0----- Attempting Submission 1 (Tue Sep 12 17:27:33 GMT 2023) -----Spin Me Right Round: Testing Accretion Spin-up in Wide Binary Main-Sequence Carbon StarsThe dwarf carbon stars are a class of post-mass transfer binaries that have accreted a significant amount of C-rich mass and angular momentum from a former AGB companion (now a white dwarf, usually undetected in the optical). We aim to use these dwarf carbon stars to better understand the physics behind mass and angular momentum transfer in binary systems, and the resulting spin-up and activity lifetimes of rejuvenated dwarfs. We propose to use joint Chandra+HST observations of 5 nearby dwarf carbon stars in wide binary systems to (1) probe the dC X-ray magnetic activity and diagnose mass-transfer spin-up, (2) constrain the coronal temperature of the dC, and (3) assess the remnant white dwarf companion cooling age through UV photometry.We plan observations of 3 interesting dwarf carbon (dC) stars, utilizing both the ACS-SBC and WFC3-UVIS detectors. This will allow us to obtain stronger UV constraints than allowed by the 1 weak GALEX NUV detection. The dCs 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.
The WFC3 ETC predcits (assuming WD T=3000K):
HE 2115-0709 -- S/N=14.5 in the NUV with UVIS+[F225W] in 2333s
LP 758-43 -- S/N=17.0 in the NUV with UVIS+[F225W] in 2334s
LP 225-12 -- S/N=11.0 in the NUV with UVIS+[F225W] in 2414s
For the UVIS observations we include a post-FLASH of 15e to aid with CTE issues as recommended.
For the UVIS observations we utilize a BOX dither.
The UVIS observations pass saturation checks with the BOT and GSC2.
The ACS ETC predicts (assuming WD T=4500K):
HE 2115-0709 -- S/N= 3.5 in the FUV with SBC+[F140LP] in 2482s
LP 758-43 -- S/N= 4.0 in the FUV with SBC+[F140LP] in 2483s
LP 225-12 -- S/N= 2.7 in the FUV with SBC+[F140LP] in 2545s
HE 2115-0709 -- S/N= 6.3 in the FUV with SBC+[F165LP] in 2496s
LP 758-43 -- S/N= 7.0 in the FUV with SBC+[F165LP] in 2497s
LP 225-12 -- S/N= 5.4 in the FUV with SBC+[F165LP] in 2577s
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.
The SBC observation passes the BOT using the GALEX catalog with all SAFE objects.
For the SBC observations we utilize a BOX dither.n/aStellar Physics and Stellar Types6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARCARBON STARCOMPOSITE SPECTRAL TYPEDANOThis object was matched into Gaia DR3.J2000J2000B=17.88, J=12.673, H=12.0, K=11.808, G=14.81, BP=15.69 RP=13.90STARCARBON STARCOMPOSITE SPECTRAL TYPEDANOThis object was matched into Gaia DR3.J2000J2000J=13.0, H=12.26, K=11.90, G=15.12, BP=16.08, RP=14.12STARCARBON STARCOMPOSITE SPECTRAL TYPEDANOThis object was matched into Gaia DR3.J2000J2000GALEX NUV=19.5931, B=17.2, R=15.1, G=15.52, BP=16.42, RP=14.59WFC3/UVISImagingNoNoF225WACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF165LPWFC3/UVISImagingNoNoF225WACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF165LPWFC3/UVISImagingNoNoF225WACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF165LPPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1falsePOS-TARGDITHER0.179LINE0.116falsefalse63.65420.02ACS-SBC-DITHER-BOX2false/private/var/folders/bl/s7q0tqnn5gbcbyvcfnrhj2rh0004nc/T/OPVisit136431540869573659.xmlThe scheduling data was generated by CASM 31.1.CASM was run in Phase II mode.(Tic-Visit
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