Gw150914: First Search for the Electromagnetic Counterpart of a Gravitational-Wave Event by the Toros Collaboration

Díaz, M. C.; Beroiz, Martín; Peñuela, T.; Macri, Lucas M.; Oelkers, Ryan J.; Yuan, Wenlong; Lambas, D. García; Cabral, Juan B.; Colazo, C.; Domínguez, M.; Sánchez, Bruno; Gurovich, S.; Lares, M.; Schneiter, M.; Graña, Darío; Renzi, Víctor; Rodríguez, Horacio Adolfo; Starck, M.; Vrech, Rubén; Artola, R.; Ferreyra, Adriana; Girardini, C.; Quiñones, C.; Tapia, L.; Tornatore, M.; Marshall, J. L.; DePoy, D. L.; Branchesi, M.; Brocato, E.; Padilla, Nelson; Pereyra, Nicolas A.; Mukherjee, Soma; Benacquista, M.; Key, J. S.

doi:10.3847/2041-8205/828/2/l16

Cited by 19 publications

(16 citation statements)

References 46 publications

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“…These rates are consistent with the variable star rates determined by previous studies (Wang, L. et al 2013;Díaz et al 2016;Oelkers et al 2016a,b).…”

Section: 1supporting

confidence: 93%

Variability Properties of Four Million Sources in the TESS Input Catalog Observed with the Kilodegree Extremely Little Telescope Survey

Oelkers

Rodriguez

Stassun

et al. 2017

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106

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The Kilodegree Extremely Little Telescope (KELT) has been surveying more than 70% of the celestial sphere for nearly a decade. While the primary science goal of the survey is the discovery of transiting, large-radii planets around bright host stars, the survey has collected more than 10 6 images, with a typical cadence between 10 − 30 minutes, for more than 4 million sources with apparent visual magnitudes in the approximate range 7 < V < 13. Here we provide a catalog of 52,741 objects showing significant large-amplitude fluctuations likely caused by stellar variability and 62,229 objects identified with likely stellar rotation periods. The detected variability ranges in rms-amplitude from 3 mmag to 2.3 mag, and the detected periods range from ∼0.1 days to 2000 days. We provide variability upper limits for all other ∼4 million sources. These upper limits are principally a function of stellar brightness, but we achieve typical 1σ sensitivity on 30-minute timescales down to ∼5 mmag at V ∼ 8, and down to ∼43 mmag at V ∼ 13. We have matched our catalog to the TESS Input catalog and the AAVSO Variable Star Index to precipitate the follow up and classification of each source. The catalog is maintained as a living database on the Filtergraph visualization portal at the URL https://filtergraph.com/kelt_vars.

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“…These rates are consistent with the variable star rates determined by previous studies (Wang, L. et al 2013;Díaz et al 2016;Oelkers et al 2016a,b).…”

Section: 1supporting

confidence: 93%

Variability Properties of Four Million Sources in the TESS Input Catalog Observed with the Kilodegree Extremely Little Telescope Survey

Oelkers

Rodriguez

Stassun

et al. 2017

Self Cite

106

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“…In the case of GW150914, different collaborations developed strategies to search for electromagnetic transients but so far, no counterparts consistent with the LIGO detection have been identified (see Brocato et al 2017;Copperwheat et al 2016;Díaz et al 2016;Ackermann et al 2016, and references therein). The Fermi Collaboration does not detect any transient events associated with GW150914 (Connaughton et al 2018).…”

Section: Discussionmentioning

confidence: 99%

Evolution of dwarf galaxies hosting GW150914-like events

Marassi

Graziani

Ginolfi

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Here we present a detailed analysis of the properties and evolution of different dwarf galaxies, candidate to host the coalescence of black hole binary systems (BHB) generating GW150914-like events. By adopting a novel theoretical framework coupling the binary population synthesis code SeBa with the Galaxy formation model GAMESH, we can investigate the detailed evolution of these objects in a well resolved cosmological volume of 4 cMpc, having a Milky Way-like (MW) galaxy forming at its center. We identify three classes of interesting candidate galaxies: MW progenitors, dwarf satellites and dwarf galaxies evolving in isolation. We find that: (i) despite differences in individual histories and specific environments the candidates reduce to only nine representative galaxies; (ii) among them, ∼ 44% merges into the MW halo progenitors by the redshift of the expected signal, while the remaining dwarfs are found as isolated or as satellites of the MW and their evolution is strongly shaped by both peculiar dynamical history and environmental feedback; (iii) a stringent condition for the environments where GW150914-like binaries can form comes from a combination of the accretion history of their DM halos and the radiative feedback in the high redshift universe; (iv) by comparing with the observed catalogues from DGS and ALLSMOG surveys we find two observed dwarfs respecting the properties predicted by our model. We finally note how the present analysis opens the possibility to build future strategies for host galaxy identification. the LIGO detectors: GW170104 (SNR = 13, Abbott et al. 2017a) and GW170814 (SNR = 18, Abbott et al. 2017b) 1 .The masses inferred for the components of the BHB generating GW150914 are M1 ∼ 36 M⊙ and M2 ∼ 29 M⊙; BHBs associated with GW170104 (and GW170814) are massive as well, with inferred component masses of M1 ∼ 31 M⊙ (∼ 30 M⊙), M2 ∼ 19 M⊙ (∼ 25 M⊙), respectively 2 .These massive BH binary systems are believed 1 Note that during the second run the lightest black hole binary so far observed was also detected (GW170608, Abbott et al. 2017c) with components in the range inferred for low-mass X-ray binaries: M 1 ∼ 12 M ⊙ and M 2 ∼ 7 M ⊙ , respectively. 2 During the referee process of our paper the LIGO-Virgo Collaboration announced the detection of four coalescing massive black

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“…60 s individual exposures were obtained while the "seeing" had a median (FWHM) of 2.8 . 10 images per field were obtained reaching limiting magnitudes of r = 21.7 ± 0.3 mag with 5σ [17]. LIGO localization regions extend over hundred of square degrees (see Fig.…”

Section: Observations By the Toros Collaborationmentioning

confidence: 96%

“…Electromagnetic Follow-up of GW150914 Mario C. Díaz Figure 3: localization probability maps of GW150914 generated by the different LVC algorithms, indicating with red dots the localization of the galaxies observed see [17] mergers where at least one of the objects is a neutron star. TOROS optimized its analysis for the small FoV selecting for observation nearby galaxies with the largest probability of hosting the event.…”

Section: Pos(multif2017)008mentioning

confidence: 99%