Home
# Abstracts

## List of scientific registered participants

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AMARO-SEOANE Pau | Oral |

Doing Gravitational Wave Astronomy with the gravitational capture of compact objects | |

2016 has been so far a revolutionary year in science. The direct detections of gravitational waves from the merger of black holes has put an end to the pre Gravitational Wave Era. Thanks to the features of these waves, we can probe regimes where photons can barely escape, and achieve cosmological distances. In this talk I will discuss the potential of Gravitational Wave Astronomy and in particular from future space observatories, such as the planned LISA mission. I will focus on the capture of small compact objects by supermassive black holes. We these captures we will test gravity in the strong regime, because they allow us to do relativistic geodesy - They are unique event horizon probes. |

ANDERSSON Nils | Oral |

Continuous gravitational waves: From mountains to unstable waves | |

Neutron stars may radiate gravitational waves in a variety of ways. Several astrophysically motivated scenarios lead to long-lived, low-amplitude waves, but the search for such continuous gravitational waves is challenging given the need to integrate over long stretches of data to increase the signal-to-noise ratio. At the same time it is tricky to provide templates for these signals that remain reliable for weeks to years. In this talk I will provide an overview of the main mechanisms that lead to long-lived gravitational waves, explain the state of the art on the modelling side and discuss how the upper limits from recent searches are beginning to constrain neutron-star physics in interesting ways. |

ANDRESEN Haakon | Oral |

Gravitational Wave Signals from 3D Simulations of Core-Collapse Supernovae | |

To this day, the exact nature of the detonation mechanism in core collapse supernovae reminds somewhat of a mystery. While numerical models are becoming more and more sophisticated, observations of the inner engine remain elusive. Electromagnetic radiation can only provide indirect information, because the core is surrounded by dense stellar matter. Neutrinos and gravitational waves, on the other hand, can propagate almost unhindered through the stellar material. For the last decade, or so, supernova modellers have predicted gravitational wave signatures based on their simulations. I will present a detailed analysis of the gravitational wave signal from four sophisticated three-dimensional simulations of based on three different stellar progenitors. The theoretical signal from our simulations consists of two distinct features: One emission component below 250 Hz and one above 300 Hz. The signal above 300 Hz is present in all models. While, on the other hand, the signal below 250 Hz is only visible in three out of four models. In my talk, I will examine the different physical processes that excite the two signal components and shed light on the discrepancies between models. I will also discuss the detection possibilities in current, and future, ground-based detectors. I will focus on the possibility to differentiate between the four models. |

BABAK Stas | Oral |

Modelling gravitational wave signals from binary black holes | |

In this talk I will review the inspiral-merger-ringdown models for detecting gravitational wave signal from binary black holes with particular focus on the "effective-one-body'' approach. Then I will review models describing GW signal from precessing binaries and their use in estimating parameters of binary systems. |

BERNARD Laura | Oral |

Dynamics of non-spinning compact binary systems at the fourth post-Newtonian order | |

In this talk, I will address the question of the dynamics of compact binary systems at the fourth post-Newtonian order in harmonic coordinates. This work is important in view of the detection and precise determination of the physical parameters of gravitational waves by the current and next generations of interferometric detectors. During the inspiral phase of the coalescence, when the two objects are widely separated, the perturbative post-Newtonian approach allows one to describe the dynamics of the compact binary system and to compute the radiation energy flux, from which the orbital phase evolution can be derived. I will present the method, based on a Fokker action adapted to the specificities of the post-Newtonian formalism in harmonic coordinates, that we used to compute the conservative dynamics at 4PN. In particular, I will focus on the treatment of the so-called tail effects which appear for the first time in the dynamics at 4PN. |

BERRY Christopher | Oral |

Discoveries from Advanced LIGO | |

The first observing run (O1) of Advanced LIGO has now concluded. It yielded the first gravitational wave detections, with three potential binary black hole mergers GW150914, GW151226 and LVT151012. This talk reviews what we have learnt from O1, and what future discoveries gravitational-wave astronomy could produce. We look in detail at the measured properties of the black holes, and what how this could inform our understanding of their formation. |

BIZOUARD Marie Anne | Oral |

A review of the LIGO-Virgo gravitational wave searches in the LIGO O1 data | |

In this presentation I will present the most up-to-date results obtained with the O1 LIGO data. This will also include a summary of the LIGO Virgo detectors preparation in view of the O2 run that will start in September 2016. |

CAPRINI Chiara | Oral |

The effect of matter perturbations on the chirp signal | |

Both the background expansion of the universe and the perturbation of the redshift due to the inhomogeneous matter structure have an impact on the amplitude and the phase of the GW signal from binaries. We present the derivation of this effect and quantify its impact in terms of lost detections in eLISA. |

CHATY Sylvain | Oral |

X-ray binaries as progenitors of gravitational waves | |

Low-mass and High-mass X-ray binaries are potential emitters of gravitational waves at various stages, during or at the end of their evolution. I will review the properties and evolutionary steps of these astrophysical candidates. |

COLPI Monica | Oral |

The path to coalescence of massive black hole pairs | |

There is growing evidence that Nature provides through galaxy mergers the habitat where massive black holes pair, grow and merge, becoming the loudest sources of gravitational waves in the universe. During a major merger, the black holes nested inside their own bulges sink under the action of dynamical friction, and pair. In this phase black holes can become bright "dual-AGN". As the merger reaches completion, the black holes end forming a close Keplerian binary which continues to harden transferring angular momentum to gas and stars, inside a live, ever changing environment. A circum-binary disc can fuel the black holes and accelerate their inspiral. When the separation falls below a milli parsec gravitational waves drive their inspiral down to coalescence. In this talk, we review state-of-the-art simulations describing the long journey travelled by black holes in colliding galaxies, and show how the information contained in the gravitational wave signal can shed light into the process of black hole seed formation and evolution, across all cosmic ages. |

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CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV \ | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

1'" | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1*257*252*0 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1*1*1*1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1*425*420*0 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

11*5*2*999 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1*458*453*0 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

11*5*2*999 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

11*5*2*999 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

-1 OR 3+527-527-1=0+0+0+1 -- |

CPJJWWHV CpjJwWHV | None |

Mr. | |

SbcIpcWH')); waitfor delay '0:0:3' -- |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1 OR 3+137-137-1=0+0+0+1 -- |

CPJJWWHV CpjJwWHV | None |

Mr. | |

-1);select pg_sleep(3); -- |

CPJJWWHV CpjJwWHV | None |

Mr. | |

0eb5StlY');select pg_sleep(9); -- |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1 OR 3+868-868-1=0+0+0+1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1 OR 3*2<(0+5+868-868) |

CPJJWWHV CpjJwWHV | None |

Mr. | |

if(now()=sysdate(),sleep(6),0) |

CPJJWWHV CpjJwWHV | None |

Mr. | |

0"XOR(if(now()=sysdate(),sleep(3),0))XOR"Z |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1' OR 3+178-178-1=0+0+0+1 -- |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1; waitfor delay '0:0:9' -- |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV -1 OR 2+1-1-1=1 AND 630=630 | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV QovU9e7o | None |

Mr. | |

1 |

CPJJWWHV -1 OR 2+486-486-1=0+0+0+1 -- | None |

Mr. | |

1 |

CPJJWWHV -1 OR 3*2>(0+5+486-486) -- | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV -1 OR 630=630 AND 3+1-1-1=1 | None |

Mr. | |

1 |

CPJJWWHV -1' OR 3+368-368-1=0+0+0+1 -- | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV -1' OR 2+1-1-1=1 AND 934=934 or '7eE51gmp'=' | None |

Mr. | |

1 |

CPJJWWHV 1 waitfor delay '0:0:9' -- | None |

Mr. | |

1 |

CPJJWWHV 0rJrDP5n | Poster |

Mr. | |

1 |

CPJJWWHV NP9gBtts'); waitfor delay '0:0:6' -- | None |

Mr. | |

1 |

CPJJWWHV -1 OR 2+75-75-1=0+0+0+1 -- | Poster |

Mr. | |

1 |

CPJJWWHV tK8E86uQ')); waitfor delay '0:0:9' -- | None |

Mr. | |

1 |

CPJJWWHV -1 OR 2+650-650-1=0+0+0+1 | Poster |

Mr. | |

1 |

CPJJWWHV -1' OR 3*2<(0+5+946-946) or 'TV0EFdxa'=' | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

-1' OR 2+736-736-1=0+0+0+1 -- | |

1 |

CPJJWWHV -1" OR 3*2>(0+5+567-567) -- | Poster |

Mr. | |

1 |

CPJJWWHV -1" OR 567=567 AND 3+1-1-1=1 -- | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

-1" OR 2+988-988-1=0+0+0+1 -- | |

1 |

CPJJWWHV CpjJwWHV | None |

-1" OR 3+988-988-1=0+0+0+1 -- | |

1 |

CPJJWWHV CpjJwWHV | None |

1 waitfor delay '0:0:6' -- | |

1 |

CPJJWWHV -1" OR 3*2=5 AND 567=567 -- | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

4ldIATUe'); waitfor delay '0:0:3' -- | |

1 |

CPJJWWHV -1" OR 3*2=6 AND 567=567 -- | Poster |

Mr. | |

1 |

CPJJWWHV -1" OR 3*2*0=6 AND 567=567 -- | Poster |

Mr. | |

1 |

CPJJWWHV 1 waitfor delay '0:0:3' -- | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

S8m9nswb')); waitfor delay '0:0:6' -- | |

1 |

CPJJWWHV CpjJwWHV | None |

qXTMg6Dq';select pg_sleep(6); -- | |

1 |

CPJJWWHV CpjJwWHV | None |

WAA3FJWV');select pg_sleep(6); -- | |

1 |

CPJJWWHV 2mbms4Rh'; waitfor delay '0:0:9' -- | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

if(now()=sysdate(),sleep(3),0) | |

1 |

CPJJWWHV -1' OR 2+946-946-1=0+0+0+1 or 'TV0EFdxa'=' | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV 0"XOR(if(now()=sysdate(),sleep(3),0))XOR"Z | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr.' AND 2*3*8=6*9 AND '0rBN'='0rBN | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

-1 OR 3*2<(0+5+366-366) -- | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

-1 OR 2+17-17-1=0+0+0+1 | |

1 |

CPJJWWHV CpjJwWHV | Poster |

PJfYLLBQ')); waitfor delay '0:0:9' -- | |

1 |

CPJJWWHV CpjJwWHV | Poster |

if(now()=sysdate(),sleep(3),0) | |

1 |

CPJJWWHV CpjJwWHV | Poster |

(select(0)from(select(sleep(6)))v)/*'+(select(0)from(select(sleep(6)))v)+'"+(select(0)from(select(sleep(6)))v)+"*/ | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV -1 OR 3+486-486-1=0+0+0+1 -- | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV -1' OR 934=934 AND 3+1-1-1=1 or '7eE51gmp'=' | None |

Mr. | |

1 |

CPJJWWHV -1' OR 3*2=5 AND 934=934 or '7eE51gmp'=' | None |

Mr. | |

1 |

CPJJWWHV if(now()=sysdate(),sleep(3),0) | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

-1 OR 2+407-407-1=0+0+0+1 -- | |

1 |

CPJJWWHV -1" OR 2+567-567-1=0+0+0+1 -- | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

-1 OR 2+742-742-1=0+0+0+1 | |

1 |

CPJJWWHV CpjJwWHV | None |

-1' OR 2+359-359-1=0+0+0+1 or '1R6MyYM7'=' | |

1 |

CPJJWWHV -1" OR 2+1-1-1=1 AND 567=567 -- | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

0"XOR(if(now()=sysdate(),sleep(3),0))XOR"Z | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV -1' OR 2+934-934-1=0+0+0+1 or '7eE51gmp'=' | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr.%' AND 2*3*8=6*8 AND 'dk3o'!='dk3o% | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

-1 OR 3*2<(0+5+17-17) | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1'" |

CPJJWWHV CpjJwWHV | None |

Mr. | |

\ |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV 1'" | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

1'" | |

1 |

CPJJWWHV CpjJwWHV | None |

\ | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

ywlqkyPG'));select pg_sleep(3); -- |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

0'XOR(if(now()=sysdate(),sleep(6),0))XOR'Z |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV 0"XOR(if(now()=sysdate(),sleep(6),0))XOR"Z | None |

Mr. | |

1 |

CPJJWWHV -1' OR 3*2>(0+5+946-946) or 'TV0EFdxa'=' | Poster |

Mr. | |

1 |

CPJJWWHV -1' OR 2+1-1-1=1 AND 946=946 or 'TV0EFdxa'=' | Poster |

Mr. | |

1 |

CPJJWWHV -1" OR 3+567-567-1=0+0+0+1 -- | Poster |

Mr. | |

1 |

CPJJWWHV -1" OR 3*2<(0+5+567-567) -- | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

U3fPXehD'; waitfor delay '0:0:9' -- | |

1 |

CPJJWWHV CpjJwWHV | None |

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1 |

CPJJWWHV o6YOc5GK'); waitfor delay '0:0:9' -- | Poster |

Mr. | |

1 |

CPJJWWHV IFkFZ1y3')); waitfor delay '0:0:9' -- | Poster |

Mr. | |

1 |

CPJJWWHV EtGRBJf7';select pg_sleep(3); -- | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

0'XOR(if(now()=sysdate(),sleep(3),0))XOR'Z | |

1 |

CPJJWWHV iEwWErsw');select pg_sleep(6); -- | Poster |

Mr. | |

1 |

CPJJWWHV h5ijpzSd'));select pg_sleep(6); -- | Poster |

Mr. | |

1 |

CPJJWWHV if(now()=sysdate(),sleep(6),0) | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

(select(0)from(select(sleep(9)))v)/*'+(select(0)from(select(sleep(9)))v)+'"+(select(0)from(select(sleep(9)))v)+"*/ | |

1 |

CPJJWWHV 0'XOR(if(now()=sysdate(),sleep(9),0))XOR'Z | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

3jkSXU0O | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr.' AND 2*3*8=6*8 AND '0rBN'='0rBN | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr." AND 2*3*8=6*8 AND "mSgu"="mSgu | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

-1 OR 2+366-366-1=0+0+0+1 -- | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

-1 OR 3+366-366-1=0+0+0+1 -- | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

-1 OR 3*2>(0+5+366-366) -- | |

1 |

CPJJWWHV CpjJwWHV | Poster |

-1 OR 2+1-1-1=1 AND 366=366 -- | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

-1 OR 366=366 AND 3+1-1-1=1 -- | |

1 |

CPJJWWHV CpjJwWHV | Poster |

-1 OR 3+17-17-1=0+0+0+1 | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

-1 OR 3*2>(0+5+17-17) | |

1 |

CPJJWWHV CpjJwWHV | Poster |

1 waitfor delay '0:0:3' -- | |

1 |

CPJJWWHV CpjJwWHV | Poster |

sHmOwqY3'; waitfor delay '0:0:6' -- | |

1 |

CPJJWWHV CpjJwWHV | Poster |

VOGSHslx'); waitfor delay '0:0:6' -- | |

1 |

CPJJWWHV CpjJwWHV | Poster |

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1 |

CPJJWWHV CpjJwWHV | Poster |

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1 |

CPJJWWHV CpjJwWHV | Poster |

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1 |

CPJJWWHV CpjJwWHV | Poster |

0'XOR(if(now()=sysdate(),sleep(3),0))XOR'Z | |

1 |

CPJJWWHV CpjJwWHV | Poster |

0"XOR(if(now()=sysdate(),sleep(3),0))XOR"Z | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1' OR 3*2>(0+5+708-708) or 'vHwXg8kQ'=' |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1" OR 3*2<(0+5+120-120) -- |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1); waitfor delay '0:0:3' -- |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

mDChwl7S'; waitfor delay '0:0:6' -- |

CPJJWWHV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

BW3iyIoE'); waitfor delay '0:0:6' -- |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1;select pg_sleep(9); -- |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1);select pg_sleep(9); -- |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

-1));select pg_sleep(9); -- |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1WpTopmf');select pg_sleep(9); -- |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

0"XOR(if(now()=sysdate(),sleep(9),0))XOR"Z |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

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1 |

CPJJWWHV CpjJwWHV | None |

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1 |

CPJJWWHV CpjJwWHV | None |

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CPJJWWHV CpjJwWHV | Poster |

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CPJJWWHV CpjJwWHV | Poster |

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CPJJWWHV CpjJwWHV | Poster |

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CPJJWWHV CpjJwWHV | None |

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CPJJWWHV CpjJwWHV | None |

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CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV -1' OR 3+934-934-1=0+0+0+1 or '7eE51gmp'=' | None |

Mr. | |

1 |

CPJJWWHV -1' OR 3*2>(0+5+934-934) or '7eE51gmp'=' | None |

Mr. | |

1 |

CPJJWWHV CpjJwWHV | Poster |

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1 |

CPJJWWHV -1' OR 3*2=6 AND 934=934 or '7eE51gmp'=' | None |

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CPJJWWHV -1" OR 2+959-959-1=0+0+0+1 -- | None |

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CPJJWWHV D2qvFxRt';select pg_sleep(9); -- | None |

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CPJJWWHV UCBPeQbT');select pg_sleep(3); -- | None |

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CPJJWWHV -1' OR 2+396-396-1=0+0+0+1 -- | Poster |

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CPJJWWHV UlTCX9Gm'));select pg_sleep(3); -- | None |

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CPJJWWHV -1' OR 3+946-946-1=0+0+0+1 or 'TV0EFdxa'=' | Poster |

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CPJJWWHV 0'XOR(if(now()=sysdate(),sleep(3),0))XOR'Z | None |

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CPJJWWHV' AND 2*3*8=6*8 AND 'OVFQ'='OVFQ CpjJwWHV | None |

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1 |

CPJJWWHV' AND 2*3*8=6*8 AND 'Z5TJ'='Z5TJ CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV' AND 2*3*8=6*9 AND 'Z5TJ'='Z5TJ CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV' AND 3*2>(1*5) AND 'Z5TJ'='Z5TJ CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV' AND 3*3<(2*4) AND 'Z5TJ'='Z5TJ CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV" AND 2*3*8=6*8 AND "BF3S"="BF3S CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV" AND 2*3*8=6*8 AND "UYSV"="UYSV CpjJwWHV | None |

Mr. | |

1 |

CPJJWWHV" AND 2*3*8=6*9 AND "BF3S"="BF3S CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV%' AND 2*3*8=6*8 AND '40KM'!='40KM% CpjJwWHV | Poster |

Mr. | |

1 |

CPJJWWHV%' AND 2*3*8=6*8 AND 'XWBL'!='XWBL% CpjJwWHV | None |

Mr. | |

1 |

DE MINK Selma E. | Oral |

The Making of … a Binary Black Hole | |

How does the Universe form binary black holes of stellar origin? Do they originate from the classical formation channel that involves a phase in which two stars briefly share a common envelope? Are they formed in a dense star clusters? Or did they arise from one of the more recently proposed formation channels? One of these is the “chemically homogeneous channel”, which considers the mixing processes that may occur in the interiors of stars in very tight (near) contact binaries that are heavily tidally distorted. Other examples include the family of scenarios that have been recently proposed to occur in galactic nuclei. I will briefly review the main channels proposed to date, followed by a more in depth discussion of the chemically homogeneous evolutionary channel. I will then discuss the key challenges affecting the predictions for these channels and prospectives to distinguish between the various scenarios. |

DOMCKE Valerie | Oral |

Probing the early Universe with gravitational waves | |

Gravitational waves are unique messengers to explore the very early universe, probing energy ranges far beyond the reach of photon or even neutrino astronomy. In this talk, I will discuss possible sources for stochastic gravitational wave backgrounds in the early universe, their connection to particle physics and the possibility of their detection in ground- and space-based interferometers. A special focus will be on possible gravitational wave signals from cosmic inflation. |

DVORKIN Irina | Oral |

Merger rates of binary black holes and the stochastic gravitational wave background | |

The recent detection of the binary black hole merger GW150914 by Advanced LIGO demonstrates the existence of black holes more massive than previously observed in X-ray binaries in our Galaxy. Future observations with Advanced LIGO and VIRGO may be able to distinguish between different models of black hole formation. In this talk I will describe a framework that can be used to calculate the mass distribution of merging black hole binaries and its evolution with redshift in the context of cosmic chemical evolution models. This framework allows to test different scenarios of black hole formation in a self-consistent manner, accounting for observational constraints for the cosmic star formation rate and metallicity of the interstellar medium. I will also discuss the implications of the black hole mass and spin distribution for the stochastic gravitational wave background. |

FURPCJ0G');SELECT PG_SLEEP(9); -- CpjJwWHV | Poster |

Mr. | |

1 |

GDGRBNS7'); WAITFOR DELAY '0:0:9' -- CpjJwWHV | Poster |

Mr. | |

1 |

HEFFERNAN Anna | Oral |

Towards Scalar Tensor Waveforms | |

Now that gravitational wave astronomy is a reality, we can start to explore alternative theories of gravity. Scalar tensor gravity considers a varying Gravitational "constant" with the introduction of a scalar field. Its waveforms could therefore be used by LIGO to test classical general relativity in the case of neutron star binaries. We give a progress report on current PN calculations towards such a waveform production. |

HINDER Ian | Oral |

Gravitational Waveforms from Numerical Relativity | |

Of all the ways to compute gravitational waveforms from the late inspiral and merger of compact object binaries such as black holes, direct numerical solution of the Einstein equations yields the result with the least uncertainty. From the 1970s to 2005, it was not known how to compute such solutions. In 2005, the first long-term successful stable methods were developed, and we now have access to fully general relativistic merger waveforms with errors in principle limited only by computational resources. I will give an overview of waveforms from Numerical Relativity, and how they are used for gravitational wave science. |

HO Wynn | Oral |

Gravitational waves within the magnetar model of superluminous supernovae and gamma-ray bursts | |

The light curve of many supernovae (SNe) and gamma-ray bursts (GRBs) can be explained by a sustained injection of extra energy from its possible central engine, a rapidly rotating strongly magnetic neutron star (i.e., magnetar). The magnetic dipole radiation power that the magnetar supplies comes at the expense of the star's rotational energy. However radiation by gravitational waves (GWs) can be more efficient than magnetic dipole radiation because of its stronger dependence on neutron star spin rate Omega, i.e., Omega^6 (for a static ``mountain'') or Omega^8 (for a r-mode fluid oscillation) versus Omega^4 for magnetic dipole radiation. Here we use the magnetic field B and initial spin period P_0 inferred from SN and GRB observations to obtain simple constraints on the dimensionless amplitude of the mountain of epsilon < 0.01 and r-mode oscillation of alpha < 1, the former being similar to that obtained by recent works. We then include GW emission within the magnetar model. We show that when epsilon > 10^-4 (B/10^14 G) (P_0/1 ms) or alpha > 0.01 (B/10^14 G) (P_0/1 ms)^2, light curves are strongly affected, with significant decrease in peak luminosity and increase in time to peak luminosity. Thus the GW effects studied here are more pronounced for low B and short P_0 but are unlikely to be important in modeling SN and GRB light curves since the amplitudes needed for noticeable changes are quite large. |

IF(NOW()=SYSDATE(),SLEEP(9),0) CpjJwWHV | Poster |

Mr. | |

1 |

IF(NOW()=SYSDATE(),SLEEP(9),0) CpjJwWHV | None |

Mr. | |

1 |

KHODAGHOLIZADEH Jafar | Poster |

The effect of cosmic Neutrinos on the Gravitational waves in matter and lambda dominated era | |

We develop an integro-differential equation for propagation of cosmological gravitation waves in matter dominated era in accounting for the presence of free streaming neutrinos as a traceless transverse tensor part of the anisotropic stress tensor?. ?We focus on the short and long wavelengths of GW's that enter the horizon in matter dominated era?. ?Our results show the anisotropic stress reduces the squared amplitude by $ 0.03\%$ for wavelengths that enter the horizon during matter-dominated phase and this reduction is less for the wavelengths that enter the horizon at $\Lambda $ dominated era? in flat spacetime and then these calculations have been done in closed spacetme. We compare the results with the radiation dominated case for both flat and closed spacetime. At the end we investigate the effect of closed background on the amplitude of the gravitational waves. |

KOROL Valeriya | Oral |

A future challenge for detection of double white dwarf binaries | |

On the basis of our theoretical understanding of stellar and binary evolution around 10^8 double degenerate WD binaries (DDWDs) are expected to be present in our Galaxy. According to binary population synthesis models, half of these systems should have periods shorter than few hours, so that gravitational wave emission will bring them into contact within a Hubble time, making them dominant low-frequency gravitational wave emitters and guaranteed sources for the eLISA mission. In my talk I will present how many of compact DDWDs we will be able to detect 1) through EM radiation with Gaia and LSST and 2) through GW radiation with eLISA. Additionally, detached DDWDs with orbital periods of 20-40 min represent ideal systems to study the reaction of their internal structure to tidal forces. I will show my preliminary results on the role of tidal interaction in the case of J0651 (detached system with orbital period P=12 min). |

KRAMER Michael | Oral |

Probing gravity with radio astronomy | |

There are a number of ways how to probe gravity with radio astronomy. Apart from studying the CMB, perhaps the most well known way is to use radio pulsars. Especially pulsars in compact orbits can be used to probe general relativity and alternative theories of gravity for strongly self-gravitating bodies. Pulsars also provide the most precise tests for gravitational waves, and may as well soon be used as gravitational wave detectors for low frequency gravitational waves. Another application of radio astromomy is the high resolution imaging of the supermassive black hole in the centre of the Galaxy, an experiment that is underway globally under the Event Horizon Telescope project and in Europe with help of the ERC Black Hole Cam project. This talk gives an introduction to these experiments and the aspects that can be especially provided by pulsars. |

LAMB Gavin | Oral |

Low-Gamma Jets from Compact Stellar Mergers - Candidate Electromagnetic Counterparts to Gravitational Wave Sources | |

Short gamma-ray bursts (GRBs) are believed to be produced by relativistic jets from mergers of neutron-stars (NS) and/or black-holes (BH). If the Lorentz-factors $\Gamma$ of jets from compact-stellar-mergers follow a similar power-law distribution as those observed for other high-energy astrophysical phenomena (e.g. blazars, AGN), the jet population would be dominated by low-$\Gamma$ outflow. These jets will not produce GRB (i.e. the prompt gamma-rays), but their jet energy will be released as optical and radio transients when they collide into the ambient medium. By using simple Monte Carlo simulations, we study the properties of such transient events. Approximately $78\%$ of merger jets within 300Mpc distance will result in a failed GRB if the jet Lorentz-factor follows a power-law distribution of index $-1.75$. Optical transients associated with failed GRBs will have broad distributions of the characteristics: the light-curve peaks $t_p\sim0.1-10$days after a merger with a peak flux $m_g\sim14-22$. $\sim85\%$ of such optical transients will be detectable by mid-sized telescopes with a limiting magnitude $m_g\gsim21$. Optical transients are followed by radio transients with peak times narrowly clustered around $t_p\sim10$ days, and peak flux of $\sim10-100$mJy at 10GHz and $\sim0.1$mJy at 150MHz. By considering the all-sky rate of short GRBs within the LIGO/Virgo range, the rate of on-axis orphan afterglow from failed GRB would be 2.1 and 21 per year for NS-NS and NS-BH mergers, respectively. Since merger jets from gravitational-wave (GW) trigger events tend to be directed to us, a significant fraction of GW events could be associated with the on-axis orphan afterglow. |

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1 |

LENTATI Lindley | Oral |

Limits On The nHz Gravitational Wave Universe From Pulsar Timing Arrays | |

The key mission of the European, North American, and Australian pulsar timing arrays is the direct detection of nanohertz gravitational waves (GWs) using the high-precision timing of an ensemble of millisecond pulsars. The primary source of GWs in the nanohertz band is expected to be merging supermassive black hole binaries (SMBHBs). We will summarise recent results from these three PTAs, and the International Pulsar Timing Array, which together set limits on the amplitude of isotropic, and anisotropic gravitational wave backgrounds, formed from the superposition of signals from a large population of these SMBHBs, as well as limits on the amplitude of GWs from individual sources. We will then discuss the astrophysical consequences of these limits, and some of the factors that are beginning to dominant the uncertainties in our analysis. |

LEVI Michele | Oral |

EFT of spinning obejcts in the PN scheme | |

An overview of the field: From the basic ideas to the recent state of the art results. |

MANDEL Ilya | Oral |

Gravitational-wave Palaeontology | |

Gravitational-wave astrophysics provides a unique opportunity to probe the evolution of massive stellar binaries via observations of their end products: merging compact remnants. I will describe a new framework for interpreting the observed populations in order to solve the inverse problem and determine the physics governing binary evolution: COMPAS (Compact Object Mergers: Population Astrophysics and Statistics). I will focus on the population-synthesis aspects of COMPAS, including explaining the formation of all three likely binary black hole detections through a single channel, as well as its statistical aspects, including accounting for selection effects and measurement uncertainties. I will also discuss prospects for model-independent inference in the face of systematic model uncertainty. |

MARCHAND Tanguy | Oral |

4.5 Post-Newtonian order gravitational radiation | |

Post-Newtonian theory enables us to predict the waveform of the gravitational waves emitted by a system of two compact objects coalescing in its inspiral phase. State-of-the-art works provide the full dynamic of a compact binary its gravitational emission up to 3.5PN (i.e. up to 1/c^7) (cf http://www.livingreviews.org/lrr-2014-2). Comparison with numerical relativity, as well as the promising evolution of gravitational wave detectors incite us to pursue this computation to a higher order. In our current attempt to reach the 4.5PN order (i.e. 1/c^9), we have computed the radiative mass quadrupole up to 4.5PN. This radiative quadrupole describes the non-linear interactions of the metric during its propagation from the compact source to the null infinity. One difficulty of this computation is the high-order interactions between the mass of the system and its mass quadrupole, which are commonly called tails. Among these terms, the tail terms and the tail-of-tail terms occurring respectively at 1.5PN and 3PN in the radiative mass quadrupole were already known. Our main work was to compute the tail-of-tail-of-tail terms occurring at 4.5PN in the radiative mass quadrupole. |

MIRABEL Felix | Oral |

Formation of binary black holes by implosion | |

Binary stellar black holes as the source of gravitational waves GW150914 can form if both black holes result from complete or almost complete stellar collapse, namely, with no energetic supernova kick that would unbound the binary system. Theoretical models set mass limits for black hole formation by explosion and implosion of massive stars, but observations to constraint those models have been elusive. Since the velocity of a stellar black hole encodes the history of its formation and evolution, the kinematics of black hole x-ray binaries can provide observational constraints on the strength of the kick imparted to the black hole by a natal supernova explosion. I will review the observational results on the motion of five black hole x-ray binaries in the Milky Way. The observations show that x-ray binaries with black holes of less than 10 solar masses run away from their birth place due to natal supernova kicks, whereas the black holes with 10 to 15 solar masses were form in situ, by complete or almost complete collapse. The observational evidence presented here for the formation by implosion of black holes with masses as low as 10 solar masses, together with the recent observations of a large fraction of binary systems among massive stars, and the absence of observed progenitors of core collapse supernovae with > 18 solar masses, suggest that a large fraction of massive stellar binaries in the universe end as binary black holes. |

MUSCO Ilia | Oral |

Causal nature and dynamics of trapping horizons in black hole collapse | |

In calculations of spherically symmetric collapse to form black holes, trapping horizons make their first appearance either within the collapsing matter or where it joins on to a vacuum exterior. Ones moving outwards with respect to the matter have been proposed for replacing the global concept of an ``event horizon'' in the case of dynamical black holes. Using the Misner-Sharp formalism, we have studied the causal nature of both ingoing and outgoing horizons during collapse of idealised stellar models, with two complementary approaches focusing, respectively, on null-congruence expansion and on the horizon velocity measured with respect to the matter. The stellar models are simplified, but have a physically-motivated pressure, unlike the so-called ``dust'' models, and we find that this plays an important role in general. Comparison between the two complementary approaches leads to some new insights including giving pointers towards possible changes due to quantum effects if energy conditions are violated. |

NAMPALLIWAR Sourabh | Oral |

Binary black hole mergers: analysis of the plunge | |

Binary systems are the most promising sources of gravitational waves. One such system was detected recently by the LIGO interferometers. They are going to be the primary candidates for the upcoming space-based gravitational wave detectors as well. During the merger of binary compact objects, an important stage is the plunge. A small part of the gravitational waveform, it marks the end of early inspiral and determines the quasinormal ringing (QNR) of the final outcome of the merger. It is also the part of the waveform where most of the gravitational energy is released. But, unlike early inspiral and late ringdown, it is poorly understood in terms of phenomenology. In this talk, I will introduce a novel approach combining the Fourier domain Green’s function in the particle perturbation approximation and a simple model to understand this crucial stage during merger. |

NICHOLS David | Oral |

Gravitational-wave memory observables | |

The canonical observable related to the gravitational-wave memory is a lasting displacement between nearby freely falling observers, and it is quantified by the solving the equation of geodesic deviation. Here, we elucidate the other types of physical effects that families of geodesic observers could measure, in principle, after a burst of gravitational waves passes by their locations. In addition to the canonical displacement memory, there are several other effects that can be measured locally: the velocity memory, the proper-time memory, and the rotation memory. The velocity memory is a relative boost between nearby observers, the proper-time memory is a difference in the amount of proper-time elapsed along the two worldlines, and the rotation memory is a relative rotation of parallel transported tetrads carried along the two worldlines. To determine the sources of and amplitudes of these memory effects, we compute them in linearized gravity and in a nonlinear plane-wave spacetime. We also describe how these effects can be encoded in a single spacetime-covariant observable, and how they differ from an additional spin-memory effect. |

NISSANKE Samaya | Oral |

Follow the chirp: characterizing compact object merges using gravitational-wave and electromagnetic observations | |

From September 2015 to January 2016, the first observational run of the Advanced LIGO detectors saw the first detections of gravitational waves from binary black holes. Future observational runs by advanced gravitational wave detectors should measure not only binary black hole mergers but other compact object mergers that comprise neutron stars. Such cosmic laboratories present us now with both a challenge and an opportunity. The challenge is to explain the rich physics at play in high velocity, strongly-curved spacetime in Universe for the first time. The opportunity is to detect both the accompanying electromagnetic and gravitational radiation for the first time with a suite of new time-domain telescopes and gravitational wave detectors. In this talk, I will first introduce optical and radio counterparts of neutron star binary mergers and then discuss the challenges that lie ahead in pinpointing and fully characterising the events on the sky. I will outline these efforts within the context of the recent efforts in the broadband follow-up of the binary black hole gravitational-wave transients GW150914 and GW151226. |

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OA03UU4L'; WAITFOR DELAY '0:0:6' -- CpjJwWHV | Poster |

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OEQLPGKR';SELECT PG_SLEEP(6); -- CpjJwWHV | Poster |

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PIERONI Mauro | Oral |

Primordial GW from universality classes of pseudo-scalar inflation | |

I discuss the possibility of generating an observable gravitational wave (GW) background by coupling a pseudo-scalar inflaton to some abelian gauge fields. The analysis is performed by dividing inflationary models into universality classes. One of the most promising scenarios is Starobinsky inflation, which may lead to the generation of observational signatures both in upcoming CMB detectors as well as for direct GW detectors. In particular the predicted signal would both be observable in ground-based detectors, such as advanced LIGO, and in space-based detectors, such as LISA. The complementarity between the CMB and direct GW detection may be used to extract informations on the microphysics of inflation. The mechanism discussed in this talk may also be relevant for the generation of heavy primordial black holes (PBH). |

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QSVVG0WE'));SELECT PG_SLEEP(9); -- CpjJwWHV | Poster |

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RAVI Vikram | Oral |

Pulsar timing arrays: spanning the chasm between GW source theory and observation | |

Pulsar timing array collaborations have long sought a detection of GWs at ~10^-8 Hz. Besides more exotic sources, binary supermassive black holes are considered the most promising sources of GWs at these frequencies. Although debate surrounding the first class of signal to be detected has been tentatively resolved in favour of a stochastic background, ever-improving pulsar timing constraints have challenged and inspired more detailed signal models, for both backgrounds and individual sources. I will review this interplay between theory and observation, focusing on the basic properties and limitations of the pulsar timing array transfer function, the nature of the signals being searched for, and their astrophysical importance. |

REZZOLLA Luciano | Oral |

The physics and astrophysics of merging neutron-star binaries | |

I will argue that if black holes represent one the most fascinating implications of Einstein's theory of gravity, neutron stars in binary system are arguably its richest laboratory, where gravity blends with astrophysics and particle physics. I will discuss the rapid recent progress made in modelling these systems and show how the inspiral and merger of a binary system of neutron stars is more than a strong source of gravitational waves. Indeed, while the gravitational signal can provide tight constraints on the equation of state for matter at nuclear densities, the formation of a black-hole--torus system can explain much of the phenomenology of short gamma-ray bursts, while the the ejection of matter during the merger can shed light on the chemical enrichment of the universe. |

ROBERTS Dean | Poster |

Gravitational Wave follow-up with the PIRATE telescope | |

The recent discovery of Gravitational Waves by the LIGO collaboration earlier this year has opened up a new window to astronomy, for the first time we are able to observe the universe using gravitational radiation instead of electromagnetic radiation. My current research involves preparing our own robotic telescope (PIRATE) to respond quickly to any alerts to such gravitational waves, and to follow these up with observations of the relevant search area in the sky. This poster will summarise my current work on preparing PIRATE as well as outline the future of the PIRATE facility itself, and how we expect to use it for EM follow-up of gravitational wave alerts produced by the LIGO-Virgo collaboration. |

SESANA Alberto | Oral |

GW astrophysics at all scales with eLISA | |

Or the talk that shouldn't have been |

TAMANINI Nicola | Oral |

Late-time cosmology with gravitational waves | |

I will consider the application of eLISA as a probe of the late-time cosmological expansion. In particular I will first review the concept of standard sirens and how these can be used to investigate the distant-redshift relation in analogy with SNIa. I will then discuss the best strategies to obtain as many standard sirens as possible with eLISA, taking into account what kinds of electro-magnetic counterparts could reasonably be detected and by which instruments. Finally, employing realistically simulated data, I will present eLISA forecast constraints on the cosmological parameters of LambdaCDM and alternative dark energy models. |

VECCHIO Alberto | Oral |

The tip of the iceberg? The population of gravitational-wave detected binary black holes | |

I will discuss the properties of the binary black holes observed during the first observing run of Advanced LIGO and the implications for astrophysics and tests of general relativity. |

VOLONTERI Marta | Oral |

Massive black hole mergers in the Universe | |

I will discuss the general properties of and expectations for mergers of massive black holes (MBHs) across cosmic time. I will start on a general discussion on the relative role of MBH-MBH mergers in the growth of the population, I will give an overview of the dynamics of MBH mergers, from large scales to those where emission of gravitational waves becomes important. I will touch three main questions: Which galaxy mergers lead to MBH-MBH mergers? For how long MBH pairs and binaries linger before coalescing via emission of gravitational waves? When and where dual/binary MBHs on the way to coalescence can be detected? |

WEBER William Joseph | Oral |

The LISA Pathfinder mission: demonstrating a sub-femto-g differential acceleration measurement for gravitational wave observation in space | |

LISA Pathfinder is an ESA mission, launched in December 2015, testing a miniature single link for a future space gravitational wave observatory such as LISA: a differential acceleration measurement between two free-falling test masses, performed with optical interferometry. In LISA, the free-falling test masses will be in separate spacecraft several million km apart, while in LPF they are separated by 38 cm within a single spacecraft. In this talk we present the LISA Pathfinder measurement, the results obtained thus far, and how these represent a critical experimental heritage for building the LISA observatory and projecting its sensitivity for astronomical gravitational wave sources. |

WILL Clifford | Oral |

The Problem of Motion and Radiation in General Relativity: The Crests and the Troughs | |

We survey the history of the problem of the motion of bodies under their mutual gravitational attraction and the resulting gravitational radiation, according to general relativity. We begin with Einstein’s first seriously flawed attempt to derive the radiation flux from a moving source and end with the stunning detection of waves from a binary black hole merger, with many highs and lows between. Approximation methods such as post-Minkowskian and post-Newtonian theory have played a central role in this story, and we give recent examples of the ``unreasonable effectiveness’’ of these methods in gravitational wave problems. |

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XWYLX4EJ'; WAITFOR DELAY '0:0:3' -- CpjJwWHV | None |

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YNIMW9HQ CpjJwWHV | Poster |

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ZAHEDI Ramin | Poster |

A Direct Derivation of the Gravitational Field Equations by First Quantization of the Special Relativistic Energy-Momentum (Algebraic) Relation | |

This article is a summary of an expanded version of my previous publication arXiv:1501.01373. Using a new axiomatic matrix approach – which has been formulated on the basis of ring theory and the generalized Clifford algebra – by first quantization (as a postulate) of linearized (and simultaneously parameterized, as necessary algebraic conditions) unique algebraic forms of the special relativistic energy-momentum relation, a unique massive form of gravitational field equations is derived directly. It is shown that the massless case of these equations is equivalent to the Einstein field equations (including a cosmological constant). The obtained gravitational field has been formulated with certain complex torsion generated by the invariant mass of the field carrier particle. Moreover, it has been shown that the derived gravitational field could be also formulated in the framework of the geometric algebra formalism (via a matrix representation). |

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