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arXiv 2023年

作者： Smart, B.M. Haffner, L.M. Barger, K.A. Ciampa, D.A. Hill, A.S. Krishnarao, D. Madsen, G.J. Department of Astronomy University of Washington SeattleWA98195 United States Department of Physics Astronomy and Mathematics University of Hertfordshire HatfieldAL10 9AB United Kingdom Department of Astronomy University of Wisconsin-Madison MadisonWI53706 United States Department of Physical Sciences Embry-Riddle Aeronautical University Daytona BeachFL32114-3900 United States Department of Physics & Astronomy Texas Christian University Fort WorthTX76129 United States Department of Computer Science Math Physics and Statistics University of British Columbia Okanagan Campus KelownaBCV1V 1V7 Canada Space Science Institute BoulderCO80301 United States Dominion Radio Astrophysical Observatory Herzberg Program in Astronomy and Astrophysics National Research Council Canada PentictonBC Canada NSF Astronomy and Astrophysics Postdoctoral Fellow Johns Hopkins University BaltimoreMD21218 United States Department of Physics Colorado College Colorado SpringsCO United States Space Telescope Science Institute BaltimoreMD21218 United States Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom

The Large Magellanic Cloud (LMC) has an extensive Hα emission halo that traces an extended, warm ionized component of its interstellar medium. Using the Wisconsin Hα Mapper (WHAM) telescope, we present the first kinematic Hα survey of an extensive region around the LMC, from ( b) = (264◦. 5, −45◦. 5) to (295◦. 5, −19◦. 5), covering +150 ≤ vLSR ≤ +390 km s−1. We find that ionized hydrogen exists throughout the galaxy and extends several degrees beyond detected neutral hydrogen emission (log (NH i/cm−2 ) ≈ 18.3) as traced by 21-cm in current surveys. Using the column density structure of the neutral gas and stellar line-of-sight depths as a guide, we estimate the upper limit mass of the ionized component of the LMC to be roughly Mionized ≈ (0.6−1.8)×109 M☉, which is comparable to the total neutral atomic gas mass in the same region (Mneutral ≈ 0.75 − 0.85 × 109 M☉). Considering only the atomic phases, we find Mionized/Mionized+neutral, to be 46%–68% throughout the LMC and its extended halo. Additionally, we find an ionized gas cloud that extends off of the LMC at ( b) ≈ (285◦, −28◦) into a region previously identified as the Leading Arm complex. This gas is moving at a similar line-of-sight velocity as the LMC and has Mionized/Mionized+neutral = 13%–51%. This study, combined with previous studies of the SMC and extended structures of the Magellanic Clouds, continues to suggest that warm, ionized gas is as massive and dynamically-important as the neutral gas in the Magellanic System. © 2023, CC BY.

关键词： Galaxies

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Probing the Galactic Diffuse Continuum Emission with COSI

arXiv

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arXiv 2023年

作者： Karwin, Christopher M. Siegert, Thomas Beechert, Jacqueline Tomsick, John A. Porter, Troy A. Negro, Michela Kierans, Carolyn Ajello, Marco Castellanos, Israel Martinez Shih, Albert Zoglauer, Andreas Boggs, Steven E. NASA Postdoctoral Program Fellow United States NASA Goddard Space Flight Center GreenbeltMD20771 United States Julius-Maximilians-Universität Würzburg Fakultät für Physik und Astronomie Institut für Theoretische Physik und Astrophysik Lehrstuhl für Astronomie Emil-Fischer-Str. 31 WürzburgD-97074 Germany Space Sciences Laboratory UC Berkeley 7 Gauss Way BerkeleyCA94720 United States W.W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305 United States Department of Physics and Astronomy Louisiana State University Baton RougeLA70803 United States Department of Physics and Astronomy Clemson University ClemsonSC29634 United States Department of Astronomy University of Maryland College ParkMD20742 United States Department of Astronomy & Astrophysics UC San Diego 9500 Gilman Drive La Jolla CA92093 United States

In 2016 the Compton Spectrometer and Imager (COSI) had a successful 46-day flight onboard NASA’s Super Pressure Balloon platform. In this work we report measurements of the Galactic diffuse continuum emission (GDCE) observed towards the inner Galaxy during the flight, which in the COSI energy band (0.2 − 5 MeV) is primarily generated from inverse Compton radiation. Within uncertainties we find overall good agreement with previous measurements from INTEGRAL/SPI and COMPTEL. Based on these initial findings, we discuss the potential for further probing the GDCE with the 2016 COSI balloon data, as well as prospects for the upcoming satellite mission. © 2023, CC BY.

关键词： Uncertainty analysis

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Climate of the Field: Snowmass 2021

arXiv

引用

arXiv 2022年

作者： Hansen, Erin V. Smith, Erica Bard, Deborah Bellis, Matthew Esquivel, Jessica Lewis, Tiffany R. Geddes, Cameron Joe, Cindy Kim, Alex G. Patel, Asmita Pronskikh, Vitaly Castro, Johan Sebastian Bonilla Chen, Thomas Y. Choi, Ami Duffy, K.E. Dunne, Katherine Gill, Mandeep S.S. Kirby, Michael Kurahashi, N. Sharma, Vivek Simon, Sara M. Singh, Rajeev Stifter, K. Wolcott, J. Department of Physics University of California BerkeleyCA United States Indiana University BloomingtonIN United States LBNL CA United States Siena College LoudonvilleNY United States Fermi National Accelerator Laboratory BataviaIL United States Astroparticle Physics Laboratory NASA Goddard Space Flight Center GreenbeltMD United States NASA Postdoctoral Program Fellow United States Lawrence Berkeley National Laboratory BerkeleyCA United States University of California Davis United States Columbia University New YorkNY United States California Institute of Technology United States University of Oxford Oxford United Kingdom Stockholm University Sweden KIPAC Stanford University CA United States Drexel University United States Virginia Tech United States Institute of Nuclear Physics Polish Academy of Sciences Kraków Poland Tufts University MedfordMA United States

How are formal policies put in place to create an inclusive, equitable, safe environment? How do these differ between different communities of practice (institutions, labs, collaborations, working groups)? What policies towards a more equitable community are working? For those that aren’t working, what external support is needed in order to make them more effective? We present a discussion of the current climate of the field in high energy particle physics and astrophysics (HEPA), as well as current efforts toward making the community a more diverse, inclusive, and equitable environment. We also present issues facing both institutions and HEPA collaborations, with a set of interviews with a selection of HEPA collaboration DEI leaders. We encourage the HEPA community and the institutions & agencies that support it to think critically about the prioritization of people in HEPA over the coming decade, and what resources and policies need to be in place in order to protect and elevate minoritized populations within the HEPA community. © 2022, CC BY.

关键词： High energy physics

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Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroidal Galaxies with 14 Years of Fermi-LAT Data

arXiv

引用

arXiv 2023年

作者： McDaniel, Alex Ajello, Marco Karwin, Christopher M. Mauro, Mattia Di Drlica-Wagner, Alex Sànchez-Conde, Miguel Department of Physics and Astronomy Clemson University ClemsonSC29631 United States NASA Postdoctoral Program Fellow NASA Goddard Space Flight Center GreenbeltMD20771 United States Dipartimento di Fisica Universitá di Torino Via P. Giuria 1 Torino10125 Italy Istituto Nazionale di Fisica Nucleare Sezione di Torino Via P. Giuria 1 Torino10125 Italy Fermi National Accelerator Laboratory P.O. Box 500 BataviaIL60510 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Instituto de Física Teórica IFT UAM-CSIC Departamento de Física Teórica Universidad Autónoma de Madrid MadridES-28049 Spain

The Milky Way dwarf spheroidal satellite galaxies (dSphs) are particularly intriguing targets to search for gamma rays from Weakly Interacting Massive Particle (WIMP) dark matter (DM) annihilation or decay. They are nearby, DM-dominated, and lack significant emission from standard astrophysical processes. Previous studies using the Fermi-Large Area Telescope (LAT) of DM-induced emission from dSphs have provided the most robust and stringent constraints on the DM annihilation cross section and mass. We report here an analysis of the Milky Way dSphs using over 14 years of LAT data along with an updated census of dSphs and J-factor estimates. While no individual dSphs are significantly detected, we do find slight excesses with respect to background at the 2 σ local significance level in both tested annihilation channels (bb¯, τ+τ−) for seven of the dSphs. We do not find a significant DM signal from the combined likelihood analysis of the dSphs (sglobal ∼ 0.5σ), yet a marginal local excess relative to background at a 2 − 3 σ level is observed at a DM mass of Mχ = 150 − 230 GeV (Mχ = 30 − 50 GeV) for DM annihilation into bb¯ (τ+τ−). Given the lack of a significant detection, we place updated constraints on the bb¯ and τ+τ− annihilation channels that are generally consistent with previous recent results. As in past studies, tension is found with some WIMP DM interpretations of the Galactic Center Excess (GCE), though the limits are consistent with other interpretations given the uncertainties of the Galactic DM density profile and GCE systematics. Based on conservative assumptions of improved sensitivity with increased Fermi-LAT exposure time and moderate increases in the sample of Milky Way dSphs, we project that the local ∼ 2 σ signal, if real, could approach the ∼ 4 σ local confidence level with additional ∼ 10 years of observation. © 2023, CC BY.

关键词： Galaxies

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The Compton Spectrometer and Imager 38

The Compton Spectrometer and Imager

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38th International Cosmic Ray Conference, ICRC 2023

作者： Tomsick, John A. Boggs, Steven E. Zoglauer, Andreas Hartmann, Dieter Ajello, Marco Burns, Eric Fryer, Chris Karwin, Chris Kierans, Carolyn Lowell, Alexander Malzac, Julien Roberts, Jarred Saint-Hilaire, Pascal Shih, Albert Siegert, Thomas Sleator, Clio Takahashi, Tadayuki Tavecchio, Fabrizio Wulf, Eric Beechert, Jacqueline Gulick, Hannah Joens, Alyson Lazar, Hadar Neights, Eliza Oliveros, Juan Carlos Martinez Matsumoto, Shigeki Melia, Tom Yoneda, Hiroki Amman, Mark Bal, Dhruv von Ballmoos, Peter Bates, Hugh Böttcher, Markus Bulgarelli, Andrea Cavazzuti, Elisabetta Chang, Hsiang-Kuang Chen, Claire Chu, Che-Yen Ciabattoni, Alex Costamante, Luigi Dreyer, Lente Fioretti, Valentina Fenu, Francesco Gallego, Savitri Ghirlanda, Giancarlo Grove, Eric Huang, Chien-You Jean, Pierre Khatiya, Nikita Knödlseder, Jürgen Krause, Martin Leising, Mark Lewis, Tiffany R. Lommler, Jan Peter Marcotulli, Lea Martinez-Castellanos, Israel Mittal, Saurabh Negro, Michela Al Nussirat, Samer Nakazawa, Kazuhiro Oberlack, Uwe Palmore, David Panebianco, Gabriele Parmiggiani, Nicolo Parsotan, Tyler Pike, Sean N. Rogers, Field Schutte, Hester Sheng, Yong Smale, Alan P. Smith, Jacob Trigg, Aaron Venters, Tonia Watanabe, Yu Zhang, Haocheng Space Sciences Laboratory University of California 7 Gauss Way BerkeleyCA94720-7450 United States Department of Astronomy & Astrophysics UC San Diego 9500 Gilman Drive La Jolla CA92093 United States Clemson University SC United States Louisiana State University Baton RougeLA70803 United States Los Alamos National Laboratory New Mexico United States NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States Institut de Recherche en Astrophysique et Planetologie 9 avenue du Colonel Roche BP 44346 Cedex 4 Toulouse31028 France Institut für Theoretische Physik und Astrophysik Universität Würzburg Campus Hubland Nord Emil-Fischer-Str. 31 Würzburg97074 Germany U.S. Naval Research Laboratory 4555 Overlook Ave. SW WashingtonDC20375 United States Kavli Institute for the Physics and Mathematics of the Universe The University of Tokyo Japan Istituto Nazionale di Astrofisica Merate Italy George Washington University United States United States Centre for Space Research North-West University Potchefstroom2520 South Africa Istituto Nazionale di Astrofisica Bologna Italy Italian Space Agency Italy Institute of Astronomy National Tsing Hua University Guangfu Rd. Hsinchu City300044 Taiwan Institut für Physik & Exzellenzcluster PRISMA+ Johannes Gutenberg-Universität Mainz Mainz55099 Germany Centre for Astrophysics Research Department of Physics Astronomy and Mathematics University of Hertfordshire College Lane HatfieldAL10 9AB United Kingdom Yale University United States University of Maryland United States Nagoya University Japan NASA Postdoctoral Program Fellow United States

The Compton Spectrometer and Imager (COSI) is a NASA Small Explorer (SMEX) satellite mission in development with a planned launch in 2027. COSI is a wide-field gamma-ray telescope designed to survey the entire sky at 0.2-5 MeV. It provides imaging, spectroscopy, and polarimetry of astrophysical sources, and its germanium detectors provide excellent energy resolution for emission line measurements. Science goals for COSI include studies of 0.511 MeV emission from antimatter annihilation in the Galaxy, mapping radioactive elements from nucleosynthesis, determining emission mechanisms and source geometries with polarization measurements, and detecting and localizing multimessenger sources. The instantaneous field of view for the germanium detectors is >25% of the sky, and they are surrounded on the sides and bottom by active shields, providing background rejection as well as allowing for detection of gamma-ray bursts and other gamma-ray flares over most of the sky. In the following, we provide an overview of the COSI mission, including the science, the technical design, and the project status. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： NASA

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The cosipy library: COSI’s high-level analysis software 38

The cosipy library: COSI’s high-level analysis software

引用

38th International Cosmic Ray Conference, ICRC 2023

作者： Martinez-Castellanos, Israel Gallego, Savitri Huang, Chien-You Karwin, Chris Kierans, Carolyn Lommler, Jan Peter Mittal, Saurabh Negro, Michela Neights, Eliza Pike, Sean N. Sheng, Yong Siegert, Thomas Yoneda, Hiroki Zoglauer, Andreas Tomsick, John A. Boggs, Steven E. Hartmann, Dieter Ajello, Marco Burns, Eric Fryer, Chris Lowell, Alexander Malzac, Julien Roberts, Jarred Saint-Hilaire, Pascal Shih, Albert Sleator, Clio Takahashi, Tadayuki Tavecchio, Fabrizio Wulf, Eric Beechert, Jacqueline Gulick, Hannah Joens, Alyson Lazar, Hadar Oliveros, Juan Carlos Martinez Matsumoto, Shigeki Melia, Tom Amman, Mark Bal, Dhruv von Ballmoos, Peter Bates, Hugh Böttcher, Markus Bulgarelli, Andrea Cavazzuti, Elisabetta Chang, Hsiang-Kuang Chen, Claire Chu, Che-Yen Ciabattoni, Alex Costamante, Luigi Dreyer, Lente Fioretti, Valentina Fenu, Francesco Ghirlanda, Giancarlo Grove, Eric Jean, Pierre Khatiya, Nikita Knödlseder, Jürgen Krause, Martin Leising, Mark Lewis, Tiffany R. Marcotulli, Lea Nussirat, Samer Al Nakazawa, Kazuhiro Oberlack, Uwe Palmore, David Panebianco, Gabriele Parmiggiani, Nicolo Parsotan, Tyler Rogers, Field Schutte, Hester Smale, Alan P. Smith, Jacob Trigg, Aaron Venters, Tonia Watanabe, Yu Zhang, Haocheng Space Sciences Laboratory University of California 7 Gauss Way BerkeleyCA94720-7450 United States Department of Astronomy & Astrophysics UC San Diego 9500 Gilman Drive La Jolla CA92093 United States Clemson University SC United States Louisiana State University Baton RougeLA70803 United States Los Alamos National Laboratory New Mexico United States NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States Institut de Recherche en Astrophysique et Planetologie 9 avenue du Colonel Roche BP 44346 Cedex 4 Toulouse31028 France Institut für Theoretische Physik und Astrophysik Universität Würzburg Campus Hubland Nord Emil-Fischer-Str. 31 Würzburg97074 Germany U.S. Naval Research Laboratory 4555 Overlook Ave. SW WashingtonDC20375 United States Kavli Institute for the Physics and Mathematics of the Universe The University of Tokyo Japan Istituto Nazionale di Astrofisica Merate Italy George Washington University United States United States Centre for Space Research North-West University Potchefstroom2520 South Africa Istituto Nazionale di Astrofisica Bologna Italy Italian Space Agency Italy Institute of Astronomy National Tsing Hua University Guangfu Rd. Hsinchu City300044 Taiwan Institut für Physik & Exzellenzcluster PRISMA+ Johannes Gutenberg-Universität Mainz Mainz55099 Germany Centre for Astrophysics Research Department of Physics Astronomy and Mathematics University of Hertfordshire College Lane HatfieldAL10 9AB United Kingdom Yale University United States University of Maryland United States Nagoya University Japan NASA Postdoctoral Program Fellow United States

The Compton Spectrometer and Imager (COSI) is a selected Small Explorer (SMEX) mission launching in 2027. It consists of a large field-of-view Compton telescope that will probe with increased sensitivity the under-explored MeV gamma-ray sky (0.2-5 MeV). We will present the current status of cosipy, a Python library that will perform spectral and polarization fits, image deconvolution, and all high-level analysis tasks required by COSI’s broad science goals: uncovering the origin of the Galactic positrons, mapping the sites of Galactic nucleosynthesis, improving our models of the jet and emission mechanism of gamma-ray bursts (GRBs) and active galactic nuclei (AGNs), and detecting and localizing gravitational wave and neutrino sources. The cosipy library builds on the experience gained during the COSI balloon campaigns and will bring the analysis of data in the Compton regime to a modern open-source likelihood-based code, capable of performing coherent joint fits with other instruments using the Multi-Mission Maximum Likelihood framework (3ML). In this contribution, we will also discuss our plans to receive feedback from the community by having yearly software releases accompanied by publicly-available data challenges. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Active Galactic Nuclei

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JWST/NIRCam Detection of the Fomalhaut C Debris Disk in Scattered Light

arXiv

引用

arXiv 2024年

作者： Lawson, Kellen Schlieder, Joshua E. Leisenring, Jarron M. Bogat, Ell Beichman, Charles A. Bryden, Geoffrey Gáspár, András Groff, Tyler D. McElwain, Michael W. Meyer, Michael R. Barclay, Thomas Calissendorff, Per De Furio, Matthew Li, Yiting Rieke, Marcia J. Ygouf, Marie Greene, Thomas P. Girard, Julien H. Gennaro, Mario Kammerer, Jens Rest, Armin Roellig, Thomas L. Sunnquist, Ben NASA-Goddard Space Flight Center GreenbeltMD United States NASA Postdoctoral Program Fellow Steward Observatory University of Arizona 933 N. Cherry Avenue TucsonAZ85721 United States Department of Astronomy University of Maryland College ParkMD20782 United States NASA Exoplanet Science Institute IPAC Jet Propulsion Laboratory California Institute of Technology 1200 E California Blvd PasadenaCA91125 United States Jet Propulsion Laboratory California Institute of Technology PasadenaCA United States Department of Astronomy University of Michigan 1085 S. University Ann ArborMI48109 United States NASA Ames Research Center MS 245-6 Moffett FieldCA94035 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States The William H. Miller III Department of Physics & Astronomy Bloomberg Center for Physics and Astronomy Johns Hopkins University 3400 N. Charles Street BaltimoreMD21218 United States European Southern Observatory Karl-Schwarzschild-Straße 2 Garching85748 Germany

Observations of debris disks offer important insights into the formation and evolution of planetary systems. Though M dwarfs make up approximately 80% of nearby stars, very few M-dwarf debris disks have been studied in detail — making it unclear how or if the information gleaned from studying debris disks around more massive stars extends to the more abundant M dwarf systems. We report the first scattered-light detection of the debris disk around the M4 star Fomalhaut C using JWST’s Near Infrared Camera (NIRCam;3.6 µm and 4.4 µm). This result adds to the prior sample of only four M-dwarf debris disks with detections in scattered light, and marks the latest spectral type and oldest star among them. The size and orientation of the disk in these data are generally consistent with the prior ALMA sub-mm detection. Though no companions are identified, these data provide strong constraints on their presence — with sensitivity sufficient to recover sub-Saturn mass objects in the vicinity of the disk. This result illustrates the unique capability of JWST for uncovering elusive M-dwarf debris disks in scattered light, and lays the groundwork for deeper studies of such objects in the 2–5 µm regime. Copyright © 2024, The Authors. All rights reserved.

关键词： Stars

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Single-shot readout of a solid-state spin in a decoherence-free subspace

arXiv

引用

arXiv 2020年

作者： Farfurnik, Demitry Pettit, R.M. Luo, Z. Waks, E. Department of Electrical and Computer Engineering Institute for Research in Electronics and Applied Physics Joint Quantum Institute University of Maryland College ParkMD20742 United States Intelligence Community Postdoctoral Research Fellowship Program University of Maryland College ParkMD20742 United States

The efficient single photon emission capabilities of quantum dot molecules position them as promising platforms for quantum information processing. Furthermore, quantum dot molecules feature a "decoherence-free" subspace that enables spin qubits with long coherence time. To efficiently read out the spin state within this subspace requires optically cycling isolated transitions that originate from a triplet manifold within the quantum dot molecule. We propose and theoretically study a two-stage spin readout protocol within this decoherence-free subspace that allows single-shot readout performance. The process incorporates a microwave π-pulse and optically cycling the isolated transitions, which induces fluorescence that allows us to identify the initial spin state. This protocol offers enhanced readout fidelity compared to previous schemes that rely on the excitation of transitions that strongly decay to multiple ground states or require long initialization via slow, optically forbidden transitions. By simulating the performance of the protocol, we show that an optimal spin readout fidelity of over 97% and single-shot readout performance are achievable for a photon collection efficiency of just 0.12%. This high readout performance for such realistic photon collection conditions within the decoherence-free subspace expands the potential of quantum dot molecules as building blocks for quantum networks. Copyright © 2020, The Authors. All rights reserved.

关键词： Spin dynamics

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A NuSTAR and Chandra Investigation of the Misaligned Outflow of PSR J1101-6101 and the Lighthouse Pulsar Wind Nebula

arXiv

引用

arXiv 2022年

作者： Klingler, Noel Hare, Jeremy Kargaltsev, Oleg Pavlov, George G. Tomsick, John Center for Space Sciences and Technology University of Maryland Baltimore County BaltimoreMD21250 United States Astrophysics Science Division NASA Goddard Space Flight Center GreenbeltMD20771 United States Center for Research and Exploration in Space Science and Technology NASA Goddard Space Flight Center GreenbeltMD20771 United States NASA Postdoctoral Program Fellow Department of Physics The George Washington University WashingtonDC20052 United States Department of Astronomy & Astrophysics The Pennsylvania State University 525 Davey Laboratory University ParkPA16802 United States Space Sciences Laboratory University of California BerkeleyCA94720 United States

PSR J1101-6101 is an energetic young pulsar which powers the remarkable Lighthouse pulsar wind nebula (PWN). The pulsar belongs to the rare type of radio- and gamma-ray-quiet pulsars which are bright in hard X-rays. Moreover, the Lighthouse PWN is remarkable for its misaligned outflow (which gave rise to the PWN's nickname). Also known as "pulsar filaments", these collimated parsec-scale X-ray structures have been recently discovered in the vicinity of a handful of fast-moving pulsars, and appear unaffected by the ram pressure which confines pulsar tails. We report on NuSTAR observations of PSR J1101-6101 and its misaligned outflow - the first observation of such a structure above ∼10 keV. We detect the outflow up to 25 keV, spatially resolve its spectral evolution with distance from the pulsar, find unambiguous evidence of spectral cooling with distance from the pulsar, and infer physical properties of the particles and magnetic field in the outflow. We also reanalzye archival Chandra data and discuss the outflow's small-scale structure. We detect pulsations from PSR J1101-6101 up to 20 keV, present the X-ray pulse profile, confirm its period derivative, and perform phase-resolved spectroscopy. Lastly, we discuss the X-ray source 2CXO J110158.4-605649 = 2XMM J110158.5-605651 (a serendipitously observed blazar) and suggest it may be the X-ray counterpart to the GeV source 4FGL J1102.0-6054. © 2022, CC BY-NC-SA.

关键词： Pulsars

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Ultra-light axions and the S8 tension: joint constraints from the cosmic microwave background and galaxy clustering

arXiv

引用

arXiv 2023年

作者： Rogers, Keir K. Hložek, Renée Laguë, Alex Ivanov, Mikhail M. Philcox, Oliver H.E. Cabass, Giovanni Akitsu, Kazuyuki Marsh, David J.E. Dunlap Institute for Astronomy & Astrophysics University of Toronto 50 St.George Street TorontoONM5S 3H4 Canada David A.Dunlap Department of Astronomy & Astrophysics University of Toronto 50 St.George Street TorontoONM5S 3H4 Canada Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104-6396 United States Canadian Institute for Theoretical Astrophysics University of Toronto 60 St.George Street TorontoONM5S 3H8 Canada School of Natural Sciences Institute for Advanced Study 1 Einstein Drive PrincetonNJ08540 United States NASA Hubble Fellowship Program Einstein Postdoctoral Fellow United States Center for Theoretical Physics Department of Physics Columbia University 538 West 120th Street New YorkNY10027 United States Simons Society of Fellows Simons Foundation New YorkNY10010 United States Department of Astrophysical Sciences Princeton University Peyton Hall 4 Ivy Lane PrincetonNJ08544 United States Theoretical Particle Physics and Cosmology King’s College London Strand LondonWC2R 2LS United Kingdom

We search for ultra-light axions as dark matter (DM) and dark energy particle candidates, for axion masses 10−32 eV ≤ ma ≤ 10−24 eV, by a joint analysis of cosmic microwave background (CMB) and galaxy clustering data – and consider if axions can resolve the tension in inferred values of the matter clustering parameter S8. We give legacy constraints from Planck 2018 CMB data, improving 2015 limits on the axion density Ωah2 by up to a factor of three;CMB data from the Atacama Cosmology Telescope and the South Pole Telescope marginally weaken Planck bounds at ma = 10−25 eV, owing to lower (and theoretically-consistent) gravitational lensing signals. We jointly infer, from Planck CMB and full-shape galaxy power spectrum and bispectrum data from the Baryon Oscillation Spectroscopic Survey (BOSS), that axions are, today, a ≤ 10−26 eV and −30 eV ≤ ma ≤ 10−28 eV. BOSS data strengthen limits, in particular at higher ma by probing high-wavenumber modes (k −1). BOSS alone finds a preference for axions at 2.7σ, for ma = 10−26 eV, but Planck disfavours this result. Nonetheless, axions in a window 10−28 eV ≤ ma ≤ 10−25 eV can improve consistency between CMB and galaxy clustering data, e. g., reducing the S8 discrepancy from 2.7σ to 1.6σ, since these axions suppress structure growth at the 8h−1 Mpc scales to which S8 is sensitive. We expect improved constraints with upcoming high-resolution CMB and galaxy lensing and future galaxy clustering data, where we will further assess if axions can restore cosmic concordance. Copyright © 2023, The Authors. All rights reserved.

关键词： Galaxies

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