RAS_WEB

Atmospheric Escape From Three Terrestrial Planets in the L 98-59 System. (arXiv:2312.00062v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fromont_E/0/1/0/all/0/1">Emeline F. Fromont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ahlers_J/0/1/0/all/0/1">John P. Ahlers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amaral_L/0/1/0/all/0/1">Laura N. R. do Amaral</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barnes_R/0/1/0/all/0/1">Rory Barnes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gilbert_E/0/1/0/all/0/1">Emily A. Gilbert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quintana_E/0/1/0/all/0/1">Elisa V. Quintana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peacock_S/0/1/0/all/0/1">Sarah Peacock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barclay_T/0/1/0/all/0/1">Thomas Barclay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Youngblood_A/0/1/0/all/0/1">Allison Youngblood</a> A critically important process affecting the climate evolution and potential habitability of an exoplanet is atmospheric escape, in which high-energy radiation from a star drives the escape of hydrogen atoms and other light elements from a planet’s atmosphere. L 98-59 is a benchmark system for studying such atmospheric processes, with three transiting terrestrial-size planets receiving Venus-like instellations (4-25Read More →

Evolution and final fate of solar metallicity stars in the mass range 7-15 Msun. I. The transition from AGB to SAGB stars, Electron Capture and Core Collapse Supernovae progenitors. (arXiv:2312.00107v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Limongi_M/0/1/0/all/0/1">Marco Limongi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roberti_L/0/1/0/all/0/1">Lorenzo Roberti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chieffi_A/0/1/0/all/0/1">Alessandro Chieffi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nomoto_K/0/1/0/all/0/1">Ken&#x27;ichi Nomoto</a> According to a standard initial mass function, stars in the range 7-12 Msun constitute ~50% (by number) of the stars more massive than ~7 Msun, but, in spite of this, their evolutionary properties, and in particular their final fate, are still scarcely studied. In this paper we present a detailed study of the evolutionary properties of solar metallicity, non rotating stars inRead More →

Reconstructing patchy helium reionization using the cosmic microwave background and large-scale structure. (arXiv:2312.00118v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Caliskan_M/0/1/0/all/0/1">Mesut &#xc7;al&#x131;&#x15f;kan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_N/0/1/0/all/0/1">Neha Anil Kumar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hotinli_S/0/1/0/all/0/1">Selim C. Hotinli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kamionkowski_M/0/1/0/all/0/1">Marc Kamionkowski</a> The intergalactic helium became fully ionized by the end of cosmic noon ($zsim2$). Similarly to the reionization of hydrogen, helium reionization is expected to be patchy, driven by luminous quasars that ionize the intergalactic gas in their surrounding environment. Probing the morphology of ionized electrons during this epoch can provide crucial information about early structure formation, including the clustering and luminosities of quasars, the accretion rates, variability, and lifetimes of active galactic nuclei, as well as theRead More →

Quasimonochromatic LISA Sources in the Frequency Domain. (arXiv:2312.00121v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Strokov_V/0/1/0/all/0/1">Vladimir Strokov</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Berti_E/0/1/0/all/0/1">Emanuele Berti</a> Among the binary sources of interest for LISA some are quasimonochromatic, in the sense that the change in the gravitational wave frequency $Delta flesssim 1;mbox{yr}^{-1}$ during the observation time. We study these sources in the frequency domain (FD) by taking into account the Doppler shift induced by LISA’s motion and the LISA pattern functions, and we compare our results with previous work in the time domain. We also discuss the transition from the quasimonochromatic case to the stationary phase approximation commonly used in Fisher matrix calculations, which applies when $DeltaRead More →

The Fibre Resolved opticAl and Near-ultraviolet Czerny-Turner Imaging Spectropolarimeter (FRANCIS). (arXiv:2312.00122v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Jess_D/0/1/0/all/0/1">D.B. Jess</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grant_S/0/1/0/all/0/1">S.D.T. Grant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bate_W/0/1/0/all/0/1">W. Bate</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_J/0/1/0/all/0/1">J. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jafarzadeh_S/0/1/0/all/0/1">S. Jafarzadeh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keys_P/0/1/0/all/0/1">P.H. Keys</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vieira_L/0/1/0/all/0/1">L.E.A. Vieira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lago_A/0/1/0/all/0/1">A. Dal Lago</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guarnieri_F/0/1/0/all/0/1">F.L. Guarnieri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christian_D/0/1/0/all/0/1">D.J. Christian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gilliam_D/0/1/0/all/0/1">D. Gilliam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banerjee_D/0/1/0/all/0/1">D. Banerjee</a> The solar physics community is entering a golden era that is ripe with next-generation ground- and space-based facilities. With ever-increasing resolving power stemming from the newest observational telescopes, it becomes more challenging to obtain (near-)simultaneous measurements at high spatial, temporal and spectral resolutions, while operating at the diffraction limit of these new facilities. Hence, in recentRead More →

The Ubiquity and Magnitude of Large FeK$alpha$ Equivalent Widths in AGN Extended Regions. (arXiv:2312.00124v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Tzanavaris_P/0/1/0/all/0/1">P. Tzanavaris</a> (1,2,3), <a href="http://arxiv.org/find/astro-ph/1/au:+Yaqoob_T/0/1/0/all/0/1">T. Yaqoob</a> (1,2), <a href="http://arxiv.org/find/astro-ph/1/au:+LaMassa_S/0/1/0/all/0/1">S. LaMassa</a> (4) ((1) CSST, UMBC, (2) CRESST, NASA/GSFC, (3) APS, (4) STScI) Narrow Fe K$alpha$ fluorescent emission lines arising at $sim$kpc-scale separations from the nucleus have only been detected in a few AGN. The detections require that the extended line emission be spatially resolved and sufficiently bright. Compared to narrow Fe K$alpha$ lines arising closer to the nucleus, they have much lower fluxes but show substantially larger equivalent widths, EW$_{rm Fe Kalpha}$. We show that, in the optically-thin limit, aRead More →

Scalable Bayesian uncertainty quantification with data-driven priors for radio interferometric imaging. (arXiv:2312.00125v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Liaudat_T/0/1/0/all/0/1">Tob&#xed;as I. Liaudat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mars_M/0/1/0/all/0/1">Matthijs Mars</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Price_M/0/1/0/all/0/1">Matthew A. Price</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pereyra_M/0/1/0/all/0/1">Marcelo Pereyra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Betcke_M/0/1/0/all/0/1">Marta M. Betcke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McEwen_J/0/1/0/all/0/1">Jason D. McEwen</a> Next-generation radio interferometers like the Square Kilometer Array have the potential to unlock scientific discoveries thanks to their unprecedented angular resolution and sensitivity. One key to unlocking their potential resides in handling the deluge and complexity of incoming data. This challenge requires building radio interferometric imaging methods that can cope with the massive data sizes and provide high-quality image reconstructions with uncertainty quantification (UQ). This work proposes a method coinedRead More →

Anatomy of Diluted Dark Matter in the Minimal Left-Right Symmetric Model. (arXiv:2312.00129v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Nemevsek_M/0/1/0/all/0/1">Miha Nemev&#x161;ek</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Zhang_Y/0/1/0/all/0/1">Yue Zhang</a> Temporary matter domination and late entropy dilution, injected by a “long-lived” particle in the early universe, serves as a standard mechanism for yielding the correct dark matter relic density. We recently pointed out the cosmological significance of diluting particle’s partial decay into dark matter. When repopulated in such a way, dark matter carries higher momentum than its thermal counterpart, resulting in a suppression of the linear matter power spectrum that is constrained by the large scale structure observations. In this work, we study the impact ofRead More →

The dense and non-homogeneous circumstellar medium revealed in radio wavelengths around the Type Ib SN 2019oys. (arXiv:2312.00131v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sfaradi_I/0/1/0/all/0/1">Itai Sfaradi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Horesh_A/0/1/0/all/0/1">Assaf Horesh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sollerman_J/0/1/0/all/0/1">Jesper Sollerman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fender_R/0/1/0/all/0/1">Rob Fender</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rhodes_L/0/1/0/all/0/1">Lauren Rhodes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Williams_D/0/1/0/all/0/1">David R. A. Williams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bright_J/0/1/0/all/0/1">Joe Bright</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Green_D/0/1/0/all/0/1">Dave A. Green</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schulze_S/0/1/0/all/0/1">Steve Schulze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gal_Yam_A/0/1/0/all/0/1">Avishay Gal-Yam</a> We present here broadband radio observations of the CSM interacting SN2019oys. SN2019oys was first detected in the optical and was classified as a Type Ib SN. Then, about $sim 100$ days after discovery, it showed an optical rebrightening and a spectral transition to a spectrum dominated by strong narrow emission lines, which suggests strongRead More →

$texttt{tdescore}$: An Accurate Photometric Classifier for Tidal Disruption Events. (arXiv:2312.00139v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Stein_R/0/1/0/all/0/1">Robert Stein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mahabal_A/0/1/0/all/0/1">Ashish Mahabal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reusch_S/0/1/0/all/0/1">Simeon Reusch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graham_M/0/1/0/all/0/1">Matthew Graham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kasliwal_M/0/1/0/all/0/1">Mansi M. Kasliwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kowalski_M/0/1/0/all/0/1">Marek Kowalski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gezari_S/0/1/0/all/0/1">Suvi Gezari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hammerstein_E/0/1/0/all/0/1">Erica Hammerstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakoneczny_S/0/1/0/all/0/1">Szymon J. Nakoneczny</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nicholl_M/0/1/0/all/0/1">Matt Nicholl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sollerman_J/0/1/0/all/0/1">Jesper Sollerman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Velzen_S/0/1/0/all/0/1">Sjoert van Velzen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yao_Y/0/1/0/all/0/1">Yuhan Yao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laher_R/0/1/0/all/0/1">Russ R. Laher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rusholme_B/0/1/0/all/0/1">Ben Rusholme</a> Optical surveys have become increasingly adept at identifying candidate Tidal Disruption Events (TDEs) in large numbers, but classifying these generally requires extensive spectroscopic resources. We here present $texttt{tdescore}$, a simple photometric classifier that is trained using a systematic census of $sim$3000 nuclear transients from theRead More →

Atmospheric metallicity and C/O of HD 189733 b from high-resolution spectroscopy. (arXiv:2312.00141v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Finnerty_L/0/1/0/all/0/1">Luke Finnerty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xuan_J/0/1/0/all/0/1">Jerry W. Xuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xin_Y/0/1/0/all/0/1">Yinzi Xin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liberman_J/0/1/0/all/0/1">Joshua Liberman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schofield_T/0/1/0/all/0/1">Tobias Schofield</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fitzgerald_M/0/1/0/all/0/1">Michael P. Fitzgerald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agrawal_S/0/1/0/all/0/1">Shubh Agrawal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baker_A/0/1/0/all/0/1">Ashley Baker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartos_R/0/1/0/all/0/1">Randall Bartos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blake_G/0/1/0/all/0/1">Geoffrey A. Blake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calvin_B/0/1/0/all/0/1">Benjamin Calvin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cetre_S/0/1/0/all/0/1">Sylvain Cetre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delorme_J/0/1/0/all/0/1">Jacques-Robert Delorme</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doppman_G/0/1/0/all/0/1">Greg Doppman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Echeverri_D/0/1/0/all/0/1">Daniel Echeverri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hsu_C/0/1/0/all/0/1">Chih-Chun Hsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jovanovic_N/0/1/0/all/0/1">Nemanja Jovanovic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_R/0/1/0/all/0/1">Ronald A. L&#xf3;pez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_E/0/1/0/all/0/1">Emily C. Martin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mawet_D/0/1/0/all/0/1">Dimitri Mawet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morris_E/0/1/0/all/0/1">Evan Morris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pezzato_J/0/1/0/all/0/1">Jacklyn Pezzato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruffio_J/0/1/0/all/0/1">Jean-Baptiste Ruffio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sappey_B/0/1/0/all/0/1">Ben Sappey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Skemer_A/0/1/0/all/0/1">Andrew Skemer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Venenciano_T/0/1/0/all/0/1">Taylor Venenciano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wallace_J/0/1/0/all/0/1">J. Kent Wallace</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wallack_N/0/1/0/all/0/1">Nicole L. Wallack</a>, <aRead More →

The ZTF Source Classification Project: III. A Catalog of Variable Sources. (arXiv:2312.00143v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Healy_B/0/1/0/all/0/1">Brian F. Healy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coughlin_M/0/1/0/all/0/1">Michael W. Coughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mahabal_A/0/1/0/all/0/1">Ashish A. Mahabal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laz_T/0/1/0/all/0/1">Theophile J. du Laz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drake_A/0/1/0/all/0/1">Andrew Drake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graham_M/0/1/0/all/0/1">Matthew J. Graham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hillenbrand_L/0/1/0/all/0/1">Lynne A. Hillenbrand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roestel_J/0/1/0/all/0/1">Jan van Roestel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szkody_P/0/1/0/all/0/1">Paula Szkody</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zielske_L/0/1/0/all/0/1">LeighAnna Zielske</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guiga_M/0/1/0/all/0/1">Mohammed Guiga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hassan_M/0/1/0/all/0/1">Muhammad Yusuf Hassan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_J/0/1/0/all/0/1">Jill L. Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nir_G/0/1/0/all/0/1">Guy Nir</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parikh_S/0/1/0/all/0/1">Saagar Parikh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Park_S/0/1/0/all/0/1">Sungmin Park</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Purohit_P/0/1/0/all/0/1">Palak Purohit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rebbapragada_U/0/1/0/all/0/1">Umaa Rebbapragada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reed_D/0/1/0/all/0/1">Draco Reed</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wold_A/0/1/0/all/0/1">Avery Wold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bloom_J/0/1/0/all/0/1">Joshua S. Bloom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masci_F/0/1/0/all/0/1">Frank J. Masci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riddle_R/0/1/0/all/0/1">Reed Riddle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">Roger Smith</a> The classification of variable objects provides insight intoRead More →

The impact of free-streaming on dwarf galaxy counts in low-density regions. (arXiv:2312.00150v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Meshveliani_T/0/1/0/all/0/1">Tamar Meshveliani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lovell_M/0/1/0/all/0/1">Mark R. Lovell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crain_R/0/1/0/all/0/1">Robert A. Crain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pfeffer_J/0/1/0/all/0/1">Joel Pfeffer</a> We study the statistics of dwarf galaxy populations as a function of environment in the cold dark matter (CDM) and warm dark matter (WDM) cosmogonies, using hydrodynamical simulations starting from initial conditions with matched phases but differing power spectra, and evolved with the EAGLE galaxy formation model. We measure the abundance of dwarf galaxies within 3~Mpc of DM haloes with a present-day halo mass similar to that of the Milky Way (MW), and find that the radial distributionRead More →

Spectroastrometry and Imaging Science with Photonic Lanterns on Extremely Large Telescopes. (arXiv:2312.00221v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_Y/0/1/0/all/0/1">Yoo Jung Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fitzgerald_M/0/1/0/all/0/1">Michael P. Fitzgerald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_J/0/1/0/all/0/1">Jonathan Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sallum_S/0/1/0/all/0/1">Steph Sallum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xin_Y/0/1/0/all/0/1">Yinzi Xin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jovanovic_N/0/1/0/all/0/1">Nemanja Jovanovic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leon_Saval_S/0/1/0/all/0/1">Sergio Leon-Saval</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Betters_C/0/1/0/all/0/1">Christopher Betters</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gatkine_P/0/1/0/all/0/1">Pradip Gatkine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guyon_O/0/1/0/all/0/1">Olivier Guyon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lozi_J/0/1/0/all/0/1">Julien Lozi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mawet_D/0/1/0/all/0/1">Dimitri Mawet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Norris_B/0/1/0/all/0/1">Barnaby Norris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vievard_S/0/1/0/all/0/1">S&#xe9;bastien Vievard</a> Photonic lanterns (PLs) are tapered waveguides that gradually transition from a multi-mode fiber geometry to a bundle of single-mode fibers. In astronomical applications, PLs can efficiently couple multi-mode telescope light into a multi-mode fiber entrance and convert it into multiple single-mode beams. The output beams are highly stableRead More →

The IACOB project X. Large-scale quantitative spectroscopic analysis of Galactic blue supergiants. (arXiv:2312.00241v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Burgos_A/0/1/0/all/0/1">Abel de Burgos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simon_Diaz_S/0/1/0/all/0/1">Sergio Sim&#xf3;n-D&#xed;az</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Urbaneja_M/0/1/0/all/0/1">Miguel A. Urbaneja</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puls_J/0/1/0/all/0/1">Joachim Puls</a> Blue supergiants (BSGs) are key objects for understanding the evolution of massive stars. However, discrepancies between theoretical predictions and empirical observations have opened up important questions yet to be answered. Studying statistically significant and unbiased samples of BSGs can help to improve the situation. We aim to perform a homogeneous and comprehensive quantitative spectroscopic analysis of a large sample of Galactic BSGs from the IACOB spectroscopic database. We derive the projected rotational velocity ($vsin i$) and macroturbulentRead More →

SN~2015da: Late-time observations of a persistent superluminous Type~IIn supernova with post-shock dust formation. (arXiv:2312.00253v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_N/0/1/0/all/0/1">Nathan Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrews_J/0/1/0/all/0/1">Jennifer E. Andrews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milne_P/0/1/0/all/0/1">Peter Milne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Filippenko_A/0/1/0/all/0/1">Alexei V. Filippenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brink_T/0/1/0/all/0/1">Thomas G. Brink</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kelly_P/0/1/0/all/0/1">Patrick L. Kelly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yuk_H/0/1/0/all/0/1">Heechan Yuk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jencson_J/0/1/0/all/0/1">Jacob E. Jencson</a> We present photometry and spectroscopy of the slowly evolving superluminous Type IIn SN2015da. SN2015da is extraordinary for its very high peak luminosity, and also for sustaining a high luminosity for several years. Even at 8,yr after explosion, SN2015da remains as luminous as the peak of a normal SNII-P. The total radiated energy integrated over this time period (with no bolometric correction)Read More →

Short Review of the main achievements of the Scalar Field, Fuzzy, Ultralight, Wave, BEC Dark Matter model. (arXiv:2312.00254v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Matos_T/0/1/0/all/0/1">Tonatiuh Matos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Urena_Lopez_L/0/1/0/all/0/1">Luis A. Ure&#xf1;a-L&#xf3;pez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_J/0/1/0/all/0/1">Jae-Weon Lee</a> The Scalar Field Dark Matter model has been known in various ways throughout its history; Fuzzy, BEC, Wave, Ultralight, Axion-like Dark Matter, etc. All of them consist in proposing that the dark matter of the universe is a spinless field $Phi$ that follows the Klein-Gordon (KG) equation of motion $BoxPhi-dV/dPhi=0$, for a given scalar field potential $V$. The difference between different models is sometimes the choice of the scalar field potential $V$. In the literature weRead More →

Discovery of radio eclipses from 4FGL J1646.5$-$4406: a new candidate redback pulsar binary. (arXiv:2312.00261v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zic_A/0/1/0/all/0/1">Andrew Zic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Z/0/1/0/all/0/1">Ziteng Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lenc_E/0/1/0/all/0/1">Emil Lenc</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaplan_D/0/1/0/all/0/1">David L. Kaplan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murphy_T/0/1/0/all/0/1">Tara Murphy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ridolfi_A/0/1/0/all/0/1">Alessandro Ridolfi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sengar_R/0/1/0/all/0/1">Rahul Sengar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hurley_Walker_N/0/1/0/all/0/1">Natasha Hurley-Walker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dobie_D/0/1/0/all/0/1">Dougal Dobie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leung_J/0/1/0/all/0/1">James K. Leung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pritchard_J/0/1/0/all/0/1">Joshua Pritchard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Y/0/1/0/all/0/1">Yuanming Wang</a> Large widefield surveys make possible the serendipitous discovery of rare sub-classes of pulsars. One such class are “spider”-type pulsar binaries, comprised of a pulsar in a compact orbit with a low-mass (sub)stellar companion. In a search for circularly-polarized radio sources in ASKAP Pilot Survey observations, we discovered highly variable and circularly polarizedRead More →