! File: 3468C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:08:49:56 coverpage: title_1: UV MOLECULAR BANDS IN HD44179 sci_cat: INTERSTELLAR MEDIUM sci_subcat: CIRCUMSTELLAR MATTER proposal_for: GO pi_fname: MICHAEL pi_mi: L. pi_lname: SITKO pi_inst: UNIV. OF CINCINNATI pi_country: USA pi_phone: 513-556-0642 hours_pri: 11.98 num_pri: 1 fos: Y hrs: Y funds_amount: 67099 funds_length: 12 off_fname: FRANK off_mi: R. off_lname: TEPE off_title: VP OF RESEARCH off_inst: UNIV. OF CINCINNATI off_addr_1: ML 627 off_addr_2: 304 BRAUNSTEIN off_city: CINCINNATI off_state: OH off_zip: 45221 off_country: USA off_phone: (513)556-2872 ! end of coverpage abstract: line_1: HD 44179, the central star of the Red Rectangle Nebula, may be line_2: a natural molecular factory. It is unique in exhibiting molecular line_3: emission bands in the ultraviolet that are as strong as the continuum, line_4: even at low spectral resolution. It is important to understand where line_5: these molecules are formed, whether they are free or adsorbed onto line_6: grain surfaces, and how the molecular emission region is related to line_7: the dusty region as a whole (geometrically). Furthermore, a proper line_8: identification of the molecular species and their physical state will line_9: make it possible to understand part of the nature of molecular line_10: formation in stars and the ejection of this material into the line_11: interstellar medium. The goals of this project are to understand line_12: the chemical and physical nature of the material giving rise to line_13: the UV bands, using high resolution spectroscopy and low resolution line_14: spectropolarimetry. line_15: The Phase I proposal was for 12.08 hours of exposure time, and 18.05 line_16: hours of spacecraft time. Phase I approval was for 18.04 hours of line_17: spacecraft time. For Phase II submission, the RPSS Source Estimator line_18: gives 11.984 hours of exposure and 18.01 hours of spacecraft time line_19: (using the revised ACQ times of 10 March 1992). At the recommendation line_20: of the Phase I review committee, the budget has been revised. ! ! end of abstract general_form_proposers: lname: SITKO fname: MICHAEL title: PI mi: L. inst: UNIV. OF CINCINNATI country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: This project consists of three parts. First, I will obtain spectropolarimetry line_2: with the FOS using G190H (1577-2331A) and G270H (2227-3306A) in order to line_3: determine the scattering geometry of the lines versus continuum. Second, I line_4: will determine the entire spectrum at 1-2A resolution from 1150-3306. The line_5: 1577-3306 spectrum will be reconstructed from the spectropolarimetry scans, line_6: since the wavelength and flux calibrations for the waveplate, gratings, line_7: detector, and entrance aperture used have been all calibrated by the FOS line_8: polarimetry team at the University of Arizona (Richard Allen & Paul Smith). line_9: The 1150-1608 region will be observed with the G130H grating of the FOS. line_10: These data will be used to locate various atomic and molecular features in line_11: the spectrum of this object. Finally, three molecular emission bands of CO line_12: (1600A, 1655A, and 1714A) and one probable CO absorption band (1930A) line_13: will be observed with the GHRS at 0.15A resolution. These observations will line_14: be used to look for rotation band structure and carbon isotopic abundances line_15: in the CO bands (A1PI-X1SIGMA and a3PI-X1SIGMA electronic transitions). line_16: All of the FOS observations will be made with the 1 arcsec aperture, line_17: sacrificing flux for spectral resolution, since these observations will be line_18: used for identifying a variety of molecular features believed to be present. line_19: This will require the highest spectral resolution with the FOS. line_20: For the GHRS observations, the flux in the UV is too low to use the line_21: Small Science Aperture, and the Large Science Aperture will be used, line_22: at the cost of reduced spectral resolution. The spectropolarimetry scans line_23: have been broken down to be able to complete a whole 8-position scan per orbit. ! question: 4 section: 1 line_1: The purpose of this project is to understand the unique UV spectral line_2: characteristics of HD 44179 and its surrounding Red Rectangle Nebula. line_3: The previous IUE data on this object were taken by the PI and consist of: line_4: 3 LWR spectra - total of 125 min, 5 SWP spectra - total of 1020 min line_5: Additional IUE spectra have also just been obtained (2/92) but not yet reduced. line_6: The earlier spectra achieved S/N of about 10 with a resolution of 8A in the line_7: region between 1550 and 2000 A. Shortward of 1550 A, the S/N dropped to about line_8: 2-3. The spectra, while exciting, did not have the spectral resolution needed line_9: to answer some of the basic questions outlined earlier. New observations with line_10: the HST will be used to improve the spectral resolution to 1.2 A across the line_11: entire spectrum (at higher S/N) and finally observe the important short line_12: wavelength region (less than 1500 A) with much improved S/N (by a factor of line_13: about 6 times). These will be used to confirm the possible detections of C2 line_14: and HC3N from the IUE study, and to search for other possible molecular line_15: species. Additional higher resolution observations at 0.14 A/diode (GHRS) are line_16: close to the wavelength spacing needed to resolve the CO rotation structure, line_17: and can be used to derive 12C/13C, which would be valuable for this object, line_18: which might be a post-AGB star exhibiting carbon dredge-up. line_19: There are no observations of the UV polarization characteristics of the object. line_20: Ground-based data show that the optical polarization of the star is about 1.5%, line_21: A comparison of the polarization properties of the UV emission lines versus the line_22: continuum may give a hint about the location of these features relative to the line_23: exciting star. The FOS/Pol is the only instrument that can do this. ! question: 6 section: 1 line_1: Reccomend that all FOS obseravtions be done with a single acquisition. line_2: Because of the brightness (V=8.9 mag) of the target, it is too bright line_3: to be acquired with ACQ/BINARY. Instead, one of the gratings used for line_4: the science observations will be used with ACQ/PEAK. The PEAK will line_5: consist of three phases, and will probably consume 1 orbit. In order line_6: to maximize the spacecraft use efficiency, this procedure should be done line_7: as infrequently as is possible. line_8: It is also desirable that the short-wavelength FOS spectrum be obtained line_9: in a manner that minimizes the terrestrial OI 1304A airglow, since this line_10: is a line that will be searched for in the spectrum. Dark time is line_11: therefore requested for this observation. ! question: 7 section: 1 line_1: All of the data will be extracted using STSDAS at the PI's line_2: home institution. The department facility consists of 4 Sun line_3: workstations, NOAO IRAF has just been installed, and STSDAS will be line_4: installed. line_5: The "lower" high resolution spectra will be used to determine line_6: central wavelengths and line profiles. These will be compared to line_7: those of known molecules, and, where possible, column densities line_8: derived. Energy spacings of many features will be compared in order line_9: to identify C(triple)C, C(triple)N, and C(single)H bonds common in line_10: carbon-chain molecules (such as cyanopolyenes), as well as look for line_11: evidence of PAHs. The PI has also just written a program that calculates line_12: the expected CO lines, based on published vibration/rotation constants. line_13: The higher resolution observations will be used to see if any line_14: rotation-band structure is present, and to try to identify the line_15: strong absorption feature at 1930 A. They will also be used to line_16: determine 12C/13C from the 4 A splitting in the CO lines. line_17: For the low resolution spectropolarimetry data, the data sets line_18: for all the different wave plate positions will be used to line_19: determine the percent and position angle of polarization. The line_20: polarization of the emission bands and continuum will be compared. line_21: Differences between these will be modeled with a star plus emission line_22: line cloud plus scattering medium model. The polarimetry spectra will be line_23: coadded to get the total intensity spectrum from 1577-3306A. ! question: 10 section: 1 line_1: The PI's department currently has 4 Sun SPARC workstations for line_2: data extraction and analyis. The facilities are, however, greatly line_3: overloaded as they are shared by 30 faculty and 70 graduate line_4: students. A Sun SPARCstation will be needed. In order to line_5: run the STSDAS/IRAF software, store the data (lots of FOS line_6: scans), and access related databases, additional hard disk line_7: drives and an exabyte tape drive are absolutely essential, and line_8: a CD ROM reader very desirable. line_9: The PI's department has no spare money for research graduate line_10: students, and little in the way of additional funds. About $500 line_11: may be available for travel to go to a meeting. The university line_12: currently has a $14M deficit, and the department took a $200K line_13: reduction for next year. Our astrophysics program is small (1 line_14: person - the PI), and needs additional support. ! !end of general form text general_form_address: lname: SITKO fname: MICHAEL mi: L. category: PI inst: UNIV. OF CINCINNATI addr_1: DEPT. OF PHYSICS addr_2: ML 011 addr_3: 400 GEOLOGY/PHYSICS BLDG city: CINCINNATI state: OH zip: 45221 country: USA phone: (513)556-0642 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD44179 name_2: RED_RECTANGLE_STAR descr_1: A, 115, 116, 117, 184, descr_2: G, 502, 504 pos_1: RA=06H 19M 58.14S +/- 1.0", pos_2: DEC=-10D 38' 13.9" +/- 1.0", pos_3: PLATE-ID=02NT equinox: J2000 comment_1: LINE FLUXES ARE VALUES ABOVE CONT. comment_2: CONT.FLAT IN F-LAMBDA AT F=1.0E-13 comment_3: IN THE REGION OF THE LINES. comment_4: SOURCE IS IN NEBULOSITY. SOURCE IS comment_5: DOUBLE, 0.3 ARCSEC SEP. comment_6: PECULIAR EXTINCTION CURVE. EM. AND comment_7: ABS. BANDS. FLUX DROPS BY 30X comment_8: GOING FROM 1600A TO 1400A. comment_9: SOURCE TOO BRIGHT FOR FOS comment_10: ACQ/BINARY. fluxnum_1: 1 fluxval_1: V=8.8,TYPE=B9III,E(B-V)=0.7 fluxnum_2: 2 fluxval_2: F-CONT(1930)=1.0+/-0.2E-13 fluxnum_3: 3 fluxval_3: F-LINE(1714)=2.0E-14, W-LINE(1714)=10 fluxnum_4: 4 fluxval_4: F-LINE(1655)=8.0E-14,W-LINE(1655)=15 fluxnum_5: 5 fluxval_5: F-LINE(1600)=2.0E-14, W-LINE(1600)=8 fluxnum_6: 6 fluxval_6: F-CONT(1500)=3.0+/-1.0E-14 fluxnum_7: 7 fluxval_7: F-CONT(1300)=3.0+/-1.0E-15 fluxnum_8: 8 fluxval_8: F-CONT(2700)=2.5+/-0.5E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD44179 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 6 fluxnum_2: 8 priority: 1 param_1: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 2-5; req_2: CYCLE 2 / 1.00-6.09 ! linenum: 2.000 targname: HD44179 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1600 num_exp: 10 time_per_exp: 10M s_to_n: 15 s_to_n_time: 100M fluxnum_1: 5 priority: 1 param_1: FP-SPLIT=STD param_2: DOPPLER=ON ! linenum: 3.000 targname: HD44179 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1655 num_exp: 10 time_per_exp: 10M s_to_n: 20 s_to_n_time: 100M fluxnum_1: 4 priority: 1 param_1: FP-SPLIT=STD param_2: DOPPLER=ON ! linenum: 4.000 targname: HD44179 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1714 num_exp: 10 time_per_exp: 10M s_to_n: 18 s_to_n_time: 100M fluxnum_1: 3 priority: 1 param_1: FP-SPLIT=STD param_2: DOPPLER=ON ! linenum: 5.000 targname: HD44179 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G200M wavelength: 1930 num_exp: 5 time_per_exp: 10M s_to_n: 17 s_to_n_time: 50M fluxnum_1: 2 priority: 1 param_1: FP-SPLIT=STD param_2: DOPPLER=ON ! linenum: 6.000 targname: HD44179 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G190H wavelength: 1577-2331 num_exp: 1 time_per_exp: 0.03S fluxnum_1: 2 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 6.01; req_2: SPATIAL SCAN; req_3: GROUP/6.00-6.08 NO GAP ! linenum: 6.010 targname: HD44179 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G190H wavelength: 1577-2331 num_exp: 1 time_per_exp: 0.03S fluxnum_1: 2 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 6.02; req_2: SPATIAL SCAN ! linenum: 6.020 targname: HD44179 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G190H wavelength: 1577-2331 num_exp: 1 time_per_exp: 1.00S fluxnum_1: 2 priority: 1 param_1: TYPE=UP param_2: SCAN-STEP=0.35 param_3: SEARCH-SIZE=3 req_1: ONBOARD ACQUISITION FOR 6.03-6.08 ! linenum: 6.030 targname: HD44179 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1577-2331 num_exp: 1 time_per_exp: 24M s_to_n: 35 fluxnum_1: 2 priority: 1 param_1: POLSCAN=8B comment_1: S/N LISTED IS THE S/N PER DIODE OF comment_2: COADDED SPECTRA. SIGMA PERCENT comment_3: POLARIZATION WITH WAVEPLATE B comment_4: AND 5 DIODE BINS IS 2.4 PERCENT comment_5: AT 1900A. ! linenum: 6.040 targname: HD44179 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1577-2331 num_exp: 1 time_per_exp: 24M s_to_n: 35 fluxnum_1: 2 priority: 1 param_1: POLSCAN=8B comment_1: S/N LISTED IS THE S/N PER DIODE OF comment_2: COADDED SPECTRA. SIGMA PERCENT comment_3: POLARIZATION WITH WAVEPLATE B comment_4: AND 5 DIODE BINS IS 2.4 PERCENT comment_5: AT 1900A. REPEAT OF LINE 6.03 ! linenum: 6.050 targname: HD44179 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1577-2331 num_exp: 1 time_per_exp: 24M s_to_n: 35 fluxnum_1: 2 priority: 1 param_1: POLSCAN=8B comment_1: S/N LISTED IS THE S/N PER DIODE OF comment_2: COADDED SPECTRA. SIGMA PERCENT comment_3: POLARIZATION WITH WAVEPLATE B comment_4: AND 5 DIODE BINS IS 2.4 PERCENT comment_5: AT 1900A. REPEAT OF LINE 6.04 ! linenum: 6.060 targname: HD44179 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1577-2331 num_exp: 1 time_per_exp: 24M s_to_n: 35 fluxnum_1: 2 priority: 1 param_1: POLSCAN=8B comment_1: S/N LISTED IS THE S/N PER DIODE OF comment_2: COADDED SPECTRA. SIGMA PERCENT comment_3: POLARIZATION WITH WAVEPLATE B comment_4: AND 5 DIODE BINS IS 2.4 PERCENT comment_5: AT 1900A. REPEAT OF LINE 6.05 ! linenum: 6.070 targname: HD44179 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2227-3306 num_exp: 1 time_per_exp: 24M s_to_n: 150 fluxnum_1: 8 priority: 1 param_1: POLSCAN=8B comment_1: S/N LISTED IS S/N PER PIXEL OF comment_2: COADDED SPECTRA. SIGMA PERCENT comment_3: POLARIZATION WITH WAVEPLATE B comment_4: AND 10 PIXEL BINS IS 0.5 PERCENT comment_5: AT 2700A. ! linenum: 6.080 targname: HD44179 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2227-3306 num_exp: 1 time_per_exp: 24M s_to_n: 150 fluxnum_1: 8 priority: 1 param_1: POLSCAN=8B comment_1: S/N LISTED IS S/N PER PIXEL OF comment_2: COADDED SPECTRA. SIGMA PERCENT comment_3: POLARIZATION WITH WAVEPLATE B comment_4: AND 10 PIXEL BINS IS 0.5 PERCENT comment_5: AT 2700A. REPEAT OF LINE 6.07 ! linenum: 6.085 targname: HD44179 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G190H wavelength: 1577-2331 num_exp: 1 time_per_exp: 0.03S fluxnum_1: 2 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 6.086; req_2: SPATIAL SCAN; req_3: GROUP/6.085-6.09 NO GAP ! linenum: 6.086 targname: HD44179 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G190H wavelength: 1577-2331 num_exp: 1 time_per_exp: 0.03S fluxnum_1: 2 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 6.087; req_2: SPATIAL SCAN ! linenum: 6.087 targname: HD44179 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G190H wavelength: 1577-2331 num_exp: 1 time_per_exp: 1.00S fluxnum_1: 2 priority: 1 param_1: TYPE=UP param_2: SCAN-STEP=0.35 param_3: SEARCH-SIZE=3 req_1: ONBOARD ACQUISITION FOR 6.09 ! linenum: 6.090 targname: HD44179 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1150-1608 num_exp: 1 time_per_exp: 250M s_to_n: 18 fluxnum_1: 7 priority: 1 param_1: STEP-PATT=DEF ! ! end of exposure logsheet scan_data: line_list: 6.00 fgs_scan: cont_dwell: D dwell_pnts: 3 dwell_secs: 0.03 scan_width: 0.0000 scan_length: 2.8000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: 1.4 wid_offset: 0.0 ! line_list: 6.01 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 0.03 scan_width: 0.7000 scan_length: 3.5000 sides_angle: 90.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 1.75 wid_offset: 0.35 ! line_list: 6.085 fgs_scan: cont_dwell: D dwell_pnts: 3 dwell_secs: 0.03 scan_width: 0.0000 scan_length: 2.8000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: 1.4 wid_offset: 0.0 ! line_list: 6.086 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 0.03 scan_width: 0.7000 scan_length: 3.5000 sides_angle: 90.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 1.75 wid_offset: 0.35 ! ! end of scan data