7326( 7) - 06/22/98 11:22 - [ 1] PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID: 7326 Version: 7 Check-in Date: 22-Jun-1998 11:20:04 1.Proposal Title: Coronagraphic, Polarimetric Imaging of T Tau with NICMOS ------------------------------------------------------------------------------------ 2. Proposal For 3. Cycle GO 7 ------------------------------------------------------------------------------------ 4. Investigators Contact? PI: David WEINTRAUB VANDERBILT UNIVERSITY CoI: Joel Kastner Massachusetts Institute of Technology N ------------------------------------------------------------------------------------ 5. Abstract Is the universe good at making planets? This question has motivated many infrared astronomy programs and is one research area in which NICMOS on HST will have an enormous, long lasting impact. Since recognizing that infrared excesses around T Tauri stars indicated the presence of preplanetary disks, we have wanted to better characterize these disks. We want to know how and how easily they form, how they interact with surrounding molecular clouds, how they feed the central stars, what disk lifetimes and masses are, and how disks survive and are impacted by the presence of stellar companions within ~100 AU. We propose to address many of these problems with a comprehensive NICMOS study of T Tau, the prototype for the entire class of T Tauri stars. T Tau has a circumstellar disk and an infrared companion less than 100 AU distant. In some ways, more is known about this disk than about any other disk around any other T Tauri star. Yet, because T Tau is so bright in the infrared, we know almost nothing about the system within ~4 arcsec of the central binary. Polarimetric, coronagraphic near-IR imaging with NICMOS is the most powerful means available with which to directly probe this inner region, which is arguable the most important and interesting region of the T Tau system. The proposed observations will yield direct indications of the structure of what is likely an example of a protoplanetary disk, and will provide insight into the relationship between this disk and the T Tau binary system. We also propose to obtain a suite of narrow- and broad-band direct images that will clarify the complicated way in which the binary interacts with Burnham's emission nebula, Hind's reflection nebula and the nearby Herbig-Haro objects. ------------------------------------------------------------------------------------ 7326( 7) - 06/22/98 11:22 - [ 2] Observations Description ------------------------ For T Tau, we will obtain unocculted multi-waveband images at high (NIC1), medium (NIC2) and low (NIC3) resolution and occulted images at medium resolution. We will obtain polarimetric images in occulted mode with NIC2 and in unocculted mode with NIC1, selected narrow band images with NIC1 and large scale maps with NIC3. We propose to obtain thermal background images for the filters in the 2 micron wavelength region and to collect polarimetric and coronagraphic calibration images of a single, A0V, photometric standard star. We note that these calibration images are absolutely essential for the accurate interpretation of the proposed polarimetric and polarimetric + coronagraphic data sets. Imaging with NIC2: Our primary goal is to use NIC2 to make coronagraphic, polarimetric images of the scattering nebula surrounding T Tau. The coronagraph blocks out a central region of 0.4 arcsec radius (7.5 times smaller than the coronagraph used in our ground based experiment) while T Tau and T Tau S are separated by 0.69 arcsec (at position angle 178 degrees). T Tau S is now eight times fainter than T Tau at K band and fainter still at shorter wavelengths (Simon et al. 1996). Therefore, in target acquisition mode with the coronagraph, NIC2 should have no problem in identifying T Tau as the brightest object in the field and placing it, rather than T Tau S, under the coronagraph. Thus, we will obtain polarimetric imaging information from a distance of 0.4 arcsec (55 AU) and beyond from T Tau and within the immediate environment of T Tau S. With 0.075 arcsec pixels, T Tau S will lie four pixels beyond the edge of the coronagraph. The experiment does not need to be done in the reverse manner (with T Tau S under the coronagraph) as T Tau S is ~2.2^m fainter than T Tau at K. The polarimetric maps will reveal which star, T Tau or T Tau S, illuminates the nebulosity in the immediate vicinity of each star. While we only can obtain coronagraphic, polarimetric images in the 1.9-2.1 microns band with NIC2, we also will obtain coronagraphic, unpolarized images of T Tau with NIC2 using the F160W filter (1.6 microns) in order to obtain high spatial resolution color and thereby extinction and column density information about the nebulosity. sectionDirect Imaging with NIC1 Polarimetric observations with the shorter-wavelength NIC1 (1 px = 0.043 arcsec) will be very valuable also, providing diffraction limited (0.095 arcsec at 1.1 microns) resolution data (barely 13 AU for T Tau). Even though there is no coronagraph available with NIC1, only 20 percent of the energy from a point source impacts the central pixel while the full energy in the PSF is distributed over almost 50 pixels. In addition, T Tau is nearly 2 magn fainter at J than at K and T Tau S is much fainter still. Finally, working in our favor is the polarimeter which reduces the light throughput by about half. We therefore expect to have great success in obtaining unocculted, polarimetric images without saturation at the highest available spatial resolution in the near-IR, using NIC1 and POLOS, POL120S and POL240S in the broad-band region centered at 1.1 microns. These images will provide polarimetric information to within 0.4 arcsec of T Tau, a region where we will be unable to observe using NIC2 and the coronagraph. Polarimetric images at two different wavebands (i.e. POLSH and POLNG) are necessary to obtain information about grain sizes. We also propose to obtain forbidden line, narrow-band images with NIC1 in the F095N, F097N (SIII and SIII continuum), F164N and F166N (Fe II and Fe II continuum) to measure the structure and location of jets in this system and to ascertain their relationship to other energetic phenomena in the region. sectionLarge Field Imaging with NIC3 With NIC3, we will obtain 130 arcsec x 130 arcsec (9-panel spiral dither) images through broad (F110W, F160W), medium (F240M) and narrow (F164N, F166N, F196N, F200N) band filters to observe the structure of the entire T Tau system, including Burnham's nebula and Hind's nebula. Making such a large map is impractical with either NIC1 or NIC2. In the past, some observers have claimed to have seen an emission bridge connecting T Tau to Hind's nebula and others have observed a jet from T Tau pointing toward the Herbig-Haro object found in Hind's nebula. The narrow-band images will provide a test of such a claim, in addition to providing details of the physics within Burnham's nebula, and testing claims for HH knots in the vicinity of both nebulae. In addition, the unprecedented clarity and resolution from HST are likely to reveal structure about the relationship between a forming star and the surrounding material in the molecular cloud heretofore unpredicted and unexpected. Orbit 1: After guide star acquisition, we will acquire the target star (NIC2-ACQ) T Tau and place it under the coronagraph (NIC2-CORON). We will then take two 100 s images with each of the filters POL0L, POL120L and POL240L. In 100 s, we can obtain good signal-to-noise ratios at flux levels of a few times 10^-2 Jy arcsec^-2. In addition, with the polarizing filters in place, we should not saturate even on T Tau S, in 100 s integrations. For T Tau, we were able to observe the polarized surface flux down to light levels down to about 10^-3 of the central intensity. This would be equivalent to K = 12-13^m arcsec^-2, or a few times 10^-2 Jy arcsec^-2. Thus, these integration times should permit us to image the faint polarized nebula out to at least 10 arcsec from the stars. By binning the data into a 1-D radial profile, we will increase our sensitivity in the radial profile study to nearly K = 20 arcsec^-2. Next, we will obtain two 100 s coronagraphic images with the F165W filter. Our limiting surface flux goals are similar with F165W, about 10^-2 Jy arcsec^-2; however, although T Tau is a little fainter at H, the unpolarized F160W filter transmits more photons than the POLNG filters so our integration times can remain unchanged. Then we will switch to NIC2 so that T Tau is no longer occulted but remains in the viewing area of NIC2; there, we will obtain 0.1 s images with each of these four filters (POL0L, POL120L, POL240L, F165W). These images will enable us to determine the intensity of the central sources (which are variable) at the epoch of the observations. These images are absolutely necessary for calibration of the target images to determine the level of scattered light in the system. As these observations are carried out at wavelengths where the thermal telescope background may be significant and variable, we next must obtain measurements of the thermal background during this same orbit. Therefore, we will next offset the telescope 120 arcsec north to a blank field and obtain a pair of 100 s integrations in each of the POL0L, POL120L, POL240L and F160W filters. Orbit 2: After guide star reacquisition and switching to NIC1 we will reobserve T Tau. Here, we seek to obtain polarimetric images at the shorter wavelengths with comparable limiting surface fluxes (10^-2 Jy arcsec^-2) as in the longer wavelength images. Thus, we propose to obtain two 100 s images with each of the filters POL0S, POL120S and POL240S. Following the polarimetric imaging, we will obtain 20 s narrow-band images with NIC1 in the SIII (F095N), SIII continuum (F097N), Fe II (F164N) and Fe II continuum (F166N) to study the jets in this system. As per the recommendation of the NICMOS manual (Chapter 10), we will plan to use general purpose background images constructed by the NICMOS team for background removal in these short wavelength images. We next will switch to NIC3 to map the region around T Tau using the 9- point SPIRAL-DITHER pattern. We will begin each pattern (position 1) at a point in the sky in between T Tau and Hind's Nebula so that these 9-point maps encompass all of the known reflection nebulosity which is primarily to the west of the star. Each image at each pattern point requires ~24 s (instrument set-up plus readout times) in addition to the designated integration time. During this orbit, we will cycle through the 9-pt map pattern once. At each map point, we will obtain 0.3 s images with each of three broad-band filters - F110W, F160W, 240W. Orbit 3: After guide star reacquisition, we will cycle through the 9- point map pattern a second time. During this SPIRAL-DITHER pattern, we will obtain 5 s maps with each of four narrow- band filters -- F164N, F166N and F212N and F215N -- at each map point. We will finish the observations of T Tau by offsetting again 120 arcsec north to obtain background observations in the F212N and F215N filters. Orbit 4: During this orbit we will obtain calibration images of an occulted standard star (HD 20149) with the same approximate H and K magnitudes as T Tau. This experiment must include coronagraphic images of a standard star well matched in IR brightness to T Tau at both wavebands at which we obtain occulted images of T Tau (F165W, POLNG) as well as polarimetric calibration images at POLNG and POLSH. After guide star acquisition with NIC2, we will place the standard star under the coronagraph and obtain two 100 s images with each of POL0L, POL120L, POL240L and two 100 s images with F165W. We will then remove the star from behind the coronagraph. Thence, we will obtain 0.1 s images with each of these four filters. Next, we will switch from NIC2 to NIC1, center the standard star in the field, and collect two 0.1 s images with each of the filters POL0S, POL120S and POL240S. (Note that the calibration standard is an A0V star; thus, it is a perfect match to T Tau at K band but will be significantly brighter -- and require less integration time -- than T Tau itself at J band.) Finally, we will switch back to NIC2 to obtain polarized, thermal background calibrations. The chosen order of Orbit 4 observations is designed to minimize target acquisition time to permit all these observations to be carried out in a single orbit. Real Time Justification ----------------------- None. Calibration Justification ------------------------- None. Additional Comments ------------------- None. ------------------------------------------------------------------------------------ 7326( 7) - 06/22/98 11:22 - [ 3] Data Distribution Media: DAT Blocking Factor: 10 Ship To: PI_Address Ship Via: Email: ------------------------------------------------------------------------------------ 7326( 7) - 06/22/98 11:22 - [ 4] TARGET LIST a) Fixed Targets ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial | Flux data No | Name | Description | Position |Eqnx | Vel. | ------------------------------------------------------------------------------------------------------------------------------------ 1 HD284419 STAR, T TAURI STAR RA=04H 21M 59.40S +/- 0.3", J2000 V = 9.60+/-1.0 DEC=19D 32' 7.5" +/- 0.3", PLATE K = 5.5+/-0.5 -ID=000P J = 7.5+/-0.5 H = 6.3+/-0.2 Comments: Note that the target is a binary star. The given coordinates are for T Tauri North (T Tau N). The companion, T Tau S, is found at 04h 21m 59.42s in RA and 19D 32' 6.4" in Dec, according to the GSC. 2 TTAU-BKG CALIBRATION, FLAT FIELD RA-OFF=0.0S+/- 1.0S, DEC- J2000 SURF-BKG(K) = 20+/-2 OFF=118"+/- 2", FROM 1 Comments: Ground-based NIR observations show that the region near T Tau, beyond about 1' north from the star, is very blank sky in the associated dark cloud. This background sky position is exactly 118 arcseconds directly north of T Tau. The position is arbitrary but nearby (within 2 arcmin) to minimize telescope overhead times. 3 HINDS-NEBULA ISM, HERBIG-HARO RA-OFF=-30"+/- 2", DEC-OFF=0"+/- J2000 V = 9.60+/-1.0 OBJECT, REFLECTION 1", FROM 1 K = 5.5+/-0.5 NEBULA J = 7.5+/-0.5 H = 6.3+/-0.2 Comments: Target 3 puts the approximate center of a dithered map, begun at this position, 30 arcsec west of T Tau, in between the star and the large reflection nebula located 30 to 60 arcsec west (smaller RA) of the star. Thus, our 25-position dithered maps made with NIC2 will be centered on T Tau in the Declination coordinate but will cover the range from 12 arcsec east to 72 arcsec west of T Tau, thereby enclosing almost all of the known IR reflection nebulosity. Fluxes are for T Tau which will be in some of the map fields. 7326( 7) - 06/22/98 11:22 - [ 5] Visit: 01 Visit Priority: Visit Requirements: DROP TO GYRO IF NECESSARY NO REACQ On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 40 HD284419 NIC2 MULTIAC NIC2 F212N SAMP-SEQ=SCAMRR,NSAMP=4, 1 DEF CUM PATTERN=XSTRIP-DITH,NUM-POS=5, DITH-SIZE=16.0,PATTERN-ORIENT=0 Comments: H2 "on-line" image ------------------------------------------------------------------------------------------------------------------------------------ 50 HD284419 NIC2 MULTIAC NIC2 F215N SAMP-SEQ=SCAMRR,NSAMP=4, 1 DEF CUM PATTERN=XSTRIP-DITH,NUM-POS=5, DITH-SIZE=16.0,PATTERN-ORIENT=0 Comments: H2 "off-line" image ------------------------------------------------------------------------------------------------------------------------------------ 70 HD284419 NIC2 MULTIAC NIC2 POL0L SAMP-SEQ=SCAMRR,NSAMP=3, 2 DEF CUM PATTERN=SPIRAL-DITH,NUM-POS=4, PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ, DITH-SIZE=1.5375 Comments: 1st in 3-image K-band polarimetric sequence. Note that we are not in danger of saturating in the 0.203 s exposures. K = 5.5, but some of this light may be diffuse nebulosity; in addition, only about 50% of this flux is trasnmitted through the polarizing filter so we expect a maximum point source brightness of 2 Jy. ------------------------------------------------------------------------------------------------------------------------------------ 80 HD284419 NIC2 MULTIAC NIC2 POL120L SAMP-SEQ=SCAMRR,NSAMP=3, 2 DEF CUM PATTERN=SPIRAL-DITH,NUM-POS=4, PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ, DITH-SIZE=1.5375 Comments: 2nd in 3-image K-band polarimetric sequence. ------------------------------------------------------------------------------------------------------------------------------------ 90 HD284419 NIC2 MULTIAC NIC2 POL240L SAMP-SEQ=SCAMRR,NSAMP=3, 2 DEF CUM PATTERN=SPIRAL-DITH,NUM-POS=4, PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ, DITH-SIZE=1.5375 Comments: Last in 3-image K-band polarimetric sequence ------------------------------------------------------------------------------------------------------------------------------------ 7326( 7) - 06/22/98 11:22 - [ 6] Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 100 TTAU-BKG NIC2 MULTIAC NIC2 POL0L SAMP-SEQ=SCAMRR,NSAMP=3, 2 DEF CUM PATTERN=SPIRAL-DITH,NUM-POS=4, PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ, DITH-SIZE=1.5375 Comments: 1st in 3-image polarimetric K-band bkgnd sequence. The DROP TO GYRO IF NECESSARY NO REACQ optional parameter for visit 1 is to encourage HST not to waste time setting up on a guide star for exposures 100, 110 and 120, which are polarized + thermal background exposures to calibrate the previous POLNG exposures. The expected small pointing drift of 0.001 arcsec per second is acceptable for these background measurements. ------------------------------------------------------------------------------------------------------------------------------------ 110 TTAU-BKG NIC2 MULTIAC NIC2 POL120L SAMP-SEQ=SCAMRR,NSAMP=3, 2 DEF CUM PATTERN=SPIRAL-DITH,NUM-POS=4, PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ, DITH-SIZE=1.5375 Comments: 2nd in 3-image polarimetric K-band bkgnd sequence. ------------------------------------------------------------------------------------------------------------------------------------ 120 TTAU-BKG NIC2 MULTIAC NIC2 POL240L SAMP-SEQ=SCAMRR,NSAMP=3, 2 DEF CUM PATTERN=SPIRAL-DITH,NUM-POS=4, PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ, DITH-SIZE=1.5375 Comments: Last in 3-image polarimetric K-band bkgnd sequence. ------------------------------------------------------------------------------------------------------------------------------------ 123 TTAU-BKG NIC2 MULTIAC NIC2 F205W PATTERN=SPIRAL-DITH,NUM-POS=4, 1 DEF CUM SAMP-SEQ=STEP2,NSAMP=6, DITH-SIZE=5.0,OFFSET=SAM-NO-REACQ Comments: These observations provide a thermal background measurement for the following mosaic. ------------------------------------------------------------------------------------------------------------------------------------ 126 HINDS-NEBUL NIC2 MULTIAC NIC2 F205W PATTERN=SPIRAL-DITH,NUM-POS=30, 1 DEF A CUM DITH-SIZE=16.0,SAMP-SEQ=STEP2, NSAMP=8 ------------------------------------------------------------------------------------------------------------------------------------ 7326( 7) - 06/22/98 11:22 - [ 7] Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 133 HINDS-NEBUL NIC2 MULTIAC NIC2 F110W PATTERN=SPIRAL-DITH,NUM-POS=30, 1 DEF A CUM DITH-SIZE=16.0,SAMP-SEQ=STEP2, NSAMP=8 Comments: There is a small risk that we may saturate a few pixels near the stellar position. This will only happen if the J-band emission emerges almost entirely from a point source; we expect that this is highly unlikely to be the case. Nevertheless, our goal here is quality measurements of a large field of view with low surface brightness. ------------------------------------------------------------------------------------------------------------------------------------ 136 HINDS-NEBUL NIC2 MULTIAC NIC2 F160W PATTERN=SPIRAL-DITH,NUM-POS=30, 1 DEF A CUM DITH-SIZE=16.0,SAMP-SEQ=STEP2, NSAMP=7 ------------------------------------------------------------------------------------------------------------------------------------ 140 HD284419 NIC1 MULTIAC NIC1 POL0S SAMP-SEQ=SCAMRR,NSAMP=8, 3 DEF CUM PATTERN=SPIRAL-DITH,NUM-POS=4, PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ, DITH-SIZE=1.5375 Comments: 1st in 3-image polarimetric J-band sequence. We expect that the brightest single pixel will contain no more than 10% of the integrated light from the star and surrounding nebula. Thus, conservatively, we estimate that saturation might occur after about 20 s so we have picked an integration time below 20 s. ------------------------------------------------------------------------------------------------------------------------------------ 150 HD284419 NIC1 MULTIAC NIC1 POL120S SAMP-SEQ=SCAMRR,NSAMP=8, 3 DEF CUM PATTERN=SPIRAL-DITH,NUM-POS=4, PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ, DITH-SIZE=1.5375 Comments: 2nd in 3-image polarimetric J-band sequence. ------------------------------------------------------------------------------------------------------------------------------------ 160 HD284419 NIC1 MULTIAC NIC1 POL240S SAMP-SEQ=SCAMRR,NSAMP=8, 3 DEF CUM PATTERN=SPIRAL-DITH,NUM-POS=4, PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ, DITH-SIZE=1.5375 Comments: Last in 3-image polarimetric J-band sequence. ------------------------------------------------------------------------------------------------------------------------------------ 170 HD284419 NIC1 MULTIAC NIC1 F095N SAMP-SEQ=STEP1,NSAMP=15, 2 DEF CUM PATTERN=TWO-CHOP,NUM-POS=2, CHOP-SIZE=1,PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ Comments: S II "on line" image ------------------------------------------------------------------------------------------------------------------------------------ 7326( 7) - 06/22/98 11:22 - [ 8] Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 180 HD284419 NIC1 MULTIAC NIC1 F097N SAMP-SEQ=STEP1,NSAMP=10, 2 DEF CUM PATTERN=TWO-CHOP,NUM-POS=2, CHOP-SIZE=1,PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ Comments: S II "off line" image ------------------------------------------------------------------------------------------------------------------------------------ 190 HD284419 NIC1 MULTIAC NIC1 F164N SAMP-SEQ=STEP1,NSAMP=7, 2 DEF CUM PATTERN=TWO-CHOP,NUM-POS=2, CHOP-SIZE=1,PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ Comments: Fe II "on line" image ------------------------------------------------------------------------------------------------------------------------------------ 200 HD284419 NIC1 MULTIAC NIC1 F166N SAMP-SEQ=STEP1,NSAMP=7, 2 DEF CUM PATTERN=TWO-CHOP,NUM-POS=2, CHOP-SIZE=1,PATTERN-ORIENT=0, OFFSET=SAM-NO-REACQ Comments: Fe II "off line" image ------------------------------------------------------------------------------------------------------------------------------------ 7326( 7) - 06/22/98 11:22 - [ 9] Summary Form for Proposal 7326 Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Apertures NIC2 NIC1 ------------------------------------------------------------------------------------------------------------------------------------ Configurations NIC2 NIC1 ------------------------------------------------------------------------------------------------------------------------------------ Opmodes MULTIACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters SAMP-SEQ=SCAMRR NSAMP=4 PATTERN=XSTRIP-DITH NUM-POS=5 DITH-SIZE=16.0 PATTERN-ORIENT=0 DITH-SIZE=1.5375 OFFSET=SAM-NO-REACQ NUM-POS=4 PATTERN=SPIRAL-DITH NSAMP=3 DITH-SIZE=5.0 NSAMP=8 SAMP-SEQ=STEP2 NSAMP=7 CHOP-SIZE=1 NUM-POS=2 PATTERN=TWO-CHOP SAMP-SEQ=STEP1 ------------------------------------------------------------------------------------------------------------------------------------ Proposal Category GO ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements DROP TO GYRO IF NECESSARY NO REACQ ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F212N F215N POL0L POL120L POL240L F205W F110W F160W POL0S POL120S POL240S F095N F097N F164N F166N ------------------------------------------------------------------------------------------------------------------------------------ Target Names HD284419 TTAU-BKG HINDS-NEBULA ------------------------------------------------------------------------------------------------------------------------------------