Observations of binary stars with the differential speckle survey instrument i instrument descriptio
The lack of peer review. Thanks for raising the issue. There are many reasons for non publication of course such as lack of interest from journals which are after all dependent on selling copy to make money like any periodical and thus charge more for advertising though this doubtful here for obvious reasons. Obtaining points of clarification ahead of peer review is reasonable though.
I think we have all begun to take exoplanet discovery as the norm when discovery by transit or RV is excruciatingly hard and arduous work , especially given the increasing magnitude of new discoveries and their enormous implications. That spectre now hovers ominously over every exciting exoplanet finding. The Proxima b signal was apparent in the data almost a year ago but it took till this summer to get sufficient evidence to publish the discovery unequivocally.
Extraordinary discoveries require extraordinary evidence and all that. The first nearby M dwarf Hab zone planet to undergo detailed atmospheric spectroscopy will be momentous. Far better to get it right prepublication , whatever the delay. The evidence to date has already been sufficient to persuade the Hubble Telescope Imaging committee to grant observation time for transit spectroscopy.
Given a speed of 0. We might have invented some kind of Warp Drive long before a Starshot-class probe arrives at Trappist-1…. But it is not the end of all hope. In that case we will need self-healing probes that can auto-repair any damage and last for centuries in the cold of interstellar space with a near-zero energy consumption.
That is also a technology that will be very useful for Starshot or any slower-than-light probe in the near future when it will be aimed at closer star systems: Both instruments would require significant but not extensive modification. For Proxima b with an 8. The polarimeter essentially blocks out any non polarised starlight in favour of more polarised light reflected off the planet thus helping isolate it.
Once this is done a specifically placed fibre optic targeted on the planet at the mirror feeds direct to ESPRESSO or via the Coude focus though thus would be harder to do. This spectrograph operates only in the visible spectrum as it is optimised for RV exoplanet discovery which is currently favoured for this approach and indeed discovered Proxima b 0n another telescope at la Silla. This would usually be limiting as atmospheric spectra reveal more in the near and mid IR , but as telescope resolution has wavelength as the numerator, the longer IR wavelengths are beyond the resolution of the 8.
This still leaves the circa — nm range of ESPRESSO however which includes several key bio signature and non bio signature absorption lines as discussed last week by Rory Barnes.
Certainly enough to suggest if Proxima b has an atmosphere , is desiccated and Venus like or even more Earth like. This has huge potential implications and could be done over a manageable number of observations nights in favourable conditions years ahead of the ELTs and in far greater detail than JWST. None of which are insurmountable though and the cost of instrumentation upgrades would be millions or a few tens of millions which is tiny in relation to the cost of building a bespoke Space telescope to do this ,which is unlikely for decades.
Geert Barentsen just tweeted the following: Watch out Harry, you are starting to emulate Trump: On Planets in Binary Systems. Comments on this entry are closed. Andrew LePage September 13, , Harry R Ray September 13, , Ashley Baldwin September 14, , Harry R Ray September 18, , Moebius September 14, , 3: Daniel Suggs September 14, , The measurement precision obtained when comparing to ephemeris positions of binaries with very well-known orbits is generally less than 2mas in separation and 0.
Differential photometry is found to have internal precision of approximately 0. We also estimate the detection limit in the cases where no companion was found. Visual orbital elements are derived for six systems. In Table3, we present our measures of double stars. There are a number of binaries observed that have orbits of relatively high quality in the Sixth Catalog of Visual Orbits of Binary Stars Hartkopf et al.
We may use these to further judge the intrinsic accuracy and precision of the measures in Table3. A listing of these objects is given in Table4, together with the orbit information.
We also estimate the detection limit at 0. WIYN speckle observations of binaries. Hipparcos number 53 F9. Of the secondary star relative to the primary, with North through East defining the positive sense.