Target BEXRB-TOO: There is no need or capability to test the scheduling of observations of generic targets in Phase I. This warning will go away the next time the proposal is loaded. Submitting to accompany joint program submitted to cxo cycle 26 per email on March 29th from Aleksandra Hamanowicz. -1401821051 Assigned ID: 5903 ----- Attempting Submission 1 (Fri Apr 05 19:11:46 GMT 2024) ----- Generic unknown ToO target template. This is a re-submission of a program from previous years. A joint ToO w/ CXO and JVLA. Probability of trigger is lower with ongoing obs window issues. -1262178199 ----- Attempting Submission 1 (Fri Oct 25 02:33:22 GMT 2024) ----- 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. Degenaar is an expert in the multi-wavelength study of accretion flows with expertise in the stellar and AGN area and significance experience analyzing Chandra and HST observations. Dr. Degenaar has significant expertise in the study of neutrons stars and simultaneous radio and X-ray observations of accreting neutron stars. Dr. van den Eijnden is an expert in the multi-wavelength study of accretion flows with expertise in the stellar area and significance experience analyzing Chandra and HST data. Dr. van den Eijnden brings expertise in the analysis of radio observations from the VLA and led the study of Swift J0243.6+6124 and the radio observations of A0535+262 during the recent giant outburst. Dr. Miller is an expert in the study of accretion flows in the X-ray band with expertise in the stellar and AGN area and significance experience analyzing high resolution X-ray spectroscopy observations from both Chandra and XMM-Newton, and is intimately involved in the upcoming XRISM mission. Dr. Reynolds is an expert in the multi-wavelength study of accretion flows with expertise in the stellar and AGN area and significant experience analyzing data from NASA X-ray missions including Chandra and HST. He has previously been involved in CXO campaigns observing A0535+262 in 2010 and GRO J1008-57 in 2019 and the recent giant outburst of A0535+262 in 2020. Dr. Walton is an expert in the study of accretion flows in the X-ray band with expertise in the stellar and AGN area and significant experience analyzing data from NASA X-ray missions including Chandra. Dr. Walton has been intimately involved in many of the ground braking observations of ULXs, which revealed the primary object to be a neutron star in at least a subset of these systems. Stellar Physics and Stellar Types 6 false false false false false false false false SUPPORTED STAR ACCRETION DISK JET NEUTRON STAR X-RAY TRANSIENT We request a single trigger in cycle 32 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 1729823399736 The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. /private/var/folders/cc/88fm8x5s22n9b23g5__npqp40000gs/T/OPVisit3040142260949020839.xml 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 17877 :visit-id "01" :proposal-version -1 :trans-version "20240604" :date "24-Oct-2024 22:29:59.0" :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 296080 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17877 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17877 :visit-id "01" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2625 :al-overhead-at-end 0 :internal-dur-at-end 440 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3005 :pcs-gap 0 ) true 1 0 This cycle 28 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