! Proposal 5947, submission 2 ! PI: Chris Impey ! Received Mon Feb 19 18:58:56 EST 1996 ! From: petry@as.arizona.edu ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5947,v 10.1 1996/04/08 13:54:37 pepsa Exp $ ! ! Refer to the HST Phase II Proposal Instructions to fill this out ! ! Anything after a "!" is ignored, and may be deleted ! ! All keywords with multiple entries are comma delimited except the ! Visit_Requirements and Special_Requirements keywords which can be ! delimited with carriage returns or semi-colons, but not commas ! ! For help call your Program Coordinator: Debra Wallace ! Phone: 410 338-4506 , E-mail: wallace@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Sat Dec 17 11:09:50 EST 1994 ! Proposal_Information Title: The Relationship Between Galaxies and Lyman-Alpha Absorbers at Low Redshift Proposal_Category: GO Scientific_Category: QSO Absorption Lines Cycle: 5 Investigators PI_name: Chris Impey PI_Institution: Steward Observatory CoI_Name: Catherine Petry CoI_Institution: Steward Observatory Contact: CoI_Name: Kathleen Flint CoI_Institution: Steward Observatory Contact: Abstract: The relationship between galaxies and low column density, metal poor quasar absorbers is still poorly understood. There is some evidence for two populations: strong Lyman-Alpha absorbers which are associated with luminous galaxies, and weak Lyman-Alpha absorbers that are uncorrelated with galaxies. Recent HST observations of the quasar pair, Q0107- 025 A,B, detect common Lyman-Alpha lines over a scale at least 500-750 h_50^-1 kpc, with an rms velocity difference of less than 100 km/s. This implies that Lyman-Alpha absorbers are larger and more quiescent than any current theoretical models predict. The physical properties of the absorbers can be most easily understood if they occupy low density, low velocity dispersion environments. In this respect, they are similar to low surface brightness galaxies, and they may represent a relatively unbiased tracer of the underlying mass distribution. We have selected 10 quasars in the Virgo region and beyond, where the 3-dimensional distribution of galaxies is extremely well mapped, and propose to observe them with GHRS to detect an estimated 40 Lyman-Alpha absorbers over the redshift range z = 0 to z = 0.1. There is no a priori selection in favor of quasars demonstrating a high density of absorbers. The results will be used to discriminate between different models of the clustering of the absorbers with respect to bright galaxies. Questions Observing_Description: Number of Lines: The proposed observations involve spectroscopy of 10 bright quasars with the GHRS using the Large Science Aperture and the G140L grating, giving a coverage of 1200-1480 Angstroms at a resolution of 0.57 Angstroms. For this wavelength range and resolution, GHRS is superior to FOS. This setup gives sensitivity to Lyman- Alpha lines over the redshift range z = 0 to z = 0.22, although the selection of lines below a redshift of 1000 km/s is difficult due to geocoronal Lyman-Alpha and the steep damping wings of Galactic Lyman-Alpha. Fortuitously, it also encompasses the short wavelength region where the COSTAR mirrors do not degrade the throughput of the GHRS. We adopted the following dependence for the density of Lyman-Alpha systems d^2N / (dz*dW) = (dN/dz)o / Wstar * (1+z)^Gamma * exp(-W/Wstar) and we adopt Gamma = 0.5, Wstar = 0.21 Angstroms, and (dN/dz)o = 17.0 from the maximum likelihood model of Bahcall et al. (1993). The addition of more recent data from the Quasar Key Project has not changed these numbers significantly (Weymann, private communication). The 4.5-sigma equivalent width limit is given by W_4.5-sigma = 9 * sqrt(Wline * d) / SNR where an unresolved line has Wline = 0.65 Angstroms, the width of a diode d = 0.57 Angstroms, and we assume unresolved lines (justified by the fact that Lyman-Alpha Doppler parameters are generally less than 100 km/s). In fact, we can usefully bin the data to 1 Angstrom resolution. Integration times are adjusted to give the expected number of Lyman-Alpha absorption lines (Nexp) to be greater than or equal to three over the range covered by ZCAT. Statistical Issues: The average value of Nexp per line of sight was set to yield about 40 Lyman- Alpha lines in the Virgo sample. The Poisson probability of detecting zero lines along a single line of sight is only 0.05, so on average we expect no more than one quasar spectrum to be lost from the analysis because it contains no Lyman-Alpha lines. A conservative detection threshold of 4.5-sigma was used. The line density will be low, and there are 500 resolution elements in the Digicon, so we are concerned with false detections of unresolved lines. Assuming normally distributed statistics, no lines at 4.5-sigma significance should be confused with noise fluctuations. We have originally selected targets according to the criterion Ngal >= (Nexp)^3, because the comparison between galaxies and absorbers involves the projection of the 3-dimensional galaxy distribution onto a 1-dimensional absorber redshift distribution. There are two objects that currently fall below this limit, however, we intend to supplement existing redshift catalogs with our own redshift survey, and greatly increase galaxy statistics for all objects. Finally, since most of the quasars do not have directly measured fluxes at 1300 Angstroms, there is the chance that an optically thick Lyman limit system will extinguish the UV continuum. This probability rises from about 20% in the integrated redshift range z = 0.5-1 to 50% in the redshift range z = 1-1.2 (Bahcall et al. 1993). Based on these numbers, there is less than a 50% chance of losing a single target to an unforeseen Lyman limit system. Bright Absorption Probes Object RA Dec z F(1300) SNR W_4.5s Nexp Ngal Orbits ----------- ---------- -------- ----- ---- ----- ---- ---- --- - PG 1211+143 12 11 44.9 14 19 53 0.085 6.55 63.98 0.09 4.76 207 2 Q 1214+1804 12 14 16.8 18 04 44 0.375 0.50 29.27 0.19 3.48 76 5 MARK 1320 12 16 34.9 -01 31 50 0.103 0.42 26.30 0.21 3.14 21 5 PG 1216+069 12 16 47.8 06 55 17 0.334 2.44 38.41 0.14 4.30 267 2 PKS 1217+02 12 17 38.3 02 20 21 0.240 0.59 27.81 0.20 3.32 57 4 Q 1228+1116 12 28 22.0 11 16 45 0.235 0.82 32.80 0.17 3.83 394 4 Q 1230+0947 12 30 53.6 09 47 55 0.420 3.72 47.43 0.12 4.89 302 2 Q 1245-0333 12 45 00.4 -03 33 47 0.379 1.95 43.21 0.13 4.64 20 3 PKS 1252+119 12 52 07.7 11 57 21 0.870 0.53 29.58 0.19 3.51 48 5 Q 1252+0200 12 52 46.4 02 00 27 0.345 3.55 46.34 0.12 4.83 28 2 Notes: F(1300) is in 1.0e-14 ergs/cm^2/s/Angstrom W_4.5s is in Angstroms Extrapolated UV flux using individual measured spectral index for all but PKS 1217+02 and Q 1214+1804 Target List: Targets were selected from the most current version of the Veron catalog (Veron-Cetty and Veron, "A Catalogue of Quasars and Active Galactic Nuclei", 6th ed., ESO Sci. Rep. 7 1993) to have Ngal > 27 within a cone of depth Delta-z = 0.1 (30,000 km/s) and half-angle 2 degrees There are two exceptions where Ngal > 20, and these quasars were chosen for their position in the southern extension of the Virgo region. Quasars are selected according to UV flux and redshift. Most are expected to have a 1300 Angstrom flux greater than 0.5e-14 erg/cm^2/s/A. Initially, the 1300 Angstrom flux was estimated by extrapolation from the V band flux (Lanzetta et al. 1991, Ap.J.Supp., 84, 109), using the average spectral index for the targets with published 1300 Angstrom spectral fluxes (Alpha = -0.71, S_Nu proportionate to Nu^Alpha). Because of the unreliability of the published V magnitudes and the large uncertainty in the average spectral index, we observed 8/10 targets spectrophotometrically to derive a spectral index for each object individually, and therefore estimating a more accurate 1300 Angstrom flux. Two targets were not observed spectrophotometrically, PKS 1217+02 and Q 1214+1804. PKS 1217+02 has a published UV spectrum (Lanzetta et al. 1991, ApJ Supp., 84, 109) which agrees with the estimated flux using the average spectral index. Q 1214+1804, which does not have a measured spectral index or a published UV spectrum, is an optically selected quasar and has a high probability of having a reliable extrapolated flux calculated from the average spectral index. The lower redshift bound is usually z = 0.1, although one object down to z = 0.08 has been included because the UV brightness offsets the increased amount of time required to detect 3 lines in a small redshift path length. The upper redshift bound is z = 0.9, to avoid the likelihood of Lyman limit absorption in quasars without previously measured UV fluxes. Since the quasars are faint, the most efficient strategy is to acquire the targets with the FOS and do a slew to the GHRS large science aperture. Time Justification: The range of integration times required to detect an average of 4 Lyman-Alpha lines varies from 60-170 minutes among the 10 targets, with an average of 110 minutes. To estimate the number of orbits required, we assumed overheads of 12 minutes for guide star acquisition, 6 minutes for guide star reaquisition, 11 minutes for each target acquisition, and 4 minutes per readout (assuming that multi-orbit integrations could be stored without readout). Where a multi-orbit exposure was required, the number of orbits chosen was that which resulted in Nexp greater than three. The 3 objects with number of orbits selected to Norbits = 1 were set to Norbits = 2, as this integral change in the number of orbits is the most efficient way to increase Nexp. The exposure time for 4 other objects was increased by one orbit, setting Nexp => 3.14 and the overall average at 4.07. No object has Norbits > 5. Two absorbers located near the southern Virgo extension have already been studied (Morris et al. 1993; Weymann et al. 1994, Ap.J., in press). The number of predicted absorbers at the Virgo redshift depends sensitively on assumptions about the population of low surface brightness galaxies in the Virgo cluster (Davies et al. 1987, Ast.Ap., 172, 500). The percentage of quasars with at least one Virgo absorber goes from 30% to 80% as the number of low surface brightness galaxies changes from 500 to 3000. Real_Time_Justification: The proposed observations can address the scientific issues raised in the proposal. Redshifts exist in ZCAT (z < 0.1) for the fields around the target quasars, and optical spectra exist with which to identify contaminating metal lines in the UV spectra. Additionally, we plan to carry out supplementary galaxy redshift surveys for all quasar fields, to sample the galaxy distribution more fully and to a higher redshift. Thus, while the average Nexp is 4 from z = 0 to z = 0.1, we will have an average Nexp of 9 for the entire accessible redshift range of Delta z = 0.22 per quasar. By Poisson statistics, we therefore anticipate a few spectra with about 12 Lyman-Alpha lines. For those fields, we will use the MX multi-object spectrograph on the Steward 90- inch telescope to conduct redshift surveys of additional galaxies down to V = 19, probing to a larger redshift than is readily available in ZCAT. The increased sampling of the 3- dimensional galaxy distribution will give a more sensitive measure of correlation with the larger number of absorbers. Calibration_Justification: None. Additional_Comments: Fixed_Targets Target_Number: 01 Target_Name: PG-1211+143 Description: Galaxy, QSO, Lyman Alpha Cloud, Ext-medium, Absorption Line System Position: RA = 12H 14M 17.68S +/- 0.1S, DEC = +14D 03' 12.3" +/- 0.5", plate-id=01TJ Equinox: 2000 RV_or_Z: Z = 0.085 Flux: V = 14.63 +/- 0.4, F(1300) = 6.55 +/- 0.7E-14 Target_Number: 02 Target_Name: Q-1214+1804 Description: Galaxy, QSO, Lyman Alpha Cloud, Ext-medium, Absorption Line System Position: RA = 12H 16M 49.1S +/- 0.1S, DEC = +17D 48' 4.4" +/- 0.5", plate-id=0590 Equinox: 2000 RV_or_Z: Z = 0.375 Flux: V = 16.7 +/- 0.4, F(1300) = 0.50 +/- 0.05E-14 Target_Number: 03 Target_Name: MARK-1320 Description: Galaxy, QSO, Lyman Alpha Cloud, Ext-medium, Absorption Line System Position: RA = 12H 19M 8.77S +/- 0.1S, DEC = -01D 48' 30.3" +/- 0.5", plate-id=00BB Equinox: 2000 RV_or_Z: Z = 0.103 Flux: V = 15. +/- 0.4, F(1300) = 0.42 +/- 0.04E-14 Target_Number: 04 Target_Name: PG-1216+069 Description: Galaxy, QSO, Lyman Alpha Cloud, Ext-medium, Absorption Line System Position: RA = 12H 19M 21.01S +/- 0.1S, DEC = +06D 38' 38" +/- 0.5", plate-id=01UQ Equinox: 2000 RV_or_Z: Z = 0.334 Flux: V = 15.75 +/- 0.4, F(1300) = 2.44 +/- 0.2E-14 Target_Number: 05 Target_Name: PKS-1217+02 Description: Galaxy, QSO, Lyman Alpha Cloud, Ext-medium, Absorption Line System Position: RA = 12H 20M 11.85S +/- 0.1S, DEC = +02D 03' 42.4" +/- 0.5", plate-id=00BB Equinox: 2000 RV_or_Z: Z = 0.240 Flux: V = 16.53 +/- 0.4, F(1300) = 0.59 +/- 0.06E-14 Target_Number: 06 Target_Name: Q-1228+1116 Description: Galaxy, QSO, Lyman Alpha Cloud, Ext-medium, Absorption Line System Position: RA = 12H 30M 54.13S +/- 0.1S, DEC = +11D 00' 11.2" +/- 0.5", plate-id=00IY Equinox: 2000 RV_or_Z: Z = 0.235 Flux: V = 17.10 +/- 0.4, F(1300) = 0.82 +/- 0.08E-14 Target_Number: 07 Target_Name: Q-1230+0947 Description: Galaxy, QSO, Lyman Alpha Cloud, Ext-medium, Absorption Line System Position: RA = 12H 33M 25.79S +/- 0.1S, DEC = +09D 31' 23.1" +/- 0.5", plate-id=00IY Equinox: 2000 RV_or_Z: Z = 0.420 Flux: V = 16.4 +/- 0.4, F(1300) = 3.72 +/- 0.4E-14 Target_Number: 08 Target_Name: Q-1245-0333 Description: Galaxy, QSO, Lyman Alpha Cloud, Ext-medium, Absorption Line System Position: RA = 12H 47M 35.030S +/- 0.1S, DEC = -03D 50' 8.60" +/- 0.5", plate-id=024P Equinox: 2000 RV_or_Z: Z = 0.379 Flux: V = 15.75 +/- 0.4, F(1300) = 1.95 +/- 0.2E-14 Target_Number: 09 Target_Name: PKS-1252+11 Description: Galaxy, QSO, Lyman Alpha Cloud, Ext-medium, Absorption Line System Position: RA = 12H 54M 38.24S +/- 0.1S, DEC = +11D 41' 6.1" +/- 0.5", plate-id=01TH Equinox: 2000 RV_or_Z: Z = 0.870 Flux: V = 16.64 +/- 0.4, F(1300) = 0.53 +/- 0.05E-14 Target_Number: 10 Target_Name: Q-1252+0200 Description: Galaxy, QSO, Lyman Alpha Cloud, Ext-medium, Absorption Line System Position: RA = 12H 55M 19.73S +/- 0.1S, DEC = +01D 44' 11.06" +/- 0.5", plate-id=00WW Equinox: 2000 RV_or_Z: Z = 0.345 Flux: V = 15.48 +/- 0.4, F(1300) = 3.55 +/- 0.4E-14 Visits Visit_Number: 1 Visit_Comments: FOS acquisition, HRS observation. Exposure_Number: 1 Target_Name: PG-1211+143 Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2.8S Special_Requirements: ONBOARD ACQ FOR 2 Exposure_Number: 2 Target_Name: PG-1211+143 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 2 Time_Per_Exposure: 1414.4S Special_Requirements: Exposure_Number: 3 Target_Name: PG-1211+143 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 1 Time_Per_Exposure: 1523.2S Special_Requirements: Comments: Expose for 2 orbits (62M); Visit_Number: 2 Visit_Comments: FOS acquisition, HRS observation. Exposure_Number: 1 Target_Name: Q-1214+1804 Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 26S Special_Requirements: ONBOARD ACQ FOR 2 Exposure_Number: 2 Target_Name: Q-1214+1804 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 7 Time_Per_Exposure: 1523.2S Special_Requirements: Exposure_Number: 3 Target_Name: Q-1214+1804 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 1 Time_Per_Exposure: 1958.4S Special_Requirements: Comments: Expose for 5 orbits (170M); Visit_Number: 3 Visit_Comments: FOS acquisition, HRS observation. Exposure_Number: 1 Target_Name: MARK-1320 Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 12.0S Special_Requirements: ONBOARD ACQ FOR 2 Exposure_Number: 2 Target_Name: MARK-1320 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 7 Time_Per_Exposure: 1523.2S Special_Requirements: Exposure_Number: 3 Target_Name: MARK-1320 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 1 Time_Per_Exposure: 1958.4S Special_Requirements: Comments: Expose for 5 orbit (165M); Visit_Number: 4 Visit_Comments: FOS acquisition, HRS observation. Exposure_Number: 1 Target_Name: PG-1216+069 Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 7.7S Special_Requirements: ONBOARD ACQ FOR 2 Exposure_Number: 2 Target_Name: PG-1216+069 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 2 Time_Per_Exposure: 1414.4S Special_Requirements: Exposure_Number: 3 Target_Name: PG-1216+069 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 1 Time_Per_Exposure: 1523.2S Special_Requirements: Comments: Expose for 2 orbits (60M); Visit_Number: 5 Visit_Comments: FOS acquisition, HRS observation. Exposure_Number: 1 Target_Name: PKS-1217+02 Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 22S Special_Requirements: ONBOARD ACQ FOR 2 Exposure_Number: 2 Target_Name: PKS-1217+02 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 6 Time_Per_Exposure: 1632.0S Special_Requirements: Comments: Expose for 4 orbits (130M); Visit_Number: 6 Visit_Comments: FOS acquisition, HRS observation. Exposure_Number: 1 Target_Name: Q-1228+1116 Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 25S Special_Requirements: ONBOARD ACQ FOR 2 Exposure_Number: 2 Target_Name: Q-1228+1116 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 6 Time_Per_Exposure: 1632.0S Comments: Expose for 4 orbits (130M); Visit_Number: 7 Visit_Comments: FOS acquisition, HRS observation. Exposure_Number: 1 Target_Name: Q-1230+0947 Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 8.3S Special_Requirements: ONBOARD ACQ FOR 2 Exposure_Number: 2 Target_Name: Q-1230+0947 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 2 Time_Per_Exposure: 1414.4S Special_Requirements: Exposure_Number: 3 Target_Name: Q-1230+0947 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 1 Time_Per_Exposure: 1523.2S Special_Requirements: Comments: Expose for 2 orbits (60M); Visit_Number: 8 Visit_Comments: FOS acquisition, HRS observation. Exposure_Number: 1 Target_Name: Q-1245-0333 Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 8.6S Special_Requirements: ONBOARD ACQ FOR 2 Exposure_Number: 2 Target_Name: Q-1245-0333 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 4 Time_Per_Exposure: 1740.8S Special_Requirements: Comments: Expose for 3 orbits (95M); Visit_Number: 9 Visit_Comments: FOS acquisition, HRS observation. Exposure_Number: 1 Target_Name: PKS-1252+11 Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 25S Special_Requirements: ONBOARD ACQ FOR 2 Exposure_Number: 2 Target_Name: PKS-1252+11 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 7 Time_Per_Exposure: 1523.2S Special_Requirements: Exposure_Number: 3 Target_Name: PKS-1252+11 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 1 Time_Per_Exposure: 1958.4S Special_Requirements: Comments: Expose for 5 orbits (165M); Visit_Number: 10 Visit_Comments: FOS acquisition, HRS observation. Exposure_Number: 1 Target_Name: Q-1252+0200 Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 5.6S Special_Requirements: ONBOARD ACQ FOR 2 Exposure_Number: 2 Target_Name: Q-1252+0200 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 2 Time_Per_Exposure: 1414.4S Special_Requirements: Exposure_Number: 3 Target_Name: Q-1252+0200 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1200-1480 Optional_Parameters: FP-SPLIT=STD; STEP-PATT=DEF Number_of_Iterations: 1 Time_Per_Exposure: 1523.2S Special_Requirements: Comments: Expose for 2 orbits (60M); Data_Distribution ! Defaults indicated; change if desired Medium: 8MM ! 8MM or 6250BPI or 1600BPI Blocking_Factor: 10 ! 10 or 1 ! Only astronomers with very old 9- ! track tape drives should consider ! a blocking factor of 1 Ship_To: PI_Address ! STSCI or PI_Address or ! PI Address from Phase I is: ! University of Arizona ! Tucson, AZ 85721 ! ! Ship_Via: UPS ! UPS (2-day) or OVERNIGHT ! Overnight shipping done at PI expense Recipient_Email: ! Needed if Ship_To: is not PI_Address !