0Assigned ID: 918
----- Attempting Submission 1 (Fri Apr 10 22:08:42 GMT 2015) -----
HST Phase I Proposal 918 (MCB23_v1.apt) successfully submitted.
Receipt: # 918-1
----- Attempting Submission 2 (Fri Apr 10 23:32:55 GMT 2015) -----
HST Phase I Proposal 918 (MCB23_v1.apt) successfully submitted.
Receipt: # 918-2
----- Attempting Submission 3 (Fri Apr 10 23:38:27 GMT 2015) -----0----- Attempting Submission 1 (Thu Jul 23 12:51:25 GMT 2015) -----Probing Supernovae Chemical Yields in Low Metallicity Environments with UV Spectroscopy of Magellanic Cloud B-type StarsSpectrum synthesis studies of the UV spectra of sharp-lined main sequence B stars provide astronomers with
some of the best determinations of the abundances of the light, Fe group, and neutron capture elements. B stars are therefore best-suited to study the chemical evolution of the Magellanic Clouds. But the HST archive is virtually devoid of high resolution spectra of such objects. We propose FUV and NUV observations with the COS G130M, G160M, G185M, and G225M gratings. The four program stars have been observed with the FUSE spacecraft, hence this project will produce continuous high-resolution spectral coverage from 950 to 2400 A and provide a permanent archive of fundamental spectra from which ground-breaking studies of the Magellanic Clouds can be performed in the decades to come. This limited program aims at producing an extragalactic, low-metallicity counterpart to the bright star library of early B stars that is currently being obtained as part of the HST Cycle 21 Treasury program "Advanced Spectral Library II: Hot Stars" (GO 13346, PI T. Ayres).
Spectral lines from most Fe group and s-process elements are found only in the UV region in B stars and information on their abundances is important for studying the chemical evolution of a galaxy, computing opacities for stellar evolution calculations, and assessing the validity of theoretical calculations of explosive nucleosynthesis. Comparing the derived abundances of iron-peak and heavier elements in galactic and Magellanic Cloud B main sequence stars will provide an empirical probe of chemical yields ejected by evolved stars and supernovae in different environments.Objective. We aim to cover the spectral region 1150-2400 A where most of the lines from the Fe-peak and heavy elements reside. The strongest and least blended lines from the Fe-peak elements (Ti III, V III, Cr III, Mn III, Fe III, Co III, Ni II, and Ni III) are found in this region. The useful lines for the neutron capture elements include Ga II (1414.4 A), Ga III (1495.0, 1534.4 A), Ge IV (1189.0, 1229.8 A), Sn III (1251.4 A), Sn IV (1314.4, 1437.5 A), Pb IV (1313.072 A), and Pb III (1553.0 A). To take advantage of the information that is contained in the spectral lines of a sharp-lined B star, high spectral resolution is essential. There is always a trade-off between spectroscopic dispersion, spectral coverage, and exposure times. We have decided to use COS for both FUV and NUV exposures. COS will provide spectra of higher SNR but at a slightly lower spectral resolution than STIS. The resolution of a typical COS spectrum is 15 km/s. Since our program stars have values of V sin i from 10-30 km/s, COS is suitable for a spectrum synthesis investigation. In fact a simulation of COS and STIS spectra for a typical star in the SMC reveals only a slightly deeper line with STIS for the slowest rotator and no difference for the star with a V sin i of 30 km/s. There is no difference in the ability to resolve closely-spaced lines.
Choice of Spectrograph. We chose a target SNR that will provide a 2-3 sigma detection of the weakest observable lines (EW ~ 10-20 mA) in stars with rotational velocities similar to those in our program stars. SNR values of 30-40 and 20 for the COS FUV and COS NUV satisfy the latter criterion. To cover the FUV region observations with both COS gratings (G130M and G160M) are necessary. But the presence of a 14-18A gap between the grating segments in the COS FUV necessitates acquiring two exposures with each grating at different central wavelengths. Each FUV exposure contains four FP-POS settings to reduce fixed-pattern noise (FPN). For the NUV seven COS settings are necessary (G185M and G225M), but the overall exposure time is about 40% less than with the STIS E230M. Two FP-POS settings are sufficient in the NUV, as it is less sensitive to FPN.
Exposure Times.The exposure times for the four FUV and seven NUV COS grating settings were calculated using the COS Exposure Time Calculator (ETC) v.23.1. Since FUSE spectra are available for our four target stars, we used the flux at 1185A in addition to fluxes from IUE LORES spectra.
CVZ Usage:
For target NGC1818-D1 only 22-Dec 2015 comes up as schedulable in Cycle 23 for full CVZ orbits. For target NGC2004-B15 there is only 30-Oct-2015. So we'll assume 5 full CVZ orbits are avaialble for each of these targets during cycle 23.
However, there exist additional scheduling opportunities for short "near-CVZ" visits. We will use two additional short one orbit CVZ visits for the NUV observations of NGC1818-D2. The orbit planner shows several days of scheduling opportunites for each of these.HOT STARS12falsetruefalsefalsefalsefalseSUPPORTEDEXT-STARB0-B2 V-IVNOCoordinates from 2MASS 6X Point Source Working Database / Catalog (Cutri+ 2006) II/281/2mass6xJ2000J20001.5E-13 erg/cm2/s/A (FUSE, 1185A)EXT-STARB0-B2 V-IVNOCoordinates from 2MASS 6X Point Source Working Database / Catalog (Cutri+ 2006) II/281/2mass6xJ2000J20001.3E-13 erg/cm2/s/A (IUE 1300 A)EXT-STARB0-B2 V-IVNOCoordinates from 2MASS 6X Point Source Working Database / Catalog (Cutri+ 2006) II/281/2mass6xJ2000J20001.7E-13 erg/cm2/s/A (FUSE 1185A)EXT-STARB0-B2 III-INOCoordinates from 2MASS 6X Point Source Working Database / Catalog (Cutri+ 2006) II/281/2mass6xCLSTAR-NGC2004-ROB-B14W61-18-3J2000J20002.5E-13 erg/cm2/s/A (FUSE 1185A)COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1623COS/NUVSpectroscopicNoNoG185M1913COS/NUVSpectroscopicNoNoG185M1941COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M2010COS/NUVSpectroscopicNoNoG225M2233COS/NUVSpectroscopicNoNoG225M2268COS/NUVSpectroscopicNoNoG225M2306COS/NUVSpectroscopicNoNoG185M1913COS/NUVSpectroscopicNoNoG185M1941COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M2010COS/NUVSpectroscopicNoNoG225M2233COS/NUVSpectroscopicNoNoG225M2268COS/NUVSpectroscopicNoNoG225M2306COS/NUVSpectroscopicNoNoG185M1913COS/NUVSpectroscopicNoNoG185M1941COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M2010COS/NUVSpectroscopicNoNoG225M2233COS/NUVSpectroscopicNoNoG225M2268COS/NUVSpectroscopicNoNoG225M2306COS/NUVSpectroscopicNoNoG185M1913COS/NUVSpectroscopicNoNoG185M1941COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M2010COS/NUVSpectroscopicNoNoG225M2233COS/NUVSpectroscopicNoNoG225M2268COS/NUVSpectroscopicNoNoG225M2306The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.1465998013000243.65855351624396(Tic-Visit
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