! $Id: 5504,v 4.1 1994/07/27 18:43:43 pepsa Exp $ coverpage: title_1: STRUCTURE OF HERBIG-HARO JETS FROM NEWBORN STARS: CYCLE4HIGH sci_cat: INTERSTELLAR MEDIUM sci_subcat: HH OBJECTS proposal_for: GO pi_fname: BO pi_lname: REIPURTH pi_inst: EUROPEAN SOUTHERN OBSERVATORY pi_country: CHILE pi_phone: 56-2-2285006 hours_pri: 18.80 num_pri: 2 wf_pc: Y ! end of coverpage abstract: line_1: Herbig-Haro jets have in recent years been subject to intense study, line_2: and it is now clear that they are an integral part of the star line_3: formation process and provide insights into the very earliest stages line_4: of stellar evolution. We propose to study two of the finest known HH line_5: jets, HH 111 and HH 47, using HST with WFPC2 and interference filters. line_6: Analytical and numerical models of HH jets have reached a high degree line_7: of sophistication, but further progress is blocked until it is line_8: established whether the observed structure of jets is formed through line_9: Kelvin-Helmholtz instabilities or time-variability in the wind from line_10: the driving source. The two competing models make definite predictions line_11: about the morphology and excitation pattern within the jet knots which line_12: can be tested with high resolution interference filter images. The line_13: very best ground-based images taken in 0.6"-0.7" seeing and line_14: deconvolved to 0.4" show tantalizing structure, but not definite line_15: enough to firmly choose between the two models. Only HST observations line_16: can provide the required resolution. ! ! end of abstract general_form_proposers: lname: REIPURTH fname: BO inst: 4740 country: CHILE esa: Y ! lname: HEATHCOTE fname: STEVE inst: 4720 country: CHILE ! lname: SCHWARTZ fname: RICHARD mi: D inst: 2750 country: USA ! lname: BALLY fname: JOHN inst: 1760 country: USA ! lname: MORSE fname: JON inst: 3470 country: USA ! lname: HARTIGAN fname: PATRICK inst: 2001 country: USA ! lname: STONE fname: JAMES mi: M inst: 2620 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We are going to observe two Herbig-Haro jets, HH111 and HH47, each of them line_2: through two narrow band filters - H-ALPHA (F656N) and [SII] (F673N). line_4: The objects are faint, so we have long exposures (HH111: 16100sec and line_5: HH47: 11850sec through each filter). These must obviously be broken up line_6: into several sub-exposures, because of orbital constraints. To minimize line_7: read-out noise (and overheads) we wish these sub-exposures to be as long line_8: as possible. Since we will have enough sub-exposures to filter out line_9: cosmic ray hits, we do not want to further sub-divide them and hence have line_10: set CR-SPLIT=NO. line_12: The objects are extended, and so there are certain constraints on the roll line_13: angle of the spacecraft in order to fit the objects into the CCD field. line_14: However, there are several alternate choices of placement, each with an line_15: accompanying range of roll angle. One case has been entered in the line_16: exposure logsheet; the other choices are given in comments. Any of them line_17: can be used if this simplifies scheduling. line_19: The objects have very high proper motions (up to 0.2'' per year) and in line_20: order to be able to compare the H-ALPHA and [SII] images of each object, line_21: these two images must be obtained within a certain relatively short line_22: interval (2 weeks). Because of the possible influence of proper motion, line_23: the interpretation of the data requires that the [SII] images are taken ! question: 3 section: 2 line_1: before the H-ALPHA images. The observations of the two objects are line_2: completely independent and can be carried out in any order. ! question: 4 section: 1 line_1: As demonstrated in detail in our Phase I proposal, the possibilities for line_2: study via groundbased observations have been exhausted for the two jets line_3: to be examined here. These jets are among the first HH jets known, and line_4: their study will permit us to settle a major current question in HH jet line_5: research, namely whether the knots represent internal working surfaces or line_6: arise as the result of flow instabilities. The observations will also line_7: elucidate the role of entrainment for the flow dynamics along the body of line_8: the jet. Finally, the high spatial resolution of HST will allow the first line_9: detailed study of the working surfaces, where the jets interact with the line_10: ambient medium. The filters we have selected have been shown to allow one line_11: to separate emission due to the bow shock from that arisong in the Mach line_12: disk. ! question: 5 section: 1 line_1: Each of the two 16100sec exposures for HH111 and each of the two 11850sec line_2: exposures for HH47 need to be broken up into shorter sub-exposures to fit line_3: into an orbit. The exposure times listed here are merely suggestions, line_4: since we do not know what are the longest possible exposures that fit line_5: into an orbit for each object. It is not essential that the sub-exposures line_6: are all of exactly the same duration. Because of the high proper line_7: motion of the objects it is essential that once the observations of an line_8: object have started then they are completed (in both filters) within a line_9: 2 week period. If this is impossible then please contact us. line_11: Because the objects are extended and just fit into the WF field there line_12: are constraints on the acceptable roll angles of the spacecraft which will line_13: allow us to observe the entire objects. The orient/aperture values given line_14: in the exposure form are only one set of several possible combinations, line_15: which we list below. Basically, out of the possible 360 degrees, there line_16: is a roughly 35 degree ``window'' every 90 degrees for which each jet line_17: will fit into a specific WF CCD (or combination of CCDs). Once the roll line_18: angle of the spacecraft is known for a given observation, the information line_19: below tells which CCD the nominal jet center should be placed in. If line_20: these requirements make the scheduling too difficult, please contact us line_21: and we will then diminish the scope of the observations by observing only line_22: parts of the jets. ! question: 5 section: 2 line_1: NOTE: If for some reason the PI cannot be reached, please contact Steve line_2: Heathcote. Also please note that Jon Morse is working at STScI. ! question: 6 section: 1 line_1: None. All we require is the standard calibration data. ! ! question: 8 section: 1 line_1: We have performed astrometry of our targets and know the positions of line_2: individual knots to within one arcsecond on the HST GSC system. ! question: 9 section: 1 line_1: R.D.Schwartz was PI on GO 2243 ``The Shock Wave Structure of Herbig-Haro line_2: Objects''. These previous observations focused on much larger and much line_3: brighter knots in a major fragmenting bow shock. We are here concerned line_4: with knots in the body of a jet with an entirely different shock line_5: structure. All the previous data are analyzed and a paper has appeared': line_7: R.D.Schwartz et al: line_8: ``Hubble Space Telescope Imaging of Herbig-Haro Object No.2'' line_9: Astron.J. 106, 740, 1993 ! question: 10 section: 1 line_1: All of us have full time positions at our institutes. We are well equipped line_2: with SUN workstations and have MIDAS and IRAF software at our disposal. We line_3: have many years of experience in reducing and analyzing the best existing line_4: similar data from the ground. ! !end of general form text general_form_address: lname: REIPURTH fname: BO category: PI inst: 4740 addr_1: EUROPEAN SOUTHERN OBSERVATORY addr_2: CASILLA 19001 city: SANTIAGO 19 country: CHILE phone: 56-2-2285006 telex: reipurth@eso.org ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HH111 descr_1: G,501,514,907,922,929 pos_1: RA = 5H 49M 06.4S +/- 1", pos_2: DEC = +02D 47' 52" +/- 1", pos_3: PLATE-ID = 0084 equinox: B1950 pos_epoch_bj: B pos_epoch_yr: 1992.00 ra_pm_val: -0.010000 dec_pm_val: 0.0100 rv_or_z: V = +27 comment_1: THE FLUX DATA IS FOR KNOT L. WE comment_2: GIVE THE EXPECTED MAXIMUM SURFACE comment_3: BRIGHTNESS IN THE KNOT. THE comment_4: SYSTEM CONTAINS MANY KNOTS A FEW comment_5: BRIGHTER THAN THIS, BUT MANY UP comment_6: TO AN ORDER OF MAGNITUDE FAINTER. comment_7: THE FLUXES GIVEN FOR 6731 ARE comment_8: ACTUALLY THE SUM OF THE FLUXES FOR comment_9: THE TWO MEMBERS OF THE 6717,31 comment_10: DOUBLET. fluxnum_1: 1 fluxval_1: SURF-LINE(6731) = 2.9 +/- 0.3 E-15 fluxnum_2: 2 fluxval_2: W-LINE(6731) = 1.8 +/- 0.1 fluxnum_3: 3 fluxval_3: SURF-LINE(6563) = 2.7 +/- 0.3 E-15 fluxnum_4: 4 fluxval_4: W-LINE(6563) = 2.2 +/- 0.1 ! targnum: 2 name_1: HH47 name_2: HH46/47 descr_1: G,501,514,907,922,929 pos_1: RA = 8H 24M 19.9S +/- 1", pos_2: DEC = -50D 50' 19" +/- 1", pos_3: PLATE-ID = 00AI equinox: B1950 pos_epoch_bj: B pos_epoch_yr: 1992.00 ra_pm_val: 0.005000 dec_pm_val: 0.0400 rv_or_z: V = +22 comment_1: THE FLUX DATA IS FOR KNOT B. WE comment_2: GIVE THE EXPECTED MAXIMUM SURFACE comment_3: BRIGHTNESS IN THE KNOT. THE comment_4: SYSTEM CONTAINS MANY KNOTS A FEW comment_5: BRIGHTER THAN THIS, BUT MANY UP comment_6: TO AN ORDER OF MAGNITUDE FAINTER. comment_7: THE FLUXES GIVEN FOR 6731 ARE comment_8: ACTUALLY THE SUM OF THE FLUXES FOR comment_9: THE TWO MEMBERS OF THE 6717,31 comment_10: DOUBLET. fluxnum_1: 1 fluxval_1: SURF-LINE(6731) = 1.7 +/- 0.3 E-15 fluxnum_2: 2 fluxval_2: W-LINE(6731) = 1.1 +/- 0.1 fluxnum_3: 3 fluxval_3: SURF-LINE(6563) = 6.8 +/- 0.3 E-16 fluxnum_4: 4 fluxval_4: W-LINE(6563) = 1.9 +/- 0.1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HH111 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F673N wavelength: 6732 num_exp: 1 time_per_exp: 9200S s_to_n: 30 s_to_n_time: 16100S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 4; req_2: SEQ 1-2.5 WITHIN 14D; req_3: ORIENT 322D +/- 17D / 1-2.5; req_4: SAME POS FOR 1.5-2.5 AS 1 comment_1: S/N IS FOR SUM OF 7 X 2300S EXPS. comment_2: FOLLOWING ALSO ACCEPTABLE FOR 1-2.5 comment_3: ORIENT 232D +/- 17D, APERTURE WF3-FIX comment_4: ORIENT 142D +/- 17D, APERTURE WF4-FIX comment_5: ORIENT 52D +/- 17D, APERTURE WF2-FIX comment_6: PA OF THE HH111 JET IS 277D ! linenum: 1.500 targname: HH111 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F673N wavelength: 6732 num_exp: 1 time_per_exp: 6800S s_to_n: 30 s_to_n_time: 16100S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 4; comment_1: S/N IS FOR SUM OF 7 X 2300S EXPS. comment_2: FOLLOWING ALSO ACCEPTABLE FOR 1-2.5 comment_3: ORIENT 232D +/- 17D, APERTURE WF3-FIX comment_4: ORIENT 142D +/- 17D, APERTURE WF4-FIX comment_5: ORIENT 52D +/- 17D, APERTURE WF2-FIX comment_6: PA OF THE HH111 JET IS 277D ! linenum: 2.000 targname: HH111 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F656N wavelength: 6562 num_exp: 1 time_per_exp: 9200S s_to_n: 33 s_to_n_time: 16100S fluxnum_1: 3 fluxnum_2: 4 priority: 2 param_1: CR-SPLIT = NO req_1: CYCLE 4; comment_1: S/N IS FOR SUM OF 7 X 2300 EXPS. comment_2: THE SAME ORIENT/APERTURE PAIR CHOSEN comment_3: FOR LINENUM 1 MUST BE USED FOR comment_4: LINENUMS 1.5-2.5. ! linenum: 2.500 targname: HH111 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F656N wavelength: 6562 num_exp: 1 time_per_exp: 6800S s_to_n: 33 s_to_n_time: 16100S fluxnum_1: 3 fluxnum_2: 4 priority: 2 param_1: CR-SPLIT = NO req_1: CYCLE 4; comment_1: S/N IS FOR SUM OF 7 X 2300 EXPS. comment_2: THE SAME ORIENT/APERTURE PAIR CHOSEN comment_3: FOR LINENUM 1 MUST BE USED FOR comment_4: LINENUMS 1.5-2.5. ! linenum: 3.000 targname: HH47 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F673N wavelength: 6732 num_exp: 1 time_per_exp: 11900S s_to_n: 13 s_to_n_time: 12000S fluxnum_1: 1 fluxnum_2: 2 priority: 3 param_1: CR-SPLIT = NO req_1: CYCLE 4; req_2: SEQ 3-4 WITHIN 14D; req_3: ORIENT 53D +/- 19D / 3-4; req_4: SAME POS FOR 4 AS 3 comment_1: S/N IS FOR SUM OF 4 X 3000S EXPS. comment_2: FOLLOWING ALSO ACCEPTABLE FOR 3-4 comment_3: ORIENT 143D +/- 19D, APERTURE WF2-FIX comment_4: ORIENT 323D +/- 19D, APERTURE WF4-FIX comment_5: ORIENT 233D +/- 19D, APERTURE WF3-FIX comment_6: PA OF THE HH47 JET IS 53D. ! linenum: 4.000 targname: HH47 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F656N wavelength: 6562 num_exp: 1 time_per_exp: 11900S s_to_n: 14 s_to_n_time: 12000S fluxnum_1: 3 fluxnum_2: 4 priority: 4 param_1: CR-SPLIT = NO req_1: CYCLE 4; req_2: SEQ 3-4 WITHIN 14D; req_3: ORIENT 53D +/- 19D / 3-4; req_4: SAME POS FOR 4 AS 3 comment_1: S/N IS FOR SUM OF 4 X 2500S EXPS. comment_2: THE SAME ORIENT/APERTURE PAIR CHOSEN comment_3: FOR LINENUM 3 MUST BE USED FOR comment_4: LINENUM 4. ! ! end of exposure logsheet ! No scan data records found