! $Id: 5379,v 12.1 1995/02/09 14:51:16 pepsa Exp $ coverpage: title_1: PROBING THE LY ALPHA FOREST AT 0.5 < Z < 1.6 USING FLARING QUASARS title_2: & BL LACS sci_cat: QUASARS & AGN sci_subcat: QUASAR ABSORPTION proposal_for: GO pi_fname: JOHN pi_lname: STOCKE pi_inst: 1762 pi_country: USA pi_phone: (303) 492-1521 hours_pri: 7.81 num_pri: 7 fos: Y off_fname: LAURENCE off_lname: NELSON off_title: DIRECTOR off_inst: 1762 off_addr_1: OFFICE OF CONTRACTS AND GRANTS off_addr_2: CAMPUS BOX B-19 off_city: BOULDER off_state: CO off_zip: 80309 off_country: USA off_phone: (303) 492-6221 ! end of coverpage abstract: line_1: We propose spectroscopic observations of flaring quasars and BL Lacs with line_2: the FOS + high resolution gratings to study the line density and clus- line_3: tering of Ly alpha only lines in the hitherto inaccessible redshift range line_4: 0.5 < z < 1.6. The purpose of these observations is to determine if line_5: continuity exists between the Ly alpha "forest" at Z > 2 and the local line_6: Ly alpha clouds recently discovered by HST. If continuity can be line_7: established, then detailed observations of the "local" clouds can be line_8: applied to the high-z clouds as well. Current and planned HST observa- line_9: tions do not address the Ly alpha forest in this redshift range because line_10: high-z QSOs are generally not bright enough to obtain spectra at high line_11: enough SNR to detect sufficient Ly alpha absorptions to conduct a line_12: statistical study. The virtue of our 6 targets is that while they are line_13: generally quiescent at V = 16-18, they occasionally flare to V < 15 line_14: for periods of several months making high SNR HST/FOS 1A resolution line_15: spectra (G190H and G270H) possible in a few ksecs. Past observations line_16: suggest that normal scheduling of these targets will be sufficient to line_17: observe them with HST in their Flaring state. Each of these proposed line_18: targets is being intensively monitored using several small aperture line_19: ground-based telescopes with CCD detectors so that a flare can be line_20: detected and HST observations scheduled when the source is bright. ! ! end of abstract general_form_proposers: lname: STOCKE fname: JOHN inst: 1762 country: USA ! lname: BURKS fname: GEOFFREY inst: 1762 country: USA ! lname: BLADES fname: J. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: BURNS fname: JACK inst: NEW MEXICO STATE UNIVERSITY country: USA ! lname: MCNAMARA fname: BERNARD inst: NEW MEXICO STATE UNIVERSITY country: USA ! lname: NEELY fname: WILLIAM inst: NF/OBSERVATORY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will obtain high SNR spectra of bright BL Lacs and quasars when they flare line_2: to V < 15 for the purpose of detecting large numbers of Ly alpha only line_3: absorption clouds at 0.5 < z < 1.6. FOS spectra will be obtained through the line_4: 1/4 x 2 arcsec slits using gratings G190H and G270H. Ly alpha only and Ly line_5: alpha + metal absorption lines will be identified in a manner similar to that line_6: described in Schneider et al (1992). At an observed equivalent width limit of line_7: ~100mA (and thus a rest equivalent width limit of ~75 mA since the G270H line_8: will give slightly lower observed limits) we expect a Ly alpha line density line_9: of 40-80 per unit redshift in each of our objects observed (Bahcall et al, line_10: 1992; Hunstead 1988) so that a minimum of 2-3 objects will need to be line_11: observed before good statistics on line densities can be determined. line_12: Given the flaring history of these objects, we expect to observe 2 of them line_13: during the two year period requested for this project. If successful, we will line_14: re-propose in a subsequent cycle to observe more flaring targets of this type. ! question: 4 section: 1 line_1: HST is clearly needed for this project because for the range of redshifts of line_2: the Ly alpha lines we intend to study, the wavelengths fall in the range line_3: 1800-3100A. Although IUE spectra are available for a few of these, the line_4: minimum equivalent widths of the low dispersion IUE spectra are ~ 1A; even if line_5: these quasars were observed for full shifts when they were at their absolute line_6: brightest ever observed, a minimum equivalent width of >500 mA would be line_7: obtained in a full-shift US1 with low particle background. Given the line_8: magnitude of the targets and the weakness of the Ly alpha absorption lines, line_9: this is clearly an HST project. line_10: The exposure times listed for each of these targets assumes an optical line_11: magnitude of V = 15 (excepting 0735+178 for which V = 14.5 is assumed) and a line_12: normal quasar spectrum (i.e. nearly a power law with spectral index of -0.5 line_13: or a (B-V)=+0.3). Using the standard DQE data from the FOS handbook checked line_14: by scaling to the results obtained by the Key Project team (Bahcall et al, line_15: 1992; Schneider et al, 1992), we have estimated the exposure times necessary line_16: to obtain 4.5 sigma observed equivalent width limit of 100 mA at 1800A and line_17: 150 mA at 3200A; this yields rest frame equivalent width limits of ~ 75mA line_18: across the entire spectral range observed. These exposure times are 3000 and line_19: 6000 secs for the G270H and G190H gratings through the 1/4 x 2 arcsec slit line_20: respectively. These are "worst case" numbers in that if our photometric line_21: monitoring and IUE "quick look" spectra show the source to be brighter than line_22: 15th, the equivalent width limits will be lower. ! question: 4 section: 2 line_1: Exceptions to this general rule are noted below: line_2: 1. PKS 0215+015: This source will not be observed with the G190H because line_3: there is a Ly limit system at 2400A observed by the IUE. line_4: 2. 0735+178: This source will also be observed with the G130H grating if it line_5: flares to V < 14.5 due to the high interest in its Ly limit system at z = 0.424 line_6: as presented in the cycle 3 Linsky et al proposal. This is the BL Lac in line_7: our sample which flares to the brightest apparent magnitude and can in line_8: principle yield the highest quality Ly alpha forest information of any line_9: extragalactic source excepting 3C273 and PKS 2155-304, both of which have line_10: already been oberved with HST and both of which are at substantially lower line_11: redshifts. The G130H exposure is timed to yield ~ 150mA rest equivalent line_12: width limits at wavelengths longer than 1300A where the strong Ly limit line_13: system occurs. By assuming V = 14.0 the G130H exposure time is 7200 secs. ! question: 5 section: 1 line_1: In order for these observations to be successful, the FOS spectra should be line_2: obtained < 2 months after STScI is notified that we have detected a flare. line_3: This requested response time is based upon the historical flaring activity of line_4: these sources (e.g. Pollock et al, 1988). Since we will continue to monitor line_5: these sources intensely with groundbased telescopes and with IUE once a flare line_6: has commenced, a slightly longer leadtime can be tolerated if the source line_7: persists in its bright state. Because weeks rather than days of response time is line_8: required for success of these observations, this is NOT a target of opportunity line_9: proposal -- normal scheduling can accommodate to the flaring timescales of these line_10: quasars and BL Lacs to ensure a successful observation. line_11: Based upon the historical flaring history of these sources, we expect to line_12: actually observe 2 of our 6 targets in the two year time fame of this proposal. ! question: 6 section: 1 line_1: none ! ! question: 8 section: 1 line_1: The necessity for ground-based support in this HST proposal is obvious; our line_2: photometric monitoring is essential to the success of this proposal. Due to line_3: its essential nature we will request an amount of funding each year (~ $30K) line_4: in "preparatory" funds to support this continuing effort. The ground-based line_5: monitoring also supports the approved cycle 1 HST target of opportunity line_6: observations proposed by Blades et al (P2638; "The near-UV spectrum of line_7: 0215+015"). This proposal is not overlapping with P2638 because those line_8: observations involve GHRS spectra of two very strong Ly alpha absoprtion line_9: systems discovered by Blades et al (1985) in the IUE LWP spectrum of line_10: 0215+015 the last time it flared. line_11: Finally, we again remark that several of our targets (e.g. 0215+015 is line_12: on the Key Project list) have already been accepted for observation with the line_13: FOS in proposals granted to the GTOs or to the Key Project team. However, line_14: without photometric monitoring it is most likely that these observations will line_15: find the source in its faint state so that none of the scientific goals line_16: described herein can be accomplished. We reiterate that if the scheduled line_17: observations happen to be made by chance when the source is flaring to V < 15, line_18: then we will withdraw this source from our proposal. line_19: Ground-based 1A resolution spectra will be obtained when the source line_20: is flaring to supplement the HST/FOS observations. These spectra are line_21: required to identify the metal line systems detected by Ly alpha in the UV. ! question: 9 section: 1 line_1: P2717 ("Probing the Voids") -- CYCLE 1: Stocke and Shull (6.7 hours FOS) line_2: was directed at searches for QSO metal absorption lines in voids. P2717 is line_3: not related to the current proposal. line_4: P3584 ("Probing the Voids II") -- CYCLE 2: Stocke and Shull (31 hours GHRS) line_5: is unrelated to this proposal; it is a search for Ly-alpha lines towards line_6: 4 QSOs behind galaxy voids. line_7: From our FOS observations of two AGNs during Cycle 1, we have obtained results line_8: in three areas. First, we discovered intrinsic absorption in PG 1351+64, with line_9: 3 components resolvable; this object appears to be an example of what we have line_10: called a "BAL Seyfert" which may be related to BAL QSOs. Second, we discovered line_11: Mg II satellite emission lines (displaced +/- 4000 km/s) in PG 1351+64 and line_12: perhaps also in Ton 951 that may result from the interaction of BAL outflows line_13: with the broad-line or narrow-line regions of the host galaxy. Third, we line_14: combined our data on these 2 AGNs with that of 4 other AGNs to study UV line_15: resonance absorption lines in the Galactic halo. Special attention was paid to line_16: the C IV/C II and Si IV/Si II ratios of the six lines of sight. The strong line_17: absorption in "high ions" toward 3C 273 may be more consistent with a nearby line_18: supernova remnant than with a hot halo. Measurements of detections and/or line_19: limits on absorption lines in voids is now in progress. ! question: 9 section: 2 line_1: "PG 1351+64: An Intrinsic Absorber at Low Redshift", Granados, A., Sachs, E., line_2: Shull, J. M., & Stocke, J. T., ApJ, to be submitted (June 1993). line_3: "PG 1351+64: An Intrinsic Absorber at Low Redshift", Granados, A., Sachs, E., line_4: Shull, J. M., and Stocke, J. T., in The Evolution and Environment of Galaxies, line_5: eds. D. Hollenbach, J. M. Shull, & H. A. Thronson, proc. Tetons III Conf. line_6: (July 1992). line_7: "A UV Study through the Complete Galactic Halo by the Analysis of HST-FOS line_8: Spectra of QSOs and AGNs", Burks, G. S., Bartko, F., Shull, J. M., line_9: Stocke, J. T., Sachs, E., Burbidge, E. M., Cohen, R., Junkkarinen, V., line_10: Harms, R., & Massa, D., BAAS, 24, 763 (AAS Abstract). line_11: "A UV Study through the Complete Galactic Halo by the Analysis of HST-FOS line_12: Spectra of QSOs and AGNs", Burks, G. S., Bartko, F., Shull, J. M., line_13: Stocke, J. T., Sachs, E., Burbidge, E. M., Cohen, R., Junkkarinen, V., line_14: Harms, R., & Massa, D., ApJ, submitted (April 1993). ! question: 10 section: 1 line_1: The Center for Astrophysics and Space Astronomy (CASA) at the University of line_2: Colorado operates computer facilities based on VAX mainframes operating with line_3: VMS, and on SUN and SPARC2 workstations operating with UNIX. For the data line_4: analysis of GHRS and FOS spectra, we will use the SUN/SPARC2 workstations, line_5: which run IRAF in a UNIX environment. Ground-based observations in support of line_6: this research also will utilize the SUN for data reductions. These computers line_7: are already in place, and NASA/HST support funds are sought to assist in ! !end of general form text general_form_address: lname: STOCKE fname: JOHN category: PI inst: 1762 addr_1: CAMPUS BOX 389 city: BOULDER state: CO zip: 803020389 country: USA phone: (303) 492-1521 telex: (SPAN) HYADES::STOCKE ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PKS0215+015 descr_1: E, 316, H, 519 pos_1: RA = 2H 17M 48.945S +/- 0.1S, pos_2: DEC = +1D 44' 49.58" +/- 0.33" equinox: 2000.0 pm_or_par: N rv_or_z: Z=1.75 fluxnum_1: 1 fluxval_1: V=15.0 fluxnum_2: 2 fluxval_2: B-V=0.3 ! targnum: 3 name_1: 0735+178 descr_1: E, 316, H, 519 pos_1: RA = 7H 38M 07.37S +/- 0.1S, pos_2: DEC = +17D 42' 18.7" +/- 0.33" equinox: 2000.0 pm_or_par: N rv_or_z: Z = 0.42 fluxnum_1: 1 fluxval_1: V=15.0 fluxnum_2: 2 fluxval_2: B-V=0.3 ! targnum: 4 name_1: 0846+513 descr_1: E, 316, H, descr_2: 519 pos_1: RA = 8H 49M 58.03S +/- 0.1S, pos_2: DEC = +51D 8' 29.0" +/- 0.5", pos_3: PLATE-ID=021E equinox: 2000.0 pm_or_par: N rv_or_z: Z = 1.86 comment_1: OBSERVE ALSO WITH FOS/BL fluxnum_1: 1 fluxval_1: V=15.0 fluxnum_2: 2 fluxval_2: B-V=0.3 ! targnum: 5 name_1: B21308+326 descr_1: E, 316, H, 519 pos_1: RA = 13H 10M 28.683S +/- 0.1S, pos_2: DEC = +32D 20' 43.35" +/- 0.33" equinox: 2000.0 pm_or_par: N rv_or_z: Z = 2.09 fluxnum_1: 1 fluxval_1: V=15.0 fluxnum_2: 2 fluxval_2: B-V=0.3 ! targnum: 6 name_1: 3C446 descr_1: E, 316, H, descr_2: 519 pos_1: RA = 22H 25M 47.031S +/- 0.1S, pos_2: DEC = -4D 57' 1.4" +/- 0.5", pos_3: PLATE-ID=02O6 equinox: 2000.0 pm_or_par: N rv_or_z: Z = 1.40 fluxnum_1: 1 fluxval_1: V=15.0 fluxnum_2: 2 fluxval_2: B-V=0.3 ! targnum: 7 name_1: 3C279 descr_1: E, 313, H, descr_2: 519 pos_1: RA = 12H 56M 11.15S +/- 0.1S, pos_2: DEC = -05D 47' 21.7" +/- 0.5", pos_3: PLATE-ID=024R equinox: 2000.0 pm_or_par: N rv_or_z: Z = 0.538 fluxnum_1: 1 fluxval_1: V=15.0 fluxnum_2: 2 fluxval_2: B-V=0.3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 6.000 targname: 0735+178 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 6.5; req_2: CYCLE 4 / 6-31; req_3: SELECT 4 OF 6-8.5 OR req_4: 15-17 OR 18-19 OR 20-22 OR req_5: 23-25 OR 26-28 OR 29-31 ! linenum: 6.500 targname: 0735+178 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=.172 param_2: SEARCH-SIZE-X=5 param_3: SEARCH-SIZE-Y=5 param_4: SCAN-STEP-Y=.172 req_1: ONBOARD ACQ FOR 7 - 8.5; ! linenum: 7.000 targname: 0735+178 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 1980S fluxnum_1: 1 priority: 1 ! linenum: 8.000 targname: 0735+178 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G270H wavelength: 2230-3200 num_exp: 1 time_per_exp: 1020S fluxnum_1: 1 priority: 1 ! linenum: 8.500 targname: 0735+178 config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G130H wavelength: 1150-1600 num_exp: 3 time_per_exp: 2295S fluxnum_1: 1 priority: 1 ! linenum: 15.000 targname: 3C446 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 15.5; comment_1: SELECT IF TARGET FLARING ! linenum: 15.500 targname: 3C446 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=.172 param_2: SEARCH-SIZE-X=5 param_3: SEARCH-SIZE-Y=5 param_4: SCAN-STEP-Y=.172 req_1: ONBOARD ACQ FOR 16, 17; ! linenum: 16.000 targname: 3C446 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 1980S fluxnum_1: 1 priority: 1 ! linenum: 17.000 targname: 3C446 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G270H wavelength: 2230-3200 num_exp: 1 time_per_exp: 1020S fluxnum_1: 1 priority: 1 ! linenum: 18.000 targname: PKS0215+015 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 18.5 comment_1: SELECT IF TARGET FLARING ! linenum: 18.500 targname: PKS0215+015 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=.172 param_2: SEARCH-SIZE-X=5 param_3: SEARCH-SIZE-Y=5 param_4: SCAN-STEP-Y=.172 req_1: ONBOARD ACQ FOR 19; ! linenum: 19.000 targname: PKS0215+015 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G270H wavelength: 2230-3200 num_exp: 1 time_per_exp: 1800S fluxnum_1: 1 priority: 1 ! linenum: 20.000 targname: 0846+513 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 20.5; comment_1: SELECT IF TARGET FLARING ! linenum: 20.500 targname: 0846+513 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=.172 param_2: SEARCH-SIZE-X=5 param_3: SEARCH-SIZE-Y=5 param_4: SCAN-STEP-Y=.172 req_1: ONBOARD ACQ FOR 21, 22; ! linenum: 21.000 targname: 0846+513 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 1980S fluxnum_1: 1 priority: 1 ! linenum: 22.000 targname: 0846+513 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G270H wavelength: 2230-3200 num_exp: 1 time_per_exp: 1020S fluxnum_1: 1 priority: 1 ! linenum: 23.000 targname: B21308+326 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 23.5; comment_1: SELECT IF TARGET FLARING ! linenum: 23.500 targname: B21308+326 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=.172 param_2: SEARCH-SIZE-X=5 param_3: SEARCH-SIZE-Y=5 param_4: SCAN-STEP-Y=.172 req_1: ONBOARD ACQ FOR 24, 25 ! linenum: 24.000 targname: B21308+326 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 1980S fluxnum_1: 1 priority: 1 ! linenum: 25.000 targname: B21308+326 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G270H wavelength: 2230-3200 num_exp: 1 time_per_exp: 1020S fluxnum_1: 1 priority: 1 ! linenum: 26.000 targname: 3C279 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 26.5; comment_1: SELECT IF TARGET FLARING ! linenum: 26.500 targname: 3C279 config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=.172 param_2: SEARCH-SIZE-X=5 param_3: SEARCH-SIZE-Y=5 param_4: SCAN-STEP-Y=.172 req_1: ONBOARD ACQ FOR 27-28 ! linenum: 27.000 targname: 3C279 config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G130H wavelength: 1150-1600 num_exp: 3 time_per_exp: 2285S fluxnum_1: 1 priority: 1 linenum: 28.000 targname: 3C279 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 1980S fluxnum_1: 1 priority: 1 linenum: 29.000 targname: 3C279 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 29.5; comment_1: SELECT IF TARGET FLARING ! linenum: 29.500 targname: 3C279 config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=.172 param_2: SEARCH-SIZE-X=5 param_3: SEARCH-SIZE-Y=5 param_4: SCAN-STEP-Y=.172 req_1: ONBOARD ACQ FOR 30-31 ! linenum: 30.000 targname: 3C279 config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G130H wavelength: 1150-1600 num_exp: 3 time_per_exp: 2285S fluxnum_1: 1 priority: 1 linenum: 31.000 targname: 3C279 config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 1980S fluxnum_1: 1 priority: 1 ! ! ! end of exposure logsheet ! No scan data records found