! File: 4341C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:22:31:14 coverpage: title_1: HIGH RESOLUTION OBSERVATIONS OF THE LOW REDSHIFT LY ALPHA title_2: FOREST:CYCLE3 MEDIUM sci_cat: QUASARS & AGN sci_subcat: QUASAR ABSORPTION proposal_for: GO pi_fname: VESA pi_mi: T pi_lname: JUNKKARINEN pi_inst: CENTER FOR ASTROPHYSICS & SPACE SCIENCES pi_country: USA pi_phone: 619-534-0735 hours_pri: 17.13 num_pri: 1 hrs: Y funds_length: 12 funds_date: OCT-93 off_fname: RICHARD off_mi: E off_lname: ATTIYEH off_title: DEAN, OGSR off_inst: 1560 off_addr_1: OFFICE OF GRADUATE STUDIES AND RESEARCH, 0003 off_addr_2: 9500 GILMAN DRIVE off_city: LA JOLLA off_state: CA off_zip: 920930003 off_country: USA off_phone: 619-534-6654 ! end of coverpage abstract: line_1: We propose high resolution UV spectroscopy of the bright low redshift QSO line_2: KUV18217+64 to study selected absorption systems in the low redshift Lyman line_3: ALPHA forest. Observations with the G160M grating and GHRS will be used to line_4: resolve the strong Lyman ALPHA and Lyman BETA absorption lines that have been line_5: detected in this QSO at z = 0.214 and z = 0.225. These observations will line_6: be used to determine the amount of structure within these absorption systems. line_7: If the lines do not have multiple components, then accurate values of the line_8: Doppler parameter will be determined and used to set upper limits to the line_9: temperature in these Ly ALPHA clouds. Ly ALPHA forest clouds are expected to line_10: evolve toward cooler temperatures at the present epoch so these observations line_11: could reveal some low temperature clouds. An understanding of the physics of line_12: Lyman ALPHA clouds is necessary in order to use observations of these clouds line_13: to probe physical conditions in the intergalactic medium over a wide range of line_14: redshift. ! ! end of abstract general_form_proposers: lname: JUNKKARINEN fname: VESA title: PI mi: T inst: CENTER FOR ASTROPHYSICS & SPACE SCIENCES country: USA ! lname: COHEN fname: ROSS mi: D inst: CENTER FOR ASTROPHYSICS & SPACE SCIENCES country: USA ! lname: BEAVER fname: EDWARD mi: A inst: CENTER FOR ASTROPHYSICS & SPACE SCIENCES country: USA ! lname: BURBIDGE fname: MARGARET inst: CENTER FOR ASTROPHYSICS & SPACE SCIENCES country: USA ! lname: SHAPIRO fname: PAUL mi: R inst: UNIVERSITY OF TEXAS country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will obtain two GHRS UV spectra of the QSO KUV18217+64 with the G160M line_2: (R=20000 nominal) grating and the Large Science Aperture. One spectrum line_3: will cover 1469 -- 1504 Angstroms (Ly alpha) and the other spectrum line_4: will cover 1236 -- 1272 Angstroms (Ly beta). The Ly alpha spectrum line_5: includes four known Ly alpha absorption lines (Bahcall et al. 1992). line_6: The integration times will be 5.3 hours and 6.6 hours, respectively, line_7: to provide S/N ratios of 12 at Ly alpha and 15 at Ly beta. The line_8: exposure times are predicted using the observed flux from the Bahcall line_9: et al. (1992) UV FOS spectrum of KUV18217+64. line_10: The exposures will be broken into approximately 5 minute segments to line_11: allow for shifting in wavelength to correct for geomagnetic and line_12: thermal drifts. Additionally, the 5 minute observations will be line_13: grouped into exposure logsheet lines approximately 80 minutes long. line_14: Each of these segments will be preceded by a SPYBAL and a wavelength line_15: lamp observation. The SPYBALs will correct for drifts perpendicular line_16: to the diode array and the wavelength lamps will allow us to correct line_17: for errors in the thermal and magnetic drift models, as well as errors line_18: in resetting the carrousel after the SPYBALs. The SPYBALs should line_19: occur close in time to the observations, but should NOT be placed line_20: between the wavelength lamp and the observations of the object. ! question: 4 section: 1 line_1: The Lyman lines of the low redshift Ly alpha forest can only be line_2: studied from space because they occur in the far UV. Observations that line_3: spectrally resolve these lines take long integration times with HST on line_4: the brightest QSOs so these observations can only be carried out with line_5: HST and GHRS at the present time. Previous HST GHRS observations at line_6: high resolution on 3C 273 can be analyzed to obtain Doppler parameter line_7: and column density estimates on weaker lines. But the redshift of 3C line_8: 273 is too low to measure Ly beta at high resolution for the observed line_9: Ly alpha lines and the spectrum of 3C 273 does not have any really line_10: strong isolated Ly alpha absorption lines. ! question: 4 section: 2 line_1: KUV18217+64 at V = 14.2 is the second brightest QSO after 3C 273 at z > line_2: 0.1. The redshift of KUV18217+64 is 0.297 so some Ly alpha clouds line_3: detected in absorption against KUV18217+64 can be studied in both Ly line_4: alpha and Ly beta. FOS observations by Bahcall et al. (1992) reveal line_5: strong absorption lines at z = 0.214 and 0.225 in both Ly alpha and Ly line_6: beta. Two observations are needed with the GHRS side 2 and the G160M line_7: grating to measure both lines. One spectrum centered at 1486 line_8: Angstroms will cover the Ly alpha absorption lines at z = 0.214, line_9: 0.225, 0.226, 0.228, while the other, centered at 1254 Angstroms will line_10: cover the corresponding Ly beta lines. line_11: Monte Carlo simulations using the line spread function published in line_12: the GHRS handbook for the large science aperture (LSA) were used to line_13: estimate the signal to noise ratio needed. Repeated chi-squared fits line_14: were used to accumulate statistics. A Doppler parameter accurate to line_15: better than +/- 10% is desirable for comparison with high redshift line_16: results (for example Carswell et al. 1992). For temperature line_17: comparisons, an error of 10% in Doppler parameter translates to about line_18: a 20% error in temperature. Accurate temperature estimates are needed line_19: because the models predict modest temperature decreases (factors of line_20: 1.5 or 2.) from redshift 2.0 to 0.2. The FOS observed equivalent width line_21: for the lambda 1489 line restricts the parameter space that must be line_22: searched if the lambda 1489 line consists of a single component Voigt line_23: profile. A S/N ratio of 12 per diode (6 per 1/4 step) is sufficient to ! question: 4 section: 3 line_1: measure (at 80% confidence) b values from the Ly alpha line at 1489 line_2: of 20.0 -1.5/+1.4 km/s and 30.0 -2.7/+1.4 km/s (determined from Monte line_3: Carlo runs of 200 spectra). At larger b values and lower column line_4: densities, the Ly beta line provides the better constraint. A S/N line_5: ratio of 15 per diode allows the b value to be determined to about +/- line_6: 4 km/s at b = 60 km/s. For even larger b values, either line provides line_7: an accurate b value. The observed Ly beta equivalent width of 0.53 line_8: Angstroms, suggests that either b = 20 km/s or b = 50 km/s for the z = line_9: 0.225 system given the observed Ly alpha with W_lambda = 0.95 line_10: Angstroms, but the one sigma uncertainty in the ratio of observed line_11: equivalent widths allows a wide range of b values: 15 < b < 60 km/s. line_12: The integration time calculation includes the following assumptions: line_13: KUV18217+64 has a flux of 3.5E-14 at 1500 and 1250 Angstroms (Bahcall et line_14: al. 1992), the GHRS side 2 G160M sensitivity is 4.30E11 at 1500 line_15: Angstroms and and 5.03E11 at 1250 Angstroms (GHRS handbook LSA line_16: aperture), and that the background is an average of 0.011 line_17: counts/second/diode with the standard burst rejection. Using the above line_18: assumptions, the countrate predicted is 0.0129 and 0.0151 line_19: (counts/second/diode) at 1500 and 1250 Angstroms respectively. The line_20: required integration time to reach S/N of 12 and 15 per diode is then line_21: 5.3 hours and 6.6 hours at 1500 and 1250 Angstroms respectively. ! question: 6 section: 1 line_1: Because of the large wavelength drifts which will occur over the line_2: course of the entire observation, periodic measurements of the line_3: wavelength scale are required in order to reconstruct the spectrum of line_4: this faint object. They are also required both to check on the line_5: accuracy of the carrousel repositioning after the SPYBALs and to line_6: correct for any errors in the model of thermal and magnetic drift. ! question: 7 section: 1 line_1: The data will be reduced and analyzed using existing software and line_2: computers at the PI's home institution. The data reduction will be line_3: done using existing software to remove background, correct detector line_4: sensitivity variations and flux the data. Computer programs have line_5: already been written for doing the chi-squared fitting using a line_6: numerical line spread function convolved with a Voigt profile. We will line_7: use the most accurate available lsf for the GHRS and can numerically line_8: investigate the additional uncertainty introduced by the approximate line_9: nature of the lsf. Monte Carlo simulations will be used to estimate line_10: the confidence level of the parameters determined from each fit. These line_11: programs have already been used to estimate the S/N required for line_12: accurate measurement of the Doppler parameter. line_13: The best estimate b values and temperature limits will be compared to line_14: the predictions of models for the Ly alpha forest at low redshift. line_15: Additional investigations using variations of the existing models or line_16: different sets of parameters, will be carried out as needed to analyze line_17: this data. ! question: 9 section: 1 line_1: Junkkarinen is a member of the FOS GTO team and has worked with GTO line_2: data, but he is not a Co-investigator. Some of the low resolution line_3: spectra obtained with the FOS are broadly pertinent to the nature of line_4: the low redshift Ly alpha forest. There is no direct relation to the line_5: goals of this project. Junkkarinen is a co-investigator on a program line_6: with Brian Espey as PI for archival studies of QSO emission lines. ! question: 9 section: 2 line_1: "Far Ultraviolet Spectroscopy of the QSO UM675 with the Faint Object line_2: Spectrograph on the Hubble Space Telescope," Beaver, E. A., Burbidge, line_3: E. M., Cohen, R. D., Junkkarinen, V. T., Lyons, R. W., Rosenblatt, E. line_4: I., Hartig, G. F., Margon, B. H., Davidsen, A. F., ApJ, 377, L1, 1991. line_7: "The Ultraviolet Absorption Spectrum of 3C 273,", Bahcall, J. N., line_8: Januzzi, B. T., Schneider, D. P., Hartig, G. F., Bohlin, R., line_9: Junkkarinen, V., ApJ, 377, L5, 1991. line_11: "The Lyman alpha Forest at Low Redshift: FOS Observations of the QSO line_12: PG 1211+143," Junkkarinen, V. T., Bartko, F., Beaver, E. A., Burbidge, line_13: E. M., Cohen, R. D., Lyons, R. W., Rosenblatt, E. I., Burks, G. S., line_14: Harms, R. J., and Henriksen, M., BAAS, 23, 1425, 1991. line_16: "Spectroscopy of QSOs with the Faint Object Spectrograph," Beaver, E. line_17: A., Burbdige, M., Cohen, R. D., Junkkarinen, V., Lyons, R., and line_18: Rosenblatt, E., Paper presented by M. Burbidge at the "Science with line_19: the Hubble Space Telescope" Conference, June 29 -- July 7, 1992, line_20: Sardinia, Italy. ! question: 9 section: 3 line_1: "HST-FOS and Ground--Based Observations of the Broad Absorption Line line_2: Quasar 0226-1024," Korista, K. T., Weymann, R. J., Morris, S. L., line_3: Kopko, M., Turnshek, D. A., Hartig, G. F., Foltz, C. B., Burbidge, E. line_4: M., and Junkkarinen, V. T., (to appear in December 20, 1992 ApJ). ! question: 10 section: 1 line_1: We intend to use existing facilities at our home institutions. We hope line_2: to pay a graduate student from UCSD to do some of the data analysis line_3: and numerical simulations that are needed for this project. Computing line_4: at UCSD will be done by sharing resources with the FOS group and line_5: through a recharge-type arrangement with CASS. ! !end of general form text general_form_address: lname: JUNKKARINEN fname: VESA mi: T category: PI inst: Center for Astrophysics & Space Sciences addr_1: CENTER FOR ASTROPHYSICS AND SPACE SCIENCES, 0111 addr_2: 9500 GILMAN DRIVE city: LA JOLLA state: CA zip: 920930111 country: USA phone: 619-534-0735 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: KUV18217+64 descr_1: E,313,H,515,519 pos_1: RA = 18H 21M 57.106S +/- 0.3", pos_2: DEC = 64D 20' 36.69" +/- 0.3", pos_3: PLATE-ID = 00T0 equinox: 2000 pm_or_par: NO rv_or_z: Z=0.297 fluxnum_1: 1 fluxval_1: V=14.1 +/- 0.5 fluxnum_2: 2 fluxval_2: F(1500)=3.5 +/- 0.5 E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: KUV18217+64 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 1 priority: 1 param_1: BRIGHT = RETURN, param_2: MAP = DEF, param_3: SEARCH-SIZE=3, param_4: LOCATE=YES req_1: ONBOARD ACQ FOR 1.1; req_2: SEQ 1.0-3.45; req_3: CYCLE 3/1.0-3.45; comment_1: USED 0.2 SEC STEP-TIMES. comment_2: IF THIS PROGRAM IS BROKEN INTO comment_3: PARTS, REPEAT LINES 1.0 AND 1.1 comment_4: AS NECESSARY. ! linenum: 1.100 targname: KUV18217+64 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 20.4S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 2.0-3.45 comment_1: USED 0.2 SEC STEP-TIMES. comment_2: THIS ACQ REFINES THE CENTERING comment_3: AFTER B-FIELD & THERMAL SHIFTS. ! linenum: 2.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1486 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 2.05 NO SLEW; req_3: SEQ 2.0-2.05 NO GAP; comment_1: THE Y-BAL. FOR 2.05 SHOULD BE DONE comment_2: PRIOR TO LINE 2.0. DO NOT INSERT A comment_3: SPYBAL AND MOVE CAROUSEL BETWEEN comment_4: LINES 2.0 AND 2.05. comment_5: SEQ IS TO OBTAIN A WAVELENGTH CAL; comment_6: W/O DRIFT ! linenum: 2.050 targname: KUV18217+64 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1486 num_exp: 15 time_per_exp: 317S s_to_n: 6.5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 2.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1486 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 2.15 NO SLEW; req_3: SEQ 2.1-2.15 NO GAP; comment_1: THE Y-BAL. FOR 2.15 SHOULD BE DONE comment_2: PRIOR TO LINE 2.1. DO NOT INSERT A comment_3: SPYBAL AND MOVE CAROUSEL BETWEEN comment_4: LINES 2.1 AND 2.15. comment_5: SEQ IS TO OBTAIN A WAVELENGTH CAL comment_6: W/O DRIFT ! linenum: 2.150 targname: KUV18217+64 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1486 num_exp: 15 time_per_exp: 317S s_to_n: 6.5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 2.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1486 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 2.25 NO SLEW; req_3: SEQ 2.20-2.25 NO GAP; comment_1: THE Y-BAL. FOR 2.25 SHOULD BE DONE comment_2: PRIOR TO LINE 2.20. DO NOT INSERT A comment_3: SPYBAL AND MOVE CAROUSEL BETWEEN comment_4: LINES 2.2 AND 2.25. comment_5: SEQ IS TO OBTAIN A WAVELENGTH CAL comment_6: W/O DRIFT. ! linenum: 2.250 targname: KUV18217+64 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1486 num_exp: 15 time_per_exp: 317S s_to_n: 6.5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 2.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1486 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 2.35 NO SLEW; req_3: SEQ 2.30-2.35 NO GAP; comment_1: THE Y-BAL. FOR 2.35 SHOULD BE DONE comment_2: PRIOR TO LINE 2.30. DO NOT INSERT A comment_3: SPYBAL AND MOVE CAROUSEL BETWEEN comment_4: LINES 2.30 AND 2.35. comment_5: SEQ IS TO OBTAIN A WAVELENGTH CAL comment_6: W/O DRIFT ! linenum: 2.350 targname: KUV18217+64 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1486 num_exp: 15 time_per_exp: 317S s_to_n: 6.5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 3.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1254 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 3.05 NO SLEW; req_3: SEQ 3.0-3.05 NO GAP; comment_1: SEQ 3.0-3.05 TO OBTAIN A WAVELENGTH comment_2: CALIB. W/O DRIFT. THE Y-BAL FOR comment_3: 3.05 SHOULD BE DONE FROM A comment_4: WAVELENGTH LAMP BEFORE LINE 3.0. comment_5: DO NOT INSERT A SPYBAL AND MOVE comment_6: CAROUSEL BETWEEN LINES 3.0 AND 3.05. ! linenum: 3.050 targname: KUV18217+64 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1254 num_exp: 15 time_per_exp: 318S s_to_n: 7 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 3.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1254 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 3.15 NO SLEW; req_3: SEQ 3.1-3.15 NO GAP; comment_1: SEQ 3.1-3.15 TO OBTAIN A WAVELENGTH comment_2: CALIB. W/O DRIFT. THE Y-BAL FOR comment_3: 3.15 SHOULD BE DONE FROM A comment_4: WAVELENGTH LAMP BEFORE LINE 3.1. comment_5: DO NOT INSERT A SPYBAL AND MOVE comment_6: CAROUSEL BETWEEN LINES 3.1 AND 3.15. ! linenum: 3.150 targname: KUV18217+64 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1254 num_exp: 15 time_per_exp: 318S s_to_n: 7 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 3.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1254 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 3.25 NO SLEW; req_3: SEQ 3.2-3.25 NO GAP; comment_1: SEQ 3.2-3.25 TO OBTAIN A WAVELENGTH comment_2: CALIB. W/O DRIFT. THE Y-BAL FOR comment_3: 3.25 SHOULD BE DONE FROM A comment_4: WAVELENGTH LAMP BEFORE LINE 3.2. comment_5: DO NOT INSERT A SPYBAL AND MOVE comment_6: CAROUSEL BETWEEN LINES 3.2 AND 3.25. ! linenum: 3.250 targname: KUV18217+64 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1254 num_exp: 15 time_per_exp: 318S s_to_n: 7 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 3.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1254 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 3.35 NO SLEW; req_3: SEQ 3.3-3.35 NO GAP; comment_1: SEQ 3.3-3.35 TO OBTAIN A WAVELENGTH comment_2: CALIB. W/O DRIFT. THE Y-BAL FOR comment_3: 3.35 SHOULD BE DONE FROM A comment_4: WAVELENGTH LAMP BEFORE LINE 3.3. comment_5: DO NOT INSERT A SPYBAL AND MOVE comment_6: CAROUSEL BETWEEN LINES 3.3 AND 3.35. ! linenum: 3.350 targname: KUV18217+64 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1254 num_exp: 15 time_per_exp: 318S s_to_n: 7 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 3.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1254 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 3.45 NO SLEW; req_3: SEQ 3.4-3.45 NO GAP; comment_1: SEQ 3.4-3.45 TO OBTAIN A WAVELENGTH comment_2: CALIB. W/O DRIFT. THE Y-BAL FOR comment_3: 3.45 SHOULD BE DONE FROM A comment_4: WAVELENGTH LAMP BEFORE LINE 3.4. comment_5: DO NOT INSERT A SPYBAL AND MOVE comment_6: CAROUSEL BETWEEN LINES 3.4 AND 3.45. ! linenum: 3.450 targname: KUV18217+64 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1254 num_exp: 15 time_per_exp: 318S s_to_n: 7 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! ! end of exposure logsheet ! No scan data records found