0Assigned ID: 874
----- Attempting Submission 1 (Fri Apr 07 21:02:07 GMT 2017) -----
----- Attempting Submission 2 (Sun Apr 09 04:02:22 GMT 2017) -----For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.0----- Attempting Submission 1 (Fri Jul 21 02:31:09 GMT 2017) -----
HST Phase II Proposal 15305 (HST_Cycle25_Cepheids_PhaseII.apt) successfully submitted.
Receipt: # 15305-1
----- Attempting Submission 2 (Fri Jul 28 14:54:57 GMT 2017) -----FP-POS 3 and 4 have now ben selected for the G130M-1291 exposures, so that segments A and B can be used.The Secret Lives of Cepheids: Completing the Picture with HST-COS Observations of the Nearest Classical Cepheids, Polaris and delta CepheiClassical Cepheids, although well studied in terms of their cosmologically important Period-Luminosity Law, are proving to be increasingly complex and astrophysically intriguing in terms of atmospheric energetics. This proposal expands on data collected by us in previous cycles to probe Cepheid atmospheres, understand their heating mechanisms and answer important questions. Our previous COS FUV spectra revealed a wealth of 10,000-300,000K plasma emission lines, phase-locked with each Cepheid's pulsation periods, showing that a pulsation-driven heating mechanism is at work. To significantly expand the parameter space of the Cepheid sample, we propose four visits to the nearest and brightest Cepheid, Polaris. Only two COS spectra of Polaris were acquired previously. But we have now seen that Cepheids undergo fairly large FUV emission line variations (flux level differences of 20x and more). Observations of the ultra-low amplitude Polaris will offer remarkable insights into the effects that even minimal pulsations have on a cool supergiant atmosphere, especially when compared to full amplitude Cepheids and also non-pulsating supergiants in the instability strip. We have also recently proven that delta Cep is an X-ray variable, with a tight pulsation phase-range where the star's X-ray activity increases by over 4x. However, no COS spectra exist at this phase, which will be necessary to determine atmospheric densities and dynamics during the X-ray enhancement. When combined with our existing X-ray and FUV data set, the proposed COS data will advance a much deeper understanding of Cepheids and their atmospheric plasmas.We propose 1 HST-COS visit (4 consecutive orbits) of the prototype Classical Cepheid delta Cep and 4 HST-COS visits (1 orbit each) of Polaris. The new data for delta Cep will allow us to study atmospheric properties and dynamics, including line ratios and flow velocities, during the phase of enhanced X-ray activity previously observed by us with both Chandra and XMM. We propose that the COS visit be phase-constrained to occur at phase ~ 0.48 for delta Cep to ensure that we observe right at or near the peak of the short-lived X-ray maximum. Polaris is a very interesting target as, although it is a Cepheid, it undergoes minimal pulsations, with a velocity amplitude almost 10x smaller than delta Cep. Also, only two phases of Polaris' pulsation cycle have yet been covered with COS, and yet flux differences are already seen between the two spectra. The new observations will allow us to map out the atmospheric variability of a near-negligible pulsator and make much more detailed relations between the amplitude of pulsation velocities and such parameters as the extent of pulsation-driven heating (emission line fluxes), and velocity / turbulence / density changes within the line-forming plasmas (line shifts, profiles and ratios). Polaris can also serve as an important bridge between the larger amplitude Cepheids previously observed with COS and the non-pulsating, non-variable and Hybrid supergiants observed with both COS and STIS. Three of the new Polaris observations will be constrained to occur around the phase of minimum radius (0.8 phase), which is where the FUV emissions of all other observed Cepheids have undergone rapid intensifications. We also request one "control" observation to occur at 0.25 phase, where the emissions should be quiet. This is to check whether any variations observed are linked to the pulsations of the Cepheid, or perhaps the result of a long-term activity cycle.Stellar Physics6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARCEPHEIDF3-F9PULSATING VARIABLENOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARCEPHEIDF3-F9PULSATING VARIABLENOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1589The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.1542238183000160.98177452969378(Tic-Visit
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