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45 results on '"Ahumada, T."'

1. Extragalactic fast X-ray transient from a weak relativistic jet associated with a Type Ic-BL supernova

Author

Sun, H., Li, W. -X., Liu, L. -D., Gao, H., Wang, X. -F., Yuan, W., Zhang, B., Filippenko, A. V., Xu, D., An, T., Ai, S., Brink, T. G., Liu, Y., Liu, Y. -Q., Wang, C. -Y., Wu, Q. -Y., Wu, X. -F., Yang, Y., Zhang, B. -B., Zheng, W. -K., Ahumada, T., Dai, Z. -G., Delaunay, J., Elias-Rosa, N., Benetti, S., Fu, S. -Y., Howell, D. A., Huang, Y. -F., Kasliwal, M. M., Karambelkar, V., Stein, R., Lei, W. -H., Lian, T. -Y., Peng, Z. -K., Ridnaia, A. V., Svinkin, D. S., Wang, X. -Y., Wang, A. -L., Wei, D. -M., An, J., Andrews, M., Bai, J. -M, Dai, C. -Y., Ehgamberdiev, S. A., Fan, Z., Farah, J., Feng, H. -C., Fynbo, J. P. U., Guo, W. -J., Guo, Z., Hu, M. -K., Hu, J. -W., Jiang, S. -Q., Jin, J. -J., Li, A., Li, J. -D., Li, R. -Z., Liang, Y. -F., Ling, Z. -X., Liu, X., Mao, J. -R., McCully, C., Mirzaqulov, D., Newsome, M., Gonzalez, E. Padilla, Pan, X., Terreran, G., Tinyanont, S., Wang, B. -T., Wang, L. -Z., Wen, X. -D., Xiang, D. -F., Xue, S. -J., Yang, J., Zhu, Z. -P., Cai, Z. -M., Castro-Tirado, A. J., Chen, F. -S., Chen, H. -L., Chen, T. -X., Chen, W., Chen, Y. -H., Chen, Y. -F., Chen, Y., Cheng, H. -Q., Cordier, B., Cui, C. -Z., Cui, W. -W., Dai, Y. -F., Fan, D. -W., Feng, H., Guan, J., Han, D. -W., Hou, D. -J., Hu, H. -B., Huang, M. -H., Huo, J., Jia, S. -M., Jia, Z. -Q., Jiang, B. -W., Jin, C. -C., Jin, G., Kuulkers, E., Li, C. -K., Li, D. -Y., Li, J. -F., Li, L. -H., Li, M. -S., Li, W., Li, Z. -D., Liu, C. -Z, Liu, H. -Y., Liu, H. -Q., Liu, M. -J., Lu, F. -J., Luo, L. -D., Ma, J., Mao, X., Nandra, K., O'Brien, P., Pan, H. -W., Rau, A., Rea, N., Sanders, J., Song, L. -M., Sun, S. -L., Sun, X. -J., Tan, Y. -Y., Tang, Q. -J., Tao, Y. -H., Wang, H., Wang, J., Wang, L., Wang, W. -X., Wang, Y. -L., Wang, Y. -S., Xiong, D. -R., Xu, H. -T., Xu, J. -J., Xu, X. -P., Xu, Y. -F., Xu, Z., Xue, C. -B., Xue, Y. -L., Yan, A. -L., Yang, H. -N., Yang, X. -T., Yang, Y. -J., Zhang, C., Zhang, J., Zhang, M., Zhang, S. -N., Zhang, W. -D., Zhang, W. -J., Zhang, Y. -H., Zhang, Z., Zhang, Z. -L., Zhao, D. -H., Zhao, H. -S., Zhao, X. -F., Zhao, Z. -J., Zhou, Y. -L., Zhu, Y. -X., and Zhu, Z. -C.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Massive stars end their life as core-collapse supernovae, amongst which some extremes are Type Ic broad-lined supernovae associated with long-duration gamma-ray bursts (LGRBs) having powerful relativistic jets. Their less-extreme brethren make unsuccessful jets that are choked inside the stars, appearing as X-ray flashes or low-luminosity GRBs. On the other hand, there exists a population of extragalactic fast X-ray transients (EFXTs) with timescales ranging from seconds to thousands of seconds, whose origins remain obscure. Known sources that contribute to the observed EFXT population include the softer analogs of LGRBs, shock breakouts of supernovae, or unsuccessful jets. Here, we report the discovery of the bright X-ray transient EP240414a detected by the Einstein Probe (EP), which is associated with the Type Ic supernova SN 2024gsa at a redshift of 0.401. The X-ray emission evolution is characterised by a very soft energy spectrum peaking at < 1.3 keV, which makes it distinct from known LGRBs, X-ray flashes, or low-luminosity GRBs. Follow-up observations at optical and radio bands revealed the existence of a weak relativistic jet that interacts with an extended shell surrounding the progenitor star. Located on the outskirts of a massive galaxy, this event reveals a new population of explosions of Wolf-Rayet stars characterised by a less powerful engine that drives a successful but weak jet, possibly owing to a progenitor star with a smaller core angular momentum than in traditional LGRB progenitors., Comment: 43 pages, 9 figures, 4 tables, submitted. Comments are welcome

Published
2024

2. The Palomar twilight survey of 'Ayl\'o'chaxnim, Atiras, and comets

Author

Bolin, B. T., Masci, F. J., Coughlin, M. W., Duev, D. A., Ivezić, Ž., Jones, R. L., Yoachim, P., Ahumada, T., Bhalerao, V., Choudhary, H., Contreras, C., Cheng, Y. -C., Copperwheat, C. M., Deshmukh, K., Fremling, C., Granvik, M., Hardegree-Ullman, K. K., Ho, A. Y. Q., Jedicke, R., Kasliwal, M., Kumar, H., Lin, Z. -Y., Mahabal, A., Monson, A., Neill, J. D., Nesvorný, D., Perley, D. A., Purdum, J. N., Quimby, R., Serabyn, E., Sharma, K., and Swain, V.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Computer Science - Artificial Intelligence, Computer Science - Machine Learning
Abstract

Near-sun sky twilight observations allow for the detection of asteroid interior to the orbit of Venus (Aylos), the Earth (Atiras), and comets. We present the results of observations with the Palomar 48-inch telescope (P48)/Zwicky Transient Facility (ZTF) camera in 30 s r-band exposures taken during evening astronomical twilight from 2019 Sep 20 to 2022 March 7 and during morning astronomical twilight sky from 2019 Sep 21 to 2022 Sep 29. More than 46,000 exposures were taken in evening and morning astronomical twilight within 31 to 66 degrees from the Sun with an r-band limiting magnitude between 18.1 and 20.9. The twilight pointings show a slight seasonal dependence in limiting magnitude and ability to point closer towards the Sun, with limiting magnitude slightly improving during summer. In total, the one Aylo, (594913) 'Ayl\'o'chaxnim, and 4 Atiras, 2020 OV1, 2021 BS1, 2021 PB2, and 2021 VR3, were discovered in evening and morning twilight observations. Additional twilight survey discoveries also include 6 long-period comets: C/2020 T2, C/2020 V2, C/2021 D2, C/2021 E3, C/2022 E3, and C/2022 P3, and two short-period comets: P/2021 N1 and P/2022 P2 using deep learning comet detection pipelines. The P48/ZTF twilight survey also recovered 11 known Atiras, one Aylo, three short-period comes, two long-period comets, and one interstellar object. Lastly, the Vera Rubin Observatory will conduct a twilight survey starting in its first year of operations and will cover the sky within 45 degrees of the Sun. Twilight surveys such as those by ZTF and future surveys will provide opportunities for discovering asteroids inside the orbits of Earth and Venus., Comment: 26 pages, 13 figures, 4 tables, accepted for publication in Icarus

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. Multi-band analyses of the bright GRB 230812B and the associated SN2023pel

Author

Hussenot-Desenonges, T., Wouters, T., Guessoum, N., Abdi, I., Abulwfa, A., Adami, C., Fernández, J. F. Agüí, Ahumada, T., Aivazyan, V., Akl, D., Anand, S., Andrade, C. M., Antier, S., Ata, S. A., D'Avanzo, P., Azzam, Y. A., Baransky, A., Basa, S., Blazek, M., Bendjoya, P., Beradze, S., Boumis, P., Bremer, M., Brivio, R., Buat, V., Bulla, M., Burkhonov, O., Burns, E., Cenko, S. B., Corradi, W., Coughlin, M. W., Daigne, F., Dietrich, T., Dornic, D., Ducoin, J. -G., Duverne, P. -A., Elhosseiny, E. G., Elnagahy, F. I., El-Sadek, M. A., Ferro, M., Floc'h, E. Le, Freeberg, M., Fynbo, J. P. U., Götz, D., Gurbanov, E., Hamed, G. M., Hasanov, E., Healy, B. F., Heintz, K. E., Hello, P., Inasaridze, R., Iskandar, A., Ismailov, N., Izzo, L., Jhawar, S., Laz, T. Jegou du, Kamel, T. M., Karpov, S., Klotz, A., Koulouridis, E., Kuin, N. P., Kochiashvili, N., Leonini, S., Lu, K. -X., Malesani, D. B., Masek, M., Mao, J., Melandri, A., Mihov, B. M., Natsvlishvili, R., Navarete, F., Nedora, V., Nicolas, J., Odeh, M., Palmerio, J., Pang, P. T. H., De Pasquale, M., Peng, H. W., Pormente, S., Peloton, J., Pradier, T., Pyshna, O., Rajabov, Y., Rakotondrainibe, N. A., Rivet, J. -P., Rousselot, L., Saccardi, A., Sasaki, N., Schneider, B., Serrau, M., Shokry, A., Slavcheva-Mihova, L., Simon, A., Sokoliuk, O., Srinivasaragavan, G., Strausbaugh, R., Tanvir, N. R., Takey, A., Thöne, C. C., Tillayev, Y., Melo, I. Tosta e, Turpin, D., Postigo, A. de Ugarte, Vasylenko, V., Vergani, S. D., Vidadi, Z., Xu, D., Wang, L. T., Wang, X. F., Winters, J. M., Zhang, X -L., and Zhu, Z.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

GRB~230812B is a bright and relatively nearby ($z =0.36$) long gamma-ray burst (GRB) that has generated significant interest in the community and has thus been observed over the entire electromagnetic spectrum. We report over 80 observations in X-ray, ultraviolet, optical, infrared, and sub-millimeter bands from the GRANDMA (Global Rapid Advanced Network for Multi-messenger Addicts) network of observatories and from observational partners. Adding complementary data from the literature, we then derive essential physical parameters associated with the ejecta and external properties (i.e. the geometry and environment) of the GRB and compare with other analyses of this event. We spectroscopically confirm the presence of an associated supernova, SN2023pel, and we derive a photospheric expansion velocity of v $\sim$ 17$\times10^3$ km s$^{-1}$. We analyze the photometric data first using empirical fits of the flux and then with full Bayesian Inference. We again strongly establish the presence of a supernova in the data, with a maximum (pseudo-)bolometric luminosity of $5.75 \times 10^{42}$ erg/s, at $15.76^{+0.81}_{-1.21}$ days (in the observer frame) after the trigger, with a half-max time width of 22.0 days. We compare these values with those of SN1998bw, SN2006aj, and SN2013dx. Our best-fit model favours a very low density environment ($\log_{10}({n_{\rm ISM}/{\rm cm}^{-3}}) = -2.38^{+1.45}_{-1.60}$) and small values for the jet's core angle $\theta_{\rm core} = 1.54^{+1.02}_{-0.81} \ \rm{deg}$ and viewing angle $\theta_{\rm obs} = 0.76^{+1.29}_{-0.76} \ \rm{deg}$. GRB 230812B is thus one of the best observed afterglows with a distinctive supernova bump.

Published
2023

5. The Palomar twilight survey of ‘Ayló’chaxnim, Atiras, and comets

Author

Bolin, B.T., Masci, F.J., Coughlin, M.W., Duev, D.A., Ivezić, Ž., Jones, R.L., Yoachim, P., Ahumada, T., Bhalerao, V., Choudhary, H., Contreras, C., Cheng, Y.-C., Copperwheat, C.M., Deshmukh, K., Fremling, C., Granvik, M., Hardegree-Ullman, K.K., Ho, A.Y.Q., Jedicke, R., Kasliwal, M., Kumar, H., Lin, Z.-Y., Mahabal, A., Monson, A., Neill, J.D., Nesvorný, D., Perley, D.A., Purdum, J.N., Quimby, R., Serabyn, E., Sharma, K., and Swain, V.

Published
2025
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6. The discovery and characterization of a kilometre sized asteroid inside the orbit of Venus

Author

Bolin, Bryce T., Ahumada, T., van Dokkum, P., Fremling, C., Granvik, M., Hardegree-Ullman, K. K., Harikane, Y., Purdum, J. N., Serabyn, E., Southworth, J., and Zhai, C.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Near-Earth asteroid population models predict the existence of bodies located inside the orbit of Venus. Despite searches up to the end of 2019, none had been found. We report discovery and follow-up observations of (594913) 'Ayl\'o'chaxnim, an asteroid with an orbit entirely interior to Venus. (594913) 'Ayl\'o'chaxnim has an aphelion distance of ~0.65 au, is ~2 km in diameter and is red in colour. The detection of such a large asteroid inside the orbit of Venus is surprising given their rarity according to near-Earth asteroid population models. As the first officially numbered and named asteroid located entirely within the orbit of Venus, we propose that the class of interior to Venus asteroids be referred to as 'Ayl\'o'chaxnim asteroids., Comment: 7 pages, 8 figures, 1 table. Published in Monthly Notices of the Royal Astronomical Society: Letters (2022). arXiv admin note: text overlap with arXiv:2009.04125

Published
2022
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7. Preliminary estimates of the Zwicky Transient Facility 'Ayl\'o'chaxnim asteroid population completeness

Author

Bolin, B. T., Ahumada, T., van Dokkum, P., Fremling, C., Hardegree-Ullman, K. K., Purdum, J. N., Serabyn, E., and Southworth, J.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Near-Earth asteroids (NEAs) are organized into five main classes: Amor, Apollo, Aten, Atira and 'Ayl\'{o}'chaxnim. Asteroids belonging to the 'Ayl\'{o}'chaxnim class are located entirely within the orbit of Venus making them difficult to detect by ground-based observatories. The first-known asteroid of this class, (594913) 'Ayl\'{o}'chaxnim, was discovered by the Zwicky Transient Facility (ZTF) in 2020 January during a twilight search for asteroids at small solar elongations that ran between September 2019 and January 2020. Due to its large diameter of $\sim$2 km, the discovery of (594913) 'Ayl\'{o}'chaxnim is surprising because contemporary NEA population models predict a scarcity of asteroids of this size located inside the orbit of Venus. To compare the discovery of (594913) 'Ayl\'{o}'chaxnim by ZTF with the predictions of NEA population models, we estimated the ZTF survey completeness at detecting 'Ayl\'{o}'chaxnim asteroids and the number of 'Ayl\'{o}'chaxnim asteroids expected to have been discovered by simulating observations of synthetic 'Ayl\'{o}'chaxnim asteroids. We find that the 'Ayl\'{o}'chaxnim population completeness of the survey is $\sim$18$\%$ and there is only a 5$\%$ probability that a single 'Ayl\'{o}'chaxnim asteroid would have been discovered. Given the small chance for (594913) 'Ayl\'{o}'chaxnim to have been discovered, its presence is either a statistical fluke or it implies that asteroid population models may need to be revised., Comment: 9 pages, 2 figures. Accepted for publication in Icarus

Published
2020

8. Kilonova Luminosity Function Constraints Based on Zwicky Transient Facility Searches for 13 Neutron Star Merger Triggers during O3

Author

Kasliwal, MM, Anand, S, Ahumada, T, Stein, R, Carracedo, AS, Andreoni, I, Coughlin, MW, Singer, LP, Kool, EC, De, K, Kumar, H, Almualla, M, Yao, Y, Bulla, M, Dobie, D, Reusch, S, Perley, DA, Cenko, SB, Bhalerao, V, Kaplan, DL, Sollerman, J, Goobar, A, Copperwheat, CM, Bellm, EC, Anupama, GC, Corsi, A, Nissanke, S, Agudo, I, Bagdasaryan, A, Barway, S, Belicki, J, Bloom, JS, Bolin, B, Buckley, DAH, Burdge, KB, Burruss, R, Caballero-García, MD, Cannella, C, Castro-Tirado, AJ, Cook, DO, Cooke, J, Cunningham, V, Dahiwale, A, Deshmukh, K, Dichiara, S, Duev, DA, Dutta, A, Feeney, M, Franckowiak, A, Frederick, S, Fremling, C, Gal-Yam, A, Gatkine, P, Ghosh, S, Goldstein, DA, Golkhou, VZ, Graham, MJ, Graham, ML, Hankins, MJ, Helou, G, Hu, Y, Ip, WH, Jaodand, A, Karambelkar, V, Kong, AKH, Kowalski, M, Khandagale, M, Kulkarni, SR, Kumar, B, Laher, RR, Li, KL, Mahabal, A, Masci, FJ, Miller, AA, Mogotsi, M, Mohite, S, Mooley, K, Mroz, P, Newman, JA, Ngeow, CC, Oates, SR, Patil, AS, Pandey, SB, Pavana, M, Pian, E, Riddle, R, Sánchez-Ramírez, R, Sharma, Y, Singh, A, Smith, R, Soumagnac, MT, Taggart, K, Tan, H, Tzanidakis, A, Troja, E, Valeev, AF, Walters, R, Waratkar, G, Webb, S, and Yu, PC

Subjects
Neutron stars, Black holes, Gravitational waves, Nucleosynthesis, R-process, Compact objects, Spectroscopy, Sky surveys, Photometry, astro-ph.HE, astro-ph.IM, 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

We present a systematic search for optical counterparts to 13 gravitational wave (GW) triggers involving at least one neutron star during LIGO/Virgo's third observing run (O3). We searched binary neutron star (BNS) and neutron star black hole (NSBH) merger localizations with the Zwicky Transient Facility (ZTF) and undertook follow-up with the Global Relay of Observatories Watching Transients Happen (GROWTH) collaboration. The GW triggers had a median localization area of 4480 deg2, a median distance of 267 Mpc, and false-alarm rates ranging from 1.5 to 10-25 yr-1. The ZTF coverage in the g and r bands had a median enclosed probability of 39%, median depth of 20.8 mag, and median time lag between merger and the start of observations of 1.5 hr. The O3 follow-up by the GROWTH team comprised 340 UltraViolet/Optical/InfraRed (UVOIR) photometric points, 64 OIR spectra, and three radio images using 17 different telescopes. We find no promising kilonovae (radioactivity-powered counterparts), and we show how to convert the upper limits to constrain the underlying kilonova luminosity function. Initially, we assume that all GW triggers are bona fide astrophysical events regardless of false-alarm rate and that kilonovae accompanying BNS and NSBH mergers are drawn from a common population; later, we relax these assumptions. Assuming that all kilonovae are at least as luminous as the discovery magnitude of GW170817 (-16.1 mag), we calculate that our joint probability of detecting zero kilonovae is only 4.2%. If we assume that all kilonovae are brighter than-16.6 mag (the extrapolated peak magnitude of GW170817) and fade at a rate of 1 mag day-1 (similar to GW170817), the joint probability of zero detections is 7%. If we separate the NSBH and BNS populations based on the online classifications, the joint probability of zero detections, assuming all kilonovae are brighter than-16.6 mag, is 9.7% for NSBH and 7.9% for BNS mergers. Moreover, no more than 10-4, or φ > 30° to be consistent with our limits. We look forward to searches in the fourth GW observing run; even 17 neutron star mergers with only 50% coverage to a depth of-16 mag would constrain the maximum fraction of bright kilonovae to

Published
2020

9. GROWTH on S190814bv: Deep Synoptic Limits on the Optical/Near-infrared Counterpart to a Neutron Star-Black Hole Merger

Author

Andreoni, I, Goldstein, DA, Kasliwal, MM, Nugent, PE, Zhou, R, Newman, JA, Bulla, M, Foucart, F, Hotokezaka, K, Nakar, E, Nissanke, S, Raaijmakers, G, Bloom, JS, De, K, Jencson, JE, Ward, C, Ahumada, T, Anand, S, Buckley, DAH, Caballero-García, MD, Castro-Tirado, AJ, Copperwheat, CM, Coughlin, MW, Cenko, SB, Gromadzki, M, Hu, Y, Karambelkar, VR, Perley, DA, Sharma, Y, Valeev, AF, Cook, DO, Fremling, UC, Kumar, H, Taggart, K, Bagdasaryan, A, Cooke, J, Dahiwale, A, Dhawan, S, Dobie, D, Gatkine, P, Golkhou, VZ, Goobar, A, Chaves, AG, Hankins, M, Kaplan, DL, Kong, AKH, Kool, EC, Mohite, S, Sollerman, J, Tzanidakis, A, Webb, S, and Zhang, K

Subjects
astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Astronomy & Astrophysics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

On 2019 August 14, the Advanced LIGO and Virgo interferometers detected the high-significance gravitational wave (GW) signal S190814bv. The GW data indicated that the event resulted from a neutron star-black hole (NSBH) merger, or potentially a low-mass binary BH merger. Due to the low false-alarm rate and the precise localization (23 deg2 at 90%), S190814bv presented the community with the best opportunity yet to directly observe an optical/near-infrared counterpart to an NSBH merger. To search for potential counterparts, the GROWTH Collaboration performed real-time image subtraction on six nights of public Dark Energy Camera images acquired in the 3 weeks following the merger, covering >98% of the localization probability. Using a worldwide network of follow-up facilities, we systematically undertook spectroscopy and imaging of optical counterpart candidates. Combining these data with a photometric redshift catalog, we ruled out each candidate as the counterpart to S190814bv and placed deep, uniform limits on the optical emission associated with S190814bv. For the nearest consistent GW distance, radiative transfer simulations of NSBH mergers constrain the ejecta mass of S190814bv to be M ej < 0.04 M o˙ at polar viewing angles, or M ej < 0.03 M o˙ if the opacity is κ < 2 cm2g-1. Assuming a tidal deformability for the NS at the high end of the range compatible with GW170817 results, our limits would constrain the BH spin component aligned with the orbital momentum to be χ < 0.7 for mass ratios Q < 6, with weaker constraints for more compact NSs.

Published
2020

10. GROWTH on S190425z: Searching Thousands of Square Degrees to Identify an Optical or Infrared Counterpart to a Binary Neutron Star Merger with the Zwicky Transient Facility and Palomar Gattini-IR

Author

Coughlin, MW, Ahumada, T, Anand, S, De, K, Hankins, MJ, Kasliwal, MM, Singer, LP, Bellm, EC, Andreoni, I, Cenko, SB, Cooke, J, Copperwheat, CM, Dugas, AM, Jencson, JE, Perley, DA, Yu, PC, Bhalerao, V, Kumar, H, Bloom, JS, Anupama, GC, Ashley, MCB, Bagdasaryan, A, Biswas, R, Buckley, DAH, Burdge, KB, Cook, DO, Cromer, J, Cunningham, V, D'A, A, Dekany, RG, Delacroix, A, Dichiara, S, Duev, DA, Dutta, A, Feeney, M, Frederick, S, Gatkine, P, Ghosh, S, Goldstein, DA, Golkhou, VZ, Goobar, A, Graham, MJ, Hanayama, H, Horiuchi, T, Hung, T, Jha, SW, Kong, AKH, Giomi, M, Kaplan, DL, Karambelkar, VR, Kowalski, M, Kulkarni, SR, Kupfer, T, Masci, FJ, Mazzali, P, Moore, AM, Mogotsi, M, Neill, JD, Ngeow, CC, Martínez-Palomera, J, Parola, VL, Pavana, M, Ofek, EO, Patil, AS, Riddle, R, Rigault, M, Rusholme, B, Serabyn, E, Shupe, DL, Sharma, Y, Singh, A, Sollerman, J, Soon, J, Staats, K, Taggart, K, Tan, H, Travouillon, T, Troja, E, Waratkar, G, and Yatsu, Y

Subjects
Gravitational wave astronomy, Transient detection, Optical telescopes, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

The third observing run by LVC has brought the discovery of many compact binary coalescences. Following the detection of the first binary neutron star merger in this run (LIGO/Virgo S190425z), we performed a dedicated follow-up campaign with the Zwicky Transient Facility (ZTF) and Palomar Gattini-IR telescopes. The initial skymap of this single-detector gravitational wave (GW) trigger spanned most of the sky observable from Palomar Observatory. Covering 8000 deg2 of the initial skymap over the next two nights, corresponding to 46% integrated probability, ZTF system achieved a depth of ≈21 m AB in g-and r-bands. Palomar Gattini-IR covered 2200 square degrees in J-band to a depth of 15.5 mag, including 32% integrated probability based on the initial skymap. The revised skymap issued the following day reduced these numbers to 21% for the ZTF and 19% for Palomar Gattini-IR. We narrowed 338,646 ZTF transient "alerts" over the first two nights of observations to 15 candidate counterparts. Two candidates, ZTF19aarykkb and ZTF19aarzaod, were particularly compelling given that their location, distance, and age were consistent with the GW event, and their early optical light curves were photometrically consistent with that of kilonovae. These two candidates were spectroscopically classified as young core-collapse supernovae. The remaining candidates were ruled out as supernovae. Palomar Gattini-IR did not identify any viable candidates with multiple detections only after merger time. We demonstrate that even with single-detector GW events localized to thousands of square degrees, systematic kilonova discovery is feasible.

Published
2019

11. GROWTH on S190510g: DECam Observation planning and follow-up of a distant binary neutron star merger candidate

Author

Andreoni, I, Goldstein, DA, Anand, S, Coughlin, MW, Singer, LP, Ahumada, T, Medford, M, Kool, EC, Webb, S, Bulla, M, Bloom, JS, Kasliwal, MM, Nugent, PE, Bagdasaryan, A, Barnes, J, Cook, DO, Cooke, J, Duev, DA, Fremling, UC, Gatkine, P, Golkhou, VZ, Kong, AKH, Mahabal, A, Martinez-Palomera, J, Tao, D, and Zhang, K

Subjects
binaries: general, gravitational waves, methods: observational, stars: neutron, supernovae: general, astro-ph.HE, astro-ph.IM, astro-ph.SR, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

The first two months of the third Advanced LIGO and Virgo observing run (2019 April-May) showed that distant gravitational-wave (GW) events can now be readily detected. Three candidate mergers containing neutron stars (NS) were reported in a span of 15 days, all likely located more than 100 Mpc away. However, distant events such as the three new NS mergers are likely to be coarsely localized, which highlights the importance of facilities and scheduling systems that enable deep observations over hundreds to thousands of square degrees to detect the electromagnetic counterparts. On 2019 May 10 02:59:39.292 UT the GW candidate S190510g was discovered and initially classified as a binary neutron star (BNS) merger with 98% probability. The GW event was localized within an area of 3462 deg2, later refined to 1166 deg2 (90%) at a distance of 227 92 Mpc. We triggered Target-of-Opportunity observations with the Dark Energy Camera (DECam), a wide-field optical imager mounted at the prime focus of the 4 m Blanco Telescope at Cerro Tololo Inter-American Observatory in Chile. This Letter describes our DECam observations and our real-time analysis results, focusing in particular on the design and implementation of the observing strategy. Within 24 hr of the merger time, we observed 65% of the total enclosed probability of the final skymap with an observing efficiency of 94%. We identified and publicly announced 13 candidate counterparts. S190510g was reclassified 1.7 days after the merger, after our observations were completed, with a "BNS merger" probability reduced from 98% to 42% in favor of a "terrestrial classification.

Published
2019

12. GROWTH on S190426c: Real-time Search for a Counterpart to the Probable Neutron Star-Black Hole Merger using an Automated Difference Imaging Pipeline for DECam

Author

Goldstein, DA, Andreoni, I, Nugent, PE, Kasliwal, MM, Coughlin, MW, Anand, S, Bloom, JS, Martínez-Palomera, J, Zhang, K, Ahumada, T, Bagdasaryan, A, Cooke, J, De, K, Duev, DA, Fremling, UC, Gatkine, P, Graham, M, Ofek, EO, Singer, LP, and Yan, L

Subjects
gravitational waves, stars: black holes, stars: neutron, surveys, astro-ph.HE, astro-ph.IM, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

The discovery of a transient kilonova following the gravitational-wave (GW) event GW170817 highlighted the critical need for coordinated rapid and wide-field observations, inference, and follow-up across the electromagnetic spectrum. In the southern hemisphere, the Dark Energy Camera (DECam) on the Blanco 4 m telescope is well suited to this task, as it is able to cover wide fields quickly while still achieving the depths required to find kilonovae like the one accompanying GW170817 to ∼500 Mpc, the binary neutron star (NS) horizon distance for current generation of LIGO/Virgo collaboration (LVC) interferometers. Here, as part of the multi-facility follow-up by the Global Relay of Observatories Watching Transients Happen collaboration, we describe the observations and automated data movement, data reduction, candidate discovery, and vetting pipeline of our target-of-opportunity DECam observations of S190426c, the first possible NS-black hole merger detected in GWs. Starting 7.5 hr after S190426c, over 11.28 hr of observations, we imaged an area of 525 deg2 (r band) and 437 deg2 (z band); this was 16.3% of the total original localization probability, and nearly all of the probability visible from the southern hemisphere. The machine-learning-based pipeline was optimized for fast turnaround, delivering transients for human vetting within 17 minutes, on average, of shutter closure. We reported nine promising counterpart candidates 2.5 hr before the end of our observations. One hour after our data-taking ended (roughly 20 hr after the announcement of S190426c), LVC released a refined skymap that reduced the probability coverage of our observations to 8.0%, demonstrating a critical need for localization updates on shorter (∼hour) timescales. Our observations yielded no detection of a bona fide counterpart to m z = 21.7 and m r = 22.2 at the 5σ level of significance, consistent with the refined LVC positioning. We view these observations and rapid inferencing as an important real-world test for this novel end-to-end wide-field pipeline.

Published
2019

13. The fast, luminous ultraviolet transient AT2018cow: Extreme supernova, or disruption of a star by an intermediate-mass black hole?

Author

Perley, DA, Mazzali, PA, Yan, L, Cenko, SB, Gezari, S, Taggart, K, Blagorodnova, N, Fremling, C, Mockler, B, Singh, A, Tominaga, N, Tanaka, M, Watson, AM, Ahumada, T, Anupama, GC, Ashall, C, Becerra, RL, Bersier, D, Bhalerao, V, Bloom, JS, Butler, NR, Copperwheat, C, Coughlin, MW, De, K, Drake, AJ, Duev, DA, Frederick, S, González, JJ, Goobar, A, Heida, M, Ho, AYQ, Horst, J, Hung, T, Itoh, R, Jencson, JE, Kasliwal, MM, Kawai, N, Khanam, T, Kulkarni, SR, Kumar, B, Kumar, H, Kutyrev, AS, Lee, WH, Maeda, K, Mahabal, A, Murata, KL, Neill, JD, Ngeow, CC, Penprase, B, Pian, E, Quimby, R, Ramirez-Ruiz, E, Richer, MG, Romań-Zúñiga, CG, Sahu, DK, Srivastav, S, Socia, Q, Sollerman, J, Tachibana, Y, Taddia, F, Tinyanont, S, Troja, E, Ward, C, Wee, J, and Yu, PC

Subjects
Black hole, stars, supernovae: general, supernova: individual: AT2018cow, astro-ph.HE, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

Wide-field optical surveys have begun to uncover large samples of fast (trise ≲ 5 d), luminous (Mpeak < -18), blue transients. While commonly attributed to the breakout of a supernova shock into a dense wind, the great distances to the transients of this class found so far have hampered detailed investigation of their properties. We present photometry and spectroscopy from a comprehensive worldwide campaign to observe AT 2018cow (ATLAS 18qqn), the first fast-luminous optical transient to be found in real time at lowredshift. Our first spectra (10 days. The spectrum remains extremely hot throughout its evolution, and the photospheric radius contracts with time (receding below R < 1014 cm after 1 month). This behaviour does not match that of any known supernova, although a relativistic jet within a fallback supernova could explain some of the observed features. Alternatively, the transient could originate from the disruption of a star by an intermediate-mass black hole, although thiswould require long-lasting emission of highly super-Eddington thermal radiation. In either case, AT 2018cow suggests that the population of fast luminous transients represents a new class of astrophysical event. Intensive follow-up of this event in its late phases, and of any future events found at comparable distance, will be essential to better constrain their origins.

Published
2019

14. DECAM-GROWTH SEARCH FOR THE FAINT AND DISTANT BINARY NEUTRON STAR AND NEUTRON STAR-BLACK HOLE MERGERS IN O3A

Author

Anand, S, Andreoni, I, Goldstein, DA, Kasliwal, MM, Ahumada, T, Barnes, J, Bloom, JS, Bulla, M, Cenko, SB, Cooke, J, Coughlin, MW, Nugent, PE, and Singer, LP

Abstract

Synoptic searches for the optical counterpart to a binary neutron star (BNS) or neutron star-black hole (NSBH) merger can pose significant challenges towards the discovery of kilonovae and performing multi-messenger science. In this work, we describe the advantage of a global multi-telescope network towards this end, with a particular focus on the key and complementary role the Dark Energy Camera (DECam) plays in multi-facility follow-up. We describe the Global Relay of Observatories Watching Transients Happen (GROWTH) Target-of-Opportunity (ToO) Marshal, a common web application we built to ingest events, plan observations, search for transient candidates, and retrieve performance summary statistics for all of the telescopes in our network. Our infrastructure enabled us to conduct observations of two events during O3a, S190426c and S190510g. Furthermore, our analysis of deep DECam observations of S190814bv conducted by the DESGW team, and access to a variety of global follow-up facilities allowed us to place meaningful constraints on the parameters of the kilonova and the merging binary. We emphasize the importance of a global telescope network in conjunction with a power telescope like DECam in performing searches for the counterparts to gravitational-wave sources.

Published
2019

15. Multi-band analyses of the bright GRB 230812B and the associated SN2023pel

Author

Hussenot-Desenonges, T, primary, Wouters, T, additional, Guessoum, N, additional, Abdi, I, additional, Abulwfa, A, additional, Adami, C, additional, Fernández, J F Agüí, additional, Ahumada, T, additional, Aivazyan, V, additional, Akl, D, additional, Anand, S, additional, Andrade, C M, additional, Antier, S, additional, Ata, S A, additional, D’Avanzo, P, additional, Azzam, Y A, additional, Baransky, A, additional, Basa, S, additional, Blazek, M, additional, Bendjoya, P, additional, Beradze, S, additional, Boumis, P, additional, Bremer, M, additional, Brivio, R, additional, Buat, V, additional, Bulla, M, additional, Burkhonov, O, additional, Burns, E, additional, Cenko, S B, additional, Coughlin, M W, additional, Corradi, W, additional, Daigne, F, additional, Dietrich, T, additional, Dornic, D, additional, Ducoin, J-G, additional, Duverne, P-A, additional, Elhosseiny, E G, additional, Elnagahy, F I, additional, El-Sadek, M A, additional, Ferro, M, additional, Le Floc’h, E, additional, Freeberg, M, additional, Fynbo, J P U, additional, Götz, D, additional, Gurbanov, E, additional, Hamed, G M, additional, Hasanov, E, additional, Healy, B F, additional, Heintz, K E, additional, Hello, P, additional, Inasaridze, R, additional, Iskandar, A, additional, Ismailov, N, additional, Izzo, L, additional, Jhawar, S, additional, du Laz, T Jegou, additional, Kamel, T M, additional, Karpov, S, additional, Klotz, A, additional, Koulouridis, E, additional, Kuin, N P, additional, Kochiashvili, N, additional, Leonini, S, additional, Lu, K-X, additional, Malesani, D B, additional, Mašek, M, additional, Mao, J, additional, Melandri, A, additional, Mihov, B M, additional, Natsvlishvili, R, additional, Navarete, F, additional, Nedora, V, additional, Nicolas, J, additional, Odeh, M, additional, Palmerio, J, additional, Pang, P T H, additional, De Pasquale, M, additional, Peng, H W, additional, Pormente, S, additional, Peloton, J, additional, Pradier, T, additional, Pyshna, O, additional, Rajabov, Y, additional, Rakotondrainibe, N A, additional, Rivet, J-P, additional, Rousselot, L, additional, Saccardi, A, additional, Sasaki, N, additional, Schneider, B, additional, Serrau, M, additional, Shokry, A, additional, Slavcheva-Mihova, L, additional, Simon, A, additional, Sokoliuk, O, additional, Srinivasaragavan, G, additional, Strausbaugh, R, additional, Takey, A, additional, Tanvir, N R, additional, Thöne, C C, additional, Tillayev, Y, additional, Melo, I Tosta e, additional, Turpin, D, additional, de Ugarte Postigo, A, additional, Vasylenko, V, additional, Vergani, S D, additional, Vidadi, Z, additional, Xu, D, additional, Wang, L T, additional, Wang, X F, additional, Winters, J M, additional, Zhang, X-L, additional, and Zhu, Z, additional

Published
2024
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16. Multiband analyses of the bright GRB 230812B and the associated SN2023pel

Author

Hussenot-Desenonges, T., Wouters, T., Guessoum, N., Abdi, I., Abulwfa, A., Adami, C., Agüí Fernández, J. F., Ahumada, T., Aivazyan, V., Akl, D., Anand, S., Andrade, C. M., Antier, S., Ata, S. A., D'Avanzo, P., Azzam, Y. A., Baransky, A., Basa, S., Blazek, M., Bendjoya, P., Beradze, S., Boumis, P., Bremer, M., Brivio, R., Buat, V., Bulla, M., Burkhonov, O., Burns, E., Cenko, S. B., Coughlin, M. W., Corradi, W., Daigne, F., Dietrich, T., Dornic, D., Ducoin, J. G., Duverne, P. A., Elhosseiny, E. G., Elnagahy, F. I., El-Sadek, M. A., Ferro, M., Le Floc'H, E., Freeberg, M., Fynbo, J. P.U., Götz, D., Gurbanov, E., Hamed, G. M., Hasanov, E., Healy, B. F., Heintz, K. E., Hello, P., Inasaridze, R., Iskandar, A., Ismailov, N., Izzo, L., Jhawar, S., Jegou du Laz, T., Kamel, T. M., Karpov, S., Klotz, A., Koulouridis, E., Kuin, N. P., Kochiashvili, N., Leonini, S., Lu, K. X., Malesani, D. B., Mašek, M., Mao, J., Melandri, A., Mihov, B. M., Natsvlishvili, R., Navarete, F., Nedora, V., Nicolas, J., Odeh, M., Palmerio, J., Pang, P. T.H., De Pasquale, M., Peng, H. W., Pormente, S., Peloton, J., Pradier, T., Pyshna, O., Rajabov, Y., Rakotondrainibe, N. A., Rivet, J. P., Rousselot, L., Saccardi, A., Sasaki, N., Schneider, B., Serrau, M., Shokry, A., Slavcheva-Mihova, L., Simon, A., Sokoliuk, O., Srinivasaragavan, G., Strausbaugh, R., Takey, A., Tanvir, N. R., Thöne, C. C., Tillayev, Y., Tosta e Melo, I., Turpin, D., de Ugarte Postigo, A., Vasylenko, V., Vergani, S. D., Vidadi, Z., Xu, D., Wang, L. T., Wang, X. F., Winters, J. M., Zhang, X. L., Zhu, Z., Hussenot-Desenonges, T., Wouters, T., Guessoum, N., Abdi, I., Abulwfa, A., Adami, C., Agüí Fernández, J. F., Ahumada, T., Aivazyan, V., Akl, D., Anand, S., Andrade, C. M., Antier, S., Ata, S. A., D'Avanzo, P., Azzam, Y. A., Baransky, A., Basa, S., Blazek, M., Bendjoya, P., Beradze, S., Boumis, P., Bremer, M., Brivio, R., Buat, V., Bulla, M., Burkhonov, O., Burns, E., Cenko, S. B., Coughlin, M. W., Corradi, W., Daigne, F., Dietrich, T., Dornic, D., Ducoin, J. G., Duverne, P. A., Elhosseiny, E. G., Elnagahy, F. I., El-Sadek, M. A., Ferro, M., Le Floc'H, E., Freeberg, M., Fynbo, J. P.U., Götz, D., Gurbanov, E., Hamed, G. M., Hasanov, E., Healy, B. F., Heintz, K. E., Hello, P., Inasaridze, R., Iskandar, A., Ismailov, N., Izzo, L., Jhawar, S., Jegou du Laz, T., Kamel, T. M., Karpov, S., Klotz, A., Koulouridis, E., Kuin, N. P., Kochiashvili, N., Leonini, S., Lu, K. X., Malesani, D. B., Mašek, M., Mao, J., Melandri, A., Mihov, B. M., Natsvlishvili, R., Navarete, F., Nedora, V., Nicolas, J., Odeh, M., Palmerio, J., Pang, P. T.H., De Pasquale, M., Peng, H. W., Pormente, S., Peloton, J., Pradier, T., Pyshna, O., Rajabov, Y., Rakotondrainibe, N. A., Rivet, J. P., Rousselot, L., Saccardi, A., Sasaki, N., Schneider, B., Serrau, M., Shokry, A., Slavcheva-Mihova, L., Simon, A., Sokoliuk, O., Srinivasaragavan, G., Strausbaugh, R., Takey, A., Tanvir, N. R., Thöne, C. C., Tillayev, Y., Tosta e Melo, I., Turpin, D., de Ugarte Postigo, A., Vasylenko, V., Vergani, S. D., Vidadi, Z., Xu, D., Wang, L. T., Wang, X. F., Winters, J. M., Zhang, X. L., and Zhu, Z.

Published
2024

17. Multiband analyses of the bright GRB 230812B and the associated SN2023pel

Author

Sub GRASP, Gravitational and Subatomic Physics (GRASP), Hussenot-Desenonges, T., Wouters, T., Guessoum, N., Abdi, I., Abulwfa, A., Adami, C., Agüí Fernández, J. F., Ahumada, T., Aivazyan, V., Akl, D., Anand, S., Andrade, C. M., Antier, S., Ata, S. A., D'Avanzo, P., Azzam, Y. A., Baransky, A., Basa, S., Blazek, M., Bendjoya, P., Beradze, S., Boumis, P., Bremer, M., Brivio, R., Buat, V., Bulla, M., Burkhonov, O., Burns, E., Cenko, S. B., Coughlin, M. W., Corradi, W., Daigne, F., Dietrich, T., Dornic, D., Ducoin, J. G., Duverne, P. A., Elhosseiny, E. G., Elnagahy, F. I., El-Sadek, M. A., Ferro, M., Le Floc'H, E., Freeberg, M., Fynbo, J. P.U., Götz, D., Gurbanov, E., Hamed, G. M., Hasanov, E., Healy, B. F., Heintz, K. E., Hello, P., Inasaridze, R., Iskandar, A., Ismailov, N., Izzo, L., Jhawar, S., Jegou du Laz, T., Kamel, T. M., Karpov, S., Klotz, A., Koulouridis, E., Kuin, N. P., Kochiashvili, N., Leonini, S., Lu, K. X., Malesani, D. B., Mašek, M., Mao, J., Melandri, A., Mihov, B. M., Natsvlishvili, R., Navarete, F., Nedora, V., Nicolas, J., Odeh, M., Palmerio, J., Pang, P. T.H., De Pasquale, M., Peng, H. W., Pormente, S., Peloton, J., Pradier, T., Pyshna, O., Rajabov, Y., Rakotondrainibe, N. A., Rivet, J. P., Rousselot, L., Saccardi, A., Sasaki, N., Schneider, B., Serrau, M., Shokry, A., Slavcheva-Mihova, L., Simon, A., Sokoliuk, O., Srinivasaragavan, G., Strausbaugh, R., Takey, A., Tanvir, N. R., Thöne, C. C., Tillayev, Y., Tosta e Melo, I., Turpin, D., de Ugarte Postigo, A., Vasylenko, V., Vergani, S. D., Vidadi, Z., Xu, D., Wang, L. T., Wang, X. F., Winters, J. M., Zhang, X. L., Zhu, Z., Sub GRASP, Gravitational and Subatomic Physics (GRASP), Hussenot-Desenonges, T., Wouters, T., Guessoum, N., Abdi, I., Abulwfa, A., Adami, C., Agüí Fernández, J. F., Ahumada, T., Aivazyan, V., Akl, D., Anand, S., Andrade, C. M., Antier, S., Ata, S. A., D'Avanzo, P., Azzam, Y. A., Baransky, A., Basa, S., Blazek, M., Bendjoya, P., Beradze, S., Boumis, P., Bremer, M., Brivio, R., Buat, V., Bulla, M., Burkhonov, O., Burns, E., Cenko, S. B., Coughlin, M. W., Corradi, W., Daigne, F., Dietrich, T., Dornic, D., Ducoin, J. G., Duverne, P. A., Elhosseiny, E. G., Elnagahy, F. I., El-Sadek, M. A., Ferro, M., Le Floc'H, E., Freeberg, M., Fynbo, J. P.U., Götz, D., Gurbanov, E., Hamed, G. M., Hasanov, E., Healy, B. F., Heintz, K. E., Hello, P., Inasaridze, R., Iskandar, A., Ismailov, N., Izzo, L., Jhawar, S., Jegou du Laz, T., Kamel, T. M., Karpov, S., Klotz, A., Koulouridis, E., Kuin, N. P., Kochiashvili, N., Leonini, S., Lu, K. X., Malesani, D. B., Mašek, M., Mao, J., Melandri, A., Mihov, B. M., Natsvlishvili, R., Navarete, F., Nedora, V., Nicolas, J., Odeh, M., Palmerio, J., Pang, P. T.H., De Pasquale, M., Peng, H. W., Pormente, S., Peloton, J., Pradier, T., Pyshna, O., Rajabov, Y., Rakotondrainibe, N. A., Rivet, J. P., Rousselot, L., Saccardi, A., Sasaki, N., Schneider, B., Serrau, M., Shokry, A., Slavcheva-Mihova, L., Simon, A., Sokoliuk, O., Srinivasaragavan, G., Strausbaugh, R., Takey, A., Tanvir, N. R., Thöne, C. C., Tillayev, Y., Tosta e Melo, I., Turpin, D., de Ugarte Postigo, A., Vasylenko, V., Vergani, S. D., Vidadi, Z., Xu, D., Wang, L. T., Wang, X. F., Winters, J. M., Zhang, X. L., and Zhu, Z.

Published
2024

18. Multiband analyses of the bright GRB 230812B and the associated SN2023pel

Author

Hussenot-desenonges, T, Wouters, T, Guessoum, N, Abdi, I, Abulwfa, A, Adami, C, Agüí fernández, J F, Ahumada, T, Aivazyan, V, Akl, D, Anand, S, Andrade, C M, Antier, S, Ata, S A, D’avanzo, P, Azzam, Y A, Baransky, A, Basa, S, Blazek, M, Bendjoya, P, Beradze, S, Boumis, P, Bremer, M, Brivio, R, Buat, V, Bulla, M, Burkhonov, O, Burns, E, Cenko, S B, Coughlin, M W, Corradi, W, Daigne, F, Dietrich, T, Dornic, D, Ducoin, J -g, Duverne, P -a, Elhosseiny, E G, Elnagahy, F I, El-sadek, M A, Ferro, M, Le floc’h, E, Freeberg, M, Fynbo, J P U, Götz, D, Gurbanov, E, Hamed, G M, Hasanov, E, Healy, B F, Heintz, K E, Hello, P, Inasaridze, R, Iskandar, A, Ismailov, N, Izzo, L, Jhawar, S, Jegou du laz, T, Kamel, T M, Karpov, S, Klotz, A, Koulouridis, E, Kuin, N P, Kochiashvili, N, Leonini, S, Lu, K -x, Malesani, D B, Mašek, M, Mao, J, Melandri, A, Mihov, B M, Natsvlishvili, R, Navarete, F, Nedora, V, Nicolas, J, Odeh, M, Palmerio, J, Pang, P T H, De pasquale, M, Peng, H W, Pormente, S, Peloton, J, Pradier, T, Pyshna, O, Rajabov, Y, Rakotondrainibe, N A, Rivet, J -p, Rousselot, L, Saccardi, A, Sasaki, N, Schneider, B, Serrau, M, Shokry, A, Slavcheva-mihova, L, Simon, A, Sokoliuk, O, Srinivasaragavan, G, Strausbaugh, R, Takey, A, Tanvir, N R, Thöne, C C, Tillayev, Y, Melo, I Tosta E, Turpin, D, De ugarte postigo, A, Vasylenko, V, Vergani, S D, Vidadi, Z, Xu, D, Wang, L T, Wang, X F, Winters, J M, Zhang, X -l, Zhu, Z, Hussenot-desenonges, T, Wouters, T, Guessoum, N, Abdi, I, Abulwfa, A, Adami, C, Agüí fernández, J F, Ahumada, T, Aivazyan, V, Akl, D, Anand, S, Andrade, C M, Antier, S, Ata, S A, D’avanzo, P, Azzam, Y A, Baransky, A, Basa, S, Blazek, M, Bendjoya, P, Beradze, S, Boumis, P, Bremer, M, Brivio, R, Buat, V, Bulla, M, Burkhonov, O, Burns, E, Cenko, S B, Coughlin, M W, Corradi, W, Daigne, F, Dietrich, T, Dornic, D, Ducoin, J -g, Duverne, P -a, Elhosseiny, E G, Elnagahy, F I, El-sadek, M A, Ferro, M, Le floc’h, E, Freeberg, M, Fynbo, J P U, Götz, D, Gurbanov, E, Hamed, G M, Hasanov, E, Healy, B F, Heintz, K E, Hello, P, Inasaridze, R, Iskandar, A, Ismailov, N, Izzo, L, Jhawar, S, Jegou du laz, T, Kamel, T M, Karpov, S, Klotz, A, Koulouridis, E, Kuin, N P, Kochiashvili, N, Leonini, S, Lu, K -x, Malesani, D B, Mašek, M, Mao, J, Melandri, A, Mihov, B M, Natsvlishvili, R, Navarete, F, Nedora, V, Nicolas, J, Odeh, M, Palmerio, J, Pang, P T H, De pasquale, M, Peng, H W, Pormente, S, Peloton, J, Pradier, T, Pyshna, O, Rajabov, Y, Rakotondrainibe, N A, Rivet, J -p, Rousselot, L, Saccardi, A, Sasaki, N, Schneider, B, Serrau, M, Shokry, A, Slavcheva-mihova, L, Simon, A, Sokoliuk, O, Srinivasaragavan, G, Strausbaugh, R, Takey, A, Tanvir, N R, Thöne, C C, Tillayev, Y, Melo, I Tosta E, Turpin, D, De ugarte postigo, A, Vasylenko, V, Vergani, S D, Vidadi, Z, Xu, D, Wang, L T, Wang, X F, Winters, J M, Zhang, X -l, and Zhu, Z

Published
2024

19. Publisher Correction: A very luminous jet from the disruption of a star by a massive black hole (Nature, (2022), 612, 7940, (430-434), 10.1038/s41586-022-05465-8)

Author

Andreoni, I. Coughlin, M.W. Perley, D.A. Yao, Y. Lu, W. Cenko, S.B. Kumar, H. Anand, S. Ho, A.Y.Q. Kasliwal, M.M. de Ugarte Postigo, A. Sagués-Carracedo, A. Schulze, S. Kann, D.A. Kulkarni, S.R. Sollerman, J. Tanvir, N. Rest, A. Izzo, L. Somalwar, J.J. Kaplan, D.L. Ahumada, T. Anupama, G.C. Auchettl, K. Barway, S. Bellm, E.C. Bhalerao, V. Bloom, J.S. Bremer, M. Bulla, M. Burns, E. Campana, S. Chandra, P. Charalampopoulos, P. Cooke, J. D’Elia, V. Das, K.K. Dobie, D. Fernández, J.F.A. Freeburn, J. Fremling, C. Gezari, S. Goode, S. Graham, M.J. Hammerstein, E. Karambelkar, V.R. Kilpatrick, C.D. Kool, E.C. Krips, M. Laher, R.R. Leloudas, G. Levan, A. Lundquist, M.J. Mahabal, A.A. Medford, M.S. Miller, M.C. Möller, A. Mooley, K.P. Nayana, A.J. Nir, G. Pang, P.T.H. Paraskeva, E. Perley, R.A. Petitpas, G. Pursiainen, M. Ravi, V. Ridden-Harper, R. Riddle, R. Rigault, M. Rodriguez, A.C. Rusholme, B. Sharma, Y. Smith, I.A. Stein, R.D. Thöne, C. Tohuvavohu, A. Valdes, F. van Roestel, J. Vergani, S.D. Wang, Q. Zhang, J. and Andreoni, I. Coughlin, M.W. Perley, D.A. Yao, Y. Lu, W. Cenko, S.B. Kumar, H. Anand, S. Ho, A.Y.Q. Kasliwal, M.M. de Ugarte Postigo, A. Sagués-Carracedo, A. Schulze, S. Kann, D.A. Kulkarni, S.R. Sollerman, J. Tanvir, N. Rest, A. Izzo, L. Somalwar, J.J. Kaplan, D.L. Ahumada, T. Anupama, G.C. Auchettl, K. Barway, S. Bellm, E.C. Bhalerao, V. Bloom, J.S. Bremer, M. Bulla, M. Burns, E. Campana, S. Chandra, P. Charalampopoulos, P. Cooke, J. D’Elia, V. Das, K.K. Dobie, D. Fernández, J.F.A. Freeburn, J. Fremling, C. Gezari, S. Goode, S. Graham, M.J. Hammerstein, E. Karambelkar, V.R. Kilpatrick, C.D. Kool, E.C. Krips, M. Laher, R.R. Leloudas, G. Levan, A. Lundquist, M.J. Mahabal, A.A. Medford, M.S. Miller, M.C. Möller, A. Mooley, K.P. Nayana, A.J. Nir, G. Pang, P.T.H. Paraskeva, E. Perley, R.A. Petitpas, G. Pursiainen, M. Ravi, V. Ridden-Harper, R. Riddle, R. Rigault, M. Rodriguez, A.C. Rusholme, B. Sharma, Y. Smith, I.A. Stein, R.D. Thöne, C. Tohuvavohu, A. Valdes, F. van Roestel, J. Vergani, S.D. Wang, Q. Zhang, J.

Abstract

In the version of this article initially published, there was in an error in the third-to-last sentence of the abstract, now reading, in part, “we calculate a rate of 0.02–0.01 +0.04 Gpc–3 yr–1”, where Gpc was spelled out as gigapascals, not gigaparsecs. Also, the scale label (2″) was missing in the lower-left corner of Fig. 1b. The errors have been corrected in the HTML and PDF versions of the article. © The Author(s), under exclusive licence to Springer Nature Limited 2023.

Published
2023

20. Publisher Correction: A very luminous jet from the disruption of a star by a massive black hole

Author

Andreoni, I., Coughlin, M.W., Perley, D.A., Yao, Y., Lu, W., Cenko, S.B., Kumar, H., Anand, S., Ho, A.Y.Q., Kasliwal, M.M., Postigo, A. de Ugarte, Sagues-Carracedo, A., Schulze, S., Kann, D.A., Kulkarni, S.R., Sollerman, J., Tanvir, N., Rest, A., Izzo, L., Somalwar, J.J., Kaplan, D.L., Ahumada, T., Anupama, G.C., Auchettl, K., Barway, S., Bellm, E.C., Bhalerao, V., Bloom, J.S., Bremer, M., Bulla, M., Burns, E., Campana, S., Chandra, P., Charalampopoulos, P., Cooke, J., D'Elia, V., Das, K.K., Dobie, D., Fernandez, J.F.A., Freeburn, J., Fremling, C., Gezari, S., Goode, S., Graham, M.J., Hammerstein, E., Karambelkar, V.R., Kilpatrick, C.D., Kool, E.C., Krips, M., Laher, R.R., Leloudas, G., Levan, A.J., Lundquist, M.J., Mahabal, A.A., Medford, M.S., Miller, M.C., Moller, A., Mooley, K.P., Nayana, A.J., Nir, G., Pang, P.T.H., Paraskeva, E., Perley, R.A., Petitpas, G., Pursiainen, M., Ravi, V., Ridden-Harper, R., Riddle, R., Rigault, M., Rodriguez, A.C., Rusholme, B., Sharma, Y., Smith, I.A., Stein, R.D., Thone, C., Tohuvavohu, A., Valdes, F., Roestel, J. van, Vergani, S.D., Wang, Q., Zhang, J., Andreoni, I., Coughlin, M.W., Perley, D.A., Yao, Y., Lu, W., Cenko, S.B., Kumar, H., Anand, S., Ho, A.Y.Q., Kasliwal, M.M., Postigo, A. de Ugarte, Sagues-Carracedo, A., Schulze, S., Kann, D.A., Kulkarni, S.R., Sollerman, J., Tanvir, N., Rest, A., Izzo, L., Somalwar, J.J., Kaplan, D.L., Ahumada, T., Anupama, G.C., Auchettl, K., Barway, S., Bellm, E.C., Bhalerao, V., Bloom, J.S., Bremer, M., Bulla, M., Burns, E., Campana, S., Chandra, P., Charalampopoulos, P., Cooke, J., D'Elia, V., Das, K.K., Dobie, D., Fernandez, J.F.A., Freeburn, J., Fremling, C., Gezari, S., Goode, S., Graham, M.J., Hammerstein, E., Karambelkar, V.R., Kilpatrick, C.D., Kool, E.C., Krips, M., Laher, R.R., Leloudas, G., Levan, A.J., Lundquist, M.J., Mahabal, A.A., Medford, M.S., Miller, M.C., Moller, A., Mooley, K.P., Nayana, A.J., Nir, G., Pang, P.T.H., Paraskeva, E., Perley, R.A., Petitpas, G., Pursiainen, M., Ravi, V., Ridden-Harper, R., Riddle, R., Rigault, M., Rodriguez, A.C., Rusholme, B., Sharma, Y., Smith, I.A., Stein, R.D., Thone, C., Tohuvavohu, A., Valdes, F., Roestel, J. van, Vergani, S.D., Wang, Q., and Zhang, J.

Abstract

Contains fulltext : 292562.pdf (Publisher’s version ) (Closed access)

Published
2023

23. A very luminous jet from the disruption of a star by a massive black hole

Author

Andreoni, I., Coughlin, M.W., Perley, D.A., Yao, Y., Lu, W., Cenko, S.B., Kumar, H., Anand, S., Ho, A.Y.Q., Kasliwal, M.M., Postigo, A. de Ugarte, Sagués-Carracedo, A., Schulze, S., Kann, D.A., Kulkarni, S.R., Sollerman, J., Tanvir, N., Rest, A., Izzo, L., Somalwar, J.J., Kaplan, D.L., Ahumada, T., Anupama, G.C., Auchettl, K., Barway, S., Bellm, E.C., Bhalerao, V., Bloom, J.S., Bremer, M., Bulla, M., Burns, E., Campana, S., Chandra, P., Charalampopoulos, P., Cooke, J., D’Elia, V., Das, K.K., Dobie, D., Fernández, J.F.A., Freeburn, J., Fremling, C., Gezari, S., Goode, S., Graham, M.J., Hammerstein, E., Karambelkar, V.R., Kilpatrick, C.D., Kool, E.C., Krips, M., Laher, R.R., Leloudas, G., Levan, A.J., Lundquist, M.J., Mahabal, A.A., Medford, M.S., Miller, M.C., Möller, A., Mooley, K.P., Nayana, A.J., Nir, G., Pang, P.T.H., Paraskeva, E., Perley, R.A., Petitpas, G., Pursiainen, M., Ravi, V., Ridden-Harper, R., Riddle, R., Rigault, M., Rodriguez, A.C., Rusholme, B., Sharma, Y., Smith, I.A., Stein, R.D., Thöne, C., Tohuvavohu, A., Valdes, F., Roestel, J. van, Vergani, S.D., Wang, Q., Zhang, J., Andreoni, I., Coughlin, M.W., Perley, D.A., Yao, Y., Lu, W., Cenko, S.B., Kumar, H., Anand, S., Ho, A.Y.Q., Kasliwal, M.M., Postigo, A. de Ugarte, Sagués-Carracedo, A., Schulze, S., Kann, D.A., Kulkarni, S.R., Sollerman, J., Tanvir, N., Rest, A., Izzo, L., Somalwar, J.J., Kaplan, D.L., Ahumada, T., Anupama, G.C., Auchettl, K., Barway, S., Bellm, E.C., Bhalerao, V., Bloom, J.S., Bremer, M., Bulla, M., Burns, E., Campana, S., Chandra, P., Charalampopoulos, P., Cooke, J., D’Elia, V., Das, K.K., Dobie, D., Fernández, J.F.A., Freeburn, J., Fremling, C., Gezari, S., Goode, S., Graham, M.J., Hammerstein, E., Karambelkar, V.R., Kilpatrick, C.D., Kool, E.C., Krips, M., Laher, R.R., Leloudas, G., Levan, A.J., Lundquist, M.J., Mahabal, A.A., Medford, M.S., Miller, M.C., Möller, A., Mooley, K.P., Nayana, A.J., Nir, G., Pang, P.T.H., Paraskeva, E., Perley, R.A., Petitpas, G., Pursiainen, M., Ravi, V., Ridden-Harper, R., Riddle, R., Rigault, M., Rodriguez, A.C., Rusholme, B., Sharma, Y., Smith, I.A., Stein, R.D., Thöne, C., Tohuvavohu, A., Valdes, F., Roestel, J. van, Vergani, S.D., Wang, Q., and Zhang, J.

Abstract

05 december 2022, Contains fulltext : 286062.pdf (Author’s version preprint ) (Open Access)

Published
2022

24. The discovery and characterization of (594913) 'Ayló'chaxnim, a kilometre sized asteroid inside the orbit of Venus

Author

Bolin, Bryce T, Ahumada, T., Van Dokkum, P., Fremling, C., Granvik, M., Hardegree-Ullman, K.K., Harikane, Y., Purdum, J.N., Serabyn, E., Southworth, J., Zhai, Chengxing, Bolin, Bryce T, Ahumada, T., Van Dokkum, P., Fremling, C., Granvik, M., Hardegree-Ullman, K.K., Harikane, Y., Purdum, J.N., Serabyn, E., Southworth, J., and Zhai, Chengxing

Abstract

Near-Earth asteroid population models predict the existence of bodies located inside the orbit of Venus. Despite searches up to the end of 2019, none had been found. We report discovery and follow-up observations of (594913) 'Ayló'chaxnim, an asteroid with an orbit entirely interior to Venus. (594913) 'Ayló'chaxnim has an aphelion distance of ∼0.65 au, is ∼2 km in diameter and is red in colour. The detection of such a large asteroid inside the orbit of Venus is surprising given their rarity according to near-Earth asteroid population models. As the first officially numbered and named asteroid located entirely within the orbit of Venus, we propose that the class of interior to Venus asteroids be referred to as 'Ayló'chaxnim asteroids. © 2022 Published by Oxford University Press on behalf of Royal Astronomical Society.

Published
2022

25. Candidate Tidal Disruption Event AT2019fdr Coincident with a High-Energy Neutrino

Author

Reusch, S., Stein, R., Kowalski, M., Van Velzen, S., Franckowiak, A., Lunardini, C., Murase, K., Winter, W., Miller-Jones, James, Kasliwal, M.M., Gilfanov, M., Garrappa, S., Paliya, V.S., Ahumada, T., Anand, S., Barbarino, C., Bellm, E.C., Brinnel, V., Buson, S., Cenko, S.B., Coughlin, M.W., De, K., Dekany, R., Frederick, S., Gal-Yam, A., Gezari, S., Giroletti, M., Graham, M.J., Karambelkar, V., Kimura, S.S., Kong, A.K.H., Kool, E.C., Laher, R.R., Medvedev, P., Necker, J., Nordin, J., Perley, D.A., Rigault, M., Rusholme, B., Schulze, S., Schweyer, T., Singer, L.P., Sollerman, J., Strotjohann, N.L., Sunyaev, R., Van Santen, J., Walters, R., Zhang, B.T., Zimmerman, E., Reusch, S., Stein, R., Kowalski, M., Van Velzen, S., Franckowiak, A., Lunardini, C., Murase, K., Winter, W., Miller-Jones, James, Kasliwal, M.M., Gilfanov, M., Garrappa, S., Paliya, V.S., Ahumada, T., Anand, S., Barbarino, C., Bellm, E.C., Brinnel, V., Buson, S., Cenko, S.B., Coughlin, M.W., De, K., Dekany, R., Frederick, S., Gal-Yam, A., Gezari, S., Giroletti, M., Graham, M.J., Karambelkar, V., Kimura, S.S., Kong, A.K.H., Kool, E.C., Laher, R.R., Medvedev, P., Necker, J., Nordin, J., Perley, D.A., Rigault, M., Rusholme, B., Schulze, S., Schweyer, T., Singer, L.P., Sollerman, J., Strotjohann, N.L., Sunyaev, R., Van Santen, J., Walters, R., Zhang, B.T., and Zimmerman, E.

Abstract

The origins of the high-energy cosmic neutrino flux remain largely unknown. Recently, one high-energy neutrino was associated with a tidal disruption event (TDE). Here we present AT2019fdr, an exceptionally luminous TDE candidate, coincident with another high-energy neutrino. Our observations, including a bright dust echo and soft late-time x-ray emission, further support a TDE origin of this flare. The probability of finding two such bright events by chance is just 0.034%. We evaluate several models for neutrino production and show that AT2019fdr is capable of producing the observed high-energy neutrino, reinforcing the case for TDEs as neutrino sources.

Published
2022

26. DECAM-GROWTH SEARCH FOR THE FAINT AND DISTANT BINARY NEUTRON STAR AND NEUTRON STAR-BLACK HOLE MERGERS IN O3A

Author

Anand, S., primary, Andreoni, I., additional, Goldstein, D. A., additional, Kasliwal, M. M., additional, Ahumada, T., additional, Barnes, J., additional, Bloom, J. S., additional, Bulla, M., additional, Cenko, S. B., additional, Cooke, J., additional, Coughlin, M. W., additional, Nugent, P. E., additional, and Singer, L. P., additional

Published
2021
Full Text
View/download PDF

27. Discovery and confirmation of the shortest gamma ray burst from a collapsar [Author Correction to: Nature Astronomy https://doi.org/10.1038/s41550-021-01428-7,]

Author

Ahumada, T., Singer, L., Anand, S., Coughlin, M., Kasliwal, M., Ryan, G., Andreoni, I., Cenko, S., Fremling, C., Kumar, H., Pang, P., Burns, E., Cunningham, V., Dichiara, S., Dietrich, T., Svinkin, D., Almualla, M., Castro-Tirado, A., De, K., Dunwoody, R., Gatkine, P., Hammerstein, E., Iyyani, S., Mangan, J., Perley, D., Purkayastha, S., Bellm, E., Bhalerao, V., Bolin, B., Bulla, M., Cannella, C., Chandra, P., Duev, D., Frederiks, D., Gal-Yam, A., Graham, M., Ho, A., Hurley, K., Karambelkar, V., Kool, E., Kulkarni, S., Mahabal, A., Masci, F., McBreen, S., Pandey, S., Reusch, S., Ridnaia, A., Rosnet, P., Rusholme, B., Carracedo, A., Smith, R., Soumagnac, M., Stein, R., Troja, E., Tsvetkova, A., Walters, R., and Valeev, A.

Abstract

Gamma-ray bursts (GRBs) are among the brightest and most energetic events in the universe. The duration and hardness distribution of GRBs has two clusters, now understood to reflect (at least) two different progenitors. Short-hard GRBs (SGRBs; T90 2 s) have been attributed to the collapse of peculiar massive stars (collapsars). The discovery of SN 1998bw/GRB 980425 marked the first association of a LGRB with a collapsar and AT 2017gfo/GRB 170817A/GW170817 marked the first association of a SGRB with a binary neutron star merger, producing also gravitational wave (GW). Here, we present the discovery of ZTF20abwysqy (AT2020scz), a fast-fading optical transient in the Fermi Satellite and the InterPlanetary Network (IPN) localization regions of GRB 200826A; X-ray and radio emission further confirm that this is the afterglow. Follow-up imaging (at rest-frame 16.5 days) reveals excess emission above the afterglow that cannot be explained as an underlying kilonova (KN), but is consistent with being the supernova (SN). Despite the GRB duration being short (rest-frame T90 of 0.65 s), our panchromatic follow-up data confirms a collapsar origin. GRB 200826A is the shortest LGRB found with an associated collapsar; it appears to sit on the brink between a successful and a failed collapsar. Our discovery is consistent with the hypothesis that most collapsars fail to produce ultra-relativistic jets.

Published
2021

28. discovery and characterization of (594913) 'Ayló'chaxnim, a kilometre sized asteroid inside the orbit of Venus.

Author

Bolin, Bryce T, Ahumada, T, van Dokkum, P, Fremling, C, Granvik, M, Hardegree-Ullman, K K, Harikane, Y, Purdum, J N, Serabyn, E, Southworth, J, and Zhai, C

Subjects
ASTEROID orbits, NEAR-earth asteroids, ASTEROID detection, SMALL solar system bodies, ORBITS (Astronomy), VENUS (Planet), ASTEROIDS
Abstract

Near-Earth asteroid population models predict the existence of bodies located inside the orbit of Venus. Despite searches up to the end of 2019, none had been found. We report discovery and follow-up observations of (594913) 'Ayló'chaxnim, an asteroid with an orbit entirely interior to Venus. (594913) 'Ayló'chaxnim has an aphelion distance of ∼0.65 au, is ∼2 km in diameter and is red in colour. The detection of such a large asteroid inside the orbit of Venus is surprising given their rarity according to near-Earth asteroid population models. As the first officially numbered and named asteroid located entirely within the orbit of Venus, we propose that the class of interior to Venus asteroids be referred to as 'Ayló'chaxnim asteroids. [ABSTRACT FROM AUTHOR]

Published
2022
Full Text
View/download PDF

29. A tidal disruption event coincident with a high-energy neutrino

Author

Stein, R, Stein, R, Velzen, SV, Kowalski, M, Franckowiak, A, Gezari, S, Miller-Jones, JCA, Frederick, S, Sfaradi, I, Bietenholz, MF, Horesh, A, Fender, R, Garrappa, S, Ahumada, T, Andreoni, I, Belicki, J, Bellm, EC, Böttcher, M, Brinnel, V, Burruss, R, Cenko, SB, Coughlin, MW, Cunningham, V, Drake, A, Farrar, GR, Feeney, M, Foley, RJ, Gal-Yam, A, Golkhou, VZ, Goobar, A, Graham, MJ, Hammerstein, E, Helou, G, Hung, T, Kasliwal, MM, Kilpatrick, CD, Kong, AKH, Kupfer, T, Laher, RR, Mahabal, AA, Masci, FJ, Necker, J, Nordin, J, Perley, DA, Rigault, M, Reusch, S, Rodriguez, H, Rojas-Bravo, C, Rusholme, B, Shupe, DL, Singer, LP, Sollerman, J, Soumagnac, MT, Stern, D, Taggart, K, van Santen, J, Ward, C, Woudt, P, Yao, Y, Stein, R, Stein, R, Velzen, SV, Kowalski, M, Franckowiak, A, Gezari, S, Miller-Jones, JCA, Frederick, S, Sfaradi, I, Bietenholz, MF, Horesh, A, Fender, R, Garrappa, S, Ahumada, T, Andreoni, I, Belicki, J, Bellm, EC, Böttcher, M, Brinnel, V, Burruss, R, Cenko, SB, Coughlin, MW, Cunningham, V, Drake, A, Farrar, GR, Feeney, M, Foley, RJ, Gal-Yam, A, Golkhou, VZ, Goobar, A, Graham, MJ, Hammerstein, E, Helou, G, Hung, T, Kasliwal, MM, Kilpatrick, CD, Kong, AKH, Kupfer, T, Laher, RR, Mahabal, AA, Masci, FJ, Necker, J, Nordin, J, Perley, DA, Rigault, M, Reusch, S, Rodriguez, H, Rojas-Bravo, C, Rusholme, B, Shupe, DL, Singer, LP, Sollerman, J, Soumagnac, MT, Stern, D, Taggart, K, van Santen, J, Ward, C, Woudt, P, and Yao, Y

Abstract

Cosmic neutrinos provide a unique window into the otherwise hidden mechanism of particle acceleration in astrophysical objects. The IceCube Collaboration recently reported the likely association of one high-energy neutrino with a flare from the relativistic jet of an active galaxy pointed towards the Earth. However a combined analysis of many similar active galaxies revealed no excess from the broader population, leaving the vast majority of the cosmic neutrino flux unexplained. Here we present the likely association of a radio-emitting tidal disruption event, AT2019dsg, with a second high-energy neutrino. AT2019dsg was identified as part of our systematic search for optical counterparts to high-energy neutrinos with the Zwicky Transient Facility. The probability of finding any coincident radio-emitting tidal disruption event by chance is 0.5%, while the probability of finding one as bright in bolometric energy flux as AT2019dsg is 0.2%. Our electromagnetic observations can be explained through a multizone model, with radio analysis revealing a central engine, embedded in a UV photosphere, that powers an extended synchrotron-emitting outflow. This provides an ideal site for petaelectronvolt neutrino production. Assuming that the association is genuine, our observations suggest that tidal disruption events with mildly relativistic outflows contribute to the cosmic neutrino flux.

Published
2021

30. Discovery and confirmation of the shortest gamma-ray burst from a collapsar

Author

Ahumada, T., Singer, L. P., Anand, S., Coughlin, M. W., Kasliwal, M. M., Ryan, G., Andreoni, I., Cenko, S. B., Fremling, C., Kumar, H., Pang, P. T. H., Burns, E., Cunningham, V., Dichiara, S., Dietrich, T., Svinkin, D. S., Almualla, M., Castro-Tirado, A. J., De, K., Dunwoody, R., Gatkine, P., Hammerstein, E., Iyyani, S., Mangan, J., Perley, D., Purkayastha, S., Bellm, E., Bhalerao, V., Bolin, B., Bulla, Mattia, Cannella, C., Chandra, P., Duev, D. A., Frederiks, D., Gal-Yam, A., Graham, M., Ho, A. Y. Q., Hurley, K., Karambelkar, V., Kool, E. C., Kulkarni, S. R., Mahabal, A., Masci, F., McBreen, S., Pandey, S. B., Reusch, S., Ridnaia, A., Rosnet, P., Rusholme, B., Carracedo, A. S., Smith, R., Soumagnac, M., Stein, R., Troja, E., Tsvetkova, A., Walters, R., Valeev, A. F., Ahumada, T., Singer, L. P., Anand, S., Coughlin, M. W., Kasliwal, M. M., Ryan, G., Andreoni, I., Cenko, S. B., Fremling, C., Kumar, H., Pang, P. T. H., Burns, E., Cunningham, V., Dichiara, S., Dietrich, T., Svinkin, D. S., Almualla, M., Castro-Tirado, A. J., De, K., Dunwoody, R., Gatkine, P., Hammerstein, E., Iyyani, S., Mangan, J., Perley, D., Purkayastha, S., Bellm, E., Bhalerao, V., Bolin, B., Bulla, Mattia, Cannella, C., Chandra, P., Duev, D. A., Frederiks, D., Gal-Yam, A., Graham, M., Ho, A. Y. Q., Hurley, K., Karambelkar, V., Kool, E. C., Kulkarni, S. R., Mahabal, A., Masci, F., McBreen, S., Pandey, S. B., Reusch, S., Ridnaia, A., Rosnet, P., Rusholme, B., Carracedo, A. S., Smith, R., Soumagnac, M., Stein, R., Troja, E., Tsvetkova, A., Walters, R., and Valeev, A. F.

Abstract

Gamma-ray bursts (GRBs) are among the brightest and most energetic events in the Universe. The duration and hardness distribution of GRBs has two clusters1, now understood to reflect (at least) two different progenitors2. Short-hard GRBs (SGRBs; T90 < 2 s) arise from compact binary mergers, and long-soft GRBs (LGRBs; T90 > 2 s) have been attributed to the collapse of peculiar massive stars (collapsars)3. The discovery of SN 1998bw/GRB 980425 (ref. 4) marked the first association of an LGRB with a collapsar, and AT 2017gfo (ref. 5)/GRB 170817A/GW170817 (ref. 6) marked the first association of an SGRB with a binary neutron star merger, which also produced a gravitational wave. Here, we present the discovery of ZTF20abwysqy (AT2020scz), a fast-fading optical transient in the Fermi satellite and the Interplanetary Network localization regions of GRB 200826A; X-ray and radio emission further confirm that this is the afterglow. Follow-up imaging (at rest-frame 16.5 days) reveals excess emission above the afterglow that cannot be explained as an underlying kilonova, but which is consistent with being the supernova. Although the GRB duration is short (rest-frame T90 of 0.65 s), our panchromatic follow-up data confirm a collapsar origin. GRB 200826A is the shortest LGRB found with an associated collapsar; it appears to sit on the brink between a successful and a failed collapsar. Our discovery is consistent with the hypothesis that most collapsars fail to produce ultra-relativistic jets., Correction in Nature Astronomy Volume 5, Issue 11, Pages 1179, November 2021 DOI:10.1038/s41550-021-01501-1, Scopus:2-s2.0-85115240373QC 20220502

Published
2021
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31. DECam-GROWTH search for the faint and distant binary neutron star and neutron star-black hole mergers in O3a

Author

Anand, S., Andreoni, I., Goldstein, D. A., Kasliwal, M. M., Ahumada, T., Barnes, J., Bloom, J. S., Bulla, Mattia, Bradley Cenko, S., Cooke, J., Coughlin, M. W., Nugent, P. E., Singer, L. P., Anand, S., Andreoni, I., Goldstein, D. A., Kasliwal, M. M., Ahumada, T., Barnes, J., Bloom, J. S., Bulla, Mattia, Bradley Cenko, S., Cooke, J., Coughlin, M. W., Nugent, P. E., and Singer, L. P.

Abstract

Synoptic searches for the optical counterpart to a binary neutron star (BNS) or neutron star-black hole (NSBH) merger can pose significant challenges towards the discovery of kilonovae and performing multi-messenger science. In this work, we describe the advantage of a global multi-telescope network towards this end, with a particular focus on the key and complementary role the Dark Energy Camera (DECam) plays in multi-facility follow-up. We describe the Global Relay of Observatories Watching Transients Happen (GROWTH) Target-of-Opportunity (ToO) Marshal, a common web application we built to ingest events, plan observations, search for transient candidates, and retrieve performance summary statistics for all of the telescopes in our network. Our infrastructure enabled us to conduct observations of two events during O3a, S190426c and S190510g. Furthermore, our analysis of deep DECam observations of S190814bv conducted by the DESGW team, and access to a variety of global follow-up facilities allowed us to place meaningful constraints on the parameters of the kilonova and the merging binary. We emphasize the importance of a global telescope network in conjunction with a power telescope like DECam in performing searches for the counterparts to gravitational-wave sources., QC 20220608

Published
2021
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32. A tidal disruption event coincident with a high-energy neutrino

Author

Stein, R., Velzen, S.V., Kowalski, M., Franckowiak, A., Gezari, S., Miller-Jones, James, Frederick, S., Sfaradi, I., Bietenholz, M.F., Horesh, A., Fender, R., Garrappa, S., Ahumada, T., Andreoni, I., Belicki, J., Bellm, E.C., Böttcher, M., Brinnel, V., Burruss, R., Cenko, S.B., Coughlin, M.W., Cunningham, V., Drake, A., Farrar, G.R., Feeney, M., Foley, R.J., Gal-Yam, A., Golkhou, V.Z., Goobar, A., Graham, M.J., Hammerstein, E., Helou, G., Hung, T., Kasliwal, M.M., Kilpatrick, C.D., Kong, A.K.H., Kupfer, T., Laher, R.R., Mahabal, A.A., Masci, F.J., Necker, J., Nordin, J., Perley, D.A., Rigault, M., Reusch, S., Rodriguez, H., Rojas-Bravo, C., Rusholme, B., Shupe, D.L., Singer, L.P., Sollerman, J., Soumagnac, M.T., Stern, D., Taggart, K., van Santen, J., Ward, C., Woudt, P., Yao, Y., Stein, R., Velzen, S.V., Kowalski, M., Franckowiak, A., Gezari, S., Miller-Jones, James, Frederick, S., Sfaradi, I., Bietenholz, M.F., Horesh, A., Fender, R., Garrappa, S., Ahumada, T., Andreoni, I., Belicki, J., Bellm, E.C., Böttcher, M., Brinnel, V., Burruss, R., Cenko, S.B., Coughlin, M.W., Cunningham, V., Drake, A., Farrar, G.R., Feeney, M., Foley, R.J., Gal-Yam, A., Golkhou, V.Z., Goobar, A., Graham, M.J., Hammerstein, E., Helou, G., Hung, T., Kasliwal, M.M., Kilpatrick, C.D., Kong, A.K.H., Kupfer, T., Laher, R.R., Mahabal, A.A., Masci, F.J., Necker, J., Nordin, J., Perley, D.A., Rigault, M., Reusch, S., Rodriguez, H., Rojas-Bravo, C., Rusholme, B., Shupe, D.L., Singer, L.P., Sollerman, J., Soumagnac, M.T., Stern, D., Taggart, K., van Santen, J., Ward, C., Woudt, P., and Yao, Y.

Abstract

Cosmic neutrinos provide a unique window into the otherwise hidden mechanism of particle acceleration in astrophysical objects. The IceCube Collaboration recently reported the likely association of one high-energy neutrino with a flare from the relativistic jet of an active galaxy pointed towards the Earth. However a combined analysis of many similar active galaxies revealed no excess from the broader population, leaving the vast majority of the cosmic neutrino flux unexplained. Here we present the likely association of a radio-emitting tidal disruption event, AT2019dsg, with a second high-energy neutrino. AT2019dsg was identified as part of our systematic search for optical counterparts to high-energy neutrinos with the Zwicky Transient Facility. The probability of finding any coincident radio-emitting tidal disruption event by chance is 0.5%, while the probability of finding one as bright in bolometric energy flux as AT2019dsg is 0.2%. Our electromagnetic observations can be explained through a multizone model, with radio analysis revealing a central engine, embedded in a UV photosphere, that powers an extended synchrotron-emitting outflow. This provides an ideal site for petaelectronvolt neutrino production. Assuming that the association is genuine, our observations suggest that tidal disruption events with mildly relativistic outflows contribute to the cosmic neutrino flux.

Published
2021

33. Optical follow-up of the neutron star–black hole mergers S200105ae and S200115j

Author

Anand, S., Coughlin, M. W., Kasliwal, M. M., Bulla, Mattia, Ahumada, T., Sagués Carracedo, A., Almualla, M., Andreoni, I., Stein, R., Foucart, F., Singer, L. P., Sollerman, J., Bellm, E. C., Bolin, B., Caballero-García, M. D., Castro-Tirado, A. J., Cenko, S. B., De, K., Dekany, R. G., Duev, D. A., Feeney, M., Fremling, C., Goldstein, D. A., Golkhou, V. Z., Graham, M. J., Guessoum, N., Hankins, M. J., Hu, Y., Kong, A. K. H., Kool, E. C., Kulkarni, S. R., Kumar, H., Laher, R. R., Masci, F. J., Mróz, P., Nissanke, S., Porter, M., Reusch, S., Riddle, R., Rosnet, P., Rusholme, B., Serabyn, E., Sánchez-Ramírez, R., Rigault, M., Shupe, D. L., Smith, R., Soumagnac, M. T., Walters, R., Valeev, Azamat F., Anand, S., Coughlin, M. W., Kasliwal, M. M., Bulla, Mattia, Ahumada, T., Sagués Carracedo, A., Almualla, M., Andreoni, I., Stein, R., Foucart, F., Singer, L. P., Sollerman, J., Bellm, E. C., Bolin, B., Caballero-García, M. D., Castro-Tirado, A. J., Cenko, S. B., De, K., Dekany, R. G., Duev, D. A., Feeney, M., Fremling, C., Goldstein, D. A., Golkhou, V. Z., Graham, M. J., Guessoum, N., Hankins, M. J., Hu, Y., Kong, A. K. H., Kool, E. C., Kulkarni, S. R., Kumar, H., Laher, R. R., Masci, F. J., Mróz, P., Nissanke, S., Porter, M., Reusch, S., Riddle, R., Rosnet, P., Rusholme, B., Serabyn, E., Sánchez-Ramírez, R., Rigault, M., Shupe, D. L., Smith, R., Soumagnac, M. T., Walters, R., and Valeev, Azamat F.

Abstract

LIGO and Virgo’s third observing run revealed the first neutron star–black hole (NSBH) merger candidates in gravitational waves. These events are predicted to synthesize r-process elements1,2 creating optical/near-infrared ‘kilonova’ emission. The joint gravitational wave and electromagnetic detection of an NSBH merger could be used to constrain the equation of state of dense nuclear matter3, and independently measure the local expansion rate of the Universe4. Here, we present the optical follow-up and analysis of two of the only three high-significance NSBH merger candidates detected to date, S200105ae and S200115j, with the Zwicky Transient Facility5. The Zwicky Transient Facility observed ~48% of S200105ae and ~22% of S200115j’s localization probabilities, with observations sensitive to kilonovae brighter than −17.5 mag fading at 0.5 mag d−1 in the g- and r-bands; extensive searches and systematic follow-up of candidates did not yield a viable counterpart. We present state-of-the-art kilonova models tailored to NSBH systems that place constraints on the ejecta properties of these NSBH mergers. We show that with observed depths of apparent magnitude ~22 mag, attainable in metre-class, wide-field-of-view survey instruments, strong constraints on ejecta mass are possible, with the potential to rule out low mass ratios, high black hole spins and large neutron star radii., QC 20201117

Published
2020
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34. A kilometer-scale asteroid inside Venus's orbit

Author

Ip, W.-H., Bolin, B., Masci, F. J., Ye, Q.-Z., Kramer, E. A., Helou, G., Ahumada, T., Coughlin, M. W., Graham, M. J., Walters, R., Deshmukh, K. P., Fremling, C., Lin, Z.-Y., Milburn, J. W., Purdum, J. N., Quimby, R., Bodewits, D., Chang, C.-K., Ngeow, C.-C., Tan, H., Zhai, C., van Dokkum, P., Granvik, M., Harikane, Y., Mowla, L. A., Burdge, K. B., Bellm, E. C., De, K., Cenko, S. B., Copperwheat, C. M., Dekany, R., Duev, D. A., Hale, D., Kasliwal, M. M., Kulkarni, S. R., Kupfer, T., Mahabal, A., Mróz, P. J., Neill, J. D., Riddle, R., Rodriguez, H., Serabyn, E., Smith, R. M., Sollerman, J., Soumagnac, M. T., Southworth, J., Yan, L., Ip, W.-H., Bolin, B., Masci, F. J., Ye, Q.-Z., Kramer, E. A., Helou, G., Ahumada, T., Coughlin, M. W., Graham, M. J., Walters, R., Deshmukh, K. P., Fremling, C., Lin, Z.-Y., Milburn, J. W., Purdum, J. N., Quimby, R., Bodewits, D., Chang, C.-K., Ngeow, C.-C., Tan, H., Zhai, C., van Dokkum, P., Granvik, M., Harikane, Y., Mowla, L. A., Burdge, K. B., Bellm, E. C., De, K., Cenko, S. B., Copperwheat, C. M., Dekany, R., Duev, D. A., Hale, D., Kasliwal, M. M., Kulkarni, S. R., Kupfer, T., Mahabal, A., Mróz, P. J., Neill, J. D., Riddle, R., Rodriguez, H., Serabyn, E., Smith, R. M., Sollerman, J., Soumagnac, M. T., Southworth, J., and Yan, L.

Abstract

Near-Earth asteroid population models predict the existence of asteroids located inside the orbit of Venus. However, despite searches up to the end of 2019, none have been found. Here we report the discovery by the Zwicky Transient Facility of the first known asteroid located inside of Venus' orbit, 2020 AV₂, possessing an aphelion distance of 0.65 au and ∼2 km in size. While it is possible that 2020 AV₂ is the largest of its kind, we find that its discovery is surprising in the context of population models where the expected count is close to zero. If this discovery is not a statistical fluke, then 2020 AV₂ may come from a yet undiscovered source population of asteroids interior to Venus, and currently favored asteroid population models may need to be adjusted.

Published
2020

35. Zinc speciation in phosphate‐affected soils

Author

I. Ahumada T., A. Bustamante, and E. B. Schalscha

Subjects
chemistry.chemical_classification, Inceptisol, Soil Science, Mineralogy, chemistry.chemical_element, Soil chemistry, Fractionation, Vertisol, Zinc, Phosphate, Andosol, chemistry.chemical_compound, chemistry, Environmental chemistry, Organic matter, Agronomy and Crop Science
Abstract

Zinc (Zn) speciation was determined in a Zn pre‐treated Andosol, Inceptisol, and a Vertisol before and after adding phosphate. The fractions obtained, i.e., soluble, exchangeable, iron‐manganese (Fe‐Mn) bound, chelated and insoluble organic forms had a different distribution in the three soils. The exchangeable form predominated in the Andosol, followed by Fe‐Mn oxide bound Zn and minor amounts of the chelated forms, whereas Fe‐Mn oxide bound Zn was very abundant in the Inceptisol and Vertisol. Sizable amounts of the exchangeable form were also present. Phosphate pre‐treatment of the Inceptisol and Vertisol did not alter the distribution of the different forms of Zn, whereas in the Andosol the exchangeable as well as the Fe‐Mn oxide bound Zn increased markedly, chelated Zn also increased somewhat.

Published
1997
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40. Heavy metals in rivers and soils in central Chile

Author

Ahumada T., I. and Schalscha B., E.

Subjects
*WATER pollution, *COPPER, *HEAVY metals, *POLLUTION, *SEWAGE, *SOIL pollution
Abstract

Industrial and domestic waste waters in Chile are discharged withoutprevious treatment into rivers and other inland waters which are used to irrigate agricultural lands. The present study reports on results obtained when analyzing inland waters for Cd, Cu, Zn, Hg and As. Copper content was found to be high in most of the rivers studied and its sources were identifiable copper mining wastewaters. Cadmium and Zn levels are above accepted levels in some instances, whereas Hg and As content of river waters under study studied were found to be within accepted levels. The more reactive chemical forms of heavy metals in soils irrigated with polluted waters, as determined by sequential extraction, were found to be the most abundant ones. These forms are easily bio-available. (c) 1998 IAWQ. Published by Elsevier Science Ltd. [ABSTRACT FROM AUTHOR]

Published
1998
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41. Desarrollo y optimización de una metodología de extracción con disolvente presurizado de derivados de alquilfenoles en biósólidosy suelos aplicación en estudios de degradación y movilidad

Author

Maricán-Riquelme, Adolfo Andrés, Richter-D, Pablo, Ahumada-T, Inés, and Universidad de Chile

Abstract

Los lodos provenientes de plantas de tratamiento de aguas residuales, por sus características, pueden ser reutilizados en la agricultura, como mejoradores de suelos o reemplazo parcial de fertilizantes. Se caracterizan por tener un elevado porcentaje de materia orgánica, la cual puede interaccionar con una serie de compuestos orgánicos tóxicos a niveles traza, como hidrocarburos aromáticos policíclicos (PAHs), plaguicidas, bifenilos policlorados (PCBs), dioxinas y furanos (PCDD/F), compuestos orgánicos volátiles (VOCs), compuestos alifáticos halogenados, fenoles y detergentes. Dentro del grupo de los detergentes, se ha puesto énfasis especialmente en los etoxilatos de nonilfenol y octilfenol, y sus metabolitos, ya que son compuestos disruptores del sistema endocrino. Para su extracción se han propuesto varios métodos modernos alternativos al método tradicional de extracción Soxhlet, como la extracción por agitación ultrasónica (USE), extracción con fluidos supercríticos (SFE), extracción con disolventes acelerada (ASE) y extracción asistida por microondas (MAE o MASE), entre otras que han demostrado tener recuperaciones similares o mejores que la extracción Soxhlet. Estas metodologías tienen grandes ventajas comparativas con respecto a la extracción Soxhlet, como la rapidez en completar la extracción, y la menor cantidad de disolvente extractante y de muestra que son necesarios. En este estudio se propone el desarrollo de un método de determinación de etoxilatos de alquilfenoles y sus derivados en muestras de biosólidos, que incremente la eficiencia y rapidez en las etapas de preparación de la muestra, respecto de un sistema de extracción Soxhlet, incorpore energía adicional (temperatura-presión del disolvente), que asista el proceso de extracción. Asimismo, se busca la optimización de las variables para la extracción de etoxilatos de alquilfenol y sus metabolitos, nonilfenol y octilfenol, desde biosólidos, y desde suelos enmendados con biosólidos, mediante el empleo de modelos de diseño estadístico, a través del análisis multivariado. De esta forma, se integrarán las ventajas y posibilidades que ofrecen las metodologías innovadoras de preparación de muestra y la detección por GC-MS en sus diferentes modalidades, permitiendo de este modo la obtención de métodos analíticos de preparación de muestra más ventajosos, respecto de métodos más tradicionales, en términos de exactitud, precisión y rapidez. La metodología de extracción con disolventes presurizados en batch (ASE), fue la que presentó mejores recuperaciones. Las condiciones óptimas para esta metodología fueron: 129 °C, 34 minutos por ciclo, en dos ciclos, y disolvente de extracción, acetona. Comparativamente con la extracción Soxhlet, esta metodología optimizada resultó ser más eficiente, en cuanto al tiempo de extracción y cantidad de disolvente. La extracción de los analitos en estudio, por ambas metodologías fue: en el caso de 4-t-OP, 1 ,2±0, 1 mg·kg- 1 y 1 ,22±0,04 mg·kg-1 ; 4-NP, 204±20 mg·kg-1 y 298±7 mg·kg-\ 4-n-OP, 54±4 mg·kg-1 y 6,4±0,4 mg·kg-\ 4-0PE 16±1 mg·kg- 1 y 0,3±0,1 mg·kg- 1 ; y 4-NPE, 1053±23 mg·kg-1 y 621±18 mg·kg-\ para los sistemas ASE y Soxhlet, respectivamente. La metodología ASE optimizada tuvo mejores recuperaciones en el caso de 4-n-OP, 4-0PE y 4-NPE, mientras que la extracción Soxhlet fue mejor en el caso de 4-NP. En el caso de 4-t-OP, ambas metodologías son comparables. Una vez optimizado el método de determinación de 4-NP y 4-NPE, se aplicó en ensayos de movilidad en columnas de lixiviación y de biodisponibilidad con plantas de trigo. Se encontró que la movilidad de 4-NP y 4-NPE mostró ser relativamente moderada. De esta forma, tanto 4-NP, como 4-NPE, presentes en el biosólido, estarían disponibles para ser absorbidos por las plantas. La biodisponibilidad de los analitos seleccionados fue determinada mediante la extracción exhaustiva en muestras de trigo cultivado en suelo, con diferentes dosis de biosólido (B) y biosólido enriquecido (BE) con 4-NP. Los analitos encontrados en mayor concentración en el trigo son 4-NP y 4-NPE. En particular la concentración de 4-NP en trigo, varía entre 3 mg·kg-1 y 33 mg·kg·\ y la de 4- NPE entre 1 ,6 mg· kg-1 y 9,5 mg· kg-1 . Es posible afirmar que estos analitos estarían significativamente biodisponibles para el trigo, cultivado en suelo tratado con biosólido. La correlación entre el contenido de 4-NP en las plantas y fracción móvil determinada a través de columnas de lixiviación, mostró correlaciones satisfactorias, tanto para la parte radicular, como para la parte aérea de la planta. Doctor en Química TERMINADA PFCHA-Becas 160 p. PFCHA-Becas

Published
2011

42. Publisher Correction: A very luminous jet from the disruption of a star by a massive black hole.

Author

Andreoni I, Coughlin MW, Perley DA, Yao Y, Lu W, Cenko SB, Kumar H, Anand S, Ho AYQ, Kasliwal MM, de Ugarte Postigo A, Sagués-Carracedo A, Schulze S, Kann DA, Kulkarni SR, Sollerman J, Tanvir N, Rest A, Izzo L, Somalwar JJ, Kaplan DL, Ahumada T, Anupama GC, Auchettl K, Barway S, Bellm EC, Bhalerao V, Bloom JS, Bremer M, Bulla M, Burns E, Campana S, Chandra P, Charalampopoulos P, Cooke J, D'Elia V, Das KK, Dobie D, Fernández JFA, Freeburn J, Fremling C, Gezari S, Goode S, Graham MJ, Hammerstein E, Karambelkar VR, Kilpatrick CD, Kool EC, Krips M, Laher RR, Leloudas G, Levan A, Lundquist MJ, Mahabal AA, Medford MS, Miller MC, Möller A, Mooley KP, Nayana AJ, Nir G, Pang PTH, Paraskeva E, Perley RA, Petitpas G, Pursiainen M, Ravi V, Ridden-Harper R, Riddle R, Rigault M, Rodriguez AC, Rusholme B, Sharma Y, Smith IA, Stein RD, Thöne C, Tohuvavohu A, Valdes F, van Roestel J, Vergani SD, Wang Q, and Zhang J

Published
2023
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43. A very luminous jet from the disruption of a star by a massive black hole.

Author

Andreoni I, Coughlin MW, Perley DA, Yao Y, Lu W, Cenko SB, Kumar H, Anand S, Ho AYQ, Kasliwal MM, de Ugarte Postigo A, Sagués-Carracedo A, Schulze S, Kann DA, Kulkarni SR, Sollerman J, Tanvir N, Rest A, Izzo L, Somalwar JJ, Kaplan DL, Ahumada T, Anupama GC, Auchettl K, Barway S, Bellm EC, Bhalerao V, Bloom JS, Bremer M, Bulla M, Burns E, Campana S, Chandra P, Charalampopoulos P, Cooke J, D'Elia V, Das KK, Dobie D, Fernández JFA, Freeburn J, Fremling C, Gezari S, Goode S, Graham MJ, Hammerstein E, Karambelkar VR, Kilpatrick CD, Kool EC, Krips M, Laher RR, Leloudas G, Levan A, Lundquist MJ, Mahabal AA, Medford MS, Miller MC, Möller A, Mooley KP, Nayana AJ, Nir G, Pang PTH, Paraskeva E, Perley RA, Petitpas G, Pursiainen M, Ravi V, Ridden-Harper R, Riddle R, Rigault M, Rodriguez AC, Rusholme B, Sharma Y, Smith IA, Stein RD, Thöne C, Tohuvavohu A, Valdes F, van Roestel J, Vergani SD, Wang Q, and Zhang J

Abstract

Tidal disruption events (TDEs) are bursts of electromagnetic energy that are released when supermassive black holes at the centres of galaxies violently disrupt a star that passes too close 1 . TDEs provide a window through which to study accretion onto supermassive black holes; in some rare cases, this accretion leads to launching of a relativistic jet 2-9 , but the necessary conditions are not fully understood. The best-studied jetted TDE so far is Swift J1644+57, which was discovered in γ-rays, but was too obscured by dust to be seen at optical wavelengths. Here we report the optical detection of AT2022cmc, a rapidly fading source at cosmological distance (redshift z = 1.19325) the unique light curve of which transitioned into a luminous plateau within days. Observations of a bright counterpart at other wavelengths, including X-ray, submillimetre and radio, supports the interpretation of AT2022cmc as a jetted TDE containing a synchrotron 'afterglow', probably launched by a supermassive black hole with spin greater than approximately 0.3. Using four years of Zwicky Transient Facility 10 survey data, we calculate a rate of [Formula: see text] per gigapascals cubed per year for on-axis jetted TDEs on the basis of the luminous, fast-fading red component, thus providing a measurement complementary to the rates derived from X-ray and radio observations 11 . Correcting for the beaming angle effects, this rate confirms that approximately 1 per cent of TDEs have relativistic jets. Optical surveys can use AT2022cmc as a prototype to unveil a population of jetted TDEs., (© 2022. The Author(s), under exclusive licence to Springer Nature Limited.)

Published
2022
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44. Candidate Tidal Disruption Event AT2019fdr Coincident with a High-Energy Neutrino.

Author

Reusch S, Stein R, Kowalski M, van Velzen S, Franckowiak A, Lunardini C, Murase K, Winter W, Miller-Jones JCA, Kasliwal MM, Gilfanov M, Garrappa S, Paliya VS, Ahumada T, Anand S, Barbarino C, Bellm EC, Brinnel V, Buson S, Cenko SB, Coughlin MW, De K, Dekany R, Frederick S, Gal-Yam A, Gezari S, Giroletti M, Graham MJ, Karambelkar V, Kimura SS, Kong AKH, Kool EC, Laher RR, Medvedev P, Necker J, Nordin J, Perley DA, Rigault M, Rusholme B, Schulze S, Schweyer T, Singer LP, Sollerman J, Strotjohann NL, Sunyaev R, van Santen J, Walters R, Zhang BT, and Zimmerman E

Abstract

The origins of the high-energy cosmic neutrino flux remain largely unknown. Recently, one high-energy neutrino was associated with a tidal disruption event (TDE). Here we present AT2019fdr, an exceptionally luminous TDE candidate, coincident with another high-energy neutrino. Our observations, including a bright dust echo and soft late-time x-ray emission, further support a TDE origin of this flare. The probability of finding two such bright events by chance is just 0.034%. We evaluate several models for neutrino production and show that AT2019fdr is capable of producing the observed high-energy neutrino, reinforcing the case for TDEs as neutrino sources.

Published
2022
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