Understanding the Death of Massive Stars Using an Astrophysical Transients Observatory

Roming, P. W. A.; Baron, E.; Bayless, Amanda J.; Brown, P. J.; Davis, Michael W.; Fialkov, Anastasia; Fleming, Brian; Fryer, Chris L.; Greathouse, T. K.; Hancock, Jed J.; Howell, D. A.; Levan, A. J.; Loeb, Abraham; Margutti, R.; McConnell, Mark L.; O’Brien, P. T.; Osborne, J. P.; Perley, D.; Schlegel, Eric M.; Starling, R. L. C.; Tanvir, N. R.; Tapley, Mark B.; Young, Patrick; Zhang, Bing

doi:10.3389/fspas.2018.00025

Cited by 3 publications

(3 citation statements)

References 100 publications

(97 reference statements)

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“…The science impact of observing the early emission from shock breakout events cannot be understated. Proposed missions such as the Astrophysical Transients Observatory (ATO; Roming et al 2018) would provide the necessary tools for rapidly observing these shock breakout events. Our simulations show that such a mission as ATO, with full-sky coverage, could detect over 1000 events.…”

Section: Discussionmentioning

confidence: 99%

Supernova Shock Breakout/Emergence Detection Predictions for a Wide-field X-Ray Survey

Bayless

Fryer

Brown

et al. 2022

ApJ

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There are currently many large-field surveys that are operational and are being planned including the powerful Vera C. Rubin Observatory Legacy Survey of Space and Time. These surveys will increase the number and diversity of transients dramatically. However, for some transients, like supernovae (SNe), we can gain more understanding by directed observations (e.g., shock breakout and γ-ray detections) than by simply increasing the sample size. For example, the initial emission from these transients can be a powerful probe of these explosions. Upcoming ground-based detectors are not ideally suited to observing the initial emission (shock emergence) of these transients. These observations require a large field-of-view X-ray mission with a UV follow-up within the first hour of shock breakout. The emission in the first 1 hr to even 1 day provides strong constraints on the stellar radius and asymmetries in the outer layers of stars, the properties of the circumstellar medium (e.g., inhomogeneities in the wind for core-collapse SNe and accreting companions in thermonuclear SNe), and the transition region between these two areas. This paper describes a simulation for the number of SNe that could be seen by a large field-of-view lobster-eye X-ray and UV observatory.

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Section: Discussionmentioning

confidence: 99%

Supernova Shock Breakout/Emergence Detection Predictions for a Wide-field X-Ray Survey

Bayless

Fryer

Brown

et al. 2022

ApJ

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“…But to disentangle all of this physics, joint UV and X-ray observations are required. The SIBEX mission (Roming et al 2018) is designed to do exactly this science and, if launched, would provide detailed observations of shock breakout, facilitating a better disentangling of the different asymmetries in this signal. For shock breakout to truly be used to constrain the supernova engine, we need to obtain detailed observations of a large number of events and couple them to increasingly detailed explosion models.…”

Section: Indirect Probe: Shock-breakout Observationsmentioning

confidence: 99%

“…Similarly, detectors such as the UltraSAT (Ben-Ami et al 2022) and CASTOR (Ménesguen et al 2017) satellites are designed to increase the number of shock-breakout detections in the UV. Whether these missions will provide sufficient information to help us understand the supernova engine remains to be determined, but it is more likely that in order to disentangle all of this physics, joint UV and X-ray observations are required such as proposed by the SIBEX mission (Roming et al 2018). In both cases, considerable modeling work is needed if we are to use these supernova observations to both constrain the engine and make predictions for extended populations.…”

Section: Concurrent Observationsmentioning

confidence: 99%

Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae

Fryer,

Burns,

Hungerford

et al. 2023

ApJ

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Core-collapse supernova explosions play a wide role in astrophysics by producing compact remnants (neutron stars or black holes) and the synthesis and injection of many heavy elements into their host galaxy. Because they are produced in some of the most extreme conditions in the universe, they can also probe physics in extreme conditions (matter at nuclear densities and extreme temperatures and magnetic fields). To quantify the impact of supernovae on both fundamental physics and our understanding of the universe, we must leverage a broad set of observables of this engine. In this paper, we study a subset of these probes using a suite of one-dimensional, parameterized mixing models: ejecta remnants from supernovae, ultraviolet, optical and infrared light curves, and transient gamma-ray emission. We review the other diagnostics and show how the different probes tie together to provide a more clear picture of the supernova engine. Join us in improving and evolving this document through active community engagement. Instructions are provided at this link: https://github.com/clfryer/MM-SNe.

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First Star-Forming Structures in Fuzzy Cosmic Filaments

et al. 2019

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In hierarchical models of structure formation, the first galaxies form in low-mass dark matter potential wells, probing the behavior of dark matter on kiloparsec (kpc) scales. Even though these objects are below the detection threshold of current telescopes, future missions will open an observational window into this emergent world. In this Letter we investigate how the first galaxies are assembled in a 'fuzzy' dark matter (FDM) cosmology where dark matter is an ultralight ∼ 10 −22 eV boson and the primordial stars are expected to form along dense dark matter filaments. Using a first-of-its-kind cosmological hydrodynamical simulation, we explore the interplay between baryonic physics and unique wavelike features inherent to FDM. In our simulation, the dark matter filaments show coherent interference patterns on the boson de Broglie scale and develop cylindrical solitonlike cores which are unstable under gravity and collapse into kpc-scale spherical solitons. Features of the dark matter distribution are largely unaffected by the baryonic feedback. On the contrary, the distributions of gas and stars, which do form along the entire filament, exhibit central cores imprinted by dark matter -a smoking gun signature of FDM.Introduction. The nearly century-old dark matter problem is one of the most intriguing mysteries in modern physics. We do not know the nature of 84 percent of matter in the Universe, yet it is thought to govern cosmic structure and hold galaxies and clusters together [1]. Observations show that on scales larger than a few megaparsecs (Mpc), the behavior of dark matter is consistent with it being collisionless [2,3]. However, on scales at and below the size of dwarf galaxies (few kpc) dark matter is not well constrained [4], allowing for many plausible theories with exotic small-scale physics and particle masses spanning over 30 orders of magnitude [5][6][7][8][9][10]. The first star-forming regions in the Universe -more susceptible to dark matter's small-scale behavior than much heavier present-day galaxies -will be revealed by next generation space telescopes and offer a unique probe of the nature of this elusive component.A leading hypothesis for the dark matter 'back-bone' of the Universe is cold dark matter (CDM), such as a thermally-produced weakly interacting massive particle (WIMP) of mass eV. CDM is collisionless and Jeans unstable to forming structure on all astrophysical scales down to a particle physics model-dependent small-scale

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Understanding the Death of Massive Stars Using an Astrophysical Transients Observatory

Cited by 3 publications

References 100 publications

Supernova Shock Breakout/Emergence Detection Predictions for a Wide-field X-Ray Survey

Supernova Shock Breakout/Emergence Detection Predictions for a Wide-field X-Ray Survey

Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae

First Star-Forming Structures in Fuzzy Cosmic Filaments

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