The ASAS-SN Bright Supernova Catalog -- IV. 2017

Holoien, T. W. -S.; Brown, J. S.; Vallely, P. J.; Stanek, K. Z.; Kochanek, C. S.; Shappee, B. J.; Prieto, J. L.; Dong, Subo; Brimacombe, J.; Bishop, D. W.; Bose, S.; Beacom, J. F.; Bersier, D.; Chen, Ping; Chomiuk, L.; Falco, E.; Holmbo, S.; Jayasinghe, T.; Morrell, N.; Pojmanski, G.; Shields, J. V.; Strader, J.; Stritzinger, M. D.; Thompson, Todd A.; Wozniak, P. R.; Bock, G.; Cacella, P.; Carballo, J. G.; Conseil, E.; Cruz, I.; Farfan, R. G.; Fernandez, J. M.; Kiyota, S.; Koff, R. A.; Krannich, G.; Marples, P.; Masi, G.; Monard, L. A. G.; Munoz, J. A.; Nicholls, B.; Post, R. S.; Stone, G.; Trappett, D. L.; Wiethoff, W. S.

doi:10.48550/arxiv.1811.08904

Cited by 3 publications

(3 citation statements)

References 43 publications

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“…Assuming a Salpeter Initial Mass Function (IMF), and an average star mass of 1 M , the Type Ia SN likelihood is 0.4% and the Type Ia SN rate is 4 × 10 −6 /yr for our GC 3 . Based on the observation statistics of the ASAS-SN collaboration (e.g., Holoien et al 2018), we assume an effective observation radius of 250 Mpc (up to redshift 0.06), or an effectively observable sphere of 0.065 Gpc 3 . Assuming a galaxy density of 0.02 Galaxies/Mpc 3 (Conselice et al 2005), there are about 1.3 × 10 6 galaxies within this sphere.…”

Section: Binary Evolution Outcomesmentioning

confidence: 99%

The Fate of Binaries in the Galactic Center: The Mundane and the Exotic

Stephan

Naoz

Ghez

et al. 2019

ApJ

107

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The Galactic Center (GC) is dominated by the gravity of a super-massive black hole (SMBH), Sagittarius A * , and is suspected to contain a sizable population of binary stars. Such binaries form hierarchical triples with the SMBH, undergoing Eccentric Kozai-Lidov (EKL) evolution, which can lead to high eccentricity excitations for the binary companions' mutual orbit. This effect can lead to stellar collisions or Roche-lobe crossings, as well as orbital shrinking due to tidal dissipation. In this work we investigate the dynamical and stellar evolution of such binary systems, especially with regards to the binaries' post-main-sequence evolution. We find that the majority of binaries (∼ 75%) is eventually separated into single stars, while the remaining binaries (∼ 25%) undergo phases of common-envelope evolution and/or stellar mergers. These objects can produce a number of different exotic outcomes, including rejuvenated stars, G2-like infrared-excess objects, stripped giant stars, Type Ia supernovae (SNe), cataclysmic variables (CVs), symbiotic binaries (SBs), or compact object binaries. We estimate that, within a sphere of 250 Mpc radius, about 7.5 to 15 Type Ia SNe per year should occur in galactic nuclei due to this mechanism, potentially detectable by ZTF and ASAS-SN. Likewise we estimate that, within a sphere of 1 Gpc 3 volume, about 10 to 20 compact object binaries form per year that could become gravitational wave sources. Based on results of EKL-driven compact object binary mergers in galactic nuclei by Hoang et al. (2018), this compact object binary formation rate translates to about 15 to 30 events per year detectable by Advanced LIGO. nature of gravity, stellar cluster dynamics, and general relativity (GR) over the last decades (e.g., Ghez et al.

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Section: Binary Evolution Outcomesmentioning

confidence: 99%

The Fate of Binaries in the Galactic Center: The Mundane and the Exotic

Stephan

Naoz

Ghez

et al. 2019

ApJ

107

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“…The SN early warning before the burst may also be achieved by monitoring the variability of progenitors with the wide field telescopes [56][57][58][59][60], which could cover a rather broadband wavelength and long distance. However, since it is still not well-established on the rate of magnitude variability [59][60][61][62] and light characteristics [63] during the late stage of the SN progenitors, independent early warning for the nearby galactic SN using pre-SN neutrinos is still useful and complementary to the optical telescope monitoring.…”

Section: Time To Collapse [Day]mentioning

confidence: 99%

Towards a complete reconstruction of supernova neutrino spectra in future large liquid-scintillator detectors

Li¹,

Li²,

Wang³

et al. 2018

Phys. Rev. D

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In this paper, we show how to carry out a relatively more realistic and complete reconstruction of supernova neutrino spectra in the future large liquid-scintillator detectors, by implementing the method of singular value decomposition with a proper regularization. For a core-collapse supernova at a distance of 10 kpc in the Milky Way, itsν e spectrum can be precisely determined from the inverse beta-decay processν e þ p → e þ þ n, for which a 20 kiloton liquid-scintillator detector with the resolution similar to the Jiangmen Underground Neutrino Observatory may register more than 5000 events. We have to rely predominantly on the elastic neutrino-electron scattering ν þ e − → ν þ e − and the elastic neutrino-proton scattering ν þ p → ν þ p for the spectra of ν e and ν x , where ν denotes collectively neutrinos and antineutrinos of all three flavors and ν x for ν μ and ν τ as well as their antiparticles. To demonstrate the validity of our approach, we also attempt to reconstruct the neutrino spectra by using the time-integrated neutrino data from the latest numerical simulations of delayed neutrino-driven supernova explosions.

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“…However, the mean values of light curve parameters like stretch and colour do drift with z, possibly due to selection effects or changes in the host galaxy properties at higher redshift. Large numbers of Type Ia supernova have also been found, or are in the process of being surveyed, by the Dark Energy Survey (Abbott et al 2019), All-Sky Automated Survey for Supernovae (Holoien et al 2018), Foundation Survey (Jones et al 2019), and Zwicky Transient Facility (Yao et al 2019).…”

Section: Type Ia Supernovaementioning

confidence: 99%

A buyer's guide to the Hubble Constant

Shah,

Lemos,

Lahav

2021

Preprint

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Since the expansion of the universe was first established by Edwin Hubble and Georges Lemaître about a century ago, the Hubble constant H 0 which measures its rate has been of great interest to astronomers. Besides being interesting in its own right, few properties of the universe can be deduced without it. In the last decade a significant gap has emerged between different methods of measuring it, some anchored in the nearby universe, others at cosmological distances. The SH0ES team has found H 0 = 73.2 ± 1.3 km s −1 Mpc −1 locally, whereas the value found for the early universe by the Planck Collaboration is H 0 = 67.4 ± 0.5 km s −1 Mpc −1 from measurements of the cosmic microwave background. Is this gap a sign that the well-established ΛCDM cosmological model is somehow incomplete? Or are there unknown systematics? And more practically, how should humble astronomers pick between competing claims if they need to assume a value for a certain purpose? In this article, we review results and what changes to the cosmological model could be needed to accommodate them all. For astronomers in a hurry, we provide a buyer's guide to the results, and make recommendations.

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The ASAS-SN Bright Supernova Catalog -- IV. 2017

Cited by 3 publications

References 43 publications

The Fate of Binaries in the Galactic Center: The Mundane and the Exotic

The Fate of Binaries in the Galactic Center: The Mundane and the Exotic

Towards a complete reconstruction of supernova neutrino spectra in future large liquid-scintillator detectors

A buyer's guide to the Hubble Constant

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