! File: 1261C.PROP ! Database: PEPDB ! Date: 16-FEB-1994:08:14:31 coverpage: title_1: OBSERVATIONS OF SS 433 - CYCLE 0 sci_cat: STELLAR ASTROPHYSICS sci_subcat: X-RAY SOURCES proposal_for: GTO/FOC pi_fname: ALEC pi_lname: BOKSENBERG pi_inst: ROYAL GREENWICH OBSERVATORY pi_country: UNITED KINGDOM pi_phone: 0 323 833171 keywords_1: SS 433; JETS. hours_pri: 6.00 num_pri: 1 time_crit: X pi_position: PROFESSOR off_fname: F. off_lname: MACCHETTO ! end of coverpage abstract: line_1: Jet formation is a widespread phenomenon in the universe. Jets have been line_2: identified is such widely disparate sites as AGNs, neutron stars and black line_3: holes, accreting hot subwards or white dwarfs and young stars embedded in line_4: cocoons of gas and dust. We propose here to study the structure and dynamics line_5: of jets in SS 433. This object affords us the best means of directly testing line_6: the physics of accretion disk formation and jet activity. Specifically, high line_7: spatial resolution images of SS 433 will reveal the presumed jets of material line_8: giving rise to the moving spectral features, definitely resolving fundamental line_9: questions on the overall geometry encompassing the ballistically flowing line_10: material. Sequential images taken at intervals of a few days will record the line_11: time development of the bursts of ejection relating to the short-lived spectral line_12: structure observed. ! ! end of abstract general_form_proposers: lname: BOKSENBERG fname: ALEC inst: ROYAL GREENWICH OBSERVATORY country: UNITED KINGDOM esa: X ! lname: PARESCE fname: FRANCESCO inst: ESA, SPACE TELESCOPE SCIENCE INSTITUTE country: USA esa: X ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Direct imaging using the f/288 mode using the objective prism or appropriate line_2: filters to accept the moving H Beta and Ly alpha features will be followed in a line_3: sequence taken over 10-20 days, complemented by some contiguous objective line_4: prism spectroscopy. Roll deconvolution will be used for Ly alpha imaging. line_6: Typical photometric data for SS 433 are V = 14.2, B-V=2.1, U-B=0.6. line_7: Interstellar extinction is severe, with AV possibly in the range 5-8 mag. The line_8: flux in a typical H Beta moving feature is 3.7x10 dex-13 erg per sq. cm. per line_9: sec. Assuming the flux ratio Ly alpha/H Beta is intrinsically about 30 the flux line_10: in a Ly alpha (red component) moving feature given the above extinction range line_11: is 3 x 10 dex-15 to 3 x 10 dex-19 erg per sq. cm. per sec. Using the line_12: geocoronal Ly alpha blocking filter, with filters or objective prism to line_13: separate the Ly alpha and H Beta images, only very short exposures are needed line_14: at H Beta (in fact, neutral density filters must be used to avoid saturation), line_15: but at Ly alpha exposures would range from 10 sec to 10 hours at the rest line_16: wavelength in the worst case because of the uncertainty in reddening. But when line_17: the red moving component is near its longest wavelength position (about 150nm) line_18: the sharp decrease in worst case reddening will decrease the exposure time by line_19: at least a factor 10, to 1 hour or less. We estimate a total observing time of line_20: 6 hours for a sequence of H Beta images with selected Ly alpha images chosen in line_21: the most effective combination to identify the time development and geometry of line_22: the moving structure. ! question: 4 section: 1 line_1: The full resolution of the FOC is needed to reveal the material exhibiting the line_2: moving spectral features and to delineate the system structure. Adequate line_3: resolution to identify ballistic jet structure can be obtained even at the line_4: wavelengths of the moving H Beta line emission and quite clear images cn be line_5: obtained at Ly alpha emission. Although reddenting is severe for this object line_6: Ly alpha still may be detectable in reasonable exposure times. ! question: 7 section: 1 line_1: Full data reduction facilities are available to us. ! question: 10 section: 1 line_1: Data reduction facilities. ! question: 13 section: 1 line_1: High spatial resolution imaging and spectroscopy of the ejection phenomenon in line_2: SS 433. ! !end of general form text general_form_address: lname: BOKSENBERG fname: ALEC title: PROF. category: PI inst: ROYAL GREENWICH OBSERVATORY addr_1: HERSTMONCEUX CASTLE addr_2: BN27 1RP city: HAILSHAM, EAST SUSSEX country: UNITED KINGDOM phone: (44)323 83333171 telex: 87451 RGOBSY G ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: SS433 descr_1: HIGHLY EVOLVED STAR pos_1: RA=19H09M21.3S+/-0.2S, pos_2: DEC=+4D53'53.1"+/-0.5" equinox: 1950 pm_or_par: N plate_req: N plate_avail: N fluxnum_1: 1 fluxval_1: V=14.2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 2.000 sequence_1: DEFINE sequence_2: CYCLE targname: SS433 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F502M wavelength: 4950 num_exp: 1 time_per_exp: 600 S priority: 1 req_1: GROUP 2-6 NO GAP; req_2: CYCLE 0 / 2-6; ! linenum: 3.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F502M wavelength: ^ num_exp: ^ time_per_exp: 600 S priority: 1 ! linenum: 4.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: PRISM1 wavelength: ^ num_exp: ^ time_per_exp: 1000 S priority: 1 ! linenum: 5.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: PRISM2 wavelength: ^ num_exp: ^ time_per_exp: 1000 S priority: 2 req_1: DARK TIME; ! linenum: 6.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F502M wavelength: 4950 num_exp: ^ time_per_exp: 900 S priority: 3 ! linenum: 7.000 sequence_1: USE sequence_2: CYCLE ! linenum: 7.500 sequence_1: USE CYCLE req_1: AFTER 7.0 BY 3D+/-0.5D ! ! end of exposure logsheet ! No scan data records found