0 Assigned ID: 3823 ----- Attempting Submission 1 (Thu Oct 20 16:54:25 GMT 2022) ----- HST Phase I Proposal 3823 successfully submitted. Receipt: # 3823-1 ----- Attempting Submission 2 (Thu Oct 20 17:05:52 GMT 2022) ----- HST Phase I Proposal 3823 successfully submitted. Receipt: # 3823-2 ----- Attempting Submission 3 (Fri Oct 21 12:53:04 GMT 2022) ----- For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. As HOPR 92589 for HST program 17276 was aproved, I have updated the phase II to include the two additional orbits that have been granted. I have set up those to cover the orbital phase of interest, during which visits 2 and 3 have failed. I did this by defining period and zero phase in each visit and setting phase timing requirements for each science exposure. I hope this was the correct way to do this, let me know if there are any issues I should address. (Still applies, 04 Aug 2023) 1304149141 ----- Attempting Submission 1 (Mon Dec 12 21:00:06 GMT 2022) ----- ----- Attempting Submission 2 (Mon Jul 31 14:12:11 GMT 2023) ----- ----- Attempting Submission 3 (Fri Aug 04 08:56:38 GMT 2023) ----- Additional orbits granted through HOPR 92589 A new radio pulsing white dwarf? In April this year, we have discovered a system showing strong optical pulses on a period of 5.3 minutes, during which the flux increases by up to a factor of four. Optical spectroscopy revealed a blue continuum added to the red spectrum of an M-type dwarf, with strong Balmer and neutral helium lines in emission. The radial velocity of the lines varies on a period of 4.03 hours, consistent with a photometric modulation observed on TESS data and clearly identifying the system as a compact binary. Perhaps most fascinating of all, the 5.3 minute pulses are also identified in radio. While radio pulses are reminiscent of neutron star or black hole binaries, the 5.3 min modulation is archetypical of the spin period of a strongly magnetic white dwarf. Only one other white dwarf binary is known to show this behaviour: the white dwarf pulsar AR Scorpii, in which the combination of a magnetic field and rapid rotation results in the acceleration of relativisitic particles that blast the inner hemisphere of the M-dwarf companion, akin to the well-known milli-second pulsars. We believe our system to be the first ever AR Sco twin, establishing white dwarf pulsars as a class. The ultimate proof of our hypothesis relies on the unambiguous identification of the white dwarf, which will be achieved through the detection of hydrogen absorption in the requested COS/G140L observations. This discovery will provide the first opportunity to test models proposed to explain the origin of AR Sco and shed light onto the evolution of close binaries. We require FUV spectroscopy of J1912 in TIME-TAG mode, which allows to re-bin the data in both time and wavelength. We will generate ultraviolet light curves and time-resolved spectra that we will bin both on the orbital period of the binary, and the spin period of the white dwarf. With these data in hand, we will (i) confirm the presence of a white dwarf in the system, (ii) measure the UV amplitude of the pulses, (iii) probe for the occurrence of flares, and (iv) probe for Zeeman splitting indicating a magnetic field. For covering the FUV, we will use COS with the G140L grating centred at 1105 A, which provides flux-calibrated coverage between 1118 and 2150 A. This configuration provides us with good coverage of Lyman-alpha, where Zeeman splitting would be most evident, and of the H2 quasi-molecular absorption at 1600 A, which is particularly sensitive to temperature (Allard et al., 2004). We used white dwarf models with the temperature estimate for AR Sco to calculate the required exposure time for our observations. To confirm the white dwarf, we require signal-to-noise ratio (SNR) of ~5 in the vicinity of the Lyman-alpha line, which according to the ETC requires ~34,800 sec. Overheads consist of guide star acquisition (6 min in the first orbit, 4 min for subsequent orbits), target acquisition (4 min in the first orbit only), and instrument overheads (5 min for the first orbit, 2 min for subsequent orbits). Our target has an orbital visibility of 55 min, so accounting for these overheads we require 12 orbits to reach the required SNR in the FUV. Our request can be broken into separate smaller visits if necessary. J1912 is the brightest object in a 25 arcsec radius, and even during the strongest detected flares its brightness does not surpass V~16, well below the brightness limit of the COS. Pelisoli is an expert in the observational study of close white dwarf binaries. Gaensicke has detailed experience in planning and analysing HST ultraviolet spectroscopy. Jaco Brink is a specialist in high-speed data, Potter and Buckley are specialists in polarimetry, Heywood and Woudt are specialists in radio, and Schwope is a specialist in X-ray -- all these types of datasets will contribute to the analysis and publication of this system. Stellar Physics and Stellar Types 3 false false true false false true false false SUPPORTED STAR INTERACTING BINARY INTERMEDIATE POLAR REGULAR VARIABLE NO J2000 J2000 COS/FUV Spectroscopic No No G140L 1105 The scheduling data was generated by CASM 31.0. 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