jeudi 16 juin 2016

Gravitational wave astronomy stays pitch-black (up to now)

No electromagnetic counterparts from optical wavelengths...
We present a search for an electromagnetic counterpart of the gravitational wave source GW151226. Using the Pan-STARRS1 telescope we mapped out 290 square degrees in the optical i_ps filter over a period starting 11.45hr after the LIGO information release (49.48hr after the GW trigger) and lasting for a further 28 days. We typically reached sensitivity limits of i_ps=20.3-20.8 and covered 26.5% of the LIGO probability skymap. We supplemented this with ATLAS survey data, reaching 31% of the probability region to shallower depths of m~19. We found 49 extragalactic transients (that are not obviously AGN), including a faint transient in a galaxy at 7Mpc (a luminous blue variable outburst) plus a rapidly decaying M-dwarf flare. Spectral classification of 20 other transient events showed them all to be supernovae. We found an unusual transient, PS15dpn, with an explosion date temporally coincident with GW151226 which evolved into a type Ibn supernova. The redshift of the transient is secure at z=0.1747 +/- 0.0001 and we find it unlikely to be linked, since the luminosity distance has a negligible probability of being consistent with that of GW151226. In the 290 square degrees surveyed we therefore do not find a likely counterpart. However we show that our survey strategy would be sensitive to Neutron Star-Nentron Star mergers producing kilonovae at D < 100 Mpc, which is promising for future LIGO/Virgo searches.
S. J. Smartt et al, (Submitted on 15 Jun 2016)


 ... to gamma ray ones
We present the Fermi Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) observations of the LIGO binary black hole merger event GW151226 and candi- date LVT151012. No candidate electromagnetic counterparts were detected by either the GBM or LAT. We present a detailed analysis of the GBM and LAT data over a range of timescales from seconds to years, using automated pipelines and new techniques for char- acterizing the upper limits across a large area of the sky. Due to the partial GBM and LAT coverage of the large LIGO localization regions at the trigger times for both events, differences in source distances and masses, as well as the uncertain degree to which emission from these sources could be beamed, these non-detections cannot be used to constrain the variety of theoretical models recently applied to explain the candidate GBM counterpart to GW150914.
J. L. Racusin et al, (Submitted on 15 Jun 2016)

mercredi 15 juin 2016

GW151226 : Second direct detection (first replication) of a gravitational wave detection !

Live : https://iframe.dacast.com/b/59062/c/268750 !






The first available animation !




The Paper !
We report the observation of a gravitational-wave signal produced by the coalescence of two stellar-mass black holes. The signal, GW151226, was observed by the twin detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) on December 26, 2015 at 03:38:53 UTC. The signal was initially identified within 70 s by an online matched-filter search targeting binary coalescences. Subsequent off-line analyses recovered GW151226 with a network signal-to-noise ratio of 13 and a significance greater than 5σ. The signal persisted in the LIGO frequency band for approximately 1 s, increasing in frequency and amplitude over about 55 cycles from 35 to 450 Hz, and reached a peak gravitational strain of 3.4±0.7±0.9×10-22. The inferred source-frame initial black hole masses are 14.2±8.3±3.7M and 7.5±2.3±2.3M, and the final black hole mass is 20.8±6.1±1.7M. We find that at least one of the component black holes has spin greater than 0.2. This source is located at a luminosity distance of 440±180±190 Mpc corresponding to a redshift of 0.09±0.03 ±0.04 . All uncertainties define a 90% credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity
GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence B. P. Abbott et al.* (LIGO Scientific Collaboration and Virgo Collaboration) (Received 31 May 2016; published 15 June 2016) 

mercredi 8 juin 2016

Higgs times seven (minus one) / sept moins une fois le boson de Higgs

750 GeV = 6×125 GeV!

The first LHC data about pp collisions at √ s = 13 TeV agree with the Standard Model (SM), except for a hint of an excess in pp → γγ peaked at invariant mass around 750 GeV [1]. We denote the new resonance with the symbol {digamma}, used in archaic greek as the digamma letter and later as the number 6 ≈ Mz/Mh, but disappeared twice... unlike many other anomalies that disappeared, the γγ excess cannot be caused by a systematic issue, neither experimental nor theoretical. Theoretically, the SM background is dominated by tree-level q→ γγ scatterings, which cannot make a γγ resonance [See {below} for a attempt of finding a Standard Model interpretation.] Experimentally, one just needs to identify two photons and measure their energy and direction. The γγ excess is either the biggest statistical fluctuation since decades, or the main discovery.
(Submitted on 30 May 2016)


750 GeV scalar boson = (6 top quarks + 6 antitop quarks) bound state?
We shall here explore the possibility that the diphoton excess in the inclusive γγ spectrum, recently found by the ATLAS and CMS collaborations [1, 2], with a mass of 750 GeV can be a bound state of particles already present in the Standard Model, namely a bound state of 6 top + 6 antitop quarks. Thus we would need no new fundamental particles, interactions or free parameters beyond the Standard Model to explain this peak, which otherwise looks like “new physics”!  
For several years we have worked on the somewhat controversial idea [3, 4, 5, 6, 7, 8] that the exchange of Higgses and gluons between 6 top and 6 antitop quarks provides sufficiently strong attraction between these quarks for a very light (compared to the mass of 12 top quarks) bound state S to be formed. The 6 tops + 6 antitops are all supposed to be in the 1s state in the atomic physics notation and, because of there being just 3 colors and 2 spin states for a top-quark, this is the maximum number allowed in the 1s shell. 
Further speculations around this bound state were mostly built up under the assumption of a hoped for new principle – the multiple point principle [9, 10, 11] – from which we actually predicted the mass of the Higgs boson long before it was found [12]. This principle says that there shall be several phases of space (i.e. several vacua) with the same energy density. One of these should have a condensate of the bound states S. It was even speculated then that such a condensate – or new vacuum – could form the interior of balls, containing highly compressed ordinary matter, which make up the dark matter [13, 14, 15]. Thus the discovery, if confirmed, of the bound state S could support a theory, in which dark matter could be incorporated into a pure Standard Model theory, only adding the multiple point principle, which predicts the values of coupling constants but otherwise without new physics.
(Submitted on 12 May 2016)

mardi 12 avril 2016

Riding on a laser beam ...

...  to chase the Starshot interstellar flight dream?


In the nearly 60 years of spaceflight we have accomplished wonderful feats of exploration that have shown the incredible spirit of the human drive to explore and understand our universe. Yet in those 60 years we have barely left our solar system with the Voyager 1 spacecraft launched in 1977 finally leaving the solar system after 37 years of flight at a speed of 17 km/s or less than 0.006% the speed of light. As remarkable as this is we will never reach even the nearest stars with our current propulsion technology in even 10 millennium. We have to radically rethink our strategy or give up our dreams of reaching the stars, or wait for technology that does not currently exist. While we all dream of human spaceflight to the stars in a way romanticized in books and movies, it is not within our power to do so, nor it is clear that this is the path we should choose. We posit a technological path forward, that while not simple, it is within our technological reach. We propose a roadmap to a program that will lead to sending relativistic probes to the nearest stars and will open up a vast array of possibilities of flight both within our solar system and far beyond. Spacecraft from gram level complete spacecraft on a wafer ("wafersats") that reach more than 1/4 c and reach the nearest star in 20 years to spacecraft with masses more than 10^5 kg (100 tons) that can reach speeds of greater than 1000 km/s. These systems can be propelled to speeds currently unimaginable with existing propulsion technologies. To do so requires a fundamental change in our thinking of both propulsion and in many cases what a spacecraft is. In addition to larger spacecraft, some capable of transporting humans, we consider functional spacecraft on a wafer, including integrated optical communications, imaging systems, photon thrusters, power and sensors combined with directed energy propulsion.

...Directed energy systems are ubiquitous, used throughout science and industry to melt or vaporize solid objects, such as for laser welding & cutting, as well as in defense. Recent advances in photonics now allow for a 2D array of phase locked laser amplifiers fed by a common low power seed laser that have already achieved near 50% wall plug conversion efficiency. It is known as a MOPA (Master Oscillator Power Amplifier) design. 
Schematic design of phased array laser driver. Wavefront sensing from both local and extended systems combined with the system metrology are critical to forming the final beam.

The technology is proceeding on a "Moore's Law" like pace with power per mass at 5 kg/kW with the size of a 1 kW amplifier not much larger than a textbook. There is already a roadmap to reduce this to 1 kg/kW in the next 5 years and discussions for advancing key aspects of the technology to higher TRL are beginning. These devices are revolutionizing directed energy applications and have the potential to revolutionize many related applications. Due to the phased array technology the system can simultaneous send out multiple beams and thus is inherently capable of simultaneous multitasking as well as multi modal.  
The laser system can be built and tested at any level from desktop to extremely large platforms. This is radically different than the older "use a huge laser" approach to photon propulsion. This is the equivalent to modern parallel processing vs an older single processor supercomputer




Parameters for full class 4 [a 10 km array] system with 1 g wafer SC and 1 m sail. Craft achieves 0.2 c in about 10 min (assuming an extended illumination) and takes about 20 years to get to Alpha Centauri. Communications rate assumes class 4 drive array is also used for reception with a 1 watt short burst from a 100 mm wafer SC. Here we use the 1 meter drive reflector as the transmit and receive optical system on the spacecraft. We also assume a photon/bit ratio near unity. In this case we get a data rate at Andromeda of about 65 kb/s. In the previous figure for the same wafer scale spacecraft the only optical system on the spacecraft was the 100 mm wafer. The data rate received at the Earth from Alpha Centauri is about 0.65 kbs during the burst assuming we can use the DE-STAR 4 driver as the receiver and only the wafer itself for the transmission optic. The plot above shows a much more conservative photon/bit ratio of 40 while unity has been achieved but never over the extremely long distances discussed here.
(Submitted on 5 Apr 2016 (v1), last revised 7 Apr 2016 (this version, v2))


//added on April 13, 2016: I guess some of the advances in photonics are spin-off applications of the late Strategic Defense Initiative but it is fascinating that they could be the backbone of the new Yuri Milner scientific/speculative breakthrough initiative publicized yesterday.
Anyway the future of large phased-array lasers in Earth orbit could definitely be in Directed Energy System for Targeting of Asteroids and exploRation at a time when nuclear ballistic missiles are likely not the most pressing threat anymore...

dimanche 3 avril 2016

After astrophysics and condensed matter theory, holography meets biology

No comment // almost
Holographic Biology 

There are successful applications of the holographic AdS/CFT correspondence to high energy and condensed matter physics. We apply the holographic approach to photosynthesis that is an important example of nontrivial quantum phenomena relevant for life which is being studied in the emerging field of quantum biology. Light harvesting complexes of photosynthetic organisms are many-body quantum systems, in which quantum coherence has recently been experimentally shown to survive for relatively long time scales even at the physiological temperature despite the decohering effects of their environments. We use the holographic approach to evaluate the time dependence of entanglement entropy and quantum mutual information in the Fenna-Matthews-Olson (FMO) protein-pigment complex in green sulfur bacteria during the transfer of an excitation from a chlorosome antenna to a reaction center. It is demonstrated that the time evolution of the mutual information simulating the Lindblad master equation in some cases can be obtained by means of a dual gravity describing black hole formation in the AdS-Vaidya spacetime. The wake up and scrambling times for various partitions of the FMO complex are discussed.
(Submitted on 30 Mar 2016)

Holographic Mystique

Thus far, in spite of many interesting developments, the overall progress towards a systematic study and classification of various ’strange’ metallic states of matter has been rather limited. To that end, it was argued that a recent proliferation of the ideas of holographic correspondence originating from string theory might offer a possible way out of the stalemate. However, after almost a decade of intensive studies into the proposed extensions of the holographic conjecture to a variety of condensed matter problems, the validity of this intriguing approach remains largely unknown. This discussion aims at ascertaining its true status and elucidating the conditions under which some of its predictions may indeed be right (albeit, possibly, for a wrong reason).

... some limited form of a bulk-boundary relationship might, in fact, be quite robust and hold regardless of whether or not the systems in question possess any particular symmetries, unlike in the original AdS/CFT construction. Naively, this form of correspondence can even be related to the Einstein’s equivalence principle (i.e., ’curvature equals force’), according to which free motion in a curved space should be indistinguishable from the effect of a physical interaction (only, this time around, in the tangential direction). 
...
Together with the systematic comparison between the predictions of the condensed matter theory holography and other, more traditional, approaches and/or experimental data it would be a necessary step towards vetting the intriguing, yet speculative, holographic ideas before the latter can be rightfully called a novel technique for tackling the ’strange metals’ and other strongly correlated materials. In any event, though, it would seem rather unlikely that a hands-on expertise in string theory will become a mandatory prerequisite for understanding the cuprates.
(Submitted on 31 Mar 2016)

Holographic Universe
... the AdS/CFT correspondence and holographic dualities have aroused immense enthusiasm in the string theory community. This constitutes, after all, normal scientific research. The phenomenon is still puzzling[45]. At a minimum, the holographic duality is an interesting tool for calculating fundamental physics. The dictionary the duality offers—between a world in flat space-time and a curved world with gravity—works in both directions. Some calculations are simpler with supergravity than in dual gauge theory. 
Gauge/gravity duality has enhanced the stature of Albert Einstein’s own theory...But, despite its recognized elegance, general relativity has been used by only a small portion of the scientific community. This is not surprising. After all, general relativity seemed confined to cases of strongly curved space-time: compact stars, the big bang, gravitational waves. Its effects were utterly negligible at the scales at work in condensed matter physics and nuclear physics. Why should gravity play a role in the quantum world? Yet, over the last twenty years general relativity has finally penetrated the world of modern physics. Specialists in condensed matter, nuclear physics, fluid turbulence, and quantum information are actively interested in general relativity. 
Why this dramatic turnaround? 
As science progresses, the virtues of cross-fertilization between different areas of knowledge have become widely appreciated. But this is the result rather than the cause. The key factor has been the AdS/CFT correspondence. Thanks to general relativity and its string theory extensions, one can now describe phenomena that have nothing to do with gravity in strong fields. 
On the other hand, the AdS/CFT correspondence has not been mathematically demonstrated. The holographic principle remains a conjecture. 
Its degree of experimental verification is zero. 
String theorists believe in it because their theory supports a specific version of holography, and, under certain important restrictions, black hole thermodynamics suggests it as well. But to conclude that it is a correct representation of nature is an enormous leap. 
We still do not know if string theory is correct. Let us suppose it is. Different formulations of the holographic principle have been tested only in situations that do not correspond to our world. The ensuing equations describe possible worlds that are similar, but not identical to our own. Extant solutions have allowed us to test the principles of string theory in limiting cases and to show the consistency of the theory, but never in situations corresponding exactly to the world in which we live. 
Suppose, on the other hand, that string theory proves false. What would become of the AdS/CFT correspondence? In loop quantum gravity, space-time emerges as the coarse-graining of fundamental structures made discrete, the atoms of space. The formation of a black hole and its ultimate evaporation are described by a unitary process that respects the laws of quantum mechanics [46] Similarly, the black holes described in the approach to non-commutative geometry do not evaporate completely and therefore escape the information paradox [47] The holographic conjecture has nonetheless improved the epistemological status of black holes. 
Their status was not always so elevated. The first exact solution of general relativity describing the space-time of a black hole was discovered by Karl Schwarzschild in 1916. Until the 1950s, general relativity theorists were embarrassed by black holes because of their singularities. Later they seemed esoteric objects, hardly believable. Then, in the decades between 1960 and 1990, they became both relevant to astrophysics, and fascinating in their own right. As we have seen, black holes have proven key for understanding quantum gravity, and the deep dualities between distant fields of theoretical physics. Perhaps someday they will become ubiquitous, because they have become useful in the description of everyday systems.  
Volume Two, Issue One, published February 9, 2016




vendredi 26 février 2016

Oh, gravitational waves, jingle, jingle in all the bands!

Dashing through space and time...
We show that the black hole binary (BHB) coalescence rates inferred from the advanced LIGO (aLIGO) detection of GW150914 imply an unexpectedly loud GW sky at milli-Hz frequencies accessible to the evolving Laser Interferometer Space Antenna (eLISA), with several outstanding consequences. First, up to thousands of BHB will be individually resolvable by eLISA; second, millions of non resolvable BHBs will build a confusion noise detectable with signal-to-noise ratio of few to hundreds; third – and perhaps most importantly – up to hundreds of BHBs individually resolvable by eLISA will coalesce in the aLIGO band within ten years. eLISA observations will tell aLIGO and all electromagnetic probes weeks in advance when and where these BHB coalescences are going to occur, with uncertainties of <10s and <1deg2 . This will allow the pre-pointing of telescopes to realize coincident GW and multi-wavelength electromagnetic observations of BHB mergers. Time coincidence is critical because prompt emission associated to a BHB merger will likely have a duration comparable to the dynamical time-scale of the systems, and is only possible with low frequency GW alerts



The multi-band GW astronomy concept. The violet lines are the total sensitivity curves (assuming two Michelson) of three eLISA configurations; from top to bottom N2A1, N2A2, N2A5 (from [11]). The orange lines are the current (dashed) and design (solid) aLIGO sensitivity curves. The lines in different blue flavours represent characteristic amplitude tracks of BHB sources for a realization of the flat population model (see main text) seen with S/N> 1 in the N2A2 configuration (highlighted as the thick eLISA middle curve), integrated assuming a five year mission lifetime. The light turquoise lines clustering around 0.01Hz are sources seen in eLISA with S/N< 5 (for clarity, we down-sampled them by a factor of 20 and we removed sources extending to the aLIGO band); the light and dark blue curves crossing to the aLIGO band are sources with S/N> 5 and S/N> 8 respectively in eLISA; the dark blue marks in the upper left corner are other sources with S/N> 8 in eLISA but not crossing to the aLIGO band within the mission lifetime. For comparison, the characteristic amplitude track completed by GW150914 is shown as a black solid line, and the chart at the top of the figure indicates the frequency progression of this particular source in the last 10 years before coalescence. The shaded area at the bottom left marks the expected confusion noise level produced by the same population model (median, 68% and 95% intervals are shown). The waveforms shown are second order post-Newtonian inspirals phenomenologically adjusted with a Lorentzian function to describe the ringdown.

...  in a three-arm LISA!
The observation of GW150914 brings unexpected prospects in multi-band GW astronomy, providing even more compelling evidence that a milli-Hz GW observatory will not only open a new window on the Universe, but will also naturally complete and enhance the payouts of the high frequency window probed by aLIGO. The scientific potential of multi-band GW astronomy is enormous, ranging from multimessenger astronomy, cosmology and ultra precise gravity tests with BHBs, to the study of the cosmological BHB merger rate, and to the mutual validation of the calibration of the two GW instruments. This is a unique new opportunity for the future of GW astronomy, and how much of this potential will be realized in practice, depends on the choice of the eLISA baseline. Should an extremely de-scoped design like the New Gravitational Observatory (NGO) [27] be adopted, all the spectacular scientific prospects outlined above will likely be lost. Re-introducing the third arm (i.e. six laser links) and increasing the arm-length to at least two million kilometres (A2) will allow observation of more than 50 resolved BHB with both eLISA and aLIGO, and the detection of the unresolved confusion noise with S/N> 30. We also stress that the most interesting systems emit at f > 10−2Hz, a band essentially ’clean’ from other sources. There, the eLISA sensitivity critically depends on the shot noise, which is determined by the number of photons collected at the detector mirrors. It is therefore important to reconsider the designed mirror size and laser power under the novel appealing prospect of observing more of these BHBs and with an higher S/N.
(Submitted on 22 Feb 2016)

Given its tremendous potential for fundamental physics and astrophysics, the European Space Agency (ESA) has selected the observation of the Universe at GW frequencies around one mHz as one of the three main science themes of the “Cosmic Vision Program” [42]. Indeed, a call for mission proposals for the “Gravitational Universe” science theme is expected for late 2016, and the L3 launch slot in 2034 has been reserved for the selected mission. The main candidate mission for this call (for which a decision will be made by 2018-19, so as to allow sufficient time for industrial production before the nominal 2034 launch date) is the evolving Laser Interferometer Space Antenna (eLISA) [43], named after the “classic LISA” concept of the late 90’s and early 2000s [44]. The eLISA mission concept consists of a constellation of three spacecraft, trailing the Earth around the Sun at a distance of about fifteen degrees. Each spacecraft will contain one or two test masses in almost perfect free fall, and laser transponders which will allow measurements of the relative proper distances of the test masses in different spacecraft via laser interferometry. This will allow the detection of the effect of possible GW signals (which would change the distance between the test masses). The most technically challenging aspect of the mission will be to maintain the test masses in almost perfect free fall. For this reason, a scaled-down version of one of eLISA’s laser links will be tested by the “LISA Pathfinder” mission. Pathfinder was launched by ESA in December 2015, and it will provide crucial tests of how well eLISA’s low frequency acceleration noise can be suppressed. 
... 
There are, however, other aspects to the eLISA mission that are yet to be evaluated and decided upon by ESA, within the constraints imposed by the allocated budget for the “Gravitational Universe” science theme. A “Gravitational Observatory Advisory Team” (GOAT) [45] has been established by ESA to advise on the scientific and technological issues pertaining to an eLISA-like mission. Variables that affect the cost of the mission include: (i) the already mentioned low-frequency acceleration noise; (ii) the mission lifetime, which is expected to range between one and several years, with longer durations involving higher costs because each component has to be thoroughly tested for the minimum duration of the mission, and may also require higher fuel consumption, since the orbital stability of the triangular constellation sets an upper limit on the mission duration and therefore achieving a longer mission may require the constellation to be further from the Earth; (iii) the length L of the constellation arms, which may range from one to several million km, with longer arms involving higher costs to put the constellation into place and to maintain a stable orbit and slowly varying distances between the spacecraft; (iv) the number of laser links between the spacecraft, i.e., the number of “arms” of the interferometer (with four links corresponding to two arms, i.e., only one interferometer, and six links to three arms, i.e., two independent interferometers at low frequencies [46]): giving up the third arm would cut costs (mainly laser power, industrial production costs), while possibly hurting science capabilities (especially source localization) and allowing for no redundancy in case of technical faults in one of the laser links.

All the black-hole mergers we take?
Gravitational waves penetrate all of cosmic history, which allows eLISA to explore scales, epochs, and new physical effects not accessible in any other way (see figure {below}). Indeed a detectable gravitational wave background in the eLISA band is predicted by a number of new physical ideas for early cosmological evolution (Hogan, 2006, Maggiore, 2000). Two important mechanisms for generating stochastic backgrounds are phase transitions in the early Universe and cosmic strings. 
... the eLISA frequency band of about 0.1 mHz to 100 mHz today corresponds to the horizon at and beyond the Terascale frontier of fundamental physics. This allows eLISA to probe bulk motions at times about 3×10-18 – 3×10-10 seconds after the Big Bang, a period not directly accessible with any other technique. Taking a typical broad spectrum into account, eLISA has the sensitivity to detect cosmological backgrounds caused by new physics active in the range of energy from 0.1 TeV to 1000 TeV, if more than a modest fraction ΩGW of about 10-5 of the energy density is converted to gravitational radiation at the time of production 
Various sources of gravitational wave background of cosmological origin are presented in detail in Binétruy et al.(2012)...

The observed (redshifted) frequency of wave-generating phenomena is shown as a function of cosmic scale factor a, with the present epoch at the right. The redshifted Hubble rate (horizon scale) is shown in black for a standard Grand Unified Theory (GUT) and a lower temperature Terascale (TeV) inflationary cosmology. Blue regions are accessible to electromagnetic (EM) observations: the Universe since recombination (right box) and cosmic microwave background (CMB) fluctuations (left box). The red bar shows the range of cosmic history accessible through eLISA from processes within the horizon up to about 1000 TeV.

One of the most promising science goals of the mission are supermassive black holes, which appear to be a key component of galaxies. They are ubiquitous in near bright galaxies and share a common evolution. The intense accretion phase that supermassive black holes experience when shining as quasi-stellar objects and active galactic nuclei erases information on how and when the black holes formed. eLISA will unravel precisely this information. Very massive black holes are expected to transit into the mass interval to which eLISA is sensitive along the course of their cosmic evolution. eLISA will then map and mark the loci where galaxies form and cluster, using black holes as clean tracers of their assembly by capturing gravitational waves emitted during their coalescence, that travelled undisturbed from the sites where they originated. On the other hand, middleweight black holes of 105M are observed in the near universe, but our knowledge of these systems is rather incomplete. eLISA will investigate a mass interval that is not accessible to current electromagnetic techniques, and this is fundamental to understand the origin and growth of supermassive black holes. Due to the transparency of the universe to gravitational waves at any redshift, eLISA will explore black holes of 105M – 107M out to a redshift z ≤ 20, tracing the growth of the black hole population.  
eLISa will also shed light on the path of black holes to coalescence in a galaxy merger. This is a complex process, as various physical mechanisms involving the interaction of the black holes with stars and gas need to be at play and work effectively, acting on different scales (from kpc down to 10-3 pc). Only at the smallest scales gravitational waves are the dominant dissipative process driving the binary to coalescence. eLISA will trace the last phase of this evolution. Dual active galactic nuclei (AGN), i.e. active black holes observed during their pairing phase, offer the view of what we may call the galactic precursors of black hole binary coalescences. They are now discovered in increasing numbers, in large surveys. By contrast, evidence of binary and recoiling AGN is poor, as the true nature of a number of candidates is not yet fully established. eLISA only will offer the unique view of an imminent binary merger by capturing its loud gravitational wave signal...  
Current electromagnetic observations are probing only the tip of the massive black hole distribution in the universe, targeting black holes with large masses, between 107M – 109M . Conversely, eLISA will be able to detect the gravitational waves emitted by black hole binaries with total mass (in the source rest frame) as small as 104 M and up to 107 M , out to a redshift as remote as z ∼ 20. eLISA will detect fiducial sources out to redshift z 10 with SNR  10 and so it will explore almost all the mass-redshift parameter space relevant for addressing scientific questions on the evolution of the black hole population. Redshifted masses will be measured to an unprecedented accuracy, up to the 0.1–1% level, whereas absolute errors in the spin determination are expected to be in the range 0.01–0.1, allowing us to reconstruct the cosmic evolution of massive black holes. eLISA observations hence have the potential of constraining the astrophysics of massive black holes along their entire cosmic history, in a mass and redshift range inaccessible to conventional electromagnetic observations 
On smaller scales, eLISA will also bring a new revolutionary perspective, in this case relative to the study of galactic nuclei. eLISA will offer the deepest view of galactic nuclei, exploring regions to which we are blind using current electromagnetic techniques and probing the dynamics of stars in the space-time of a Kerr black hole, by capturing the gravitational waves emitted by stellar black holes orbiting the massive black hole. Extreme mass ratio inspirals (EMRI) detections will allow us to infer properties of the stellar environment around a massive black hole, so that our understanding of stellar dynamics in galactic nuclei will be greatly improved. Detection of EMRIs from black holes in the eLISA mass range, that includes black holes similar to the Milky Way’s, will enable us to probe the population of central black holes in an interval of masses where electromagnetic observations are challenging... 
General Relativity has been extensively tested in the weak field regime both in the solar system and by using binary pulsars. eLISA will provide a unique opportunity of confronting GR in the highly dynamical strong field regime of massive black holes. eLISA will be capable of detecting inspiral and/or merger plus ring-down parts of the gravitational wave signal from coalescing massive black holes binaries of comparable mass. For the nearby events (z ∼ 1) the last several hours of the gravitational wave signal will be clearly seen in the data, allowing direct comparison with the waveforms predicted by GR. The inspiral phase could be observed by eLISA up to a year before the final merger with relatively large SNR. Comparison of the observed inspiral rate with the predictions of GR will provide a valuable test of the theory in the regime of strong, dynamical gravitational fields. 
The merger of two black holes could be observed by eLISA throughout the Universe if it falls into the detector band. 
Pau Amaro-Seoane et al.
(Submitted on 17 Jan 2012)

mercredi 24 février 2016

Taking (some) fun out of {go fast} scientific [reports]

Wet blanket policy...
Disclaimer: this first paragraph is just cheap entertaining and self-deprecating of the blogger, no offence to any real scientist of course!
The playful science popularizer Bob Burstard is looking for a freshsucker to swindle. Looking off in the distance, Bob sees a happy-go-lucky science enthusiast Alice Arxivpecker, minding the recent discovery of gravitational waves (GW) while whistling through internet. The cunning Burstard quickly types a draft report and polishes a catchy headline, causing Alice to web surf directly through his front page. He then tries to show her his theory to explain the Gamma-Ray Burst serendipitously detected 0.4 seconds after the GW event...

Then comes some serious information.

... on a Gamma ray burst associated with GW150914

The Fermi/GBM team reported a possible hard X-ray transient on 2015-09-14 at 09:50:45.8 UTC, about 0.4 s after the reported LIGO/Virgo burst trigger time, and lasting for about one second (Blackburn et al. 2015; Connaughton, V. et al 2016). The light travel time can introduce a time difference between INTEGRAL and Fermi detections of up to ±0.5 s, depending on the source position within the LVC error region. We do not observe any excess within a -0.5 s to +0.5 s window around the Fermi/GBM trigger (Figure 1), and set a 3-sigma upper limit of 1.5×10-7erg cm-2 in one second, assuming a typical short hard GRB, characterized by Band model with parameters α = −0.5, β = −2.5, Epeak = 1000 keV. A substantial part of the candidate event in the GBM comes from the high-energy BGO detector, above 100 keV (Blackburn et al. 2015), where the Fermi/GBM effective area is about a factor 30-40 smaller than that of the INTEGRAL/SPI-ACS... Finally, we stress that to compare the GBM and SPI-ACS sensitivities, it is inappropriate to use a soft spectral model as in the computation of our early flux upper limits (Ferrigno et al. 2015), since the spectral properties of the GBM candidate are very different.
V. Savchenko et al., (Submitted on 12 Feb 2016)



... a search of the INTEGRAL-ACS data revealed a detection rate of only 55% of GBM-detected weak short GRBs (Briggs et al., in preparation). We do not consider, therefore, the non-detection of GW150914-GBM by INTEGRAL-ACS, a sufficient reason to reject our candidate
V. Connaughton, et al. 
(Submitted on 11 Feb 2016 (v1), last revised 16 Feb 2016 (this version, v3))



... and the first evidence for nearly neutral black holes?
I have shown that for black hole - black hole (BH-BH) mergers, if at least one of the BHs carry even a small amount of charge Q, the inspiral process generates a loop circuit, which induces a magnetic dipole. The system behaves like a giant pulsar with an increasing wind power. If q can be as large as ∼ (10-5 − 10-4), the magnetospheric wind right before the coalescence would make a short-duration GRB. The GRB is expected to be delayed with respect to the GW chirp signal. The putative short GRB signal associated with GW 150914 (Connaughton et al. 2016) can be well interpreted with this theory. 
The nearly isotropic nature of this wind pulse suggests that every BH-BH merger could be associated with a short electromagnetic transient if Q is not strictly zero. The question is whether q can be large enough to make it observable. Given the large event rate of BH-BH mergers revealed by the detection of GW 150914 (Abbott et al. 2016b), the non-detection of very bright short GRBs already suggests that for the majority of BHs, q cannot significantly exceed 10-5. This is consistent with the general expectation that BHs are essentially not charged. Pessimistically, the weak short GRB signal detected by the Fermi/GBM team ... is a chance coincidence and non-physical. If so, the upper limit of a signal (Savchenko et al. 2016) would constrain q to be below a few 10-5 .
Bing Zhang (UNLV)
(Submitted on 15 Feb 2016 (v1), last revised 16 Feb 2016 (this version, v2))

//update February 26 2016
The physical constraints required by the association of the Fermi GBM signal contemporaneous with GW150914 - radiative power of 1049 erg.s-1 , and corresponding magnetic fields on the black hole of the order of 1012 Gauss - are astrophysically highly implausible. Combined with the relatively high random probability of coincidence of 0.22 percents, we conclude that the electromagnetic signal is likely unrelated to the BH merger. 
... requiring that the magnetic field is produced by electric charge on one of the black holes (Zhang 2016) would imply a charge Q = GM√(LEM)c5/2 = 5×1016 coulombs. This horrific amount of electric charge would have produced the electric field near the horizon E = √(LEM)c3/2/(GM)=2×1012 in cgs units (statvolts per centimeter), amounting to nearly 5% of the quantum Schwinger field EQ = me2c3/(e).
Maxim Lyutikov (Purdue University)
(Submitted on 23 Feb 2016)