Author: "Matheson, T." - Searchworks@Jio Institute Digital Library Search Results

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1. The Lure of Power and the Triumph of Capital: An Ironic Reading of Major Barbara

Author: Matheson, T. J.
Published: 2019
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2. Anomaly Detection and Approximate Similarity Searches of Transients in Real-time Data Streams

Author: Aleo, P. D., Engel, A. W., Narayan, G., Angus, C. R., Malanchev, K., Auchettl, K., Baldassare, V. F., Berres, A., de Boer, T. J. L., Boyd, B. M., Chambers, K. C., Davis, K. W., Esquivel, N., Farias, D., Foley, R. J., Gagliano, A., Gall, C., Gao, H., Gomez, S., Grayling, M., Jones, D. O., Lin, C. -C., Magnier, E. A., Mandel, K. S., Matheson, T., Raimundo, S. I., Shah, V. G., Soraisam, M. D., de Soto, K. M., Vicencio, S., Villar, V. A., and Wainscoat, R. J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present LAISS (Lightcurve Anomaly Identification and Similarity Search), an automated pipeline to detect anomalous astrophysical transients in real-time data streams. We deploy our anomaly detection model on the nightly ZTF Alert Stream via the ANTARES broker, identifying a manageable $\sim$1-5 candidates per night for expert vetting and coordinating follow-up observations. Our method leverages statistical light-curve and contextual host-galaxy features within a random forest classifier, tagging transients of rare classes (spectroscopic anomalies), of uncommon host-galaxy environments (contextual anomalies), and of peculiar or interaction-powered phenomena (behavioral anomalies). Moreover, we demonstrate the power of a low-latency ($\sim$ms) approximate similarity search method to find transient analogs with similar light-curve evolution and host-galaxy environments. We use analogs for data-driven discovery, characterization, (re-)classification, and imputation in retrospective and real-time searches. To date we have identified $\sim$50 previously known and previously missed rare transients from real-time and retrospective searches, including but not limited to: SLSNe, TDEs, SNe IIn, SNe IIb, SNe Ia-CSM, SNe Ia-91bg-like, SNe Ib, SNe Ic, SNe Ic-BL, and M31 novae. Lastly, we report the discovery of 325 total transients, all observed between 2018-2021 and absent from public catalogs ($\sim$1% of all ZTF Astronomical Transient reports to the Transient Name Server through 2021). These methods enable a systematic approach to finding the "needle in the haystack" in large-volume data streams. Because of its integration with the ANTARES broker, LAISS is built to detect exciting transients in Rubin data., Comment: 44 pages (68 pages with Appendix), 15 figures, accepted to ApJ
Published: 2024

3. Windows on the Universe: Establishing the Infrastructure for a Collaborative Multi-messenger Ecosystem

Author: The 2023 Windows on the Universe Workshop White Paper Working Group, Ahumada, T., Andrews, J. E., Antier, S., Blaufuss, E., Brady, P. R., Brazier, A. M., Burns, E., Cenko, S. B., Chandra, P., Chatterjee, D., Corsi, A., Coughlin, M. W., Coulter, D. A., Fu, S., Goldstein, A., Guy, L. P., Hooper, E. J., Howell, S. B., Humensky, T. B., Kennea, J. A., Jarrett, S. M., Lau, R. M., Lewis, T. R., Lu, L., Matheson, T., Miller, B. W., Narayan, G., Nikutta, R., Rajagopal, J. K., Rest, A., Ruiz-Rocha, K. M., Runnoe, J., Sand, D. J., Santander, M., Solares, H. A. A., Soraisam, M. D., Street, R. A., Tohuvavohu, A., Vieira, J., Vieregg, A., Vigeland, S. J., Vitale, S., White, N. E., Wyatt, S. D., and Yuan, T.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: In this White Paper, we present recommendations for the scientific community and funding agencies to foster the infrastructure for a collaborative multi-messenger and time-domain astronomy (MMA/TDA) ecosystem. MMA/TDA is poised for breakthrough discoveries in the coming decade. In much the same way that expanding beyond the optical bandpass revealed entirely new and unexpected discoveries, cosmic messengers beyond light (i.e., gravitational waves, neutrinos, and cosmic rays) open entirely new windows to answer some of the most fundamental questions in (astro)physics: heavy element synthesis, equation of state of dense matter, particle acceleration, etc. This field was prioritized as a frontier scientific pursuit in the 2020 Decadal Survey on Astronomy and Astrophysics via its "New Windows on the Dynamic Universe" theme. MMA/TDA science presents technical challenges distinct from those experienced in other disciplines. Successful observations require coordination across myriad boundaries -- different cosmic messengers, ground vs. space, international borders, etc. -- all for sources that may not be well localized, and whose brightness may be changing rapidly with time. Add that all of this work is undertaken by real human beings, with distinct backgrounds, experiences, cultures, and expectations, that often conflict. To address these challenges and help MMA/TDA realize its full scientific potential in the coming decade (and beyond), the second in a series of community workshops sponsored by the U.S. National Science Foundation (NSF) and NASA titled "Windows on the Universe: Establishing the Infrastructure for a Collaborative Multi-Messenger Ecosystem" was held on October 16-18, 2023 in Tucson, AZ. Here we present the primary recommendations from this workshop focused on three key topics -- hardware, software, and people and policy. [abridged], Comment: Workshop white paper
Published: 2024

4. Perfecting our set of spectrophotometric standard DA white dwarfs

Author: Calamida, A., Matheson, T., Olszewski, E. W., Saha, A., Axelrod, Tim, Shanahan, C., Holberg, J., Points, S., Narayan, G., Malanchev, K., Ridden-Harper, R., Gentile-Fusillo, N., Raddi, R., Bohlin, R., Rest, A., Hubeny, I., Deustua, S., Mackenty, . J., Sabbi, E., and Stubbs, C. W.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We verified for photometric stability a set of DA white dwarfs with Hubble Space Telescope magnitudes from the near-ultraviolet to the near-infrared and ground-based spectroscopy by using time-spaced observations from the Las Cumbres Observatory network of telescopes. The initial list of 38 stars was whittled to 32 final ones which comprise a high quality set of spectrophotometric standards. These stars are homogeneously distributed around the sky and are all fainter than r ~ 16.5 mag. Their distribution is such that at least two of them would be available to be observed from any observatory on the ground at any time at airmass less than two. Light curves and different variability indices from the Las Cumbres Observatory data were used to determine the stability of the candidate standards. When available, Pan-STARRS1, Zwicky Transient Facility and TESS data were also used to confirm the star classification. Our analysis showed that four DA white dwarfs may exhibit evidence of photometric variability, while a fifth is cooler than our established lower temperature limit, and a sixth star might be a binary. In some instances, due to the presence of faint nearby red sources, care should be used when observing a few of the spectrophotometric standards with ground-based telescopes. Light curves and finding charts for all the stars are provided., Comment: 48 pages, 50 figures, accepted for publication on ApJ
Published: 2022
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5. Optical follow-up of gravitational wave triggers with DECam during the first two LIGO/VIRGO observing runs

Author: Herner, K., Annis, J., Brout, D., Soares-Santos, M., Kessler, R., Sako, M., Butler, R., Doctor, Z., Palmese, A., Allam, S., Tucker, D. L., Sobreira, F., Yanny, B., Diehl, H. T., Frieman, J., Glaeser, N., Garcia, A., Sherman, N. F., Bechtol, K., Berger, E., Chen, H. Y., Conselice, C. J., Cook, E., Cowperthwaite, P. S., Davis, T. M., Drlica-Wagner, A., Farr, B., Finley, D., Foley, R. J., Garcia-Bellido, J., Gill, M. S. S., Gruendl, R. A., Holz, D. E., Kuropatkin, N., Lin, H., Marriner, J., Marshall, J. L., Matheson, T., Neilsen, E., Paz-Chinchón, F., Sauseda, M., Scolnic, D., Williams, P. K. G., Avila, S., Bertin, E., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Carrasco-Kind, M., Carretero, J., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Eifler, T. F., Everett, S., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Krause, E., Kuehn, K., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Wester, W., and Zhang, Y.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Gravitational wave (GW) events detectable by LIGO and Virgo have several possible progenitors, including black hole mergers, neutron star mergers, black hole--neutron star mergers, supernovae, and cosmic string cusps. A subset of GW events are expected to produce electromagnetic (EM) emission that, once detected, will provide complementary information about their astrophysical context. To that end, the LIGO--Virgo Collaboration (LVC) sends GW candidate alerts to the astronomical community so that searches for their EM counterparts can be pursued. The DESGW group, consisting of members of the Dark Energy Survey (DES), the LVC, and other members of the astronomical community, uses the Dark Energy Camera (DECam) to perform a search and discovery program for optical signatures of LVC GW events. DESGW aims to use a sample of GW events as standard sirens for cosmology. Due to the short decay timescale of the expected EM counterparts and the need to quickly eliminate survey areas with no counterpart candidates, it is critical to complete the initial analysis of each night's images as quickly as possible. We discuss our search area determination, imaging pipeline, and candidate selection processes. We review results from the DESGW program during the first two LIGO--Virgo observing campaigns and introduce other science applications that our pipeline enables., Comment: 15 pages, 7 figures, accepted in Astronomy and Computing, matches accepted version
Published: 2020
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6. The Palomar Transient Factory Core-collapse Supernova Host-galaxy Sample. I. Host-galaxy Distribution Functions and Environment Dependence of Core-collapse Supernovae

Author: Schulze, S, Yaron, O, Sollerman, J, Leloudas, G, Gal, A, Wright, AH, Lunnan, R, Gal-Yam, A, Ofek, EO, Perley, DA, Filippenko, AV, Kasliwal, MM, Kulkarni, SR, Neill, JD, Nugent, PE, Quimby, RM, Sullivan, M, Strotjohann, NL, Arcavi, I, Ben-Ami, S, Bianco, F, Bloom, JS, De, K, Fraser, M, Fremling, CU, Horesh, A, Johansson, J, Kelly, PL, Knežević, N, Knežević, S, Maguire, K, Nyholm, A, Papadogiannakis, S, Petrushevska, T, Rubin, A, Yan, L, Yang, Y, Adams, SM, Bufano, F, Clubb, KI, Foley, RJ, Green, Y, Harmanen, J, Ho, AYQ, Hook, IM, Hosseinzadeh, G, Howell, DA, Kong, AKH, Kotak, R, Matheson, T, McCully, C, Milisavljevic, D, Pan, YC, Poznanski, D, Shivvers, I, Van Velzen, S, and Verbeek, KK
Subjects: Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: Several thousand core-collapse supernovae (CCSNe) of different flavors have been discovered so far. However, identifying their progenitors has remained an outstanding open question in astrophysics. Studies of SN host galaxies have proven to be powerful in providing constraints on the progenitor populations. In this paper, we present all CCSNe detected between 2009 and 2017 by the Palomar Transient Factory. This sample includes 888 SNe of 12 distinct classes out to redshift z ≈ 1. We present the photometric properties of their host galaxies from the far-ultraviolet to the mid-infrared and model the host-galaxy spectral energy distributions to derive physical properties. The galaxy mass function of Type Ic, Ib, IIb, II, and IIn SNe ranges from 105 to 1011.5 M o˙, probing the entire mass range of star-forming galaxies down to the least-massive star-forming galaxies known. Moreover, the galaxy mass distributions are consistent with models of star-formation-weighted mass functions. Regular CCSNe are hence direct tracers of star formation. Small but notable differences exist between some of the SN classes. Type Ib/c SNe prefer galaxies with slightly higher masses (i.e., higher metallicities) and star formation rates than Type IIb and II SNe. These differences are less pronounced than previously thought. H-poor superluminous supernovae (SLSNe) and SNe Ic-BL are scarce in galaxies above 1010 M o˙. Their progenitors require environments with metallicities of < 0.4 and < 1 solar, respectively. In addition, the hosts of H-poor SLSNe are dominated by a younger stellar population than all other classes of CCSNe. Our findings corroborate the notion that low metallicity and young age play an important role in the formation of SLSN progenitors.
Published: 2021

7. Nebular H$\alpha$ Limits for Fast Declining Type Ia Supernovae

Author: Sand, D. J., Amaro, R. C., Moe, M., Graham, M. L., Andrews, J. E., Burke, J., Cartier, R., Eweis, Y., Galbany, L., Hiramatsu, D., Howell, D. A., Jha, S. W., Lundquist, M., Matheson, T., McCully, C., Milne, P., Smith, Nathan, Valenti, S., and Wyatt, S.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: One clear observational prediction of the single degenerate progenitor scenario as the origin of type Ia supernovae (SNe) is the presence of relatively narrow ($\approx$1000 km s$^{-1}$) H$\alpha$ emission at nebular phases, although this feature is rarely seen. We present a compilation of nebular phase H$\alpha$ limits for SN Ia in the literature and demonstrate that this heterogenous sample has been biased towards SN Ia with relatively high luminosities and slow decline rates, as parameterized by $\Delta$m$_{15}(B)$, the difference in $B$-band magnitude between maximum light and fifteen days afterward. Motivated by the need to explore the full parameter space of SN~Ia and their subtypes, we present two new and six previously published nebular spectra of SN Ia with $\Delta$m$_{15}(B)$$ > $1.3 mag (including members of the transitional and SN1991bg-like subclasses) and measure nondetection limits of $L_{H\alpha}$$~<~$0.85--9.9$\times$10$^{36}$ ergs s$^{-1}$, which we confirmed by implanting simulated H$\alpha$ emission into our data. Based on the lastest models of swept-up material stripped from a nondegenerate companion star, these $L_{H\alpha}$ values correspond to hydrogen mass limits of $M_H$$~\lesssim~$1-3$\times$10$^{-4}$ $M_{\odot}$, roughly three orders of magnitude below that expected for the systems modeled, although we note that no simulations of H$\alpha$ nebular emission in such weak explosions have yet been performed. Despite the recent detection of strong H$\alpha$ in ASASSN-18tb (SN 2018fhw; $\Delta$m$_{15}(B)$ = 2.0 mag), we see no evidence that fast declining systems are more likely to have late time H$\alpha$ emission, although a larger sample is needed to confirm this result., Comment: 11 pages, 3 figures, two tables. ApJ Letters accepted
Published: 2019
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8. PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses

Author: Pian, E, Mazzali, PA, Moriya, TJ, Rubin, A, Gal-Yam, A, Arcavi, I, Ben-Ami, S, Blagorodnova, N, Bufano, F, Filippenko, AV, Kasliwal, M, Kulkarni, SR, Lunnan, R, Manulis, I, Matheson, T, Nugent, PE, Ofek, E, Perley, DA, Prentice, SJ, and Yaron, O
Subjects: radiative transfer, stars: massive, galaxies: star formation, transients: supernovae, astro-ph.HE, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: The hydrogen-poor supernova (SN) PTF11rka (z = 0.0744), reported by the Palomar Transient Factory, was observed with various telescopes starting a few days after the estimated explosion time of 2011 December 5 UT and up to 432 rest-frame days thereafter. The rising part of the light curve was monitored only in the RPTF filter band, and maximum in this band was reached ∼30 rest-frame days after the estimated explosion time. The light curve and spectra of PTF11rka are consistent with the core-collapse explosion of a ∼10 M⊙ carbon-oxygen core evolved from a progenitor of main-sequence mass 25-40 M⊙, that liberated a kinetic energy Ek≈4 × 1051 erg, expelled ∼8 M⊙ of ejecta, and synthesized ∼0.5 M⊙ of 56Ni. The photospheric spectra of PTF11rka are characterized by narrow absorption lines that point to suppression of the highest ejecta velocities (∼ 15 000 km s-1). This would be expected if the ejecta impacted a dense, clumpy circumstellar medium. This in turn caused them to lose a fraction of their energy (∼5 × 1050 erg), less than 2 per cent of which was converted into radiation that sustained the light curve before maximum brightness. This is reminiscent of the superluminous SN 2007bi, the light-curve shape and spectra of which are very similar to those of PTF11rka, although the latter is a factor of 10 less luminous and evolves faster in time. PTF11rka is in fact more similar to gamma-ray burst SNe in luminosity, although it has a lower energy and a lower Ek/Mej ratio.
Published: 2020

9. A Search for Optical Emission from Binary-Black-Hole Merger GW170814 with the Dark Energy Camera

Author: Doctor, Z., Kessler, R., Herner, K., Palmese, A., Soares-Santos, M., Annis, J., Brout, D., Holz, D. E., Sako, M., Rest, A., Cowperthwaite, P., Berger, E., Foley, R. J., Conselice, C. J., Gill, M. S. S., Allam, S., Balbinot, E., Butler, R. E., Chen, H. -Y., Chornock, R., Cook, E., Diehl, H. T., Farr, B., Fong, W., Frieman, J., Fryer, C., García-Bellido, J., Margutti, R., Marshall, J. L., Matheson, T., Metzger, B. D., Nicholl, M., Paz-Chinchón, F., Salim, S., Sauseda, M., Secco, L. F., Smith, N., Smith, R. C., Vivas, A. K., Tucker, D. L., Abbott, T. M. C., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., D'Andrea, C. B., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kent, S., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Menanteau, F., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R. L. C., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Walker, A. R., and Wester, W.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Binary black hole (BBH) mergers found by the LIGO and Virgo detectors are of immense scientific interest to the astrophysics community, but are considered unlikely to be sources of electromagnetic emission. To test whether they have rapidly fading optical counterparts, we used the Dark Energy Camera to perform an $i$-band search for the BBH merger GW170814, the first gravitational wave detected by three interferometers. The 87-deg$^2$ localization region (at 90\% confidence) centered in the Dark Energy Survey (DES) footprint enabled us to image 86\% of the probable sky area to a depth of $i\sim 23$ mag and provide the most comprehensive dataset to search for EM emission from BBH mergers. To identify candidates, we perform difference imaging with our search images and with templates from pre-existing DES images. The analysis strategy and selection requirements were designed to remove supernovae and to identify transients that decline in the first two epochs. We find two candidates, each of which is spatially coincident with a star or a high-redshift galaxy in the DES catalogs, and they are thus unlikely to be associated with GW170814. Our search finds no candidates associated with GW170814, disfavoring rapidly declining optical emission from BBH mergers brighter than $i\sim 23$ mag ($L_{\rm optical} \sim 5\times10^{41}$ erg/s) 1-2 days after coalescence. In terms of GW sky map coverage, this is the most complete search for optical counterparts to BBH mergers to date, Comment: 11 pages, 3 figures
Published: 2018
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10. Photometry and spectroscopy of faint candidate spectrophotometric standard DA white dwarfs

Author: Calamida, A., Matheson, T., Saha, A., Olszewski, E., Narayan, G., Claver, J., Shanahan, C., Holberg, J., Axelrod, T., Bohlin, R., Stubbs, C. W., Deustua, S., Hubeny, I., Mackenty, J., Points, S., Rest, A., and Sabbi, E.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present precise photometry and spectroscopy for 23 candidate spectrophotometric standard white dwarfs. The selected stars are distributed in the Northern hemisphere and around the celestial equators and are all fainter than r ~ 16.5 mag. This network of stars, when established as standards, together with the three Hubble Space Telescope primary CALSPEC white dwarfs, will provide a set of spectrophotometric standards to directly calibrate data products to better than 1%. These new faint standard white dwarfs will have enough signal-to-noise ratio in future deep photometric surveys and facilities to be measured accurately while still avoiding saturation in such surveys. They will also fall within the dynamic range of large telescopes and their instruments for the foreseeable future. This paper discusses the provenance of the observational data for our candidate standard stars. The comparison with models, reconciliation with reddening, and the consequent derivation of the full spectral energy density distributions for each of them is reserved for a subsequent paper., Comment: 31 pages, 17 figures, 10 tables, ApJ in press (accepted on December 23rd, 2018)
Published: 2018
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11. Oxygen and helium in stripped-envelope supernovae

Author: Fremling, C., Sollerman, J., Kasliwal, M. M., Kulkarni, S. R., Barbarino, C., Ergon, M., Karamehmetoglu, E., Taddia, F., Arcavi, I., Cenko, S. B., Clubb, K., De Cia, A., Duggan, G., Filippenko, A. V., Gal-Yam, A., Graham, M. L., Horesh, A., Hosseinzadeh, G., Howell, D. A., Kuesters, D., Lunnan, R., Matheson, T., Nugent, P. E., Perley, D. A., Quimby, R. M., and Saunders, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present an analysis of 507 spectra of 173 stripped-envelope (SE) supernovae (SNe) discovered by the untargeted Palomar Transient Factory (PTF) and intermediate PTF (iPTF) surveys. Our sample contains 55 Type IIb SNe (SNe IIb), 45 Type Ib SNe (SNe Ib), 56 Type Ic SNe (SNe Ic), and 17 Type Ib/c SNe (SNe Ib/c). We compare the SE SN subtypes via measurements of the pseudo-equivalent widths (pEWs) and velocities of the He I $\lambda\lambda5876, 7065$ and O I $\lambda7774$ absorption lines. Consistent with previous work, we find that SNe Ic show higher pEWs and velocities in O I $\lambda7774$ compared to SNe IIb and Ib. The pEWs of the He I $\lambda\lambda5876, 7065$ lines are similar in SNe Ib and IIb after maximum light. The He I $\lambda\lambda5876, 7065$ velocities at maximum light are higher in SNe Ib compared to SNe IIb. We have identified an anticorrelation between the He I $\lambda7065$ pEW and O I $\lambda7774$ velocity among SNe IIb and Ib. This can be interpreted as a continuum in the amount of He present at the time of explosion. It has been suggested that SNe Ib and Ic have similar amounts of He, and that lower mixing could be responsible for hiding He in SNe Ic. However, our data contradict this mixing hypothesis. The observed difference in the expansion rate of the ejecta around maximum light of SNe Ic ($V_{\mathrm{m}}=\sqrt{2E_{\mathrm{k}}/M_{\mathrm{ej}}}\approx15,000$ km s$^{-1}$) and SNe Ib ($V_{\mathrm{m}}\approx9000$ km s$^{-1}$) would imply an average He mass difference of $\sim1.4$ $M_{\odot}$, if the other explosion parameters are assumed to be unchanged between the SE SN subtypes. We conclude that SNe Ic do not hide He but lose He due to envelope stripping., Comment: 18 pages, 6 figures, accepted for publication in Astronomy and Astrophysics
Published: 2018
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12. A gravitational-wave standard siren measurement of the Hubble constant

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Chia, H., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, A. K. W., Chung, S., Ciani, G., Ciolfi, R., Cirelli, C. E., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Cohen, D., Colla, A., Collette, C. G., Cominsky, L. R., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dálya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Day, B., De, S., DeBra, D., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., Demos, N., Denker, T., Dent, T., De Pietri, R., Dergachev, V., De Rosa, R., DeRosa, R. T., De Rossi, C., DeSalvo, R., de Varona, O., Devenson, J., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., Doctor, Z., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Douglas, R., Álvarez, M. Dovale, Downes, T. P., Drago, M., Dreissigacker, C., Driggers, J. C., Du, Z., Ducrot, M., Dupej, P., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenstein, R. A., Essick, R. C., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M. M., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finstad, D., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J. A., Forsyth, P. W. F., Forsyth, S. S., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E. M., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glover, L., Goetz, E., Goetz, R., Gomes, S., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Gretarsson, E. M., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Haster, C. -J., Haughian, K., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Houston, E. A., Howell, E. J., Hreibi, A., Hu, Y. M., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Indik, N., Inta, R., Intini, G., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kasprzack, M., Katolik, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Kéfélian, F., Keitel, D., Kemball, A. J., Kennedy, R., Kent, C., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimbrell, S. J., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Krämer, C., Kringel, V., Krishnan, B., Królak, A., Kuehn, G., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Landry, M., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, K., Lehmann, J., Lenon, A., Leonardi, M., Leroy, N., Letendre, N., Levin, Y., Li, T. G. F., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Lo, R. K. L., Lockerbie, N. A., London, L. T., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lück, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Machenschalk, B., MacInnis, M., Macleod, D. M., Hernandez, I. Magaña, Magaña-Sandoval, F., Zertuche, L. Magaña, Magee, R. M., Majorana, E., Maksimovic, I., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McNeill, L., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Mejuto-Villa, E., Melatos, A., Mendell, G., Mercer, R. A., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, B. B., Miller, J., Millhouse, M., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Ming, J., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moffa, D., Moggi, A., Mogushi, K., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mours, B., Mow-Lowry, C. M., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Napier, K., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Nevin, L., Newport, J. M., Newton, G., Ng, K. K. Y., Nguyen, T. T., Nichols, D., Nielsen, A. B., Nissanke, S., Nitz, A., Noack, A., Nocera, F., Nolting, D., North, C., Nuttall, L. K., Oberling, J., O'Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O'Reilly, B., Ormiston, R., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Page, J., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Howard, Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perez, C. J., Perreca, A., Perri, L. M., Pfeiffer, H. P., Phelps, M., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pirello, M., Pitkin, M., Poe, M., Poggiani, R., Popolizio, P., Porter, E. K., Post, A., Powell, J., Prasad, J., Pratt, J. W. W., Pratten, G., Predoi, V., Prestegard, T., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Reyes, S. D., Ricci, F., Ricker, P. M., Rieger, S., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, J. D., Romano, R., Romel, C. L., Romie, J. H., Rosińska, D., Ross, M. P., Rowan, S., Rüdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sampson, L. M., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Scheel, M., Scheuer, J., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shaffer, T. J., Shah, A. A., Shahriar, M. S., Shaner, M. B., Shao, L., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, A., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, B., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sonnenberg, J. A., Sorazu, B., Sorrentino, F., Souradeep, T., Spencer, A. P., Srivastava, A. K., Staats, K., Staley, A., Steer, D., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sunil, S., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., Tápai, M., Taracchini, A., Tasson, J. D., Taylor, J. A., Taylor, R., Tewari, S. V., Theeg, T., Thies, F., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forné, A., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trinastic, J., Tringali, M. C., Trozzo, L., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., van der Schaaf, L., van Heijningen, J. V., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Viceré, A., Viets, A. D., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wessel, E. K., Weßels, P., Westerweck, J., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., Whiting, B. F., Whittle, C., Wilken, D., Williams, D., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J., Wong, K. W. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, S., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yu, Hang, Yu, Haocun, Yvert, M., Zadrożny, A., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, L., Zhang, M., Zhang, T., Zhang, Y. -H., Zhao, C., Zhou, M., Zhou, Z., Zhu, S. J., Zhu, X. J., Zimmerman, A. B., Zucker, M. E., Zweizig, J., Foley, R. J., Coulter, D. A., Drout, M. R., Kasen, D., Kilpatrick, C. D., Madore, B. F., Murguia-Berthier, A., Pan, Y. -C., Piro, A. L., Prochaska, J. X., Ramirez-Ruiz, E., Rest, A., Rojas-Bravo, C., Shappee, B. J., Siebert, M. R., Simon, J. D., Ulloa, N., Annis, J., Soares-Santos, M., Brout, D., Scolnic, D., Diehl, H. T., Frieman, J., Berger, E., Alexander, K. D., Allam, S., Balbinot, E., Blanchard, P., Butler, R. E., Chornock, R., Cook, E. R., Cowperthwaite, P., Drlica-Wagner, A., Durret, F., Eftekhari, T., Finley, D. A., Fong, W., Fryer, C. L., García-Bellido, J., Gill, M. S . S., Gruendl, R. A., Hartley, W., Herner, K., Huterer, D., Kessler, R., Li, T. S., Lin, H., Lopes, P. A. A., Lourenço, A. C. C., Margutti, R., Marriner, J., Marshall, J. L., Matheson, T., Medina, G. E., Metzger, B. D., Muñoz, R. R., Muir, J., Nicholl, M., Nugent, P., Palmese, A., Paz-Chinchón, F., Quataert, E., Sako, M., Sauseda, M., Schlegel, D. J., Secco, L. F., Smith, N., Sobreira, F., Stebbins, A., Villar, V. A., Vivas, A. K., Wester, W., Williams, P. K. G., Yanny, B., Zenteno, A., Abbott, T. M. C., Abdalla, F. B., Bechtol, K., Benoit-Lévy, A., Bertin, E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Dietrich, J. P., Estrada, J., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gutierrez, G., Hartley, W. G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Suchyta, E., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Tucker, D. L., Vikram, V., Walker, A. R., Weller, J., Zhang, Y., Haislip, J. B., Kouprianov, V. V., Reichart, D. E., Tartaglia, L., Sand, D. J., Valenti, S., Yang, S., Arcavi, Iair, Hosseinzadeh, Griffin, Howell, D. Andrew, McCully, Curtis, Poznanski, Dovi, Vasylyev, Sergiy, Tanvir, N. R., Levan, A. J., Hjorth, J., Cano, Z., Copperwheat, C., de Ugarte-Postigo, A., Evans, P. A., Fynbo, J. P. U., González-Fernández, C., Greiner, J., Irwin, M., Lyman, J., Mandel, I., McMahon, R., Milvang-Jensen, B., O'Brien, P., Osborne, J. P., Perley, D. A., Pian, E., Palazzi, E., Rol, E., Rosetti, S., Rosswog, S., Rowlinson, A., Schulze, S., Steeghs, D. T. H., Thöne, C. C., Ulaczyk, K., Watson, D., Wiersema, K., Lipunov, V. M., Gorbovskoy, E., Kornilov, V. G., Tyurina, N ., Balanutsa, P., Vlasenko, D., Gorbunov, I., Podesta, R., Levato, H., Saffe, C., Buckley, D. A. H., Budnev, N. M., Gress, O., Yurkov, V., Rebolo, R., and Serra-Ricart, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The detection of GW170817 in both gravitational waves and electromagnetic waves heralds the age of gravitational-wave multi-messenger astronomy. On 17 August 2017 the Advanced LIGO and Virgo detectors observed GW170817, a strong signal from the merger of a binary neutron-star system. Less than 2 seconds after the merger, a gamma-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO-Virgo-derived location of the gravitational-wave source. This sky region was subsequently observed by optical astronomy facilities, resulting in the identification of an optical transient signal within $\sim 10$ arcsec of the galaxy NGC 4993. These multi-messenger observations allow us to use GW170817 as a standard siren, the gravitational-wave analog of an astronomical standard candle, to measure the Hubble constant. This quantity, which represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Our measurement combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using electromagnetic data. This approach does not require any form of cosmic "distance ladder;" the gravitational wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be $70.0^{+12.0}_{-8.0} \, \mathrm{km} \, \mathrm{s}^{-1} \, \mathrm{Mpc}^{-1}$ (maximum a posteriori and 68% credible interval). This is consistent with existing measurements, while being completely independent of them. Additional standard-siren measurements from future gravitational-wave sources will provide precision constraints of this important cosmological parameter., Comment: 26 pages, 5 figures, Nature in press. For more information see https://dcc.ligo.org/LIGO-P1700296/public
Published: 2017
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13. 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

Author: Cowperthwaite, P. S., Berger, E., Villar, V. A., Metzger, B. D., Nicholl, M., Chornock, R., Blanchard, P. K., Fong, W., Margutti, R., Soares-Santos, M., Alexander, K. D., Allam, S., Annis, J., Brout, D., Brown, D. A., Butler, R. E., Chen, H. -Y., Diehl, H. T., Doctor, Z., Drout, M. R., Eftekhari, T., Farr, B., Finley, D. A., Foley, R. J., Frieman, J. A., Fryer, C. L., García-Bellido, J., Gill, M. S. S., Guillochon, J., Herner, K., Holz, D. E., Kasen, D., Kessler, R., Marriner, J., Matheson, T., Neilsen, Jr., E. H., Quataert, E., Palmese, A., Rest, A., Sako, M., Scolnic, D. M., Smith, N., Tucker, D. L., Williams, P. K. G., Balbinot, E., Carlin, J. L., Cook, E. R., Durret, F., Li, T. S., Lopes, P. A. A., Lourenço, A. C. C., Marshall, J. L., Medina, G. E., Muir, J., Muñoz, R. R., Sauseda, M., Schlegel, D. J., Secco, L. F., Vivas, A. K., Wester, W., Zenteno, A., Zhang, Y., Abbott, T. M. C., Banerji, M., Bechtol, K., Benoit-Lévy, A., Bertin, E., Buckley-Geer, E., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Dietrich, J. P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., March, M., Martini, P., McMahon, R. G., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Ogando, R. L. C., Plazas, A. A., Roe, N., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Yanny, B., and Zuntz, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present UV, optical, and NIR photometry of the first electromagnetic counterpart to a gravitational wave source from Advanced LIGO/Virgo, the binary neutron star merger GW170817. Our data set extends from the discovery of the optical counterpart at $0.47$ days to $18.5$ days post-merger, and includes observations with the Dark Energy Camera (DECam), Gemini-South/FLAMINGOS-2 (GS/F2), and the {\it Hubble Space Telescope} ({\it HST}). The spectral energy distribution (SED) inferred from this photometry at $0.6$ days is well described by a blackbody model with $T\approx 8300$ K, a radius of $R\approx 4.5\times 10^{14}$ cm (corresponding to an expansion velocity of $v\approx 0.3c$), and a bolometric luminosity of $L_{\rm bol}\approx 5\times10^{41}$ erg s$^{-1}$. At $1.5$ days we find a multi-component SED across the optical and NIR, and subsequently we observe rapid fading in the UV and blue optical bands and significant reddening of the optical/NIR colors. Modeling the entire data set we find that models with heating from radioactive decay of $^{56}$Ni, or those with only a single component of opacity from $r$-process elements, fail to capture the rapid optical decline and red optical/NIR colors. Instead, models with two components consistent with lanthanide-poor and lanthanide-rich ejecta provide a good fit to the data, the resulting "blue" component has $M_\mathrm{ej}^\mathrm{blue}\approx 0.01$ M$_\odot$ and $v_\mathrm{ej}^\mathrm{blue}\approx 0.3$c, and the "red" component has $M_\mathrm{ej}^\mathrm{red}\approx 0.04$ M$_\odot$ and $v_\mathrm{ej}^\mathrm{red}\approx 0.1$c. These ejecta masses are broadly consistent with the estimated $r$-process production rate required to explain the Milky Way $r$-process abundances, providing the first evidence that BNS mergers can be a dominant site of $r$-process enrichment., Comment: 13 Pages, 3 Figures, 2 Tables. ApJL, In Press. Keywords: GW170817, LVC
Published: 2017
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14. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. I. Dark Energy Camera Discovery of the Optical Counterpart

Author: Soares-Santos, M., Holz, D. E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H., Kessler, R., Sako, M., Allam, S., Tucker, D. L., Butler, R. E., Palmese, A., Doctor, Z., Diehl, H. T., Frieman, J., Yanny, B., Lin, H., Scolnic, D., Cowperthwaite, P., Neilsen, E., Marriner, J., Kuropatkin, N., Hartley, W. G., Paz-Chinchón, F., Alexander, K. D., Balbinot, E., Blanchard, P., Brown, D. A., Carlin, J. L., Conselice, C., Cook, E. R., Drlica-Wagner, A., Drout, M. R., Durret, F., Eftekhari, T., Farr, B., Finley, D. A., Foley, R. J., Fong, W., Fryer, C. L., García-Bellido, J., Gill, M. S . S., Gruendl, R. A., Hanna, C., Kasen, D., Li, T. S., Lopes, P. A. A., Lourenço, A. C. C., Margutti, R., Marshall, J. L., Matheson, T., Medina, G. E., Metzger, B. D., Muñoz, R. R., Muir, J., Nicholl, M., Quataert, E., Rest, A., Sauseda, M., Schlegel, D. J., Secco, L. F., Sobreira, F., Stebbins, A., Villar, V. A., Walker, A. R., Wester, W., Williams, P. K. G., Zenteno, A., Zhang, Y., Abbott, T. M. C., Abdalla, F. B., Banerji, M., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Lahav, O., Lima, M., Maia, M. A. G., March, M., McMahon, R. G., Menanteau, F., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R. L. C., Petravick, D., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Vikram, V., Wechsler, R. H., and Weller, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the Dark Energy Camera (DECam) discovery of the optical counterpart of the first binary neutron star merger detected through gravitational wave emission, GW170817. Our observations commenced 10.5 hours post-merger, as soon as the localization region became accessible from Chile. We imaged 70 deg$^2$ in the $i$ and $z$ bands, covering 93\% of the initial integrated localization probability, to a depth necessary to identify likely optical counterparts (e.g., a kilonova). At 11.4 hours post-merger we detected a bright optical transient located $10.6''$ from the nucleus of NGC\,4993 at redshift $z=0.0098$, consistent (for $H_0 = 70$\, km s$^{-1}$ Mpc$^{-1}$) with the distance of $40 \pm 8$\, Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes $i\approx 17.30$ and $z\approx 17.45$, and thus an absolute magnitude of $M_i = -15.7$, in the luminosity range expected for a kilonova. We identified 1,500 potential transient candidates. Applying simple selection criteria aimed at rejecting background events such as supernovae, we find the transient associated with NGC\,4993 as the only remaining plausible counterpart, and reject chance coincidence at the 99.5\% confidence level. We therefore conclude that the optical counterpart we have identified near NGC\,4993 is associated with GW170817. This discovery ushers in the era of multi-messenger astronomy with gravitational waves, and demonstrates the power of DECam to identify the optical counterparts of gravitational-wave sources., Comment: 9 Pages, 3 Figures, 2 Tables. ApJL, In Press. Keywords: GW170817, LVC
Published: 2017
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15. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/VIRGO GW170817. IV. Detection of Near-infrared Signatures of r-process Nucleosynthesis with Gemini-South

Author: Chornock, R., Berger, E., Kasen, D., Cowperthwaite, P. S., Nicholl, M., Villar, V. A., Alexander, K. D., Blanchard, P. K., Eftekhari, T., Fong, W., Margutti, R., Williams, P. K. G., Annis, J., Brout, D., Brown, D. A., Chen, H. -Y., Drout, M. R., Foley, R. J., Frieman, J. A., Fryer, C. L., Holz, D. E., Matheson, T., Metzger, B. D., Quataert, E., Rest, A., Sako, M., Scolnic, D. M., Smith, N., and Soares-Santos, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present a near-infrared spectral sequence of the electromagnetic counterpart to the binary neutron star merger GW170817 detected by Advanced LIGO/Virgo. Our dataset comprises seven epochs of J+H spectra taken with FLAMINGOS-2 on Gemini-South between 1.5 and 10.5 days after the merger. In the initial epoch, the spectrum is dominated by a smooth blue continuum due to a high-velocity, lanthanide-poor blue kilonova component. Starting the following night, all subsequent spectra instead show features that are similar to those predicted in model spectra of material with a high concentration of lanthanides, including spectral peaks near 1.07 and 1.55 microns. Our fiducial model with 0.04 M_sun of ejecta, an ejection velocity of v=0.1c, and a lanthanide concentration of X_lan=1e-2 provides a good match to the spectra taken in the first five days, although it over-predicts the late-time fluxes. We also explore models with multiple fitting components, in each case finding that a significant abundance of lanthanide elements is necessary to match the broad spectral peaks that we observe starting at 2.5 d after the merger. These data provide direct evidence that binary neutron star mergers are significant production sites of even the heaviest r-process elements., Comment: 9 pages, 4 figures, 1 table, ApJL, in press
Published: 2017
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16. Oxygen and helium in stripped-envelope supernovae

Author: Fremling, C, Sollerman, J, Kasliwal, MM, Kulkarni, SR, Barbarino, C, Ergon, M, Karamehmetoglu, E, Taddia, F, Arcavi, I, Cenko, SB, Clubb, K, De, A, Duggan, G, Filippenko, AV, Gal-Yam, A, Graham, ML, Horesh, A, Hosseinzadeh, G, Howell, DA, Kuesters, D, Lunnan, R, Matheson, T, Nugent, PE, Perley, DA, Quimby, RM, and Saunders, C
Subjects: Astronomical Sciences, Physical Sciences, supernovae: general, stars: abundances, stars: mass-loss, techniques: spectroscopic, astro-ph.HE, astro-ph.SR, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We present an analysis of 507 spectra of 173 stripped-envelope (SE) supernovae (SNe) discovered by the untargeted Palomar Transient Factory (PTF) and intermediate PTF (iPTF) surveys. Our sample contains 55 Type IIb SNe (SNe IIb), 45 Type Ib SNe (SNe Ib), 56 Type Ic SNe (SNe Ic), and 17 Type Ib/c SNe (SNe Ib/c). We have compared the SE SN subtypes via measurements of the pseudo-equivalent widths (pEWs) and velocities of the HeI λλ5876, 7065 and OI λ7774 absorption lines. Consistent with previous work, we find that SNe Ic show higher pEWs and velocities in OI λ7774 compared to SNe IIb and Ib. The pEWs of the HeI λλ5876, 7065 lines are similar in SNe Ib and IIb after maximum light. The HeI λλ5876, 7065 velocities at maximum light are higher in SNe Ib compared to SNe IIb. We identify an anticorrelation between the HeI λ7065 pEW and OI λ7774 velocity among SNe IIb and Ib. This can be interpreted as a continuum in the amount of He present at the time of explosion. It has been suggested that SNe Ib and Ic have similar amounts of He, and that lower mixing could be responsible for hiding He in SNe Ic. However, our data contradict this mixing hypothesis. The observed difference in the expansion rate of the ejecta around maximum light of SNe Ic (Vm = √2Ek/Mej ≈ 15 000 km s-1) and SNe Ib (Vm ≈ 9000 km s-1) would imply an average He mass difference of ∼1.4 M⊙, if the other explosion parameters are assumed to be unchanged between the SE SN subtypes. We conclude that SNe Ic do not hide He but lose He due to envelope stripping.
Published: 2018

17. Spectra of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

Author: Quimby, RM, Cia, AD, Gal-Yam, A, Leloudas, G, Lunnan, R, Perley, DA, Vreeswijk, PM, Yan, L, Bloom, JS, Cenko, SB, Cooke, J, Ellis, R, Filippenko, AV, Kasliwal, MM, Kleiser, IKW, Kulkarni, SR, Matheson, T, Nugent, PE, Pan, YC, Silverman, JM, Sternberg, A, Sullivan, M, and Yaron, O
Subjects: supernovae: general, astro-ph.HE, astro-ph.SR, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: Most Type I superluminous supernovae (SLSNe-I) reported to date have been identified by their high peak luminosities and spectra lacking obvious signs of hydrogen. We demonstrate that these events can be distinguished from normal-luminosity SNe (including Type Ic events) solely from their spectra over a wide range of light-curve phases. We use this distinction to select 19 SLSNe-I and four possible SLSNe-I from the Palomar Transient Factory archive (including seven previously published objects). We present 127 new spectra of these objects and combine these with 39 previously published spectra, and we use these to discuss the average spectral properties of SLSNe-I at different spectral phases. We find that Mn ii most probably contributes to the ultraviolet spectral features after maximum light, and we give a detailed study of the O ii features that often characterize the early-time optical spectra of SLSNe-I. We discuss the velocity distribution of O ii, finding that for some SLSNe-I this can be confined to a narrow range compared to relatively large systematic velocity shifts. Mg ii and Fe ii favor higher velocities than O ii and C ii, and we briefly discuss how this may constrain power-source models. We tentatively group objects by how well they match either SN 2011ke or PTF12dam and discuss the possibility that physically distinct events may have been previously grouped together under the SLSN-I label.
Published: 2018

18. A DECam Search for an Optical Counterpart to the LIGO Gravitational Wave Event GW151226

Author: Cowperthwaite, P. S., Berger, E., Soares-Santos, M., Annis, J., Brout, D., Brown, D. A., Buckley-Geer, E., Cenko, S. B., Chen, H. Y., Chornock, R., Diehl, H. T., Doctor, Z., Drlica-Wagner, A., Drout, M. R., Farr, B., Finley, D. A., Foley, R. J., Fong, W., Fox, D. B., Frieman, J., Garcia-Bellido, J., Gill, M. S. S., Gruendl, R. A., Herner, K., Holz, D. E., Kasen, D., Kessler, R., Lin, H., Margutti, R., Marriner, J., Matheson, T., Metzger, B. D., Neilsen Jr., E. H., Quataert, E., Rest, A., Sako, M., Scolnic, D., Smith, N., Sobreira, F., Strampelli, G. M., Villar, V. A., Walker, A. R., Wester, W., Williams, P. K. G., Yanny, B., Abbott, T. M. C., Abdalla, F. B., Allam, S., Armstrong, R., Bechtol, K., Benoit-Levy, A., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Dietrich, J. P., Evrard, A. E., Neto, A. Fausti, Fosalba, P., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gutierrez, G., Honscheid, K., James, D. J., Johnson, M. W. G., Johnson, M. D., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Reil, K., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, R. C., Suchyta, E., Tarle, G., Thomas, D., Thomas, R. C., Tucker, D. L., and Weller, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the results of a Dark Energy Camera (DECam) optical follow-up of the gravitational wave (GW) event GW151226, discovered by the Advanced LIGO detectors. Our observations cover 28.8 deg$^2$ of the localization region in the $i$ and $z$ bands (containing 3% of the BAYESTAR localization probability), starting 10 hours after the event was announced and spanning four epochs at $2-24$ days after the GW detection. We achieve $5\sigma$ point-source limiting magnitudes of $i\approx21.7$ and $z\approx21.5$, with a scatter of $0.4$ mag, in our difference images. Given the two day delay, we search this area for a rapidly declining optical counterpart with $\gtrsim 3\sigma$ significance steady decline between the first and final observations. We recover four sources that pass our selection criteria, of which three are cataloged AGN. The fourth source is offset by $5.8$ arcsec from the center of a galaxy at a distance of 187 Mpc, exhibits a rapid decline by $0.5$ mag over $4$ days, and has a red color of $i-z\approx 0.3$ mag. These properties roughly match the expectations for a kilonova. However, this source was detected several times, starting $94$ days prior to GW151226, in the Pan-STARRS Survey for Transients (dubbed as PS15cdi) and is therefore unrelated to the GW event. Given its long-term behavior, PS15cdi is likely a Type IIP supernova that transitioned out of its plateau phase during our observations, mimicking a kilonova-like behavior. We comment on the implications of this detection for contamination in future optical follow-up observations., Comment: 7 Pages, 2 Figures, 1 Table. Accepted to ApJL, updated to better match published version
Published: 2016
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19. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands., Comment: For the main Letter, see arXiv:1602.08492
Published: 2016
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20. Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. 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D., Páta, P., Vitek, S., Adame, J. A., Konig, S., Rendón, F., Sanguino, T. de J. Mateo, Fernández-Muñoz, R., Yock, P. C., Rattenbury, N., Allen, W. H., Querel, R., Jeong, S., Park, I. H., Bai, J., Cui, Ch., Fan, Y., Wang, Ch., Hiriart, D., Lee, W. H., Claret, A., Sánchez-Ramírez, R., Pandey, S. B., Mediavilla, T., Sabau-Graziati, L., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Armstrong, R., Benoit-Lévy, A., Berger, E., Bernstein, R. A., Bertin, E., Brout, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Carretero, J., Castander, F. J., Chornock, R., Cowperthwaite, P. S., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doctor, Z., Drlica-Wagner, A., Drout, M. R., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fong, W. -F., Fosalba, P., Fox, D. B., Frieman, J., Fryer, C. L., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Herner, K., Honscheid, K., James, D. J., Johnson, M. D., Johnson, M. W. G., Karliner, I., Kasen, D., Kent, S., Kessler, R., Kim, A. G., Kind, M. C., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Margutti, R., Marriner, J., Martini, P., Matheson, T., Melchior, P., Metzger, B. D., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R., Petravick, D., Plazas, A. A., Quataert, E., Roe, N., Romer, A. K., Roodman, A., Rosell, A. C., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Sheldon, E., Smith, N., Smith, R. C., Soares-Santos, M., Sobreira, F., Stebbins, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Wester, W., Yanny, B., Zuntz, J., Connaughton, V., Burns, E., Goldstein, A., Briggs, M. S., Zhang, B. -B., Hui, C. M., Jenke, P., Wilson-Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., Greiner, J., von Kienlin, A., Kippen, R. M., McBreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., Veres, P., Yu, H. -F., Blackburn, L., Ackermann, M., Ajello, M., Albert, A., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Cominsky, L. R., Costanza, F., Cuoco, A., D'Ammando, F., de Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gomez-Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hill, A. B., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kensei, S., Kocevski, D., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Li, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J., Maldera, S., Manfreda, A., Marelli, M., Mayer, M., Mazziotta, M. N., McEnery, J. E., Meyer, M., Michelson, P. F., Mirabal, N., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Parkinson, P. M. Saz, Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D'Avanzo, P., D'Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. -L., Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. R., Bhalerao, V., Miller, A. A., Barlow, T., Bellm, E., Manulis, I., Rana, J., Laher, R., Masci, F., Surace, J., Rebbapragada, U., Van Sistine, A., Sesar, B., Perley, D., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Hurley, K., Golenetskii, S. V., Aptekar, R. L., Frederiks, D. D., Svinkin, D. S., Rau, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., Abe, F., Doi, M., Fujisawa, K., Kawabata, K. S., Morokuma, T., Motohara, K., Tanaka, M., Ohta, K., Yanagisawa, K., Yoshida, M., Baltay, C., Rabinowitz, D., Ellman, N., Rostami, S., Bersier, D. F., Bode, M. F., Collins, C. A., Copperwheat, C. M., Darnley, M. J., Galloway, D. K., Gomboc, A., Kobayashi, S., Mazzali, P., Mundell, C. G., Piascik, A. S., Pollacco, Don, Steele, I. A., Ulaczyk, K., Broderick, J. W., Fender, R. P., Jonker, P. G., Rowlinson, A., Stappers, B. W., Wijers, R. A. M. J., Lipunov, V., Gorbovskoy, E., Tyurina, N., Kornilov, V., Balanutsa, P., Kuznetsov, A., Buckley, D., Rebolo, R., Serra-Ricart, M., Israelian, G., Budnev, N. M., Gress, O., Ivanov, K., Poleshuk, V., Tlatov, A., Yurkov, V., Kawai, N., Serino, M., Negoro, H., Nakahira, S., Mihara, T., Tomida, H., Ueno, S., Tsunemi, H., Matsuoka, M., Croft, S., Feng, L., Franzen, T. M. O., Gaensler, B. M., Johnston-Hollitt, M., Kaplan, D. L., Morales, M. F., Tingay, S. J., Wayth, R. B., Williams, A., Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Wright, D. E., Schultz, A., Denneau, L., Flewelling, H., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., E., F. Olivares, Campbell, H., Kotak, R., Sollerman, J., Smith, M., Dennefeld, M., Anderson, J. P., Botticella, M. T., Chen, T. -W., Valle, M. D., Elias-Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kupfer, T., Harmanen, J., Galbany, L., Guillou, L. Le, Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Razza, A., Terreran, G., Valenti, S., Gal-Yam, A., Ćwiek, A., Ćwiok, M., Mankiewicz, L., Opiela, R., Zaremba, M., Żarnecki, A. F., Onken, C. A., Scalzo, R. A., Schmidt, B. P., Wolf, C., Yuan, F., Evans, P. A., Kennea, J. A., Burrows, D. N., Campana, S., Cenko, S. B., Marshall, F. E., Nousek, J., O'Brien, P., Osborne, J. P., Palmer, D., Perri, M., Siegel, M., Tagliaferri, G., Klotz, A., Turpin, D., Laugier, R., Beroiz, M., Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Colazo, C., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., DePoy, D. L., Padilla, N., Pereyra, N. A., Benacquista, M., Tanvir, N. R., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Milvang-Jensen, B., Watson, D., Irwin, M., Fernandez, C. G., McMahon, R. G., Banerji, M., Gonzalez-Solares, E., Schulze, S., Postigo, A. de U., Thoene, C. C., Cano, Z., and Rosswog, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams., Comment: For Supplement, see https://arxiv.org/abs/1604.07864
Published: 2016
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21. A Dark Energy Camera Search for an Optical Counterpart to the First Advanced LIGO Gravitational Wave Event GW150914

Author: Soares-Santos, M., Kessler, R., Berger, E., Annis, J., Brout, D., Buckley-Geer, E., Chen, H., Cowperthwaite, P. S., Diehl, H. T., Doctor, Z., Drlica-Wagner, A., Farr, B., Finley, D. A., Flaugher, B., Foley, R. J., Frieman, J., Gruendl, R. A., Herner, K., Holz, D., Lin, H., Marriner, J., Neilsen, E., Rest, A., Sako, M., Scolnic, D., Sobreira, F., Walker, A. R., Wester, W., Yanny, B., Abbott, T. M. C., Abdalla, F. B., Allam, S., Armstrong, R., Banerji, M., Benoit-Lévy, A., Bernstein, R. A., Bertin, E., Brown, D. A., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cenko, S. B., Chornock, R., Crocce, M., D'Andrea, C. B., da Costa, L. N., Desai, S., Dietrich, J. P., Drout, M. R., Eifler, T. F., Estrada, J., Evrard, A. E., Fairhurst, S., Fernandez, E., Fischer, J., Fong, W., Fosalba, P., Fox, D. B., Fryer, C. L., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gutierrez, G., Honscheid, K., James, D. J., Karliner, I., Kasen, D., Kent, S., Kuropatkin, N., Kuehn, K., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., Margutti, R., Martini, P., Matheson, T., McMahon, R. G., Metzger, B. D., Miller, C. J., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R., Peoples, J., Plazas, A. A., Quataert, E., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Smith, N., Smith, R. C., Stebbins, A., Sutton, P. J., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, R. C., Tucker, D. L., Vikram, V., Wechsler, R. H., and Weller, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We report initial results of a deep search for an optical counterpart to the gravitational wave event GW150914, the first trigger from the Advanced LIGO gravitational wave detectors. We used the Dark Energy Camera (DECam) to image a 102 deg$^2$ area, corresponding to 38% of the initial trigger high-probability sky region and to 11% of the revised high-probability region. We observed in i and z bands at 4-5, 7, and 24 days after the trigger. The median $5\sigma$ point-source limiting magnitudes of our search images are i=22.5 and z=21.8 mag. We processed the images through a difference-imaging pipeline using templates from pre-existing Dark Energy Survey data and publicly available DECam data. Due to missing template observations and other losses, our effective search area subtends 40 deg$^{2}$, corresponding to 12% total probability in the initial map and 3% of the final map. In this area, we search for objects that decline significantly between days 4-5 and day 7, and are undetectable by day 24, finding none to typical magnitude limits of i= 21.5,21.1,20.1 for object colors (i-z)=1,0,-1, respectively. Our search demonstrates the feasibility of a dedicated search program with DECam and bodes well for future research in this emerging field., Comment: 6 pages, 1 figure. Updated references. Submitted to ApJL
Published: 2016
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22. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. IV. Detection of Near-infrared Signatures of r-process Nucleosynthesis with Gemini-South

Author: Chornock, R, Berger, E, Kasen, D, Cowperthwaite, PS, Nicholl, M, Villar, VA, Alexander, KD, Blanchard, PK, Eftekhari, T, Fong, W, Margutti, R, Williams, PKG, Annis, J, Brout, D, Brown, DA, Chen, H-Y, Drout, MR, Farr, B, Foley, RJ, Frieman, JA, Fryer, CL, Herner, K, Holz, DE, Kessler, R, Matheson, T, Metzger, BD, Quataert, E, Rest, A, Sako, M, Scolnic, DM, Smith, N, and Soares-Santos, M
Subjects: binaries: close, nuclear reactions, nucleosynthesis, abundances, stars: neutron, astro-ph.HE, astro-ph.GA, astro-ph.SR, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: We present a near-infrared spectral sequence of the electromagnetic counterpart to the binary neutron star merger GW170817 detected by Advanced Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo. Our data set comprises seven epochs of J+H spectra taken with FLAMINGOS-2 on Gemini-South between 1.5 and 10.5 days after the merger. In the initial epoch, the spectrum is dominated by a smooth blue continuum due to a high-velocity, lanthanide-poor blue kilonova component. Starting the following night, all of the subsequent spectra instead show features that are similar to those predicted in model spectra of material with a high concentration of lanthanides, including spectral peaks near 1.07 and 1.55 μm. Our fiducial model with 0.04 M o of ejecta, an ejection velocity of v = 0.1c, and a lanthanide concentration of X lan = 10-2 provides a good match to the spectra taken in the first five days, although it over-predicts the late-time fluxes. We also explore models with multiple fitting components, in each case finding that a significant abundance of lanthanide elements is necessary to match the broad spectral peaks that we observe starting at 2.5 days after the merger. These data provide direct evidence that binary neutron star mergers are significant production sites of even the heaviest r-process elements.
Published: 2017

23. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. II. UV, Optical, and Near-infrared Light Curves and Comparison to Kilonova Models

Author: Cowperthwaite, PS, Berger, E, Villar, VA, Metzger, BD, Nicholl, M, Chornock, R, Blanchard, PK, Fong, W, Margutti, R, Soares-Santos, M, Alexander, KD, Allam, S, Annis, J, Brout, D, Brown, DA, Butler, RE, Chen, H-Y, Diehl, HT, Doctor, Z, Drout, MR, Eftekhari, T, Farr, B, Finley, DA, Foley, RJ, Frieman, JA, Fryer, CL, García-Bellido, J, Gill, MSS, Guillochon, J, Herner, K, Holz, DE, Kasen, D, Kessler, R, Marriner, J, Matheson, T, Neilsen, EH, Quataert, E, Palmese, A, Rest, A, Sako, M, Scolnic, DM, Smith, N, Tucker, DL, Williams, PKG, Balbinot, E, Carlin, JL, Cook, ER, Durret, F, Li, TS, Lopes, PAA, Lourenço, ACC, Marshall, JL, Medina, GE, Muir, J, Muñoz, RR, Sauseda, M, Schlegel, DJ, Secco, LF, Vivas, AK, Wester, W, Zenteno, A, Zhang, Y, Abbott, TMC, Banerji, M, Bechtol, K, Benoit-Lévy, A, Bertin, E, Buckley-Geer, E, Burke, DL, Capozzi, D, Rosell, A Carnero, Kind, M Carrasco, Castander, FJ, Crocce, M, Cunha, CE, D’Andrea, CB, da Costa, LN, Davis, C, DePoy, DL, Desai, S, Dietrich, JP, Drlica-Wagner, A, Eifler, TF, Evrard, AE, Fernandez, E, Flaugher, B, Fosalba, P, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Goldstein, DA, Gruen, D, Gruendl, RA, Gutierrez, G, Honscheid, K, Jain, B, James, DJ, Jeltema, T, Johnson, MWG, and Johnson, MD
Subjects: Space Sciences, Astronomical Sciences, Physical Sciences, binaries: close, catalogs, gravitational waves, stars: neutron, surveys, astro-ph.HE, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Space sciences
Abstract: We present UV, optical, and near-infrared (NIR) photometry of the first electromagnetic counterpart to a gravitational wave source from Advanced Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo, the binary neutron star merger GW170817. Our data set extends from the discovery of the optical counterpart at 0.47-18.5 days post-merger, and includes observations with the Dark Energy Camera (DECam), Gemini-South/FLAMINGOS-2 (GS/F2), and the Hubble Space Telescope (HST). The spectral energy distribution (SED) inferred from this photometry at 0.6 days is well described by a blackbody model with T ≈ 8300 K, a radius of R ≈ 4.5 × 1014cm (corresponding to an expansion velocity of v ≈ 0.3c), and a bolometric luminosity of Lbol ≈ 5 × 1041 erg s-1. At 1.5 days we find a multi-component SED across the optical and NIR, and subsequently we observe rapid fading in the UV and blue optical bands and significant reddening of the optical/NIR colors. Modeling the entire data set, we find that models with heating from radioactive decay of 56Ni, or those with only a single component of opacity from r-process elements, fail to capture the rapid optical decline and red optical/NIR colors. Instead, models with two components consistent with lanthanide-poor and lanthanide-rich ejecta provide a good fit to the data; the resulting "blue" component has Mblueej 0.1 M⊙ and vblueej ≈ 0.3c, and the "red" component has and Mredej ≈ 0.04 M⊙ and vredej ≈ 0.1 c. These ejecta masses are broadly consistent with the estimated r-process production rate required to explain the Milky Way r-process abundances, providing the first evidence that binary neutron star (BNS) mergers can be a dominant site of r-process enrichment.
Published: 2017

24. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. I. Discovery of the Optical Counterpart Using the Dark Energy Camera

Author: Soares-Santos, M, Holz, DE, Annis, J, Chornock, R, Herner, K, Berger, E, Brout, D, Chen, H-Y, Kessler, R, Sako, M, Allam, S, Tucker, DL, Butler, RE, Palmese, A, Doctor, Z, Diehl, HT, Frieman, J, Yanny, B, Lin, H, Scolnic, D, Cowperthwaite, P, Neilsen, E, Marriner, J, Kuropatkin, N, Hartley, WG, Paz-Chinchón, F, Alexander, KD, Balbinot, E, Blanchard, P, Brown, DA, Carlin, JL, Conselice, C, Cook, ER, Drlica-Wagner, A, Drout, MR, Durret, F, Eftekhari, T, Farr, B, Finley, DA, Foley, RJ, Fong, W, Fryer, CL, García-Bellido, J, Gill, MSS, Gruendl, RA, Hanna, C, Kasen, D, Li, TS, Lopes, PAA, Lourenço, ACC, Margutti, R, Marshall, JL, Matheson, T, Medina, GE, Metzger, BD, Muñoz, RR, Muir, J, Nicholl, M, Quataert, E, Rest, A, Sauseda, M, Schlegel, DJ, Secco, LF, Sobreira, F, Stebbins, A, Villar, VA, Vivas, K, Walker, AR, Wester, W, Williams, PKG, Zenteno, A, Zhang, Y, Abbott, TMC, Abdalla, FB, Banerji, M, Bechtol, K, Benoit-Lévy, A, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Castander, FJ, Crocce, M, Cunha, CE, D’Andrea, CB, da Costa, LN, Davis, C, Desai, S, Dietrich, JP, Doel, P, Eifler, TF, Fernandez, E, Flaugher, B, Fosalba, P, Gaztanaga, E, Gerdes, DW, and Giannantonio, T
Subjects: binaries: close, catalogs, gravitational waves, stars: neutron, surveys, astro-ph.HE, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: We present the Dark Energy Camera (DECam) discovery of the optical counterpart of the first binary neutron star merger detected through gravitational-wave emission, GW170817. Our observations commenced 10.5 hr post-merger, as soon as the localization region became accessible from Chile. We imaged 70 deg2 in the i and z bands, covering 93% of the initial integrated localization probability, to a depth necessary to identify likely optical counterparts (e.g., a kilonova). At 11.4 hr post-merger we detected a bright optical transient located from the nucleus of NGC 4993 at redshift z = 0.0098, consistent (for km s-1 Mpc-1) with the distance of 40 ±8 Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes of and , and thus an absolute magnitude of , in the luminosity range expected for a kilonova. We identified 1500 potential transient candidates. Applying simple selection criteria aimed at rejecting background events such as supernovae, we find the transient associated with NGC 4993 as the only remaining plausible counterpart, and reject chance coincidence at the 99.5% confidence level. We therefore conclude that the optical counterpart we have identified near NGC 4993 is associated with GW170817. This discovery ushers in the era of multi-messenger astronomy with gravitational waves and demonstrates the power of DECam to identify the optical counterparts of gravitational-wave sources.
Published: 2017

25. Deja Vu All Over Again: The Reappearance of Supernova Refsdal

Author: Kelly, P. L., Rodney, S. A., Treu, T., Strolger, L. G., Foley, R. J., Jha, S. W., Selsing, J., Brammer, G., Bradac, M., Cenko, S. B., Graham, M. L., Graur, O., Filippenko, A. V., Hjorth, J., Matheson, T., McCully, C., Molino, A., Nonino, M., Riess, A. G., Schmidt, K. B., Tucker, B., von der Linden, A., Weiner, B. J., and Zitrin, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: In Hubble Space Telescope (HST) imaging taken on 10 November 2014, four images of supernova (SN) "Refsdal" (redshift z=1.49) appeared in an Einstein-cross--like configuration (images S1-S4) around an early-type galaxy in the cluster MACS J1149.5+2223 (z=0.54). Almost all lens models of the cluster have predicted that the SN should reappear within a year in a second host-galaxy image created by the cluster's potential. In HST observations taken on 11 December 2015, we find a new source at the predicted position of the new image of SN Refsdal approximately 8" from the previous images S1-S4. This marks the first time the appearance of a SN at a particular time and location in the sky was successfully predicted in advance! We use these data and the light curve from the first four observed images of SN Refsdal to place constraints on the relative time delay and magnification of the new image (SX), compared to images S1-S4. This enables us, for the first time, to test "blind" lens model predictions of both magnifications and time delays for a lensed SN. We find that the timing and brightness of the new image are consistent with the blind predictions of a fraction of the models. The reappearance illustrates the discriminatory power of this blind test and its utility to uncover sources of systematic uncertainty. From planned HST photometry, we expect to reach a precision of 1-2% on the time delay between S1-S4 and SX., Comment: Accepted ApJL version
Published: 2015
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26. Flash Spectroscopy: Emission Lines from the Ionized Circumstellar Material around $<10$-Day-Old Type II Supernovae

Author: Khazov, D., Yaron, O., Gal-Yam, A., Manulis, I., Rubin, A., Kulkarni, S. R., Arcavi, I., Kasliwal, M. M., Ofek, E. O., Cao, Y., Perley, D., Sollerman, J., Horesh, A., Sullivan, M., Filippenko, A. V., Nugent, P. E., Howell, D. A., Cenko, S. B., Silverman, J. M., Ebeling, H., Taddia, F., Johansson, J., Laher, R. R., Surace, J., Rebbapragada, U. D., Wozniak, P. R., and Matheson, T.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Supernovae (SNe) embedded in dense circumstellar material (CSM) may show prominent emission lines in their early-time spectra ($\leq 10$ days after the explosion), owing to recombination of the CSM ionized by the shock-breakout flash. From such spectra ("flash spectroscopy"), we can measure various physical properties of the CSM, as well as the mass-loss rate of the progenitor during the year prior to its explosion. Searching through the Palomar Transient Factory (PTF and iPTF) SN spectroscopy databases from 2009 through 2014, we found 12 Type II SNe showing flash-ionized (FI) signatures in their first spectra. All are younger than 10 days. These events constitute 14\% of all 84 SNe in our sample having a spectrum within 10 days from explosion, and 18\% of SNe~II observed at ages $<5$ days, thereby setting lower limits on the fraction of FI events. We classified as "blue/featureless" (BF) those events having a first spectrum which is similar to that of a black body, without any emission or absorption signatures. It is possible that some BF events had FI signatures at an earlier phase than observed, or that they lack dense CSM around the progenitor. Within 2 days after explosion, 8 out of 11 SNe in our sample are either BF events or show FI signatures. Interestingly, we found that 19 out of 21 SNe brighter than an absolute magnitude $M_R=-18.2$ belong to the FI or BF groups, and that all FI events peaked above $M_R=-17.6$ mag, significantly brighter than average SNe~II., Comment: Accepted to ApJ
Published: 2015
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27. Light Echoes of Ancient Transients with the Blanco CTIO 4m Telescope

Author: Rest, A., Sinnott, B., Welch, D. L., Prieto, J. L., Bianco, F. B., Matheson, T., Smith, R. C., and Suntzeff, N. B.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: For over a century, light echoes have been observed around variable stars and transients. The discovery of centuries-old light echoes from supernovae in the Large Magellanic Cloud has allowed the spectroscopic characterization of these events using modern instrumentation, even in the complete absence of any visual record of those events. Here we review the pivotal role the Blanco 4m telescope played in these discoveries., Comment: 13 pages, 7 figures, conference paper for "Fifty Years of Wide Field Studies in the Southern Hemisphere" conference proceedings
Published: 2015

28. A DECAM SEARCH FOR AN OPTICAL COUNTERPART TO THE LIGO GRAVITATIONAL-WAVE EVENT GW151226

Author: Cowperthwaite, PS, Berger, E, Soares-Santos, M, Annis, J, Brout, D, Brown, DA, Buckley-Geer, E, Cenko, SB, Chen, HY, Chornock, R, Diehl, HT, Doctor, Z, Drlica-Wagner, A, Drout, MR, Farr, B, Finley, DA, Foley, RJ, Fong, W, Fox, DB, Frieman, J, Garcia-Bellido, J, Gill, MSS, Gruendl, RA, Herner, K, Holz, DE, Kasen, D, Kessler, R, Lin, H, Margutti, R, Marriner, J, Matheson, T, Metzger, BD, Neilsen, EH, Quataert, E, Rest, A, Sako, M, Scolnic, D, Smith, N, Sobreira, F, Strampelli, GM, Villar, VA, Walker, AR, Wester, W, Williams, PKG, Yanny, B, Abbott, TMC, Abdalla, FB, Allam, S, Armstrong, R, Bechtol, K, Benoit-Lévy, A, Bertin, E, Brooks, D, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Castander, FJ, Cunha, CE, D’Andrea, CB, da Costa, LN, Desai, S, Dietrich, JP, Evrard, AE, Neto, A Fausti, Fosalba, P, Gerdes, DW, Giannantonio, T, Goldstein, DA, Gruen, D, Gutierrez, G, Honscheid, K, James, DJ, Johnson, MWG, Johnson, MD, Krause, E, Kuehn, K, Kuropatkin, N, Lima, M, Maia, MAG, Marshall, JL, Menanteau, F, Miquel, R, Mohr, JJ, Nichol, RC, Nord, B, Ogando, R, Plazas, AA, Reil, K, Romer, AK, Sanchez, E, Scarpine, V, Sevilla-Noarbe, I, Smith, RC, Suchyta, E, Tarle, G, Thomas, D, Thomas, RC, Tucker, DL, and Weller, J
Subjects: binaries: close, catalogs, gravitational waves, stars: neutron, surveys, astro-ph.HE, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: We report the results of a Dark Energy Camera optical follow-up of the gravitational-wave (GW) event GW151226, discovered by the Advanced Laser Interferometer Gravitational-wave Observatory detectors. Our observations cover 28.8 deg2 of the localization region in the i and z bands (containing 3% of the BAYESTAR localization probability), starting 10 hr after the event was announced and spanning four epochs at 2-24 days after the GW detection. We achieve point-source limiting magnitudes of and , with a scatter of 0.4 mag, in our difference images. Given the two-day delay, we search this area for a rapidly declining optical counterpart with significance steady decline between the first and final observations. We recover four sources that pass our selection criteria, of which three are cataloged active galactic nuclei. The fourth source is offset by 5.8 arcsec from the center of a galaxy at a distance of 187 Mpc, exhibits a rapid decline by 0.5 mag over 4 days, and has a red color of mag. These properties could satisfy a set of cuts designed to identify kilonovae. However, this source was detected several times, starting 94 days prior to GW151226, in the Pan-STARRS Survey for Transients (dubbed as PS15cdi) and is therefore unrelated to the GW event. Given its long-term behavior, PS15cdi is likely a Type IIP supernova that transitioned out of its plateau phase during our observations, mimicking a kilonova-like behavior. We comment on the implications of this detection for contamination in future optical follow-up observations.
Published: 2016

29. A DARK ENERGY CAMERA SEARCH FOR AN OPTICAL COUNTERPART TO THE FIRST ADVANCED LIGO GRAVITATIONAL WAVE EVENT GW150914

Author: Soares-Santos, M, Kessler, R, Berger, E, Annis, J, Brout, D, Buckley-Geer, E, Chen, H, Cowperthwaite, PS, Diehl, HT, Doctor, Z, Drlica-Wagner, A, Farr, B, Finley, DA, Flaugher, B, Foley, RJ, Frieman, J, Gruendl, RA, Herner, K, Holz, D, Lin, H, Marriner, J, Neilsen, E, Rest, A, Sako, M, Scolnic, D, Sobreira, F, Walker, AR, Wester, W, Yanny, B, Abbott, TMC, Abdalla, FB, Allam, S, Armstrong, R, Banerji, M, Benoit-Levy, A, Bernstein, RA, Bertin, E, Brown, DA, Burke, DL, Capozzi, D, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Castander, FJ, Cenko, SB, Chornock, R, Crocce, M, D'Andrea, CB, da Costa, LN, Desai, S, Dietrich, JP, Drout, MR, Eifler, TF, Estrada, J, Evrard, AE, Fairhurst, S, Fernandez, E, Fischer, J, Fong, W, Fosalba, P, Fox, DB, Fryer, CL, Garcia-Bellido, J, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gutierrez, G, Honscheid, K, James, DJ, Karliner, I, Kasen, D, Kent, S, Kuropatkin, N, Kuehn, K, Lahav, O, Li, TS, Lima, M, Maia, MAG, Margutti, R, Martini, P, Matheson, T, McMahon, RG, Metzger, BD, Miller, CJ, Miquel, R, Mohr, JJ, Nichol, RC, Nord, B, Ogando, R, Peoples, J, Plazas, AA, Quataert, E, Romer, AK, Roodman, A, Rykoff, ES, Sanchez, E, Scarpine, V, Schindler, R, and Schubnell, M
Subjects: binaries: close, catalogs, gravitational waves, stars: neutron, surveys, Astronomy & Astrophysics, Astronomical and Space Sciences
Published: 2016

30. TYPE II SUPERNOVA ENERGETICS and COMPARISON of LIGHT CURVES to SHOCK-COOLING MODELS

Author: Rubin, A, Gal-Yam, A, De Cia, A, Horesh, A, Khazov, D, Ofek, EO, Kulkarni, SR, Arcavi, I, Manulis, I, Yaron, O, Vreeswijk, P, Kasliwal, MM, Ben-Ami, S, Perley, DA, Cao, Y, Cenko, SB, Rebbapragada, UD, Woźniak, PR, Filippenko, AV, Clubb, KI, Nugent, PE, Pan, YC, Badenes, C, Howell, DA, Valenti, S, Sand, D, Sollerman, J, Johansson, J, Leonard, DC, Horst, JC, Armen, SF, Fedrow, JM, Quimby, RM, Mazzali, P, Pian, E, Sternberg, A, Matheson, T, Sullivan, M, Maguire, K, and Lazarevic, S
Subjects: supernovae: general, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: During the first few days after explosion, Type II supernovae (SNe) are dominated by relatively simple physics. Theoretical predictions regarding early-time SN light curves in the ultraviolet (UV) and optical bands are thus quite robust. We present, for the first time, a sample of 57 R-band SN II light curves that are well-monitored during their rise, with detections during the first 10 days after discovery, and a well-constrained time of explosion to within 1-3 days. We show that the energy per unit mass (E/M) can be deduced to roughly a factor of five by comparing early-time optical data to the 2011 model of Rabinak & Waxman, while the progenitor radius cannot be determined based on R-band data alone. We find that SN II explosion energies span a range of E/M = (0.2-20) ×1051 erg/(10 ), and have a mean energy per unit mass of erg/(10 ), corrected for Malmquist bias. Assuming a small spread in progenitor masses, this indicates a large intrinsic diversity in explosion energy. Moreover, E/M is positively correlated with the amount of 56Ni produced in the explosion, as predicted by some recent models of core-collapse SNe. We further present several empirical correlations. The peak magnitude is correlated with the decline rate (), the decline rate is weakly correlated with the rise time, and the rise time is not significantly correlated with the peak magnitude. Faster declining SNe are more luminous and have longer rise times. This limits the possible power sources for such events.
Published: 2016

31. FLASH SPECTROSCOPY: EMISSION LINES FROM THE IONIZED CIRCUMSTELLAR MATERIAL AROUND <10-DAY-OLD TYPE II SUPERNOVAE

Author: Khazov, D, Yaron, O, Gal-Yam, A, Manulis, I, Rubin, A, Kulkarni, SR, Arcavi, I, Kasliwal, MM, Ofek, EO, Cao, Y, Perley, D, Sollerman, J, Horesh, A, Sullivan, M, Filippenko, AV, Nugent, PE, Howell, DA, Cenko, SB, Silverman, JM, Ebeling, H, Taddia, F, Johansson, J, Laher, RR, Surace, J, Rebbapragada, UD, Wozniak, PR, and Matheson, T
Subjects: Space Sciences, Physical Sciences, supernovae: general, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: Supernovae (SNe) embedded in dense circumstellar material (CSM) may show prominent emission lines in their early-time spectra (≤10 days after the explosion), owing to recombination of the CSM ionized by the shock-breakout flash. From such spectra ("flash spectroscopy"), we can measure various physical properties of the CSM, as well as the mass-loss rate of the progenitor during the year prior to its explosion. Searching through the Palomar Transient Factory (PTF and iPTF) SN spectroscopy databases from 2009 through 2014, we found 12 SNe II showing flash-ionized (FI) signatures in their first spectra. All are younger than 10 days. These events constitute 14% of all 84 SNe in our sample having a spectrum within 10 days from explosion, and 18% of SNe II observed at ages
Published: 2016

32. Light Echoes from Eta Carinae's Great Eruption: Spectrophotometric Evolution and the Rapid Formation of Nitrogen-rich Molecules

Author: Prieto, J. L., Rest, A., Bianco, F. B., Matheson, T., Smith, N., Walborn, N. R., Hsiao, E. Y., Chornock, R., Alvarez, L. Paredes, Campillay, A., Contreras, C., Gonzalez, C., James, D., Knapp, G. R., Kunder, A., Margheim, S., Morrell, N., Phillips, M. M., Smith, R. C., Welch, D. L., and Zenteno, A.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present follow-up optical imaging and spectroscopy of one of the light echoes of $\eta$ Carinae's 19th-century Great Eruption discovered by Rest et al. (2012). By obtaining images and spectra at the same light echo position between 2011 and 2014, we follow the evolution of the Great Eruption on a three-year timescale. We find remarkable changes in the photometric and spectroscopic evolution of the echo light. The $i$-band light curve shows a decline of $\sim 0.9$ mag in $\sim 1$ year after the peak observed in early 2011 and a flattening at later times. The spectra show a pure-absorption early G-type stellar spectrum at peak, but a few months after peak the lines of the [Ca II] triplet develop strong P-Cygni profiles and we see the appearance of [Ca II] 7291,7324 doublet in emission. These emission features and their evolution in time resemble those observed in the spectra of some Type IIn supernovae and supernova impostors. Most surprisingly, starting $\sim 300$ days after peak brightness, the spectra show strong molecular transitions of CN at $\gtrsim 6800$ \AA. The appearance of these CN features can be explained if the ejecta are strongly Nitrogen enhanced, as it is observed in modern spectroscopic studies of the bipolar Homunculus nebula. Given the spectroscopic evolution of the light echo, velocities of the main features, and detection of strong CN, we are likely seeing ejecta that contributes directly to the Homunculus nebula., Comment: accepted in ApJL
Published: 2014
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33. Slow-speed supernovae from the Palomar transient factory: Two channels

Author: White, CJ, Kasliwal, MM, Nugent, PE, Gal-Yam, A, Howell, DA, Sullivan, M, Goobar, A, Piro, AL, Bloom, JS, Kulkarni, SR, Laher, RR, Masci, F, Ofek, EO, Surace, J, Ben-Ami, S, Cao, Y, Cenko, SB, Hook, IM, Jönsson, J, Matheson, T, Sternberg, A, Quimby, RM, and Yaron, O
Subjects: supernovae: general, supernovae: individual (iPTF 13an, PTF 09ego, PTF 09eiy, PTF 09eoi, PTF 10xk, PTF 10bvr, PTF 10ujn, PTF 10acdh, PTF 11hyh, SN 2002cx, SN 2002es), surveys, techniques: spectroscopic, astro-ph.HE, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: Since the discovery of the unusual prototype SN 2002cx, the eponymous class of Type I (hydrogen-poor) supernovae with low ejecta speeds has grown to include approximately two dozen members identified from several heterogeneous surveys, in some cases ambiguously. Here we present the results of a systematic study of 1077 Type I supernovae discovered by the Palomar Transient Factory, leading to nine new members of this peculiar class. Moreover, we find there are two distinct subclasses based on their spectroscopic, photometric, and host galaxy properties: "SN 2002cx-like" supernovae tend to be in later-type or more irregular hosts, have more varied and generally dimmer luminosities, have longer rise times, and lack a Ti II trough when compared to "SN 2002es-like" supernovae. None of our objects show helium, and we counter a previous claim of two such events. We also find that the occurrence rate of these transients relative to Type Ia supernovae is (90% confidence), lower compared to earlier estimates. Combining our objects with the literature sample, we propose that these subclasses have two distinct physical origins.
Published: 2015

34. Type-Ia Supernova Rates to Redshift 2.4 from CLASH: the Cluster Lensing And Supernova survey with Hubble

Author: Graur, O., Rodney, S. A., Maoz, D., Riess, A. G., Jha, S. W., Postman, M., Dahlen, T., Holoien, T. W. -S., McCully, C., Patel, B., Strolger, L. -G., Benitez, N., Coe, D., Jouvel, S., Medezinski, E., Molino, A., Nonino, M., Bradley, L., Koekemoer, A., Balestra, I., Cenko, S. B., Clubb, K. I., Dickinson, M. E., Filippenko, A. V., Frederiksen, T. F., Garnavich, P., Hjorth, J., Jones, D. O., Leibundgut, B., Matheson, T., Mobasher, B., Rosati, P., Silverman, J. M., U, V., Jedruszczuk, K., Li, C., Lin, K., Mirmelstein, M., Neustadt, J., Ovadia, A., and Rogers, E. H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the supernova (SN) sample and Type-Ia SN (SN Ia) rates from the Cluster Lensing And Supernova survey with Hubble (CLASH). Using the Advanced Camera for Surveys and the Wide Field Camera 3 on the Hubble Space Telescope (HST), we have imaged 25 galaxy-cluster fields and parallel fields of non-cluster galaxies. We report a sample of 27 SNe discovered in the parallel fields. Of these SNe, ~13 are classified as SN Ia candidates, including four SN Ia candidates at redshifts z > 1.2. We measure volumetric SN Ia rates to redshift 1.8 and add the first upper limit on the SN Ia rate in the range 1.8 < z < 2.4. The results are consistent with the rates measured by the HST/GOODS and Subaru Deep Field SN surveys. We model these results together with previous measurements at z < 1 from the literature. The best-fitting SN Ia delay-time distribution (DTD; the distribution of times that elapse between a short burst of star formation and subsequent SN Ia explosions) is a power law with an index of -1.00 +0.06(0.09) -0.06(0.10) (statistical) +0.12 -0.08 (systematic), where the statistical uncertainty is a result of the 68% and 95% (in parentheses) statistical uncertainties reported for the various SN Ia rates (from this work and from the literature), and the systematic uncertainty reflects the range of possible cosmic star-formation histories. We also test DTD models produced by an assortment of published binary population synthesis (BPS) simulations. The shapes of all BPS double-degenerate DTDs are consistent with the volumetric SN Ia measurements, when the DTD models are scaled up by factors of 3-9. In contrast, all BPS single-degenerate DTDs are ruled out by the measurements at a >99% significance level., Comment: Accepted by ApJ. 19 pages, 14 figures, 6 tables. Minor corrections
Published: 2013
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35. The Infrared Light Curve of SN 2011fe in M101 and the Distance to M101

Author: Matheson, T., Joyce, R. R., Allen, L. E., Saha, A., Silva, D. R., Wood-Vasey, W. M., Adams, J. J., Anderson, R. E., Beck, T. L., Bentz, M. C., Bershady, M. A., Binkert, W. S., Butler, K., Camarata, M. A., Eigenbrot, A., Everett, M., Gallagher, J. S., Glikman, P. M. Garnavich E., Harbeck, D., Hargis, J. R., Herbst, H., Horch, E. P., Howell, S. B., Jha, S., Kaczmarek, J. F., Knezek, P., Manne-Nicholas, E., Mathieu, R. D., Meixner, M., Milliman, K., Power, J., Rajagopal, J., Reetz, K., Rhode, K. L., Schechtman-Rook, A., Schwamb, M. E., Schweiker, H., Simmons, B., Simon, J. D., Summers, D., Young, M. D., Weyant, A., Wilcots, E. M., Will, G., and Williams, D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present near infra-red light curves of supernova (SN) 2011fe in M101, including 34 epochs in H band starting fourteen days before maximum brightness in the B-band. The light curve data were obtained with the WIYN High-Resolution Infrared Camera (WHIRC). When the data are calibrated using templates of other Type Ia SNe, we derive an apparent H-band magnitude at the epoch of B-band maximum of 10.85 \pm 0.04. This implies a distance modulus for M101 that ranges from 28.86 to 29.17 mag, depending on which absolute calibration for Type Ia SNe is used., Comment: 9 pages, 3 figures, emulateapj style, accepted for publication in The Astrophysical Journal
Published: 2012
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36. The Spectroscopic Diversity of Type Ia Supernovae

Author: Blondin, S., Matheson, T., Kirshner, R. P., Mandel, K. S., Berlind, P., Calkins, M., Challis, P., Garnavich, P. M., Jha, S. W., Modjaz, M., Riess, A. G., and Schmidt, B. P.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We present 2603 spectra of 462 nearby Type Ia supernovae (SN Ia) obtained during 1993-2008 through the Center for Astrophysics Supernova Program. Most of the spectra were obtained with the FAST spectrograph at the FLWO 1.5m telescope and reduced in a consistent manner, making data set well suited for studies of SN Ia spectroscopic diversity. We study the spectroscopic and photometric properties of SN Ia as a function of spectroscopic class using the classification schemes of Branch et al. and Wang et al. The width-luminosity relation appears to be steeper for SN Ia with broader lines. Based on the evolution of the characteristic Si II 6355 line, we propose improved methods for measuring velocity gradients, revealing a larger range than previously suspected, from ~0 to ~400 km/s/day considering the instantaneous velocity decline rate at maximum light. We find a weaker and less significant correlation between Si II velocity and intrinsic B-V color at maximum light than reported by Foley et al., owing to a more comprehensive treatment of uncertainties and host galaxy dust. We study the extent of nuclear burning and report new detections of C II 6580 in 23 early-time spectra. The frequency of C II detections is not higher in SN Ia with bluer colors or narrower light curves, in conflict with the recent results of Thomas et al. Based on nebular spectra of 27 SN Ia, we find no relation between the FWHM of the iron emission feature at ~4700 A and Dm15(B) after removing the two low-luminosity SN 1986G and SN 1991bg, suggesting that the peak luminosity is not strongly dependent on the kinetic energy of the explosion for most SN Ia. Finally, we confirm the correlation of velocity shifts in some nebular lines with the intrinsic B-V color of SN Ia at maximum light, although several outliers suggest a possible non-monotonic behavior for the largest blueshifts., Comment: 36 pages (emulateapj), 23 figures. Accepted for publication in AJ. Spectroscopic data available at http://www.cfa.harvard.edu/supernova/SNarchive.html . New SNID template set available at http://marwww.in2p3.fr/~blondin/software/snid/index.html . Minor changes from v1 to conform to published version
Published: 2012
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37. The BigBOSS Experiment

Author: Schlegel, D., Abdalla, F., Abraham, T., Ahn, C., Prieto, C. Allende, Annis, J., Aubourg, E., Azzaro, M., Baltay, S. Bailey. C., Baugh, C., Bebek, C., Becerril, S., Blanton, M., Bolton, A., Bromley, B., Cahn, R., Carton, P. -H., Cervantes-Cota, J. L., Chu, Y., Cortes, M., Dawson, K., Dey, A., Dickinson, M., Diehl, H. T., Doel, P., Ealet, A., Edelstein, J., Eppelle, D., Escoffier, S., Evrard, A., Faccioli, L., Frenk, C., Geha, M., Gerdes, D., Gondolo, P., Gonzalez-Arroyo, A., Grossan, B., Heckman, T., Heetderks, H., Ho, S., Honscheid, K., Huterer, D., Ilbert, O., Ivans, I., Jelinsky, P., Jing, Y., Joyce, D., Kennedy, R., Kent, S., Kieda, D., Kim, A., Kim, C., Kneib, J. -P., Kong, X., Kosowsky, A., Krishnan, K., Lahav, O., Lampton, M., LeBohec, S., Brun, V. Le, Levi, M., Li, C., Liang, M., Lim, H., Lin, W., Linder, E., Lorenzon, W., de la Macorra, A., Magneville, Ch., Malina, R., Marinoni, C., Martinez, V., Majewski, S., Matheson, T., McCloskey, R., McDonald, P., McKay, T., McMahon, J., Menard, B., Miralda-Escude, J., Modjaz, M., Montero-Dorta, A., Morales, I., Mostek, N., Newman, J., Nichol, R., Nugent, P., Olsen, K., Padmanabhan, N., Palanque-Delabrouille, N., Park, I., Peacock, J., Percival, W., Perlmutter, S., Peroux, C., Petitjean, P., Prada, F., Prieto, E., Prochaska, J., Reil, K., Rockosi, C., Roe, N., Rollinde, E., Roodman, A., Ross, N., Rudnick, G., Ruhlmann-Kleider, V., Sanchez, J., Sawyer, D., Schimd, C., Schubnell, M., Scoccimaro, R., Seljak, U., Seo, H., Sheldon, E., Sholl, M., Shulte-Ladbeck, R., Slosar, A., Smith, D. S., Smoot, G., Springer, W., Stril, A., Szalay, A. S., Tao, C., Tarle, G., Taylor, E., Tilquin, A., Tinker, J., Valdes, F., Wang, J., Wang, T., Weaver, B. A., Weinberg, D., White, M., Wood-Vasey, M., Yang, J., Yeche, X. Yang. Ch., Zakamska, N., Zentner, A., Zhai, C., and Zhang, P.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: BigBOSS is a Stage IV ground-based dark energy experiment to study baryon acoustic oscillations (BAO) and the growth of structure with a wide-area galaxy and quasar redshift survey over 14,000 square degrees. It has been conditionally accepted by NOAO in response to a call for major new instrumentation and a high-impact science program for the 4-m Mayall telescope at Kitt Peak. The BigBOSS instrument is a robotically-actuated, fiber-fed spectrograph capable of taking 5000 simultaneous spectra over a wavelength range from 340 nm to 1060 nm, with a resolution R = 3000-4800. Using data from imaging surveys that are already underway, spectroscopic targets are selected that trace the underlying dark matter distribution. In particular, targets include luminous red galaxies (LRGs) up to z = 1.0, extending the BOSS LRG survey in both redshift and survey area. To probe the universe out to even higher redshift, BigBOSS will target bright [OII] emission line galaxies (ELGs) up to z = 1.7. In total, 20 million galaxy redshifts are obtained to measure the BAO feature, trace the matter power spectrum at smaller scales, and detect redshift space distortions. BigBOSS will provide additional constraints on early dark energy and on the curvature of the universe by measuring the Ly-alpha forest in the spectra of over 600,000 2.2 < z < 3.5 quasars. BigBOSS galaxy BAO measurements combined with an analysis of the broadband power, including the Ly-alpha forest in BigBOSS quasar spectra, achieves a FOM of 395 with Planck plus Stage III priors. This FOM is based on conservative assumptions for the analysis of broad band power (kmax = 0.15), and could grow to over 600 if current work allows us to push the analysis to higher wave numbers (kmax = 0.3). BigBOSS will also place constraints on theories of modified gravity and inflation, and will measure the sum of neutrino masses to 0.024 eV accuracy., Comment: This report is based on the BigBOSS proposal submission to NOAO in October 2010, and reflects the project status at that time with minor updates
Published: 2011

38. A Spectroscopic and Photometric Survey of Novae in M31

Author: Shafter, A. W., Darnley, M. J., Hornoch, K., Filippenko, A. V., Bode, M. F., Ciardullo, R., Misselt, K. A., Hounsell, R. A., Chornock, R., and Matheson, T.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report the results of a multi-year spectroscopic and photometric survey of novae in M31 that resulted in a total of 53 spectra of 48 individual nova candidates. Two of these, M31N 1995-11e and M31N 2007-11g, were revealed to be long-period Mira variables, not novae. These data double the number of spectra extant for novae in M31 through the end of 2009 and bring to 91 the number of M31 novae with known spectroscopic classifications. We find that 75 novae (82%) are confirmed or likely members of the Fe II spectroscopic class, with the remaining 16 novae (18%) belonging to the He/N (and related) classes. These numbers are consistent with those found for Galactic novae. We find no compelling evidence that spectroscopic class depends sensitively on spatial position or population within M31 (i.e., bulge vs. disk), although the distribution for He/N systems appears slightly more extended than that for the Fe II class. We confirm the existence of a correlation between speed class and ejection velocity (based on line width), as in the case of Galactic novae. Follow-up photometry allowed us to determine light-curve parameters for a total of 47 of the 91 novae with known spectroscopic class. We confirm that more luminous novae generally fade the fastest, and that He/N novae are typically faster and brighter than their Fe II counterparts. In addition, we find a weak dependence of nova speed class on position in M31, with the spatial distribution of the fastest novae being slightly more extended than that of slower novae., Comment: Accepted for publication in the Astrophysical Journal. The manuscript is 123 pages with 29 figures
Published: 2011
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39. Direct Confirmation of the Asymmetry of the Cas A Supernova with Light Echoes

Author: Rest, A., Foley, R. J., Sinnott, B., Welch, D. L., Badenes, C., Filippenko, A. V., Bergmann, M., Bhatti, W. A., Blondin, S., Challis, P., Damke, G., Finley, H., Huber, M. E., Kasen, D., Kirshner, R. P., Matheson, T., Mazzali, P., Minniti, D., Nakajima, R., Narayan, G., Olsen, K., Sauer, D., Smith, R. C., and Suntzeff, N. B.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We report the first detection of asymmetry in a supernova (SN) photosphere based on SN light echo (LE) spectra of Cas A from the different perspectives of dust concentrations on its LE ellipsoid. New LEs are reported based on difference images, and optical spectra of these LEs are analyzed and compared. After properly accounting for the effects of finite dust-filament extent and inclination, we find one field where the He I and H alpha features are blueshifted by an additional ~4000 km/s relative to other spectra and to the spectra of the Type IIb SN 1993J. That same direction does not show any shift relative to other Cas A LE spectra in the Ca II near-infrared triplet feature. We compare the perspectives of the Cas A LE dust concentrations with recent three-dimensional modeling of the SN remnant (SNR) and note that the location having the blueshifted He I and H alpha features is roughly in the direction of an Fe-rich outflow and in the opposite direction of the motion of the compact object at the center of the SNR. We conclude that Cas A was an intrinsically asymmetric SN. Future LE spectroscopy of this object, and of other historical SNe, will provide additional insight into the connection of explosion mechanism to SN to SNR, as well as give crucial observational evidence regarding how stars explode., Comment: 13 pages, 7 figures, accepted for publication in ApJ
Published: 2010
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40. Characteristic velocities of stripped-envelope core-collapse supernova cores

Author: Maurer, I., Mazzali, P. A., Deng, J., Filippenko, A. V., Hamuy, M., Kirshner, R. P., Matheson, T., Modjaz, M., Pian, E., Stritzinger, M., Taubenberger, S., and Valenti, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The velocity of the inner ejecta of stripped-envelope core-collapse supernovae (CC-SNe) is studied by means of an analysis of their nebular spectra. Stripped-envelope CC-SNe are the result of the explosion of bare cores of massive stars ($\geq 8$ M$_{\odot}$), and their late-time spectra are typically dominated by a strong [O {\sc i}] $\lambda\lambda$6300, 6363 emission line produced by the innermost, slow-moving ejecta which are not visible at earlier times as they are located below the photosphere. A characteristic velocity of the inner ejecta is obtained for a sample of 56 stripped-envelope CC-SNe of different spectral types (IIb, Ib, Ic) using direct measurements of the line width as well as spectral fitting. For most SNe, this value shows a small scatter around 4500 km s$^{-1}$. Observations ($< 100$ days) of stripped-envelope CC-SNe have revealed a subclass of very energetic SNe, termed broad-lined SNe (BL-SNe) or hypernovae, which are characterised by broad absorption lines in the early-time spectra, indicative of outer ejecta moving at very high velocity ($v \geq 0.1 c$). SNe identified as BL in the early phase show large variations of core velocities at late phases, with some having much higher and some having similar velocities with respect to regular CC-SNe. This might indicate asphericity of the inner ejecta of BL-SNe, a possibility we investigate using synthetic three-dimensional nebular spectra., Comment: 14 pages, 10 figures, MNRAS accepted
Published: 2009
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41. Pushing the Boundaries of Conventional Core-Collapse Supernovae: The Extremely Energetic Supernova SN 2003ma

Author: Rest, A., Foley, R. J., Gezari, S., Narayan, G., Draine, B., Olsen, K., Huber, M., Matheson, T., Garg, A., Welch, D. L., Becker, A. C., Challis, P., Clocchiatti, A., Cook, K. H., Damke, G., Meixner, M., Miknaitis, G., Minniti, D., Morelli, L., Nikolaev, S., Pignata, G., Prieto, J. L., Smith, R. C., Stubbs, C., Suntzeff, N. B., Walker, A. R., Wood-Vasey, W. M., Zenteno, A., Wyrzykowski, L., Udalski, A., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Szewczyk, O., Ulaczyk, K., and Poleski, R.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We report the discovery of a supernova (SN) with the highest apparent energy output to date and conclude that it represents an extreme example of the Type IIn subclass. The SN, which was discovered behind the Large Magellanic Cloud at z = 0.289 by the SuperMACHO microlensing survey, peaked at M_R = -21.5 mag and only declined by 2.9 mag over 4.7 years after the peak. Over this period, SN 2003ma had an integrated bolometric luminosity of 4 x 10^51 ergs, more than any other SN to date. The radiated energy is close to the limit allowed by conventional core-collapse explosions. Optical spectra reveal that SN 2003ma has persistent single-peaked intermediate-width hydrogen lines, a signature of interaction between the SN and a dense circumstellar medium. The light curves show further evidence for circumstellar interaction, including a long plateau with a shape very similar to the classic SN IIn 1988Z -- however, SN 2003ma is ten times more luminous at all epochs. The fast velocity measured for the intermediate-width H_alpha component (~6000 km/s) points towards an extremely energetic explosion (> 10^52 ergs), which imparts a faster blast-wave speed to the post-shock material and a higher luminosity from the interaction than is observed in typical SNe IIn. Mid-infrared observations of SN 2003ma suggest an infrared light echo is produced by normal interstellar dust at a distance ~0.5 pc from the SN., Comment: 21 pages, 15 figures, accepted for publication in ApJ
Published: 2009
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42. Distance determination to 12 Type II-P Supernovae using the Expanding Photosphere Method

Author: Jones, M. I., Hamuy, M., Lira, P., Maza, J., Clocchiatti, A., Phillips, M., Morrell, N., Roth, M., Suntzeff, N. B., Matheson, T., Filippenko, A. V., Foley, R. J., and Leonard, D. C.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We use early-time photometry and spectroscopy of 12 Type II plateau supernovae (SNe IIP) to derive their distances using the expanding photosphere method (EPM). We perform this study using two sets of Type II supernova (SN II) atmosphere models, three filter subsets ($\{BV\}$, $\{BVI\}$, $\{VI\}$), and two methods for the host-galaxy extinction, which leads to 12 Hubble diagrams. We find that systematic differences in the atmosphere models lead to $\sim $50% differences in the EPM distances and to a value of ${\rm H_0}$ between 52 and 101 ${\rm km s^{-1} Mpc^{-1}}$. Using the $\{VI\}$ filter subset we obtain the lowest dispersion in the Hubble diagram, {${\rm \sigma_{\mu} = 0.32}$ mag}. We also apply the EPM analysis to the well-observed SN IIP 1999em. With the $\{VI\}$ filter subset we derive a distance ranging from 9.3 $\pm$ 0.5 Mpc to 13.9 $\pm$ 1.4 Mpc depending on the atmosphere model employed., Comment: Accepted for publication in the Astrophysical Journal
Published: 2009
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43. Type Ia supernova science 2010-2020

Author: Howell, D. A., Conley, A., Della Valle, M., Nugent, P. E., Perlmutter, S., Marion, G. H., Krisciunas, K., Badenes, C., Mazzali, P., Aldering, G., Antilogus, P., Baron, E., Becker, A., Baltay, C., Benetti, S., Blondin, S., Branch, D., Brown, E. F., Deustua, S., Ealet, A., Ellis, R. S., Fouchez, D., Freedman, W., Gal-Yam, A., Jha, S., Kasen, D., Kessler, R., Kim, A. G., Leonard, D. C., Li, W., Livio, M., Maoz, D., Mannucci, F., Matheson, T., Neill, J. D., Nomoto, K., Panagia, N., Perrett, K., Phillips, M., Poznanski, D., Quimby, R., Rest, A., Riess, A., Sako, M., Soderberg, A. M., Strolger, L., Thomas, R., Turatto, M., van Dyk, S., and Wood-Vasey, W. M.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: In the next decade Type Ia supernovae (SNe Ia) will be used to test theories predicting changes in the Dark Energy equation of state with time. Ultimately this requires a dedicated space mission like JDEM. SNe Ia are mature cosmological probes --- their limitations are well characterized, and a path to improvement is clear. Dominant systematic errors include photometric calibration, selection effects, reddening, and population-dependent differences. Building on past lessons, well-controlled new surveys are poised to make strides in these areas: the Palomar Transient Factory, Skymapper, La Silla QUEST, Pan-STARRS, the Dark Energy Survey, LSST, and JDEM. They will obviate historical calibrations and selection biases, and allow comparisons via large subsamples. Some systematics follow from our ignorance of SN Ia progenitors, which there is hope of determining with SN Ia rate studies from 0
Published: 2009

44. Type Ia supernova rate measurements to redshift 2.5 from candels: Searching for prompt explosions in the early universe

Author: Rodney, SA, Riess, AG, Strolger, LG, Dahlen, T, Graur, O, Casertano, S, Dickinson, ME, Ferguson, HC, Garnavich, P, Hayden, B, Jha, SW, Jones, DO, Kirshner, RP, Koekemoer, AM, McCully, C, Mobasher, B, Patel, B, Weiner, BJ, Cenko, SB, Clubb, KI, Cooper, M, Filippenko, AV, Frederiksen, TF, Hjorth, J, Leibundgut, B, Matheson, T, Nayyeri, H, Penner, K, Trump, J, Silverman, JM, U, V, Azalee Bostroem, K, Challis, P, Rajan, A, Wolff, S, Faber, SM, Grogin, NA, and Kocevski, D
Subjects: infrared: general, supernovae: general, surveys, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) was a multi-cycle treasury program on the Hubble Space Telescope (HST) that surveyed a total area of ∼0.25 deg2 with ∼900 HST orbits spread across five fields over three years. Within these survey images we discovered 65 supernovae (SNe) of all types, out to z ∼ 2.5. We classify ∼24 of these as Type Ia SNe (SNe Ia) based on host galaxy redshifts and SN photometry (supplemented by grism spectroscopy of six SNe). Here we present a measurement of the volumetric SN Ia rate as a function of redshift, reaching for the first time beyond z = 2 and putting new constraints on SN Ia progenitor models. Our highest redshift bin includes detections of SNe that exploded when the universe was only ∼3 Gyr old and near the peak of the cosmic star formation history. This gives the CANDELS high redshift sample unique leverage for evaluating the fraction of SNe Ia that explode promptly after formation ( 40 Myr. However, mild tension is apparent between ground-based low-z surveys and space-based high-z surveys. In both CANDELS and the sister HST program CLASH (Cluster Lensing And Supernova Survey with Hubble), we find a low rate of SNe Ia at z > 1. This could be a hint that prompt progenitors are in fact relatively rare, accounting for only 20% of all SN Ia explosions - though further analysis and larger samples will be needed to examine that suggestion. © 2014. The American Astronomical Society. All rights reserved.
Published: 2014

45. Spectroscopy of High-Redshift Supernovae from the ESSENCE Project: The First Four Years

Author: Foley, R. J., Matheson, T., Blondin, S., Chornock, R., Silverman, J. M., Challis, P., Clocchiatti, A., Filippenko, A. V., Kirshner, R. P., Leibundgut, B., Sollerman, J., Spyromilio, J., Tonry, J. L., Davis, T. M., Garnavich, P. M., Jha, S. W., Krisciunas, K., Li, W., Pignata, G., Rest, A., Riess, A. G., Schmidt, B. P., Smith, R. C., Stubbs, C. W., Tucker, B. E., and Wood-Vasey, W. M.
Subjects: Astrophysics
Abstract: We present the results of spectroscopic observations from the ESSENCE high-redshift supernova (SN) survey during its first four years of operation. This sample includes spectra of all SNe Ia whose light curves were presented by Miknaitis et al. (2007) and used in the cosmological analyses of Davis et al. (2007) and Wood-Vasey et al. (2007). The sample represents 273 hours of spectroscopic observations with 6.5 - 10-m-class telescopes of objects detected and selected for spectroscopy by the ESSENCE team. We present 174 spectra of 156 objects. Combining this sample with that of Matheson et al. (2005), we have a total sample of 329 spectra of 274 objects. From this, we are able to spectroscopically classify 118 Type Ia SNe. As the survey has matured, the efficiency of classifying SNe Ia has remained constant while we have observed both higher-redshift SNe Ia and SNe Ia farther from maximum brightness. Examining the subsample of SNe Ia with host-galaxy redshifts shows that redshifts derived from only the SN Ia spectra are consistent with redshifts found from host-galaxy spectra. Moreover, the phases derived from only the SN Ia spectra are consistent with those derived from light-curve fits. By comparing our spectra to local templates, we find that the rate of objects similar to the overluminous SN 1991T and the underluminous SN 1991bg in our sample are consistent with that of the local sample. We do note, however, that we detect no object spectroscopically or photometrically similar to SN 1991bg. Although systematic effects could reduce the high-redshift rate we expect based on the low-redshift surveys, it is possible that SN 1991bg-like SNe Ia are less prevalent at high redshift., Comment: 21 pages, 17 figures, accepted to AJ
Published: 2008
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46. A Second Case of Variable Na I D Lines in a Highly-Reddened Type Ia Supernova (with Erratum)

Author: Blondin, S., Prieto, J. L., Patat, F., Challis, P., Hicken, M., Kirshner, R. P., Matheson, T., and Modjaz, M.
Subjects: Astrophysics
Abstract: (Original) Recent high-resolution spectra of the Type Ia SN 2006X have revealed the presence of time-variable and blueshifted Na I D features, interpreted by Patat et al. as originating in circumstellar material within the progenitor system. The variation seen in SN 2006X induces relatively large changes in the total Na I D equivalent width ($\Delta\rm{EW}\approx 0.5 \unicode{x212B}$ in just over two weeks), that would be detectable at lower resolutions. We have used a large data set comprising 2400 low-resolution spectra of 450 Type Ia supernovae (SNe Ia) obtained by the CfA Supernova Program to search for variable Na I D features. Out of the 31 SNe Ia (including SN 2006X) in which we could have detected similar EW variations, only one other (SN 1999cl) shows variable Na I D features, with an even larger change over a similar ~10-day timescale ($\Delta\rm{EW} = 1.66 \pm 0.21 \unicode{x212B}$). Interestingly, both SN 1999cl and SN 2006X are the two most highly-reddened objects in our sample, raising the possibility that the variability is connected to dusty environments. (Erratum) The large variation in the Na I D equivalent width observed in SN 1999cl results in fact from a measurement error. Our new measurements show that the EW variation is significantly lower, at $0.43 \pm 0.14 \unicode{x212B}$. While the EW variation remains statistically significant (3.1$\sigma$ different from zero), it is now below the detection threshold of 0.5 $\unicode{x212B}$ derived from the Monte Carlo simulations published in the original paper. As a result, SN 1999cl should no longer be considered as an object displaying variable Na I D lines in our study. The fraction of SNe Ia in our sample displaying Na I D lines thus goes from $\sim$6% (2/31) in the original study to $\sim$3% (1/31) in the revised analysis, SN 2006X being the only SN Ia in our sample with variable Na I D lines., Comment: 10 pages, 5 figures (original paper); 6 pages, 6 figures (Erratum). ApJ, accepted
Published: 2008
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47. GALEX Spectroscopy of SN 2005ay suggests a UV spectral uniformity among type II-P supernovae

Author: Gal-Yam, A., Bufano, F., Barlow, T., Baron, E., Benetti, S., Cappellaro, E., Challis, P. J., Ellis, R. S., Filippenko, A. V., Foley, R. J., Fox, D. B., Hicken, M., Kirshner, R. P., Leonard, D. C., Li, W., Maoz, D., Matheson, T., Mazzali, P. A., Modjaz, M., Nomoto, K., Ofek, E. O., Simon, J., Small, T., Smith, G. P., Turatto, M., Van Dyk, S. D., and Zampieri, L.
Subjects: Astrophysics
Abstract: We present the first results from our GALEX program designed to obtain ultraviolet (UV) spectroscopy of nearby core-collapse supernovae (SNe). Our first target, SN 2005ay in the nearby galaxy NGC 3938, is a typical member of the II-P SN subclass. Our spectra show remarkable similarity to those of the prototypical type II-P event SN 1999em, and resemble also Swift observations of the recent type II-P event SN 2005cs. Taken together, the observations of these three events trace the UV spectral evolution of SNe II-P during the first month after explosion, as required in order to interpret optical observations of high-redshift SNe II-P, and to derive cross-filter K-corrections. While still highly preliminary, the apparent UV homogeneity of SNe II-P bodes well for the use of these events as cosmological probes at high redshift., Comment: ApJL, submitted, comments welcome
Published: 2008
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48. Exploring the Outer Solar System with the ESSENCE Supernova Survey

Author: Becker, A. C., Arraki, K., Kaib, N. A., Wood-Vasey, W. M., Aguilera, C., Blackman, J. W., Blondin, S., Challis, P., Clocchiatti, A., Covarrubias, R., Damke, G., Davis, T. M., Filippenko, A. V., Foley, R. J., Garg, A., Garnavich, P. M., Hicken, M., Jha, S., Kirshner, R. P., Krisciunas, K., Leibundgut, B., Li, W., Matheson, T., Miceli, A., Miknaitis, G., Narayan, G., Pignata, G., Prieto, J. L., Rest, A., Riess, A. G., Salvo, M. E., Schmidt, B. P., Smith, R. C., Sollerman, J., Spyromilio, J., Stubbs, C. W., Suntzeff, N. B., Tonry, J. L., and Zenteno, A.
Subjects: Astrophysics
Abstract: We report the discovery and orbit determination of 14 trans-Neptunian objects (TNOs) from the ESSENCE Supernova Survey difference imaging dataset. Two additional objects discovered in a similar search of the SDSS-II Supernova Survey database were recovered in this effort. ESSENCE repeatedly observed fields far from the Solar System ecliptic (-21 deg < beta < -5 deg), reaching limiting magnitudes per observation of I~23.1 and R~23.7. We examine several of the newly detected objects in detail, including 2003 UC_414 which orbits entirely between Uranus and Neptune and lies very close to a dynamical region that would make it stable for the lifetime of the Solar System. 2003 SS_422 and 2007 TA_418 have high eccentricities and large perihelia, making them candidate members of an outer class of trans-Neptunian objects. We also report a new member of the ''extended'' or ''detached'' scattered disk, 2004 VN_112, and verify the stability of its orbit using numerical simulations. This object would have been visible to ESSENCE for only ~2% of its orbit, suggesting a vast number of similar objects across the sky. We emphasize that off-ecliptic surveys are optimal for uncovering the diversity of such objects, which in turn will constrain the history of gravitational influences that shaped our early Solar System., Comment: 5 pages, 1 table, accepted for publication in ApJL
Published: 2008
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49. Scattered-Light Echoes from the Historical Galactic Supernovae Cassiopeia A and Tycho (SN 1572)

Author: Rest, A., Welch, D. L., Suntzeff, N. B., Oaster, L., Lanning, H., Olsen, K., Smith, R. C., Becker, A. C., Bergmann, M., Challis, P., Clocchiatti, A., Cook, K. H., Damke, G., Garg, A., Huber, M. E., Matheson, T., Minniti, D., Prieto, J. L., and Wood-Vasey, W. M.
Subjects: Astrophysics
Abstract: We report the discovery of an extensive system of scattered light echo arclets associated with the recent supernovae in the local neighbourhood of the Milky Way: Tycho (SN 1572) and Cassiopeia A. Existing work suggests that the Tycho SN was a thermonuclear explosion while the Cas A supernova was a core collapse explosion. Precise classifications according to modern nomenclature require spectra of the outburst light. In the case of ancient SNe, this can only be done with spectroscopy of their light echo, where the discovery of the light echoes from the outburst light is the first step. Adjacent light echo positions suggest that Cas A and Tycho may share common scattering dust structures. If so, it is possible to measure precise distances between historical Galactic supernovae. On-going surveys that alert on the development of bright scattered-light echo features have the potential to reveal detailed spectroscopic information for many recent Galactic supernovae, both directly visible and obscured by dust in the Galactic plane., Comment: 4 pages, 4 color figures, accepted for publication in ApJL
Published: 2008
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50. Time Dilation in Type Ia Supernova Spectra at High Redshift

Author: Blondin, S., Davis, T. M., Krisciunas, K., Schmidt, B. P., Sollerman, J., Wood-Vasey, W. M., Becker, A. C., Challis, P., Clocchiatti, A., Damke, G., Filippenko, A. V., Foley, R. J., Garnavich, P. M., Jha, S. W., Kirshner, R. P., Leibundgut, B., Li, W., Matheson, T., Miknaitis, G., Narayan, G., Pignata, G., Rest, A., Riess, A. G., Silverman, J. M., Smith, R. C., Spyromilio, J., Stritzinger, M., Stubbs, C. W., Suntzeff, N. B., Tonry, J. L., Tucker, B. E., and Zenteno, A.
Subjects: Astrophysics
Abstract: We present multiepoch spectra of 13 high-redshift Type Ia supernovae (SNe Ia) drawn from the literature, the ESSENCE and SNLS projects, and our own separate dedicated program on the ESO Very Large Telescope. We use the Supernova Identification (SNID) code of Blondin & Tonry to determine the spectral ages in the supernova rest frame. Comparison with the observed elapsed time yields an apparent aging rate consistent with the 1/(1+z) factor (where z is the redshift) expected in a homogeneous, isotropic, expanding universe. These measurements thus confirm the expansion hypothesis, while unambiguously excluding models that predict no time dilation, such as Zwicky's "tired light" hypothesis. We also test for power-law dependencies of the aging rate on redshift. The best-fit exponent for these models is consistent with the expected 1/(1+z) factor., Comment: 14 pages (emulateapj), 10 figures; accepted for publication in ApJ. Version with full-resolution figures available at http://www.cfa.harvard.edu/~sblondin/publications/timedilation/
Published: 2008
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