Scientific Category is a required field. Science Keywords: Select from 2 to 5 items. Please specify your scheduling constraints or 'No Constraints' on all Observation forms. 0 Assigned ID: 1126 ----- Attempting Submission 1 (Wed Aug 19 13:43:55 GMT 2020) ----- Joint Chandra/HST Proposal has been triggered via CXO. v2 w/ updated visibility per comments from Patricia. v3 w/ updated acq exptime==1s per comments from Dan. v4 w/ updated to GAIA DR2 ICRS coords per comments from Dan. 268035742 ----- Attempting Submission 1 (Wed Sep 16 18:58:45 GMT 2020) ----- ----- Attempting Submission 2 (Fri Nov 13 16:18:02 GMT 2020) ----- ----- Attempting Submission 3 (Fri Nov 13 17:30:53 GMT 2020) ----- HST Phase II Proposal 16422 successfully submitted. Receipt: # 16422-3 ----- Attempting Submission 4 (Fri Nov 13 17:52:34 GMT 2020) ----- ----- Attempting Submission 5 (Sat Nov 14 15:00:22 GMT 2020) ----- HST Phase II Proposal 16422 successfully submitted. Receipt: # 16422-5 ----- Attempting Submission 6 (Sun Nov 15 14:15:17 GMT 2020) ----- Observations of the population of ultra luminous X-ray sources has revealed that at least a subset of this group contains a neutron star primary. Thus, dramatically demonstrating the viability of super-Eddington accretion for this source class. However, the physics of these super-Eddington accretion flows are poorly understood with the sources typically lying at Mpc distances. The population of Galactic Be/X-ray binaries (BeXRBs) are known to have giant outbursts that enter the super-Eddington regime and promise the opportunity to learn much about this mode of accretion. Herein, we propose to obtain simultaneous high resolution X-ray, UV and radio spectroscopy of the next bright Galactic BeXRB to enter a giant outburst when the neutron star will be accreting in the super-Eddington regime. Studies of giant outbursts of other BeXRBs are highly warranted to determine that winds and jets indeed occur simultaneously in the super-Eddington regime. We note that ULXs are too distant to detect a compact radio jet, so determining the co-existence of winds and jets at highly super-Eddington accretion rates can ONLY be achieved with Galactic BeXRBs, as we aim to target with this proposal. To be able to confirm the presence of both winds and jets in the super-Eddington regime, we therefore proposed for and were granted (quasi-simultaneous) Chandra/HETGS, HST/STIS and JVLA observations of the next giant outburst of a BeXRB. In a BeXRB accreting a super Eddington luminosities, we expect the UV emission to evolve when the accretion envelope develops and shields the outer disk from the inner X-ray emitting region, e.g., Shakura & Sunyaev (1973). In this regime we might expect the UV emission to be dominated by the re-reprocessing component detected in soft X-rays. The high S/N and spectral resolution of STIS will be key here as the kinematics of the accretion inflow and wind will be encoded in the spectral lines. Obtaining observational evidence for wind outflows in ULXs is highly challenging due to the high absorption and distance to these systems. However, low resolution HST/ACS prism spectroscopy has had some limited success and demonstrated the presence of a complex highly ionized outflow at these accretion rates (e.g. M81 X-1, Bregman et al., 2012). We are requesting observations with STIS with the MAMA detector and the E140M grating, which will provide wavelength coverage from 1150 - 1800 Ang . The high dispersion provided by this grating will ensure the safety of the MAMA detector as these sources can be very bright (> 0.06 Jy; lambda_c ~ 2200Ang). In the event of a fainter UV counterpart, a lower resolution grating will be utilized. Accurate flux estimates will be provided by Swift/UVOT observations in support of this program. GYRO MODE: As our program is a joint ToO w/ Chandra & JVLA, reduced gyro mode observations would reduce our ability to observe a quasi-random outburst from an unknown source (though likely in Galactic plane). Fingers crossed! Dr. Reynolds is an expert in the multi-wavelength study of accretion flows and has previously studied the relativistic wind in the the Be/X-ray binary 1A0535+262. Dr. Miller is an expert in the study of accretion flows with an emphasis on the generation of accretion disk winds and jets. Dr. Degenaar is an expert in the multi-wavelngth study of accretion flows and neutron stars. Dr. Walton is an expert in the study of accretion flows and the ULX extra-galactic source population. Dr. van den Eijnden is an expert in the study of accretion flows and has lead previous programs that lead to the discovery of a simultaneous wind/jet system in the Be/X-ray binary Swift J0243.6+6124. 6 false false false false false false false SUPPORTED STAR ACCRETION DISK BE X-RAY TRANSIENT NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coords are ICRS from GAIA DR2. Observation awarded through CXO program. Observation to occur quasi-simultaneously with CXO (+\- 1 day). The source is currently undergoing a large type-II outburst. The program has been triggered. Further trigger details should come via CXO. J2000 STIS/FUV-MAMA Spectroscopic No No E140M 1425 /private/var/folders/vw/wc02pwpd4g9clwmh404r3p_80080n0/T/OPVisit7934584680876778312.xml 1605449448587 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. Source is bright (<10 Vega or >50mJy) at 2200 Ang Template for original proopsal, trigger target is below. (Tic-Visit :proposal-id 16422 :visit-id "02" :proposal-version -1 :trans-version "20200619" :date "15-Nov-2020 09:10:48.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 157008 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16422 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16422 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2535 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2928 :pcs-gap 0 ) true 1 0 Grating changed to E140M as the source is bright and has measured Swift/UVOT fluxes during this outburst of >50mJy @2200 Ang.