Assigned ID: 138
----- Attempting Submission 1 (Thu Feb 24 08:51:43 GMT 2011) -----Nolan and Alison et al. -- This resubmission corrects some inconsistancies in the submission of 10/10/2011 regarding the offset stasr QCQs between the CCD spectra and UV-MAMA spectra visits which Nolan discovered a few days ago. All star ACQs for the 9 objects and visit pairs not yet observed have been double-checked and made identical between the visit "pairs" for each nebula. The slit position angles and stated ORIENTS have further been checked and found to be A-OK from the previous submission. No coordinate changes or slit paraments have been done relative to the 10/10/2011 template. Only few seconds of time changes in the first orbit exposures of the UV-MAMA visits in a few cases resulted from the ACQ exposure time adjustments. Therefore, scheduling should be as previously done for the 10/10/2011 tmeplate (I hope). Apologies for the errors in the previous submission. (Reggie Dufour)
NOTES ON NEWEST RESUBMISSION (2/9/2012): Paired CCD-UVMAMA visits for same target GROUPED within 10days to insure the two visits are done within the same visibilty windows as per the PC's recommendation.
NEW 5 MARCH 2012: ADDED AN ORBIT 32 TO REDO THE VISIT 31 NUV-MAMA ACQ FAILURE AS APPROVED WITH A HOPR----- Attempting Submission 1 (Fri Jul 08 15:20:29 GMT 2011) -----
HST Phase II Proposal 12600 (gpneapt2f.apt) successfully submitted.
----- Attempting Submission 3 (Mon Oct 10 15:10:14 GMT 2011) -----
----- Attempting Submission 4 (Mon Dec 12 16:38:11 GMT 2011) -----
----- Attempting Submission 5 (Wed Jan 25 05:35:53 GMT 2012) -----
----- Attempting Submission 6 (Thu Feb 09 13:54:55 GMT 2012) -----
----- Attempting Submission 7 (Mon Mar 05 22:46:15 GMT 2012) -----Carbon and Nitrogen Enrichment Patterns in Planetary NebulaeThe goal of this project is to assess the role played in carbon production by low and intermediate mass stars (LIMS), i.e. the progenitors of planetary nebulae (PNe). One of the most pressing problems in galactic chemical evolution today is understanding the relative roles of LIMS (1-8 M_sun) versus massive stars (8-120 M_sun) in affecting the cosmic level of the element C. We are launching a fresh, ambitious project whose purpose is to employ STIS to obtain UV spectra of unprecedented-quality of 10 carefully chosen, bright solar metallicity PNe spanning a broad range in progenitor mass. Line strength measurements of important emission lines of C, N, and O such as OIII] 1660-6, NIII] 1747-54, CIII] 1907-9, and (when He++ is strong) CIV] 1550 and OIV] 1400 in each object will be used along with our own in-house abundance software to determine ion and element abundances for these three species. In turn, these results will be used to assess stellar yields (productivity rates) available in the literature. Favored yield sets will be used to calculate our own chemical evolution models in order to assess directly the importance of intermediate-mass stars in the cosmic evolution of C.SPECIAL GO 12600 APT PHASE II TEMPLATE UPDATE ON 24 JANUARY 2012
(FROM PREV TEMPLATE 10/10/11)
It was discovered there were some inconsistances between the CCD visit ACQ's and the connected UV-MAMA visit ACQ's due to changes in the objects and slit positions of the 10 October 2011 resubmitted template (due to safety issues). This submission corrects these such that the offset star ACQ's are identical between the CCD spectra and UV-MAMA spectra visits.
All coordinates for the offset stars and slit positions and ORIENTS are not changed from the 10/10/11 template, nor are slit widths (some minor exposure changes in the UV-MAMA first orbit visits due to offset star ACQ exposures (< 10 sec) so no review of previous UV-MAMA safety issues seem warranted.
To reiterate: No coordinate or slit offsets and position angles from previous template were made.
------------------------
SCIENCE REQUIREMENTS -- Our major science goals are predicated on obtaining accurate CNO abundances in the PNe from UV lines of ions not observable from the ground: C:N:O ≈ (C^+ + C^2+ + C^3+): (N^+ + N^2+ + N^3+): (O^+ + O^2+ + O^3+) where most of the ions of C & N have only strong lines in the UV. Therefore, the determination of accurate CNO abundances in PNe requires UV and optical spectrophotometry obtained using ratios of emission lines from identical spatial sampling of locations in the nebulae. Specifically, the most important UV lines are: carbon – C II] 2323–2329Å multiplet, C III] 1907+1909Å (density sensitive) doublet, & C IV 1548+1550Å doublet; nitrogen – N III] 1747–1750Å multiplet; N IV] 1483+1486Å doublet; NV 1239+1243Å doublet; oxygen – [O II] 2470Å, O III] 1661+1666Å doublet & O IV 1398+1407Å doublet. The ~20 necessary optical lines are standard and not listed here. The ensemble of these lines not only provides information on their corresponding ionic abundances, but also provides new electron temperature and density diagnostics {e.g., [O III] (1661+6)/(4959+ 5007)Å, [Ne III] 1815/3869Å, [O II] 2470/3727Å, C III] 1907/1909Å, [Ne V] 1575/3426Å, [Ar III] 3109/7136Å, etc.}. Note that many of these temperature and density diagnostic ratios require cospatial UV and optical spectra, which our observation plan gives special attention to ensuring. Note also that these would be the first precisely co-spatial UV-optical longslit spectra of Galactic PNe ever made. This will permit new science such as investigating spatial variations in CN abundances from UV-optical lines derived using traditional techniques for varying ionization regions across the slit.
Our target list consists of ten PNe spanning a large range of N/O abundances, but all with near-solar O/H (N/O varies by two orders of magnitude in our sample: from 0.026 for IC 3568 to 7.2 for NGC 6537). They are among the largest and brightest PNe that satisfy these abundance criteria (among ~100 considered). Most have some IUE observations, and all but PB6 (due to its small apparent size) and NGC 6778 have HST WFPC2 imagery, which is important for determining slit placement to maximize data quality.
OBSERVATIONAL AND PLANNING CONSIDERATIONS -- STIS Configurations and Visits -- majority of our target PNe are quite extended in size, for which the longslit capability of STIS (up to 25″ long for the UVMAMAs and 52″ long for the optical-CCD spectra) can be used to great advantage. For most nebulae, we propose observations across three orbits in two visits. The first one-orbit visit will consist of observations with the CCD for offset star acquisition (in most cases the central star of the PN) and then slit placement, followed by (triple) spectra with the G430L, G430M/4451, G750L, & G750M/6581 configurations. The second visit of (usually) two orbits consists of a "duplicate" CCD star ACQ and then offset to the (identical!) slit placement with the CCD visit and maximum (paired) exposures with the FUV/MAMA detector using the G140L grating. The next orbit will be a simple reacquisition followed by NUV/MAMA (paired) spectra taken with the G230L & G230M/1884 gratings. The G…M spectra are intended to resolve important diagnostic lines: 1907/9 C III], Hγ /4363[O III], & Hα/[Ν ΙΙ] triplet, which are blended with the low dispersion (L-grating) spectra. In order to have the desired spectral coverage and resolution with a co-spatial slit we choose the 0.2″ wide slit for the G…L spectra but with the 0.5" wide slit for the G...M spectra to increase throughput.
Using archival IUE UV spectra and (mostly our own) optical spectra, we did S/N calculations of emission lines in several of the PNe with the STIS ETC (two examples, PB6 & NGC 3242 are given in detail in the Phase I proposal) and we found that we can get good S/N and adequate spectral resolution (particularly in the UV) using the 0.2″ slit (as compared to the 0.5″ or 2.0″) with the G…L gratings. We also found that, when higher spectral resolution is needed to separate important emission line groups, using a wider 0.5″ slit with the G…M gratings is optimal given the tradeoff between increased photon input and spectral resolution degradation by the slit width without sacrificing significant spatial resolution. Specifically, we calculate that the average emission line resolution (FWHM) with the 0.2″ wide slit will be ~5Å with G140L, ~12Å with G230L, ~21Å with G430L, and ~39Å with G750L for an extended source which fills the slit. Similarly, for our M grating settings with the 0.5″ wide slit, the corresponding line FWHM are ~1.8Å for G230M/1884 (just resolving the C III] 1907/9Å doublet), ~5.6Å for G430M/4451 (resolving Hγ 4340Å from [O III] 4363Å), and ~11Å for G750M/6581 (resolving the Hα-[N II] triplet and density-sensitive [S II] doublet).
For the development of the Phase II observation template here, we studied WFPC2 imagery of eight of the PNe with HLA, Aladin, and SIMBAD to determine accurate ICRS coordinates of the relatively bright (V ~ 10-13 mag in most cases) central stars and determined CCD ACQ exposure times using the STIS ETC (in all cases the ETC# is given for reference). For several cases, the central stars were so bright as to necessitate using the F25ND3 filter to attenuate the light for an optimum CCD/ACQ exposure of ~1-10 seconds. For four of the PNe: NGC 5315, NGC 6778, PB6, & NGC 6537, the central stars are faint and we used a nearby V ~14 star to do the initial CCD/ACQ then offset to the nebula position. The ORIENT values (or ranges) were determined from WFPC2 or ground-based images of the nebulae within the observational windows for each nebula revealed by the Phase II APT. In most cases, we adjusted the ORIENTs such that at least one, and sometimes more, 7-10 day observation windows were schedulable during the Cycle 19 period. In all cases we avoid the central stars of the PNe to be safe with the MAMA detectors. Moreover, in addition to our inspection of previous STIS-MAMA spectra of PNe (particularly for NGC 7009, which is a high surface brightness PN), we ran STIS ETC calculations (based on the NGC 7009 UV-optical spectrum in the ETC) for the strongest lines expected in each of the grating passbands to check MAMA safety issues (the "generic" ETC#'s are given for each configuration for the approximate exposure times used). We think we are well within the MAMA safety limits in our exposures.
UPDATE 10/10/2011 -- Due to the STIS "5 arc second rule" we have had to replace IC 4593, IC 418, and NGC 6572 with IC 3568, NGC 7662, and NGC 5315, respectively, due to their small size making it impossible to get quality spectra with the slit > 5" from the central stars. For all ten PNe, IUE SWP and LWP/R large aperture spectra of the central stars were combined and inputted into the STIS spectroscopic ETC to check G140L and G230L UV-MAMA count rates. As noted previously IC 4593, IC 418, and NGC 6572 had central stars with strong UV continua that exceeded the safe limits and had to be replaced. Two other PNe, NGC 3242 and NGC 7662 had central stars with UV continua too bright for the G230L bandpass but the large size of the nebulae enabled useful scientific data to be taken with the STIS slit > 5 arc sec from the central star. For the record, the STIS spectroscopic ETC run numbers are:
IC 3568: 242112/3 NGC 3242: 240547/8* NGC 7662: 242135/8* NGC 5882: 240533/4 IC 2165: 240549/50
NGC 5315: 242175/6 NGC 6778: 240553/4 PB6: 24195/6 NGC 2440: 242025/6 NGC 6537: 240472/3
*Count rate for G230L spectra exceeded safe limits so (all parts of) the slit was placed > 5" from central star.
We further looked at HLA WFPC2 images of all but two (PB6 & NGC 6778) of the PNe and there were no stars brighter than V~14 within 10 arcsec of any part of the slit even with the range of ORIENTS.
Finally, running the BOT for GSC2 & GALEX, the only red flags that came up were for visits 14 (GSC2) and 5(Galex). Visit 5 is NGC 3242 which has a UV bright star and the slit location is > 5" away. Visit 14 is IC 2165 which has been shown safe based on IUE spectra inputted into the STIS spectroscopic ETC.None are requested.No special calibration requirements are anticipated.The key observational issue for which our science is based on is to have EXACT identical CCD and MAMA slit placements during the two visits for each PN. To facilitate this with the guide stars, as well as noting the science requires a complete set of UV-optical STIS spectra of each nebula to be in hand before analysis can begin, we request that the two visits be scheduled close in time (also assures that the same HST guide stars will be identically place in the FGS detectors).ISM AND CIRCUMSTELLAR MATTER12false0.00.0falsefalsefalsefalseSUPPORTEDISMPLANETARY NEBULAGSC2-N3YX000276J2000J2000J=13.9ISMPLANETARY NEBULAThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000ISMPLANETARY NEBULACentral Star of NGC 7662; HD 220733; V = 13.2, B-V =+0.4
(12/12/2011 -- Coordinates revised slightly to reflect GSC2 values rather than ICRS; star is GSC2 N2T3032629)HD220733J2000J2000ISMPLANETARY NEBULAThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000B=13.30ISMPLANETARY NEBULAThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000ISMPLANETARY NEBULAThis is GSC2 star S7S9168836J2000J2000STARUNDESIGNATEDThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARUNDESIGNATEDThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000ISMPLANETARY NEBULAThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000ISMPLANETARY NEBULAThis object was generated by the targetselector and retrieved from the SIMBAD database.GSC2-3MIRANG4GJ2000J2000ISMEJECTAEMISSION LINE NEBULAPLANETARY NEBULAThis offset position is 0.50 sec east of central star (target 1); slit oriented PA = 20 deg (+/- 10)J2000ISMEJECTAEMISSION LINE NEBULAPLANETARY NEBULASlit position venter is 5.5 arc seconds south of central star; slit PA=107+/-5 deg.J2000ISMEJECTAEMISSION LINE NEBULAPLANETARY NEBULAPosition is 5.5" south of central star; slit PA = 107 +/- 5 deg.J2000ISMEJECTAEMISSION LINE NEBULAPLANETARY NEBULAJ2000ISMEJECTAEMISSION LINE NEBULAPLANETARY NEBULAJ2000ISMEJECTAEMISSION LINE NEBULAPLANETARY NEBULAThe slit position is centered 0.4" N of central star (V =14, 4, B-V = 0.16); slit PA = 100 deg.J2000ISMEJECTAEMISSION LINE NEBULAPLANETARY NEBULAJ2000ISMEJECTAEMISSION LINE NEBULAPLANETARY NEBULAJ2000ISMEJECTAEMISSION LINE NEBULAPLANETARY NEBULAJ2000ISMEJECTAEMISSION LINE NEBULAPLANETARY NEBULAJ2000STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230M1884STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430M4451STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230M1884STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430M4451STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230M1884STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430M4451STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230M1884STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430M4451STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230M1884STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430M4451STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230M1884STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430M4451STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230M1884STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430M4451STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230M1884STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430M4451STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230M1884STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430M4451STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230M1884STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430M4451STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750M6581/private/var/folders/XG/XGHCrLZUH1GGRryr1w5VwU+++TQ/-Tmp-/OPVisit1739488401641796659.xmlTiming link suitability includes constraints ([Group (01 02) Within 10.0 days] [Sequence (01 02) within 10.0 days])The scheduling data was generated by CASM 20.0.CASM was run in Phase II mode.SLIT PA = 180 +/- 10 deg(Tic-Visit
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