The Dark Energy Survey: Data Release 1

Abbott, T. M. C.; Abdalla, F. B.; Allam, S.; Amara, Adam; Annis, J.; Asorey, J.; Ávila, S.; Ballester, O.; Banerji, M.; Barkhouse, W. A.; Baruah, L.; Baumer, Michael; Bechtol, K.; Becker, M. R.; Benoit-Lévy, A.; Bernstein, G. M.; Bertin, E.; Blazek, Jonathan; Bocquet, S.; Brooks, D.; Brout, D.; Buckley-Geer, E.; Burke, D. L.; Busti, V. C.; Campisano, Riccardo; Cardiel-Sas, Laia; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Cawthon, R.; Chang, C.; Chen, X.; Conselice, Christopher J.; Costa, G. S. Da; Crocce, M.; Cunha, C. E.; D’Andrea, C. B.; Costa, L. N. da; Das, Ritanjan; Daues, Greg; Davis, Tamara M.; Davis, C.; Vicente, J. De; DePoy, D. L.; DeRose, J.; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Dodelson, Scott; Doel, P.; Drlica-Wagner, A.; Eifler, T. F.; Elliott, Ann; Evrard, A. E.; Farahi, Arya; Neto, A. Fausti; Fernández, E.; Finley, D. A.; Flaugher, B.; Foley, R. J.; Fosalba, P.; Friedel, D. N.; Frieman, J.; García-Bellido, J.; Gaztañaga, E.; Gerdes, D. W.; Giannantonio, T.; Gill, M. S.; Glazebrook, Karl; Goldstein, D.; Gower, Michelle; Gruen, David; Gruendl, R. A.; Gschwend, J.; Gupta, R.; Gutiérrez, G.; Hamilton, S.; Hartley, W. G.; Hinton, S. R.; Hislop, J. M.; Hollowood, D. L.; Honscheid, K.; Hoyle, B.; Huterer, Dragan; Jain, Bhuvnesh; James, D. J.; Jeltema, T.; Johnson, M. W. G.; Johnson, Michael D.; Kacprzak, T.; Kent, S.; Khullar, Gourav; Klein, Matthias; Kovács, András; Koziol, Andrea M.; Krause, E.; Kremin, Anthony; Krön, Richard G.; Kuêhn, K.; Kuhlmann, S. E.; Kuropatkin, N.; Lahav, O.; Lasker, J.; Li, T. S.; Li, R. T.; Liddle, Andrew R.; Lima, M.; Lin, Hsing Wen; López-Reyes, P.; MacCrann, N.; Maia, M. A. G.; Maloney, J. D.; Manera, Marc; March, M.; Marriner, J.; Marshall, J. L.; Martini, Paul; McClintock, Thomas; McKay, T. A.; McMahon, R. G.; Melchior, P.; Menanteau, F.; Miller, Christopher J.; Miquel, R.; Mohr, J. J.; Morganson, E.; Mould, Jeremy; Neilsen, Eric H.; Nichol, R. C.; Nogueira, Francisco Gleiberson dos Santos; Nord, B.; Nugent, P.; Nunes, Ludmila; Ogando, R. L. C.; Old, Lyndsay; Pace, Andrew B.; Palmese, A.; Paz-Chinchón, F.; Peiris, Hiranya V.; Percival, W.; Petravick, D.; Plazas, A. A.; Poh, J.; Pond, C.; Porredon, A.; Pujol, Arnau; Réfrégier, Alexandre; Reil, K.; Ricker, P. M.; Rollins, R. P.; Romer, A. K.; Roodman, A.; Rooney, Philip; Ross, Ashley J.; Rykoff, E. S.; Šako, M.; Sánchez, Marı́a Luisa Fernández; Sánchez, E.; Santiago, B.; Saro, A.; Scarpine, V.; Scolnic, Dan; Serrano, S.; Sevilla-Noarbe, I.; Sheldon, E.; Shipp, Nora; Silveira, Maria Luíza Gesser da; Smith, M.; Smith, Randall; Smith, J. A.; Soares-Santos, M.; Sobreira, F.; Song, J.; Stebbins, Albert; Suchyta, E.; Sullivan, M.; Swanson, M. E. C.; Tarlè, G.; Thaler, J. J.; Thomas, Daniel; Thomas, R. C.; Troxel, M. A.; Tucker, D. L.; Vikram, V.; Vivas, A. Katherina; Walker, A. R.; Wechsler, Risa H.; Weller, J.; Wester, W.; Wolf, R. C.; Wu, Hao-Yi; Yanny, B.; Zenteno, A.; Zhang, Y.; Zuntz, J.; Juneau, Stéphanie; Fitzpatrick, Michael J.; Nikutta, Robert; Nidever, David L.; Olsen, Knut; Scott, A.

doi:10.3847/1538-4365/aae9f0

Cited by 658 publications

(454 citation statements)

References 53 publications

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“…The CO(3-2) and (4-3) line luminosities of the detected hosts were L ′ CO (3-2) = 0.3-6 × 10 9 (K km s −1 pc 2 ) and L ′ CO (4-3) = 1-3 × 10 9 (K km s −1 pc 2 ), respectively. The CO spectra, velocity-integrated CO maps, and continuum maps are shown in Figure 2 along with optical images taken from the Hubble Legacy Archive 2 and the public data of the Dark Energy Survey (DES; Abbott et al 2018;Morganson et al 2018;Flaugher et al 2015). Dust continuum emission is detected in only three hosts (GRB 051006, 051117B, and 110918A), whereas the upper limits for the nondetections were consistent with those expected from their SFRs (see Section 4.4).…”

Section: Observations and Resultsmentioning

confidence: 71%

ALMA CO Observations of the Host Galaxies of Long-duration Gamma-Ray Bursts. I. Molecular Gas Scaling Relations

Hatsukade

Ohta

Hashimoto

et al. 2020

ApJ

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We present the results of CO observations toward 14 host galaxies of long-duration gamma-ray bursts (GRBs) at z = 0.1-2.5 by using the Atacama Large Millimeter/submillimeter Array. We successfully detected CO(3-2) or CO(4-3) emission in eight hosts (z = 0.3-2), which more than doubles the sample size of GRB hosts with CO detection. The derived molecular gas mass is M gas = (0.2-6) × 10 10 M ⊙ assuming metallicity-dependent CO-to-H 2 conversion factors. By using the largest sample of GRB hosts with molecular gas estimates (25 in total, of which 14 are CO-detected) including results from the literature, we compared molecular gas properties with those of other star-forming galaxies (SFGs). The GRB hosts tend to have a higher molecular gas mass fraction (µ gas ) and a shorter gas depletion timescale (t depl ) as compared with other SFGs at similar redshifts especially at z 1. This could be a common property of GRB hosts or an effect introduced by the selection of targets which are typically above the main-sequence line. To eliminate the effect of selection bias, we analyzed µ gas and t depl as a function of the distance from the main-sequence line (δMS). We find that the GRB hosts follow the same scaling relations as other SFGs, where µ gas increases and t depl decreases with increasing δMS. No molecular gas deficit is observed when compared to other SFGs of similar SFR and stellar mass. These findings suggest that the same star-formation mechanism is expected to be happening in GRB hosts as in other SFGs.

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Section: Observations and Resultsmentioning

confidence: 71%

ALMA CO Observations of the Host Galaxies of Long-duration Gamma-Ray Bursts. I. Molecular Gas Scaling Relations

Hatsukade

Ohta

Hashimoto

et al. 2020

ApJ

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“…The sub-arcsecond localization for FRB 180924 allows us to uniquely identify the host by combining public observations from the Dark Energy Survey (20) with deeper images of the field we obtained with the Very Large Telescope (VLT), long-slit spectra with the Gemini South Telescope, and integral-field spectra with the Keck-II telescope and the VLT (see (17) for details of instrumental setups). Fig.…”

Section: The Burst Host Galaxymentioning

confidence: 99%

“…We referenced positions of the host dark energy survey (DES, (20)) galaxy to the optical reference frame using Gaia (21). The Gaia reference frame is known to be well aligned with ICRF3 used for radio astrometry (21).…”

Section: S17 Optical Astrometrymentioning

confidence: 99%

“…Summing up the flux from the FRB host galaxy, and using transformations between the V + I and g + i filters (58) we find i = 20.28 ± 0.05 and g = 21.57 ± 0.04. For comparison, the integrated magnitudes from the DES Catalog (20) are i = 20.14 ± 0.02 and g = 21.62 ± 0.02.…”

Section: S18 Fors2 Optical Imagingmentioning

confidence: 99%

“…The measured being the position given in the catalog, and the corrected is after the Gaia-DES offsets listed in Table S2 have been applied. For the DES positions the 1 sigma radius of the circle is the astrometric precision of 151 mas (20). Figure S2: Comparison of incoherent and interferometric burst localization.…”

Section: S25 Acknowledgmentsmentioning

confidence: 99%

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A single fast radio burst localized to a massive galaxy at cosmological distance

Bannister

Deller

Phillips

et al. 2019

Science

412

353

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Fast Radio Bursts (FRBs) are brief radio emissions from distant astronomical sources. Some are known to repeat, but most are single bursts. Non-repeating FRB observations have had insufficient positional accuracy to localize them to an individual host galaxy. We report the interferometric localization of the single pulse FRB 180924 to a position 4 kpc from the center of a luminous galaxy at redshift 0.3214. The burst has not been observed to repeat. The properties of the burst and its host are markedly different from the only other accurately localized FRB source. The integrated electron column density along the line of sight closely matches models of the intergalactic medium, indicating that some FRBs are clean probes of the baryonic component of the cosmic web.Cosmological observations have shown that baryons comprise 4% of the energy density of the Universe, of which only about 10% is in cold gas and stars (1), with the remainder residing in a diffuse plasma surrounding and in between galaxies and galaxy clusters. The location and density of this material has been challenging to characterize, and up to 50% of it remains unaccounted (2).Fast radio bursts (FRBs; ref.(3)) are bright bursts of radio waves with millisecond duration. They can potentially be used to detect, study, and map this medium, as bursts of emission are dispersed and scattered by their 1 arXiv:1906.11476v1 [astro-ph.HE] 27 Jun 2019 dual-polarization beams on the sky using digital beamforming, producing a total field-of-view of ∼ 30 deg 2 . For burst detection, the beamformers produces channelized autocorrelation spectra for both linear polarizations of all beams, with an integration time of 864 µs and channel bandwidth of 1 MHz in these observations. We used 336 channels centered at 1320 MHz. A real-time detection pipeline incoherently adds the spectra from all available antennas (24 antennas in these observations) and polarization channels, then searches (16) the result for dispersed pulses (17).Burst localization is completed with a second data product that utilizes both the amplitude and phase information of the burst radiation. The beamformers store samples of the complex electric field for all beams and both polarizations in a ring buffer of 3.1 s duration, with the oldest data being continuously overwritten by new data. The data are saved for offline interferometric analysis only when the pipeline identifies a candidate. For the searches reported here the triggering required pulses with widths less than 9 ms and S/N > 10.Previous searches with ASKAP used antennas pointed in different directions to maximize sky coverage (10,16). In contrast, our observations used antennas all pointed in the same direction, enabling the array to act as an interferometer capable of sub-arcsecond localization with a 30 deg 2 field of view. We targeted high Galactic latitude fields (Galactic latitude |b| ∼ 50 • ), that had been observed previously (10, 16), and Southern circumpolar fields. The high-latitude fields were observed regularly through 2017 and earl...

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Cosmology with Gravitational Waves: A Review

et al. 2022

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Standard sirens have been the central paradigm in gravitational‐wave cosmology so far. From the gravitational wave signature of compact star binaries, it is possible to measure the luminosity distance of the source directly, and if additional information on the source redshift is provided, a measurement of the cosmological expansion can be performed. This review article discusses several methodologies that have been proposed to use gravitational waves for cosmological studies. Methods that use only gravitational‐wave signals and methods that use gravitational waves in conjunction with additional observations such as electromagnetic counterparts and galaxy catalogs will be discussed. The review also discusses the most recent results on gravitational‐wave cosmology, starting from the binary neutron star merger GW170817 and its electromagnetic counterpart and finishing with the population of binary black holes, observed with the third Gravitational‐wave Transient Catalog GWTC–3.

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The Dark Energy Survey: Data Release 1

Cited by 658 publications

References 53 publications

ALMA CO Observations of the Host Galaxies of Long-duration Gamma-Ray Bursts. I. Molecular Gas Scaling Relations

ALMA CO Observations of the Host Galaxies of Long-duration Gamma-Ray Bursts. I. Molecular Gas Scaling Relations

A single fast radio burst localized to a massive galaxy at cosmological distance

Cosmology with Gravitational Waves: A Review

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