0 Assigned ID: 1079 ----- Attempting Submission 1 (Tue Feb 26 07:58:24 GMT 2013) ----- HST Phase I Proposal 1079 (cyc21-HH1-2_APT.pdf.apt) successfully submitted. ----- Attempting Submission 2 (Tue Feb 26 08:04:31 GMT 2013) ----- HST Phase I Proposal 1079 (cyc21-HH1-2_APT.pdf.apt) successfully submitted. ----- Attempting Submission 3 (Wed Feb 27 06:47:36 GMT 2013) ----- Added an optional parameter of FLASH=10 to all exposures for post-flash -743730845 ----- Attempting Submission 1 (Wed Jun 19 20:16:46 GMT 2013) ----- HST Phase II Proposal 13484 (prop13484_HH12.apt) successfully submitted. ----- Attempting Submission 2 (Wed Jun 19 20:19:03 GMT 2013) ----- HST Phase II Proposal 13484 (prop13484_HH12.apt) successfully submitted. ----- Attempting Submission 3 (Thu Jun 20 01:22:57 GMT 2013) ----- HST Phase II Proposal 13484 (prop13484_HH12.apt) successfully submitted. ----- Attempting Submission 4 (Fri Jun 21 03:59:16 GMT 2013) ----- HST Phase II Proposal 13484 (prop13484_HH12.apt) successfully submitted. ----- Attempting Submission 5 (Sat Jun 22 02:44:37 GMT 2013) ----- ----- Attempting Submission 6 (Fri Aug 30 21:35:40 GMT 2013) ----- Structure, Excitation, and Evolution of Shocks: A Multi- Wavelength Study of Herbig-Haro 1/2 More than 1000 Herbig-Haro (HH) objects are known today. Among these, HH 1 and HH 2 are taking a special place because they remain the brightest known HH objects in the sky. As such, they have been studied at all wavelengths, from X-rays to the radio continuum, and with all observing techniques. Adding to this their fine bipolar morphology displaying two major bow shocks and a finely collimated jet, it is no surprise that HH 1 and 2 constitute the reference frame against which data on all other HH objects are compared. We propose to observe HH 1/2 with the following narrowband filters (in order of wavelength) offered by WFC3: [Ne IV] 2425, Mg II 2795+2802, [O II] 3726+28, H-beta 4861, [O III] 5007, [O I] 6300, H-alpha 6563, [S II] 6717, and [S II] 6731. These lines probe different shock velocities and physical parameters, hence the analysis of the resulting images allow us to explore a number of scientific questions related to the physical conditions in the shocks, their structure and their kinematics. We have at our disposal the sophisticated adaptive grid code "yguazu'' in which the gasdynamic equations are integrated together with a many-species ionization network. This allows us to compute both 2D and full 3D models of HH flows from which we can directly obtain predictions of emission maps in all of the above transitions, aiding the interpretation of the line ratio maps. The resulting study will provide a major step forward in our understanding of the shock physics of outflows from young stars. Note: We have received permission to change the three quad filters ([Ne IV] 2425, [S II] 6717, [S II] 6731) and instead add 1 orbit to MgII and 1 orbit to [OII] to improve S/N. HH 1/2 are the two brightest HH objects in the sky, which permits us to study them in these transitions at a much more limited number of orbits than other HH flows. However, our previous HST images have documented that the emission knots span a large range in flux in H alpha and [SII], from the brightest knots to faint diffuse emission at the detection limit. As an example, the S/N ratio in our 1 orbit (3x800 sec) H alpha WFPC2 images for the brightest pixel in HH 2 is 10^4, and in HH 1 it is >10^2. WFC3 has a smaller pixel scale, but a higher throughput, so WFC3 would have a signal that is ((0.04''/pix)/(0.10''/pix))^2 x (22%/11%) = 0.32 smaller in an equivalent exposure time. This difference is insignificant compared to the large range of flux ratios from knot to knot, so we retain 1 orbit for the H alpha filter. The Halpha/[SII] ratio is ~4.5 for the brightest parts in HH 2, but drops below 1 (with a lowest value of 0.25) over most of the remaining shock regions, while for HH 1 the Halpha/[SII] ratio is ~3.5, and again at or below 1 for the remaining structures of the object. Hence, 1 orbit will provide a similar good S/N ratio as our WFPC2 images. The new, so far unobserved transitions are, based on optical/ultraviolet spectra integrating across much of HH 1/2, from a factor of a few to more than a factor 10 fainter than Halpha, but since they probe very different shock regions, the line ratios change widely across the two objects. Based on the very limited available information, we have decided to also use one orbit for each of these filters, accepting that there may be filters in which only the brighter knots will have sufficient S/N to allow a proper analysis. We are allocated 9 orbits of WFC3 UVIS imaging for this project and we group the observations into 3 visits. In the first visit we use two orbits in F373N ([OII] 3726/3728) filter, and one orbit each in F502N ([OIII] 5007) and F631N ([OI] 6300). The [OII] orbits use a 4-point dithering in two orbits; the [OIII] and [OI] orbits use a 2-point dithering. In the second visit we use one orbit each for filters F656N (H alpha 6563), F487N (H beta 4861), and F673N ([SII] 6717/6731), each with a 2-point dithering. In the third visit the filter F280N (Mg II 2795/2802) and a 4-point dithering is used for two orbits. All observations have the same central pointing. The total extent of the HH 1-2 bipolar flow is 172'', matched to the WFC3 diagonal of 229''. We would like these 3 visits observed as close together as possible, not exceeding a month in interval. This is important due to the significant tangential motion of the objects, so the closer in time the visits can be made, the better. RESOLVED STAR FORMATION Default false false false false false SUPPORTED ISM HERBIG-HARO OBJECT The target Herbig-Haro Object HH 1-2 contains bright knots and diffuse emission. 17.38 is the V-magnitude of the Cohen-Schwartz Star in the field. J2000 J2000 WFC3/UVIS Imaging No No FQ243N WFC3/UVIS Imaging No No F280N WFC3/UVIS Imaging No No F373N WFC3/UVIS Imaging No No F487N WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F631N WFC3/UVIS Imaging No No FQ672N WFC3/UVIS Imaging No No FQ674N WFC3/UVIS Imaging No No F656N POS-TARG DITHER DITHER 4 2.414 WFC3-UVIS-DITHER-BOX false 81.785 true 0.112 0.173 2 85.759 POS-TARG WFC3-UVIS-GAP-LINE 23.884 1 false POS-TARG DITHER 3.633 LINE 2.352 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 2 false /private/var/folders/6G/6GkLnHqREralVgHdgtc7Ek+++TQ/-Tmp-/OPVisit8650933254971186626.xml Timing link suitability includes constraints ([Group (01 03 04) Within 30.0 days]) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 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