Science Keywords: Select from 2 to 5 items. Science Keywords is a required field. Please specify your scheduling constraints or 'No Constraints' on all Observation forms. 0 Assigned ID: 1053 ----- Attempting Submission 1 (Fri Aug 09 11:40:23 GMT 2019) ----- HST Phase I Proposal 1053 (Reynolds.apt) successfully submitted. Receipt: # 1053-1 Joint Chandra/HST Proposal has been updated with target (GRO J1008-57). The old generic target have been left in place. The grating has been changed to G140L due to source brightness and E(B-V) ~ 2.4. Please confirm that the acq sequence is ok. Source flux updated to ~0.01 mJy at 2000 Ang, and optical flux to V~15 (vega). Acq updated to 5s through 50CCD. Science exposure have been divided into 3x~800s. Acq updated to 5s through 50LP. ---------------------------------- Acq updated to 0.5s through 50LP Obs sequence updated to 3x811s exposures with a wavecal during occulation at end of orbit. -1412062063 ----- Attempting Submission 2 (Thu Sep 19 16:47:06 GMT 2019) ----- ----- Attempting Submission 3 (Fri May 22 19:39:42 GMT 2020) ----- ----- Attempting Submission 5 (Sat May 23 23:24:23 GMT 2020) ----- HST Phase II Proposal 15998 successfully submitted. Receipt: # 15998-5 ----- Attempting Submission 6 (Sat May 23 23:29:36 GMT 2020) ----- HST Phase II Proposal 15998 successfully submitted. Receipt: # 15998-6 ----- Attempting Submission 7 (Tue May 26 00:57:59 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. 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. Massive Black Holes And Their Host Galaxies 6 false false false false false false false SUPPORTED STAR ACCRETION DISK BE X-RAY TRANSIENT NO This object was generated by the target selector and retrieved from the SIMBAD database. 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 ~0.01 mJy at 2000 Ang STAR ACCRETION DISK BE X-RAY TRANSIENT We request a single trigger in cycle 27 to occur quasi-simultaneously with a CXO and VLA observation. We have an approved program with Swift to monitor a bright outburst from a Be/X-ray binary, via 40 monitoring observations. The spectra provided by Swift will be used in combination with data from Swift/BAT and MAXI to trigger the proposed Chandra/HST/JVLA observation. We will trigger this program based on an observation of a known BeXRB at a luminosity in excess of 50% Eddington, e.g., see the BeXRB catalogue1 (Raguzova et al. 2005) or the ESO BeXRB monitor2 . Based on the typical duration of a large outburst (30 - 90 days), we estimate a required turn around time of 21 days, i.e., medium in CXO parlance. The program trigger will come via the CXO office. Next type-II BeXRB outburst ~60 mJy at 2200 Ang STIS/FUV-MAMA Spectroscopic No No E140M 1425 /Users/markrey/chandra_prop/chandra_c21/be_xrb/phaseII/OP-cache/bexrb_too_groj1008-57_phaseII-v01.xml 1590104075638 The scheduling data was generated by CASM 28.0. CASM was run in Phase II mode. The acq exptime is a fiducial configuration given the unknown nature of the target at the current time. Given the system will contain a Be-star, we expect it to be bright (V~10). (Tic-Visit :proposal-id 15998 :visit-id "01" :proposal-version -1 :trans-version "20191203" :date "21-May-2020 19:34:35.0" :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 15998 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15998 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2749 :al-overhead-at-end 0 :internal-dur-at-end 375 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0 This cycle 27 HST/STIS observation is on hold pending trigger of our CXO TAC awarded joint CXO/HST/JVLA observation We have an approved program with Swift to monitor a bright out-burst from a Be/X-ray binary, via 40 monitoring observations. The spectra provided by Swift will be used in combination with data from Swift/BAT and MAXI to trigger the proposed Chandra/HST/JVLA observation. We will trigger this program based on an observation of a known BeXRB at a luminosity in excess of 50% Eddington, e.g., see the BeXRB catalogue1 (Raguzova et al. 2005) or the ESO BeXRB monitor2. Based on the typical duration of a large outburst (30 - 90 days), we estimate a required turn around time of ~21 days 1590454520688 /private/var/folders/vw/wc02pwpd4g9clwmh404r3p_80080n0/T/OPVisit16286187725651743721.xml The scheduling data was generated by CASM 28.0. CASM was run in Phase II mode. The acq exptime is a fiducial configuration given the previously unknown nature of the target. Given the actual target -- GRO J1008-57 -- has V ~ 14, this needs to be potentially updated. The grating option has been changed to G140L as the source is extincted and has measured Swift/UVOT fluxes during previous outbursts of ~0.01mJy @2000 Ang. We expect a S/N of ~3 in the continumm in 1ks. Line emission from the accretion flow is expected on top of this. (Tic-Visit :proposal-id 15998 :visit-id "02" :proposal-version -1 :trans-version "20191203" :date "25-May-2020 20:55:20.0" :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 226592 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15998 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15998 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2996 :al-overhead-at-end 85 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3389 :pcs-gap 0 ) true 1 0 Grating changed to G140L as the source is extincted and has measured Swift/UVOT fluxes during previous type II outbursts of ~0.01mJy @2000 Ang. We expect a S/N of ~3 in the continumm in 1ks. Line emission from the accretion flow is expected on top of this.