUM-DEEP SURVEY: CYCLE 1 OBSERVATIONS line_8: S.Lilly coI (continuations in 4018, 4029, 4105, 4106) line_9: 2695 - "MORPHOLOGY OF PKS 1614+051, A QUASAR-GALAXY PAIR AT line_10: Z=3.21 M.Dickinson coI line_11: 2698 - "LYMAN-ALPHA IMAGING OF YOUNG AND FORMING GALAXIES AT line_12: LARGE REDSHIFTS " M.Dickinson coI line_13: 3543 - "THE DEEP ULTRAVIOLET SKY ", Simon J. Lilly PI line_14: 3654 - "HIGH RESOLUTION MORPHOLOGIES AND COLORS IN DISTANT line_15: RADIO GALAXIES "M.Dickinson coI line_17: None are directly related to this proposal. line_19: No results have yet been published. ! question: 10 section: 1 line_1: Sun workstations at JPL, U of Toronto, and UC Berkeley. line_2: However we expect to need one additional SPARCstation LX line_3: and 1GB disk drive and have budgeted 50% of this cost to line_4: STScI, with the remainder coming from JPL funds. Op line_5: We have IRAF/SDAS installed and have developed numerous software line_6: routines relevant to the data reduction and analysis which we line_7: will apply (see Section 7.) ! !end of general form text general_form_address: lname: Eisenhardt fname: Peter mi: R category: PI inst: 2370 addr_1: MS 169-327 addr_2: Jet Propulsion Laboratory addr_3: 4800 Oak Grove Drive city: Pasadena state: CA zip: 91109 country: USA phone: 818-354-4395 telex: prme@kromos.jpl.nasa.gov ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: B20902+34 descr_1: E,315,322,325 pos_1: RA = 9H 2M 24.80S +/- 0.03S, pos_2: DEC = +34D 19' 57.0" +/- 0.3" equinox: 1950 rv_or_z: Z = 3.395 comment_1: OBSERVED R AND 5342 FLUXES 100 comment_2: TIMES LARGER BUT EXTENDED OVER comment_3: SEVERAL ARCSEC. GOAL IS S/N=5 comment_4: ON UNRESOLVED STRUCTURES WITH comment_5: 1% OF OBSERVED TOTAL FLUXES. comment_6: OUR GROUNDBASED IMAGES SHOW comment_7: MUCH SUBSTRUCTURE IN THIS OBJECT. fluxnum_1: 1 fluxval_1: R=28.5 fluxnum_2: 2 fluxval_2: F-LINE(5342)=30 +/- 5 E-18 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: B20902+34 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F622W num_exp: 1 time_per_exp: 2100.00S s_to_n: 5 s_to_n_time: 18000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: SEQ 1.0-1.5 NO GAP; req_2: POS TARG +0.00, +0.00; req_3: CYCLE 4 / 1.0-3.5; req_4: SAME ORIENT FOR 1.5-3.5 AS 1.0; req_5: GROUP 1.0-3.5 WITHIN 20D comment_1: ADJUST EXP TIME +INFINITY/-10% TO FIT comment_2: IN AN ALIGNMENT. 3 EXP/POS FOR CR comment_3: DETECTION, UNINTERRUPTED EXPOSURES comment_4: NEEDED TO ACHIEVE DESIRED S/N. ! linenum: 1.500 targname: B20902+34 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F622W num_exp: 2 time_per_exp: 2400.00S s_to_n: 5 s_to_n_time: 18000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: SAME POS FOR 1.5 AS 1.0 ! linenum: 2.000 targname: B20902+34 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F622W num_exp: 1 time_per_exp: 2400.00S s_to_n: 5 s_to_n_time: 18000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: POS TARG +0.322, +0.322; req_2: SEQ 2.0-2.5 NO GAP comment_1: ADJUST EXP TIME +INFINITY/-10% comment_2: TO FIT IN AN ALIGNMENT. SECOND POS comment_3: TO AVOID PATTERN NOISE. FOR ALL 3 POS comment_4: USE SAME OPTIMUM CENTER BUT NOTE THAT comment_5: POS TARG REQT DOES NOT IMPLY A NEED comment_6: FOR ABSOLUTE POINTING ACCURACY < 1" ! linenum: 2.500 targname: B20902+34 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F622W num_exp: 2 time_per_exp: 2400.00S s_to_n: 5 s_to_n_time: 18000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: SAME POS FOR 2.5 AS 2.0 ! linenum: 3.000 targname: B20902+34 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F622W num_exp: 1 time_per_exp: 2400.00S s_to_n: 5 s_to_n_time: 18000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: POS TARG +0.460, -0.138; req_2: SEQ 3.0-3.5 NO GAP comment_1: ADJUST EXP TIME +INFINITY/-10% comment_2: TO FIT IN AN ALIGNMENT. comment_3: THIRD POS TO AVOID BLEMISHES ! linenum: 3.500 targname: B20902+34 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F622W num_exp: 2 time_per_exp: 2400.00S s_to_n: 5 s_to_n_time: 18000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: SAME POS FOR 3.5 AS 3.0 ! ! end of exposure logsheet ! No scan data records found