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Spectral Element 1 is a required field.
Please specify your scheduling constraints or 'No Constraints' on all Observation forms.0Assigned ID: 1121
----- Attempting Submission 1 (Wed Aug 19 13:41:16 GMT 2020) -----Joint Chandra/HSTWe added a second FUV exposure with the F165LP filter to help with the SBC red leak.-996203301----- Attempting Submission 1 (Tue Sep 15 22:19:16 GMT 2020) -----X-rays from a Unique Spun-up Post Mass Transfer Main Sequence Carbon StarCarbon stars (C>O) were long assumed to all be giants, because only AGB stars dredge up significant carbon into their atmospheres. We now know that dwarf carbon (dC) stars are actually far more common than C giants. The dCs have accreted C-rich envelope material from an AGB companion, eventually yielding a white dwarf and a dC that has gained both significant mass and angular momentum. We propose a Chandra study of the nearest known typical dC, J0435+3401, to investigate its extreme X-ray spectral properties and variability, while using HST to constrain the cooling age of its white dwarf companion. Since dCs are the likely progenitors of CH, BaII and CEMP stars, and probably also interacting binaries like CVs, novae, or SN Ia, our results will have wide-ranging implications.We plan observations of an interesting dwarf carbon (dC) star, utilizing both the ACS-SBC and WFC3-UVIS detectors. This will allow us to obtain stronger UV constraints than allowed by the weak GALEX NUV detection. The dC must have (from an evolutionary perspective) a WD component. Since no WD features are evident in the optical spectrum the WD must be relatively cool, implying Gyr since its AGB phase. We seek to detect and constrain its age using these NUV and FUV HST observations.
For all ETC calculations we assume a 7,000K blackbody normalized to the GALEX NUV magnitude, with E(B-V) =0.606.
For the FUV observations, we use both the [F140LP] and [F165LP] filters in order to account for the red leak of the SBC as recommneded. We fit both observations into 1 orbit and the ACS ETC estimates a S/N~7 for both filter obeservations.
THe WFC3 ETC predcits S/N=100 in the NUV with UVIS+[F225W] in 2384s.
For both the SBC and UVIS observations we utilize a BOX dither. For the UVIS observations we include a post-FLASH of 11e to aid with CTE issues as recommended.
The SBC observation passes the BOT using the GALEX catalog with all SAFE objects. The UVIS observations pass saturation checks with the BOT and GSC2.n/aStellar Physics and Stellar Types6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARCARBON STARJ2000J2000B=15.2, R=13.5, G=13.7165, NUV=22.08, E(B-V)=0.606, dC+DA?ACS/WFCSpectroscopicNoNoACS/SBCImagingNoNoF150LPPOS-TARGDITHER0.179LINE0.116falsefalse63.65420.02ACS-SBC-DITHER-BOX1falsePOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX2false/private/var/folders/pq/0q6qw20n6xxb77g5kk6yy8480000gn/T/OPVisit12148510308983647097.xmlThe scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.(Tic-Visit
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