Assigned ID: 823
----- Attempting Submission 1 (Fri Feb 26 23:49:51 GMT 2010) -----
HST Phase I Proposal 823 (HST Cycle 18 beta Dor TEST.apt) successfully submitted.
----- Attempting Submission 2 (Fri Feb 26 23:52:13 GMT 2010) -----
used the new target in visit 16.
----- Attempting Submission 1 (Fri Jul 09 19:11:46 GMT 2010) -----
----- Attempting Submission 2 (Tue Feb 15 05:01:55 GMT 2011) -----
----- Attempting Submission 3 (Tue May 17 18:19:07 GMT 2011) -----
----- Attempting Submission 4 (Mon May 23 14:51:29 GMT 2011) -----
There are warnings about not using ACQ/SEARCH exposures. We are confident in the coordinates of the targets and do not believe these exposures to be necessary.
Probing the Atmospheres of Cepheids with HST-COS: Pulsation Dependences, Plasma Dynamics and Heating Mechanisms
Classical Cepheids, although well studied in terms of their cosmologically crucial Period-Luminosity Law, are proving themselves to be increasingly complex and astrophysically intriguing objects. The major aim of this proposal is to probe their stellar atmospheres and try to understand the mechanisms by which they are heated. Archival IUE UV spectra revealed the presence and variability of 10^4 - 10^5 K plasma emission lines, correlated to the pulsation period of the studied Cepheids, indicating that a pulsation-driven heating mechanism may be at work. However, the spectra were of low resolution and also contaminated by scattered light, precluding a more thorough analysis. We propose multiple observations of two selected Cepheids (beta Dor and delta Cep - the prototype of all Classical Cepheids) with HST-COS through the G130M and G160M gratings. The COS spectra will provide comprehensive and detailed diagnostics of the atmospheric plasmas around these Cepheids, and will give us the best look yet at how large-scale, radial pulsations affect the upper atmospheres of supergiants. The phase constraints placed on some of the visits will also allow possible phase-lags between the emission lines to be detailed, giving important additional information into the heating mechanism. Numerous emission lines are covered by the G130M and G160M wavelength range (~1150-1750A), including N V 1240, O I 1305, C IV 1550 and He II 1640. When combined with our approved and ongoing X-ray observations of Cepheids, the HST-COS data will allow us to construct an understanding of Cepheid atmospheric plasmas with temperature from tens of thousands up to millions of degrees - the most thorough atmospheric study to date for this important class of pulsating stars.
We will observe each of the two Cepheids in the G130M and G160M elements. Five observations will be phase-constrained and three will not be. This will allow us to have an excellent sampling of the Cepheid pulsations and will allow line intensitiy and RV changes to be measured as the Cepheid pulsates.
COOL STARS
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SUPPORTED
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This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
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J2000
STAR
CEPHEID
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J2000
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J2000
STAR
CEPHEID
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This object was generated by the targetselector and retrieved from the SIMBAD database.
Proper Motion retrieved from Hipparcos: the New Reduction (van Leeuwen 2007)
J2000
STAR
CEPHEID
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J2000
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