Here’s a comprehensive list of all work published by members of the DES Collaboration, with arXiv links to all papers.
THE ELECTROMAGNETIC COUNTERPART OF THE BINARY NEUTRON STAR MERGER LIGO/VIRGO GW170817. I. DISCOVERY OF THE OPTICAL COUNTERPART USING THE DARK ENERGY CAMERA
This is the first paper of the series describing results of our followup observations of GW170817 using DECam. We present observations that led to our independent discovery of the optical source and we establish its association with GW170817 by showing that none of the 1500 other sources found within the event localization region could plausibly be associated with the event. We monitored the source for over two weeks and provide the lightcurve data as a machine-readable file in this link. Detailed modeling of the source is performed in a companion paper (Cowperthwaite et al. 2017). A measurement of the Hubble constant, the first utilizing a gravitational wave event as a standard siren measurement of distance, is enabled by this work (LVC, et al. 2017). A study of the event’s host galaxy (Palmese et al. 2017) and of the probability of detecting more of these sources in past and future surveys (Scolnic et al. 2017) also resulted from this program which is featured in an overview paper of all followup programs (LVC, et al. 2017).
THE ELECTROMAGNETIC COUNTERPART OF THE BINARY NEUTRON STAR MERGER LIGO/VIRGO GW170817. II. UV, OPTICAL, AND NEAR-IR LIGHT CURVES AND COMPARISON TO KILONOVA MODELS
This paper presents photometry of the optical/NIR counterpart to GW170817 using data from DECam, the Hubble Space Telescope, and Gemini-South. We model these data finding that they are consistent with the emission expected for an r-process powered kilonova. The inferred ejecta mass is consistent with the suggestion that neutron star mergers are a dominant site of r-process production in the Universe.
This paper announces the first multi-messenger observations of a binary neutron star merger, which was detected in gravitational waves, as a short gamma-ray burst, and as an electromagnetic transient. The optical observations identified the source as in the galaxy NGC 4993, which LIGO/Virgo determined is at a distance of 40 Mpc from the gravitational-wave signal. The multi-band light curves and spectra are consistent with a kilonova explosion produced by the neutron star merger.
This paper presents the first standard siren measurement of the Hubble constant. The gravitational wave measurement of GW170817 provides a direct estimate of the distance to the source, without the use any sort of distance ladder. Instead, the distance is calibrated by the theory of general relativity. The identification of the host galaxy, NGC 4993, allows a completely independent measurement of the redshift of the source. By combining these two quantities, we determine a value for the Hubble constant. This value, while consistent with existing measurements, is a completely novel and independent way to measure this crucially important cosmological quantity.
In this paper, we attempt to answer the question “How many kilonovae (KNe) can be found in past, present and future datasets?” We use the DES-GW light-curve and an estimate of the rate, and detailed simulations of 11 different surveys, to predict KN discovery numbers for each survey. While we find that it is not highly likely more than a couple KNe can be found in past datasets, we predict that tens of KNe can be found in future datasets, and some of these KNe may be even at higher redshift than the sensitivity of future GW experiments.