https://cplberry.com/publications/2025-12-13T20:56:49+00:00weekly0.6https://cplberry.com/outreach/https://cplberry.com/wp-content/uploads/2014/07/camscisoc.pngCam Sci Soc posterAwesome poster designed for a talk I gave to the University of Cambridge's Science Society.2025-11-19T18:42:19+00:00weekly0.6https://cplberry.com/group/2025-10-08T13:00:05+00:00weekly0.6https://cplberry.com/curriculum-vitae/2025-08-16T21:33:38+00:00weekly0.6https://cplberry.com/contact/https://cplberry.com/wp-content/uploads/2014/07/tarantula2_hst_1280.jpgtarantula2_hst_1280Star Formation in the Tarantula Nebula2025-08-16T21:30:11+00:00weekly0.6https://cplberry.com/teaching/2025-08-16T21:26:03+00:00weekly0.6https://cplberry.com/research/https://cplberry.com/wp-content/uploads/2014/07/fig_psaltis_plot.pngPsaltis plotTests of GR plotting as functions of gravitational potential ε and spacetime curvature ξ. Current tests probe a wide range, but are yet to reach the most extreme regimes close to the surfaces of compact objects. The dashed line represents the event horizon of Schwarzschild black holes. Credit: <a href="http://www.repository.cam.ac.uk/handle/1810/245139">Berry (2013)</a>.</em>2025-08-16T21:17:45+00:00weekly0.6https://cplberry.com/2015/02/07/equaquette/https://cplberry.com/wp-content/uploads/2015/02/pngxkcd: (Pure evil. Credit: xkcdhttps://cplberry.com/wp-content/uploads/2015/02/willie.gifWillieTrousers are not standardised, but units are! The Springfield Police are shocked when Willie forgets his. Credit: Foxhttps://cplberry.com/wp-content/uploads/2015/01/pi-pie10.jpgPi piePi pie! Perfect for any mathematical dinner party. Credit: Tasty retreat2023-10-31T12:14:53+00:00monthlyhttps://cplberry.com/2018/01/17/gw170817-the-papers/https://cplberry.com/wp-content/uploads/2018/01/afterglow-xray-radio.pngGW170817 X-ray excessX-ray (top) and radio (bottom) observations from Chandra and the Very Large Array, respectively. The X-ray observations show an excess after around 900 days, but their is not sign in radio. The red and orange lines show estimated synchrotron emission for different power laws. The grey curve shows synchrotron emission from the dynamical ejecta of a kilonova from a numerical relativity simulation of a neutron star merger. Figure 2 of Hajela et al. (2021).https://cplberry.com/wp-content/uploads/2018/01/fig1_lc_03jun2020.pngAfterglow of GW170817's source to 940 days post-mergerOptical, radio and X-ray light-curves, scaled by a best-fit spectral index so that the different observations lie on top of each other, for GW170817's afterglow. The top panel shows the individual observations, labelled by observatory and observing band. The bottom panel shows a moving average. Fig. 1 of Makhathini et al. (2020).https://cplberry.com/wp-content/uploads/2018/01/gw170817_fong_2019.pngAfterglow of GW170817's source to 584 days post-mergerLeft: Optical afterglow observed until 584 days post-merger together with predictions for a structured jet and a quasi-spherical outflow (Wu & MacFadyen 2018). Right: Radio, optical and X-ray observations to 535 days, 534 days and 533 days post-merger-respectively. Triangles denote upper limits. Fig. 2 and Fig. 3 of Fong et al. (2019).https://cplberry.com/wp-content/uploads/2018/01/fig3.pngLight curves to one year after GW170817Radio, optical and X-ray observations to 358 days after merger. The coloured lines show fitted Gaussian jet models. Fig. 3 of Lamb et al. (2018).https://cplberry.com/wp-content/uploads/2018/01/h0_marginal_posterior_plj_dh350.pngHubble constant with VLBI jet inclination constraintsPosterior probability distribution for the Hubble constant inferred from GW170817 using only gravitational waves, and folding in models for the jet and radio observations. The lines symmetric mark 68% intervals. The coloured bands are measurements from the cosmic microwave background (Planck) and supernovae (SHoES). Figure 2 of Hotokezaka et al. (2018)https://cplberry.com/wp-content/uploads/2018/01/gw170817spindisk_60.pngGW170817 component spinsEstimated orientation and magnitude of the two component spins. The left pair is for the high-spin prior and so magnitudes extend to 0.89, and the right pair are for the low-spin prior and extend to 0.05. In each, the distribution for the more massive component is on the left, and for the smaller component on the right. The probability is binned into areas which have uniform prior probabilities. Results are shown at a point in the inspiral corresponding to a gravitational-wave frequency of 100 Hz. Parts of Figure 8 and 9 of the GW170817 Properties Paper.https://cplberry.com/wp-content/uploads/2018/01/gw170817_pepaper_bw_speclims_50.pngGW170817 post-merger upper limitsNoise amplitude spectral density for the detectors used, prior and posterior strain upper limits, and selected numerical simulations as a function of frequency. The signal upper limits are Bayesian 90% credible bounds for the signal in Hanford, but is derived from a coherent analysis of all three indicated detectors. Figure 13 of the GW170817 Properties Paper.https://cplberry.com/wp-content/uploads/2018/01/gw170817_m1_m2_spin_60.pngGW170817 binary massesEstimated masses for the two neutron stars in the binary using the high-spin (left) and low-spin (right) priors. The two-dimensional plot follows a line of constant chirp mass which is too narrow to resolve on this scale. Results are shown for four different waveform models. Figure 5 of the GW170817 Properties Paper.https://cplberry.com/wp-content/uploads/2018/01/m-r_imrdnrt_lowspin_75.pngGW170817 neutron star mass and radiusPosterior probability distributions for neutron star masses and radii (blue for the more massive neutron star, orange for the lighter). The left plot uses the equation-of-state insensitive relations, and the right uses the parametrised equation-of-state model. In the one-dimensional plots, the dashed lines indicate the priors. The lines in the top left indicate the size of a Schwarzschild Black hole and the Buchadahl limit for the collapse of a neutron star. Figure 3 of the GW170817 Equation-of-state Paper.https://cplberry.com/wp-content/uploads/2018/01/lambda1-lambda2_imrdnrt_lowspin_ul1.pngGW170817 tidal parametersProbability distributions for the tidal parameters of the two neutron stars. The tidal deformation of the more massive neutron star must be greater than that for the smaller neutron star. The green shading and (50% and 90%) contours are calculated using the equation-of-state insensitive relations. The blue contours are for the parametrised equation-of-state model. The orange contours are from the GW170817 Properties Paper, where we don't assume a common equation of state. The black lines are predictions from a selection of different equations of state Figure 1 of the GW170817 Equation-of-state Paper.2023-08-17T14:06:49+00:00monthlyhttps://cplberry.com/2015/07/26/whats-up-doc/https://cplberry.com/wp-content/uploads/2015/07/2015-06-13-12-43-48.jpgNijō Castle garden and pondGardens of Nijō Castle, Kyoto.https://cplberry.com/wp-content/uploads/2015/07/2015-06-16-10-17-58.jpgKAGRA constructionThe in-construction Kamioka Gravitational Wave Detector (KAGRA). It is being built underground, in an old mine in the Hida Mountains.https://cplberry.com/wp-content/uploads/2015/07/2015-06-28-16-00-50.jpgTemple lanternsLanterns at the Jogyesa temple, Seoul.2023-04-16T11:58:37+00:00monthlyhttps://cplberry.com/2021/06/29/gw200115-gw200105/https://cplberry.com/wp-content/uploads/2021/06/nsbh_rates.pngInferred neutron star–black hole binaryProbability distribution for the neutron star–black hole binary merger rate density. The green curve shows the event-based rate assuming all neutron star–black hole binaries are like GW200105 or GW200115. THe black line assumes a broader population that also includes GW190814 and higher mass black holes. The vertical lines mark the 90% credible interval. Figure 9 of the NSBH Discovery Paper.https://cplberry.com/wp-content/uploads/2021/06/m1_spin_115_corner_plot.pngGW200115 primary mass and spinEstimated primary mass, and spin component in the orbital plane and spin component aligned with the orbital angular momentum for GW200115. The (off-diagonal) two-dimensional plots show the correlations between parameters. The solid lines indicate 50% and 90% credible regions with the high-spin prior for the secondary, and the dashed lines show the same for the low-spin prior. The (on-diagonal) one-dimensional plots show probability densities. The vertical lines indicate 90% credible intervals. The black lines show the priors. Figure 7 of the NSBH Discovery Paper.https://cplberry.com/wp-content/uploads/2021/06/spin_disk_plus_contours_nsbh.pngGW200105 and GW200115 component spinsEstimated orientation and magnitude of the two component spins for GW200105 (left) and GW200115 (right). The distribution for the more massive primary component is on the left, and for the lighter secondary component on the right. The probability is binned into areas which have uniform prior probabilities, so if we had learnt nothing, the plot would be uniform. The maximum spin magnitude of 1 is appropriate for black holes. The solid line shows the 90% credible region using the high spin prior (which is used for the rest of the plot) and the dashed line shows the 90% contour for the low-spin prior. Figure 6 of the NSBH Discovery Paper.https://cplberry.com/wp-content/uploads/2021/06/triangle_plot_comparison_bothpriors_em_lec-e1624894241650.pngGW200105, GW200115, GW190426_152155 and GW190814 binary massesEstimated masses for the binary primary and secondary masses for neutron star–black hole binary candidates. The two-dimensional plot shows the 90% probability contour. For GW200105 and GW200115 we show results for two different spin priors for the secondary. The one-dimensional plot shows individual masses; the vertical lines mark 90% bounds away from equal mass. Estimates for the maximum neutron star mass are shown for comparison with the mass of the secondary. Figure 4 of the NSBH Discovery Paper.https://cplberry.com/wp-content/uploads/2021/06/o3a-o3b_full_final_gstlal_nsbh_background_plot_sslushn.pngDetection statistics for GW200105, GW200115 and GW190426_152155Detection statistics for GW200105, GW200115 and GW190426_152155, showing they compare to background data. The plot shows the signal-to-noise ratio and signal-consistency statistic from the GstLAL algorithm. The coloured density plot shows the distribution of background triggers. LHO indicates a trigger from LIGO Hanford, and LLO indicates a trigger from LIGO Livingston. GW200105 is distinct from anything else seen in O3. However, GW200105 is calculated less significant than GW200115 as it only has a trigger from a single detector. Figure 3 of the NSBH Discovery Paper.https://cplberry.com/wp-content/uploads/2021/06/gw200105-gw200115-qtransform2.pngGW200105 and GW200115 spectrogramsTime–frequency plots for GW200105 (left) and GW200115 (right) as measured by LIGO Hanford, LIGO Livingston and Virgo. LIGO Hanford was not observing at the time of GW200105. The chirp of a binary coalescence is clearest in Livingston for GW200105; these are usually hard to see for these types of signals. The Livingston data for GW200105 is shown after glitch subtraction, and the Livingston data for GW200115 shows light-scattering glitches at low frequencies. Figure 1 of the NSBH Discovery Paper.https://cplberry.com/wp-content/uploads/2021/06/mtotvsqpost.pngO3a mass ratios and total massesEstimated total mass and mass ratio of the binary sources for the candidates in O3a. The contours mark the 90% credible regions. The dashed lines mark a robust upper limit on the maximum neutron star mass. Figure 6 of the GWTC-2 Paper.https://cplberry.com/wp-content/uploads/2021/06/rates_intrinsic_bhns_colors.pngRate densities of neutron star–black hole binary mergers from isolated binary evolutionPredictions for the neutron star–black hole binary merger rate density as modelled by the COMPAS population synthesis code. The different models illustrate variations in the input physics, highlighting the range of predictions for isolated binary evolution. Other channels could potentially form neutron star–black hole binaries too. Figure 9 of Broekgaarden et al. (2021)https://cplberry.com/wp-content/uploads/2021/06/dance_like_noone_watching-6.pngDance like no-one is watchingTime to tick neutron star–black hole binaries of the checklist. Part of a comic by Nutsinee Kijbunchoo drawn following the discovery of GW170817 showing Rai Weiss rather happy with his work.https://cplberry.com/wp-content/uploads/2021/06/masses_of_dead_stars_ligo_virgo_gw200105_gw200115_errorbars.pngMasses in the stellar graveyard: GW200115 and GW200105The population of compact objects (black holes and neutron stars) observed with gravitational waves and with electromagnetic astronomy, including a few that are uncertain. The sources for GW200115 (left) and GW200105 (right) are highlighted.2021-08-28T19:23:25+00:00monthlyhttps://cplberry.com/2015/05/05/britgrav15/https://cplberry.com/wp-content/uploads/2015/05/fig_britgrav_inst_2.pngBritGrav talk instituionsProportion of talks at BritGrav 15 by institution. https://cplberry.com/wp-content/uploads/2015/05/fig_britgrav_inst_1.pngBritGrav attendance institutionsProportion of participants at BritGrav 15 by institution. Birmingham, as host, comes out top.https://cplberry.com/wp-content/uploads/2015/05/fig_britgrav_level_1.pngBritGrav career levelsProportion of participants at BritGrav 15 by (self-reported) career level. https://cplberry.com/wp-content/uploads/2015/05/fig_britgrav_level_2.pngBritGrav talks career levelsProportion of talks at BritGrav 15 by (self-reported) career level. The majority are by PhD students.https://cplberry.com/wp-content/uploads/2015/05/nielsen.pngNSBH time–frequency plotsSlides demonstrating the difficulty of detecting gravitational-wave signals from Alex Nielsen's talk on searching for neutron star–black hole binaries with gravitational waves. Fortunately we don't do it by eye (although if you flick between the slides you can notice the difference).https://cplberry.com/wp-content/uploads/2015/05/oniga-e1456140659170.pngGravitational Shroedinger's catSlide from Teodora Oniga's BritGrav 15 talk on Gauge invariant quantum gravitational decoherence. There are not enough cats featured in slides on gravitational physics.2021-07-15T10:27:55+00:00monthlyhttps://cplberry.com/2020/09/02/gw190521/https://cplberry.com/wp-content/uploads/2020/09/gw190521-agn.pngLocation of the potential counterpart for GW190521The three dimensional localisation for GW190521. The lines indicate the position of the claimed electromagnetic counterpart from around an active galactic nucleus. This location lies at the 70% credible level. Credit: Will Farrhttps://cplberry.com/wp-content/uploads/2020/08/chis_vf.pngGW190521 effective inspiral and precession spinsEstimated effective inspiral spin and effective precession spin. We show results several different waveform models and use the numerical relativity surrogate (NRSur PHM) as our best results. The two-dimensional shows the 90% probability contour. The dotted lines in one-dimensional plots the symmetric 90% credible interval. We also show the prior distributions in the one-dimensional plots. Part of Figure 1 of the GW190521 Implications Paper.https://cplberry.com/wp-content/uploads/2020/08/ringdown_figure_mfaf_vf.pngRingdown mass and spin measurementsEstimated redshifted mass and spin for the final black hole. We show results several different insprial–merger–ringdown waveform models, which we use for our standard analysis, as well as ringdown-only waveforms. The two-dimensional shows the 90% probability contour. The dotted lines in one-dimensional plots the symmetric 90% credible interval. The mass is safely above the conventional lower limit to be considered an intermediate-mass black hole. Part of Figure 9 of the GW190521 Implications Paper.https://cplberry.com/wp-content/uploads/2020/08/mfaf_vf.pngGW190521 final black hole mass and spinEstimated mass and spin for the final black hole. We show results several different waveform models and use the numerical relativity surrogate (NRSur PHM) as our best results. The two-dimensional shows the 90% probability contour. The dotted lines in one-dimensional plots the symmetric 90% credible interval. The mass is safely above the conventional lower limit to be considered an intermediate-mass black hole. Figure 3 of the GW190521 Implications Paper.https://cplberry.com/wp-content/uploads/2020/08/figure1_whitedata_reconstructions_qscan.pngGW190521 waveform reconstructions and spectrogramsVisualisations of GW190521. The top panels show whitened data and reconstructed waveforms from the template-free detection algorithm cWB, BayesWave (which reconstructs the signal from sine–Gaussian wavelets), and our parameter estimation code LALInference (which uses binary black hole waveforms). The bottom panels show time–frequency plots: each plot has a different scale as the signal is loudest in LIGO Livingston and hardly noticeable in Virgo. As the signal is so short, we don't see the usual chirp of a binary coalescence clearly. Figure 1 of the GW190521 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/08/m1m2_vf.pngGW190521 binary massesEstimated masses for the two components in the binary. We show results several different waveform models and use the numerical relativity surrogate (NRSur PHM) as our best results. The two-dimensional shows the 90% probability contour. The dotted lines in one-dimensional plots the symmetric 90% credible interval. Part of Figure 1 of the GW190521 Implications Paper.https://cplberry.com/wp-content/uploads/2020/08/mzams_mrem-1.pngInitial mass vs final massRemnant (white dwarf, neutron star or black hole) mass for different initial (zero age main sequence) stellar masses. This is just for single stars, and ignores all the complicated things that can happen in binaries. The different coloured lines indicate different metallicities (higher metallicity stars lose more mass through stellar winds). The two panels are for two different supernova models. The grey bars indicate potential mass gaps: the lower core collapse mass gap (only predicted by the Rapid model) and the upper pair-instability mass gap. The tick marks in the middle are various claimed gravitational-wave source, colour-coded by the total mass of the binary. Figure 1 of Zevin et al. (2020).2021-06-28T18:17:33+00:00monthlyhttps://cplberry.com/2020/04/18/gw190412/https://cplberry.com/wp-content/uploads/2020/04/figures_chip_pub.pngGW190412 effective precession spin parameterEstimated effective precession spin parameter. Results are shown for two different waveform models. To indicate how much (or little) we've learnt, the prior probability distribution is shown: the global prior is what we would get if we had learnt nothing, the restricted prior is what we would have after placing cuts on the effective inspiral spin parameter and mass ratio to match our observations. We are definitely getting information on precession from the data. Figure 5 of the GW190412 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/04/figures_chi_eff_q_all_pub.pngGW190412 mass ratio and effective inspiral spin412 mass ratio and effective inspiral spinEstimated mass ratio for the two components in the binary and the effective inspiral spin (a mass-weighted combination of the spins perpendicular to the orbital plane). We show results for two different model waveforms. Systems with unequal masses are difficult to model, so we have some extra uncertainty from the accuracy of our models. The two-dimensional shows the 90% probability contour. The one-dimensional plots show the probability distributions and the the dotted lines mark the central 90%. Figure 2 of the GW190412 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/04/gauss_odds_ratios_both.pngOdds ratios for different binary black holes being hierarchical mergersOdds of binary black holes being a hierarchical merger verses being original generation binary. 1G indicates first generation black holes formed from the collapse of stars, 2G indicates a black hole formed from the merger of two 1G black holes. These are preliminary results using the GWTC-1 results plus GW!90412. Fig. 15 of Kimball et al. (2020).https://cplberry.com/wp-content/uploads/2020/04/figures_beta_posterior.pngPower-law index for mass ratio distribution including GW190412Estimated power-law slope for the binary black hole mass ratio distribution. Dotted lines show the results with our first ten detections, and solid lines include GW190412. Results are shown for two different waveform models. Figure 11 of the GW190412 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/04/figures_chip.pngGW190412 effective precession spin parameterEstimated effective precession spin parameter. Results are shown for two different waveform models. To indicate how much (or little) we've learnt, the prior probability distribution is shown: the global prior is what we would get if we had learnt nothing, the restricted prior is what we would have after placing cuts on the effective inspiral spin parameter and mass ratio to match our observations. We are definitely getting information on precession from the data. Figure 5 of the GW190412 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/04/figures_chi_eff_q_all.pngGW190412 mass ratio and effective inspiral spin412 mass ratio and effective inspiral spinEstimated mass ratio for the two components in the binary and the effective inspiral spin (a mass-weighted combination of the spins perpendicular to the orbital plane). We show results for two different model waveforms. Systems with unequal masses are difficult to model, so we have some extra uncertainty from the accuracy of our models. The two-dimensional shows the 90% probability contour. The one-dimensional plots show the probability distributions and the the dotted lines mark the central 90%. Figure 2 of the GW190412 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/04/figures_gw190412-q-transform.pngGW190412 spectrogramTime–frequency plots for GW190412 as measured by LIGO Hanford, LIGO Livingston and Virgo. The chirp of a binary coalescence is clearer in two LIGO detectors, with the signal being loudest in Livingston. Figure 1 of the GW190412 Discovery Paper.2021-06-28T18:17:24+00:00monthlyhttps://cplberry.com/2020/06/23/gw190814/https://cplberry.com/wp-content/uploads/2020/06/formation_channels-e1593356377624.pngGW190814 possible formation channelsTwo possible ways of forming GW190814-like systems through isolated binary evolution. In Channel A the heavier black hole forms first from the initially more massive star. In Channel B, the initially more massive star transfers so much mass to its companion that we get a mass inversion, and the lighter component forms first. In the plot, a is the orbital separation, e is the orbital inclination, t is the time since the stars started their life on the main sequence. The letters on the right indicate the evolution phase: ZAMS is zero-age main sequence, Ms is main sequence (burning hydrogen), CHeB is core helium burning (once the hydrogen has been used up), and BH and NS mean black hole and neutron star. At low metallicities (when stars have few elements heavier than hydrogen and helium), the two channels are about as common, as metallicity increases Channel A becomes more common. Figure 6 of Zevin et al. (2020).https://cplberry.com/wp-content/uploads/2020/06/spin_disk_plot_gw190814.pngGW190814 component spinsEstimated orientation and magnitude of the two component spins. The distribution for the more massive primary component is on the left, and for the lighter secondary component on the right. The probability is binned into areas which have uniform prior probabilities, so if we had learnt nothing, the plot would be uniform. The maximum spin magnitude of 1 is appropriate for black holes. On account of the mass ratio, we get a good measurement of the spin of the primary, but not the secondary. Figure 6 of the GW190814 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/06/eos_constraints.pngNeutron star equation of state with and without GW190814Constraints on the neutron star equation of state, showing how density changes with pressure. The blue curve just uses GW170817, implicitly assuming that GW190814 is from a binary black hole, while the orange shows what happens if we include GW190814, assuming it is from a neutron star–black hole binary. The 90% and 50% credible contours are shown as the dark and lighter bands, and the dashed lines indicate the 90% region of the prior. Figure 8 of the GW190814 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/06/mass_1_mass_2_contour_with_ns_bounds.pngGW190814 binary massesEstimated masses for the two components in the binary. We show results several different waveform models (which include spin precession and higher order multiple moments). The two-dimensional shows the 90% probability contour. The one-dimensional plot shows individual masses; the dotted lines mark 90% bounds away from equal mass. Estimates for the maximum neutron star mass are shown for comparison with the mass of the lighter component. Figure 3 of the GW190814 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/06/skymap.pngSky localization for GW190814's sourceSky localizations for GW190814's source. The blue dashed contour shows the preliminary localization using only LIGO Livingston and Virgo data, and the solid orange shows the preliminary localization adding in Hanford data. The dashed green contour shows and updated localization used by many for their follow-up studies. The solid purple contour shows our final result. All contours are for 90% probabilities. Figure 2 of the GW190814 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/06/gw190814-q-transform.pngGW190814 spectrogramTime–frequency plots for GW190814 as measured by LIGO Hanford, LIGO Livingston and Virgo. The chirp of a binary coalescence is clearest in Livingston. For long signals, like GW190814, it is usually hard to pick out the chirp by eye. Figure 1 of the GW190814 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/06/massplot_graveyard_190814.pngMasses in the stellar graveyard: GW190814The population of compact objects (black holes and neutron stars) observed with gravitational waves and with electromagnetic astronomy, including a few that are uncertain. GW190814 is highlighted. It is not clear if its lighter component is a black hole or neutron star.2021-06-26T17:17:21+00:00monthlyhttps://cplberry.com/2020/01/06/gw190425/https://cplberry.com/wp-content/uploads/2020/01/figures_mr.pngGW190425 neutron star mass and radiusProbability distributions for neutron star masses and radii (blue for the more massive neutron star, orange for the lighter), assuming that GW190425's source is a binary neutron star. The left plots use the high-spin assumption, the right plots use the low-spin assumptions. The top plots use equation-of-state insensitive relations, and the bottom use parametrised equation-of-state models incorporating the requirement that neutron stars can be 1.97 solar masses. Similar analyses were done in the GW170817 Equation-of-state Paper. In the one-dimensional plots, the dashed lines indicate the priors. Figure 16 of the GW190425 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/01/figures_gw190425_detection.pngDetection statistics for GW190425Detection statistics for GW190425 showing how it stands out from the background. The left plot shows the signal-to-noise ratio (SNR) and signal-consistency statistic from the GstLAL algorithm, which made the detection. The coloured density plot shows the distribution of background triggers. Right shows the detection statistic from PyCBC, which combines the SNR and their signal-consistency statistic. The lines show the background distributions. GW190425 is more significant than everything apart from GW170817. Adapted from Figures 1 and 6 of the GW190425 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/01/figures_m1_m2.pngGW190425 binary massesEstimated masses for the two components in the binary. We show results for two different spin limits. The two-dimensional shows the 90% probability contour, which follows a line of constant chirp mass. The one-dimensional plot shows individual masses; the dotted lines mark 90% bounds away from equal mass. The masses are in the range expected for neutron stars. Figure 3 of the GW190425 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/01/figures_mtot_dns-1.pngComparison of binary massesComparison of the total binary mass of the 10 known binary neutron stars in our Galaxy that will merge in a Hubble time and GW190425's source (with both the high-spin and low-spin assumptions). We also show a Gaussian fit to the Galactic binaries. GW190425's source is higher mass than previously known binary neutron stars. Figure 5 of the GW190425 Discovery Paper.https://cplberry.com/wp-content/uploads/2020/01/lalinference.pngLALInference sky localization for S190425zEarly sky localization for GW190425. Darker areas are more probable. This localization was circulated in GCN 24228 on 26 April and was used to guide follow-up, even though it covers a huge amount of the sky (the 90% area is about 18% of the sky).2021-06-26T14:11:28+00:00monthlyhttps://cplberry.com/2015/08/18/hold-b/https://cplberry.com/wp-content/uploads/2015/08/qualifications.jpgMy qualificationsMy collection of qualifications.https://cplberry.com/wp-content/uploads/2015/08/atlasgif-ngsversion-1438794000481.gifMaps of the ArcticNational Geographic atlases from 1999 to 2014, showing how Arctic ice has melted. 2021-03-20T18:11:04+00:00monthlyhttps://cplberry.com/2016/02/23/gw150914-the-papers/https://cplberry.com/wp-content/uploads/2016/02/comp_spin_pos1.pngGW150914 component spinsEstimated orientation and magnitude of the two component spins from the precessing IMRPhenom model. The magnitude is between 0 and 1 and is perfectly aligned with the orbital angular momentum if the angle is 0. The distribution for the more massive black hole is on the left, and for the smaller black hole on the right.https://cplberry.com/wp-content/uploads/2016/02/dist_thetajn1.pngGW150914 distance and inclinationEstimated luminosity distance and binary inclination angle. The dotted lines mark the edge of our 90% probability intervals. The different coloured curves show different models: they agree which made me incredibly happy!https://cplberry.com/wp-content/uploads/2016/02/final_mass_spin1.pngGW150914 final black hole mass and spinEstimated mass and spin for the final black hole. The dotted lines mark the edge of our 90% probability intervals. The different coloured curves show different models: they agree which still makes me incredibly happy!https://cplberry.com/wp-content/uploads/2016/02/m1_m21.pngGW150914 binary massesEstimated masses for the two black holes in the binary. The dotted lines mark the edge of our 90% probability intervals. The different coloured curves show different models: they agree which made me incredibly happy!https://cplberry.com/wp-content/uploads/2016/02/c01_reconstruction1.pngGW150914 recovered waveformsRecovered gravitational waveforms from our analysis of The Event. The dark band shows our estimate for the waveform without assuming a particular source. The light bands show results if we assume it is a binary black hole (BBH) as predicted by general relativity. They match really well!https://cplberry.com/wp-content/uploads/2016/02/contours1.pngGW150914 sky localizationThe different sky maps for GW150914 in an orthographic projection. The contours show the 90% region for each algorithm. The faint circles show lines of constant time delay between the two detectors. The LALInference map is our best result.https://cplberry.com/wp-content/uploads/2016/02/p_greaterthan_epo.pngGW150914 predicted number of detectionsThe percentage chance of making 0, 10, 35 and 70 more detections of binary black holes as time goes on and detector sensitivity improves (based upon our data so far).https://cplberry.com/wp-content/uploads/2016/02/waveformexplained-8.pngGravitational wave infographicThe shape of the gravitational wave encodes the properties of the source. This information is what lets us infer parameters. The example signal is GW150914. I made this explainer with Ban Farr and Nutsinee Kijbunchoo for the LIGO Magazine.https://cplberry.com/wp-content/uploads/2016/02/em-tiles.pngGW150914 EM follow-up footpirntsFootprints of observations compared with the 50% and 90% areas of the initially distributed (cWB: thick lines; LIB: thin lines) sky maps. The all-sky observations are not shown. The grey background is the Galactic plane.https://cplberry.com/wp-content/uploads/2016/02/em-timeline.pngGW150914 timelineTimeline for observations of GW15014. The top (grey) band shows information about gravitational waves. The second (blue) band shows high-energy (gamma- and X-ray) observations. The third and fourth (green) bands show optical and near-infrared observations respectively. The bottom (red) band shows radio observations.2021-03-03T17:09:17+00:00monthlyhttps://cplberry.com/2016/02/11/gw150914/https://cplberry.com/wp-content/uploads/2016/02/uob-vine.gifUoB applauseThe moment of the announcement of the first observation of gravitational waves. Credit: Kat Groverhttps://cplberry.com/wp-content/uploads/2016/02/c01_reconstruction.pngGW150914 recovered waveformsRecovered gravitational waveforms from our analysis of The Event. The dark band shows our estimate for the waveform without assuming a particular source. The light bands show results if we assume it is a binary black hole (BBH) as predicted by general relativity. They match really well!https://cplberry.com/wp-content/uploads/2016/02/lambda_g.pngGW150914 graviton Compton wavelength constraintsBounds on the Compton wavelength of the graviton. The Compton wavelength is a length defined by the mass of a particle: smaller masses mean large wavelengths. We place much better limits than existing tests from the Solar System or the double pulsar. There are some cosmological tests which are stronger still (but they make assumptions about dark matter).https://cplberry.com/wp-content/uploads/2016/02/fig1_split_v17_top_standalone.pngGW150914 filtered signalThe Event's signal as measured by LIGO Hanford and LIGO Livingston. The shown signal has been filtered to make it more presentable. You can clearly see that both observatories see that same signal, and even without fancy analysis, that there are definitely some wibbles there!https://cplberry.com/wp-content/uploads/2016/02/final_mass_spin.pngGW150914 final black hole mass and spinEstimated mass and spin for the final black hole. The dotted lines mark the edge of our 90% probability intervals. The different coloured curves show different models: they agree which still makes me incredibly happy!https://cplberry.com/wp-content/uploads/2016/02/m1_m2.pngGW150914 binary massesEstimated masses for the two black holes in the binary. The dotted lines mark the edge of our 90% probability intervals. The different coloured curves show different models: they agree which made me incredibly happy!https://cplberry.com/wp-content/uploads/2016/02/fig1_split_v17_bottom_standalone.pngGW150914 time–frequency plotA time–frequency plot that shows The Event's signal power in the detectors. You can see the signal increase in frequency as time goes on: the characteristic chirp of a binary merger!2021-02-27T14:44:57+00:00monthlyhttps://cplberry.com/2020/02/09/gw-data-guides/https://cplberry.com/wp-content/uploads/2020/02/figures_gaussnorm.pngHanford and Livingston residualsDistribution of residuals for 4 seconds of data around GW150914 after subtracting the maximum likelihood waveform. The residuals are the whitened Fourier amplitudes, and they should be consistent with a unit Gaussian. THe residuals follow the expected distribution and show no sign of non-Gaussianity. Figure 14 of the Data Analysis Guide.https://cplberry.com/wp-content/uploads/2020/02/figures_timeh1.pngHanford time seriesData processing to reveal GW150914. The top panel shows raw Hanford data. The second panel shows a window function being applied. The third panel shows the data after being whitened. The bottom panel shows the whitened data after a bandpass filter is applied to pick out the signal. We don't use the bandpass filter in our analysis (it is just for illustration), but the other steps reflect how we treat our data. Figure 2 of the Data Analysis Guide.https://cplberry.com/wp-content/uploads/2020/02/please-think-of-the-children.jpgHelen Lovejoy"Oh, won't somebody please think of the children?" Credit: Foxhttps://cplberry.com/wp-content/uploads/2020/02/data.gifDataExcited Data. Credit: Paramounthttps://cplberry.com/wp-content/uploads/2020/02/timeline-screenshot.pngTimeline ScreenshotScreenshot of the GWOSC Timeline showing observing from the fifth science run (S5) on the initial detector era through to the second observing run (O2) of the advanced detector era. Bars show observing of GEO 600 (G1), Hanford (H1 and H2), Livingston (L1) and Virgo (V1). Hanford initial had two detectors housed within its site, the plan in the advanced detector era is to install the equipment as LIGO India instead.https://cplberry.com/wp-content/uploads/2020/02/voiqru4dd193jsllwzmiruepsr4.gifDataI thought I saw a 2! Credit: Fox2021-01-25T10:55:44+00:00monthlyhttps://cplberry.com/2014/08/19/imbh/https://cplberry.com/wp-content/uploads/2014/08/2014-08-19-14-52-33.jpgMarshmallowsMarshmallows2020-09-02T12:16:52+00:00monthlyhttps://cplberry.com/2020/01/12/1903-04058/https://cplberry.com/wp-content/uploads/2020/01/y056rfb.pngEcceruElme's Falcon classExamples of the proposed Falcon glitch class, illustrating the key features (and where the name comes from). This new glitch class was suggested by Gravity Spy citizen scientist EcceruElme.https://cplberry.com/wp-content/uploads/2020/01/roc.pngRaven Peck and Water Jet searchesPerformance of the similarity search for Raven Peck (left) and Water Jet (right) glitches: the fraction of known glitches of the desired class that have a higher similarity score (compared to an example of that glitch class) than a given percentage of full data set. Results are shown for three different ways of defining similarity: the DIRECT machine-learning feature space (think line), a principal component analysis (medium line) and a comparison of pixels (thin line). Adapted from Figure 3 of Coughlin et al. (2019).https://cplberry.com/wp-content/uploads/2020/01/raven-peck-water-jet.pngNon-Gravity Spy classes of glitchExample Raven Peck (left) and Water Jet (right) glitches. These classes of glitch are not included in the usual Gravity Spy scheme. Adapted from Figure 3 of Coughlin et al. (2019).https://cplberry.com/wp-content/uploads/2020/01/new-glitches.pngNew Gravity Spy glitchesExample Helix (left) and Paired Dove glitches. These classes were identified by Gravity Spy citizen scientists. Helix glitches are related to related to hiccups in the auxiliary lasers used to calibrate the detectors by pushing on the mirrors. Paired Dove glitches are related to motion of the beamsplitter in the interferometer. Adapted from Figure 8 of Zevin et al. (2017).https://cplberry.com/wp-content/uploads/2020/01/training_set_feature_space.pngGlitch classification clustersVisualisation showing the clustering of different glitches in the Gravity Spy feature space. Each point is a different glitch from our training set. The feature space has more than three dimensions: this visualisation was made using a technique which preserves the separation and clustering of different and similar points. Figure 1 of Coughlin et al. (2019)https://cplberry.com/wp-content/uploads/2020/01/gravityspy-gw170104.pngGW170104 Gravity Spy spectrogramSpectrogram showing the upward-sweeping chirp of gravitational wave GW170104 as seen in Gravity Spy. I correctly classified this as a Chirp.https://cplberry.com/wp-content/uploads/2020/01/workflows.pngGravity Spy infrastructure including similarity searchHow Gravity Spy works: the interconnection of machine-learning classification and citizen-scientist classification. The similarity search is used to identify glitches similar to one which do not fit into current classes. Figure 2 of Coughlin et al. (2019).2020-08-01T21:36:34+00:00monthlyhttps://cplberry.com/2019/04/20/astro2020/https://cplberry.com/wp-content/uploads/2019/04/lisa-s.gifLisa SimpsonAs an aspiring scientist, Lisa Simpson is a strong supporter of the LISA mission. Credit: Foxhttps://cplberry.com/wp-content/uploads/2019/04/geodesic.pngOrbit around a rotating black holeA short section of an orbit around a spinning black hole. While inspirals last for years, this would represent only a few hours around a million solar mass black hole. The position is measured in terms of the gravitational radius.https://cplberry.com/wp-content/uploads/2019/04/fig_bbhrates.pngDetections and boost factorExpected rate of binary black hole detections per redshift bin as a function of A+ boost factor for three redshift bins. The merging binaries are assumed to be uniformly distributed with a constant merger rate roughly consistent with current observations: the solid line is about the current median, while the dashed and dotted lines are roughly the 90% bounds.https://cplberry.com/wp-content/uploads/2019/04/fig_imbhb-spectrum.pngLow-frequency noise curve parametersRequirements on the low-frequency noise power spectrum necessary to detect an optimally oriented intermediate-mass binary black hole system with two 100 solar mass components at a redshift of 10.https://cplberry.com/wp-content/uploads/2019/04/fig_boostq1.pngBoost, binary mass and redshiftThe boost factor (relative to A+) needed to detect a binary with a total mass out to a given redshift. The binaries are assumed to have equal-mass, nonspinning components. The blue curve highlights the reach at a boost factor of 10. The solid and dashed white lines indicate the maximum reach of Cosmic Explorer and the Einstein Telescope, respectively.https://cplberry.com/wp-content/uploads/2019/04/data.gifVictory for The Next Generation crewData is pleased. Credit: Paramounthttps://cplberry.com/wp-content/uploads/2019/04/horizon-fig-plus.pngDetection horizons for future gravitational-wave detectorsThe detection horizon (the distance to which sources can be detected) for Advanced LIGO (aLIGO), its upgrade A+, and the proposed Cosmic Explorer (CE) and Einstein Telescope (ET). The horizon is plotted for binaries with equal-mass, nonspinning components. Adapted from Hall & Evans (2019).https://cplberry.com/wp-content/uploads/2019/04/white-paper_waveform_time.pngIntermediate-mass binary black hole signalThe gravitational wave signal from the final stages of inspiral, merger and ringdown of a two 100 solar mass black holes at a redshift of 10. The signal chirps up in frequency. The colour coding shows parts of the signal above different frequencies.2020-08-01T21:11:44+00:00monthlyhttps://cplberry.com/2014/11/08/interstellar/https://cplberry.com/wp-content/uploads/2014/11/blackhole20190410.jpgThe shadow of a black holeThe shadow of a black hole reconstructed from the radio observations of the Event Horizon Telescope. The black hole lies at the center of M87, and is about 6.5 billion solar masses. Credit: Event Horizon Teamhttps://cplberry.com/wp-content/uploads/2014/11/fig152.pngRedshift and the INterstellar black holeLight-bending around a black hole. This is figure 15 from James, von Tunzelmann, Franklin & Thorne (2015). The top image shows an accretion disc as seen in Interstellar, but without the lens flare. The middle image also includes (Doppler and gravitational) redshifting that changes the colour of the light. To make the colour changes clear, the brightness has been artificially kept constant. The bottom image also includes the changes in brightness that would come with redshifting. This is what the black hole and accretion disc would actually look like, but it was though too confusing for the actual film.https://cplberry.com/wp-content/uploads/2014/11/f4a.pngEHT simulationSimulated Event Horizon Telescope image of Sagittarius A*.https://cplberry.com/wp-content/uploads/2014/11/milky-way-black-hole.pngEHT simulation of Sgr A*False colour image of what the Event Horizon Telescope could see when look at Sagittarius A*. https://cplberry.com/wp-content/uploads/2014/11/ut_interstellaropener_f.pngInterstellar GargantuaLight-bending around the black hole Gargantua in Interstellarhttps://cplberry.com/wp-content/uploads/2014/11/2014-08-08-16-35-03.jpgGravitation textbooksGravitation by Misner, Thorne &Wheeler, and General Theory of Relativity by Dirac.https://cplberry.com/wp-content/uploads/2014/11/interstellar_black_hole_.pngInterstellar black-hole close upGargantua, the black hole in Interstella2020-07-04T22:08:32+00:00monthlyhttps://cplberry.com/2014/10/26/right-good/https://cplberry.com/wp-content/uploads/2014/10/binary_pulsar.pngBinary pulsar plotThe orbital decay of the Hulse-Taylor binary pulsar (PSR B1913+16). The points are measured values, while the curve is the theoretical prediction for gravitational waves. Credit: Weisberg & Taylor (2005).https://cplberry.com/wp-content/uploads/2014/10/pp.pngThe pp chainThe stellar thermonuclear reactions, adapted from Giunti & Kim. The traditional names of the produced neutrinos are given in bold and the branch names are given in parentheses. Percentages indicate branching fractions.2020-06-07T22:35:54+00:00monthlyhttps://cplberry.com/2020/03/21/1912-04268/https://cplberry.com/wp-content/uploads/2020/03/num_sources.pngNumber of eclipsing sourcesProbability of observing at least one eclipsing source amongst a number of observed sources. Compact binary coalescences (CBCs, shown in purple) are the most rare, continuous gravitational waves (CGWs) eclipsed by the Sun (red) or by a companion (red) are more common. Here we assume companions are stars about a tenth the mass of the neutron star. The number of neutron stars with binary companions is estimated using the COSMIC population synthesis code. Figure 1 of Marchant et al. (2020).https://cplberry.com/wp-content/uploads/2020/03/sources2.pngEclipse scenariosTwo types of eclipse: the eclipse of a distant gravitational wave source by the Sun, and gravitational waves from an accreting neutron star eclipsed by its companion. Either scenario could enable us to see gravitational waves passing through a star. Figure 2 of Marchant et al. (2020).2020-03-21T23:58:34+00:00monthlyhttps://cplberry.com/2020/01/26/1903-07813/https://cplberry.com/wp-content/uploads/2020/01/bh-merger.gifBlack hole mergerCombining black holes. The result of a merger is a larger black hole with significant spin. From Dawn Finney.https://cplberry.com/wp-content/uploads/2020/01/rnaas.pngGenerational likelihoodRelative likelihood of a binary black hole being second-generation versus first-generation for different values of the chirp mass and the magnitude of the effective inspiral spin. The white contour gives the 90% credible area for GW170729. Figure 1 of Kimball et al. (2019).2020-03-21T19:27:21+00:00monthlyhttps://cplberry.com/2017/01/14/top-2016/2020-03-21T19:16:30+00:00monthlyhttps://cplberry.com/2015/05/14/1411-6934/https://cplberry.com/wp-content/uploads/2015/05/fig_4572_lalinference_relabel.pngBinary neutron-star sky mapProbability that of a gravitational-wave signal coming from different points on the sky. The darker the red, the higher the probability. The star indicates the true location. This is one of the worst localized events from our study for O1.https://cplberry.com/wp-content/uploads/2015/05/fig_mc_mean_sum_bias_err.pngChirp-mass biasFraction of events with difference between the mean estimated and true chirp mass smaller than a given value. There is an error because we are not including the effects of spin, but this is small. Again, the type of noise makes little difference. This is Figure 15 of Berry et al. (2015).https://cplberry.com/wp-content/uploads/2015/05/fig_90_snr.pngSky localization vs SNRSky localization (the size of the patch of the sky that we're 90% sure contains the source location) varies with the signal-to-noise ratio (how loud the signal is). The results for BAYESTAR and LALInference agree, as do the results with Gaussian and recoloured noise. This is Figure 9 of Berry et al. (2015).2020-02-09T21:27:31+00:00monthlyhttps://cplberry.com/2015/09/12/monty-carla/https://cplberry.com/wp-content/uploads/2015/09/montycarla.jpgMonty and CarlaMonty, Carla and the other samplers explore the probability landscape.2020-02-09T21:18:20+00:00monthlyhttps://cplberry.com/2016/12/10/gw150914-the-rise-of-the-revenge/https://cplberry.com/wp-content/uploads/2016/12/systematic_inclination.pngStudy of systematic errorsParameter estimation results for two different GW150914-like numerical relativity waveforms for different inclinations and polarization angles. The bands show the recovered 90% credible interval, and the dark lines the median values. The dotted lines show the true values. The (grey) polarization angle was chosen so that the detector is approximately insensitive to the plus polarization.https://cplberry.com/wp-content/uploads/2016/12/comp_spin_pos_comparison.pngGW150914 SEOBNRv3 comparison on component spinsComparison of orientations and magnitudes of the two component spins. The spin is perfectly aligned with the orbital angular momentum if the angle is 0. The left disk shows results using the precessing IMRPhenom model, the right using the precessing EOBNR model. In each, the distribution for the more massive black hole is on the left, and for the smaller black hole on the right.https://cplberry.com/wp-content/uploads/2016/12/seobnrv3_comp.pngGW150914 SEOBNRv3 comparisonComparison of parameter estimates for GW150914 using different waveform models. The bars show the 90% credible intervals, the dark bars show the uncertainty on the 5%, 50% and 95% quantiles from the finite number of posterior samples. The top bar is for the non-precessing EOBNR model, the middle is for the precessing IMRPhenom model, and the bottom is for the fully precessing EOBNR model.2020-02-09T21:16:02+00:00monthlyhttps://cplberry.com/2016/06/15/gw151226/https://cplberry.com/wp-content/uploads/2016/06/o1-significance.pngO1 CBC binary black hole search resultsSearch results for PyCBC (left) and GstLAL (right). The histograms show the number of candidate events (orange squares) compare to the background. The further an orange square is to the right of the lines, the more significant it is. Different backgrounds are shown including and excluding GW150914 (top row) and GW151226 (bottom row).https://cplberry.com/wp-content/uploads/2016/06/violin_all_panels.pngGW150914 and GW151226 waveform parameter boundsProbability distributions for waveform parameters. The top row shows bounds from just GW150914, the second from just GW151226, and the third from combining the two. A deviation of zero is consistent with general relativity.https://cplberry.com/wp-content/uploads/2016/06/stackedposterior_celest.pngO1 celestial sky localizationEstimated sky localization (in right ascension and declination) for each of the events in O1. The contours mark the 50% and 90% credible regions.https://cplberry.com/wp-content/uploads/2016/06/stackedposterior_earth.pngO1 sky localization relative to detectorsEstimated sky localization relative to the Earth for each of the events in O1. The contours mark the 50% and 90% credible regions. H+ and L+ mark the locations of the two observatories.https://cplberry.com/wp-content/uploads/2016/06/all_events_pe_distance.pngO1 luminosity distancesProbability distributions for the luminosity distance of the source of each of the three events in O1.https://cplberry.com/wp-content/uploads/2016/06/all_events_pe_mf_af.pngO1 final black hole masses and spinsEstimated masses and spins of the remnant black holes for each of the events in O1. The contours mark the 50% and 90% credible regions.https://cplberry.com/wp-content/uploads/2016/06/all_events_pe_mratio_chieff.pngO1 mass ratios and effective spinsEstimated mass ratios and effective spins for each of the events in O1. The contours mark the 50% and 90% credible regions.https://cplberry.com/wp-content/uploads/2016/06/all_events_pe_m1_m2.pngO1 binary black hole massesEstimated masses for the two binary black holes for each of the events in O1. The contours mark the 50% and 90% credible regions. The grey area is excluded from our convention on masses.https://cplberry.com/wp-content/uploads/2016/06/ligo-christmas.pngA LIGO ChristmasI assume someone left out milk and cookies at the observatories. A not too subtle hint from Nutsinee Kijbunchoo's comic in the LIGO Magazine. https://cplberry.com/wp-content/uploads/2016/06/comp_spin_pos.pngGW151226 component spinsEstimated orientation and magnitude of the two component spins. Calculated with our precessing waveform model. The distribution for the more massive black hole is on the left, and for the smaller black hole on the right.2020-02-08T15:55:27+00:00monthlyhttps://cplberry.com/2015/09/26/o1-is-here/https://cplberry.com/wp-content/uploads/2015/09/ligo_sites.pngThe LIGO sitesAerial views of LIGO Hanford (left) and LIGO Livingston (right). Credit: LIGO/Caltech/MIT.2020-02-08T15:54:23+00:00monthlyhttps://cplberry.com/2017/06/01/gw170104/https://cplberry.com/wp-content/uploads/2017/06/2017-06-03-15-18-27.jpgLake AnnecyView across Lac d'Annecy. Taken after the Gravitational Wave Physics and Astronomy Workshop, June 2017.https://cplberry.com/wp-content/uploads/2017/06/chieff_allevents_prior.pngEffective inspiral spin parameter for all eventsEstimated effective inspiral spin parameter for all events. To indicate how much (or little) we've learnt, the prior probability distribution for GW170104 is shown (the other priors are similar). Figure 5 of the GW170104 Supplemental Material.https://cplberry.com/wp-content/uploads/2017/06/dist_thetajn.pngGW170104 distance and inclinationEstimated luminosity distance and binary inclination angle. The two-dimensional shows the probability distribution for GW170104 as well as 50% and 90% contours. The one-dimensional plot shows results using different waveform models. The dotted lines mark the edge of our 90% probability intervals. Figure 4 of the GW170104 Supplemental Material.https://cplberry.com/wp-content/uploads/2017/06/final_mass_spin.pngGW170104 final black hole mass and spinEstimated mass and spin for the final black hole. The two-dimensional shows the probability distribution for GW170104 as well as 50% and 90% contours. The one-dimensional plot shows results using different waveform models. The dotted lines mark the edge of our 90% probability intervals. Figure 6 of the GW170104 Supplemental Material.https://cplberry.com/wp-content/uploads/2017/06/comp_spin_overall.pngGW170104 component spinsEstimated orientation and magnitude of the two component spins. The distribution for the more massive black hole is on the left, and for the smaller black hole on the right. The probability is binned into areas which have uniform prior probabilities, so if we had learnt nothing, the plot would be uniform. Part of Figure 3 of the GW170104 Discovery Paper.https://cplberry.com/wp-content/uploads/2017/06/eff_spins_prior.pngGW170104 effective spin parametersEstimated effective inspiral spin parameter and effective precession spin parameter. The two-dimensional shows the probability distribution for GW170104 as well as 50% and 90% contours. The one-dimensional plot shows results using different waveform models, as well as the prior probability distribution. The dotted lines mark the edge of our 90% probability intervals. We learn basically nothing about precession. Part of Figure 3 of the GW170104 Discovery Paper.https://cplberry.com/wp-content/uploads/2017/06/m1_m2_allevents.pngGW170104 binary masses together with previous eventsEstimated masses for the two black holes in the binary. The two-dimensional shows the probability distribution for GW170104 as well as 50% and 90% contours for all events. The one-dimensional plots show results using different waveform models. The dotted lines mark the edge of our 90% probability intervals. Figure 2 of the GW170104 Discovery Paper.https://cplberry.com/wp-content/uploads/2017/06/wf_reconstructions.pngGW170104 recovered waveformsRecovered gravitational waveforms from analysis of GW170104. The broader orange band shows our estimate for the waveform without assuming a particular source. The narrow blue bands show results if we assume it is a binary black hole (BBH) as predicted by general relativity. The two match nicely, showing no evidence for any extra features not included in the binary black hole models. Figure 4 of the GW170104 Discovery Paper.https://cplberry.com/wp-content/uploads/2017/06/h1l1-h1_dcs-calib_strain_c01-l1_dcs-calib_strain_c01-qscan_only.pngGW170104 spectrogramTime–frequency plots for GW170104 as measured by Hanford (top) and Livingston (bottom). The signal is clearly visible as the upward sweeping chirp. Part of Figure 1 of the GW170104 Discovery Paper.2020-02-08T15:50:09+00:00monthlyhttps://cplberry.com/2017/09/27/gw170814/https://cplberry.com/wp-content/uploads/2017/09/whitedata_strain_snr_qscan_v11.pngGW170814 Figure 1A cartoon of three different ways to visualise GW170814 in the three detectors. The top panel shows the signal-to-noise ratio the search template that matched GW170814. They peak at the time corresponding to the merger. The peaks are clear in Hanford and Livingston. The peak in Virgo is less exceptional, but it matches the expected time delay and amplitude for the signal. The middle panels show time–frequency plots. The upward sweeping chirp is visible in Hanford and Livingston, but less so in Virgo as it is less sensitive. The plot is zoomed in so that its possible to pick out the detail in Virgo, but the chirp is visible for a longer stretch of time than plotted in Livingston. The bottom panel shows whitened and band-passed strain data, together with the 90% region of the binary black hole templates used to infer the parameters of the source (the narrow dark band), and an unmodelled, coherent reconstruction of the signal (the wider light band) . The agreement between the templates and the reconstruction is a check that the gravitational waves match our expectations for binary black holes. The whitening of the data mirrors how we do the analysis, by weighting noise at different frequency by an estimate of their typical fluctuations. The signal does certainly look like the inspiral, merger and ringdown of a binary black hole. Figure 1 of the GW170814 Paper.https://cplberry.com/wp-content/uploads/2017/09/gw170814_localization.pngGW170814 localization90% probability localizations for GW170814. The large banana shaped (and banana coloured, but not banana flavoured) curve uses just the two LIGO detectors, the area is 1160 square degrees. The green shows the improvement adding Virgo, the area is just 100 square degrees. Both of these are calculated using BAYESTAR, a rapid localization algorithm. The purple map is the final localization from our full parameter estimation analysis, its area is just 60 square degrees. Whereas BAYESTAR only uses the best matching template from the search, the full parameter estimation analysis is free to explore a range of different templates. Part of Figure 3 of the GW170814 Paper.https://cplberry.com/wp-content/uploads/2017/09/41114_2016_4_fig10.jpgGravitational wave polarizationsThe six polarizations of a metric theory of gravity. The wave is travelling in the z direction. (a) and (b) are the plus and cross tensor polarizations of general relativity. (c) and (d) are the scalar breathing and longitudinal modes, and (e) and (f) are the vector polarizations. Figure 10 from Will (2014).https://cplberry.com/wp-content/uploads/2017/09/gravitationalwave_polarizations.gifGravitational wave polarizationsThe two polarizations of gravitational waves: plus (left) and cross (right). Here, the wave is travelling into or out of the screen. https://cplberry.com/wp-content/uploads/2017/09/smash-challenge.pngNew challenger approachingUnlocking a new character in Smash Bros. is always exciting.2020-01-28T02:20:40+00:00monthlyhttps://cplberry.com/2018/12/07/o2-catalogue/https://cplberry.com/wp-content/uploads/2018/12/figures_rate_v_z-1.pngRate evolutionEvolution of the binary black hole merger rate (blue), showing median, 50% and 90% intervals. For comparison, a non-evolving rate calculated using Model B is shown too. Fig. 6 of the O2 Populations Paper.https://cplberry.com/wp-content/uploads/2018/12/figures_posterior_spin_mag_both-horiz.pngSpin magnitude distributionsInferred spin magnitude distributions. The left shows results for the parametric distribution, assuming a mixture of almost aligned and isotropic spin, with the median (solid), 50% and 90% intervals shaded, and the posterior predictive distribution as the dashed line. Results are included both for beta distributions which can be singular at 0 and 1, and with these excluded. Model V is a very low spin model used for comparison. The right shows a binned reconstruction of the distribution for aligned and isotropic distributions, showing the median and 90% intervals. Fig. 8 of the O2 Populations Paper.https://cplberry.com/wp-content/uploads/2018/12/figures_rate_v_m1_q-1.pngMass distributionsBinary black hole merger rate as a function of primary mass (top) and mass ratio (bottom). The solid lines and bands show the medians and 90% intervala. The dashed line shows the posterior predictive distribution: our expectation for future observations averaging over our uncertainties. Fig. 2 of the O2 Populations Paper.https://cplberry.com/wp-content/uploads/2018/12/figures_theta_jn_distance_log-1.pngO1 and O2 distances and inclinationsEstimated luminosity distances and orbital inclinations for each of the events in O1 and O2. From lowest chirp mass (left; red) to highest (right; purple): GW170817 (solid), GW170608 (dashed), GW151226 (solid), GW151012 (dashed), GW170104 (solid), GW170814 (dashed), GW170809 (dashed), GW170818 (dashed), GW150914 (solid), GW170823 (dashed), GW170729 (solid). The contours mark the 90% credible regions. An inclination of zero means that we're looking face-on along the direction of the total angular momentum. Part of Fig. 7 of the O2 Catalogue Paper.https://cplberry.com/wp-content/uploads/2018/12/figures_chi_p_categorical_violin_conditioned-1.pngO1 and O2 effective precession spin parametersEstimated effective inspiral spin parameters for each of the events in O1 and O2. From lowest chirp mass (left; red) to highest (right; purple): GW170817, GW170608, GW151226, GW151012, GW170104, GW170814, GW170809, GW170818, GW150914, GW170823, GW170729. The left (coloured) part of the plot shows the posterior distribution; the right (white) shows the prior conditioned by the effective inspiral spin parameter constraints. Part of Fig. 5 of the O2 Catalogue Paper.https://cplberry.com/wp-content/uploads/2018/12/figures_chi_eff_sns_violin-1.pngO1 and O2 effective inspiral spin parametersEstimated effective inspiral spin parameters for each of the events in O1 and O2. From lowest chirp mass (left; red) to highest (right; purple): GW170817, GW170608, GW151226, GW151012, GW170104, GW170814, GW170809, GW170818, GW150914, GW170823, GW170729. Part of Fig. 5 of the O2 Catalogue Paper.https://cplberry.com/wp-content/uploads/2018/12/figures_mf_af_90pc-1.pngO1 and O2 final black hole masses and spinsEstimated final masses and spins for each of the binary black hole events in O1 and O2. From lowest chirp mass (left; red–orange) to highest (right; purple): GW170608 (dashed), GW151226 (solid), GW151012 (dashed), GW170104 (solid), GW170814 (dashed), GW170809 (dashed), GW170818 (dashed), GW150914 (solid), GW170823 (dashed), GW170729 (solid). The contours mark the 90% credible regions. Part of Fig. 4 of the O2 Catalogue Paper.https://cplberry.com/wp-content/uploads/2018/12/figures_m1_m2_90pc-2.pngO1 and O2 binary massesEstimated masses for the two binary objects for each of the events in O1 and O2. From lowest chirp mass (left; red) to highest (right; purple): GW170817 (solid), GW170608 (dashed), GW151226 (solid), GW151012 (dashed), GW170104 (solid), GW170814 (dashed), GW170809 (dashed), GW170818 (dashed), GW150914 (solid), GW170823 (dashed), GW170729 (solid). The contours mark the 90% credible regions. The grey area is excluded from our convention on masses. Part of Fig. 4 of the O2 Catalogue Paper.https://cplberry.com/wp-content/uploads/2018/12/figures_rate_v_z.pngRate evolutionEvolution of the binary black hole merger rate (blue), showing median, 50% and 90% intervals. For comparison, reference non-evolving rates (from the O2 Catalogue Paper) are shown too. Fig. 5 of the O2 Populations Paper.https://cplberry.com/wp-content/uploads/2018/12/figures_posterior_spin_mag_horiz.pngSpin magnitude distributionsInferred spin magnitude distributions. The left shows results for the parametric distribution, assuming a mixture of almost aligned and isotropic spin, with the median (solid), 50% and 90% intervals shaded, and the posterior predictive distribution as the dashed line. The right shows a binned reconstruction of the distribution for aligned and isotropic distributions, showing the median and 90% intervals. Fig. 7 of the O2 Populations Paper.2020-01-26T03:53:03+00:00monthlyhttps://cplberry.com/2020/01/19/1906-11299/https://cplberry.com/wp-content/uploads/2020/01/tausf.pngEnrichment probabiltyProbability of cluster enrichment and number of enriching binary neutron star mergers as a function of the timescale of star formation. Dashed lines are used of a cluster of a million solar masses and solid lines are used for a cluster of half this mass. Results are shown for Model D. THe build up happens around the same time in different models. FigProbability of cluster enrichment and number of enriching binary neutron star mergers as a function of the timescale of star formation. Dashed lines are used of a cluster of a million solar masses and solid lines are used for a cluster of half this mass. Results are shown for Model D. The build up happens around the same time in different models. Figure 5 in Zevin et al. (2019).ure 5 in Zevin et al. (2019).https://cplberry.com/wp-content/uploads/2020/01/primordial.pngProperties of enriching binary neutron starsPost-supernova binary neutron star properties (systemic velocity vs inspiral time, and orbital separation vs eccentricity) for our population models. The lines in the left-hand plots show the bounds for a binary to enrich a cluster of a given virial radius: viable binaries are below the lines. In both plots, red, blue and green points are the binaries which could enrich clusters of virial radii 1 pc, 3 pc and 10 pc; of the other points, purple indicates systems where the secondary star went through Case BB mass transfer. Figure 2 of Zevin et al. (2019).https://cplberry.com/wp-content/uploads/2020/01/periodic_table_v3.pngOrigin of the Solar System elementsPeriodic table showing the origins of different elements found in our Solar System. Credit: Jennifer Johnsonhttps://cplberry.com/wp-content/uploads/2020/01/cluster-e1579392189344.pngCluster binary formation timeTime taken for double black hole (DHB, shown in blue), neutron star–black hole (NSBH, shown in green), and double neutron star (DNS, shown in purple) binaries to form and then inspiral to merge in globular cluster simulations. Circles and dashed histograms show results for the standard cluster model. Triangles and solids histograms show results when black holes are artificially removed. Figure 1 of Zevin et al. (2019).https://cplberry.com/wp-content/uploads/2020/01/ngc1898_hubble_2913.jpgNGC 1898 globular clusterHubble Space Telescope image of the stars of NGC 1898, a globular cluster in the Large Magellanic Cloud. Credit: ESA/Hubble & NASA2020-01-23T18:29:14+00:00monthlyhttps://cplberry.com/2017/11/16/gw170608/https://cplberry.com/wp-content/uploads/2017/11/all-masses.pngLow-mass X-ray binary massesEstimated black hole masses inferred from low-mass X-ray binary observations. Figure 1 of Farr et al. (2011).https://cplberry.com/wp-content/uploads/2017/11/bh-family.pngKnitted black hole familyThe growing family of black holes. From Dawn Finney.https://cplberry.com/wp-content/uploads/2017/11/spindisk_imrppv2_c01_hlclean.pngGW170608 component spinsEstimated orientation and magnitude of the two component spins. The distribution for the more massive black hole is on the left, and for the smaller black hole on the right. The probability is binned into areas which have uniform prior probabilities, so if we had learnt nothing, the plot would be uniform. This analysis assumed spin magnitudes less than 0.89, which is why there is an apparent cut-off. Part of Figure 3 of the GW170608 Paper.https://cplberry.com/wp-content/uploads/2017/11/m1_m2_comp151226.pngGW170608 binary masses compared with GW151226Estimated masses for the two black holes in the binary. The two-dimensional shows the probability distribution for GW170608 as well as 50% and 90% contours for GW151226, the other contender for the lightest black hole binary. The one-dimensional plots on the sides show results using different waveform models. The dotted lines mark the edge of our 90% probability intervals. The one-dimensional plots at the top show the probability distributions for the total mass and chirp mass. Figure 2 of the GW170608 Paper.https://cplberry.com/wp-content/uploads/2017/11/p170608-q-transform.pngGW170608 spectrogramTime–frequency plots for GW170608 as measured by LIGO Hanford and Livingston. The chirp is clearer in Hanford, despite it being less sensitive, because of the sources position. Figure 1 of the GW170608 Paper.https://cplberry.com/wp-content/uploads/2017/11/a2l-lho.pngAngle-to-length commissioning disturbanceImprint of angular coupling commissioning in Hanford. The left panel shows a spectrogram of strain data, you can clearly see the excitations between ~19 Hz and ~23 Hz. The right panel shows the amplitude spectral density for Hanford before and during the procedure, as well as for Livingston. The commissioning adds extra noise in the broad peak about 20 Hz. There are no disturbances above ~30 Hz. Figure 4 of GW170608 Paper.https://cplberry.com/wp-content/uploads/2017/11/beampositionfluctuations.pngPitch to length couplingExamples of how angular fluctuations can couple to length measurements. Here are examples of how pitch rotations in the suspension level above the test mass can couple to length measurement. Yaw fluctuations can also have an impact. Figure 1 of Kasprzack & Yu (2016).2020-01-22T03:52:25+00:00monthlyhttps://cplberry.com/2017/10/16/gw170817/https://cplberry.com/wp-content/uploads/2017/10/screenshot_20190905-114234_messages.jpgScreenshot of text messagesText messages from our gravitational-wave candidate event database GraceDB. The final message is for GW170817, or as it was known at the time, G298048. It certainly caught my attention. The messages above are for GW170814, that was picked up multiple times by our search algorithms. It was a busy week.https://cplberry.com/wp-content/uploads/2017/10/76f6a3d2-5909-4f84-809a-be112653df18.jpgNobel medalA Nobel prize. Credit: Associated Press/F. Vergarahttps://cplberry.com/wp-content/uploads/2017/10/h0-inference.pngHubble constantPosterior probability distribution for the Hubble constant inferred from GW170817. The lines mark 68% and 95% intervals. The coloured bands are measurements from the cosmic microwave background (Planck) and supernovae (SHoES). Figure 1 of the GW170817 Hubble Constant Paper.https://cplberry.com/wp-content/uploads/2017/10/bns_figure4.pngGW170817 binary massesEstimated masses for the two neutron stars in the binary. We show results for two different (aligned) spin limits. The two-dimensional shows the 90% probability contour, which follows a line of constant chirp mass. The one-dimensional plot shows individual masses; the dotted lines mark 90% bounds away from equal mass. Figure 4 of the GW170817 Discovery Paper.https://cplberry.com/wp-content/uploads/2017/10/g1701866-v5-q-transform-30-1col-cside.pngGW170817 spectrogramTime–frequency plots for GW170104 as measured by Hanford, Livingston and Virgo. The signal is clearly visible in the two LIGO detectors as the upward sweeping chirp. It is not visible in Virgo because of its lower sensitivity and the source's position in the sky. Figure 1 of the GW170817 Discovery Paper.https://cplberry.com/wp-content/uploads/2017/10/timeline-with-spectrum-amgv7.pngTimeline of multimessenger observationsThe timeline of observations of GW170817's source. Shaded dashes indicate times when information was reported in a Circular. Solid lines show when the source was observable in a band: the circles show a comparison of brightnesses for representative observations. Figure 2 of the Multimessenger Astronomy Paper.https://cplberry.com/wp-content/uploads/2017/10/fig1.pngGW170817 localizations from gamma-rays, gravitational waves and optical observationsLocalization of the gravitational-wave, gamma-ray, and optical signals. The main panel shows initial gravitational-wave 90% areas in green (with and without Virgo) and gamma-rays in blue (the IPN triangulation from the time delay between Fermi and INTEGRAL, and the Fermi GBM localization). The inset shows the location of the optical counterpart (the top panel was tken 10.9 hours after merger, the lower panel is a pre-merger reference without the transient). Figure 1 of the Multimessenger Astronomy Paper.https://cplberry.com/wp-content/uploads/2017/10/bns_figure2.pngRaw Livingston GW170817 dataSpectrogram of Livingston data showing part of GW170817's chirp as well as the glitch. The lower panel shows how we removed the glitch: the grey line shows gating window that was applied for preliminary results, to zero the affected times, the blue shows a fitted model of the glitch that was subtracted for final results. Figure 2 of the GW170817 Discovery Paperhttps://cplberry.com/wp-content/uploads/2017/10/xbqqegq.gifJaws dolly zoomDolly zoom from Jaws2020-01-18T16:46:11+00:00monthlyhttps://cplberry.com/2020/01/02/1805-07370/https://cplberry.com/wp-content/uploads/2020/01/gw170814-lensing-figure1.pngGalaxy clusters and GW170814's sky locationSky localization for GW170814 and the galaxy clusters Abell 3084 (filled circle), and SMACS J0304.3−4401 (open). The left plot shows the low-latency Bayestar localization (LIGO only dotted, LIGO and Virgo solid), and the right shows the refined LALInference sky maps (solid from GCN 21493, which we used for our observations, and dotted from GWTC-1). The dashed lines shows the Galactic plane. Figure 1 of Smith et al. (2019). 2020-01-02T14:22:35+00:00monthlyhttps://cplberry.com/2018/06/16/1304-0670-2-the-explosioning/https://cplberry.com/wp-content/uploads/2018/06/obsscen_fig2_ranges_70.pngObserving timelinePlausible time line of observing runs with Advanced LIGO (Hanford and Livingston), advanced Virgo and KAGRA. It is too early to give a timeline for LIGO India. The numbers above the bars give binary neutron star ranges (italic for achieved, roman for target). Figure 2 of the Observing Scenarios Document.https://cplberry.com/wp-content/uploads/2018/06/bigtable.pngObserving ccenarios tableSummary of different observing scenarios with the advanced detectors. We assume a 70–75% duty factor for each instrument (including Virgo for the second scenario's sky localization, even though it only joined O2 for the final month). Table 3 from the Observing Scenarios Document.https://cplberry.com/wp-content/uploads/2018/06/fig_o1_far_70.pngO1 transient search resultsOffline transient search results from O1. The plot shows the number of events found verses false alarm rate: if there were no gravitational waves we would expect the points to follow the dashed line. The left panel shows the results of the templated search for compact binary coalescences, the right panel shows the unmodelled burst search. GW150914, GW151226 and LVT151012 are found by the templated search; GW150914 is also seen in the burst search. Arrows indicate bounds on the significance. Figure 3 of the Observing Scenarios Document.https://cplberry.com/wp-content/uploads/2018/06/fig_sensitivity_70.pngAdvanced LIGO, Avdance Virgo and KAGRA sensitivity curve progressionTarget evolution of the Advanced LIGO and Advanced Virgo detectors with time. The lower the sensitivity curve, the further away we can detect sources. The distances quoted are binary neutron star (BNS) ranges, the average distance we could detect a binary neutron star system. The BNS-optimized curve is a proposal to tweak the detectors for finding BNSs. Figure 1 of the Observing Scenarios Document.2019-08-20T20:11:46+00:00monthlyhttps://cplberry.com/2018/08/10/1801-08009/https://cplberry.com/wp-content/uploads/2018/08/banamuber.png3-dimensional fruitLeft: Localization (yellow) with a network of two low-sensitivity detectors. The sky location is uncertain, but we know the source must be nearby. Right: Localization (green) with a network of three high-sensitivity detectors. We have good constraints on the source location, but it could now be at a much greater range of distances. Not to scale.https://cplberry.com/wp-content/uploads/2018/08/fig_dp_90_vol_snr.png90% localization volumesLocalization volume as a function of signal-to-noise ratio. The top panel shows results for two-detector observations: the LIGO-Hanford and LIGO-Livingston (HL) network similar to in the first observing run, and the LIGO and Virgo (HLV) network similar to the second observing run. The bottom panel shows all observations for the HLV network including those with all three detectors which are colour coded by the fraction of the total signal-to-noise ratio from Virgo. In both panels, there are fiducial lines scaling inversely with the sixth power of the signal-to-noise ratio. Adapted from Fig. 4 of Del Pozzo et al. (2018).https://cplberry.com/wp-content/uploads/2018/08/galaxies_3d_dp.pngMost probable galaxiesGalaxies within the 90% credible volume of an example simulated source, colour coded by probability. The galaxies are from the GLADE Catalogue; incompleteness in the plane of the Milky Way causes the missing wedge of galaxies. Part of Figure 5 of Del Pozzo et al. (2018).2019-08-20T20:10:41+00:00monthlyhttps://cplberry.com/2018/06/11/1711-06287/https://cplberry.com/wp-content/uploads/2018/06/standarddeviationplotcut.pngPopulation synthesis parameter measurement precisionMeasurement precision for the four population parameters after 1000 detections. We quantify the precision with the standard deviation estimated from the Fisher matrix. We show results from 1500 realisations of the population to give an idea of scatter. Figure 5 of Barrett et al. (2018)https://cplberry.com/wp-content/uploads/2018/06/freqbootstrappedellipsescut.pngPopulation synthesis Fisher matrix covariancesFisher matrix estimates for measurement precision of the four population parameters. We show 1500 different realisations of the binary population to give an idea of scatter. Figure 6 of Barrett et al. (2018)https://cplberry.com/wp-content/uploads/2018/06/differentredshiftscut.pngCOMPAS binary black hole merger ratesBinary black hole merger rate at three different redshifts as calculated by COMPAS. We show the rate in 30 different chirp mass bins for our default population parameters. Figure 2 of Barrett et al. (2018)2019-07-09T17:09:01+00:00monthlyhttps://cplberry.com/2017/09/09/1703-06873/https://cplberry.com/wp-content/uploads/2017/09/triangle_plot.gifTriangle plot for formation channel fractionsProbability distribution for the fraction of binaries from each of the four spin misalignment populations for different numbers of observations.2018-12-05T12:10:53+00:00monthlyhttps://cplberry.com/2016/10/22/1603-07333/https://cplberry.com/wp-content/uploads/2016/10/proj3d1.png3D localiztion with LIGO detectorsThree-dimensional localization showing the 20%, 50%, and 90% credible levels for a typical two-detector early Advanced LIGO event. The Earth is shown at the centre. The true location is marked by the cross.2018-08-10T20:37:09+00:00monthlyhttps://cplberry.com/2018/03/31/1608-08951/https://cplberry.com/wp-content/uploads/2018/03/1104519.jpgDr. STransient resonances remind me of Spirographs. Thanks Frinkiachttps://cplberry.com/wp-content/uploads/2018/03/fig_res_pop_snr_overlap.pngFig_res_pop_SNR_overlapDistribution of signal-to-noise ratios for extreme-mass-ratio inspirals. In blue (solid outline), we have the results ignoring transient resonances. In orange (dashed outline), we have the distribution including the reduction due to resonance jumps. Events falling below 15 are deemed to be undetectable. Figure 10 of Berry et al. (2016)https://cplberry.com/wp-content/uploads/2018/03/2to3resonantorbit2.gif2:3 resonance EMRIA 2:3 resonance traces the same parts of the radial–polar coordinate space over and over. Credit: Rob Colehttps://cplberry.com/wp-content/uploads/2018/03/nonresonantorbit.gifNon-resonant EMRIA non-resonant orbit will eventually fill the radial–polar coordinate plane. Credit: Rob Colehttps://cplberry.com/wp-content/uploads/2018/03/fig_res_jump_calc_white.pngTransient resonance jumpA jump in the orbital energy across a 2:3 resonance. The plot shows the difference between the approximate adiabatic evolution and the instantaneous evolution including the resonance. The thickness of the blue line is from oscillations on the orbital timescale which is too short to resolve here. The dotted red line shows the fitted size of the jump. Figure 4 of Berry et al. (2016)2018-07-05T13:40:07+00:00monthlyhttps://cplberry.com/2016/03/05/1304-0670/https://cplberry.com/wp-content/uploads/2016/03/aligo_adv_sensitivity.pngAdvanced LIGO and Advanced Virgo sensitivity timelinePlausible evolution of the Advanced LIGO and Advanced Virgo detectors with time. The lower the sensitivity curve, the further away we can detect sources. The distances quoted are ranges we could see binary neutrons stars (BNSs) to. The BNS-optimized curve is a proposal to tweak the detectors for finding BNSs.2018-06-16T17:34:56+00:00monthlyhttps://cplberry.com/2018/05/23/1703-09722/https://cplberry.com/wp-content/uploads/2018/05/emrideltaq.pngQuadrupole deviation uncerrtaintyDistribution of (one standard deviation) of uncertainties for deviations in the quadrupole moment of the massive object spacetime. Results are shown for the different astrophysical models, and for the different waveform models. Figure 13 of Babak et al. (2017).https://cplberry.com/wp-content/uploads/2018/05/emrideltad_over_d.pngFractional distance uncertaintyDistribution of (one standard deviation) fractional uncertainties for measurements of the luminosity distance. Results are shown for the different astrophysical models, and for the different waveform models. Part of Figure 12 of Babak et al. (2017).https://cplberry.com/wp-content/uploads/2018/05/emrideltaspin.pngSpin uncertaintyDistribution of (one standard deviation) uncertainties for measurements of the massive black hole spin. Results are shown for the different astrophysical models, and for the different waveform models. The measurements are more precise with the AKK model, as this includes extra signal from the end of the inspiral. Part of Figure 11 of Babak et al. (2017).https://cplberry.com/wp-content/uploads/2018/05/emrideltam_over_m.pngFractional mass uncertaintyDistribution of (one standard deviation) fractional uncertainties for measurements of the massive black hole (redshifted) mass. Results are shown for the different astrophysical models, and for the different waveform models. The measurements are more precise with the AKK model, as this includes extra signal from the end of the inspiral. Part of Figure 11 of Babak et al. (2017).https://cplberry.com/wp-content/uploads/2018/05/tumblr_owvtl9ny5k1qf5hjqo4_540.gifCaptain America PatienceOne of the most valuable traits a student or soldier can have: patience. Credit: Sony/Marvelhttps://cplberry.com/wp-content/uploads/2018/05/mbins.pngEMRIs as a function of massNumber of extreme-mass-ratio inspirals for different size massive black holes in different astrophysical models. Model 1 (M1) is our best estimate, the others explore variations on this. Models 11 and 12 (M11 and M12) are designed to be cover the extremes, being the most pessimistic and optimistic combinations. The solid and dashed lines are for two different waveform models, which are designed to give an indication of potential variation. They agree for models 10 and 11 (M10 and M11) where the massive black hole is not spinning. Figure 8 of Babak et al. (2017).https://cplberry.com/wp-content/uploads/2018/05/ngc4676_hst.jpgNGC 4676 The MiceHubble image of the colliding galaxies known as The Mice. Credit: ACS Science & Engineering Teamhttps://cplberry.com/wp-content/uploads/2018/05/emri_0.jpgExtreme-mass-ratio inspiralArtistic impression of the spacetime for an extreme-mass-ratio inspiral, with a smaller stellar-mass black hole orbiting a massive black hole. This image is mandatory when talking about extreme-mass-ratio inspirals. Credit: NASA2018-06-15T18:04:02+00:00monthlyhttps://cplberry.com/2015/01/10/1408-0740/https://cplberry.com/wp-content/uploads/2015/01/energy_density.pngEnergy-density spectrumGravitational-wave sensitivity-curve plot using the energy density that cosmologists love. The proper name of the plotted quantity is the critical energy density per logarithmic frequency interval multiplied by the reduced Hubble constant squared. I prefer Bob.https://cplberry.com/wp-content/uploads/2015/01/asd.pngGravitational-wave ASDGravitational-wave sensitivity-curve plot using the square root of the power spectral density (the amplitude spectral density).https://cplberry.com/wp-content/uploads/2015/01/characteristic_strain.pngCharacteristic-strain spectrumGravitational-wave sensitivity-curve plot using characteristic strain. The area between the detector's curve and the top of the box for a source indicates how loud that signal would be.2020-01-13T14:25:26+00:00monthlyhttps://cplberry.com/2016/10/01/1508-05336/https://cplberry.com/wp-content/uploads/2016/10/2016-10-06-14-55-41.jpgWoolly gravitational wave sky localizationA knitted globe with the two LIGO sites marked in red, and a typical gravitational-wave sky localization stitched on. The handiwork of Hannah Middleton.https://cplberry.com/wp-content/uploads/2016/10/mass_snr.pngMass fraction uncertainty vs SNRFractional statistical uncertainties in chirp mass (top), mass ratio (middle) and total mass (bottom) estimates as a function of network signal-to-noise ratio for both the fully spinning analysis and the quicker non-spinning analysis. The lines indicate approximate power-law trends to guide the eye.https://cplberry.com/wp-content/uploads/2016/10/mass_comp.pngProbability distributions for binary neutron star massesRough outlines for 90% credible regions for component masses for a random assortments of signals. The circles show the true values. The coloured lines indicate the extent of the distribution with different limits on the spins. The grey area is excluded from our convention on masses.https://cplberry.com/wp-content/uploads/2016/10/time_hist.pngCode run timeDistribution of run times for binary neutron star signals. Low-latency sky localization is done with BAYESTAR; medium-latency non-spinning parameter estimation is done with LALInference and TaylorF2 waveforms, and high-latency fully spinning parameter estimation is done with LALInference and SpinTaylorT4 waveforms. The LALInference results are for 2000 posterior samples.2017-10-15T18:14:06+00:00monthlyhttps://cplberry.com/2016/08/27/1602-02453/https://cplberry.com/wp-content/uploads/2016/08/imrtgr_plots.pngGW150914 inspiral/merger–ringdown consistency testResults from the consistency test for The Event. The top panels final mass and spin measurements from the low frequency (inspiral) part of the waveform, the high frequency (post-inspiral) part, and the entire (IMR) waveform. The bottom panel shows the fractional difference between the high and low frequency results. If general relativity is correct, we expect the distribution to be consistent with (0,0), indicated by the cross. https://cplberry.com/wp-content/uploads/2016/08/imrtgr_plots_single_posterior.pngInspiral/merger–ringdown consistency testResults from the consistency test. The top panels show the outlines of the 50% and 90% credible levels for the low frequency (inspiral) part of the waveform, the high frequency (merger–ringdown) part, and the entire (inspiral–merger–ringdown, IMR) waveform. The bottom panel shows the fractional difference between the high and low frequency results. If general relativity is correct, we expect the distribution to be consistent with (0,0), indicated by the cross. The left panels show a general relativity simulation, and the right panel shows a waveform from a modified theory of gravity.2017-10-15T12:42:30+00:00monthlyhttps://cplberry.com/2017/09/24/o1-papers/https://cplberry.com/wp-content/uploads/2017/09/e_v_f.pngO1 burst uppler limits on gravitational-wave energyGravitational-wave energy at 50% detection efficiency for standard sources at a distance of 10 kpc. Figure 2 of the O1 Burst Paperhttps://cplberry.com/wp-content/uploads/2017/09/grb150906b_errorbox_cropped.pngGRB 150906B localizationInterplanetary Network (IPN) localization for GRB 150906B and nearby galaxies. Figure 1 from the O1 Gamma-Ray Burst Paper.https://cplberry.com/wp-content/uploads/2017/09/o1-neutronstar.pngComparison of O1 upper limits to estimatesComparison of upper limits for binary neutron star (BNS; top) and neutron star–black hole binaries (NSBH; bottom) merger rates with theoretical and observational limits. The blue bars show O1 limits, the green and orange bars show projections for future observing runs. Figures 6 and 7 from the O1 Binary Neutron Star/Neutron Star–Black Hole Paper.https://cplberry.com/wp-content/uploads/2017/09/figure4.pngO1 BNS upper limits90% confidence upper limits on the binary neutron star merger rate. These rates assume randomly orientated spins up to 0.05. Figure 4 of the O1 Binary Neutron Star/Neutron Star–Black Hole Paper.https://cplberry.com/wp-content/uploads/2017/09/imbhb_2d.pngO1 IMBHB upper limitsResults from the O1 search for intermediate mass black hole binaries. The left panel shows the 90% confidence upper limit on the merger rate (per cubic gigaparsec per year). The right panel shows the effective search distance (in gigaparsec). Each circle is a different injection. All have zero spin, except two 100+100 solar mass sets, where chi indicates the spins . Figure 2 of the O1 Intermediate Mass Black Hole Binary Paper.2017-10-13T13:17:42+00:00monthlyhttps://cplberry.com/2017/07/23/summer-is-coming/https://cplberry.com/wp-content/uploads/2017/07/instagram-day-2-53.jpgKit Harington, Emilia Clarke and Peter DinklageGame of Thrones stars Kit Harington, Emilia Clarke and Peter Dinklage, Comic-Con 2013https://cplberry.com/wp-content/uploads/2017/07/seven-of-nine.jpgSeven of NineStart Trek: Voyager's Seven of Ninehttps://cplberry.com/wp-content/uploads/2017/07/grail.jpgHoly GrailChoose wiselyhttps://cplberry.com/wp-content/uploads/2017/07/trogdor.pngTrogdor!Trogdor2017-07-30T17:22:59+00:00monthlyhttps://cplberry.com/2014/09/24/how-big-is-a-black-hole/https://cplberry.com/wp-content/uploads/2014/09/daisy.jpgDaisyDaisy, a spherical cowhttps://cplberry.com/wp-content/uploads/2014/09/no-return-sign.jpgNo return signPoint of no return2016-11-25T10:25:17+00:00monthlyhttps://cplberry.com/2016/11/19/1510-03621/https://cplberry.com/wp-content/uploads/2016/11/ul_full.png90% upper limits on continuous gravitational-wave strains90% confidence upper limits on the gravitational-wave strain at different frequencies. Each dot is for a different 1 Hz band. Some bands are noisy and feature instrumental artefacts which have to be excluded from the analysis, these are noted as the filled (magenta) circles. In this case, the upper limit only applies to the part of the band away from the disturbance.2016-11-19T13:50:07+00:00monthlyhttps://cplberry.com/2016/05/30/1510-03474/https://cplberry.com/wp-content/uploads/2016/05/2016-05-30-15-58-531.jpgBank holiday ScrabbleBank holiday family Scrabble game.https://cplberry.com/wp-content/uploads/2016/05/milkyway_pulsars_local2.pngOrion spur spotlightsArtist's impression of the local part of the Milky Way. The Orion spur connects the Perseus and Sagittarius arms. The yellow cones mark the extent of the search (the pink circle shows the equivalent all-sky sensitivity). Green stars indicate known pulsars.2016-10-08T15:29:48+00:00monthlyhttps://cplberry.com/2016/10/08/1605-03233/https://cplberry.com/wp-content/uploads/2016/10/search_reach.pngS6 all-sky search reachRange of the PowerFlux search for rotating neutron stars assuming that spin-down is entirely due to gravitational waves. The solid lines show the upper limits as a function of the gravitational-wave frequency and its rate of change; the dashed lines are the corresponding limits on ellipticity, and the dotted line marks the maximum searched spin-down.2016-10-08T15:28:18+00:00monthlyhttps://cplberry.com/2016/08/23/1605-01707/https://cplberry.com/wp-content/uploads/2016/08/fig_binomialtest-e1471968398213.pngRadio transient/gravitational wave search resultsSearch results for gravitational waves coincident with radio transients. The probabilities for each time containing just noise (blue) match the expected background distribution (dashed). This is consistent with a non-detection.2016-10-08T11:57:37+00:00monthlyhttps://cplberry.com/2015/01/31/1410-8310/https://cplberry.com/wp-content/uploads/2015/01/zoidberg.jpgZoidberg non-detectionThis paper doesn't claim a detection of gravitational waves, but it doesn't stink like Zoidberg.https://cplberry.com/wp-content/uploads/2015/01/crab_xrayopt_full.jpgCrab pulsar in X-ray and optical lightComposite image of Hubble (red) optical observations and Chandra (blue) X-ray observations of the Crab pulsar. Credit: Hester et al.https://cplberry.com/wp-content/uploads/2015/01/lighthouse.gifPulsar lighthouseThe mandatory cartoon of a pulsar that everyone uses. Credit: M. Kramer2016-10-08T11:55:02+00:00monthlyhttps://cplberry.com/2015/05/23/the-a-level-team/https://cplberry.com/wp-content/uploads/2015/05/fig_number_asym1.pngA-level asymmetry vs numberSmoothed distribution of gender asymmetry for AS subjects (in England 2013/2014). The area under the curve gives the number of subjects.https://cplberry.com/wp-content/uploads/2015/05/fig_subject_asym1.pngA-level asymmetrySmoothed distribution of gender asymmetry for AS subjects (in England 2013/2014). The area under the curve gives the number of subjects.https://cplberry.com/wp-content/uploads/2015/05/fig_subject_asym_big.pngA-level asymmetry with smoothingHeavily smoothed distribution of gender asymmetry for AS subjects (in England 2013/2014). The area under the curve gives the number of subjects.https://cplberry.com/wp-content/uploads/2015/05/computing_psychology.pngLovelace and FreudAda, Countess of Lovelace, mathematician and first computer programmer, and Sigmund Freud, neurologist and founder of psychoanalysis.https://cplberry.com/wp-content/uploads/2015/05/fig_continue_asym.pngA-level continuation vs asymmetryScatter plot of the gender asymmetry and difference in percentage progression of AS subjects (in England 2013/2014).https://cplberry.com/wp-content/uploads/2015/05/fig_continue_rank1.pngA-level continuationPercentage continuation from AS to A2 for different subjects (in England 2013/2014). The dotted line indicates the average.https://cplberry.com/wp-content/uploads/2015/05/fig_colour_rank.pngA-level numberStudent numbers in the most popular subjects at AS level (in England 2013/2014).2016-10-01T14:05:29+00:00monthlyhttps://cplberry.com/2015/11/07/1412-5942/https://cplberry.com/wp-content/uploads/2015/11/postcasa_snr_positions_greentext2.jpgSearched supernova remnantsThe nine young supernova remnants searched for continuous gravitational waves. The yellow dot marks the position of the Solar System. The green markers show the supernova remnants, which are close to the Galactic plane. Two possible positions for Vela Jr were used, since we are uncertain of its distance. Original image: NASA/JPL-Caltech/ESO/R. Hurt.https://cplberry.com/wp-content/uploads/2015/10/g19_lg.jpgA supernova remnant in the Milky Way located about 28,000 light years from EarthThe youngest known supernova remnant, G1.9+0.3, observed in X-ray and optical light. The ejected material forms a shock wave as it pushes the interstellar material out of the way. Credit: NASA/CXC/NCSU/DSS/Borkowski et al.2016-10-01T13:59:17+00:00monthlyhttps://cplberry.com/2015/11/21/gr100/https://cplberry.com/wp-content/uploads/2015/11/einsteinshow.jpgEinstein blackboardHappy birthday general relativity! Einstein presented his field equations to the Prussian Academy of Science on 25 November 1915.https://cplberry.com/wp-content/uploads/2015/11/postersmall.pngThe search for gravitational wavesMerging black holes create ripples in space time. These can be detected with a laser interferometer. Credit: Gravitational Wave Grouphttps://cplberry.com/wp-content/uploads/2015/11/map-geodesic.jpgGeodesic mapThe shortest way to travel from London Heathrow airport (LHR) to JFK International airport (JFK). Credit: Mr Reid.2016-08-27T16:59:56+00:00monthlyhttps://cplberry.com/2016/06/04/1511-01431/https://cplberry.com/wp-content/uploads/2016/06/prob_m1source_over_100_func_m1source.pngProbability of 100 solar mass sourceProbability that the larger black hole is over 100 solar masses. The mass ratio is the mass of the stellar-mass black hole divided by the mass of the intermediate-mass black hole.https://cplberry.com/wp-content/uploads/2016/06/mtot-mc-bounds.pngChirp-mass accuracyMeasured chirp mass for systems of different total masses. The shaded regions show the 90% credible interval and the dashed lines show the true values. The mass ratio is the mass of the stellar-mass black hole divided by the mass of the intermediate-mass black hole.https://cplberry.com/wp-content/uploads/2016/06/mtot-mtotal-bounds.pngTotal-mass accuracyMeasured total mass for systems of different total masses. The shaded regions show the 90% credible interval and the dashed lines show the true values. The mass ratio is the mass of the stellar-mass black hole divided by the mass of the intermediate-mass black hole.https://cplberry.com/wp-content/uploads/2016/06/il_570xn-198887243.jpgAdopt a black holeAdorable black hole (available for adoption).2016-08-27T12:27:15+00:00monthlyhttps://cplberry.com/2016/07/16/pokemon-li-go/https://cplberry.com/wp-content/uploads/2016/07/550259main_arctafull.jpgCentaurus A's jetsJets from Centaurus A are bigger than the galaxy itself! This image is a composite of X-ray (blue), microwave (orange) and visible light. You can see the jets pushing out huge bubbles above and below the galaxy. We think the jets are powered by the galaxy's central supermassive black hole. https://cplberry.com/wp-content/uploads/2016/07/bh.jpgBlack hole PokémonMy black hole Pokémon2016-08-14T14:03:21+00:00monthlyhttps://cplberry.com/2014/12/23/humbug/https://cplberry.com/wp-content/uploads/2014/12/bulletcluster_12.jpgThe bullet cluster: smoking gun for dark matterThe merging bullet cluster. A composite of an optical image (showing galaxies), an X-ray image (in red, showing the hot gas), and a map of the total mass (in blue, from gravitational lensing).https://cplberry.com/wp-content/uploads/2014/12/esa_rosetta_osiris_colour.jpgRosetta OSIRISColour image of 67P/Churyumov-Gerasimenko from Rosetta. Credit: ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDAhttps://cplberry.com/wp-content/uploads/2014/12/297755main_gpn-2001-000009_full.jpgApollo 8 EarthriseEarthrisehttps://cplberry.com/wp-content/uploads/2014/12/image_1864_2e-kepler-186f.jpgKepler-186fKepler-186, a system which has a planet on the edge of the habitable zone.https://cplberry.com/wp-content/uploads/2014/12/nhov20141201_0058.jpgNew Horizons 2014/12/01Full trajectory of New Horizonshttps://cplberry.com/wp-content/uploads/2014/12/ssc2011-05b_sm.jpgHow gravitational lensing works.Gravitational lensing by a galaxy cluster.https://cplberry.com/wp-content/uploads/2014/12/alma-hl-tau-protoplanetary-disk.jpgHL Tau protoplanetary discALMA image of the young star HL Tau and its protoplanetary disc. This best image ever of planet formation reveals multiple rings and gaps that herald the presence of emerging planets as they sweep their orbits clear of dust and gas. Credit: ALMA, C. Brogan & B. Saxtonhttps://cplberry.com/wp-content/uploads/2014/12/7443_20130617073008_bsc3_130606_15-13-51_llo_itmx.jpgLIGO commissioningInspection of LIGO optical systems.https://cplberry.com/wp-content/uploads/2014/12/hireslivingston_7.jpgLIGO LivingstonLIGO Livingston, Louisiana.https://cplberry.com/wp-content/uploads/2014/12/square.pngAbell 209 componentsDifferent views of cluster Abell 2092016-07-15T16:42:21+00:00monthlyhttps://cplberry.com/2016/04/02/1511-04398/https://cplberry.com/wp-content/uploads/2016/04/far_s5_s6.pngSTAMP S5 and S6 searchFalse alarm rate (FAR) distribution of triggers from S5 (black circles) and S6 (red triangles) as a function of the signal-to-noise ratio. The background noise distributions are shown by the solid black and dashed red lines respectively. An idealised Gaussian noise background is shown in cyan. There are no triggers significantly above the expected background level.https://cplberry.com/wp-content/uploads/2016/04/2016-03-21-18-51-25.jpgGrand CanyonSunset over the Grand Canyon. One of the perks of academia is the travel. A group of us from Birmingham went on a small adventure after the LIGO–Virgo Meeting.https://cplberry.com/wp-content/uploads/2016/04/2016-03-15-19-24-34.jpgLVC cakeCelebratory cake from the March LIGO–Virgo Meeting. It was delicious.2016-06-05T11:53:53+00:00monthlyhttps://cplberry.com/2015/04/24/1412-0605/https://cplberry.com/wp-content/uploads/2015/04/swift-scox-1.jpgScorpius X-1 in X-raySwift X-ray Telescope image of Scorpius X-1 and the X-ray nova J1745-26 (a stellar-mass black hole), along with the scale of moon, as they would appear in the field of view from Earth. Credit: NASA/Goddard Space Flight Center/S. Immler and H. Krimm2016-05-30T11:57:28+00:00monthlyhttps://cplberry.com/2015/12/09/ocelots/https://cplberry.com/wp-content/uploads/2015/11/2015-06-16-09-40-01.jpgKAGRA control roomThe control room of KAGRA, the gravitational-wave detector in the Hida Mountains, Japan. I visited June 2015.https://cplberry.com/wp-content/uploads/2015/11/announcements-physics.jpg2015 Physics announcement2015 Physics Nobel laureates, Takaaki Kajita and Arthur B. McDonald. Credit: Nobel Foundation.https://cplberry.com/wp-content/uploads/2015/11/sno-hi-res.jpgSNOThe Sudbury Neutrino Observatory detector, a 12-metre sphere containing 1000 tonnes of heavy water which is two kilometres underground. Credit: SNOLAB.https://cplberry.com/wp-content/uploads/2015/10/sun-at-night.jpgThe neutrino Sun at nightThe Sun at night. Solar neutrinos as detected by Super-Kamioknade looking through the Earth. Credit: Marcus Chown & Super-Kamiokande.https://cplberry.com/wp-content/uploads/2015/10/particle_poster_big_2012.jpgThe Particle ZooThe charming bestiary of subatomic particles made by Particle Zoo.2016-02-27T14:47:51+00:00monthlyhttps://cplberry.com/2015/03/15/1411-4547/https://cplberry.com/wp-content/uploads/2015/03/cqg507871f1_online.jpgAdvanced LIGO interferometerFig. 1 from Aasi et al. (2015), the Advanced LIGO optical configuration. All the acronyms have to be carefully placed in order for things to work. The laser beam starts from the left, passing through subsystems to make sure it's stable. The two interferometer arms are at the top and right of the diagram. The laser is bounced many times between the mirrors to build up sensitivity. The interference pattern is read out at the bottom. Normally, the light should interfere destructively, so the output is dark. A change to this indicates a change in length between the arms. That could be because of a passing gravitational wave.2015-09-26T15:33:01+00:00monthlyhttps://cplberry.com/2014/09/07/sports-science/https://cplberry.com/wp-content/uploads/2014/09/cadbury_chocolate_medals__47462_zoom.jpgCadbury's chocolate medalsChocolate modelshttps://cplberry.com/wp-content/uploads/2014/09/the-breakfast-club-movie-poster.jpgThe Breakfast Club movie posterThe Breakfast Club2015-05-23T18:57:51+00:00monthlyhttps://cplberry.com/2014/09/28/white-pink-and-camouflage/https://cplberry.com/wp-content/uploads/2014/09/thebigbangtheory.jpgThe Big Bang Theory gangThe Big Bang Theory's popularity has been credited with encouraging more students to take physics. The cast reflects traditional stereotypes: the men are physicists, an astronomer and an engineer, the women are two biologists and Penny.2015-05-23T18:57:38+00:00monthlyhttps://cplberry.com/2014/11/02/peter-piper/2015-02-27T16:16:38+00:00monthlyhttps://cplberry.com/2015/02/27/peck-pickled-peppers/2015-02-27T16:13:41+00:00monthlyhttps://cplberry.com/2014/10/18/imply/https://cplberry.com/wp-content/uploads/2014/10/impossible.jpgImpossibleMr. Impossiblehttps://cplberry.com/wp-content/uploads/2014/10/homer-rdoughnut.jpgHomer loves donutsDoughnut love: probably fine.2015-02-07T17:50:57+00:00monthlyhttps://cplberry.com/2014/08/13/aibohphobia/https://cplberry.com/wp-content/uploads/2014/08/polar.pngPolar treasure mapTreasure map using polar coordinateshttps://cplberry.com/wp-content/uploads/2014/08/cartesian.pngCartesian treasure mapTreasure map using Cartesian coordinates2014-10-25T11:34:26+00:00monthlyhttps://cplberry.com/2014/08/16/what-the-dickens/2014-10-25T11:27:36+00:00monthlyhttps://cplberry.com/2014/08/09/113/2014-10-25T10:35:31+00:00monthlyhttps://cplberry.com/blog/2014-07-12T16:02:28+00:00weekly0.6https://cplberry.comdaily1.02025-12-13T20:56:49+00:00