Science Keywords: Select from 2 to 5 items. Science Keywords is a required field. US Admin CoI is a required field. Wavelength is a required field. Wavelength is a required field. Wavelength is a required field. Wavelength is a required field. 0 Assigned ID: 1615 ----- Attempting Submission 1 (Wed Nov 15 16:43:58 GMT 2017) ----- Joint NRAO Changed the Segement parameter from "A" to "BOTH" for the G130M as requested. 1276976749 ----- Attempting Submission 1 (Thu Nov 30 13:28:35 GMT 2017) ----- HST Phase II Proposal 15411 (HST_COS_Mrk1018.aptx) successfully submitted. Receipt: # 15411-1 ----- Attempting Submission 2 (Mon Dec 11 15:57:26 GMT 2017) ----- VLBA monitoring of the extraordinary changing-look quasar Mrk 1018 Last year, we discovered the first-ever unambiguous case of a changing look quasar completing a full cycle, Mrk1018, which first transitioned from a Sy 1.9 to a Sy 1 nucleus in 1984, remained broad-lined for about 30 years, and transitioned back to a Sy 1.9 sometime between 2013 and 2016. We were granted ToO VLBA observations during the second semester of 2016, which indicated flux density and spectral variability of the AGN core of Mrk1018 at GHz frequencies and, very remarkably, showed the emergence of a new compact component on December 2016). Additional VLBA DDT observations have shown the VLBA source disappear, while HST photometry is now dropping, while we expected it to be raising, Here, we request up to four multi-frequency VLBA observations to be done contemporaneously with requested HST COS observations and approved Chandra X-ray and optical monitoring to shed light on the nature of the puzzling behavior of Mrk 1018 and the (now disappeared) new source. The VLBA, with its unique multi-frequency capabilities and milliarcsecond angular resolution, may hold the key to understanding Mrk1018 and, by extension, the wider class of changing look AGN. These COS-FUV observations are part of a coordinated multi-wavelength monitoring program combining radio (VLBA), X-rays (Chandra), and optical observations of the changing-look AGN Mrk1018. Each epoch we obtain a 2 orbit long FUV spectrum with the G140L grating to cover the FUV continuum at high S/N as well as the flux and shape of broad emission lines such as Lya and CIV. Although we have 4 epochs of VLBA and chandra observations granted, one will be in the extended sun block zone between end of February and beginning of June. Hence, we use two orbits to obtain a higher resolution spectrum with the G130M grating of the Lya line which is prone to various narrow absorption lines. This is necessary to calibrate the modelling of the broad Lya emission line in the low resolution spectra based on a single high-resolution spectrum. Massive Black Holes And Their Host Galaxies 6 false false false false false false SUPPORTED GALAXY ACCRETION DISK JET NUCLEUS SEYFERT NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates were then slightly adjusted on subarcsec scale to match the coordinates of previous successfull observations J2000 J2000 300 counts/s in the 4s long COS NUV (PSA and MIRRORA) acquisition images from Feb 2017 COS/FUV Spectroscopic No No G140L COS/FUV Spectroscopic No No G140L COS/FUV Spectroscopic No No G140L COS/FUV Spectroscopic No No G140L /tmp/OPVisit4917600864936006443.xml The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. 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