I had to click the box for "We have not submitted a similar coordinated proposal for another observatory's peer review this year." to allow submission.
However, we did submit a proposal to the Chandra peer review and this APT submission was requested becase of that.
This comment still applies 4/3/2024.-860136394Assigned ID: 5901
----- Attempting Submission 1 (Wed Apr 03 03:02:42 GMT 2024) -----
HST Phase I Proposal 5901 successfully submitted.
Receipt: # 5901-1
----- Attempting Submission 2 (Thu Apr 04 00:18:55 GMT 2024) -----
HST Phase I Proposal 5901 successfully submitted.
Receipt: # 5901-20----- Attempting Submission 1 (Sun Oct 20 18:50:52 GMT 2024) -----
----- Attempting Submission 2 (Tue Nov 12 14:00:28 GMT 2024) -----X-Ray Jets in MicroquasarsWe propose Target of Opportunity (ToO) observations for detailed studies of X-ray jets from microquasars. Following the discovery by Chandra of radio/X-ray jets in five microquasars, it becomes clear that X-ray jets are probably much more common than previously thought, and they offer an exciting new way to probe the physics of relativistic jets from black holes and their feedback on the ISM. The proposed ToO observations are optimized to discover and study (flux evolution, morphology, SED, proper motion, ...) new X-ray jets from microquasars, triggered by their detection as radio lobes. This will have implications not only for the study of jets from Galactic X-ray binaries, but also for our understanding of relativistic jets from active galactic nuclei (AGN).HST observations in the IR will complement the measurements of the extended jets in the radio and X-rays and be used to bridge the gap in the spectral energy distribution. We will use WFC3 with the F160W. The observations will be 1 HST orbit for the first two Chandra observations and 2 HST orbits for the two final observations when we expect the jets to be much fainter and more extended. On each orbit, we will observe with the WFC3/F160W with 2 dither positions. The response for HST is longer than 3 weeks, therefore not constraining for HST. The separation between observations will be approximately by one month, except for the last observation which will 2 months after the third.Prof. Stephane Corbel, PI, is an expert in multi-wavelength observations of accreting binaries and has conducted all Chandra observing campaigns leading to all detections of X-ray jets in microquasars. Expert in Chandra observations. PI of radio observations with ATCA and VLA. Member of MeerKAT large program ThunderKAT. Co-I of Swift X-ray observations.
Prof. Philip Kaaret, acting Co-PI, is an expert in X-ray data analysis, including Chandra , as well as HST analysis.
Dr John Tomsick is an expert in X-ray and optical data analysis, including Chandra.
Dr Giulia Migliori is an expert in X-ray observations of accreting binaries, including Chandra and high resolution imaging. She is also an expert in AGNs physics and their detailed modeling.
Prof. Robert Fender is an expert in multi-wavelength observations of accreting binaries and the PI of the MeerKAT large program ThunderKAT, allowing weekly radio observations of accreting binaries. Also PI of radio observations with AMI.
Dr Jerry Orosz is an expert in optical and near-infrared observations and will led the OIR follow-up observations.
Dr Tasso Tzioumis is an expert of radio observations and will conduct the ATCA radio observations.
The proposed observations, if accepted, will be analysed and published by a new PhD student (e.g. Noa Grollimund).Stellar Physics and Stellar TypesSupermassive Black Holes and Active Galaxies6falsefalsefalsefalsefalsefalsefalsetruePRIMARY150trueSUPPORTEDSince the flux information is used to check for over-illumination of sensitive detectors, we give the V-mag for the central black hole. It will be a point source and be significantly brighter than the extended jets that are the science focus of the proposal. In the decaying phases of the outburst, i.e. when the transient radio jets are observed, the black hole should be dimmer than 19th magnitude in V.
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