! File: 4978C.PROP
! Database: PEPDB
! Date: 23-FEB-1994:13:25:36
coverpage:
title_1: LYMAN-ALPHA REGION OF QSOS WITH STRONG ABSORPTION LINES:
title_2: FUTURE CYCLE OBSERVATIONS - EXPO
sci_cat: QUASARS & AGN
sci_subcat: QUASAR ABSORPTION
proposal_for: GTO/HRS
cont_id: 1193
pi_title: DR.
pi_fname: EDWARD
pi_lname: BEAVER
pi_inst: UC, SAN DIEGO
pi_country: USA
pi_phone: (619) 534-1878
keywords_1: QUASARS, ABSORPTION LINES, 21-CM
hours_pri: 1.68
num_pri: 2
wf_pc: Y
pi_position: RESEARCH PHYSICIST
! end of coverpage
abstract:
line_1: FOS spectra have been obtained of the Ly-alpha region of 3 quasars
line_2: with 21 cm absorption, 3CR 196, PKS 1229-021, and 3CR 286.
line_3: The absorbing object is almost certainly a galaxy disk in each case.
line_4: Measurement of the damped Ly-alpha line will determine the H I column
line_5: density in the 21 cm absorption system, and comparison with 21 cm will
line_6: yield the spin temperature. The number of contributing components will
line_7: be determined from existing or new 21 cm observations. Comparison with
line_8: optical observations will allow the determination of chemical
line_9: abundances with respect to H for elements with low-ionization lines.
line_10: Images taken after the new WF/PC installation may identify the
line_11: absorbing galaxy and, if so, will allow us to characterize the impact
line_12: parameter and Hubble type of galaxies producing damped Ly-alpha
line_13: absorption at moderate redshift. Two of these will be done in this
line_14: proposal.
!
! end of abstract
general_form_proposers:
lname: COHEN
fname: ROSS
inst: UC, SAN DIEGO
country: USA
!
lname: BEAVER
fname: EDWARD
inst: UC, SAN DIEGO
country: USA
!
! end of general_form_proposers block
general_form_text:
question: 3
section: 1
line_1: We will use the WFC with F702W
line_2: to image 3CR 196 and PKS1229-021. 1200S per image.
!
question: 4
section: 1
line_1: The absorbing objects are lost in the point spread function of the
line_2: quasar in ground-based images.
!
question: 7
section: 1
line_1: These observations will be reduced using the standard imaging
line_2: reduction software available for WF/PC data. Calibration
line_3: will be done using the results of SV observations.
line_4: Already existing software will be used to subtract the image of
line_5: the background quasar.
!
question: 9
section: 1
line_1: PI has received data from a number of
line_2: GTO programs, SAT, and ERO programs. Related
line_3: programs which have had observations are as
line_4: follows:
line_5: 1026 - ``UV Spectra of Low-Redshift-QSOs'': related,
line_6: 1027 - ``UV Spectra of QSOs with z> 3.1'': not related,
line_7: 1190 - ``FUV Emission LIne Profiles of W Serpentis
line_8: Binaries'': not related
line_11: Observations of UM 675 have shown
line_12: that any He I Gunn--Peterson effect is small, that
line_13: He I absorption lines are not strong, that
line_14: predictions of the ``Lyman valley'' may be
line_15: correct, and that low redshift Ly-alpha is more
line_16: prevalent than expected. Observations of low
line_17: redshift QSOs (including 3C 273) have shown even
line_18: more clearly that Ly-alpha absorption occurs in
line_19: greater numbers than expected, as well as showing
line_20: emission--line profile differences more clearly
line_21: than from earlier data. Unexpectedly, Ly-alpha
line_22: is {\it narrower} than H-alpha.
line_23: ``Far--Ultraviolet Spectroscopy of the Quasar UM
!
question: 9
section: 2
line_1: 675 with the Faint Object Spectrograph on the
line_2: Hubble Space Telescope'', E.A.Beaver,
line_3: E.M.Burbidge, R.D.Cohen, V.T.Junkkarinen,
line_4: R.W.Lyons, E.I.Rosenblatt, G.F.Hartig, B.Margon,
line_5: and A.F.Davidsen, {\it Ap.J.(Lett.)}, {\bf 377},
line_6: L1, 1991.
line_7: ``First Results from the GHRS: UV Spectra of a
line_8: Starburst Knot in NGCC 1068'', Hutchings, J.B.,
line_9: Bruhweiler, G.C., Boggess, A., Heap, S.R., Ebbets,
line_10: D.C., Beaver, E., Rosenblatt, E., Truonmg, K.Q.,
line_11: Perez, M., and Westmacott, R., 1991, APJ
line_12: (Letters), 377, 1991.
!
question: 10
section: 1
line_1: The majority of the resources required for this project other than the
line_2: normal facilities of a university (librarys, offices, etc.) were
line_3: supplied by NASA to the members of the GHRS IDT for these projects.
line_4: These include all the computing facilities required for the completion
line_5: of data reduction and analysis.
line_6: Optical and IR ground--based observing facilities and support are
line_7: provided by the University of California.
!
!end of general form text
general_form_address:
lname: COHEN
fname: ROSS
category: CON
inst: UNIV. OF CALIF.,SAN DIEGO
addr_1: CASS DEPT., C0111
addr_2: 9500 Gilman Drive
city: LA JOLLA
state: CA
zip: 920930111
country: USA
phone: (619)534-2664
telex: (619)534-6316(FAX)
!
lname: BEAVER
fname: EDWARD
title: DR.
category: PI
inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO
addr_1: CASS DEPT., C011
addr_2: 9500 Gilman Drive
city: LA JOLLA
state: CA
zip: 920930111
country: USA
phone: 619-534-1878
telex: (619)534-6316(FAX)
!
! end of general_form_address records
fixed_targets:
targnum: 2
name_1: PKS1229-021
name_2: 4C02.55
descr_1: E,314,
descr_2: H,515,516
pos_1: RA=12H 31M 59.999S +/- 0.3",
pos_2: DEC=-02D 24' 5.34" +/- 0.3",
pos_3: PLATE-ID = 00BB
equinox: 2000
rv_or_z: Z=1.038
fluxnum_1: 1
fluxval_1: V=16.75+/-1.0
!
targnum: 3
name_1: 3C196
name_2: 4C48.22
descr_1: E,314,
descr_2: H,515,516
pos_1: RA=08H 13M 36.059S +/- 0.3",
pos_2: DEC=48D 13' 2.49" +/- 0.3",
pos_3: PLATE-ID = 02HE
equinox: 2000
rv_or_z: Z=0.871
fluxnum_1: 1
fluxval_1: V=17.8+/-1.0
!
! end of fixed targets
! No solar system records found
! No generic target records found
exposure_logsheet:
linenum: 8.000
targname: PKS1229-021
config: WFC
opmode: IMAGE
aperture: ANY
sp_element: F702W
num_exp: 1
time_per_exp: 1200S
fluxnum_1: 1
priority: 1
req_1: CYCLE 9 / 8
!
linenum: 13.000
targname: 3C196
config: WFC
opmode: IMAGE
aperture: ANY
sp_element: F702W
num_exp: 1
time_per_exp: 1200S
fluxnum_1: 1
priority: 1
req_1: CYCLE 9 / 13
!
! end of exposure logsheet
! No scan data records found