! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! Id: 6100 Foltz ! ! For help call your Program Coordinator: Max Mutchler ! Phone: 410 338-1321 , E-mail: mutchler@stsci.edu Proposal_Information Title: Measuring the Characteristic Size of Lyman-Alpha Forest Clouds Proposal_Category: GO Scientific_Category: Quasars Cycle: 5 Investigators PI_name: Craig Foltz PI_Institution: Multiple Mirror Telescope Observatory CoI_Name: Chris Impey CoI_Institution: Steward Observatory CoI_Name: Nadine Dinshaw CoI_Institution: Steward Observatory Contact: Y CoI_Name: Ray Weymann CoI_Institution: Observatories of the Carnegie Institution of Washington CoI_Name: Simon Morris CoI_Institution: Dominion Astrophysical Observatory Abstract: ! Free format text (please update) We are obtaining FOS UV spectra (GO Program 5320) of three pairs of quasars with projected separations less than two arcminutes in order to constrain the sizes of Lyman-Alpha forest clouds. We anticipated that these observations would yield improved upper limits of ~ 100 kpc and so were surprised when the spectra of the first pair, Q0107-025 A,B (z = 0.956, 0.952, separation 1.44 arcmin), showed a large number of absorption lines common to both spectra. Assuming that these are Lyman-Alpha forest lines, the directly-measured lower limit on the sizes of the clouds at 0.32 <= z <= 0.90 is between 300 and 450 kpc (H_0=80, q_0=0.5). This is an order of magnitude larger than the best published lower limit. Furthermore, the rms velocity difference between the absorption lines along the two lines of sight is only about 100 km/sec. These results challenge all current theoretical models for the absorbers. Perhaps even more exciting is the fact the there is a third bright quasar, LBQS 0107-0232 (z=0.728, B_J=18.4), lying a few arcminutes away from the pair (separations 2.00 and 2.93 arcmin from Q0107-025 A,B), which will allow us to sample scales from 300 kpc to nearly 1 Mpc. We are requesting time to make FOS observations of these three quasars in order to: (1) extend the wavelength coverage of the observations of Q0107-025A,B to contain the Lyman alpha emission line and (2) obtain spectra of the Lyman-Alpha forest in LBQS 0107-0232. Questions ! Free format text (please update) Observing_Description: Spectroscopic observations of the three quasars fall into two categories: First, FOS/RD observations of LBQS 0107-0232 with G190H. The difference in B_J magnitude between Q0107-0232 and Q0107-025A is well-known from the LBQS plates to be 0.3 +/- 0.1 mag (barring variability). The exposure time was then calculated from the S/N realized in the GO 5320 observations of Q0107-025A, using this magnitude difference and assuming that both quasars have the same spectral slope. The latter assumption is more-or-less consistent with the optical data; if anything, Q0107-0232 is somewhat bluer than Q0107-025A. Our calculations indicate that 420 minutes of integration (11 orbits) will give S/N approximately equal to that of the Q0107-025A,B spectra obtained in GO 5320. The predicted count rates are a factor of 15 above the dark rate, which we have therefore assumed to be negligible in estimating the exposure time. Second, FOS/RD observations of all Q0107-025 A,B will be taken with G270H to extend the wavelength coverage to contain the Lyman alpha emission lines in each quasar. This will also complete our spectral coverage on these two objects from 1200 to 5500 Angstrom. Count rates for these observations were estimated from Figure 1.2.3 in the FOS Manual by extrapolating the GO program 5320 fluxes to longer wavelength (the spectra are essentially flat in F_Lambda). In one orbit we would expect to achieve a S/N of about 16 (per diode) at the short wavelength end of the spectrum of Q0107-025A (the fainter of the pair), inadequate for our purposes. In two orbits we will realize a S/N greater than 25 (per diode) at all wavelengths in the range 2200 - 3100 Angstrom. Therefore, we will use two orbits on each of the two quasars Q0107-025A,B for these data. We are very concerned about the accuracy of the wavelength calibration since it limits the accuracy of measurements of velocity differences between the three lines of sight. We therefore specify that a wavelength calibration exposure be taken upon each visit to a target and after a grating change. Furthermore, we request that the same guide star be used for both of the G270H observations. Spectroscopic observations covering the range from 3150 to 5500 Angstrom at a resolution of 1 Angstrom have been collected at the Multiple Mirror Telescope. These will overlap the G270H spectra of Q0107-025 A&B at their blue ends and extend to longward of the Mg II Lambda2798 emission line, thereby completing the coverage from shortward of Lyman Alpha emission to longward of Mg II. Coupled with the G270H spectra, these should allow us to identify any metal-line absorption systems which could have members which are mis-identified as Lyman Alpha forest lines. More importantly, the G270H data will allow us to identify absorption lines in the Lyman alpha emission line, which could be effected by the ionizing flux from the quasars (the proximity effect). Real_Time_Justification: Calibration_Justification: The success of this proposal relies on whether the absorption features in one quasar can be unambiguously identified as common (or not) to those in the other quasar in the pair. This demands accurate zero-point calibration of the wavelength scale. According to Papers I and II of the HST Quasar Absorption Line Key Project, the rms scatter in the zero point is about 0.5 Angstrom (60-80 km/sec) in the G190H and G270H gratings. The offsets can be determined from the Galactic absorption lines, however in calibrating the G190H spectra only the AlII 1670 line is suitable and is not always well detected. Therefore, one wavelength calibration frame following an exposure of LBQS 0107-0232 with the G190H is requested. We will not need a calibration frame for every exposure because the relative zero-point shifts between exposures of a given quasar can be calculated by cross-correlating the individual exposures of the same quasar. Note that the GO 5320 observations achieved an uncertainty in the difference in wavelengths between the members of a common pair of about 40 km/sec because the observations of the two quasars used the same guide star, thereby minimizing the uncertainty in the relative positioning of the two quasars in the spectrograph aperture. We request that the same procedure be used for the G270H observations of Q0107-025 A,B, i.e. the same guide stars should be used for both observations. Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: Q0107-025A Alternate_Names: PB8553 Description: Galaxy, Lyman Alpha Cloud Position: RA = 01H 10M 13.16S +/- 1S, DEC = -02D 19' 54.2" +/- 1", PLATE-ID = 00WM Equinox: J2000 Epoch: 1982.886 RV_or_Z: Z=0.956 Flux: V=18.2 Comments: COMPONENT A OF QUASAR PAIR Q0107-025A,B Target_Number: 2 Target_Name: Q0107-025B Alternate_Names: PB6291 Description: Galaxy, Lyman Alpha Cloud Position: RA = 01H 10M 16.28S +/- 1S, DEC = -02D 18' 52.4" +/- 1", PLATE-ID = 00WM Equinox: J2000 Epoch: 1982.886 RV_or_Z: Z=0.952 Flux: V=17.4 Comments: COMPONENT B OF QUASAR PAIR Q0107-025A,B Target_Number: 3 Target_Name: Q0107-0232 Alternate_Names: LBQS 0107-0232 Description: Galaxy, Lyman Alpha Cloud Position: RA = 01H 10M 14.47S +/- 1S, DEC = -02D 16' 58.9" +/- 1", Equinox: J2000 Epoch: 1982.886 RV_or_Z: Z=0.728 Flux: V=18.5 Visits ! Section 6 Visit_Number: 1 Visit_Comments: USE SAME GUIDE STARS FOR TARGETS 1 AND 2 AND FOR ALL EXPOSURES IN THIS VISIT Exposure_Number: 1 Target_Name: Q0107-025A Config: FOS/RD Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Number_of_Iterations: 1 Time_Per_Exposure: 62.6S Special_Requirements: ONBOARD ACQ FOR 2-5 Exposure_Number: 2 Target_Name: Q0107-025A Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: 2223-3278 Number_of_Iterations: 1 Time_Per_Exposure: 26M Exposure_Number: 3 Target_Name: Q0107-025A Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: 2223-3278 Number_of_Iterations: 1 Time_Per_Exposure: 40M Exposure_Number: 4 Target_Name: Q0107-025A Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: 2223-3278 Number_of_Iterations: 1 Time_Per_Exposure: 40M Exposure_Number: 5 Target_Name: Q0107-025A Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: 2223-3278 Number_of_Iterations: 1 Time_Per_Exposure: 40M Exposure_Number: 6 Target_Name: Q0107-025B Config: FOS/RD Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Number_of_Iterations: 1 Time_Per_Exposure: 32.7S Special_Requirements: ONBOARD ACQ FOR 7-9 Comments: USE SAME GUIDE STARS AS FOR TARGET 1 Exposure_Number: 7 Target_Name: Q0107-025B Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: 2223-3278 Number_of_Iterations: 1 Time_Per_Exposure: 28M Exposure_Number: 8 Target_Name: Q0107-025B Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: 2223-3278 Number_of_Iterations: 1 Time_Per_Exposure: 40M Exposure_Number: 9 Target_Name: Q0107-025B Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: 2223-3278 Number_of_Iterations: 1 Time_Per_Exposure: 40M Visit_Number: 2 Visit_Comments: USE SAME GUIDE STARS FOR ALL EXPOSURES IN THIS VISIT; KEEP TELESCOPE POSITION AND ORIENTATION THE SAME FOR ALL EXPOSURES IN THIS VISIT Exposure_Number: 10 Target_Name: Q0107-0232 Config: FOS/RD Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Number_of_Iterations: 1 Time_Per_Exposure: 100.6S Special_Requirements: ONBOARD ACQ FOR 11,13,15,17,19,21,23,25 Exposure_Number: 11 Target_Name: Q0107-0232 Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1590-2312 Number_of_Iterations: 1 Time_Per_Exposure: 24M Exposure_Number: 12 Target_Name: Q0107-0232 Config: WFPC2 Opmode: IMAGE Aperture: WFALL Sp_Element: F606W Number_of_Iterations: 1 Time_Per_Exposure: 15M Optional_Parameters: CR-SPLIT=NO Special_Requirements: PAR WITH 11 Exposure_Number: 13 Target_Name: Q0107-0232 Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1590-2312 Number_of_Iterations: 1 Time_Per_Exposure: 37M Exposure_Number: 14 Target_Name: Q0107-0232 Config: WFPC2 Opmode: IMAGE Aperture: WFALL Sp_Element: F606W Number_of_Iterations: 1 Time_Per_Exposure: 15M Optional_Parameters: CR-SPLIT=NO Special_Requirements: PAR WITH 13 Exposure_Number: 15 Target_Name: Q0107-0232 Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1590-2312 Number_of_Iterations: 1 Time_Per_Exposure: 37M Exposure_Number: 16 Target_Name: Q0107-0232 Config: WFPC2 Opmode: IMAGE Aperture: WFALL Sp_Element: F606W Number_of_Iterations: 1 Time_Per_Exposure: 15M Optional_Parameters: CR-SPLIT=NO Special_Requirements: PAR WITH 15 Exposure_Number: 17 Target_Name: Q0107-0232 Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1590-2312 Number_of_Iterations: 1 Time_Per_Exposure: 37M Exposure_Number: 18 Target_Name: Q0107-0232 Config: WFPC2 Opmode: IMAGE Aperture: WFALL Sp_Element: F606W Number_of_Iterations: 1 Time_Per_Exposure: 15M Optional_Parameters: CR-SPLIT=NO Special_Requirements: PAR WITH 17 Exposure_Number: 19 Target_Name: Q0107-0232 Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1590-2312 Number_of_Iterations: 1 Time_Per_Exposure: 37M Exposure_Number: 20 Target_Name: Q0107-0232 Config: WFPC2 Opmode: IMAGE Aperture: WFALL Sp_Element: F606W Number_of_Iterations: 1 Time_Per_Exposure: 15M Optional_Parameters: CR-SPLIT=NO Special_Requirements: PAR WITH 19 Exposure_Number: 21 Target_Name: Q0107-0232 Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1590-2312 Number_of_Iterations: 1 Time_Per_Exposure: 37M Exposure_Number: 22 Target_Name: Q0107-0232 Config: WFPC2 Opmode: IMAGE Aperture: WFALL Sp_Element: F606W Number_of_Iterations: 1 Time_Per_Exposure: 15M Optional_Parameters: CR-SPLIT=NO Special_Requirements: PAR WITH 21 Exposure_Number: 23 Target_Name: Q0107-0232 Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1590-2312 Number_of_Iterations: 1 Time_Per_Exposure: 37M Exposure_Number: 24 Target_Name: Q0107-0232 Config: WFPC2 Opmode: IMAGE Aperture: WFALL Sp_Element: F606W Number_of_Iterations: 1 Time_Per_Exposure: 15M Optional_Parameters: CR-SPLIT=NO Special_Requirements: PAR WITH 23 Exposure_Number: 25 Target_Name: Q0107-0232 Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1590-2312 Number_of_Iterations: 1 Time_Per_Exposure: 37M Exposure_Number: 26 Target_Name: Q0107-0232 Config: WFPC2 Opmode: IMAGE Aperture: WFALL Sp_Element: F606W Number_of_Iterations: 1 Time_Per_Exposure: 15M Optional_Parameters: CR-SPLIT=NO Special_Requirements: PAR WITH 25 Exposure_Number: 27 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1590-2312 Number_of_Iterations: 1 Time_Per_Exposure: DEF Comments: DO NOT CHANGE GRATING POSITION BETWEEN EXPOSURES 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 !