RAS_WEB

Photometric Characterization and Trajectory Accuracy of Starlink Satellites: Implications for Ground-Based Astronomical Surveys. (arXiv:2208.03226v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Halferty_G/0/1/0/all/0/1">Grace Halferty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reddy_V/0/1/0/all/0/1">Vishnu Reddy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Campbell_T/0/1/0/all/0/1">Tanner Campbell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battle_A/0/1/0/all/0/1">Adam Battle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Furfaro_R/0/1/0/all/0/1">Roberto Furfaro</a> Starlink is a low-Earth orbit (LEO) satellite constellation operated by Space Exploration Technologies Corp. (SpaceX) which aims to provide global satellite internet access. Thus far, most photometric observations of Starlink satellites have primarily been from citizen scientists’ visual observations without using quantitative detectors. This paper aims to characterize Starlink satellites and investigate the impact of mega constellations on ground-based astronomy, considering both the observed magnitude and two-line element (TLE) residuals. We collected 353 observations ofRead More →

Spectral and timing analysis of BeXRB eRASSU J050810.4-660653 recently discovered in the Large Magellanic Cloud (LMC). (arXiv:2208.03222v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ghising_M/0/1/0/all/0/1">Manoj Ghising</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tobrej_M/0/1/0/all/0/1">Mohammed Tobrej</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tamang_R/0/1/0/all/0/1">Ruchi Tamang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rai_B/0/1/0/all/0/1">Binay Rai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paul_B/0/1/0/all/0/1">Bikash Chandra Paul</a> We have studied the Be/X-ray binary (BeXRB) pulsar eRASSU J050810.4-660653 recently discovered in the Large Magellanic Cloud (LMC). Timing and spectral features of the source have been discussed in detail using NuSTAR & XMM-Newton observations. Coherent pulsation of the source was detected at $sim 40.578;pm;0.001$ s using NuSTAR observation. We analyzed pulse profiles of the source in different energy bands using NuSTAR & XMM-Newton data. The pulse-profile evolved with time butRead More →

Can Satellite Mega-Constellations Justify their Impact on Astronomy?. (arXiv:2111.04592v3 [physics.soc-ph] UPDATED) <a href="http://arxiv.org/find/physics/1/au:+Petchetti_S/0/1/0/all/0/1">Sai Charan Petchetti</a> Private space companies are increasingly commercializing near-earth space. Some estimates show that more than 100,000 satellites may orbit the Earth by 2030. This increase in the number of satellites has many consequences for science, particularly astronomy. Satellite mega-constellations for satellite Internet connectivity are one of the main drivers behind the explosion in the number of satellites. Here, we briefly note whether such satellite mega-constellations can justify their impact on astronomy. Private space companies are increasingly commercializing near-earth space. Some estimates show that more than 100,000 satellites may orbit the EarthRead More →

TOI-3757 b: A low density gas giant orbiting a solar-metallicity M dwarf. (arXiv:2203.07178v3 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Kanodia_S/0/1/0/all/0/1">Shubham Kanodia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Libby_Roberts_J/0/1/0/all/0/1">Jessica Libby-Roberts</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Canas_C/0/1/0/all/0/1">Caleb I. Canas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ninan_J/0/1/0/all/0/1">Joe P. Ninan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mahadevan_S/0/1/0/all/0/1">Suvrath Mahadevan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stefansson_G/0/1/0/all/0/1">Gudmundur Stefansson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_A/0/1/0/all/0/1">Andrea S.J. Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_S/0/1/0/all/0/1">Sinclaire Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monson_A/0/1/0/all/0/1">Andrew Monson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parker_B/0/1/0/all/0/1">Brock A. Parker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kobulnicky_H/0/1/0/all/0/1">Henry A. Kobulnicky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Swaby_T/0/1/0/all/0/1">Tera N. Swaby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Powers_L/0/1/0/all/0/1">Luke Powers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beard_C/0/1/0/all/0/1">Corey Beard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bender_C/0/1/0/all/0/1">Chad F. Bender</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blake_C/0/1/0/all/0/1">Cullen H. Blake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cochran_W/0/1/0/all/0/1">William D. Cochran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_J/0/1/0/all/0/1">Jiayin Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diddams_S/0/1/0/all/0/1">Scott A. Diddams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fredrick_C/0/1/0/all/0/1">Connor Fredrick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_A/0/1/0/all/0/1">Arvind F. Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halverson_S/0/1/0/all/0/1">Samuel Halverson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hearty_F/0/1/0/all/0/1">Fred Hearty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Logsdon_S/0/1/0/all/0/1">Sarah E. Logsdon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Metcalf_A/0/1/0/all/0/1">Andrew J. Metcalf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McElwain_M/0/1/0/all/0/1">MichaelRead More →

Primordial Lepton Asymmetries in the Precision Cosmology Era: Current Status and Future Sensitivities from BBN and the CMB. (arXiv:2208.03201v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Escudero_M/0/1/0/all/0/1">Miguel Escudero</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Ibarra_A/0/1/0/all/0/1">Alejandro Ibarra</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Maura_V/0/1/0/all/0/1">Victor Maura</a> Using a new sample of extremely metal poor systems, the EMPRESS survey has recently reported a primordial helium abundance that is $3sigma$ smaller than the prediction from the Standard BBN scenario. This measurement could be interpreted as a hint for a primordial lepton asymmetry in the electron neutrino flavor. Motivated by the EMPRESS results, we present a comprehensive analysis of the lepton asymmetry using measurements of the abundances of primordial elements, along with CMB data fromRead More →

Possibility of Additional Intergalactic and Cosmological Dark Matter. (arXiv:2207.12408v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Frampton_P/0/1/0/all/0/1">Paul H Frampton</a> The entropies of the known entities in the universe add to a total which is some twenty orders of magnitude below the holographic limit. Based on an assumption that the entropies should saturate the limit, we suggest that there exists dark matter, in the form of extremely massive primordial black holes, in addition to the dark matter known to exist inside galaxies and clusters of galaxies. The entropies of the known entities in the universe add to a total which is some twenty orders of magnitude below the holographic limit.Read More →

Three-Dimensional Structure of the Central Molecular Zone. (arXiv:2208.02451v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sofue_Y/0/1/0/all/0/1">Yoshiaki Sofue</a> A detailed comparison of HI and CO line cube data of the Galactic Center (GC) region from the archives is obtained. The central molecular zone (CMZ) is shown to be embedded in the HI disc (central HI zone, CHZ) of radius $sim 320$ pc and vertical scale height $sim 70$ pc. A radio continuum belt is shown to run parallel to molecular Arms I and II. The belt draws a double-infinity shape on the sky, connecting Sgr E ($lsim -1^circ.2)$, C, B1, B2 and Sgr D ($+1^circ.2$), and is interpreted as aRead More →

Disentangling Multiple Stochastic Gravitational Wave Background Sources in PTA Datasets. (arXiv:2208.02307v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Kaiser_A/0/1/0/all/0/1">Andrew R. Kaiser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pol_N/0/1/0/all/0/1">Nihan S. Pol</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McLaughlin_M/0/1/0/all/0/1">Maura A. McLaughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_S/0/1/0/all/0/1">Siyuan Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hazboun_J/0/1/0/all/0/1">Jeffrey S. Hazboun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kelley_L/0/1/0/all/0/1">Luke Zoltan Kelley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simon_J/0/1/0/all/0/1">Joseph Simon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taylor_S/0/1/0/all/0/1">Stephen R. Taylor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vigeland_S/0/1/0/all/0/1">Sarah J. Vigeland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Witt_C/0/1/0/all/0/1">Caitlin A. Witt</a> With strong evidence of a common-spectrum stochastic process in the most recent datasets from the NANOGrav Collaboration, the European Pulsar Timing Array (PTA), Parkes PTA, and the International PTA, it is crucial to assess the effects of the several astrophysical and cosmological sources that could contribute to the stochastic gravitational wave background (GWB). UsingRead More →

Running vacuum versus Holographic dark energy: a cosmographic comparison. (arXiv:2207.14250v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Rezaei_M/0/1/0/all/0/1">Mehdi Rezaei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peracaula_J/0/1/0/all/0/1">Joan Sola Peracaula</a> We perform a comparative study of different types of dynamical dark energy models (DDES) using the cosmographic method. Among the models being examined herein we have the Running Vacuum models (RVMs), which have demonstrated considerable ability to fit the overall cosmological data at a level comparable to the standard cosmological model, $Lambda$CDM, and capable of alleviating the $sigma_8$ and $H_0$ tensions. At the same time we address a variety of Holographic dark energy models (HDEs) with different options for the time (redshift)-varying model parameter $c=c(z)$. WeRead More →

Chaotic diffusion of asteroids in the exterior 1:2 mean motion resonance with Mars. (arXiv:2207.14047v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Christou_A/0/1/0/all/0/1">Apostolos A. Christou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dermott_S/0/1/0/all/0/1">Stanley F. Dermott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_D/0/1/0/all/0/1">Dan Li</a> The inner asteroid belt between 2.1 and 2.5 au is of particular dynamical significance because it is the dominant source of both chondritic meteorites and near-Earth asteroids. This inner belt is bounded by an eccentricity-type secular resonance and by the 1:3 mean motion resonance with Jupiter. Unless asteroid perihelia are low enough to allow scattering by Mars, escape requires transport to one of the bounding resonances. In addition Yarkovsky forces are generally ineffective in changing either the eccentricityRead More →

Dynamical Friction in fuzzy dark matter: circular orbits. (arXiv:2207.13740v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Buehler_R/0/1/0/all/0/1">Robin Buehler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desjacques_V/0/1/0/all/0/1">Vincent Desjacques</a> We investigate the dynamical friction (DF) acting on circularly-moving perturbers in fuzzy dark matter (FDM) backgrounds. After condensation, FDM is described by a single wave function satisfying a Schr”odinger-Poisson equation. An equivalent, hydrodynamic formulation can be obtained through the Madelung transform. Here, we consider both descriptions and restrict our analysis to linear response theory. We take advantage of the hydrodynamic formulation to derive a fully analytic solution to the DF in steady-state and for a finite time perturbation. We compare our prediction to a numerical implementation of theRead More →

Periodic variable A-F spectral type stars in the northern TESS continuous viewing zone. (arXiv:2207.12922v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Skarka_M/0/1/0/all/0/1">M. Skarka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zak_J/0/1/0/all/0/1">J. &#x17d;&#xe1;k</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fedurco_M/0/1/0/all/0/1">M. Fedurco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paunzen_E/0/1/0/all/0/1">E. Paunzen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henzl_Z/0/1/0/all/0/1">Z. Henzl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masek_M/0/1/0/all/0/1">M. Ma&#x161;ek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karjalainen_R/0/1/0/all/0/1">R. Karjalainen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arias_J/0/1/0/all/0/1">J. P. Sanchez Arias</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sodor_A/0/1/0/all/0/1">&#xc1;. S&#xf3;dor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Auer_R/0/1/0/all/0/1">R. F. Auer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kabath_P/0/1/0/all/0/1">P. Kab&#xe1;th</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karjalainen_M/0/1/0/all/0/1">M. Karjalainen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liska_J/0/1/0/all/0/1">J. Li&#x161;ka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stegner_D/0/1/0/all/0/1">D. &#x160;tegner</a> The goal of our study is to provide a reliable classification of variability of A-F stars brighter than 11 mag located in the northern TESS continuous viewing zone. We also aim at thorough discussion about issues in the classification related to the data characteristicsRead More →

Pantheon+ tomography and Hubble tension. (arXiv:2207.10927v6 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_D/0/1/0/all/0/1">Deng Wang</a> The recently released Type Ia supernovae (SNe Ia) sample, Pantheon+, is an updated version of Pantheon and has very important cosmological implications. To explore the origin of the enhanced constraining power and internal correlations of datasets in different redshifts, we perform a comprehensively tomographic analysis of the Pantheon+ sample without and with the Cepheid host distance calibration, respectively. For both cases, after dividing the sample to 10 bins, we find that the first bin in the redshift range $zin[0.00122, , 0.227235]$ dominates the constraining power of the whole sample and there is no evidenceRead More →

COSMOS2020: The cosmic evolution of the stellar-to-halo mass relation for central and satellite galaxies up to z~5. (arXiv:2203.10895v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Shuntov_M/0/1/0/all/0/1">M. Shuntov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCracken_H/0/1/0/all/0/1">H. J. McCracken</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gavazzi_R/0/1/0/all/0/1">R. Gavazzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laigle_C/0/1/0/all/0/1">C. Laigle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weaver_J/0/1/0/all/0/1">J. R. Weaver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davidzon_I/0/1/0/all/0/1">I. Davidzon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ilbert_O/0/1/0/all/0/1">O. Ilbert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kauffmann_O/0/1/0/all/0/1">O. B. Kauffmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faisst_A/0/1/0/all/0/1">A. Faisst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dubois_Y/0/1/0/all/0/1">Y. Dubois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koekemoer_A/0/1/0/all/0/1">A. M. Koekemoer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moneti_A/0/1/0/all/0/1">A. Moneti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milvang_Jensen_B/0/1/0/all/0/1">B. Milvang-Jensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mobasher_B/0/1/0/all/0/1">B. Mobasher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanders_D/0/1/0/all/0/1">D. B. Sanders</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Toft_S/0/1/0/all/0/1">S. Toft</a> We use the COSMOS2020 catalogue to measure the stellar-to-halo mass relation (SHMR) divided by central and satellite galaxies from $z=0.2$ to $z = 5.5$. Starting from accurate photometric redshifts we measure theRead More →

The relation between optical and $gamma$-ray emission in BL Lac sources. (arXiv:2207.09764v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Mura_G/0/1/0/all/0/1">G. La Mura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_J/0/1/0/all/0/1">J. Becerra Gonzalez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiaro_G/0/1/0/all/0/1">G. Chiaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciroi_S/0/1/0/all/0/1">S. Ciroi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Otero_Santos_J/0/1/0/all/0/1">J. Otero-Santos</a> The relativistic jets produced by some Active Galactic Nuclei (AGNs) are among the most efficient persistent sources of non-thermal radiation and represent an ideal laboratory for studying high-energy interactions. In particular, when the relativistic jet propagates along the observer’s line of sight, the beaming effect produces dominant signatures in the observed spectral energy distribution (SED), from the radio domain up to the highest energies, with the further possibility of resulting in radiation-particle multi-messenger associations.Read More →

Atomic Gas Dominates the Baryonic Mass of Star-forming Galaxies at $z approx 1.3$. (arXiv:2207.08834v3 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Chowdhury_A/0/1/0/all/0/1">Aditya Chowdhury</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kanekar_N/0/1/0/all/0/1">Nissim Kanekar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chengalur_J/0/1/0/all/0/1">Jayaram N. Chengalur</a> We present a comparison between the average atomic gas mass, $langle M_{Atom}rangle$ (including HI and He), the average molecular gas mass, $langle M_{Mol}rangle$, and the average stellar mass, $langle M_*rangle$, of a sample of star-forming galaxies at $zapprox0.75-1.45$, to probe the baryonic composition of galaxies in and during the epoch of peak star-formation activity in the universe. The $langle M_{Atom}rangle$ values of star-forming galaxies in two stellar-mass matched samples at $z=0.74-1.25$ and $z=1.25-1.45$, were derived by stacking their HIRead More →

A bottom-up search for Lyman-continuum leakage in the Hubble Ultra Deep Field. (arXiv:2206.10799v3 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Rivera_Thorsen_T/0/1/0/all/0/1">T. Emil Rivera-Thorsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hayes_M/0/1/0/all/0/1">Matthew Hayes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melinder_J/0/1/0/all/0/1">Jens Melinder</a> Context: Studies of the production and escape of Lyman Continuum from galaxies often rely on array of indirect observational tracers in preselection of candidate leakers. Aims: Here, we investigate how much ionizing radiation might be missed due to these selection criteria by completely removing them and performing a search selected purely from rest-frame LyC emission; and how that affects our estimates of the ionizing background. Methods: We invert the conventional method and perform a bottom-up search for Lyman-continuum leaking galaxiesRead More →

Is [Y/Mg] a Reliable Age Diagnostic for FGK Stars?. (arXiv:2206.10624v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Berger_T/0/1/0/all/0/1">Travis A. Berger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saders_J/0/1/0/all/0/1">Jennifer L. van Saders</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huber_D/0/1/0/all/0/1">Daniel Huber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaidos_E/0/1/0/all/0/1">Eric Gaidos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlieder_J/0/1/0/all/0/1">Joshua E. Schlieder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Claytor_Z/0/1/0/all/0/1">Zachary R. Claytor</a> Current spectroscopic surveys are producing large catalogs of chemical abundances for stars of all types. The yttrium to magnesium ratio, [Y/Mg], has emerged as a candidate age indicator for solar twins in the local stellar neighborhood. However, it is unclear whether it is a viable age diagnostic for more diverse stellar types, so we investigate [Y/Mg] as an age indicator for the FGK-type planet host stars observed by $Kepler$. WeRead More →

Gaia Data Release 3: Mapping the asymmetric disc of the Milky Way. (arXiv:2206.06207v3 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Gaia/0/1/0/all/0/1">Gaia Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Drimmel_R/0/1/0/all/0/1">R. Drimmel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romero_Gomez_M/0/1/0/all/0/1">M. Romero-Gomez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chemin_L/0/1/0/all/0/1">L. Chemin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramos_P/0/1/0/all/0/1">P. Ramos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poggio_E/0/1/0/all/0/1">E. Poggio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ripepi_V/0/1/0/all/0/1">V. Ripepi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrae_R/0/1/0/all/0/1">R. Andrae</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blomme_R/0/1/0/all/0/1">R. Blomme</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cantat_Gaudin_T/0/1/0/all/0/1">T. Cantat-Gaudin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castro_Ginard_A/0/1/0/all/0/1">A. Castro-Ginard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clementini_G/0/1/0/all/0/1">G. Clementini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Figueras_F/0/1/0/all/0/1">F. Figueras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fouesneau_M/0/1/0/all/0/1">M. Fouesneau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fremat_Y/0/1/0/all/0/1">Y. Fremat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jardine_K/0/1/0/all/0/1">K. Jardine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khanna_S/0/1/0/all/0/1">S. Khanna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lobel_A/0/1/0/all/0/1">A. Lobel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshall_D/0/1/0/all/0/1">D. J. Marshall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muraveva_T/0/1/0/all/0/1">T. Muraveva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_A/0/1/0/all/0/1">A.G.A. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vallenari_A/0/1/0/all/0/1">A. Vallenari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prusti_T/0/1/0/all/0/1">T. Prusti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruijne_J/0/1/0/all/0/1">J.H.J. de Bruijne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arenou_F/0/1/0/all/0/1">F. Arenou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Babusiaux_C/0/1/0/all/0/1">C. Babusiaux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biermann_M/0/1/0/all/0/1">M. Biermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Creevey_O/0/1/0/all/0/1">O.L. Creevey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ducourant_C/0/1/0/all/0/1">C. Ducourant</a>, <aRead More →