High Energy Astrophysical Phenomena (astro-ph.HE)
Thu, 13 Apr 2023
1.A Contribution of the HAWC Observatory to the TeV era in the High Energy Gamma-Ray Astrophysics: The case of the TeV-Halos
Authors:Ramiro Torres-Escobedo The HAWC Collaboration, Hao Zhou The HAWC Collaboration, Eduardo de la Fuente The HAWC Collaboration, A. U. Abeysekara The HAWC Collaboration, A. Albert The HAWC Collaboration, R. Alfaro The HAWC Collaboration, C. Alvarez The HAWC Collaboration, J. D. Álvarez The HAWC Collaboration, J. R. Angeles Camacho The HAWC Collaboration, J. C. Arteaga-Velázquez The HAWC Collaboration, K. P. Arunbabu The HAWC Collaboration, D. Avila Rojas The HAWC Collaboration, H. A. Ayala Solares The HAWC Collaboration, R. Babu The HAWC Collaboration, V. Baghmanyan The HAWC Collaboration, A. S. Barber The HAWC Collaboration, J. Becerra Gonzalez The HAWC Collaboration, E. Belmont-Moreno The HAWC Collaboration, S. Y. BenZvi The HAWC Collaboration, D. Berley The HAWC Collaboration, C. Brisbois The HAWC Collaboration, K. S. Caballero-Mora The HAWC Collaboration, T. Capistrán The HAWC Collaboration, A. Carramiñana The HAWC Collaboration, S. Casanova The HAWC Collaboration, O. Chaparro-Amaro The HAWC Collaboration, U. Cotti The HAWC Collaboration, J. Cotzomi The HAWC Collaboration, S. Coutiño de León The HAWC Collaboration, C. de León The HAWC Collaboration, L. Diaz-Cruz The HAWC Collaboration, R. Diaz Hernandez The HAWC Collaboration, J. C. Díaz-Vélez The HAWC Collaboration, B. L. Dingus The HAWC Collaboration, M. Durocher The HAWC Collaboration, M. A. DuVernois The HAWC Collaboration, R. W. Ellsworth The HAWC Collaboration, K. Engel The HAWC Collaboration, C. Espinoza The HAWC Collaboration, K. L. Fan The HAWC Collaboration, K. Fang The HAWC Collaboration, M. Fernández Alonso The HAWC Collaboration, B. Fick The HAWC Collaboration, H. Fleischhack The HAWC Collaboration, J. L. Flores The HAWC Collaboration, N. I. Fraija The HAWC Collaboration, D. Garcia The HAWC Collaboration, J. A. García-González The HAWC Collaboration, G. García-Torales The HAWC Collaboration, F. Garfias The HAWC Collaboration, G. Giacinti The HAWC Collaboration, H. Goksu The HAWC Collaboration, M. M. González The HAWC Collaboration, J. A. Goodman The HAWC Collaboration, J. P. Harding The HAWC Collaboration, S. Hernandez The HAWC Collaboration, I. Herzog The HAWC Collaboration, J. Hinton The HAWC Collaboration, B. Hona The HAWC Collaboration, D. Huang The HAWC Collaboration, F. Hueyotl-Zahuantitla The HAWC Collaboration, C. M. Hui The HAWC Collaboration, B. Humensky The HAWC Collaboration, P. Hüntemeyer The HAWC Collaboration, A. Iriarte The HAWC Collaboration, A. Jardin-Blicq The HAWC Collaboration, H. Jhee The HAWC Collaboration, V. Joshi The HAWC Collaboration, D. Kieda The HAWC Collaboration, G J. Kunde The HAWC Collaboration, S. Kunwar The HAWC Collaboration, A. Lara The HAWC Collaboration, J. Lee The HAWC Collaboration, W. H. Lee The HAWC Collaboration, D. Lennarz The HAWC Collaboration, H. León Vargas The HAWC Collaboration, J. Linnemann The HAWC Collaboration, A. L. Longinotti The HAWC Collaboration, R. López-Coto The HAWC Collaboration, G. Luis-Raya The HAWC Collaboration, J. Lundeen The HAWC Collaboration, K. Malone The HAWC Collaboration, V. Marandon The HAWC Collaboration, O. Martinez The HAWC Collaboration, I. Martinez-Castellanos The HAWC Collaboration, H. Martínez-Huerta The HAWC Collaboration, J. Martínez-Castro The HAWC Collaboration, J. A. J. Matthews The HAWC Collaboration, J. McEnery The HAWC Collaboration, P. Miranda-Romagnoli The HAWC Collaboration, J. A. Morales-Soto The HAWC Collaboration, E. Moreno The HAWC Collaboration, M. Mostafá The HAWC Collaboration, A. Nayerhoda The HAWC Collaboration, L. Nellen The HAWC Collaboration, M. Newbold The HAWC Collaboration, M. U. Nisa The HAWC Collaboration, R. Noriega-Papaqui The HAWC Collaboration, L. Olivera-Nieto The HAWC Collaboration, N. Omodei The HAWC Collaboration, A. Peisker The HAWC Collaboration, Y. Pérez Araujo The HAWC Collaboration, E. G. Pérez-Pérez The HAWC Collaboration, C. D. Rho The HAWC Collaboration, C. Rivière The HAWC Collaboration, D. Rosa-Gonzalez The HAWC Collaboration, E. Ruiz-Velasco The HAWC Collaboration, J. Ryan The HAWC Collaboration, H. Salazar The HAWC Collaboration, F. Salesa Greus The HAWC Collaboration, A. Sandoval The HAWC Collaboration, M. Schneider The HAWC Collaboration, H. Schoorlemmer The HAWC Collaboration, J. Serna-Franco The HAWC Collaboration, G. Sinnis The HAWC Collaboration, A. J. Smith The HAWC Collaboration, R. W. Springer The HAWC Collaboration, P. Surajbali The HAWC Collaboration, I. Taboada The HAWC Collaboration, M. Tanner The HAWC Collaboration, K. Tollefson The HAWC Collaboration, I. Torres The HAWC Collaboration, R. Turner The HAWC Collaboration, F. Ureña-Mena The HAWC Collaboration, L. Villaseñor The HAWC Collaboration, X. Wang The HAWC Collaboration, I. J. Watson The HAWC Collaboration, T. Weisgarber The HAWC Collaboration, F. Werner The HAWC Collaboration, E. Willox The HAWC Collaboration, J. Wood The HAWC Collaboration, G. B. Yodh The HAWC Collaboration, A. Zepeda The HAWC Collaboration
Abstract: We present a short overview of the TeV-Halos objects as a discovery and a relevant contribution of the High Altitude Water \v{C}erenkov (HAWC) observatory to TeV astrophysics. We discuss history, discovery, knowledge, and the next step through a new and more detailed analysis than the original study in 2017. TeV-Halos will contribute to resolving the problem of the local positron excess observed on the Earth. To clarify the latter, understanding the diffusion process is mandatory.
2.Radio timing constraints on the mass of the binary pulsar PSR J1528-3146
Authors:A. Berthereau, L. Guillemot, P. C. C. Freire, M. Kramer, V. Venkatraman Krishnan, I. Cognard, G. Theureau, M. Bailes, M. C. i Bernadich, M. E. Lower
Abstract: PSR J1528-3146 is a 60.8 ms pulsar orbiting a heavy white dwarf (WD) companion, with an orbital period of 3.18 d. This work aimed at characterizing the pulsar's astrometric, spin and orbital parameters by analyzing timing measurements conducted at the Parkes, MeerKAT and Nan\c{c}ay radio telescopes over almost two decades. The measurement of post-Keplerian perturbations to the pulsar's orbit can be used to constrain the masses of the two component stars of the binary, and in turn inform us on the history of the system. We analyzed timing data from the Parkes, MeerKAT and Nan\c{c}ay radio telescopes collected over $\sim$16 yrs, obtaining a precise rotation ephemeris for PSR J1528-3146. A Bayesian analysis of the timing data was carried out to constrain the masses of the two components and the orientation of the orbit. We further analyzed the polarization properties of the pulsar, in order to constrain the orientations of the magnetic axis and of the line-of-sight with respect to the spin axis. We measured a significant rate of advance of periastron for the first time, and put constraints on the Shapiro delay in the system and on the rate of change of the projected semi-major axis of the pulsar's orbit. The Bayesian analysis yielded measurements for the pulsar and companion masses of respectively $M_p = 1.61_{-0.13}^{+0.14}$ M$_\odot$ and $M_c = 1.33_{-0.07}^{+0.08}$ M$_\odot$ (68\% C.L.), confirming that the companion is indeed massive. This companion mass as well as other characteristics of PSR J1528$-$3146 make this pulsar very similar to PSR J2222-0137, a 32.8 ms pulsar orbiting a WD whose heavy mass ($\sim 1.32$ M$_\odot$) was unique among pulsar-WD systems until now. Our measurements therefore suggest common evolutionary scenarios for PSRs J1528-3146 and J2222-0137.
3.GRB 211211A-like Events and How Gravitational Waves May Tell Their Origin
Authors:Yi-Han Iris Yin, Bin-Bin Zhang, Hui Sun, Jun Yang, Yacheng Kang, Lijing Shao, Yu-Han Yang, Bing Zhang
Abstract: GRB 211211A is a rare burst with a genuinely long duration, yet its prominent kilonova association provides compelling evidence that this peculiar burst was the result of a compact binary merger. However, the exact nature of the merging objects, whether they were neutron star pairs, neutron star-black hole systems, or neutron star-white dwarf systems, remains unsettled. This Letter delves into the rarity of this event and the possibility of using current and next-generation gravitational wave detectors to distinguish between the various types of binary systems. Our research reveals an event rate density of $\gtrsim 5.67^{+13.04}_{-4.69} \times 10^{-3}\ \rm Gpc^{-3} yr^{-1}$ for GRB 211211A-like GRBs, which is significantly smaller than that of typical long and short GRB populations. We further calculated that if the origin of GRB 211211A is a result of a neutron star-black hole merger, it would be detectable with a significant signal-to-noise ratio, given the LIGO-Virgo-KAGRA designed sensitivity. On the other hand, a neutron star-white dwarf binary would also produce a considerable signal-to-noise ratio during the inspiral phase at decihertz and is detectable by next-generation space-borne detectors DECIGO and BBO. However, to detect this type of system with millihertz space-borne detectors like LISA, Taiji, and TianQin, the event must be very close, approximately 3 Mpc in distance or smaller.
4.Interpolated kilonova spectra models: necessity for a phenomenological, blue component in the fitting of AT2017gfo spectra
Authors:Marko Ristic, Richard O'Shaughnessy, V. Ashley Villar, Ryan T. Wollaeger, Oleg Korobkin, Chris L. Fryer, Christopher J. Fontes, Atul Kedia
Abstract: In this work, we present a simple interpolation methodology for spectroscopic time series, based on conventional interpolation techniques (random forests) implemented in widely-available libraries. We demonstrate that our existing library of simulations is sufficient for training, producing interpolated spectra that respond sensitively to varied ejecta parameter, post-merger time, and viewing angle inputs. We compare our interpolated spectra to the AT2017gfo spectral data, and find parameters similar to our previous inferences using broadband light curves. However, the spectral observations have significant systematic short-wavelength residuals relative to our models, which we cannot explain within our existing framework. Similar to previous studies, we argue that an additional blue component is required. We consider a radioactive heating source as a third component characterized by light, slow-moving, lanthanide-free ejecta with $M_{\rm th} = 0.003~M_\odot$, $v_{\rm th} = 0.05$c, and $\kappa_{\rm th} = 1$ cm$^2$/g. When included as part of our radiative transfer simulations, our choice of third component reprocesses blue photons into lower energies, having the opposite effect and further accentuating the blue-underluminosity disparity in our simulations. As such, we are unable to overcome short-wavelength deficits at later times using an additional radioactive heating component, indicating the need for a more sophisticated modeling treatment.