! $Id: 5675,v 6.1 1994/08/10 15:01:28 pepsa Exp $ coverpage: title_1: OCCULTATION STUDIES OF RE1149+28: AN OBJECT WITH AN EXTREME title_2: EUV/OPTICAL RATIO sci_cat: HOT STARS sci_subcat: ERUPTIVE BINARIES proposal_for: GO/CAR cont_id: 4449 pi_fname: JONATHAN pi_mi: PD pi_lname: MITTAZ pi_inst: 8054 pi_country: U.K. hours_pri: 9.80 num_pri: 1 fos: Y off_fname: LEN off_lname: CULHANE off_title: LAB. DIRECTOR off_inst: 8054 off_addr_1: MULLARD SPACE SCIENCE LABORATORY off_addr_2: HOLMBURY ST. MARY off_addr_3: NR. DORKING off_city: SURREY off_country: UK off_phone: UK-483 274111 ! end of coverpage abstract: line_1: One of the fundamental and outstanding problems to be line_2: resolved in AM Her stars is the origin of the high ratio line_3: of the soft/hard X-ray flux ratio compared to the value line_4: (~ 1) predicted in the conventional shock model. The only line_5: explanation so far advanced is that of a `blobby' accretion line_6: flow which directly penetrates and heats the white dwarfs line_7: photosphere, thereby enhancing the soft X-ray flux at the line_8: expense of the hard X-ray flux. Clearly, knowledge of the line_9: state of the gas near the white dwarf is crucial in trying to line_10: understand this problem. We propose to probe the structure line_11: of the inner, UV emitting accretion stream in RE1149+28, the line_12: most extreme example of a EUV bright system. RE1149+28 has line_13: the highest EUV/optical ratio of any known AM Her, and line_14: therefore it might be expected that most of the accretion line_15: occurs via blobs. By studying the UV line emission in line_16: RE1149+28 we can gain critical information on the gas close line_17: into the WD surface, such a study being facilitated by that line_18: fact that RE1149+28 is a pole occulting system. The line_19: structure of the accretion stream can therefore be observed line_20: as it crosses the limb of the white dwarf. ! ! end of abstract general_form_proposers: lname: MITTAZ fname: JONATHAN title: PI mi: PD inst: 8054 country: UK esa: Y ! lname: ROSEN fname: SIMON mi: R inst: 8042 country: UK esa: Y ! lname: MASON fname: KEITH mi: O inst: 8054 country: UK esa: Y ! lname: HOWELL fname: STEVE mi: B inst: 3180 country: US ! lname: ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Our investigation requires well spectrally resolved, good S/N line_2: spectra with sufficient temperal resolution to adequately sample the line_3: orbital cycle. Using the G130H grating we will cover the important line_4: lines of N V, Si IV and C IV. In order to adequately sample the line_5: critical phases when the accretion stream crosses the limb of the line_6: white dwarf (likely duration 5-10 minutes), exposure times of line_7: approximately 1 minute are required to achive sufficent time line_8: resolution as well as reasonable S/N (including the effects of line_9: phase binning). The 1.0 arcsec aperture will be used. line_10: To ensure that we obtain data during line_11: the limb crossing, as well as to study the orbital effects in line_12: detail, we require prefer uniform phase coverage. Unfortunately, line_13: the orbital period of RE1149+28 is nearly commensurate with that line_14: of HST, drifting by 0.06 in phase each orbit. Within the total line_15: exposure time we can not obtain uniform phase coverage using line_16: contigous orbits, but we can cover all phases. Ideally we would line_17: like to get uniform coverage, which would mean having some gaps line_18: between contiguous observations by spreading all the observations line_19: over 1.5 days. Therefore, we would like several visits if line_20: possible over a 1.5 day period, but if this is not possible line_21: contiguous orbits will cover all phases, if not uniformly. line_22: In the optical, RE1149+28 varies between 17.2 and 17.8 with a line_23: quasi-sinuosoidal lightcurve. ! question: 5 section: 1 line_1: We request near contiguous observations of RE1149+28. We do not line_2: want strictly contiguous observations, however, due to the beat line_3: between the 90 minute orbital period of RE1149+28 and the 96 line_4: minute orbital period of HST giving rise to a beat period of 1 day. line_5: Since the total spacecraft time (including earth blocks etc.) is line_6: approx. 19 hours we would not be able to cover the complete line_7: orbital period. We would therefore prefer the observations to be line_8: spread over at least 1 day to ensure we get a complete phase line_9: coverage while observing as near to contiguous as can be managed. line_10: One possibility is splitting the time into two blocks, each line_11: contiguous but spread over 1.5 days. Strictly contiguous line_12: observations will cover all phases, though not uniformly. ! question: 6 section: 1 line_1: Routine FOS calibration data will be sufficient for our purposes ! question: 8 section: 1 line_1: We will be endevouring to obtain simultaneous or near simultaneous line_2: optical spectroscopy on La Palma and one of use (SBH) will also line_3: obtain time on the Lowell telescopes. Therefore we will be able line_4: to compare the behaviour of the UV and optical lines at the same line_5: epoch. This may be particularly useful with regard to searching line_6: for ionization structure. However, we stress that we will be line_7: seeking to arrange suitable optical observations that fit in with line_8: the HST schedule, rather than requiring HST observations to be line_9: dependent on optical observations. ! ! !end of general form text general_form_address: lname: MITTAZ fname: DR. JONATHAN mi: PD category: PI inst: 8054 addr_1: MULLARD SPACE SCIENCE LABORATORY, addr_2: HOLMBURY ST. MARY addr_3: NR DORKING city: SURREY country: U.K. phone: 0483 274111 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: RE1149545+284512 descr_1: A,153 pos_1: RA = 11H 49M 55.709S +/- 0.07", pos_2: DEC = +28D 45' 07.56" +/- 1", pos_3: PLATE-ID = 01TE equinox: J2000 comment_1: THE FLUX DATA PROVIDED ARE PURELY comment_2: EXTRAPOLATIONS BASED ON THE V comment_3: MAGNITUDE AND ASSUMING A TYPICAL comment_4: AM-HER CONTINUUM MODEL (EG. comment_5: MARASCHI ET AL 1984) AND AN comment_6: EQUIVALENT WIDTH OF ORDER 100 FOR comment_7: UV EMISSION LINES (EG. MUKAI ET AL comment_8: 1986). THE ERRORS ON THE comment_9: MAGNITUDES REFLECT THE INTRINSIC comment_10: VARIABILITY. fluxnum_1: 1 fluxval_1: V = 17.5 +/- 0.3 fluxnum_2: 2 fluxval_2: B-V = 0.5 +/- 0.3 fluxnum_3: 3 fluxval_3: F-CONT(1550) = 3.49 E-15 fluxnum_4: 4 fluxval_4: F-LINE(1550) = 3.5 E-13 fluxnum_5: 5 fluxval_5: W-LINE(1550) = 5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: RE1149545+284512 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 73S priority: 1 req_1: CYCLE 4 / 1-13; req_2: ONBOARD ACQ FOR 2-6 comment_1: NOTE STAR IS VARIABLE BY ~ 0.3 comment_2: MAG ABOUT THE MEAN USED. ! linenum: 2.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 39M s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 req_1: SEQ 1-6 NO GAP; comment_1: S/N FOR LINE PEAK AT CIV 1550 comment_2: THE DATA IS REQUESTED TO BE comment_3: CONTIGUOUS IF POSSIBLE WITHIN TWO comment_4: BLOCKS (2-6,8-13) WHICH SHOULD BE comment_5: SEPARATED BY A MULTIPLE OF 0.5 DAYS comment_6: FOR OPTIMUM BINARY PHASE COVERAGE. ! linenum: 3.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 39M s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 comment_1: S/N FOR LINE PEAK AT CIV 1550 ! linenum: 4.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 39M s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 comment_1: S/N FOR LINE PEAK AT CIV 1550 ! linenum: 5.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 39M s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 comment_1: S/N FOR LINE PEAK AT CIV 1550 ! linenum: 6.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 1820S s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 comment_1: S/N FOR LINE PEAK AT CIV 1550 ! linenum: 7.000 targname: RE1149545+284512 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 73S priority: 1 req_1: ONBOARD ACQ FOR 8-13; req_2: AFTER 1 BY 24H +/- 12H; comment_1: NOTE STAR IS VARIABLE BY ~ 0.3 comment_2: MAG ABOUT THE MEAN USED. ! linenum: 8.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 39M s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 req_1: SEQ 7-13 NO GAP; comment_1: S/N FOR LINE PEAK AT CIV 1550 ! linenum: 9.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 39M s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 comment_1: S/N FOR LINE PEAK AT CIV 1550 ! linenum: 10.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 39M s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 comment_1: S/N FOR LINE PEAK AT CIV 1550 ! linenum: 11.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 39M s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 comment_1: S/N FOR LINE PEAK AT CIV 1550 ! linenum: 12.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 39M s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 comment_1: S/N FOR LINE PEAK AT CIV 1550 ! linenum: 13.000 targname: RE1149545+284512 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 1820S s_to_n: 10 s_to_n_time: 4M fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: STEP-PATT=DEF param_2: STEP-TIME=0.5 param_3: SUB-STEP=4 param_4: COMB=YES param_5: READ-TIME=65 comment_1: S/N FOR LINE PEAK AT CIV 1550 ! ! end of exposure logsheet ! No scan data records found