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3 results on '"Astronomy data modeling"'

1. Measurement of Galactic 26Al with the Compton Spectrometer and Imager

Author

Jacqueline Beechert, Thomas Siegert, John A. Tomsick, Andreas Zoglauer, Steven E. Boggs, Terri J. Brandt, Hannah Gulick, Pierre Jean, Carolyn Kierans, Hadar Lazar, Alexander Lowell, Jarred M. Roberts, Clio Sleator, Peter von Ballmoos, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Gamma-ray telescopes, Stellar nucleosynthesis, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], High altitude balloons, Gamma-ray lines, Astrophysics - High Energy Astrophysical Phenomena, Nuclear Experiment, Astrophysics::Galaxy Astrophysics, Astronomy data modeling
Abstract

The Compton Spectrometer and Imager (COSI) is a balloon-borne compact Compton telescope designed to survey the 0.2-5 MeV sky. COSI's energy resolution of $\sim$0.2% at 1.8 MeV, single-photon reconstruction, and wide field of view make it capable of studying astrophysical nuclear lines, particularly the 1809 keV $\gamma$-ray line from decaying Galactic $^{26}$Al. Most $^{26}$Al originates in massive stars and core-collapse supernova nucleosynthesis, but the path from stellar evolution models to Galaxy-wide emission remains unconstrained. In 2016, COSI had a successful 46-day flight on a NASA superpressure balloon. Here, we detail the first search for the 1809 keV $^{26}$Al line in the COSI 2016 balloon flight using a maximum likelihood analysis. We find a Galactic $^{26}$Al flux of $(8.6 \pm 2.5) \times 10^{-4}$ ph cm$^{-2}$ s$^{-1}$ within the Inner Galaxy ($|\ell| \leq 30^{\circ}$, $|b| \leq 10^{\circ}$) with 3.7$\sigma$ significance above background. Within uncertainties, this flux is consistent with expectations from previous measurements by SPI and COMPTEL. This analysis demonstrates COSI's powerful capabilities for studies of $\gamma$-ray lines and underscores the scientific potential of future compact Compton telescopes. In particular, the next iteration of COSI as a NASA Small Explorer satellite has recently been approved for launch in 2025., Comment: 23 pages, 22 figures, accepted by The Astrophysical Journal (ApJ)

Published
2022
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2. Low Water Outgassing from (24) Themis and (65) Cybele: 3.1 μ m Near-IR Spectral Implications

Author

T. G. Müller, Michael Küppers, D. Teyssier, I. Valtchanov, N. Biver, Hideaki Fujiwara, T. L. Lim, Sonia Fornasier, Dominique Bockelée-Morvan, Laurence O'Rourke, Humberto Campins, Sunao Hasegawa, Agence Spatiale Européenne (ESA), European Space Agency (ESA), Max-Planck-Institut für Extraterrestrische Physik (MPE), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), European Space Astronomy Centre (ESAC), University of Central Florida [Orlando] (UCF), Faculty of Science and Technology [Tokyo], Seikei University, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AUTRES, and Dept. of Physics

Subjects
010504 meteorology & atmospheric sciences, Thermal inertia, Main belt asteroids, Main-belt comets, Astrophysics, 01 natural sciences, symbols.namesake, Far infrared, Bond albedo, 0103 physical sciences, Comets, 010303 astronomy & astrophysics, Astronomy data modeling, 0105 earth and related environmental sciences, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Spectrometer, Astronomy and Astrophysics, Small solar system bodies, Space observatory, Asteroids, Outgassing, 13. Climate action, Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], symbols, Water vapor
Abstract

International audience; Asteroids (24) Themis and (65) Cybele have an absorption feature at 3.1 μm reported to be directly linked to surface water ice. We searched for water vapor escaping from these asteroids with the Herschel Space Observatory Heterodyne Instrument for the Far Infrared. While no H 2 O line emission was detected, we obtain sensitive 3σ water production rate upper limits of Q(H 2 O)

Published
2020
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3. SN 2018fif: The Explosion of a Large Red Supergiant Discovered in Its Infancy by the Zwicky Transient Facility

Author

Ben Rusholme, Peter Nugent, S. Bradley Cenko, Eli Waxman, Russ R. Laher, Daniel A. Perley, N. P. Konidaris, Maayane T. Soumagnac, Christoffer Fremling, Barak Zackay, I. Irani, Avishay Gal-Yam, Emir Karamehmetoglu, Shrinivas R. Kulkarni, Steve Schulze, Eran O. Ofek, Mansi M. Kasliwal, Mickael Rigault, Jesper Sollerman, Eric C. Bellm, Jan van Roestel, Richard Dekany, Thomas Kupfer, Reed Riddle, Rachel Bruch, James D. Neill, V. Zach Golkhou, Jonathan Morag, Noam Ganot, Yang Yang, Rick Burruss, Virginia Cunningham, Ofer Yaron, Matthew J. Graham, Frank J. Masci, Adam Rubin, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Atomic, Physical Chemistry, Particle and Plasma Physics, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Red supergiant, Nuclear, 010303 astronomy & astrophysics, QC, Astronomy data modeling, Astrophysics::Galaxy Astrophysics, QB, 0105 earth and related environmental sciences, Physics, Type II supernovae, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Molecular, Astronomy and Astrophysics, Radius, First light, Observational astronomy, Transient sources, Ultraviolet transient sources, Stars, Supernova, Supernovae, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Degeneracy (mathematics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

High cadence transient surveys are able to capture supernovae closer to their first light than before. Applying analytical models to such early emission, we can constrain the progenitor stars properties. In this paper, we present observations of SN2018fif (ZTF18abokyfk). The supernova was discovered close to first light and monitored by the Zwicky Transient Facility (ZTF) and the Neil Gehrels Swift Observatory. Early spectroscopic observations suggest that the progenitor of SN2018fif was surrounded by relatively small amounts of circumstellar material (CSM) compared to all previous cases. This particularity, coupled with the high cadence multiple-band coverage, makes it a good candidate to investigate using shock-cooling models. We employ the SOPRANOS code, an implementation of the model by Sapir & Waxman and its extension to early times by Morag, Sapir & Waxman. Compared with previous implementations, SOPRANOS has the advantage of including a careful account of the limited temporal validity domain of the shock-cooling model as well as allowing usage of the entirety of the early UV data. We find that the progenitor of SN2018fif was a large red supergiant, with a radius of R=744.0_{-128.0}^{+183.0} solar radii and an ejected mass of Mej=9.3_{-5.8}^{+0.4} solar masses. Our model also gives information on the explosion epoch, the progenitor inner structure, the shock velocity and the extinction. The distribution of radii is double-peaked, with lower radii corresponding to lower values of the extinction, earlier recombination times and better match to the early UV data. If these correlations persist in future objects, denser spectroscopic monitoring constraining the time of recombination, as well as accurate UV observations (e.g. with ULTRASAT), will help break the radius-extinction degeneracy and independently determine both., Accepted by ApJ

Published
2020
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