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13,358 results on '"ANDREWS, J."'

2. Winds of change: why binary black hole formation is metallicity dependent, while binary neutron star formation is not

Author

van Son, L. A. C., Roy, S. K., Mandel, I., Farr, W. M., Lam, A., Merritt, J., Broekgaarden, F. S., Sander, A., and Andrews, J. J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Both detailed and rapid population studies alike predict that binary black hole (BHBH) formation is orders of magnitude more efficient at low metallicity than high metallicity, while binary neutron star (NSNS) formation remains mostly flat with metallicity, and black hole-neutron star (BHNS) mergers show intermediate behavior. This finding is a key input to employ double compact objects as tracers of low-metallicity star formation, as spectral sirens, and for merger rate calculations. Yet, the literature offers various (sometimes contradicting) explanations for these trends. We investigate the dominant cause for the metallicity dependence of double compact object formation. We find that the BHBH formation efficiency at low metallicity is set by initial condition distributions, and conventional simulations suggest that about one in eight interacting binary systems with sufficient mass to form black holes will lead to a merging BHBH. We further find that the significance of metallicities in double compact object formation is a question of formation channel. The stable mass transfer and chemically homogeneous evolution channels mainly diminish at high metallicities due to changes in stellar radii, while the common envelope channel is primarily impacted by the combined effects of stellar winds and mass-scaled natal kicks. Outdated giant wind prescriptions exacerbate the latter effect, suggesting BHBH formation may be much less metallicity dependent than previously assumed. NSNS formation efficiency remains metallicity independent as they form exclusively through the common envelope channel, with natal kicks that are uncorrelated with mass. Forthcoming GW observations will provide valuable constraints on these findings, Comment: 14 pages, 8 Figures, Submitted to ApJ, Scripts and data to reproduce this work are at https://github.com/LiekeVanSon/ZdependentFormEff , and https://zenodo.org/records/13999532

Published
2024

3. The effect of mass loss in models of red supergiants in the Small Magellanic Cloud

Author

Zapartas, E., de Wit, S., Antoniadis, K., Muñoz-Sanchez, G., Souropanis, D., Bonanos, A. Z., Maravelias, G., Kovlakas, K., Kruckow, M. U., Fragos, T., Andrews, J. J., Bavera, S. S., Briel, M., Gossage, S., Kasdagli, E., Rocha, K. A., Sun, M., Srivastava, P. M., and Xing, Z.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The rate and mechanism of mass loss of red supergiants (RSGs) remain poorly understood, especially at low metallicities. Motivated by the new empirical prescription by Yang et al. 2023, based on the largest and most complete sample in the Small Magellanic Cloud, we investigate the impact of different popular and recent RSG mass-loss prescriptions that span a range of RSG mass-loss rates on the evolution and observable properties of single massive stars. Our results show that higher mass-loss rates result in earlier envelope stripping and shorter RSG lifetimes, particularly for the more luminous stars, leading to a steeper luminosity function and predicting hotter final positions for the SN progenitors. None of the considered mass-loss prescriptions is fully consistent with all observational constraints, highlighting ongoing uncertainties in deriving and modeling RSGs mass loss. The mass-loss rates suggested by Kee et al. predict rapid envelope stripping, inconsistent with the observed population of luminous RSGs and SN progenitor detections, while the models implementing the commonly used de Jager et al. and the recent Beasor et al. prescriptions overestimate the number of luminous RSGs. While the increased mass-loss rates for luminous RSGs predicted by Yang et al. lead to better agreement with the observed RSG luminosity function, naturally reproducing the updated Humphreys-Davidson limit, they also produce luminous yellow supergiant progenitors not detected in nearby supernovae. We also estimate that binary interactions tend to slightly increase the formation of luminous RSGs due to mass accretion or merging. Our study examines the impact of RSG mass loss during the late stages of massive stars, highlighting the significance of using comprehensive observational data, exploring the uncertainties involved, and considering the effects of binary-induced or episodic mass loss., Comment: submitted in A&A

Published
2024

4. Three Quenched, Faint Dwarf Galaxies in the Direction of NGC 300: New Probes of Reionization and Internal Feedback

Author

Sand, D. J., Mutlu-Pakdil, B., Jones, M. G., Karunakaran, A., Andrews, J. E., Bennet, P., Crnojevic, D., Donatiello, G., Drlica-Wagner, A., Fielder, C., Martinez-Delgado, D., Martinez-Vazquez, C. E., Spekkens, K., Doliva-Dolinsky, A., Hunger, L. C., Carlin, J. L., Cerny, W., Hai, T. N., McQuinn, K. B. W, Pace, A. B., and Smercina, A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We report the discovery of three faint and ultra-faint dwarf galaxies -- Sculptor A, Sculptor B and Sculptor C -- in the direction of NGC 300 (D=2.0 Mpc), a Large Magellanic Cloud-mass galaxy. Deep ground-based imaging with Gemini/GMOS resolves all three dwarf galaxies into stars, each displaying a red giant branch indicative of an old, metal-poor stellar population. No young stars or HI gas are apparent, and the lack of a GALEX UV detection suggests that all three systems are quenched. Sculptor C (D=2.04$^{+0.10}_{-0.13}$ Mpc; $M_V$=$-$9.1$\pm$0.1 mag or $L_V$=(3.7$^{+0.4}_{-0.3}$)$\times$10$^5$ $L_{\odot}$) is consistent with being a satellite of NGC 300. Sculptor A (D=1.35$^{+0.22}_{-0.08}$ Mpc; $M_V$=$-$6.9$\pm$0.3 mag or $L_V$=(5$^{+1}_{-1}$)$\times$10$^4$ $L_{\odot}$) is likely in the foreground of NGC 300 and at the extreme edge of the Local Group, analogous to the recently discovered ultra-faint Tucana B in terms of its physical properties and environment. Sculptor B (D=2.48$^{+0.21}_{-0.24}$ Mpc; $M_V$=$-$8.1$\pm$0.3 mag or $L_V$=(1.5$^{+0.5}_{-0.4}$)$\times$10$^5$ $L_{\odot}$) is likely in the background, but future distance measurements are necessary to solidify this statement. It is also of interest due to its quiescent state and low stellar mass. Both Sculptor A and B are $\gtrsim$2-4 $r_{vir}$ from NGC 300 itself. The discovery of three dwarf galaxies in isolated or low-density environments offers an opportunity to study the varying effects of ram pressure stripping, reionization and internal feedback in influencing the star formation history of the faintest stellar systems., Comment: 15 pages, 5 figures. ApJ Letters submitted

Published
2024

5. A study in scarlet -- II. Spectroscopic properties of a sample of Intermediate Luminosity Red Transients

Author

Valerin, G., Pastorello, A., Mason, E., Reguitti, A., Benetti, S., Cai, Y. -Z., Chen, T. -W., Eappachen, D., Elias-Rosa, N., Fraser, M., Gangopadhyay, A., Hsiao, E. Y., Howell, D. A., Inserra, C., Izzo, L., Jencson, J., Kankare, E., Kotak, R., Lundqvist, P., Mazzali, P. A., Misra, K., Pignata, G., Prentice, S. J., Sand, D. J., Smartt, S. J., Stritzinger, M. D., Tartaglia, L., Valenti, S., Anderson, J. P., Andrews, J. E., Amaro, R. C., Barbarino, C., Brennan, S., Bufano, F., Callis, E., Cappellaro, E., Dastidar, R., Della Valle, M., Fiore, A., Fulton, M. D., Galbany, L., Gromadzki, M., Heikkilä, T., Hiramatsu, D., Karamehmetoglu, E., Kuncarayakti, H., Leloudas, G., Limongi, M., Lundquist, M., McCully, C., Müller-Bravo, T. E., Nicholl, M., Ochner, P., Gonzalez, E. Padilla, Paraskeva, E., Pellegrino, C., Rau, A., Reichart, D. E., Reynolds, T. M., Roy, R., Salmaso, I., Shahbandeh, M., Singh, M., Sollerman, J., Turatto, M., Tomasella, L., Wyatt, S., and Young, D. R.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We investigate the spectroscopic characteristics of Intermediate Luminosity Red Transients (ILRTs), a class of elusive objects with peak luminosity between that of classical novae and standard supernovae. We present the extensive optical and near-infrared (NIR) spectroscopic monitoring of four ILRTs, namely NGC 300 2008OT-1, AT 2019abn, AT 2019ahd and AT 2019udc. First we focus on the evolution of the most prominent spectral features observed in the low resolution spectra, then we discuss more in detail the high resolution spectrum collected for NGC 300 2008OT-1 with the Very Large Telescope equipped with UVES. Finally we analyse late time spectra of NGC 300 2008OT-1 and AT 2019ahd through comparisons with both synthetic and observed spectra. Balmer and Ca lines dominate the optical spectra, revealing the presence of slowly moving circumstellar medium (CSM) around the objects. The line luminosity of H$\alpha$, H$\beta$ and Ca II NIR triplet presents a double peaked evolution with time, possibly indicative of interaction between fast ejecta and the slow CSM. The high resolution spectrum of NGC 300 2008OT-1 reveals a complex circumstellar environment, with the transient being surrounded by a slow ($\sim$30 km s$^{-1}$) progenitor wind. At late epochs, optical spectra of NGC 300 2008OT-1 and AT 2019ahd show broad ($\sim$2500 km s$^{-1}$) emission features at $\sim$6170 A and $\sim$7000 A which are unprecedented for ILRTs. We find that these lines originate most likely from the blending of several narrow lines, possibly of iron-peak elements., Comment: 28 pages, 19 figures. Submitted to A&A

Published
2024

6. A study in scarlet -- I. Photometric properties of a sample of Intermediate Luminosity Red Transients

Author

Valerin, G., Pastorello, A., Reguitti, A., Benetti, S., Cai, Y. -Z., Chen, T. -W., Eappachen, D., Elias-Rosa, N., Fraser, M., Gangopadhyay, A., Hsiao, E. Y., Howell, D. A., Inserra, C., Izzo, L., Jencson, J., Kankare, E., Kotak, R., Mazzali, P. A., Misra, K., Pignata, G., Prentice, S. J., Sand, D. J., Smartt, S. J., Stritzinger, M. D., Tartaglia, L., Valenti, S., Anderson, J. P., Andrews, J. E., Amaro, R. C., Brennan, S., Bufano, F., Callis, E., Cappellaro, E., Dastidar, R., Della Valle, M., Fiore, A., Fulton, M. D., Galbany, L., Heikkilä, T., Hiramatsu, D., Karamehmetoglu, E., Kuncarayakti, H., Leloudas, G., Lundquist, M., McCully, C., Müller-Bravo, T. E., Nicholl, M., Ochner, P., Gonzalez, E. Padilla, Paraskeva, E., Pellegrino, C., Reichart, D. E., Reynolds, T. M., Roy, R., Salmaso, I., Singh, M., Turatto, M., Tomasella, L., Wyatt, S., and Young, D. R.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We investigate the photometric characteristics of a sample of Intermediate Luminosity Red Transients (ILRTs), a class of elusive objects with peak luminosity between that of classical novae and standard supernovae. We present the multi-wavelength photometric follow-up of four ILRTs, namely NGC 300 2008OT-1, AT 2019abn, AT 2019ahd and AT 2019udc. Through the analysis and modelling of their spectral energy distribution and bolometric light curves we infer the physical parameters associated with these transients. All four objects display a single peaked light curve which ends in a linear decline in magnitudes at late phases. A flux excess with respect to a single black body emission is detected in the infrared domain for three objects in our sample, a few months after maximum. This feature, commonly found in ILRTs, is interpreted as a sign of dust formation. Mid infrared monitoring of NGC 300 2008OT-1 761 days after maximum allows us to infer the presence of $\sim$10$^{-3}$-10$^{-5}$ M$_{\odot}$ of dust, depending on the chemical composition and the grain size adopted. The late time decline of the bolometric light curves of the considered ILRTs is shallower than expected for $^{56}$Ni decay, hence requiring an additional powering mechanism. James Webb Space Telescope observations of AT 2019abn prove that the object has faded below its progenitor luminosity in the mid-infrared domain, five years after its peak. Together with the disappearance of NGC 300 2008OT-1 in Spitzer images seven years after its discovery, this supports the terminal explosion scenario for ILRTs. With a simple semi-analytical model we try to reproduce the observed bolometric light curves in the context of few M$_{\odot}$ of material ejected at few 10$^{3}$ km s$^{-1}$ and enshrouded in an optically thick circumstellar medium., Comment: 21 pages, 15 figures plus 20 additional pages of data in appendix. Submitted to A&A

Published
2024

7. Crowdsourcing with Enhanced Data Quality Assurance: An Efficient Approach to Mitigate Resource Scarcity Challenges in Training Large Language Models for Healthcare

Author

Barai, P., Leroy, G., Bisht, P., Rothman, J. M., Lee, S., Andrews, J., Rice, S. A., and Ahmed, A.

Subjects
Computer Science - Computation and Language, Computer Science - Artificial Intelligence
Abstract

Large Language Models (LLMs) have demonstrated immense potential in artificial intelligence across various domains, including healthcare. However, their efficacy is hindered by the need for high-quality labeled data, which is often expensive and time-consuming to create, particularly in low-resource domains like healthcare. To address these challenges, we propose a crowdsourcing (CS) framework enriched with quality control measures at the pre-, real-time-, and post-data gathering stages. Our study evaluated the effectiveness of enhancing data quality through its impact on LLMs (Bio-BERT) for predicting autism-related symptoms. The results show that real-time quality control improves data quality by 19 percent compared to pre-quality control. Fine-tuning Bio-BERT using crowdsourced data generally increased recall compared to the Bio-BERT baseline but lowered precision. Our findings highlighted the potential of crowdsourcing and quality control in resource-constrained environments and offered insights into optimizing healthcare LLMs for informed decision-making and improved patient care., Comment: Published in AMIA Summit, Boston, 2024. https://knowledge.amia.org/Info2024/pdf/Info2024a022/Info2024fl021

Published
2024

8. A JWST Medium Resolution MIRI Spectrum and Models of the Type Ia supernova 2021aefx at +415 d

Author

Ashall, C., Hoeflich, P., Baron, E., Shahbandeh, M., DerKacy, J. M., Medler, K., Shappee, B. J., Tucker, M. A., Fereidouni, E., Mera, T., Andrews, J., Baade, D., Bostroem, K. A., Brown, P. J., Burns, C. R., Burrow, A., Cikota, A., de Jaeger, T., Do, A., Dong, Y., Dominguez, I., Fox, O., Galbany, L., Hsiao, E. Y., Krisciunas, K., Khaghani, B., Kumar, S., Lu, J., Maund, J. R., Mazzali, P., Morrell, N., Patat, F., Pfeffer, C., Phillips, M. M., Schmidt, J., Stangl, S., Stevens, C. P., Stritzinger, M. D., Suntzeff, N. B., Telesco, C. M., Wang, L., and Yang, Y.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present a JWST MIRI/MRS spectrum (5-27 $\mathrm{\mu}$m) of the Type Ia supernova (SN Ia), SN 2021aefx at $+415$ days past $B$-band maximum. The spectrum, which was obtained during the iron-dominated nebular phase, has been analyzed in combination with previous JWST observations of SN 2021aefx, to provide the first JWST time series analysis of an SN Ia. We find the temporal evolution of the [Co III] 11.888 $\mathrm{\mu}$m feature directly traces the decay of $^{56}$Co. The spectra, line profiles, and their evolution are analyzed with off-center delayed-detonation models. Best fits were obtained with White Dwarf (WD) central densities of $\rho_c=0.9-1.1\times 10^9$g cm$^{-3}$, a WD mass of M$_{\mathrm{WD}}$=1.33-1.35M$_\odot$, a WD magnetic field of $\approx10^6$G, and an off-center deflagration-to-detonation transition at $\approx$ 0.5 $M_\odot$ seen opposite to the line of sight of the observer (-30). The inner electron capture core is dominated by energy deposition from $\gamma$-rays whereas a broader region is dominated by positron deposition, placing SN 2021aefx at +415 d in the transitional phase of the evolution to the positron-dominated regime. The formerly `flat-tilted' profile at 9 $\mathrm{\mu}$m now has significant contribution from [Ni IV], [Fe II], and [Fe III] and less from [Ar III], which alters the shape of the feature as positrons excite mostly the low-velocity Ar. Overall, the strength of the stable Ni features in the spectrum is dominated by positron transport rather than the Ni mass. Based on multi-dimensional models, our analysis is consistent with a single-spot, close-to-central ignition with an indication for a pre-existing turbulent velocity field, and excludes a multiple-spot, off-center ignition., Comment: Accepted for publication in ApJ

Published
2024

9. Clinical Meaningfulness in Alzheimer’s Disease Clinical Trials. A Report from the EU-US CTAD Task Force

Author

Angioni, D., Cummings, J., Lansdall, C. J., Middleton, L., Sampaio, C., Gauthier, S., Cohen, S., Petersen, R. C., Rentz, D. M., Wessels, A. M., Hendrix, S. B., Jessen, F., Carrillo, M. C., Doody, R. S., Irizarry, M., Andrews, J. S., Vellas, B., Aisen, P., Andrieu, Sandrine, Bateman, Randall, Batrla, Richard, Bell, Joanne, Bosson, Oskar, Bozeat, Sasha, Brooks, Dawn, Haeberlein, Samantha Budd, Buracchio, Teresa, Cho, Min, Choung, Matthew, Cook, Gavin, Crisitello, Darrin, Dangond, Fernando, de Santi, Susan, Dennehy, Ellen, Dhadda, Shobha, Dhillon, Harjeet, Dunn, Billy, Egan, Michael, Elwood, Fiona, Eriksson, Sven, Fagan, Tom, Fillit, Howard, Freskgard, Per-Ola, Gallagher, Diana, Gangi, Gopi, Granda, Carlos, Greeley, David, Gronblad, Anna-Kaija, Hampel, Harald, Hawthorne, Paul, Henley, David, Herring, Joe, Hersch, Steve, Holt, Bill, Iwatsubo, Takeshi, Jones, Daryl, Kahl, Anja, Kinney, Gene, Kolb, Hartmuth, Kramer, Lynn, Kulic, Luka, Kumar, Sanjay, Lannfelt, Lars, Lawson, John, Legrand, Valérie, Lenington, Rachel, Longo, Frank, Matthews, Brandy, Masterman, Donna, McLinden, Kristina, Mikels, Sarah, Miller, Michael, Mintun, Mark, Moebius, Hans, Monteiro, Cecilia, Morken, Mario, Murphy, Jennifer, Odergren, Tomas, Osswald, Gunilla, Parnas, Laura, Patru, Maria-Magdalena, Prazma, Charlene, Raman, Rema, Reyderman, Larisa, Rogers, Sharon, Roman, Lise, Romano, Gary, Roskey, Mark, Rubino, Ivana, Ryan, Laurie, Salloway, Stephen, Schindler, Rachel, Schneider, Lon, Scott, David, Sims, John, Skovronsky, Daniel, Soto, Marion, Sperling, Reisa, Steukers, Lennert, Stoops, Erik, Strittmatter, Stephen, Tahami, Amir, Tamagnan, Gilles, Tariot, Gilles, Toloue, Masoud, Touchon, Jacques, Vanmechelen, Eugeen, Walt, Len, Weinberg, Mark, Weiner, Michael, White, Anne, Wiesel, Iris, Wilson, David, Yarenis, Lisa, Zago, Wagner, and Zhou, Jin

Published
2024
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10. JWST NIRSpec+MIRI Observations of the nearby Type IIP supernova 2022acko

Author

Shahbandeh, M., Ashall, C., Hoeflich, P., Baron, E., Fox, O., Mera, T., DerKacy, J., Stritzinger, M. D., Shappee, B., Law, D., Morrison, J., Pauly, T., Pierel, J., Medler, K., Andrews, J., Baade, D., Bostroem, A., Brown, P., Burns, C., Burrow, A., Cikota, A., Cross, D., Davis, S., de Jaeger, T., Do, A., Dong, Y., Hsiao, E., Dominguez, I., Galbany, L., Janzen, D., Jencson, J., Hoang, E., Karamehmetoglu, E., Khaghani, B., Krisciunas, K., Kumar, S., Lu, J., Mazzali, P., Morrell, N., Patat, F., Pearson, J., Pfeffer, C., Wang, L., Yang, Y., Cai, Y. Z., Camacho-Neves, Y., Elias-Rosa, N., Lundquist, M., Maund, J., Phillips, M., Rest, A., Retamal, N., Stangl, S., Shrestha, M., Stevens, C., Suntzeff, N., Telesco, C., Tucker, M., Foley, R., Jha, S., Kwok, L., Larison, C., LeBaron, N., Moran, S., Rho, J., Salmaso, I., Schmidt, J., and Tinyanont, S.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present JWST spectral and photometric observations of the Type IIP supernova (SN) 2022acko at ~50 days past explosion. These data are the first JWST spectral observations of a core-collapse SN. We identify ~30 different H I features, other features associated with products produced from the CNO cycle, and s-process elements such as Sc II and Ba II. By combining the JWST spectra with ground-based optical and NIR spectra, we construct a full Spectral Energy Distribution from 0.4 to 25 microns and find that the JWST spectra are fully consistent with the simultaneous JWST photometry. The data lack signatures of CO formation and we estimate a limit on the CO mass of < 10^{-8} solar mass. We demonstrate how the CO fundamental band limits can be used to probe underlying physics during stellar evolution, explosion, and the environment. The observations indicate little mixing between the H envelope and C/O core in the ejecta and show no evidence of dust. The data presented here set a critical baseline for future JWST observations, where possible molecular and dust formation may be seen.

Published
2024

11. 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

12. JWST MIRI/MRS Observations and Spectral Models of the Under-luminous Type Ia Supernova 2022xkq

Author

DerKacy, J. M., Ashall, C., Hoeflich, P., Baron, E., Shahbandeh, M., Shappee, B. J., Andrews, J., Baade, D., Balangan, E. F, Bostroem, K. A., Brown, P. J., Burns, C. R., Burrow, A., Cikota, A., de Jaeger, T., Do, A., Dong, Y., Dominguez, I., Fox, O., Galbany, L., Hoang, E. T., Hsiao, E. Y., Janzen, D., Jencson, J. E., Krisciunas, K., Kumar, S., Lu, J., Lundquist, M., Evans, T. B. Mera, Maund, J. R., Mazzali, P., Medler, K., Retamal, N. E. Meza, Morrell, N., Patat, F., Pearson, J., Phillips, M. M., Shrestha, M., Stangl, S., Stevens, C. P., Stritzinger, M. D., Suntzeff, N. B., Telesco, C. M., Tucker, M. A., Valenti, S., Wang, L., and Yang, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present a JWST mid-infrared spectrum of the under-luminous Type Ia Supernova (SN Ia) 2022xkq, obtained with the medium-resolution spectrometer on the Mid-Infrared Instrument (MIRI) $\sim130$ days post-explosion. We identify the first MIR lines beyond 14 $\mu$m in SN Ia observations. We find features unique to under-luminous SNe Ia, including: isolated emission of stable Ni, strong blends of [Ti II], and large ratios of singly ionized to doubly ionized species in both [Ar] and [Co]. Comparisons to normal-luminosity SNe Ia spectra at similar phases show a tentative trend between the width of the [Co III] 11.888 $\mu$m feature and the SN light curve shape. Using non-LTE-multi-dimensional radiation hydro simulations and the observed electron capture elements we constrain the mass of the exploding white dwarf. The best-fitting model shows that SN 2022xkq is consistent with an off-center delayed-detonation explosion of a near-Chandrasekhar mass WD (M$_{\rm ej}$ $\approx 1.37$ M$_{\odot}$) of high-central density ($\rho_c \geq 2.0\times10^{9}$ g cm$^{-3}$) seen equator on, which produced M($^{56}$Ni) $= 0.324$ M$_{\odot}$ and M($^{58}$Ni) $\geq 0.06$ M$_{\odot}$. The observed line widths are consistent with the overall abundance distribution; and the narrow stable Ni lines indicate little to no mixing in the central regions, favoring central ignition of sub-sonic carbon burning followed by an off-center DDT beginning at a single point. Additional observations may further constrain the physics revealing the presence of additional species including Cr and Mn. Our work demonstrates the power of using the full coverage of MIRI in combination with detailed modeling to elucidate the physics of SNe Ia at a level not previously possible., Comment: 31 pages, 18 figures, accepted to ApJ; updated to accepted version

Published
2023

13. Keck Infrared Transient Survey I: Survey Description and Data Release 1

Author

Tinyanont, S., Foley, R. J., Taggart, K., Davis, K. W., LeBaron, N., Andrews, J. E., Bustamante-Rosell, M. J., Camacho-Neves, Y., Chornock, R., Coulter, D. A., Galbany, L., Jha, S. W., Kilpatrick, C. D., Kwok, L. A., Larison, C., Pierel, J. R., Siebert, M. R., Aldering, G., Auchettl, K., Bloom, J. S., Dhawan, S., Filippenko, A. V., French, K. D., Gagliano, A., Grayling, M., Jacobson-Galán, W. V., Jones, D. O., Saux, X. Le, Macias, P., Mandel, K. S., McCully, C., Gonzalez, E. Padilla, Rest, A., Rojas-Bravo, C., Skrutskie, M. F., Thorp, S., Wang, Q., and Ward, S. M.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present the Keck Infrared Transient Survey (KITS), a NASA Key Strategic Mission Support program to obtain near-infrared (NIR) spectra of astrophysical transients of all types, and its first data release, consisting of 105 NIR spectra of 50 transients. Such a data set is essential as we enter a new era of IR astronomy with the James Webb Space Telescope (JWST) and the upcoming Nancy Grace Roman Space Telescope (Roman). NIR spectral templates will be essential to search JWST images for stellar explosions of the first stars and to plan an effective Roma} SN Ia cosmology survey, both key science objectives for mission success. Between 2022 February and 2023 July, we systematically obtained 274 NIR spectra of 146 astronomical transients, representing a significant increase in the number of available NIR spectra in the literature. The first data release includes data from the 2022A semester. We systematically observed three samples: a flux-limited sample that includes all transients $<$17 mag in a red optical band (usually ZTF r or ATLAS o bands); a volume-limited sample including all transients within redshift $z < 0.01$ ($D \approx 50$ Mpc); and an SN Ia sample targeting objects at phases and light-curve parameters that had scant existing NIR data in the literature. The flux-limited sample is 39% complete (60% excluding SNe Ia), while the volume-limited sample is 54% complete and is 79% complete to $z = 0.005$. All completeness numbers will rise with the inclusion of data from other telescopes in future data releases. Transient classes observed include common Type Ia and core-collapse supernovae, tidal disruption events (TDEs), luminous red novae, and the newly categorized hydrogen-free/helium-poor interacting Type Icn supernovae. We describe our observing procedures and data reduction using Pypeit, which requires minimal human interaction to ensure reproducibility.

Published
2023

14. Index

Author

Andrews, J. Cutler

Published
2011

18. Cover

Author

Andrews, J. Cutler

Published
2011

28. 24. Thirty

Author

Andrews, J. Cutler

Published
2011

29. Notes

Author

Andrews, J. Cutler

Published
2011

43. Foreword

Author

Andrews, J. Cutler

Published
2011

48. Evidence for late-time dust formation in the ejecta of supernova SN~1995N from emission-line asymmetries

Author

Wesson, R., Bevan, A. M., Barlow, M. J., De Looze, I., Matsuura, M., Clayton, G., and Andrews, J.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present a study of the dust associated with the core-collapse supernova SN~1995N. Infrared emission detected 14--15 years after the explosion was previously attributed to thermally echoing circumstellar material associated with the SN progenitor. We argue that this late-time emission is unlikely to be an echo, and is more plausibly explained by newly formed dust in the supernova ejecta, indirectly heated by the interaction between the ejecta and the CSM. Further evidence in support of this scenario comes from emission line profiles in spectra obtained 22 years after the explosion; these are asymmetric, showing greater attenuation on the red wing, consistent with absorption by dust within the expanding ejecta. The spectral energy distribution and emission line profiles at epochs later than $\sim$5000 days are both consistent with the presence of about 0.4~M$_\odot$ of amorphous carbon dust. The onset of dust formation is apparent in archival optical spectra, taken between 700 and 1700 days after the assumed explosion date. As this is considerably later than most other instances where the onset of dust formation has been detected, we argue that the explosion date must be later than previously assumed., Comment: 14 pages, 16 figures. Accepted for publication in Monthly Notices of the Royal Astronomical Society

Published
2023

49. Statistical inference for sketching algorithms

Author

Browne, R. P. and Andrews, J. L.

Subjects
Statistics - Methodology
Abstract

Sketching algorithms use random projections to generate a smaller sketched data set, often for the purposes of modelling. Complete and partial sketch regression estimates can be constructed using information from only the sketched data set or a combination of the full and sketched data sets. Previous work has obtained the distribution of these estimators under repeated sketching, along with the first two moments for both estimators. Using a different approach, we also derive the distribution of the complete sketch estimator, but additionally consider the error term under both repeated sketching and sampling. Importantly, we obtain pivotal quantities which are based solely on the sketched data set which specifically not requiring information from the full data model fit. These pivotal quantities can be used for inference on the full data set regression estimates or the model parameters. For partial sketching, we derive pivotal quantities for a marginal test and an approximate distribution for the partial sketch under repeated sketching or repeated sampling, again avoiding reliance on a full data model fit. We extend these results to include the Hadamard and Clarkson-Woodruff sketches then compare them in a simulation study.

Published
2023

50. The LHCb upgrade I

Author

LHCb collaboration, Aaij, R., Abdelmotteleb, A. S. W., Beteta, C. Abellan, Abudinén, F., Achard, C., Ackernley, T., Adeva, B., Adinolfi, M., Adlarson, P., Afsharnia, H., Agapopoulou, C., Aidala, C. A., Ajaltouni, Z., Akar, S., Akiba, K., Albicocco, P., Albrecht, J., Alessio, F., Alexander, M., Albero, A. Alfonso, Aliouche, Z., Cartelle, P. Alvarez, Amalric, R., Amato, S., Amey, J. L., Amhis, Y., An, L., Anderlini, L., Andersson, M., Andreani, A., Andreianov, A., Andreotti, M., Andreou, D., Andrews, J. E., Anelli, M., Anjam, A., Ao, D., Archilli, F., Arnaud, K., Artamonov, A., Artuso, M., Ashby, J., Aslanides, E., Atzeni, M., Audurier, B., Rocha, D. Ayres, Perea, I. B Bachiller, Bachmann, S., Bachmayer, M., Back, J. J., Bailly-reyre, A., Rodriguez, P. Baladron, Balagura, V., Balbi, G., Baldini, W., Balla, A., Baltazar, M., Band, H., Leite, J. Baptista de Souza, Barbetti, M., Barclay, P., Barlow, R. J., Barsuk, S., Barter, W., Bartolini, M., Baryshnikov, F., Basels, J. M., Bassi, G., Baszczyk, M., Lopes, J. C. Batista, Batsukh, B., Battig, A., Bay, A., Beck, A., Becker, M., Bedeschi, F., Bediaga, I. B., Beigbeder-Beau, C., Beiter, A., Belin, S., Bellee, V., Belous, K., Belov, I., Belyaev, I., Benane, G., Bencivenni, G., Benettoni, M., Ben-Haim, E., Berezhnoy, A., Bernard, F., Bernet, R., Andres, S. Bernet, Berninghoff, D., Bernstein, H. C., Bertella, C., Bertolin, A., Betancourt, C., Betti, F., Bezshyiko, Ia., Bezshyyko, O., Bhasin, S., Bhom, J., Bian, L., Bieker, M. S., Biesuz, N. V., Billoir, P., Biolchini, A., Birch, M., Bishop, F. C. R., Bitadze, A., Bizzeti, A., Blago, M. P., Blake, T., Blanc, F., Blank, J. E., Blusk, S., Bobulska, D., Bochin, B., Boelhauve, J. A., Garcia, O. Boente, Boettcher, T., Bogdanova, G., Boiaryntseva, I., Boldyrev, A., Bolognani, C. S., Bolzonella, R., Bondar, N., Booth, M. J., Borgato, F., Borghi, S., Borsato, M., Borsuk, J. T., Boterenbrood, H., Bouchiba, S. A., Bowcock, T. J. V., Boyaryntsev, A., Boyer, A., Bozzi, C., Bradley, M. J., Braun, S., Rodriguez, A. Brea, Bregliozzi, G., Bridges, K., Briere, M. M. J., Brock, M., Brodski, M., Brodzicka, J., Gonzalo, A. Brossa, Brown, C., Brown, J., Brummitt, A. J., Brundu, D., Brunetti, L., Buda, L., Buonaura, A., Buonincontri, L., Burke, A. T., Burmistrov, L., Burr, C., Bursche, A., Butkevich, A., Butter, J. S., Buytaert, J., Byczynski, W., Cachemiche, J. P., Cadeddu, S., Cai, H., Caillet, A., Calabrese, R., Calefice, L., Calegari, D., Cali, S., Calvi, M., Gomez, M. Calvo, Campana, P., Perez, D. H. Campora, Quezada, A. F. Campoverde, Canfer, S., Capelli, S., Capriotti, L., Carassiti, V., Carbone, A., Cardinale, R., Cardini, A., Carletti, M., Carniti, P., Carroll, J., Carus, L., Vidal, A. Casais, Caspary, R., Casse, G., Cattaneo, M., Cavallero, G., Cavallini, V., Ceelie, L., Celani, S., Cerasoli, J., Cervenkov, D., Cesare, S., Chadaj, B., Chadwick, A. J., Chahrour, I., Chanal, H., Chapman, M. G., Charles, M., Charpentier, Ph., Chaumat, V. J., Barajas, C. A. Chavez, Chefdeville, M., Chen, C., Chen, S., Chernov, A., Chernov, E., Chernyshenko, S., Chiozzi, S., Chobanova, V., Cholak, S., Chrzaszcz, M., Chubykin, A., Chulikov, V., Ciambrone, P., Cicala, M. F., Vidal, X. Cid, Ciezarek, G., Cifra, P., Citterio, M., Ciullo, G., Clark, K., Clarke, P. E. L., Clemencic, M., Cliff, H. V., Closier, J., Cobbledick, J. L., Coco, V., Coelli, S., Cogan, J., Cogneras, E., Cojocariu, L., Collins, P., Colombo, T., Congedo, L., Conti, N., Contu, A., Cooke, N., Corredoira, I., Corti, G., Ramusino, A. Cotta, Couturier, B., Cowan, G. A., Craik, D. C., Torres, M. Cruz, Currie, R., Da Silva, C. L., Dadabaev, S., Dai, L., Dai, X., Dall'Occo, E., Dalseno, J., D'Ambrosio, C., Damen, A., Daniel, J., Danilina, A., d'Argent, P., Daudon, F., Davies, J. E., Davis, A., Davis, J., Francisco, O. De Aguiar, De Benedetti, F., de Boer, J., De Bruyn, K., De Capua, S., De Cian, M., Da Graca, U. De Freitas Carneiro, De Lucia, E., De Miranda, J. M., de Oliveira, R., De Paula, L., De Roo, K., De Serio, M., De Simone, D., De Simone, P., De Vellis, F., de Vries, J. A., De Wit, E., Dean, C. T., Debernardis, F., Decamp, D., Deckenhoff, M., Dedu, V., Del Buono, L., Delaney, B., Dembinski, H. -P., Denis, C., Denysenko, V., Deschamps, O., Dettori, F., Dey, B., Di Bari, D., Di Nezza, P., Diachkov, I., Didenko, S., Maronas, L. Dieste, Dijkstra, H., Ding, S., Dobishuk, V., Doets, M., Doherty, F., Dolmatov, A., Domke, M., Dong, C., Donohoe, A. M., Dordei, F., Dorosz, P., Reis, A. C. dos, Douglas, L., Downes, A. G., Duarte, O., Duda, P., Dudek, M. W., Dufour, L., Duk, V., Dumps, R., Durante, P., Duras, M. M., Durham, J. M., Dutta, D., Duval, P. Y., Dziewiecki, M., Dziurda, A., Dzyuba, A., Easo, S., Egede, U., Egorychev, V., Orro, C. Eirea, Eisenhardt, S., Ejopu, E., Ekelhof, R., Ek-In, S., Eklund, L., Elashri, M. E, Ellbracht, J., Elvin, A., Ely, S., Ene, A., Epple, E., Escher, S., Eschle, J., Esen, S., Evans, T., Fabiano, F., Falcao, L. N., Fan, Y., Fang, B., Fantini, L., Faria, M., Farry, S., Fazzini, D., Felkowski, L. F, Feo, M., Declara, P. Fernandez, Gomez, M. Fernandez, Fernez, A. D., Ferrari, F., Ferreira, R., Lopes, L. Ferreira, Rodrigues, F. Ferreira, Sole, S. Ferreres, Ferrillo, M., Ferro-Luzzi, M., Filippov, S., Fini, R. A., Fiorini, M., Firlej, M., Fischer, K. M., Fitzgerald, D. S., Fitzpatrick, C., Fiutowski, T., Fleuret, F., Flores, L., Fontana, M., Fontanelli, F., Forty, R., Foulds-Holt, D., Fournier, C., Lima, V. Franco, Sevilla, M. Franco, Frank, M., Franzoso, E., Frau, G., Freestone, J., Frei, C., Frei, R., Frelier, J., Friday, D. A., Frontini, L. F, Fu, J., Fuehring, Q., Fulghesu, T., Fuzipeg, C., Gabriel, E., Galati, G., Galati, M. D., Galka, M., Torreira, A. Gallas, Galli, D., Gallorini, S., Gambetta, S., Gan, Y., Gandelman, M., Gandini, P., Gao, R., Gao, Y., Garau, M., Martin, L. M. Garcia, Moreno, P. Garcia, Pardiñas, J. García, Plana, B. Garcia, Rosales, F. A. Garcia, Garrido, L., Garroum, N., Garsed, P. J., Gascon, D., Gaspar, C., Gasq, C., Gatta, M., Gavardi, L., Gebolis, P. M., Geertsema, R. E., Gerick, D., Gerken, L. L., Germann, D., Gersabeck, E., Gersabeck, M., Gershon, T., Getz, S. A., Giambastiani, L., Gibson, V., Giemza, H. K., Gilman, A. L., Giovannetti, M., Gioventù, A., Girard, O. G., Gironell, P. Gironella, Giugliano, C., Giza, M. A., Gizdov, K., Gkougkousis, E. L., Gligorov, V. V., Göbel, C., Golinka-Bezshyyko, L., Golobardes, E., Golubkov, D., Golutvin, A., Gomes, A., Fernandez, S. Gomez, Abrantes, F. Goncalves, Goncerz, M., Gong, G., Gorelov, I. V., Gotti, C., Grabowski, J. P., Grammatico, T., Cardoso, L. A. Granado, Grant, F., Graugés, E., Graverini, E., Graziani, G., Grecu, A. T., Greeven, L. M., Greim, R., Grieser, N. A., Grillo, L., Gromov, S., Gromov, V., Grub, N., Cazon, B. R. Gruberg, Grynyov, B., Gu, C., Guarise, M., Guerin, S., Guittiere, M., Günther, P. A., Gushchin, E., Guth, A., Guz, Y., Gys, T., Hachon, F., Hadavizadeh, T., Hadjivasiliou, C., Haefeli, G., Haen, C., Haimberger, J., Haines, S. C., Halewood-leagas, T., Halvorsen, M. M., Hamilton, P. M., Hammerich, J., Hamrat, S., Han, Q., Han, X., Hansen, E. B., Hansmann-Menzemer, S., Hao, L., Harnew, N., Harrison, T., Hasse, C., Hatch, M., He, J., Heijhoff, K., Hemmer, F. H, Henderson, C., Henderson, R. D. L., Hennequin, A. M., Hennessy, K., Henry, L., Herd, J., Herold, T., Heuel, J., Hicheur, A., Hill, D., Hilton, M., Hoft, G. T., Hollitt, S. E., Hopchev, P. H., Hornberger, O., Horswill, J., Hou, R., Hou, Y., Hu, J., Hu, W., Hu, X., Huang, W., Huang, X., Hulsbergen, W., Hummel, S., Hunter, R. J., Hushchyn, M., Hutanu, O. E., Hutchcroft, D., Hynds, D., Ibis, P., Idzik, M., Ilin, D., Ilten, P., Inglessi, A., Iniukhin, A., Insa, C., Ishteev, A., Ivshin, K., Jacobsson, R., Jage, H., Elles, S. J. Jaimes, Jakobsen, S., Jamet, O., Jans, E., Jashal, B. K., Jaspers, M., Jawahery, A., Jevaud, M., Jevtic, V., Jiang, E., Jiang, X., Jiang, Y., John, D., John, M., Johnson, D., Jones, C. R., Jones, T. P., Jost, B., Jurik, N., Juszczak, I., Kandybei, S., Kang, Y., Karacson, M., Kariuki, J. M., Karpenkov, D., Karpinski, W., Karpov, M., Kaufmann, K., Kautz, J. W., Kayzel, F., Keizer, F., Keller, D. M., Kenzie, M., Ketel, T., Khanji, B., Kharisova, A., Kholodenko, S., Khreich, G., Kirn, T., Kirsebom, V. S., Kitouni, O., Klaver, S., Kleijne, N., Klimaszewski, K., Kmiec, M. R., Kok, H., Koliiev, S., Kolk, L., Kondybayeva, A., Konoplyannikov, A., Kopciewicz, P., Kopecna, R., Koppenburg, P., Korolev, M., Kos, J., Kostiuk, I., Kot, O., Kotriakhova, S., Kozachuk, A., Kozlov, V. S., Kraan, M., Kravchenko, P., Kravchuk, L., Krawczyk, R. D., Kreps, M., Kretzschmar, S., Krokovny, P., Krupa, W., Krzemien, W., Kubat, J., Kubis, S., Kucewicz, W., Kucharczyk, M., Kudryavtsev, V., Kuhlman, A., Kuilman, W. C., Kulikova, E. K, Kuonen, A. K., Kupfer, N., Kupsc, A., Kvaratskheliya, T., Lacarrere, D., Lafferty, G., Lai, A., Lampis, A., Lancierini, D., Gomez, C. Landesa, Lane, J. J., Lane, R., Langenbruch, C., Langer, J., Langstaff, M., Lantwin, O., Latham, T., Lazzari, F., Lazzaroni, M., Dortz, O. Le, Gac, R. Le, Lee, S. H., Lefèvre, R., Leflat, A., Legotin, S., Lemaitre, F., Lenisa, P., Leroy, O., Lesiak, T., Leverington, B., Li, A., Li, H., Li, K., Li, P., Li, P. -R., Li, S., Li, T., Li, Y., Li, Z., Liang, X., Lieunard, B., Lin, C., Lin, T., Lindner, R., Lisovskyi, V., Litvinov, R., Liu, G., Liu, H., Liu, Q., Liu, S., Salvia, A. Lobo, Loi, A., Lollini, R., Castro, J. Lomba, Longstaff, I., Lopes, J. H., Huertas, A. Lopez, Soliño, S. López, Louis, D., Lovell, G. H., Loveridge, P., Lowe, A. D., Lu, Y., Lucarelli, C., Lucchesi, D., Luchuk, S., Martinez, M. Lucio, Lukashenko, V., Lukianov, A., Luo, H., Luo, Y., Lupato, A., Luppi, E., Lupton, O., Lusiani, A., Lutz, L. F., Lynch, K., Lyu, X. -R., Ma, R., Maccolini, S., Machefert, F., Maciuc, F., Mackay, I., Macko, V., Mackowiak, P., Maddrell-Mander, S., Mohan, L. R. Madhan, Maevskiy, A., Magne, M., Maisuzenko, D., Majewski, M. W., Malaguti, R., Malczewski, J. J., Malde, S., Malecki, B., Malinin, A., Malkinski, K., Maltsev, T., Manca, G., Mancinelli, G., Mancuso, C., Escalero, R. Manera, Manuzzi, D., Manzari, C. A., Marangotto, D., Marchand, J. F., Marconi, U., Mariani, S., Benito, C. Marin, Marks, J., Marshall, A. M., Marshall, P. J., Martelli, G., Martellotti, G., Martinazzoli, L., Martinelli, M., Santos, D. Martinez, Vidal, F. Martinez, Masic, B., Massafferri, A., Materok, M., Matev, R., Mathad, A., Mathe, Z., Matiunin, V., Matteuzzi, C., Mattioli, K. R., Mauri, A., Maurice, E., Mauricio, J., de Cos, J. Mazorra, Mazurek, M., McCann, M., Mcconnell, L., McGrath, T. H., McHugh, N. T., McNab, A., McNulty, R., Mead, J. V., Meadows, B., Meier, G., Meier-villardita, L., Melnychuk, D., Meloni, S., Merk, M., Merli, A., Meunier, J. L., Garcia, L. Meyer, Miao, D., Mikhasenko, M., Milanes, D. A., Millard, E., Miller, G., Milovanovic, M., Minard, M. -N., Minotti, A., Minutoli, S., Miralles, T., Mitchell, S. E., Mitreska, B., Mittelstaedt, T., Mitzel, D. S., Mödden, A., Modenese, L., Mogini, A., Mohammed, R. A., Moise, R. D., Mokhnenko, S., Mombächer, T., Monk, M., Monroy, I. A., Monteil, S., Monti, M., Morandin, M., Morello, G., Morello, M. J., Morgenthaler, M. P., Moron, J., Morris, A. B., Morris, A. G., Mountain, R., Mu, H., Muhammad, E., Muheim, F., Mulder, M., Muley, S., Müller, D., Müller, K., Munneke, B., Murphy, C. H., Murray, D., Murta, R., Muzzetto, P., Naik, P., Naik, S. A., Nakada, T., Nandakumar, R., Nanut, T., Nasteva, I., Nazarov, E., Needham, M., Neri, I., Neri, N., Neubert, S., Neufeld, N., Neustroev, P., Newcombe, R., Trung, T. Nguyen, Nicolini, J., Nicotra, D., Niel, E. M., Nieswand, S., Nikitin, N., Nolte, N. S., Normand, C., Fernandez, J. Novoa, Nowak, G. N, Nunez, C., O'Bannon, T., Oblakowska-Mucha, A., Obraztsov, V., O'Dell, J., Oeser, T., Okamura, S., Oldeman, R., Oliva, F., Olive, P., Onderwater, C. J. G., O'Neil, R. H., Orlov, V., Goicochea, J. M. Otalora, Ovsiannikova, T., Owen, P., Oyanguren, A., Ozcelik, O., Padeken, K. O., Pagare, B., Pais, P. R., Pajero, T., Palano, A., Palutan, M., Pan, Y., Panshin, G., Paoletti, E., Paolucci, L., Papanestis, A., Pappagallo, M., Pappalardo, L. L., Pappenheimer, C., Parker, W., Parkes, C., Pasquali, L., Passalacqua, B., Passaleva, G., Pastore, A., Patel, M., Patrignani, C., Pavlenko, D., Pawley, C. J., Pearce, A., Regales, M. D. P. Peco, Pellegrino, A., Peltier, F., Altarelli, M. Pepe, Perazzini, S., Pereima, D., Castro, A. Pereiro, Perret, P., Perro, A., Perry, M., Pessina, G., Petridis, K., Petrolini, A., Petrucci, S., Petruzzo, M., Pham, H., Philippov, A., Piandani, R., Pica, L., Olloqui, E. Picatoste, Piccini, M., Piedigrossi, D., Pietrzyk, B., Pietrzyk, G., Pili, M., Pillet, N., Pilorz, E. M., Pinci, D., Pisani, F., Pizzichemi, M., Placinta, V., Plews, J., Casasus, M. Plo, Polci, F., Lener, M. Poli, Poluektov, A., Polukhina, N., Polyakov, I., Polyakov, V., Polycarpo, E., Pomery, G. J., Ponce, S., Pons, X., Poplawski, K., Popov, D., Poslavskii, S., Prasanth, K., Pratt, D., Promberger, L., Prouve, C., Pugatch, V., Puill, V., Punzi, G., Qi, H. R., Qian, W., Qin, N., Qu, S., Quagliani, R., Raab, N. V., Rachwal, B., Rademacker, J. H., Rajagopalan, R., Rama, M., Ramaherison, J. J., Pernas, M. Ramos, Rangel, M. S., Ratnikov, F., Raven, G., De Miguel, M. Rebollo, Redi, F., Reich, J., Reiss, F., Alepuz, C. Remon, Ren, Z., Resmi, P. 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Scantlebury, Scarabotto, A., Schael, S., Scherl, S., Schiller, M., Schimmel, A., Schindler, H., Schipper, J. D., Schmeitz, R., Schmelling, M., Schmidt, B., Schmitt, S., Schneider, O., Schneider, T., Schopper, A., Schubiger, M., Schulte, S., Schune, M. H., Schwemmer, R., Sciascia, B., Sciuccati, A., Sellam, S., Semennikov, A., Soares, M. Senghi, Sergi, A., Serra, N., Sestak, J., Sestini, L., Seuthe, A., Seyfert, P., Shang, Y., Shangase, D. M., Shapkin, M., Shchemerov, I., Shchutska, L., Shears, T., Shekhtman, L., Shen, Z., Sheng, S., Sherman, M. s, Shevchenko, V., Shi, B., Shields, E. B., Shimizu, Y., Shmanin, E., Shorkin, R., Shupperd, J. D., Siddi, B. G., Siebig, S., Sigmund, D., Sigurdsson, S., Coutinho, R. Silva, Simi, G., Simone, S., Singla, M., Skidmore, N., Skuza, R., Skwarnicki, T., Slater, M. W., Slattery, K., Slazyk, I., Smallwood, J. C., Smeaton, J. G., Smith, E., Smith, K., Smith, M., Smith, N. A., Snoch, A., Lavra, L. Soares, Socha, J-L., Sokoloff, M. D., Soler, F. J. 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Subjects
High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract

The LHCb upgrade represents a major change of the experiment. The detectors have been almost completely renewed to allow running at an instantaneous luminosity five times larger than that of the previous running periods. Readout of all detectors into an all-software trigger is central to the new design, facilitating the reconstruction of events at the maximum LHC interaction rate, and their selection in real time. The experiment's tracking system has been completely upgraded with a new pixel vertex detector, a silicon tracker upstream of the dipole magnet and three scintillating fibre tracking stations downstream of the magnet. The whole photon detection system of the RICH detectors has been renewed and the readout electronics of the calorimeter and muon systems have been fully overhauled. The first stage of the all-software trigger is implemented on a GPU farm. The output of the trigger provides a combination of totally reconstructed physics objects, such as tracks and vertices, ready for final analysis, and of entire events which need further offline reprocessing. This scheme required a complete revision of the computing model and rewriting of the experiment's software., Comment: All figures and tables, along with any supplementary material and additional information, are available at http://lhcbproject.web.cern.ch/lhcbproject/Publications/LHCbProjectPublic/LHCb-DP-2022-002.html (LHCb public pages)

Published
2023
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