Identification and mitigation of narrow spectral artifacts that degrade searches for persistent gravitational waves in the first two observing runs of Advanced LIGO

Covas, P. B.; Effler, A.; Goetz, E.; Meyers, P. M.; Neunzert, A.; Oliver, M.; Pearlstone, B. L.; Roma, V. J.; Schofield, R. M. S.; Adya, V. B.; Astone, P.; Biscoveanu, S.; Callister, T. A.; Christensen, N.; Colla, A.; Coughlin, E.; Coughlin, M. W.; Crowder, S. G.; Dwyer, S. E.; Eggenstein, H.-B.; Hourihane, S.; Kandhasamy, S.; Liu, W.; Lundgren, A. P.; Matas, A.; McCarthy, R.; McIver, J.; Mendell, G.; Ormiston, R. G.; Palomba, C.; Papa, M. A.; Piccinni, O. J.; Rao, K.; Riles, K.; Sammut, L.; Schlassa, S.; Sigg, D.; Strauss, N. A.; Tao, D.; Thorne, K. A.; Thrane, E.; Trembath-Reichert, Stephen; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Adams, C.; Adhikari, R. X.; Ananyeva, A.; Appert, S.; Arai, K.; Aston, S. M.; Austin, C.; Ballmer, S. W.; Barker, D.; Barr, B.; Barsotti, L.; Bartlett, J.; Bartos, I.; Batch, J. C.; Bejger, M.; Bell, A. S.; Betzwieser, J.; Billingsley, G.; Birch, J.; Biscans, S.; Biwer, C.; Blair, C. D.; Blair, R. M.; Bork, R.; Brooks, A. F.; Cao, H.; Ciani, G.; Clara, F.; Clearwater, P.; Cooper, S. J.; Corban, P.; Countryman, S. T.; Cowart, M. J.; Coyne, D. C.; Cumming, A.; Cunningham, L.; Danzmann, K.; Costa, C. F. Da Silva; Daw, E. J.; DeBra, D.; DeRosa, R. T.; DeSalvo, R.; Dooley, K. L.; Doravari, S.; Driggers, J. C.; Edo, T. B.; Etzel, T.; Evans, M.; Evans, T. M.; Factourovich, M.; Fair, H.; Galiana, A. Fernández; Ferreira, E. C.; Fisher, R. P.; Fong, H.; Frey, R.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Gateley, B.; Giaime, J. A.; Giardina, K. D.; Goetz, R.; Goncharov, B.; Gras, S.; Gray, C.; Grote, H.; Gushwa, K. E.; Gustafson, E. K.; Gustafson, R.; Hall, E. D.; Hammond, G.; Hanks, J.; Hanson, J.; Hardwick, T.; Harry, G. M.; Heintze, M. C.; Heptonstall, A. W.; Hough, J.; Inta, R.; Izumi, K.; Jones, R.; Karki, S.; Kasprzack, M.; Kaufer, S.; Kawabe, K.; Kennedy, R.; Kijbunchoo, N.; Kim, W.; King, E. J.; King, Peter; Kissel, J. S.; Korth, W. Z.; Kuehn, G.; Landry, M.; Lantz, B.; Laxen, M.; Liu, J.; Lockerbie, N. A.; Lormand, M.; MacInnis, M.; Macleod, D. M.; Márka, S.; Márka, Z.; Markosyan, A. S.; Maros, E.; Marsh, P.; Martin, Ian; Мартынов, Д. В.; Mason, K.; Massinger, T. J.; Matichard, F.; Mavalvala, N.; McClelland, D. E.; McCormick, S.; McCuller, L.; McIntyre, G.; McRae, T.; Merilh, E. L.; Miller, John M.; Mittleman, R.; Mo, Geoffrey; Mogushi, K.; Moraru, D.; Moreno, G.; Mueller, G.; Mukund, N.; Mullavey, A.; Münch, J.; Nelson, T. J. N.; Nguyen, P.; Nuttall, L. K.; Oberling, J.; Oktavia, O.; Oppermann, P.; Oram, Richard J.; O’Reilly, B.; Ottaway, D. J.; Overmier, H.; Palamos, J. R.; Parker, W.; Pele, A.; Penn, S.; Perez, C. J.; Phelps, M.; Pierro, V.; Pinto, I. M.; Principe, M.; Prokhorov, L.; Puncken, O.; Quetschke, V.; Quintero, E. A.; Radkins, H.; Raffai, P.; Ramirez, K. E.; Reid, S.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Romel, C. L.; Romie, J. H.; Ross, M. P.; Rowan, S.; Ryan, K.; Sadecki, T.; Sanchez, E. J.; Sanchez, L. E.; Sandberg, V.; Savage, R. L.; Sellers, D.; Shaddock, D. A.; Shaffer, T.; Shapiro, B.; Shoemaker, D. H.; Slagmolen, B. J. J.; Smith, B.; Smith, J. R.; Sorazu, B.; Spencer, A. P.; Staley, A.; Strain, K. A.; Sun, L.; Tanner, D. B.; Tasson, J. D.; Taylor, Robert W.; Thomas, M.; Thomas, P.; Toland, K.; Torrie, C. I.; Traylor, G.; Tse, M.; Tuyenbayev, D.; Vajente, G.; Valdes, G.; Veggel, A. A. van; Vecchio, A.; Veitch, P. J.; Venkateswara, K.; Vo, T.; Vorvick, C.; Wade, M.; Walker, M.; Ward, R. L.; Warner, J.; Weaver, B.; Weiss, R.; Weßels, P.; Willke, B.; Wipf, C. C.; Wofford, J. K.; Worden, J.; Yamamoto, H.; Yancey, C. C.; Yu, Hang; Yu, Haocun; Zhang, L.; Zhu, S. J.; Zucker, M. E.; Zweizig, J.

doi:10.1103/physrevd.97.082002

Cited by 138 publications

(161 citation statements)

References 44 publications

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“…To an excellent approximation, the noise in the two LIGO interferometers is statistically independent, with the exception of particular very narrow bands with electronic line disturbances [21], which are excluded from the analysis. The normalized signal strength using cross correlation of all simultaneous DFTs in the observation time can be written as…”

Section: Resultsmentioning

confidence: 99%

Searching for dark photon dark matter in LIGO O1 data

et al. 2019

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A gravitational wave detector can be used to search for dark photon dark matter. We use the publicly available data from LIGO's first observing run, O1, to perform the first such search. We find that, if a dark photon is the gauge boson of U (1)B, LIGO-O1 data has already provided a sensitivity better in a mass band around mA ∼ 4 × 10 −13 eV than achieved by prior experiments. Substantially improved search sensitivity is expected during the coming years of continued data taking by LIGO and other gravitational wave detectors in a growing global network.

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Section: Resultsmentioning

confidence: 99%

Searching for dark photon dark matter in LIGO O1 data

et al. 2019

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“…If necessary, the detector noise can also be studied in much more detail than was required for this pilot search, e.g. using correlations with auxilliary channels to veto instrumental lines [42]. We also used only an ad-hoc veto version of the line-robust statistic from [54], while a semi-coherent transient-aware version [69] or a customized coherent version would offer the potential for more robust suppression of single-detector instrumental artifacts.…”

Section: Discussionmentioning

confidence: 99%

“…Where the frequency matches up with a harmonic of a known comb of disturbances, the corresponding comb spacing is listed. [42] put SFTs as used for the main search. At each sample value of τ , we use the lalapps MakeFakeData v5 program [41] to simulate a set of signals with varying h 0 , uniformly distributed over the whole search range in {f,ḟ , t 0 } and also randomized over the remaining amplitude parameters {cos ι, ψ, φ 0 }.…”

Section: Appendix B: Details On Ul Proceduresmentioning

confidence: 99%

First search for long-duration transient gravitational waves after glitches in the Vela and Crab pulsars

Keitel¹,

Woan

Pitkin

et al. 2019

Phys. Rev. D

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Gravitational waves (GWs) can offer a novel window into the structure and dynamics of neutron stars. Here we present the first search for long-duration quasi-monochromatic GW transients triggered by pulsar glitches. We focus on two glitches observed in radio timing of the Vela pulsar (PSR J0835-4510) on 12 December 2016 and the Crab pulsar (PSR J0534+2200) on 27 March 2017, during the Advanced LIGO second observing run (O2). We assume the GW frequency lies within a narrow band around twice the spin frequency as known from radio observations. Using the fully-coherent transient-enabled F-statistic method, we search for transients of up to four months in length. We find no credible GW candidates for either target, and through simulated signal injections we set 90% upper limits on (constant) GW strain as a function of transient duration. For the larger Vela glitch, we come close to beating an indirect upper limit for when the total energy liberated in the glitch would be emitted as GWs, thus demonstrating that similar post-glitch searches at improved detector sensitivity can soon yield physical constraints on glitch models.

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“…Notable instrumental contaminants affecting the searches described here include spectral combs of narrow lines in both interferometers, many of which were identified after the run had ended and were mitigated for future runs [3,4,15]. For instance an 8-Hz comb in H1 with the even harmonics (16-Hz comb) being especially strong, was ascribed to digitization roundoff error in a high-frequency excitation applied in order to servo- 10 -24 10 -23 upper limit h 0 95% worst-case upper limit upper limit for circularly polarized GWs FIG.…”

Section: Ligo Interferometers and The O1 Observing Runmentioning

confidence: 99%

Loosely coherent search in LIGO O1 data for continuous gravitational waves from Terzan 5 and the Galactic Center

et al. 2019

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We report results of a search for continuous gravitational waves from a region covering the globular cluster Terzan 5 and the galactic center. Continuous gravitational waves are expected from fastspinning, slightly non-axisymmetric isolated neutron stars as well as more exotic objects. The regions that we target are believed to be unusually abundant in neutron stars. We use a new loosely coherent search method that allows to reach unprecedented levels of sensitivity for this type of search. The search covers the frequency band 475-1500 Hz and frequency time derivatives in the range of [−3.0, +0.1] × 10 −8 Hz/s, which is a parameter range not explored before with the depth reached by this search. As to be expected with only a few months of data from the same observing run, it is very difficult to make a confident detection of a continuous signal over such a large parameter space. A list of parameter space points that passed all the thresholds of this search is provided. We follow-up the most significant outlier on the newly released O2 data and cannot confirm it. We provide upper limits on the gravitational wave strength of signals as a function of signal frequency.1 The 7% is derived from the results of Monte Carlo simulations of this search on simulated signals [13].

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Identification and mitigation of narrow spectral artifacts that degrade searches for persistent gravitational waves in the first two observing runs of Advanced LIGO

Cited by 138 publications

References 44 publications

Searching for dark photon dark matter in LIGO O1 data

Searching for dark photon dark matter in LIGO O1 data

First search for long-duration transient gravitational waves after glitches in the Vela and Crab pulsars

Loosely coherent search in LIGO O1 data for continuous gravitational waves from Terzan 5 and the Galactic Center

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